{"id": "conditionality_train_pos_0000", "text": "-in monitor, you have to rely on the small information display on the front of the camera. Press the power/mode button to cycle through the different modes until you land on time-lapse and press the settings button on the side of the camera to select it. This will bring up the time-lapse options, including resolution and interval. Use the power/mode button to cycle through the list of options, and the shutter button to change them. If you have GoPro’s accompanying smartphone app, you can control all of these settings through the app, which is much more straightforward. It’s available on both Android and iOS. Other tips Remember, in Time Lapse Video mode, your camera will only store the final MP4 video, not the individual stills captured. If you want to save the individual stills, select Time Lapse Photo mode. This won’t automatically stitch a video for you, but it will give you more control in post-production, where you can zoom and pan around the 12MP photos to add motion to your time-lapse video. Also, as with any video, it’s helpful to record a little more than you think you’ll need. You never know when you’ll need a little more footage or need to trim the beginning and end for an intro. With a time-lapse, however, getting “a little more than you’ll need” may translate to quite a few minutes of extra recording time, depending on your interval, so it is best if you can plan your shot ahead of time and know exactly how much footage you’ll need.", "label": 1, "domain": "news", "token_count": 318, "matched_pair_id": "conditionality_00722", "split": "train"}
{"id": "conditionality_train_pos_0001", "text": "We present interferometric imaging at 33 GHz, with the new superextended configuration of the Very Small Array (VSA), of a very deep decrement in the cosmic microwave background (CMB) temperature. This decrement is located in the direction of the Corona Borealis supercluster, at a position with no known galaxy clusters, and was discovered by a previous VSA survey (Genova-Santos et al.). A total area of 3 sq.deg. has now been imaged, with an angular resolution of 7 arcmin and a flux sensitivity of 5 mJy/beam. These observations confirm the presence of this strong and resolved negative spot at -41+/-5 mJy/beam (-258+/-29 muK), with a signal to noise level of 8. This structure is also present in the WMAP 5-year data. The temperature of the W-band (94 GHz) data at the position of the decrement agrees within 1.2-sigma with that observed by the VSA at 33 GHz, and within 0.2-sigma with the Sunyaev-Zel'dovich (SZ) spectrum. Our analyses show that it is a non-Gaussian feature in the CMB at a level of 4.8-sigma. The probability of finding such a deviation or larger in CMB Gaussian simulations is only 0.19 per cent. Therefore, an explanation other than primordial CMB is required. We have considered the possibility of an SZ effect generated in a diffuse, extended warm/hot gas distribution. This hypothesis is especially relevant, as the presence of such structures, if confirmed, could provide the location for a significant fraction of the missing baryons in the Local Universe.", "label": 1, "domain": "academic", "token_count": 353, "matched_pair_id": "conditionality_00054", "split": "train"}
{"id": "conditionality_train_pos_0002", "text": "In recent work, Benjamin Schumacher and Michael~D. Westmoreland investigate a version of quantum mechanics which they call \"modal quantum theory\" but which we prefer to call \"discrete quantum theory\". This theory is obtained by instantiating the mathematical framework of Hilbert spaces with a finite field instead of the field of complex numbers. This instantiation collapses much the structure of actual quantum mechanics but retains several of its distinguishing characteristics including the notions of superposition, interference, and entanglement. Furthermore, discrete quantum theory excludes local hidden variable models, has a no-cloning theorem, and can express natural counterparts of quantum information protocols such as superdense coding and teleportation. Our first result is to distill a model of discrete quantum computing from this quantum theory. The model is expressed using a monadic metalanguage built on top of a universal reversible language for finite computations, and hence is directly implementable in a language like Haskell. In addition to superpositions and invertible linear maps, the model includes conventional programming constructs including pairs, sums, higher-order functions, and recursion. Our second result is to relate this programming model to relational programming, e.g., a pure version of Prolog over finite relations. Surprisingly discrete quantum computing is identical to conventional logic programming except for a small twist that is responsible for all the ``quantum-ness.'' The twist occurs when merging sets of answers computed by several alternatives: the answers are combined using an \"exclusive\" version of logical disjunction. In other words, the two branches of a choice junction exhibit an \"interference\" effect: an answer is produced from the junction if it occurs in one or the other branch but not both.", "label": 1, "domain": "academic", "token_count": 337, "matched_pair_id": "conditionality_00305", "split": "train"}
{"id": "conditionality_train_pos_0003", "text": "such government or entity has authority, and ``(ii) the aggregate amount involved in all court orders and agreements with respect to the violation, investigation, or inquiry is $600 or more. ``(B) Adjustment of reporting threshold.--The Secretary may adjust the $600 amount in subparagraph (A)(ii) as necessary in order to ensure the efficient administration of the internal revenue laws. ``(3) Time of filing.--The return required under this subsection shall be filed at the time the agreement is entered into, as determined by the Secretary. ``(b) Statements To Be Furnished to Individuals Involved in the Settlement.--Every person required to make a return under subsection (a) shall furnish to each person who is a party to the suit or agreement a written statement showing-- ``(1) the name of the government or entity, and ``(2) the information supplied to the Secretary under subsection (a)(1). The written statement required under the preceding sentence shall be furnished to the person at the same time the government or entity provides the Secretary with the information required under subsection (a). ``(c) Appropriate Official Defined.--For purposes of this section, the term `appropriate official' means the officer or employee having control of the suit, investigation, or inquiry or the person appropriately designated for purposes of this section.''. (b) Conforming Amendment.--The table of sections for subpart B of part III of subchapter A of chapter 61 of the Internal Revenue Code of 1986 is amended by inserting after the item relating to section 6050W the following new item: ``Sec. 6050X. Information with respect to certain fines, penalties, and other amounts.''. (c) Effective Date.--The amendments made by this section shall apply to amounts paid or incurred on or after the date of the enactment of this Act, except that such amendments shall not apply to amounts paid or incurred under any binding order or agreement entered into before such date. Such exception shall not apply to an order or agreement requiring court approval unless the approval was obtained before such date.", "label": 1, "domain": "government", "token_count": 415, "matched_pair_id": "conditionality_01026", "split": "train"}
{"id": "conditionality_train_pos_0004", "text": "can “make it” despite their ancestors having faced historical discrimination, then it’s your fault if you can’t. They’re not suffering from “Irish Amnesia” as much as “Irish Flattery” or “Irish Selfishness.” In 2002, leftist activist Tom Hayden attempted to revise Irish America’s reactionary, right-wing legacy by proposing an alternative history in his book, Irish on the Inside. Hayden recounts some of the most notable historical instances of Irish American resistance, including stories of the San Patricios and the Molly Maguires. As with most radical leftist history, these stories are often omitted from U.S. history curricula. In sharp contrast to the dominant image of America’s Irish, Edward Said, a Palestinian American intellectual and founder of the academic field of postcolonial studies, lauded Ireland for its “fabulous culture of resistance.” “I am so grateful to Ireland,” he said in a June 1999 interview in Dublin four years before his death. “You have had many more years of imperialism than we [Palestinians] have had, and you have produced a fabulous culture of resistance and an extraordinary spirit, which I desperately hope we can measure up to by about 10 percent.” Said’s admiration of Irish resilience in response to centuries of British colonialism fills me with melancholy and distress when I consider the pervasive perception of contemporary Irish America. I urge Americans of Irish descent to collectively revisit and deepen their understanding of the colonial and oppressive conditions that produced the Irish diaspora. I advocate for St. Patrick’s Day to become a day of remembrance of Ireland and Irish America’s intertwined historical experiences of oppression. Perhaps consider organizing an “Irish Stand” like the one in New York City, an occasion of resistance to colonial and oppressive systems across ethnicities, races, genders, and classes, rather than the typical event with green beer, corned beef and cabbage, and shamrock decorations. And if you do, you can still have a pint.", "label": 1, "domain": "news", "token_count": 404, "matched_pair_id": "conditionality_00633", "split": "train"}
{"id": "conditionality_train_pos_0005", "text": "Molecular globules and pillars are spectacular features, found only in the interface region between a molecular cloud and an HII-region. Impacting Far-ultraviolet (FUV) radiation creates photon dominated regions (PDRs) on their surfaces that can be traced by typical cooling lines. With the GREAT receiver onboard SOFIA we mapped and spectrally resolved the [CII] 158 micron atomic fine-structure line and the highly excited 12CO J=11-10 molecular line from three objects in Cygnus X (a pillar, a globule, and a strong IRAS source). We focus here on the globule and compare our data with existing Spitzer data and recent Herschel Open-Time PACS data. Extended [CII] emission and more compact CO-emission was found in the globule. We ascribe this emission mainly to an internal PDR, created by a possibly embedded star-cluster with at least one early B-star. However, external PDR emission caused by the excitation by the Cyg OB2 association cannot be fully excluded. The velocity-resolved [CII] emission traces the emission of PDR surfaces, possible rotation of the globule, and high-velocity outflowing gas. The globule shows a velocity shift of ~2 km/s with respect to the expanding HII-region, which can be understood as the residual turbulence of the molecular cloud from which the globule arose. This scenario is compatible with recent numerical simulations that emphazise the effect of turbulence. It is remarkable that an isolated globule shows these strong dynamical features traced by the [CII]-line, but it demands more observational studies to verify if there is indeed an embedded cluster of B-stars.", "label": 1, "domain": "academic", "token_count": 351, "matched_pair_id": "conditionality_00434", "split": "train"}
{"id": "conditionality_train_pos_0006", "text": "Maps of low-inclination nearby galaxies in Sloan Digitized Sky Survey u-g, g-r and r-i colors are used to determine whether Ultraluminous X-ray sources (ULXs) are predominantly associated with star-forming regions of their host galaxies. An empirical selection criterion is derived from colors of HII regions in M81 and M101 that differentiates between the young, blue stellar component and the older disk and bulge population. This criterion is applied to a sample of 58 galaxies of Hubble type S0 and later and verified through an application of Fisher's linear discriminant analysis. It is found that 60% (49%) of ULXs in optically-bright environments are within regions blueward of their host galaxy's HII regions compared to only 27% (0%) of a control sample according to the empirical (Fisher) criterion. This is an excess of 3-sigma above the 32% (27%) expected if the ULXs were randomly distributed within their galactic hosts. This indicates a ULX preference for young, approximately <10 Myr, OB associations. However, none of the ULX environments have the morphology and optical brightness suggestive of a massive young super star cluster though several are in extended or crowded star-forming (blue) environments that may contain clusters unresolved by Sloan imaging. Ten of the 12 ULX candidates with estimated X-ray luminosities in excess of 3e39 erg/s are equally divided among the group of ULX environments redward of HII regions and the group of optically faint regions. This likely indicates that the brightest ULXs turn on at a time somewhat later than typical of HII regions; say 10-20 Myr after star formation has ended. This would be consistent with the onset of an accretion phase as the donor star ascends the giant branch if the donor is a <20 solar-mass star.", "label": 1, "domain": "academic", "token_count": 392, "matched_pair_id": "conditionality_00156", "split": "train"}
{"id": "conditionality_train_pos_0007", "text": "We use analytical and N-body methods to examine the survival of wide stellar binaries against repeated encounters with dark substructures orbiting in the dark matter haloes of dwarf spheroidal galaxies (dSphs). Our models adopt cosmologically-motivated conditions wherein dSphs are dark-matter dominated systems that form hierarchically and orbit about a host galaxy. Our analytical estimates show that wide binaries are disrupted at a rate that is proportional to the local density of dark substructures averaged over the life-time of the binary population. The fact that external tides can efficiently strip dark substructures from the outskirts of dSphs implies that the present number and distribution of binaries is strongly coupled with the mass evolution of individual galaxies. Yet we show that for the range of dynamical masses and Galactocentric distances spanned by Milky Way dSphs, a truncation in the separation function at a_max <~ 0.1 pc is expected in all these galaxies. An exception may be the Sagittarius dSph, which has lost most of is dark matter envelope to tides and is close to full disruption. Our simulations indicate that at separations larger than a_max the perturbed binary distribution scales as dN/da \\propto a^{-2.1} independently of the mass and density of substructures. These results may be used to determine whether the binary separation function found in dwarf galaxies is compatible with the scale-free hierarchical picture that envisions the existence of dark substructures in all galactic haloes. We show that the ACS camera on board of the Hubble telescope may be able to test this prediction in dSphs at heliocentric distances <100 kpc, even if the binary fraction amounts only 10% of the stellar population.", "label": 1, "domain": "academic", "token_count": 360, "matched_pair_id": "conditionality_00233", "split": "train"}
{"id": "conditionality_train_pos_0008", "text": "If you’re lucky, every once in a while you get to spend an evening with great artists. You enjoy an up-close look at their work, and learn about their philosophy, inspirations and struggles. You get insight into what their work means to them. If you’re really lucky, you get to talk to them about your own work. The Ojai Photo Club turns this rare opportunity into a regular event. Once a month the club hosts a free presentation that’s open to the public. In the past the club has hosted talks by rock ’n’ roll photographer Guy Webster, documentary photographer Colin Finlay and surf photographer Elizabeth Pepin Silva. After the presentation, club members are invited to have their own print or digital photos reviewed by the guest, and then everyone chats over refreshments. It’s all very informal, supportive and inspiring. The members range from high school students to retirees, and include professional and nonprofessional photographers from all over Ventura County. The atmosphere is noncompetitive, but the quality of work is high, and members seek to help each other get better. “It’s a thrilling thing to see a photographer’s growth,” says Myrna Cambianica, the club’s education chair. The Ojai Photo Club will host its next presenter on Tuesday, June 20, at Help of Ojai’s Kent Hall. Internationally renowned photographer, archivist and educator Lewis Watts will present “Documenting the Cultural Landscape,” which will show the trajectory of his work and depict “how journey and culture are evidenced in the landscape.” Watts first became fascinated with the effects of migration while visiting France as a graduate student in the 1960s. He began asking the questions: “What happens when people go from one place to another? What do they bring with them? What remains intact and what changes?” These questions still resonate in Watts’ work and have propelled him to travel the world, from the American South to France, Cuba and Greece. He recently visited the Syrian refugee camp in Calais and was struck by what he encountered. “There was a consistent dignity,” Watts recalls. “I heard stories of horrendous ordeals, and yet everyone was very generous. They had nothing, but they offered me tea and coffee.” Wherever Watts has traveled, he says he’s noticed “traces of what people have brought with them,” and adds that, “there are certain things that are locked in the past.” Even while trying to assimilate to a new", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00517", "split": "train"}
{"id": "conditionality_train_pos_0009", "text": "During the last decade, the FORS1 instrument of the ESO VLT has been extensively used to study stellar magnetism. A number of interesting discoveries of magnetic fields in several classes of stars have been announced, many of which obtained at a ~3 sigma level; some of the discoveries are confirmed by measurements obtained with other instruments, some are not. Here we investigate the reasons for the discrepancies between the results obtained with FORS1 and those obtained with other instruments. Using the ESO FORS pipeline, we have developed a semi-automatic procedure for magnetic field determination. We have applied this procedure to the full content of circular spectropolarimetric measurements of the FORS1 archive. We have devised and applied a number of consistency checks to our field determinations, and we have compared our results to those previously published in the literature. We find that for high signal-to-noise ratio measurements, photon noise does not account for the full error bars. We discuss how field measurements depend on the specific algorithm adopted for data reduction, and we show that very small instrument flexures, negligible in most of the instrument applications, may be responsible for some spurious field detections in the null profiles. Finally, we find that we are unable to reproduce some results previously published in the literature. Consequently, we do not confirm some important discoveries of magnetic fields obtained with FORS1 and reported in previous publications. Our revised field measurements show that there is no contradiction between the results obtained with the low-resolution spectropolarimeter FORS1 and those obtained with high-resolution spectropolarimeters. FORS1 is an instrument capable of performing reliable magnetic field measurements, provided that the various source of uncertainties are properly taken into account.", "label": 1, "domain": "academic", "token_count": 342, "matched_pair_id": "conditionality_00397", "split": "train"}
{"id": "conditionality_train_pos_0010", "text": "In our SCUBA survey of Perseus, we find that the fraction of protostellar cores increases towards higher masses and the most massive cores are all protostellar. In this paper we consider the possible explanations of this apparent mass dependence in the evolutionary status of these cores, and the implications for protostellar evolution and the mapping of the embedded core mass function (CMF) onto the stellar IMF. We consider the following potential causes: dust temperature; selection effects in the submillimetre and in the mid-infrared observations used for pre/protostellar classification; confusion and multiplicity; transient cores; and varying evolutionary timescales. We develop Core Mass Evolution Diagrams (CMEDs) to investigate how the mass evolution of individual cores maps onto the observed CMF. Two physical mechanisms -- short timescales for the evolution of massive cores, and continuing accumulation of mass onto protostellar cores -- best explain the relative excess of protostars in high mass cores and the rarity of massive starless cores. In addition, confusion both increases the likelihood that a protostar is identified within a core, and increases mass assigned to a core. The observed pre/protostellar mass distributions are consistent with faster evolution and a shorter lifetime for higher-mass prestellar cores. We rule out longer timescales for higher-mass prestellar cores. The differences in the prestellar and protostellar mass distributions imply that the prestellar CMF (and possibly the combined pre+protostellar CMF) should be steeper than the IMF. A steeper prestellar CMF can be reconciled with the observed similarity of the CMF and the IMF in some regions if a second opposing effect is present, such as the fragmentation of massive cores into multiple systems.", "label": 1, "domain": "academic", "token_count": 357, "matched_pair_id": "conditionality_00050", "split": "train"}
{"id": "conditionality_train_pos_0011", "text": "We present long slit spectrophotometry considering the presence of thermal inhomogeneities (t^2) of two HII regions in the Small Magellanic Cloud (SMC): NGC 456 and NGC 460. Physical conditions and chemical abundances were determined for three positions in NGC 456 and one position in NGC 460, first under the assumption of uniform temperature and then allowing for the possibility of thermal inhomogeneities. We determined t^2 values based on three different methods: i) by comparing the temperature derived using oxygen forbidden lines with the temperature derived using helium recombination lines, ii) by comparing the abundances derived from oxygen forbidden lines with those derived from oxygen recombination lines, and iii) by comparing the abundances derived from ultraviolet carbon forbidden lines with those derived from optical carbon recombination lines. The first two methods averaged t^2=0.067+-0.013 for NGC 456 and t^2=0.036+-0.027 for NGC 460. These values of t^2 imply that when gaseous abundances are determined with collisionally excited lines they are underestimated by a factor of nearly 2. From these objects and others in the literature, we find that in order to account for thermal inhomogeneities and dust depletion, the O/H ratio in low metallicity HII regions should be corrected by 0.25-0.45 dex depending on the thermal structure of the nebula, or by 0.35 dex if such information is not available.", "label": 1, "domain": "academic", "token_count": 311, "matched_pair_id": "conditionality_00386", "split": "train"}
{"id": "conditionality_train_pos_0012", "text": "If you look good, you feel good! That is why more men and women are becoming interested in fashion each day. Good fashion means choosing a great style and wearing it well. Continue on into this article for fashion advice you can use yourself. If you are going directly from work to an evening out on the town, take a few makeup basics with you to change your look. Consider darker lipstick and some smoky eye shadow to transform your look. You may also darken your blush a bit, providing some contour for darker time. These three products will ease the transition. Wear cropped pants in a more flattering way by choosing capris, pedal pushers, and bermuda shorts that do not fall at the widest part of your calf. Choose pants that end above the knee or closer to the ankle. You should also avoid flared styles to keep your look streamlined. If you are starting to go gray, try using a vegetable dye. As long as it is just a few strands that are causing anxiety, this product should do the trick. It turns the gray a shade that is a tad lighter than the rest of your hair. Using vegetable dye will make it look as though you have nice, new highlights and will then fade out over about three months. A good fashion tip is to select your clothing for the day based on color. You don't want to step outside with your shirt and shorts clashing because they're complimentary colors. Experiment with different color combinations and see which colors you like and which color combinations you don't like so much. How to apply your makeup depends on where you are going. For example, if you are going for an interview, keep your makeup looking natural and highlight your best feature. For instance, if you have beautiful eyes, wear a soft color that enhances the color of your eyes. If your best feature is your cheekbones, add a little color to the apple of your cheeks. If you have a lighter skin tone and you are looking to dye your hair a darker shade, consider dying it a dark shade of brown instead of opting for jet black. Choosing a brown tone is much more flattering since it will not make you look too washed out. Use up all your beauty products before getting rid of them. For tubed products, use a toothpaste tube squeezer to get every last drop. Try to get the last of the product by turning them upside down and squeezing the last bit out. Sometimes you can cut off the top to get another two", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00591", "split": "train"}
{"id": "conditionality_train_pos_0013", "text": "Share Bethesda Game Studios has spent the last day teasing something Fallout-related, and we now know the project is not a remastered game from the past. Instead, the developer is working on Fallout 76 — though we don’t yet know what that happens to be. Fallout 76 was announced alongside a teaser trailer set to “Take Me Home, Country Roads,” which offers few details on what the game actually is. We see Vault-Tec gear sitting on a bed, and a poster in one room makes it clear that the game takes place in 2076 — a year before the Great War that destroyed much of the world. Vault 76, where these rooms are located, is in pristine condition. A small soccer field is located on the first floor, and a colorful diner — complete with a Vault Boy mascot — is located on the top. “In Vault 76, our future begins,” a voice says as the trailer ends. More information on Fallout 76 will be provided at Bethesda’s E3 showcase on June 10, but it doesn’t appear the game will be a full-scale single-player title like Fallout: New Vegas. According to Kotaku, the game will feature some degree of online connectivity, though it remains to be seen what that actually means. It’s reportedly in development at Bethesda Game Studios’ original Maryland location, as well as in its Austin, Texas, location, which was formerly called BattleCry Studios. Bethesda’s E3 Showcase is shaping up to be one of the most exciting this year, because we don’t know much about what the company is bringing. Rage 2 was recently announced with a gameplay trailer, and Bethesda has confirmed the game will be shown at the event, but the rest of its lineup remains a mystery. With Doom being more than two years old at this point, we expect that a sequel will be shown, and we’re crossing our fingers for any information on the Elder Scrolls series. If you’re new to the Fallout series, you can purchase Fallout 4: Game of the Year Edition right now for less than $40. It comes with the original game and its DLC, and if you want even more, Fallout 3 on Xbox 360 is backward compatible with the Xbox One.", "label": 1, "domain": "news", "token_count": 451, "matched_pair_id": "conditionality_00712", "split": "train"}
{"id": "conditionality_train_pos_0014", "text": "In the context of a strongly coupled Electroweak Symmetry Breaking, composite light scalar singlet and composite triplet of heavy vectors may arise from an unspecified strong dynamics and the interactions among themselves and with the Standard Model gauge bosons and fermions can be described by a $SU(2)_L\\times SU(2)_R/SU(2)_{L+R}$ Effective Chiral Lagrangian. In this framework, the production of the $V^{+}V^{-}$ and $V^{0}V^{0}$ final states at the LHC by gluon fusion mechanism is studied in the region of parameter space consistent with the unitarity constraints in the elastic channel of longitudinal gauge boson scattering and in the inelastic scattering of two longitudinal Standard Model gauge bosons into Standard Model fermions pairs. The expected rates of same-sign di-lepton and tri-lepton events from the decay of the $V^{0}V^{0}$ final state are computed and their corresponding backgrounds are estimated. It is of remarkable relevance that the $V^{0}V^{0}$ final state can only be produced at the LHC via gluon fusion mechanism since this state is absent in the Drell-Yan process. It is also found that the $V^{+}V^{-}$ final state production cross section via gluon fusion mechanism is comparable with the $V^{+}V^{-}$ Drell-Yan production cross section. The comparison of the $V^{0}V^{0}$ and $V^{+}V^{-}$ total cross sections will be crucial for distinguishing the different models since the vector pair production is sensitive to many couplings. This will also be useful to determine if the heavy vectors are only composite vectors or are gauge vectors of a spontaneously broken gauge symmetry.", "label": 1, "domain": "academic", "token_count": 364, "matched_pair_id": "conditionality_00254", "split": "train"}
{"id": "conditionality_train_pos_0015", "text": "shall prepare and publish a report that assesses the susceptibility of critical electric infrastructure to electromagnetic pulse events and geomagnetic disturbances. (b) Contents.--The report under subsection (a) shall-- (1) examine the risk of electromagnetic pulse events and geomagnetic disturbances, using both computer-based simulations and experimental testing; (2) assess the full spectrum of possible events and disturbances and the likelihood that the events and disturbances would cause significant disruption to the transmission and distribution of electric power; and (3) seek to quantify and reduce uncertainties associated with estimates for electromagnetic pulse events and geomagnetic disturbances. (c) FERC Assessment.--Not later than 1 year after publication of the report under subsection (a), the Federal Energy Regulatory Commission, in coordination with the Secretary of Energy and in consultation with electric utilities and the ERO (as defined in section 215(a) of the Federal Power Act (16 U.S.C. 824o(a)), shall submit to Congress an assessment of whether and to what extent infrastructure affecting the transmission of electric power in interstate commerce should be hardened against electromagnetic events and geomagnetic disturbances, including an estimate of the costs and benefits of options to harden the infrastructure. SEC. 7. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go-Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 333, "matched_pair_id": "conditionality_01014", "split": "train"}
{"id": "conditionality_train_pos_0016", "text": "men's circuit, she'd be like 700 in the world\". Shortly after she tweeted that while she \"adores and respects\" him, he should \"keep me out of your statements that are not factually based\". Skip Twitter post by @serenawilliams Dear John, I adore and respect you but please please keep me out of your statements that are not factually based. — Serena Williams (@serenawilliams) June 26, 2017 Report Omnipresence (she's everywhere) Image copyright Getty Images Image caption Serena greets George Clooney at the royal wedding As one of the few celebrities to attend the royal wedding as a close friend of the Duchess of Sussex, Serena seems to be everywhere and know almost everyone. At her own wedding last year, celebrity guests included Beyonce, Jay-Z, Ciara and Kim Kardashian. Serena even appeared in the music video for Beyonce's Sorry in 2016 and recently launched her own clothing line. Super Strength Image copyright Getty Images Image caption Serena with husband Alexis Ohanian When Serena posted a picture on Snapchat revealing a pregnancy bump with the caption \"20 weeks\" (and then swiftly deleted it), many were left in shock. It didn't take long for fans to work out that she'd been eight weeks pregnant at the end of January, which meant she won the Australian Open for the seventh time while expecting a baby. \"If anything, this pregnancy has given me a new power,\" she told Vogue magazine during an interview with just a month to go. After her win at the French Open yesterday, she tweeted a picture of her at the tournament with the caption: \"For all the moms out there who had a tough recovery from pregnancy - here you go.\" \"If I can do it, so can you.\" Follow Newsbeat on Instagram, Facebook and Twitter. Listen to Newsbeat live at 12:45 and 17:45 every weekday on BBC Radio 1 and 1Xtra - if you miss us you can listen back here.", "label": 1, "domain": "news", "token_count": 409, "matched_pair_id": "conditionality_00799", "split": "train"}
{"id": "conditionality_train_pos_0017", "text": "Aims: We present multiwavelength observations of one of the most distant gamma-ray bursts detected so far, GRB 080913. Based on these observations, we consider whether it could be classified as a short-duration GRB and discuss the implications for the progenitor nature and energy extraction mechanisms. Methods: Multiwavelength X-ray, near IR and millimetre observations were made between 20.7 hours and 16.8 days after the event. Results: Whereas a very faint afterglow was seen at the 3.5m CAHA telescope in the nIR, the X-ray afterglow was clearly detected in both Swift and XMM-Newton observations. An upper limit is reported in the mm range. We have modeled the data assuming a collimated $\\theta_0$ $\\gtrsim$ 3$^\\circ$ blast wave with an energy injection at 0.5 days carrying $5\\sim 10^{52}$ erg or approximately 12 times the initial energy of the blast wave. We find that GRB 080913 shares many of the gamma-ray diagnostics with the more recent burst GRB 090423 for being classified as short had they ocurred at low redshift. If the progenitor were a compact binary merger, it is likely composed by a NS and BH. The Blandford-Znajek (BZ) mechanism is the preferred one to extract energy from the central, maximally-rotating BH. Both the magnetic field close to the event horizon (B) and the BH mass ($M_{bh}$) are restricted within a relatively narrow range, such that $(B / 3\\times 10^{16} \\rm{G}) (M_{bh} / 7 M_\\odot) \\sim 1$. Similar constraints on the central BH hold for collapsar-like progenitor systems if the BZ-mechanism works for the system at hand.", "label": 1, "domain": "academic", "token_count": 394, "matched_pair_id": "conditionality_00086", "split": "train"}
{"id": "conditionality_train_pos_0018", "text": "If you’re a woman with a bit of life experience, you already know you’re the boss. You’re more likely to drive health care decisions in your family, control household spending, care for millennials and elders, start a business and initiate a divorce. You have the longevity advantage over men. In other words, you rule. But does the world know it? Older women can sometimes feel like they’re invisible to workplaces and businesses, but they're actually the trailblazers others should be watching, says Joseph F. Coughlin, director of the AgeLab at the Massachusetts Institute of Technology and author of the new book, “The Longevity Economy: Unlocking the World’s Fastest-Growing, Most Misunderstood Market.” As people get older, the future is female, he argues, with women better prepared for life after middle age than their male peers. “One of the greatest under-appreciated sources of innovation and new business may in fact be women over 50 with new ideas, lots of life ahead of them and with the verve to get it done,” Coughlin told TODAY. He explained why older women will rule the world. Why the future is female: Coughlin: Women do more. They have more education than at any time in history. They’re likely to live longer. A woman is the researcher of the house. Women are far more likely to go online not just to do research for themselves, but be the go-to researcher for millennials, who identify their middle-aged mothers as their best friend. She is the caregiver-in-chief. Women are caring for more parents than they had ever planned — their parents as well as their in-laws. Getting to 100 is so common now that we see birthday cards in the drugstore for centenarians. There may be three or four generations under the care of one matriarch. A woman is the chief consumer officer of the house. She’s the one who knows what groceries are bought, what bills are being paid, how that house actually works. The majority of car purchases are directly influenced or done by women. If they’re luxury cars, the numbers go up even more. Home improvement is directed by the woman. Probably most striking is that 80-90 cents on the dollar of every healthcare decision is made by a woman. Because of all these factors, she is likely to be the person who is closest to understanding what the new jobs and the opportunities of living longer, better are", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00752", "split": "train"}
{"id": "conditionality_train_pos_0019", "text": "in ordinary speech, needs therefore to be rethought. Why? Because the current seemingly entertaining nostalgia boom hints at this older type of nostalgia: a search for home, identity and authenticity. And this double-sided nostalgia comes with the digital world and that is why I wish to explore here the idea of digital nostalgia. What is digital nostalgia? Digital nostalgia encompasses several not necessarily separate types of nostalgia expressed, experienced, or made because of, via or within the digital world. In other words, there is nostalgia for the digital, nostalgia expressed via the digital or both (Niemeyer, 2015). The first type means that nostalgia has arrived in a world where the digital is omnipresent, but it does not alter the forms of nostalgia already in existence before the invention of the web. For some this can mean a longing for access to the technologies that connect, especially in places where the infrastructure is not established or access is politically forbidden. For others it might be the other way round, a longing for a society with less social acceleration. Media and communication technologies are, therefore, an essential part of such longings: they can be the reason for the need to escape the apparent acceleration of time and reduction of space; they can trigger nostalgic memories of our past; and they are sometimes the object of our nostalgic feelings. Likewise, media and communication technologies can become a space for “nostalgizing” (Niemeyer 2014; Sedikides el. al., 2015). Here, digital environments become a space for expressing various types of nostalgia. There is of course nostalgia for a geographical place or a time that is no more or will not be for a while. Refugees use technologies and media to cope with the painful present, to connect within their linguistic communities. Media, culture and language even at distance are here what used to be the old medicine for Swiss mercenaries (folk songs, meeting people with the same language), and it works also for those who never left or never had to leave their country: reconnecting to people, music, food, even in the digital world can appease homesickness. And this nostalgia can expand into urban spaces and become a mixed nostalgia of online and offline activities. Nostalgia for the analogue and the digital If your friend publishes a picture on the web with her or his cell phone, adding a filter to make the shot look old even if it was just taken minutes ago, we could ask whether the notion of nostalgia is still adequate here.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00553", "split": "train"}
{"id": "conditionality_train_pos_0020", "text": "We continue our lattice simulations of QCD with 2 flavours of colour-sextet quarks as a model for conformal or walking technicolor. A 2-loop perturbative calculation of the $\\beta$-function which describes the evolution of this theory's running coupling constant predicts that it has a second zero at a finite coupling. This non-trivial zero would be an infrared stable fixed point, in which case the theory with massless quarks would be a conformal field theory. However, if the interaction between quarks and antiquarks becomes strong enough that a chiral condensate forms before this IR fixed point is reached, the theory is QCD-like with spontaneously broken chiral symmetry and confinement. However, the presence of the nearby IR fixed point means that there is a range of couplings for which the running coupling evolves very slowly, i.e. it 'walks'. We are simulating the lattice version of this theory with staggered quarks at finite temperature studying the changes in couplings at the deconfinement and chiral-symmetry restoring transitions as the temporal extent ($N_t$) of the lattice, measured in lattice units, is increased. Our earlier results on lattices with $N_t=4,6$ show both transitions move to weaker couplings as $N_t$ increases consistent with walking behaviour. In this paper we extend these calculations to $N_t=8$. Although both transition again move to weaker couplings the change in the coupling at the chiral transition from $N_t=6$ to $N_t=8$ is appreciably smaller than that from $N_t=4$ to $N_t=6$. This indicates that at $N_t=4,6$ we are seeing strong coupling effects and that we will need results from $N_t > 8$ to determine if the chiral-transition coupling approaches zero as $N_t \\rightarrow \\infty$, as needed for the theory to walk.", "label": 1, "domain": "academic", "token_count": 402, "matched_pair_id": "conditionality_00334", "split": "train"}
{"id": "conditionality_train_pos_0021", "text": "Optimal binary labelings, input distributions, and input alphabets are analyzed for the so-called bit-interleaved coded modulation (BICM) capacity, paying special attention to the low signal-to-noise ratio (SNR) regime. For 8-ary pulse amplitude modulation (PAM) and for 0.75 bit/symbol, the folded binary code results in a higher capacity than the binary reflected gray code (BRGC) and the natural binary code (NBC). The 1 dB gap between the additive white Gaussian noise (AWGN) capacity and the BICM capacity with the BRGC can be almost completely removed if the input symbol distribution is properly selected. First-order asymptotics of the BICM capacity for arbitrary input alphabets and distributions, dimensions, mean, variance, and binary labeling are developed. These asymptotics are used to define first-order optimal (FOO) constellations for BICM, i.e. constellations that make BICM achieve the Shannon limit $-1.59 \\tr{dB}$. It is shown that the $\\Eb/N_0$ required for reliable transmission at asymptotically low rates in BICM can be as high as infinity, that for uniform input distributions and 8-PAM there are only 72 classes of binary labelings with a different first-order asymptotic behavior, and that this number is reduced to only 26 for 8-ary phase shift keying (PSK). A general answer to the question of FOO constellations for BICM is also given: using the Hadamard transform, it is found that for uniform input distributions, a constellation for BICM is FOO if and only if it is a linear projection of a hypercube. A constellation based on PAM or quadrature amplitude modulation input alphabets is FOO if and only if they are labeled by the NBC; if the constellation is based on PSK input alphabets instead, it can never be FOO if the input alphabet has more than four points, regardless of the labeling.", "label": 1, "domain": "academic", "token_count": 425, "matched_pair_id": "conditionality_00194", "split": "train"}
{"id": "conditionality_train_pos_0022", "text": "Following previous theoretical work by Srinivasan (FOCS 2001) and the first author (STACS 2006) and a first experimental evaluation on random instances (ALENEX 2009), we investigate how the recently developed different approaches to generate randomized roundings satisfying disjoint cardinality constraints behave when used in two classical algorithmic problems, namely low-congestion routing in networks and max-coverage problems in hypergraphs. We generally find that all randomized rounding algorithms work well, much better than what is guaranteed by existing theoretical work. The derandomized versions produce again significantly better rounding errors, with running times still negligible compared to the one for solving the corresponding LP. It thus seems worth preferring them over the randomized variants. The data created in these experiments lets us propose and investigate the following new ideas. For the low-congestion routing problems, we suggest to solve a second LP, which yields the same congestion, but aims at producing a solution that is easier to round. Experiments show that this reduces the rounding errors considerably, both in combination with randomized and derandomized rounding. For the max-coverage instances, we generally observe that the greedy heuristics also performs very good. We develop a strengthened method of derandomized rounding, and a simple greedy/rounding hybrid approach using greedy and LP-based rounding elements, and observe that both these improvements yield again better solutions than both earlier approaches on their own. For unit disk max-domination, we also develop a PTAS. Contrary to all other algorithms investigated, it performs not much better in experiments than in theory; thus, unless extremely good solutions are to be obtained with huge computational resources, greedy, LP-based rounding or hybrid approaches are preferable.", "label": 1, "domain": "academic", "token_count": 347, "matched_pair_id": "conditionality_00244", "split": "train"}
{"id": "conditionality_train_pos_0023", "text": "It was recently shown that the power spectrum in redshift space can be written as a sum of cross-power spectra between number weighted velocity moments. We investigate the properties of these power spectra for simulated galaxies and dark matter halos and compare them to the dark matter power spectra, generalizing the concept of the bias. Because all of the quantities are number weighted this approach is well defined even for sparse systems such as massive halos, in contrasts to the previous approaches to RSD where velocity correlations have been explored. We find that the number density weighting leads to a strong scale dependence of the bias terms for momentum density auto-correlation and cross-correlation with density. This trend becomes more significant for the more biased halos and leads to an enhancement of RSD power relative to the linear theory. Fingers-of-god effects, which in this formalism come from the correlations of the higher order moments beyond the momentum density, lead to smoothing of the power spectrum and can reduce this enhancement of power, but are relatively small for halos with no small-scale velocity dispersion. In comparison, for a more realistic galaxy sample with satellites the velocity dispersion generated by satellite motions inside the halos leads to a larger power suppression on small scales, but this depends on the satellite fraction. We investigate several statistics such as the two-dimensional power spectrum, its multipole moments, its powers of mu^2, and configuration space statistics. Overall we find that the nonlinear effects in realistic galaxy samples such as luminous red galaxies affect the redshift space clustering on very large scales: for example, the quadrupole moment is affected by 10% for k<0.1h/mpc, which means that these effects need to be understood if we want to extract cosmological information from the redshift space distortions.", "label": 1, "domain": "academic", "token_count": 358, "matched_pair_id": "conditionality_00469", "split": "train"}
{"id": "conditionality_train_pos_0024", "text": "Though the bulk of the observed optical flux from the discs of intermediate-redshift lensed quasars is formed well outside the region of strong relativistic boosting and light-bending, relativistic effects have important influence on microlensing curves. The reason is in the divergent nature of amplification factors near fold caustics increasingly sensitive to small spatial size details. Higher-order disc images produced by strong light bending around the black hole may affect the amplification curves, making a contribution of up to several percent near maximum amplification. In accordance with theoretical predictions, some of the observed high-amplification events possess fine structure. Here we consider three putative caustic crossing events, one by SBS1520+530 and two events for individual images of the Einstein's cross (QSO J2237+0305). Using relativistic disc models allows to improve the fits, but the required inclinations are high, about 70deg or larger. Such high inclinations apparently contradict the absence of any strong absorption that is likely to arise if a disc is observed edge-on through a dust torus. Still, the high inclinations are required only for the central parts of the disc, that allows the disc itself to be initially tilted by 60-90deg with respect to the black hole and aligned toward the black hole equatorial plane near the last stable orbit radius. For SBS1520+530, an alternative explanation for the observed amplification curve is a superposition of two subsequent fold caustic crossings. While relativistic disc models favour black hole masses ~10^10 solar (several times higher than the virial estimates) or small Eddington ratios, this model is consistent with the observed distribution of galaxies over peculiar velocities only if the black hole mass is about 3 10^8 solar.", "label": 1, "domain": "academic", "token_count": 367, "matched_pair_id": "conditionality_00428", "split": "train"}
{"id": "conditionality_train_pos_0025", "text": "If you want to read something that will move you to tears, read Lauren Stewart’s account of meeting the man who received the heart of her fiancée, dirt-track racing star Bryan Clauson. Clauson died last August 7 from injuries suffered in a crash at the Belleville (Kansas) Midget Nationals USAC midget race. You can read the full story here: http://foxs.pt/2nVPVsA Considered the nation’s top short-track dirt-car driver, Clauson won four USAC national championships and finished 23rd in last year’s Indianapolis 500. He also raced in NASCAR for a time. Clauson, 27, had planned to run 200 races last year, and had run 116 at the time of his fatal crash. Stewart and Clauson were scheduled to get married Feb. 4. Clauson was an organ donor and after his death, his organs helped save the lives of five different individuals, one of whom Stewart calls “Dan the Heart Man” — the man who received a transplant of Clauson’s heart. After Clauson’s death, a organ donation program called The Bryan Clauson Race to Save Lives was established. Clauson’s family and Stewart set up an initial of getting 200 people to sign up in honor of the 200 races Clauson planned to run. To date, more than 6,000 people have registered as donors, helping some genuine to come from tragedy. gallery: Bryan Clauson’s racing career in photos FOX Fantasy Auto Form a Racing Team, Compete for Prizes Play Now!", "label": 1, "domain": "news", "token_count": 321, "matched_pair_id": "conditionality_00729", "split": "train"}
{"id": "conditionality_train_pos_0026", "text": "Very-high-energy (VHE, E \\gtrsim 100 GeV) gamma rays emitted by extragalactic sources, such as blazars, initiate electromagnetic cascades in the intergalactic medium. The cascade photons arrive at the earth with angular and temporal distributions correlated with the extragalactic magnetic field (EGMF). We have developed a new semi-analytical model of the cascade properties which is more accurate than previous analytic approaches and faster than full Monte Carlo simulations. Within its range of applicability, our model can quickly generate cascade spectra for a variety of source emission models, EGMF strengths, and assumptions about the source livetime. In this Letter, we describe the properties of the model and demonstrate its utility by exploring the gamma-ray emission from the blazar RGB J0710+591. In particular, we predict, under various scenarios, the VHE and high-energy (HE, 100 MeV \\lesssim E \\lesssim 300 GeV) fluxes detectable with the VERITAS and Fermi Large Area Telescope (LAT) observatories. We then develop a systematic framework for comparing the predictions to published results, obtaining constraints on the EGMF strength. At a confidence level of 95%, we find the lower limit on the EGMF strength to be ~ 2 \\times 10^{-16} Gauss if no limit is placed on the livetime of the source or ~ 3 \\times 10^{-18} Gauss if the source livetime is limited to the past ~ 3 years during which Fermi observations have taken place.", "label": 1, "domain": "academic", "token_count": 324, "matched_pair_id": "conditionality_00339", "split": "train"}
{"id": "conditionality_train_pos_0027", "text": "cost of the monthly collection of premiums as determined by the report submitted pursuant to subparagraph (D). ``(D) Report.--Not later than six months after the date of the enactment of this Act, the Comptroller General shall submit a report to the Committee on Financial Services of the House of Representatives and the Committee on Banking, Housing, and Urban Affairs of the Senate, that sets forth all of the costs associated with the monthly payment of premiums, including any up- front costs associated with infrastructure development, the impact on all policyholders including those that exercise the option to pay monthly and those that do not, options for minimizing the costs, particularly the costs to policyholders, and the feasibility of adopting practices that serve to minimize costs to policyholders such as automatic payments and electronic payments. ``(E) Annual reports.--On an annual basis, the Administrator shall report to the Committee on Financial Services of the House of Representatives and the Committee on Banking, Housing, and Urban Affairs of the Senate the ongoing costs associated with the monthly payment of premiums.''. (b) Implementation.--Clause (ii) of section 1307(a)(1)(B) of the National Flood Insurance Act of 1968 (42 U.S.C. 4014(a)(1)(B)(ii)) is amended by inserting before ``any administrative expenses'' the following: ``the costs associated with the monthly collection of premiums provided for in section 1308(g) (42 U.S.C. 4015(g)), but only if such costs exceed the operating costs and allowances set forth in clause (i) of this subparagraph, and''.", "label": 1, "domain": "government", "token_count": 322, "matched_pair_id": "conditionality_00836", "split": "train"}
{"id": "conditionality_train_pos_0028", "text": "cost reporting periods beginning on or after October 1, 2001, and before October 1, 2002, 50 percent; and ``(iii) with respect to cost reporting periods beginning on or after October 1, 2002, and before October 1, 2003, 25 percent.''. (b) Limit on Reductions Under Balanced Budget Act.--Section 1886(b) of the Social Security Act (42 U.S.C. 1395ww(b)) is amended by adding at the end the following: ``(8)(A) Notwithstanding the amendments made by sections 4411, 4414, 4415, and 4416 of the Balanced Budget Act of 1997, in the case of a psychiatric facility (as defined in subparagraph (B)(ii)), the amount of payment for the operating costs of inpatient hospital services for cost reporting periods beginning on or after October 1, 1997, and before October 1, 2000, shall not be less than the applicable percentage (as defined in subparagraph (B)(i)) of the amount that would have been paid for such costs if such amendments did not apply. ``(B) For purposes of this paragraph: ``(i) The term `applicable percentage' means-- ``(I) 95 percent for cost reporting periods beginning on or after October 1, 1997, and before October 1, 1998; ``(II) 92.5 percent for cost reporting periods beginning on or after October 1, 1998, and before October 1, 1999; and ``(III) 90 percent for cost reporting periods beginning on or after October 1, 1999, and before October 1, 2000. ``(ii) The term `psychiatric facility' means-- ``(I) a psychiatric hospital; and ``(II) a psychiatric unit described in the matter following clause (v) of subsection (d)(1)(B).''. (c) Effective Date.--The amendments made by subsections (a) and (b) shall apply as if included in the enactment of the Balanced Budget Act of 1997.", "label": 1, "domain": "government", "token_count": 443, "matched_pair_id": "conditionality_00941", "split": "train"}
{"id": "conditionality_train_pos_0029", "text": "We assess the evolutionary status of the intriguing object Walker 90/V590 Mon, which is located about 20 arcminutes northwest of the Cone Nebula near the center of the open cluster NGC 2264. This object, according to its most recent optical spectral type determination (B7), which we confirmed, is at least 3 magnitudes too faint in V for the cluster distance, but it shows the classical signs of a young pre-main sequence object, such as highly variable Halpha emission, Mg II emission, IR excess, UV continuum, and optical variability. We analyzed a collection of archival and original data on Walker 90, covering 45 years including photometry, imaging, and spectroscopic data ranging from ultraviolet to near-infrared wavelengths. According to star formation processes, it is expected that, as this object clears its primordial surroundings, it should become optically brighter, show a weakening of its IR excess and present decreasing line emissions. This behavior is supported by our observations and analysis, but timescales are expected to be longer than the one observed here. Based on photometric data secured in 2007, we find Walker 90 at its brightest recorded optical magnitude. We document an evolution in spectral type over the past five decades (from A2/A3 to currently B7 and as early as B4), along with a decrease in the near-infrared K fluxes. From near-infrared images secured in 2004, Walker 90 appears as a point source placing an upper limit of 0.1 arcsec for its diameter. We conclude that many observational features are explained if W90 is a flared disk system, surrounded by an inclined optically thick accretion disk.", "label": 1, "domain": "academic", "token_count": 345, "matched_pair_id": "conditionality_00057", "split": "train"}
{"id": "conditionality_train_pos_0030", "text": "If future neutrino oscillation experiments show that the neutrino mass spectrum is with normal ordering, m1 < m2 < m3, and the searches for neutrinoless double beta-decay with sensitivity to values of the effective Majorana mass |<m>| > 0.01 eV give negative results, the next frontier in the quest for neutrinoless double beta-decay will correspond to |<m>| ~ 0.001 eV. Assuming that massive neutrinos are Majorana particles and their exchange is the dominant mechanism generating neutrinoless double beta-decay, we analise the conditions under which |<m>|, in the case of three neutrino mixing and neutrino mass spectrum with normal ordering, would satisfy |<m>| > 0.001 eV. We consider the specific cases of i) normal hierarchical neutrino mass spectrum, ii) of relatively small value of the CHOOZ angle theta13 as well as iii) the general case of spectrum with normal ordering, partial hierarchy and a value of theta13 close to the existing upper limit. We study the ranges of the lightest neutrino mass m1 and/or of sin^2 theta13, for which |<m>|> 0.001 eV and discuss the phenomenological implications of such scenarios. We provide also an estimate of |<m>| when the three neutrino masses and the neutrino mixing originate from neutrino mass term of Majorana type for the (left-handed) flavour neutrinos and m1 Ue1^2 + m2 U_e2^2 + m3 Ue3^2 =0, but there does not exist a symmetry which forbids the neutrinoless double beta-decay.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00034", "split": "train"}
{"id": "conditionality_train_pos_0031", "text": "24 hours a day. Every day. This seems beyond NTP rat-like exposure, and perhaps even beyond the long exposures that caused many Connecticut cops to contract testicular and brain cancer from their radar guns. With many radiation safety protocols, you reduce radiation injury by increasing distance, decreasing time exposed, and increasing shielding, whereas the Apple Watch seems to be doing the opposite. In my totally non-expert, non-learned, non-medically-trained, non-scientific, monkey-at-best opinion, it is a near certainty and inevitability that such constant close contact and exposure will increase the odds of a radiation-induced-DNA-bit-flip and cause cancer. [Update: Even the CDC is noting that the “International Agency for Research on Cancer (IARC) has classified RF radiation as a ‘possible human carcinogen.’”] Minimize-RF Personally, I would like to see Apple do something to mitigate against this possibility. Apple should implement a ‘minimize-RF-mode’ for the Apple Watch. It would work like Airplane mode and turn off all the RF transceivers on the watch. This would have the added benefit of saving a ton of battery life. And then, only when you turn your wrist to see the time, would it temporarily turn on the transceivers, get a burst download/upload of what was needed, and then turn off soon thereafter. Such a mode would also block out a lot of interruptions, including emergency texts and notifications. Overall, blocking out a bit more noise, these days, for me at least, is more a feature than it is a bug. I wonder if Apple has thought about this issue, and if the company has done any studies or experiments in this regard. If so, I wonder if Apple would share its findings on the issue. If not, I wonder if it should?", "label": 1, "domain": "news", "token_count": 373, "matched_pair_id": "conditionality_00569", "split": "train"}
{"id": "conditionality_train_pos_0032", "text": "If it is primarily a display, then only the most responsible people should be given cash. But if it is about science, the money must be dispensed more randomly, with the likelihood that some people will waste it on drugs. Advertisement Continue reading the main story At a meeting at City Hall, the SEED project manager Lori Ospina urged that the program be designed to yield valid scientific data. That involves choosing participants on the basis of narrow demographic criteria — perhaps their age, their race, their income. But that approach could expose the city to charges that the program is not inclusive enough. “The trolls I’ve been dealing with on social media and in real life have very racialized views of how this is going to work,” Mr. Tubbs said. “As the first black mayor of this city, it would be very dangerous if the only people to get this were black.” He wants to select participants who are most likely to spend their money wisely, generating stories of working poor people lifted by extra cash. Photo People like Shay Holliman. As a child, her mother was incarcerated. She was raised by her grandmother, along with nine other children. They crammed into apartments full of cockroaches, moving from state to state to stay ahead of the bill collectors. She had a baby. She worked at McDonald’s, but she lacked reliable child care, making the job impossible. She could not pay rent on her $600 a month welfare check. One night, she found herself walking the Stockton streets, her infant daughter in a carrier against her chest, pulling two suitcases full of everything she owned. Taking shelter with a sister consumed by drug addiction, she fell into a vortex of violence. She served 11 years in prison for killing a man who she said had attacked her sister. She emerged with a problem that confronts many people in Stockton: She was eager to work, yet she was vulnerable to criminal background checks that deny jobs to convicted felons. Advertisement Continue reading the main story She worked inside commercial freezers and as a driver. Recently, she took a job at a nonprofit that helps people released from prison set up lives on the outside. “I’m finally living my dream,” she said. In some quarters, the basic income experiment has provoked talk that free money will prompt people to ditch work. “Oh, my,” said Ms. Holliman, who still carries credit card debt of more than $500 and does not earn enough money to regularly", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00603", "split": "train"}
{"id": "conditionality_train_pos_0033", "text": "We shortly discuss the observable consequences of the two hypotheses about the origin of life on Earth and Mars: the Lithopanspermia (Mars to Earth or viceversa) and the origin from a unique progenitor, that for Earth is called LUCA (the LUCA hypothesis). To test the possibility that some lifeforms similar to the terrestrial ones may survive on Mars, we designed and built two simulators of Martian environments where to perform experiments with different bacterial strains: LISA and mini-LISA. Our LISA environmental chambers can reproduce the conditions of many Martian locations near the surface trough changes of temperature, pressure, UV fluence and atmospheric composition. Both simulators are open to collaboration with other laboratories interested in performing experiments on many kind of samples (biological, minerals, electronic) in situations similar to that of the red planet. Inside LISA we have studied the survival of several bacterial strains and endospores. We verified that the UV light is the major responsible of cell death. Neither the low temperature, nor the pressure, nor the desiccation or the atmospheric changes were effective in this sense. We found that some Bacillus strains have a particular capability to survive for some hours in Martian conditions without being screened by dust or other shields. We also simulated the coverage happening on a planet by dust transported by the winds, blowing on the samples a very small quantity of volcanic ash grains or red iron oxide particles. Samples covered by these dust grains have shown a high percentage of survival, indicating that under the surface dust, if life were to be present on Mars in the past, some bacteria colonies or cells could still be present.", "label": 1, "domain": "academic", "token_count": 329, "matched_pair_id": "conditionality_00199", "split": "train"}
{"id": "conditionality_train_pos_0034", "text": "This paper studies multiple-proof quantum Merlin-Arthur (QMA) proof systems in the setting when the completeness-soundness gap is small. Small means that we only lower-bound the gap with an inverse-exponential function of the input length, or with an even smaller function. Using the protocol of Blier and Tapp [arXiv:0709.0738], we show that in this case the proof system has the same expressive power as non-deterministic exponential time (NEXP). Since single-proof QMA proof systems, with the same bound on the gap, have expressive power at most exponential time (EXP), we get a separation between single and multi-prover proof systems in the 'small-gap setting', under the assumption that EXP is not equal to NEXP. This implies, among others, the nonexistence of certain operators called disentanglers (defined by Aaronson et al. [arXiv:0804.0802]), with good approximation parameters. We also show that in this setting the proof system has the same expressive power if we restrict the verifier to be able to perform only Bell-measurements, i.e., using a BellQMA verifier. This is not known to hold in the usual setting, when the gap is bounded by an inverse-polynomial function of the input length. To show this we use the protocol of Chen and Drucker [arXiv:1011.0716]. The only caveat here is that we need at least a linear amount of proofs to achieve the power of NEXP, while in the previous setting two proofs were enough. We also study the case when the proof-lengths are only logarithmic in the input length and observe that in some cases the expressive power decreases. However, we show that it doesn't decrease further if we make the proof lengths to be even shorter.", "label": 1, "domain": "academic", "token_count": 373, "matched_pair_id": "conditionality_00451", "split": "train"}
{"id": "conditionality_train_pos_0035", "text": "We investigate the distribution of the interstellar dust towards six small volumes of the sky in the region of the Gum nebula. New high-quality four-colour uvby and H\\beta\\ Str\\\"omgren photometry obtained for 352 stars in six selected areas of Kapteyn, complemented with data obtained in a previous investigation for two of these areas, were used to estimate the colour excess and distance to these objects. The obtained colour excess versus distance diagrams, complemented with other information, when available, were analysed in order to infer the properties of the interstellar medium permeating the observed volumes. On the basis of the overall standard deviation in the photometric measurements, we estimate that colour excesses and distances are determined with an accuracy of 0.010 mag and better than 30%, respectively, for a sample of 520 stars. A comparison with 37 stars in common with the new Hipparcos catalogue attests to the high quality of the photometric distance determination. The obtained colour excess versus distance diagrams testify to the low density volume towards the observed lines-of-sight. Very few stars out to distances of 1 kpc from the Sun have colour excesses larger than E(b-y) = 0.1 mag. In spite of the low density character of the interstellar medium towards the Puppis-Vela direction, the obtained reddening as a function of the distance indicates that two or more interstellar structures are crossed towards the observed lines-of-sight. One of these structures may be associated with the very low density wall of the Local Cavity, which has a distance of 100-150 pc from the Sun. Another structure might be related to the Gum nebula, and if so, its front face would be located at about 350 pc from the Sun.", "label": 1, "domain": "academic", "token_count": 363, "matched_pair_id": "conditionality_00453", "split": "train"}
{"id": "conditionality_train_pos_0036", "text": "onnell, Sandycove, Co. Dublin, late of Waterford, Limerick and Grangebeg, Fethard, peacefully at home. James Joseph (Jim), predeceased by his wife Joanelle; sadly missed by his children Aoife, Alan and Colm, daughters-in-law Lynn and Deirdre, granddaughters Leah, Saoirse, Caoimhe, Neasa, Doireann and Béibhinn; sister Nora, nieces, nephews, extended family and wide circle of friends. Removal Thursday from his residence to the Church of the Assumption, Dalkey arriving 5pm. Funeral on Friday after 10am Mass to Mount Jerome Crematorium. House private. Enquiries to Quinns of Glasthule, tel: 01 2806756. The death has occurred of Bridget (Ciss) O'Brien (née Cooney), St. Patrick's Road, Ballysimon, peacefully at Athlunkard House Nursing Home in her 101st year. Beloved wife of the late Pakie and dearest mother of Pat, Mary, Brendan, Joseph and John. Deeply regretted by her loving family, brother Tom, daughters-in-law, grandchildren, great-grandchildren, nieces, nephews, relatives and friends. Reposing at Griffin's Funeral Home, John's Gate on Friday from 5pm. Removal at 6.30pm to St. Brigid’s Church. Requiem Mass on Saturday at 10am. Burial afterwards in Mount St. Oliver Cemetery. The death has occurred of William (Billy) Cleary, formerly of Hyde Road Prospect, late of Athlunkard House, Nursing Home, peacefully in the presence of his family at University Hospital Limerick. Beloved son of the late Una and Bobby. Dear brother of Mary, Rita and Bobby. Will be sadly missed by his sisters, brother, brothers-in-law, nieces, nephews, other relatives and friends. Reposing at Cross' Funeral Home, Gerald Griffin Street, Friday from 6pm to 7.30pm followed by Humanist Service. Private Cremation to take place later. No flowers please. Donations, if desired, to a charity of your choice.", "label": 1, "domain": "news", "token_count": 467, "matched_pair_id": "conditionality_00788", "split": "train"}
{"id": "conditionality_train_pos_0037", "text": "Theoretical emission-line ratios involving Fe XI transitions in the 257-407 A wavelength range are derived using fully relativistic calculations of radiative rates and electron impact excitation cross sections. These are subsequently compared with both long wavelength channel Extreme-Ultraviolet Imaging Spectrometer (EIS) spectra from the Hinode satellite (covering 245-291 A), and first-order observations (235-449 A) obtained by the Solar Extreme-ultraviolet Research Telescope and Spectrograph (SERTS). The 266.39, 266.60 and 276.36 A lines of Fe XI are detected in two EIS spectra, confirming earlier identifications of these features, and 276.36 A is found to provide an electron density diagnostic when ratioed against the 257.55 A transition. Agreement between theory and observation is found to be generally good for the SERTS data sets, with discrepancies normally being due to known line blends, while the 257.55 A feature is detected for the first time in SERTS spectra. The most useful Fe XI electron density diagnostic is found to be the 308.54/352.67 intensity ratio, which varies by a factor of 8.4 between N_e = 10^8 and 10^11 cm^-3, while showing little temperature sensitivity. However, the 349.04/352.67 ratio potentially provides a superior diagnostic, as it involves lines which are closer in wavelength, and varies by a factor of 14.7 between N_e = 10^8 and 10^11 cm^-3. Unfortunately, the 349.04 A line is relatively weak, and also blended with the second-order Fe X 174.52 A feature, unless the first-order instrument response is enhanced.", "label": 1, "domain": "academic", "token_count": 361, "matched_pair_id": "conditionality_00193", "split": "train"}
{"id": "conditionality_train_pos_0038", "text": "2)(B). ``(C) For the Railroad Retirement Board, an additional $600,000 for the purposes described in paragraph (3)(B). ``(D) For the Secretary of Veterans Affairs, an additional $625,000 for the Information Systems Technology account''. (b) Extension of Special Credit for Certain Government Retirees.-- (1) In general.--In the case of an eligible individual (as defined in section 2202(b) of the American Recovery and Reinvestment Tax Act of 2009, applied by substituting ``2011'' for ``2009''), with respect to the first taxable year of such individual beginning in 2011, section 2202 of the American Recovery and Reinvestment Tax Act of 2009 shall be applied by substituting ``2011'' for ``2009'' each place it appears. (2) Conforming amendment.--Subsection (c) of section 36A of the Internal Revenue Code of 1986 is amended by inserting ``, and any credit allowed to the taxpayer under section 2(b)(1) of the Emergency Senior Citizens Relief Act of 2010'' after ``the American Recovery and Reinvestment Tax Act of 2009''. (c) Effective Date.-- (1) In general.--Except as otherwise provided in paragraph (2), the amendments made by this section shall take effect on the date of the enactment of this Act. (2) Application of rule relating to deceased individuals.-- The amendment made by subsection (a)(5)(F) shall take effect as if included in section 2201 of the American Recovery and Reinvestment Tax Act of 2009.", "label": 1, "domain": "government", "token_count": 333, "matched_pair_id": "conditionality_00925", "split": "train"}
{"id": "conditionality_train_pos_0039", "text": "In dynamical percolation, the status of every bond is refreshed according to an independent Poisson clock. For graphs which do not percolate at criticality, the dynamical sensitivity of this property was analyzed extensively in the last decade. Here we focus on graphs which percolate at criticality, and investigate the dynamical sensitivity of the infinite cluster. We first give two examples of bounded degree graphs, one which percolates for all times at criticality and one which has exceptional times of nonpercolation. We then make a nearly complete analysis of this question for spherically symmetric trees with spherically symmetric edge probabilities bounded away from 0 and 1. One interesting regime occurs when the expected number of vertices at the nth level that connect to the root at a fixed time is of order n(\\log n)^\\alpha. R. Lyons (1990) showed that at a fixed time, there is an infinite cluster a.s. if and only if \\alpha >1. We prove that the probability that there is an infinite cluster at all times is 1 if \\alpha > 2, while this probability is 0 if 1<\\alpha \\le 2. Within the regime where a.s. there is an infinite cluster at all times, there is yet another type of ``phase transition'' in the behavior of the process: if the expected number of vertices at the nth level connecting to the root at a fixed time is of order n^\\theta with \\theta > 2, then the number of connected components of the set of times in [0,1] at which the root does not percolate is finite a.s., while if 1<\\theta < 2, then the number of such components is infinite with positive probability.", "label": 1, "domain": "academic", "token_count": 362, "matched_pair_id": "conditionality_00017", "split": "train"}
{"id": "conditionality_train_pos_0040", "text": "Exceptions to Nonprofit Athletic Organization Liability Protection.--If the laws of a State limit nonprofit athletic organization liability subject to one or more of the following conditions, such conditions shall not be construed as inconsistent with this section: (1) A State law that requires a nonprofit athletic organization to adhere to risk management procedures, including mandatory training of its employees, agents, or volunteers. (2) A State law that makes the nonprofit athletic organization liable for the acts or omissions of its employees, agents, and volunteers to the same extent as an employer is liable for the acts or omissions of its employees. (3) A State law that makes a limitation of liability inapplicable if the civil action was brought by an officer of a State or local government pursuant to State or local law. (d) Nonapplicability to Certain Claims.--The limitation on liability provided by subsection (a) does not apply to an action or claim arising out of a Federal, State, or local antitrust, labor, environmental, defamation, tortious interference of contract law, or civil rights law, or any other Federal, State, or local law providing protection from discrimination. SEC. 5. PREEMPTION. This Act preempts the laws of any State to the extent that such laws are inconsistent with this Act, except that this Act shall not preempt any State law that provides additional protection from liability relating to the rule-making activities of nonprofit athletic organizations. SEC. 6. EFFECTIVE DATE. (a) In General.--This Act shall take effect on the date of enactment of this Act. (b) Application.--This Act applies to any claim for harm caused by an act or omission of a nonprofit athletic organization that is filed on or after the effective date of this Act but only if the harm that is the subject of the claim or the conduct that caused the harm occurred on or after such effective date.", "label": 1, "domain": "government", "token_count": 381, "matched_pair_id": "conditionality_00877", "split": "train"}
{"id": "conditionality_train_pos_0041", "text": "The new physics required to explain the anomalies recently reported by the D0 and CDF collaborations, namely the top forward-backward asymmetry (FBA), the like-sign dimuon charge asymmetry in semileptonic b decay, and the CDF dijet excess, has to feature an amount of flavor symmetry in order to satisfy the severe constrains arising from flavor violation. In this paper we show that, once baryon number conservation is imposed, color & weak triplet scalars with hypercharge $Y=1/3$ can feature the required flavor structure as a consequence of standard model gauge invariance. The color & weak triplet model can simultaneously explain the top FBA and the dimuon charge asymmetry or the dimuon charge asymmetry and the CDF dijet excess. However, the CDF dijet excess appears to be incompatible with the top FBA in the minimal framework. Our model for the dimuon asymmetry predicts the observed pattern $h_d\\ll h_s$ in the region of parameter space required to explain the top FBA, whereas our model for the CDF dijet anomaly is characterized by the absence of beyond the SM b-quark jets in the excess region. Compatibility of the color & weak triplet with the electroweak constraints is also discussed. We show that a Higgs boson mass exceeding the LEP bound is typically favored in this scenario, and that both Higgs production and decay can be significantly altered by the triplet. The most promising collider signature is found if the splitting among the components of the triplet is of weak scale magnitude.", "label": 1, "domain": "academic", "token_count": 325, "matched_pair_id": "conditionality_00354", "split": "train"}
{"id": "conditionality_train_pos_0042", "text": "Project Fi may have many fans—after all, it gives you service across three US carriers plus international roaming at an affordable pay-as-you-go rate—but one thing subscribers don't enjoy is the lack of selection when it comes to phones. Fi hears that, and to make up for it, it's adding the Moto G6, LG G7 ThinQ, and LG V35 ThinQ to its lineup. The affordable G6 is even available to pre-order today. It’s official—we’re welcoming the moto g6, LG G7 ThinQ, and LG V35 ThinQ to Project Fi.https://t.co/OKTVfzjeGM pic.twitter.com/EdyPAUw3MV — Project Fi (@projectfi) May 30, 2018 The two LG phones won't be arriving at Fi until \"next month,\" though you can sign up to be notified for each at the listings on Project Fi's site. For more information on details like specs, you can check out our prior coverage for the Moto G6, LG G7 ThinQ, and LG V35 ThinQ. The V35 was only just announced today, but if you're familiar with past LG V30 phones, you'll get the gist. Pricing for each covers the low and high-end, with the G6 priced at $199 on Project Fi, while the G7 is $749, and the V35 is a whopping $899. Fi might be bringing more choices, but the price-points may leave something to be desired. New subscribers can also take advantage of occasional discounts for Fi (like our $20 referral credit), so if the new pricing stuns you a bit, odds are discounts will be coming.", "label": 1, "domain": "news", "token_count": 347, "matched_pair_id": "conditionality_00768", "split": "train"}
{"id": "conditionality_train_pos_0043", "text": "Revenue Code of 1986 is amended-- (1) by inserting ``5-year carryback of certain losses.--'' after ``(H)'', and (2) by striking ``or 2002'' and inserting ``, 2002, 2007, or 2008''. (b) Temporary Suspension of 90 Percent Limit on Certain NOL Carrybacks.--Subclause (I) of section 56(d)(1)(A)(ii) of the Internal Revenue Code of 1986 is amended-- (1) by striking ``or 2002'' and inserting ``, 2002, 2007, or 2008'', and (2) by striking ``and 2002'' and inserting ``, 2002, 2007, or 2008''. (c) Effective Dates.-- (1) In general.--Except as provided in paragraph (2), the amendments made by this section shall apply to net operating losses for taxable years ending after December 31, 2006. (2) Election.--In the case of a net operating loss for a taxable year ending during 2007 or 2008-- (A) any election made under section 172(b)(3) of the Internal Revenue Code of 1986 may (notwithstanding such section) be revoked before November 1, 2008, and (B) any election made under section 172(j) of such Code shall (notwithstanding such section) be treated as timely made if made before November 1, 2008.", "label": 1, "domain": "government", "token_count": 313, "matched_pair_id": "conditionality_00960", "split": "train"}
{"id": "conditionality_train_pos_0044", "text": "the date of the enactment of this Act by any person if the aggregate amount of fuel alcohol held by such person on such date does not exceed 2,000 gallons. The preceding sentence shall apply only if such person submits to the Secretary (at the time and in the manner required by the Secretary) such information as the Secretary shall require for purposes of this paragraph. (B) Exempt fuel.--For purposes of subparagraph (A), there shall not be taken into account fuel held by any person which is exempt from the tax imposed by paragraph (1) by reason of paragraph (4) or (5). (C) Controlled groups.--For purposes of this paragraph-- (i) Corporations.-- (I) In general.--All persons treated as a controlled group of corporations shall be treated as 1 person. (II) Controlled group of corporations.--The term ``controlled group of corporations'' has the meaning given to such term by subsection (a) of section 1563 of such Code; except that for such purposes the phrase ``more than 50 percent'' shall be substituted for the phrase ``at least 80 percent'' each place it appears in such subsection. (ii) Nonincorporated persons under common control.--Under regulations prescribed by the Secretary, principles similar to the principles of clause (i) shall apply to a group of persons under common control where 1 or more of such persons is not a corporation. (7) Other laws applicable.--All provisions of law, including penalties, applicable with respect to the taxes imposed by section 4081 of such Code shall, insofar as applicable and not inconsistent with the provisions of this subsection, apply with respect to the floor stock taxes imposed by paragraph (1) to the same extent as if such taxes were imposed by such section 4081.", "label": 1, "domain": "government", "token_count": 364, "matched_pair_id": "conditionality_00936", "split": "train"}
{"id": "conditionality_train_pos_0045", "text": "TAIPEI (Taiwan News) -- Limited numbers of individual passengers will be given free rides on the Taoyuan mass rapid transit (MRT) line beginning tomorrow, according to Taoyuan Mass Transit Corp. As part of the second phase of the month-long free trial run, from Feb. 16 - Mar. 1 individual passengers will be allowed to travel for free between 8 a.m. and 4 p.m., however they must first obtain a queue number, which will be available at 7:40 a.m., 9:40 a.m., 11:40 a.m., and 1:40 p.m. each day. Only 20,000 queue numbers will be provided per day, though children below the age of 6 can ride without a queue number. During this phase, passengers will have access to all 21 stations, including Taipei Main Station and the airport stations. China Airlines and EVA Airways will have check-in counters at the Taipei Main Station, as well as their respective subsidiaries Mandarin Airlines and UNI Airways. As long as they arrive at the Taipei Main Station check in counter three hours in advance, passengers can check their luggage and receive seat assignments and boarding passes. Taoyuan Mayor Cheng Wen-tsan (鄭文燦) told the media on Tuesday that the Airport MRT will officially open to all passengers on Mar. 2 with tickets available at a 50 percent discount during the first month of operation. The trains will run from 6 a.m. to 11 p.m. every day. After the first month of normal operations, Cheng said passengers will receive a 40 percent discount and employees of companies of up to 300 people will receive a 50 percent discount on fares if they purchase a 3-month pass.", "label": 1, "domain": "news", "token_count": 365, "matched_pair_id": "conditionality_00507", "split": "train"}
{"id": "conditionality_train_pos_0046", "text": "We present optical photometry and spectroscopy of the peculiar Type IIn/Ibn supernova SN2011hw. Its light curve exhibits a slower decline rate than normal SNeIbc, with a peak absolute magnitude of -19.5 (unfiltered) and a secondary peak of -18.3 mag (R). Spectra of SN2011hw are unusual compared to normal SN types, most closely resembling the spectra of SNeIbn. We center our analysis on comparing SN 2011hw to the well-studied TypeIbn SN2006jc. While the two SNe have many important similarities, the differences are quite telling: compared to SN2006jc, SN2011hw has weaker HeI and CaII lines and relatively stronger H lines, its light curve has a higher luminosity and slower decline rate, and emission lines associated with the progenitor's CSM are narrower. One can reproduce the unusual continuum shape of SN2011hw with equal contributions of a 6000K blackbody and a spectrum of SN2006jc. We attribute this emission component and many other differences between the two SNe to extra opacity from a small amount of additional H in SN2011hw, analogous to the small H mass that makes SNeIIb differ from SNeIb. Slower speeds in the CSM and elevated H content suggest a connection between the progenitor of SN2011hw and the class of Ofpe/WN9 stars, which have been associated with LBVs in their hot quiescent phases between outbursts, and are H-poor - but not H-free like classical Wolf-Rayet (WR) stars. We conclude that the similarities and differences between SN2011hw and SN2006jc can be largely understood if their progenitors exploded at different points in the transitional evolution from an LBV to a WR star.", "label": 1, "domain": "academic", "token_count": 380, "matched_pair_id": "conditionality_00436", "split": "train"}
{"id": "conditionality_train_pos_0047", "text": "able for all subsequent taxable years. ``(C) Ownership requirement.--The ownership requirement of this subparagraph is met with respect to any foreign corporation if the domestic corporation owns within the meaning of section 958(a), or is considered as owning by applying the rules of ownership of section 958(b), 80 percent or more of the total combined voting power of all classes of stock entitled to vote of such foreign corporation.''. (b) Effective Dates.-- (1) In general.--The amendments made by this section shall apply with respect to taxable years beginning after December 31, 1986. (2) Time for filing election when return filed.--For any taxable year beginning after December 31, 1986, with respect to which a domestic corporation has filed a return of income tax imposed under chapter 1 of the Internal Revenue Code of 1986 prior to the date of enactment of this Act, a domestic corporation may make the election allowed under section 902(c)(7) of the Internal Revenue Code of 1986 within 120 days of the date of enactment of this Act, but only if for such taxable year any one or more of the following conditions exists: (A) The period of limitations for assessment and collection, as defined in section 6501(a) of such Code, has not expired. (B) If the limitations period described in paragraph (1) has been extended by agreement between the Secretary and the taxpayer pursuant to section 6501(c)(4) of such Code, such extended period has not expired. (C) The period of limitations for filing a claim for refund pursuant to section 6511(a) of such Code has not expired. (D) The proper amount of tax due for the taxable year is the subject of a petition to the Tax Court pursuant to section 6213 of such Code and a decision of the Tax Court on the merits of the petition, if any, has not yet become final. (E) The proper amount of tax due for the taxable year is the subject of a civil action for refund before a Federal district pursuant to section 1346(a) of title 28, United States Code, or before the Federal Court of Claims pursuant to section 1491(a)(1) of such title, and a decision on the merits of the refund action, if any, has not yet become final.", "label": 1, "domain": "government", "token_count": 477, "matched_pair_id": "conditionality_01017", "split": "train"}
{"id": "conditionality_train_pos_0048", "text": "A growing sample of white dwarfs (WDs) with metal-enriched atmospheres are accompanied by excess infrared emission, indicating that they are encircled by a compact dusty disk of solid debris. Such `WD debris disks' are thought to originate from the tidal disruption of asteroids or other minor bodies, but the precise mechanism(s) responsible for transporting matter to the WD surface remains unclear, especially in those systems with the highest inferred metal accretion rates dM_Z/dt ~ 1e8-1e10 g/s. Here we present global time-dependent calculations of the coupled evolution of the gaseous and solid components of WD debris disks. Solids transported inwards (initially due to PR drag) sublimate at tens of WD radii, producing a source of gas that accretes onto the WD surface and viscously spreads outwards in radius, where it overlaps with the solid disk. If the aerodynamic coupling between the solids and gaseous disks is sufficiently strong (and/or the gas viscosity sufficiently weak), then gas builds up near the sublimation radius faster than it can viscously spread away. Since the rate of drag-induced solid accretion increases with gas density, this results in a runaway accretion process, during which the WD accretion rate reaches values orders of magnitude higher than can be achieved by PR drag alone. We explore the evolution of WD debris disks across a wide range of physical conditions and calculate the predicted distribution of observed accretion rates dM_Z/dt, finding reasonable agreement with the current sample. Although the conditions necessary for runaway accretion are at best marginally satisfied given the minimal level of aerodynamic drag between circular gaseous and solid disks, the presence of other stronger forms of solid-gas coupling---such as would result if the gaseous disk is only mildly eccentric---substantially increase the likelihood of runaway accretion.", "label": 1, "domain": "academic", "token_count": 389, "matched_pair_id": "conditionality_00416", "split": "train"}
{"id": "conditionality_train_pos_0049", "text": "if American Media had collaborated with the Saudis on the magazine or been paid by them. Saud Kabli, the Saudi Embassy’s communications director, said the embassy had “no role in the production of the magazine.” “We don’t have a problem with the magazine, but we just don’t think it is effective,” Kabli said. Metadata embedded in the PDF file, obtained by the AP from two different individuals, show it was produced by an AMI production employee at 8:41 p.m. on Feb. 19. Shortly thereafter, it started circulating internally among Saudi officials, including the embassy’s military office, according to individuals familiar with the situation. It was also passed to Nail al-Jubeir, the former embassy spokesman and brother of Saudi Foreign Minister Adel al-Jubeir, recently named Saudi ambassador to Ireland, the individuals said. By the next day — Feb. 20 — Saudi officials had started forwarding it to Washington foreign policy contacts, giving them an early look, said the individuals, who weren’t authorized to discuss the situation and requested anonymity. A month later, on March 19, Prince Mohammed arrived in the US, with the magazine serving as his literary red carpet. “Meet the next king,” the cover exclaimed, describing the crown prince as “our closest Middle East ally destroying terrorism” and the visionary behind a “city of the future” which “will be operated by robots.” The magazine draws heavily from newswire photos and stock images — many with no connection to Saudi Arabia, according to Tineye, a reverse-image search tool. Among the supposed Saudi Arabian highlights pictured are sand-dune surfing in Namibia, a massive indoor greenhouse in the Netherlands and wildlife pictures taken in Zambia and Israel. “There are lots of things that warrant answers,” political law attorney Josh Rosenstein said about the pro-Saudi magazine. As Saudi Arabia starts to open up to Western entertainment, American Media has sought to expand its media empire into the kingdom — the kind of lucrative opportunity that often comes with the blessing of the Saudi royal court. Last summer, Pecker dined at the White House with Trump and a French businessman with close business ties to the Saudis, and later traveled to Riyadh to pitch Saudi investors on helping AMI acquire Time magazine, The New York Times reported. AMI denied making such an ask. Trump’s son-in-law and senior aide, Jared Kushner, has also tried to enlist Prince Mohammed’s help with his ambitious Mideast peace initiative. Kushner", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00828", "split": "train"}
{"id": "conditionality_train_pos_0050", "text": "We have developed the Smoothed Bandpass Calibration (SBC) method and the best suitable scan pattern to optimize radio spectroscopic observations. Adequate spectral smoothing is applied to the spectrum toward OFF-source blank sky adjacent to a target source direction for the purpose of bandpass correction. Because the smoothing process reduces noise, the integration time for OFF-source scans can be reduced keeping the signal-to-noise ratio. Since the smoothing is not applied to ON-source scans, the spectral resolution for line features is kept. An optimal smoothing window is determined by bandpass flatness evaluated by Spectral Allan Variance (SAV). An efficient scan pattern is designed to the OFF-source scans within the bandpass stability timescale estimated by Time-based Allan Variance (TAV). We have tested the SBC using the digital spectrometer, VESPA, on the VERA Iriki station. For the targeted noise level of 5e-4 as a ratio to the system noise, the optimal smoothing window was 32 - 60 ch in the whole bandwidth of 1024 ch, and the optimal scan pattern was designed as a sequence of 70-s ON + 10-s OFF scan pairs. The noise level with the SBC was reduced by a factor of 1.74 compared with the conventional method. The total telescope time to achieve the goal with the SBC was 400 s, which was 1/3 of 1200 s required by the conventional way. Improvement in telescope time efficiency with the SBC was calculated as 3x, 2x and 1.3x for single-beam, dual-beam, and on-the-fly (OTF) scans, respectively. The SBC works to optimize scan patterns for observations from now, and also works to improve signal-to-noise ratios of archival data if ON- and OFF-source spectra are individually recorded, though the efficiency depends on the spectral stability of the receiving system.", "label": 1, "domain": "academic", "token_count": 392, "matched_pair_id": "conditionality_00452", "split": "train"}
{"id": "conditionality_train_pos_0051", "text": ".--In this section: ``(1) The term `covered claims' means claims for disability compensation submitted to the Secretary based on a covered mental health condition alleged to have been incurred or aggravated by military sexual trauma. ``(2) The terms `covered mental health condition' and `military sexual trauma' have the meanings given such terms in section 1154(c)(3) of this title.''. (2) Clerical amendment.--The table of sections at the beginning of such chapter, as amended by subsection (b), is further amended by adding at the end the following new item: ``1165. Annual reports on claims for disabilities incurred or aggravated by military sexual trauma.''. (d) Effective Date.--Subsection (c) of section 1154 of title 38, United States Code, as added by subsection (a), shall apply with respect to any claim for disability compensation under laws administered by the Secretary of Veterans Affairs for which no final decision has been made before the date of the enactment of this Act. SEC. 4. INFORMATION FOR MEMBERS OF THE ARMED FORCES REGARDING AVAILABILITY OF SERVICES AT VET CENTERS. (a) In General.--The Secretary of Defense shall inform members of the Armed Forces, using mechanisms available to the Secretary, of the eligibility of such members for services at Vet Centers. (b) Information From Sexual Assault Response Coordinators.--The Secretary shall ensure that Sexual Assault Response Coordinators of the Department of Defense advise members of the Armed Forces who report instances of military sexual trauma regarding the eligibility of such members for services at Vet Centers. (c) Definitions.--In this section: (1) Military sexual trauma.--The term ``military sexual trauma'' means psychological trauma described in section 1720D(a)(1) of title 38, United States Code. (2) Vet center.--The term ``Vet Center'' has the meaning given that term in section 1712A(h) of such title.", "label": 1, "domain": "government", "token_count": 402, "matched_pair_id": "conditionality_00875", "split": "train"}
{"id": "conditionality_train_pos_0052", "text": "If Jan. 1 is truly a day for optimism, then count the Rangers in. It hasn’t been an easy road for the Blueshirts, now almost at the halfway mark of this season following their sweep of the two-game New Year’s Eve trip that went through the bowels of the standings against Arizona and Colorado. To look back on the first 39 games with a record of 26-12-1, good enough for third place in the behemoth of the Metropolitan Division, is to see these Rangers are in the process of weathering the storm of injuries rather well. The big hope rests with the fact it won’t be too long before they will be put back together. There are three more games before the Rangers get their first taste of the newly mandated five-day “bye week,” starting Sunday. There is a chance Rick Nash could return from his nagging groin injury sometime before then, with a game at home against the Sabres on Tuesday, followed by road games against the Flyers on Wednesday and the Blue Jackets on Saturday. If John Tortorella’s Columbus club can keep winning, the game Saturday would be to break the all-time win streak record of 17 — and boy, wouldn’t that be a scene? Whether Nash plays or not, by the Jan. 13 end of the break the Rangers will have played six games in 20 days. Soon after they return, both Mika Zibanejad and Pavel Buchnevich will be on constant watch for their availability coming back from a broken leg and from back and core problems, respectively. The most recent time the Rangers dressed a lineup with Nash, Zibanejad and Buchnevich was Nov. 12, after which Buchnevich went back on injured reserve, having now missed 24 straight games and 29 of the past 37. Zibanejad then broke his leg in a game against the Panthers on Nov. 20, and has now missed 20 straight. Nash first hurt his groin on the soft ice of Barclays Center on Dec. 6, and has now missed nine of 11 games because of it. During the team’s terrific 13-4-0 start, it was buoyed by the idea of its offensive depth, and how it was getting production from all four lines. But that depth has been tested, and missing three of the team’s top-six forwards is not an easy thing to overcome. But the defense has tightened up, the goalt", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00807", "split": "train"}
{"id": "conditionality_train_pos_0053", "text": "If you have yet to make it to a game, you might want to fit one in your schedule. LOUISVILLE, KY (WAVE) – In an effort to be more transparent, Louisville City FC has released a list of its owners. The list, released Friday, includes the University of Louisville's new Athletic Director, one of UofL's Trustees Sandra Frazier, former U.S. Ambassador Matthew Barzun and restauranteur Vincenzo Gabriele. In the letter sent out on Friday, Louisville City FC's Executive Vice President, Brad Estes said they are proud to have a \"fine group of owners, as they are pillars in our community.\" MORE FROM WAVE3.COM + Letter: Postel accuses Pitino of 'pattern ... of inappropriate behavior' + 2 UofL basketball coaches placed on administrative leave + Man charged for stabbing near Churchill Downs The letter went on to explain that the owners' investments, in many cases, are held within LLC or other investment vehicles. \"We believe the goal is to seek to understand the individuals behind the LLCs, which is why we are releasing individual names and not legal entities,\" Estes said. The full list of Louisville City FC Owners is as follows: Andrew Beck Barrett Nichols Breck Jones Bruce Aitken Carolyn Mountjoy Chester Musselman Christian Olsen Dan Okruhlica David & Carol Rickert Gabriel Cardenas Garett Jackson Garrett Bates Garvin Brown George Duthie Gill Holland Hassan Miyanji Henry Sanders Jacob Brown Jim Shircliffe Jimmy Kirchdorfer John Hollenbach John Kallis John Neace John Oakley John Pieper Jose Donis Justin Akin Ken Stilger Lee Groza Mark Kirchdorfer Matthew Barzun Mike Mountjoy Pradeep Padmanabhan Rory McMahan Sandra Frazier Scott Ferguson Scott Kronick Stuart Ferguson Terry Stilger Thomas Forsha Tim Mulloy Thomas Mueller Tysen Smith Vince Tyra Vincenzo Gabriele Will Sanders Copyright 2017 WAVE 3 News. All rights reserved.", "label": 1, "domain": "news", "token_count": 418, "matched_pair_id": "conditionality_00697", "split": "train"}
{"id": "conditionality_train_pos_0054", "text": "[abridged] We analyze a sample of 9 massive clusters at 0.4<z<0.6 observed with MegaCam in 4 photometric bands (g,r,i,z) from the core to a radius of 5 Mpc (~4000 galaxies). Galaxy cluster candidates are selected using photometric redshifts computed with HyperZ. Morphologies are estimated with galSVM in two broad morphological types (early-type and late-type). We examine the morphological composition of the red-sequence and the blue-cloud and study the relations between galaxies and their environment through the morphology-density relations (T-Sigma) and the morphology-radius relation (T-R) in a mass limited sample (log(M/Msol)>9.5). We find that the red sequence is already in place at z~0.5 and it is mainly composed of very massive (log(M/Msol)>11.3) early-type galaxies. These massive galaxies seem to be already formed when they enter the cluster, probably in infalling groups, since the fraction remains constant with the cluster radius. Their presence in the cluster center could be explained by a segregation effect reflecting an early assembly history. Any evolution that takes place in the galaxy cluster population occurs therefore at lower masses (10.3<log(M/Msol)<11.3). For these galaxies, the evolution, is mainly driven by galaxy-galaxy interactions in the outskirts as revealed by the T-Sigma relation. Finally, the majority of less massive galaxies (9.5<log(M/Msol)<10.3) are late-type galaxies at all locations, suggesting that they have not started the morphological transformation yet even if this low mass bin might be affected by incompleteness.", "label": 1, "domain": "academic", "token_count": 349, "matched_pair_id": "conditionality_00155", "split": "train"}
{"id": "conditionality_train_pos_0055", "text": "In our previous paper [12] (Rev. Math. Phys. 16, 383-420 (2004)), a general framework was outlined to treat the approximate solutions of semilinear evolution equations; more precisely, a scheme was presented to infer from an approximate solution the existence (local or global in time) of an exact solution, and to estimate their distance. In the first half of the present work the abstract framework of \\cite{uno} is extended, so as to be applicable to evolutionary PDEs whose nonlinearities contain derivatives in the space variables. In the second half of the paper this extended framework is applied to theincompressible Navier-Stokes equations, on a torus T^d of any dimension. In this way a number of results are obtained in the setting of the Sobolev spaces H^n(T^d), choosing the approximate solutions in a number of different ways. With the simplest choices we recover local existence of the exact solution for arbitrary data and external forces, as well as global existence for small data and forces. With the supplementary assumption of exponential decay in time for the forces, the same decay law is derived for the exact solution with small (zero mean) data and forces. The interval of existence for arbitrary data, the upper bounds on data and forces for global existence, and all estimates on the exponential decay of the exact solution are derived in a fully quantitative way (i.e., giving the values of all the necessary constants; this makes a difference with most of the previous literature). Nextly, the Galerkin approximate solutions are considered and precise, still quantitative estimates are derived for their H^n distance from the exact solution; these are global in time for small data and forces (with exponential time decay of the above distance, if the forces decay similarly).", "label": 1, "domain": "academic", "token_count": 362, "matched_pair_id": "conditionality_00019", "split": "train"}
{"id": "conditionality_train_pos_0056", "text": "to paragraph (3), the term `applicable percentage' means-- ``(i) with respect to covered OPD services furnished during the first full calendar year (and any portion of the immediately preceding calendar year) for which the prospective payment system established under section 1833(t) of such Act is in effect, 95 percent, ``(ii) with respect to the second full calendar year for which such system is in effect, 90 percent, and ``(iii) with respect to the third full calendar year for which such system is in effect, 85 percent. ``(B) Covered opd services.--The term `covered OPD services' has the meaning given to such term in section 1833(t)(1)(B) of such Act. ``(3) Application to certain hospitals.--In the case of hospitals described in section 1833(t)(8) of such Act, the `applicable percentage' for a calendar year (or portion thereof) shall be the same applicable percentage that applies to covered OPD services furnished by hospitals that are not described in such section during such calendar year (or portion thereof). ``(4) Rule of construction.--Nothing in this subsection shall be construed as affecting the amount of cost sharing paid by individuals enrolled under part B of title XVIII of the Social Security Act for covered OPD services.''. (2) Conforming amendment.--Section 1833(t)(1)(A) of the Social Security Act (42 U.S.C. 1395l(t)(1)(A)) is amended by inserting ``except as provided in section 4523(e) of the Balanced Budget Act of 1997,'' after ``1999,''. (d) Effective Date.-- (1) Special adjustments for certain visits.--The amendments made by subsection (a) shall apply to items and services furnished on or after January 1, 2000. (2) Market basket; temporary limits on reductions.--The amendments made by subsections (b) and (c) are effective as if included in the enactment of the Balanced Budget Act of 1997.", "label": 1, "domain": "government", "token_count": 422, "matched_pair_id": "conditionality_00938", "split": "train"}
{"id": "conditionality_train_pos_0057", "text": "We have compiled a sample of 16 orbits for very low-mass stellar (<0.1 Msun) and brown dwarf binaries, enabling the first comprehensive study of the eccentricity distribution for such objects. We find that very low-mass binaries span a broad range of eccentricities (0.03<e<0.83), with a median eccentricity of 0.34. We examine potential observational biases in this sample, and for visual binaries we show through Monte Carlo simulations that appropriate selection criteria result in all eccentricities being equally represented (<5% difference between input and output e distributions). The orbits of this sample of very low-mass binaries show some significant differences from their solar-type counterparts. They lack a correlation between orbital period and eccentricity and display a much higher fraction of near-circular orbits (e<0.1) than solar-type stars, which together suggest a different formation mechanism or dynamical history for these two populations. Very low-mass binaries also do not follow the e^2 distribution of Ambartsumian (1937), which would be expected if their orbits were distributed in phase space according to a function of energy alone (e.g., the Boltzmann distribution). We find that numerical simulations of very low-mass star formation do not completely reproduce the observed properties of our binary sample. The cluster formation model of Bate (2009) agrees very well with the overall e distribution, but lack any high-e (>0.6) binaries at orbital periods comparable to our sample. In contrast, the circumstellar disk fragmentation model of Stamatellos & Whitworth (2009) predicts only high-e binaries and thus is highly inconsistent with our sample. These discrepancies could be explained if multiple formation processes have produced the field population.", "label": 1, "domain": "academic", "token_count": 355, "matched_pair_id": "conditionality_00319", "split": "train"}
{"id": "conditionality_train_pos_0058", "text": "OTTAWA — A man has been charged with 10 counts of first-degree murder and 13 counts of attempted murder after a van struck pedestrians along one of Toronto's busiest thoroughfares, conjuring memories of recent similar attacks, including in France, Germany and Spain. Monday's events sent the city reeling, sowing confusion and fear. So why have no terrorism charges been laid in the case? Here's a look at the Canadian legal regime on terrorism: DEFINITION: The Criminal Code defines terrorism as an act carried out \"for a political, religious or ideological purpose, objective or cause\" intended to intimidate the public by causing death or serious bodily harm, endangering health and safety, or interfering with an essential service. OFFENCES: The code includes offences that target financing and participation in a terrorist group, as well as facilitating and instructing others to commit terrorist acts. WHAT THE EXPERTS SAY: When Criminal Code offences for terrorism were introduced as a part of the Anti-Terrorism Act in 2001, Parliament decided that one of the things that should help distinguish such offences from other forms of violent crime was the specific motivational definition, said Wesley Wark of the University of Ottawa's graduate school of public and international affairs. \"Some violent crimes may have the same effect as terrorism but if the motivational element cannot be demonstrated then they are not considered, legally, acts of terrorism, even if they terrorize,\" Wark said. It can also be difficult for police and legal counsel to establish the motivation in a way that meets the evidentiary standards of a court, he added. The terrorism offences in Canadian law \"do not work well\" with so-called lone-wolf suspects who act on their own, given the code's emphasis on participating in or contributing to the activities of a terrorist group, said Kent Roach, a law professor at the University of Toronto who has written extensively about national security. OTHER CASES: There is expert consensus that whenever it's appropriate to lay terrorism charges, that should happen, even if it makes no ultimate difference to the criminal sanction, such as the length of sentence imposed, Wark said.", "label": 1, "domain": "news", "token_count": 432, "matched_pair_id": "conditionality_00598", "split": "train"}
{"id": "conditionality_train_pos_0059", "text": "Amid multiple investigations and controversies over the cost of travel by Trump administration officials, two senators are asking the Office of Management and Budget to provide more detail about the administration's policies on travel spending. Several members of Trump's cabinet have been under scrutiny for the cost of their travel and other expensive purchases. The president asked former Health and Human Services Secretary Tom Price to resign last September after reports that his travel on private planes cost more than $1 million of taxpayer money. Sen. Gary Peters, D-Michigan, the ranking member of theFederal Spending Oversight and Emergency Management subcommittee, and Sen. Joni Ernst, R-Iowa, wrote to Office of Management and Budget Director Mick Mulvaney on Monday asking him to explain how the Trump administration is enforcing rules on the cost of government travel and whether OMB has reviewed any other relevant guidance or rules. \"It is our duty to provide oversight and ensure that taxpayer money is spent responsibly, without waste, fraud, or abuse,\" the senators wrote in the letter, which was reviewed by ABC News. \"As you have said yourself about past issues with Administration travel, “just because something is legal doesn’t make it right.” We owe it to the American people to ensure with the utmost vigilance that tax dollars are being spent appropriately.\" The senators are also asking Mulvaney for documents on all travel approved by the White House Chief of Staff related to travel on government-owned or charter planes. OMB said in a memo issued after Price resigned that some travel would need to be approved by the chief of staff and that the chief of staff would provide further guidance on the use of government and private planes. There are multiple investigations pending from congressional committees and agency watchdogs seeking more information about whether officials' travel spending followed all the relevant rules. The inspectors general at the Environmental Protection Agency and Department of Interior have ongoing investigations into travel spending and the IG from the Department of Veterans Affairs already published a report into Secretary David Shulkin's spending on a trip to Europe. Federal law says that government officials should use the least expensive travel option available and should use commercial flights, unless otherwise authorized.", "label": 1, "domain": "news", "token_count": 427, "matched_pair_id": "conditionality_00537", "split": "train"}
{"id": "conditionality_train_pos_0060", "text": "2119(c) of the Public Health Service Act (42 U.S.C. 300aa-19(c)) is amended by striking ``not less often than four times per year and''. SEC. 9. CONFORMING AMENDMENT TO TRUST FUND PROVISION. Section 9510(c)(1)(A) of the Internal Revenue Code of 1986 is amended by striking ``(as in effect'' and all that follows through ``for vaccine-related injury or death'' and inserting ``(as in effect on the effective date of the National Vaccine Injury Compensation Program Improvement Act of 2005) for vaccine-related injury or death''. SEC. 10. INCREASE IN LIMIT ON ADMINISTRATIVE EXPENSES. (a) Increase in Limit on Administrative Expenses.--Section 9510(c)(1)(B) of the Internal Revenue Code of 1986 is amended by striking ``(but not in excess of $9,500,000 for any fiscal year)'' and inserting ``(but not in excess of $10,000,000 for any fiscal year)''. (b) Administrative Expenses of Bureau of Public Debt.--Section 9510(c)(1) of the Internal Revenue Code of 1986, as amended by section 9 and subsection (a), is further amended-- (1) in subparagraph (A)(ii), by striking ``or'' at the end; (2) in subparagraph (B), by striking the period at the end and inserting ``, and''; and (3) by adding at the end the following: ``(C) the payment of administrative and personnel expenses that the Bureau of the Public Debt incurs for financial services for the Trust Fund.''. SEC. 11. PUBLIC SERVICE ANNOUNCEMENT CAMPAIGN. Section 2110(c) of the Public Health Service Act (42 U.S.C. 300aa- 10(c)) is amended by striking the period at the end and inserting ``, including by conducting a public service announcement campaign.''. SEC. 12. APPLICATION. The provisions of and amendments made by sections 2, 3, 4, 5, 6, 7, and 9 apply to a petition filed under section 2111 of the Public Health Service Act (42 U.S.C. 300aa-11) if the petition is pending on or filed after the date of the enactment of this Act.", "label": 1, "domain": "government", "token_count": 487, "matched_pair_id": "conditionality_00859", "split": "train"}
{"id": "conditionality_train_pos_0061", "text": "Context. For accurately measuring intensities and determining magnetic field strengths of small-scale solar (magnetic) structure, knowledge of and compensation for the point spread function is crucial. For images recorded with the Swedish 1-meter Solar Telescope, restoration with Multi-Frame Blind Deconvolution and Joint Phase Diverse Speckle methods lead to remarkable improvements in image quality but granulation contrasts that are too low, indicating additional stray light. Aims. We propose a method to compensate for stray light from high-order atmospheric aberrations not included in MFBD and JPDS processing. Methods. To compensate for uncorrected aberrations, a reformulation of the image restoration process is proposed that allows the average effect of hundreds of high-order modes to be compensated for by relying on Kolmogorov statistics for these modes. The applicability of the method requires simultaneous measurements of Fried's parameter r0. The method is tested with simulations as well as real data and extended to include compensation for conventional stray light. Results. We find that only part of the reduction of granulation contrast in SST images is due to uncompensated high-order aberrations. The remainder is still unaccounted for and attributed to stray light from the atmosphere, the telescope with its re-imaging system and to various high-altitude seeing effects. Conclusions. We conclude that statistical compensation of high-order modes is a viable method to reduce the loss of contrast occurring when a limited number of aberrations is explicitly compensated for with MFBD and JPDS processing. We show that good such compensation is possible with only 10 recorded frames. The main limitation of the method is that already MFBD and JPDS processing introduces high-order compensation that, if not taken into account, can lead to over-compensation.", "label": 1, "domain": "academic", "token_count": 352, "matched_pair_id": "conditionality_00245", "split": "train"}
{"id": "conditionality_train_pos_0062", "text": "The outer disk of the LMC is studied in order to unveil clues about its formation and evolution. Complementing our previous studies in innermost fields (3<R<7 kpc), we obtained deep color magnitude diagrams in 6 fields with radius from 5.2 to 9.2 kpc. The comparison with isochrones shows that while the oldest population is approximately coeval in all fields, the age of the youngest populations increases with increasing radius. Low-resolution spectroscopy in the infrared CaII triplet region has been obtained for about 150 stars near the tip red giant branch in the same fields. Radial velocities and stellar metallicities have been obtained from these spectra. The metallicity distribution of each field has been analyzed together with those previously studied. The metal content of the most metal-poor objects, which are also the oldest according to the derived age-metallicity relationships, is similar in all fields independently of the radius. However, while the metallicity of the most metal-rich objects measured, which are the youngest ones, remains constant in the inner 6 kpc, it decreases with increasing radius from there off. The same is true for the mean metallicity. According to the derived age-metallicity relationships, which are consistent with being the same in all fields, this result may be interpreted as an outside-in formation scheme in opposition with the inside-out scenario predicted by LCDM cosmology for a galaxy like the LMC. The analysis of the radial velocities of our sample of giants shows that they follow a rotational cold disk kinematics. The velocity dispersion increases as metallicity decreases indicating that the most metal-poor/oldest objects are distributed in a thicker disk than the most metal-rich/youngest ones in agreement with the findings in other disks such as that of the Milky Way. They do not seem to be part of a hot halo, if one exists in the LMC.", "label": 1, "domain": "academic", "token_count": 382, "matched_pair_id": "conditionality_00344", "split": "train"}
{"id": "conditionality_train_pos_0063", "text": "shares. They can take advantage of technological advancements in voting platforms that allow them to leave standing instructions on how they want their votes cast on particular proposals. “Because they have such a huge work flow, institutions will flag certain types of proposals and will develop guidelines on how they want to vote on them,” Mr. Callan said. “Platforms for institutions integrate all that.” Ms. Fisch, the law professor, asked why a similar process couldn’t be set up for individual investors. In a coming article in the Minnesota Law Review, she argued that low individual investor turnout is a result of an antiquated voting system. In the article, “Standing Voting Instructions: Empowering the Excluded Retail Investor,” she contended that “current regulatory restrictions impede market-based innovation” that could allow individual investors’ voices to be heard. The Securities and Exchange Commission has weighed in on this problem recently. Acknowledging that the low level of voting by individual investors is a concern, it sponsored a roundtable on proxy voting in 2015. A major agenda item was how to increase individual investor participation. But proposals for a system that would allow individuals to leave standing instructions for the voting of their shares have gone nowhere. As Ms. Fisch noted, the commission has voiced concerns that such a system would require investors to make voting decisions before they had received proxy materials “containing the disclosures mandated under the federal securities laws and possibly without consideration of the specific issues to be voted upon.” The agency also warned that the availability of standing voting instructions might mean investors would not bother to read the proxy statement. Still, regulations have gotten in the way of what might be the natural market development of tools to encourage individual investor voting, Ms. Fisch said. “When the voting platforms and proxy advisers work with institutional investors, they provide tools for categorizing issues and proposals to accommodate investor voting preferences even though the issues might differ a little,” she added. “I would envision a platform being able to provide retail investors that same sort of functionality.” Ms. Fisch and others are convinced that individual investors are interested in the makeup of corporate boards, executive pay and other governance matters. Given that technology can lower the hurdles these shareholders face in expressing their views, it seems unfair to ignore it.", "label": 1, "domain": "news", "token_count": 455, "matched_pair_id": "conditionality_00606", "split": "train"}
{"id": "conditionality_train_pos_0064", "text": "We report the results of N-body simulations of disrupting satellites aimed at exploring whether the observed features of dSphs can be accounted for with simple, mass-follows-light (MFL) models including tidal disruption. As a test case, we focus on the Carina dwarf Spheroidal (dSph), which presently has the most extensive data at large radius. We find that previous N-body, MFL simulations of dSphs did not sufficiently explore the parameter space of satellite mass, density and orbital shape to find adequate matches to Galactic dSph systems, whereas with a systematic survey of parameter space we are able to find tidally disrupting, MFL satellite models that rather faithfully reproduce Carina's velocity profile, velocity dispersion profile and projected density distribution over its entire sampled radius. The successful MFL model satellites have very eccentric orbits, currently favored by Cold Dark Matter (CDM) models, and central velocity dispersions that still yield an accurate representation of the bound mass and observed central M/L~40 of Carina, despite inflation of the velocity dispersion outside the dSph core by unbound debris. Our survey of parameter space also allows us to address a number of commonly held misperceptions of tidal disruption and its observable effects on dSph structure and dynamics. The simulations suggest that even modest tidal disruption can have a profound effect on the observed dynamics of dSph stars at large radii. Satellites that are well-described by tidally disrupting MFL models could still be fully compatible with L-CDM if for example they represent a later stage in the evolution of luminous subhalos.", "label": 1, "domain": "academic", "token_count": 326, "matched_pair_id": "conditionality_00039", "split": "train"}
{"id": "conditionality_train_pos_0065", "text": "Type II-plateau supernovae (SNe IIP) are the results of the explosions of red supergiants and are the most common subclass of core-collapse supernovae. Past observations have shown that the outer layers of the ejecta of SNe IIP are largely spherical, but the degree of asphericity increases toward the core. We present evidence for high degrees of asphericity in the inner cores of three recent SNe IIP (SNe 2006my, 2006ov, and 2007aa), as revealed by late-time optical spectropolarimetry. The three objects were all selected to have very low interstellar polarization (ISP), which minimizes the uncertainties in ISP removal and allows us to use the continuum polarization as a tracer of asphericity. The three objects have intrinsic continuum polarizations in the range of 0.83-1.56% in observations taken after the end of the photometric plateau, with the polarization dropping to almost zero at the wavelengths of strong emission lines. Our observations of SN 2007aa at earlier times, taken on the photometric plateau, show contrastingly smaller continuum polarizations (~0.1%). The late-time H-alpha and [O I] line profiles of SN 2006ov provide further evidence for asphericities in the inner ejecta. Such high core polarizations in very ordinary core-collapse supernovae provide further evidence that essentially all core-collapse supernova explosions are highly aspherical, even if the outer parts of the ejecta show only small deviations from spherical symmetry.", "label": 1, "domain": "academic", "token_count": 319, "matched_pair_id": "conditionality_00182", "split": "train"}
{"id": "conditionality_train_pos_0066", "text": "Rules similar to the rules of paragraphs (2) and (4) of section 408(e) shall apply to dairy farm savings accounts, and any amount treated as distributed under such rules shall be treated as not used to pay qualified distributions. ``(f) Tax Treatment of Distributions.-- ``(1) In general.--Any amount paid or distributed out of a dairy farm savings account (other than a rollover contribution described in paragraph (4)) shall be included in gross income of the account beneficiary in the manner provided under section 72. Rules similar to the rules of paragraphs (2) and (3)(H) of section 408(d) shall apply for purposes of this paragraph. ``(2) Additional tax on non-qualified distributions.-- ``(A) In general.--The tax imposed by this chapter on the account beneficiary for any taxable year in which there is a payment or distribution from a dairy farm savings account of such beneficiary which is not a qualified distribution shall be increased by 15 percent of the amount of such payment or distribution which is not a qualified distribution. ``(B) Exception for disability or death.-- Subparagraph (A) shall not apply if the payment or distribution is made after the account beneficiary becomes disabled within the meaning of section 72(m)(7) or dies. ``(3) Excess contributions returned before due date of return.-- ``(A) In general.--If any excess contribution is contributed for a taxable year to a dairy farm savings account of an individual, paragraph (2) shall not apply to distributions from the dairy farm savings accounts of such individual (to the extent such distributions do not exceed the aggregate excess contributions to all such accounts of such individual for such year) if-- ``(i) such distribution is received by the individual on or before the last day prescribed by law (including extensions of time) for filing such individual's return for such taxable year, and ``(ii) such distribution is accompanied by the amount of net income attributable to such excess contribution. Any net income described in clause (ii) shall be included in the gross income of the individual for the taxable year in which it is received. ``(B) Excess contribution.--For purposes of subparagraph (A), the term `excess contribution' means any contribution (other than a rollover contribution) which is not deductible under this section. ``(4) Rollover contribution.--An amount is described in this paragraph as a rollover contribution if it meets the requirements of subparagraphs (A) and (B).", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00974", "split": "train"}
{"id": "conditionality_train_pos_0067", "text": "We investigate the level of fine-tuning of neutralino Dark Matter below 200 GeV in the low-energy phenomenological minimal supersymmetric Standard Model taking into account the newest results from XENON100 and the Large Hadron Collider as well as all other experimental bounds from collider physics and the cosmological abundance. We find that current and future direct Dark Matter searches significantly rule out a large area of the untuned parameter space, but solutions survive which do not increase the level of fine-tuning. As expected, the level of tuning tends to increase for lower cross-sections, but regions of resonant neutralino annihilation still allow for a band at light masses, where the fine-tuning stays small even below the current experimental limits for direct detection cross-sections. For positive values of the supersymmetric Higgs mass parameter \\mu large portions of the allowed parameter space are excluded, but there still exist untuned solutions at higher neutralino masses which will essentially be ruled out if XENON1t does not observe a signal.For negative \\mu untuned solutions are not much constrained by current limits of direct searches and, if the neutralino mass was found outside the resonance regions, a negative \\mu-term would be favored from a fine-tuning perspective. Light stau annihilation plays an important role to fulfill the relic density condition in certain neutralino mass regions. Finally we discuss, in addition to the amount of tuning for certain regions in the neutralino mass-direct detection cross-section plane, the parameter mapping distribution if the allowed model parameter space is chosen to be scanned homogeneously (randomized).", "label": 1, "domain": "academic", "token_count": 320, "matched_pair_id": "conditionality_00481", "split": "train"}
{"id": "conditionality_train_pos_0068", "text": "of the amounts made available under subsection (a) may be used by the Secretaries for Federal administration the program described in that subsection, including providing technical assistance and carrying out evaluations for the program described in that subsection. ``(c) Period of Availability.--The funds appropriated pursuant to subsection (a) for a fiscal year shall be available for Federal obligation for that fiscal year and the succeeding 4 fiscal years. ``SEC. 199B. DEFINITIONS. ``For purposes of this subtitle: ``(1) Community college.--The term `community college' has the meaning given the term `junior or community college' in section 312(f) of the Higher Education Act of 1965 (20 U.S.C. 1058(f)). ``(2) Educational or career training program.--The term `educational or career training program' means-- ``(A) a career pathway program, as defined in section 3; or ``(B) a program with an integrated education and training approach, as defined in section 203.''. (b) Conforming Amendment.--The table of contents for the Workforce Innovation and Opportunity Act is amended by inserting after the items relating to subtitle E of title I the following: ``Subtitle F--Community College to Career Fund ``Sec. 199. Community college and industry partnerships program. ``Sec. 199A. Authorization of appropriations. ``Sec. 199B. Definition.''. (c) Effective Date.--This Act, including the amendments made by this Act, takes effect as if included in the Workforce Innovation and Opportunity Act.", "label": 1, "domain": "government", "token_count": 317, "matched_pair_id": "conditionality_01000", "split": "train"}
{"id": "conditionality_train_pos_0069", "text": "Evolutionary trends in the surface abundances of heavier elements have recently been identified in the globular cluster NGC 6397 ([Fe/H]=-2), indicating the operation of atomic diffusion in these stars. Such trends constitute important constraints for the extent to which diffusion modifies the internal structure and surface abundances of solar-type, metal-poor stars. We perform an independent check of the reality and size of abundance variations within this metal-poor globular cluster. Observational data covering a large stellar sample, located between the cluster turn-off point and the base of the red giant branch, are homogeneously analysed. The spectroscopic data were obtained with the medium-high resolution spectrograph FLAMES/GIRAFFE on VLT-UT2. We derive independent effective-temperature scales from profile fitting of Balmer lines and by applying colour-temperature calibrations to Str\\\"omgren uvby and broad-band BVI photometry. An automated spectral analysis code is used together with a grid of MARCS model atmospheres to derive stellar surface abundances of Mg, Ca, Ti, and Fe. We identify systematically higher iron abundances for more evolved stars. The turn-off point stars are found to have 0.13dex lower surface abundances of iron compared to the coolest, most evolved stars in our sample. There is a strong indication of a similar trend in magnesium, whereas calcium and titanium abundances are more homogeneous. Within reasonable error limits, the obtained abundance trends are in agreement with the predictions of stellar structure models including diffusive processes (sedimentation, levitation), if additional turbulent mixing below the outer convection zone is included.", "label": 1, "domain": "academic", "token_count": 329, "matched_pair_id": "conditionality_00077", "split": "train"}
{"id": "conditionality_train_pos_0070", "text": "Liverpool manager Jurgen Klopp has revealed that he wants to strengthen his squad before the transfer window closes. The Reds’ defensive frailties were exposed during their 3-3 draw at Watford. Klopp’s interest in signing Southampton captain Virgil van Dijk is well known. While the German boss was keen to focus on the work that can be done on the training ground to solve his side’s difficulties with defending set-pieces and pointed out that signing one new player would not solve the problem, he acknowledged that reinforcements are needed. He suggested that current injury problems, which kept Adam Lallana, Nathaniel Clyne, Daniel Sturridge and wantaway attacking midfielder Philippe Coutinho out of the game at Vicarage Road, had accentuated a lack of depth in his squad. Asked if he needed a new centre-back, Klopp told the Liverpool Echo: “We are still working on all parts. We cannot build them. We have to have talks, we’re looking at all parts of the team. “The squad at the moment is not too wide for a lot of games because decisive players are not available. But that’s our situation.” He continued: “People will say I need to buy a new player in the position. I don’t know if that makes real sense. “We did well in the pre-season in this situation. We conceded goals, but we also did good things. We can’t only focus on one thing, but we know it’s an important thing, of course. “I don’t feel comfortable because I can’t change it at the moment. But I know what to do.” Klopp had previously revealed that he wants to sign a new midfielder before the transfer window closes, which suggests there could be at least two new arrivals at Anfield over the next few weeks. A further signing could be need if Coutinho gets his move to Barcelona.", "label": 1, "domain": "news", "token_count": 378, "matched_pair_id": "conditionality_00683", "split": "train"}
{"id": "conditionality_train_pos_0071", "text": "If your kids are still riding high on Jurassic World: Fallen Kingdom euphoria after watching the movie at the cinema, satiate their hunger for all things dino at Dinosaur Kingdom, a mobile dino-themed entertainment park that will be set-up at various locations around Malaysia. The first location is at Setia Ecohill, Semenyih where visitors can come on over starting 14 June 2018 until 8 July 2018. Organised by Themepaktu, Dinosaur Kingdom consists of more than 25 attractions that can be enjoyed by young and old alike. The main attraction at the Themepaktu Dinosaur Kingdom is the 40-minutes live show, featuring dinosaur animatronics depicting exciting scenes set in the Jurassic age. You and your kids can also explore the Raptor Maze, ride a Dinosaur Bumper Boat in “The Swamp”, join a drift race,or climb up to a Pterosaur’s Nest, among other interactive activities to be enjoyed here. With attractions such as a baby dinosaur trail to scope out, a triceratops train ride to go on, and raptor races to test your riding skills and dexterity, it’s a great opportunity to get the kids away from their gadgets and have an amazing time getting physically active in the outdoors. So if you’re thinking about where to bring the kids to during this Hari Raya school holidays, consider a trip to Dinosaur Kingdom to be included in your plans. Themepaktu Dinosaur Kingdom Duration: 14 June until 8 July 2018 Opening Hours: 12 pm to 10.30 pm daily Entrance fee: RM30 per person (includes entry to the park, exhibition, Live Show, Education Hub and Fossil Site) Tokens for rides: RM3 per token, also available in 10-token packs and Entrance + 10 Tokens package for RM30 Go to themepaktu.com for more information.", "label": 1, "domain": "news", "token_count": 387, "matched_pair_id": "conditionality_00565", "split": "train"}
{"id": "conditionality_train_pos_0072", "text": "and metropolitan planning organizations under sections 5303 and 5304 of this title and sections 134 and 135 of title 23; ``(B) effective measures of the outcome or performance of transportation programs-- ``(i) across all modes of transportation; and ``(ii) with respect to the transportation program as a whole, rather than individual projects within the transportation program; and ``(C) a strategy to ensure that the Secretary continuously refines and standardizes data elements, models, and other estimating methods to steadily improve public and political confidence in the use of the outcome-oriented performance measures established under paragraph (1) as a basis for making transportation investments. ``(3) Availability of plan.--The Secretary shall make the plan developed under paragraph (1) available to the public on the website of the Department of Transportation. ``(e) Comprehensive Report to Congress.--Not later than 21 months after the date of enactment of this section, the Secretary shall submit to Congress a comprehensive report on the pilot program that includes-- ``(1) a summary of the results of the case studies under subsection (c); ``(2) the plan developed under subsection (d); ``(3) a summary of lessons learned with respect to challenges encountered by each program participant; and ``(4) recommendations, if any, for legislation to improve-- ``(A) the guidance provided to States and metropolitan planning organizations for generating and collecting sound, outcome-based data; and ``(B) data-based performance measurement, analysis, and accountability for transportation programs. ``(f) Authorization of Appropriations.--There is authorized to be appropriated from the Highway Trust Fund to carry out this section, $15,000,000 for the 2-year period beginning on the date of enactment of this section.''. SEC. 2. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 443, "matched_pair_id": "conditionality_00878", "split": "train"}
{"id": "conditionality_train_pos_0073", "text": "We present a finite difference method to solve a new type of nonlocal hydrodynamic equations that arise in the theory of spatially inhomogeneous Bloch oscillations in semiconductor superlattices. The hydrodynamic equations describe the evolution of the electron density, electric field and the complex amplitude of the Bloch oscillations for the electron current density and the mean energy density. These equations contain averages over the Bloch phase which are integrals of the unknown electric field and are derived by singular perturbation methods. Among the solutions of the hydrodynamic equations, at a 70 K lattice temperature, there are spatially inhomogeneous Bloch oscillations coexisting with moving electric field domains and Gunn-type oscillations of the current. At higher temperature (300 K) only Bloch oscillations remain. These novel solutions are found for restitution coefficients in a narrow interval below their critical values and disappear for larger values. We use an efficient numerical method based on an implicit second-order finite difference scheme for both the electric field equation (of drift-diffusion type) and the parabolic equation for the complex amplitude. Double integrals appearing in the nonlocal hydrodynamic equations are calculated by means of expansions in modified Bessel functions. We use numerical simulations to ascertain the convergence of the method. If the complex amplitude equation is solved using a first order scheme for restitution coefficients near their critical values, a spurious convection arises that annihilates the complex amplitude in the part of the superlattice that is closer to the cathode. This numerical artifact disappears if the space step is appropriately reduced or we use the second-order numerical scheme.", "label": 1, "domain": "academic", "token_count": 323, "matched_pair_id": "conditionality_00449", "split": "train"}
{"id": "conditionality_train_pos_0074", "text": "if that program provides protection for public safety, the environment, or excavators that is equivalent to, or greater than, protection under a program that meets the minimum standards set forth in section 6103. ``(d) Report.--Within 3 years after the date of the enactment of the Comprehensive One-call Notification Act of 1997, the Secretary shall begin to include the following information in reports submitted under section 60124 of this title-- ``(1) a description of the extent to which each State has adopted and implemented the minimum Federal standards under section 6103 or maintains an alternative program under subsection (c); ``(2) an analysis by the Secretary of the overall effectiveness of the State's one-call notification program and the one-call notification systems operating under such program in achieving the purposes of this chapter; ``(3) the impact of the State's decisions on the extent of required participation in one-call notification systems on prevention of damage to underground facilities; and ``(4) areas where improvements are needed in one-call notification systems in operation in the State. The report shall also include any recommendations the Secretary determines appropriate. If the Secretary determines that the purposes of this chapter have been substantially achieved, no further report under this section shall be required. ``Sec. 6105. REVIEW OF ONE-CALL SYSTEM BEST PRACTICES ``(a) Study of Existing One-Call Systems.--Except as provided in subsection (d), the Secretary, in consultation with other appropriate Federal agencies, State agencies, one-call notification system operators, underground facility operators, excavators, and other interested parties, shall undertake a study of damage prevention practices associated with existing one-call notification systems. ``(b) Purpose of Study of Damage Prevention Practices.--The purpose of the study is to assemble information in order to determine which existing one-call notification systems practices appear to be the most effective in preventing damage to underground facilities and in protecting the public, the environment, excavators, and public service disruption. As part of the study, the Secretary shall at a minimum consider-- ``(1) the methods used by one-call notification systems and others to encourage participation by excavators and owners of underground facilities; ``(2) the methods by which one-call notification systems promote awareness of their programs, including use of public service announcements and educational materials and programs; ``(3) the methods by which one-call notification systems receive and distribute information from excavators and underground facility owners; ``(4) the use of any performance and service standards to verify the effectiveness of a", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00958", "split": "train"}
{"id": "conditionality_train_pos_0075", "text": "if any) made under this clause, including the evaluations conducted under subclauses (II) through (IV). ``(v) No changes to adjustment factors that prevent activities consistent with national health policy goals.--In making any changes to the adjustment factors, including adjustment for health status under paragraph (3), the Secretary shall ensure that the changes do not prevent Medicare Advantage organizations from performing or undertaking activities that are consistent with national health policy goals, including activities to promote early detection and better care coordination, the use of health risk assessments, care plans, and programs to slow the progression of chronic diseases. ``(vi) Opportunity for review and public comment regarding changes to adjustment factors.--For changes to adjustment factors effective for 2017 and subsequent years, in addition to providing notice of such changes in the announcement under subsection (b)(2), the Secretary shall provide an opportunity for review of proposed changes of not less than 60 days and a public comment period of not less than 30 days before implementing such changes.''. SEC. 3. SENSE OF CONGRESS. It is the sense of Congress that-- (1) the Centers for Medicare & Medicaid Services has inadvertently created a star rating system under section 1853(o)(4) of the Social Security Act (42 U.S.C. 1395w- 23(o)(4)) for Medicare Advantage plans that lacks proper accounting for the socioeconomic status of enrollees in such plans and the extent to which such plans serve individuals who are also eligible for medical assistance under title XIX of such Act; and (2) Congress will work with the Centers for Medicare & Medicaid Services and stakeholders, including beneficiary groups and managed care organizations, to ensure that such rating system properly accounts for the socioeconomic status of enrollees in such plans and the extent to which such plans serve such individuals described in paragraph (1).", "label": 1, "domain": "government", "token_count": 372, "matched_pair_id": "conditionality_00833", "split": "train"}
{"id": "conditionality_train_pos_0076", "text": "We present a detailed analysis of 108 helium-line (DB) white dwarfs based on model atmosphere fits to high signal-to-noise optical spectroscopy. We derive a mean mass of 0.67 Mo for our sample, with a dispersion of only 0.09 Mo. White dwarfs also showing hydrogen lines, the DBA stars, comprise 44% of our sample, and their mass distribution appears similar to that of DB stars. As in our previous investigation, we find no evidence for the existence of low-mass (M < 0.5 Mo) DB white dwarfs. We derive a luminosity function based on a subset of DB white dwarfs identified in the Palomar-Green survey. We show that 20% of all white dwarfs in the temperature range of interest are DB stars, although the fraction drops to half this value above Teff ~ 20,000 K. We also show that the persistence of DB stars with no hydrogen features at low temperatures is difficult to reconcile with a scenario involving accretion from the interstellar medium, often invoked to account for the observed hydrogen abundances in DBA stars. We present evidence for the existence of two different evolutionary channels that produce DB white dwarfs: the standard model where DA stars are transformed into DB stars through the convective dilution of a thin hydrogen layer, and a second channel where DB stars retain a helium-atmosphere throughout their evolution. We finally demonstrate that the instability strip of pulsating V777 Her white dwarfs contains no nonvariables, if the hydrogen content of these stars is properly accounted for.", "label": 1, "domain": "academic", "token_count": 324, "matched_pair_id": "conditionality_00336", "split": "train"}
{"id": "conditionality_train_pos_0077", "text": "The presence of extremely compact galaxies at z~2 and their subsequent growth in physical size has been the cause of much puzzlement. We revisit the question using deep infrared Wide Field Camera 3 data to probe the rest-frame optical structure of 935 host galaxies selected with 0.4<z<2.5 and stellar masses M* > 10^10.7 Msol using optical and near-infrared photometry in the UKIRT Ultra Deep Survey and GOODS-South fields of the CANDELS survey. At each redshift, the most compact sources are those with little or no star formation, and we find that the mean size of these systems grows by a factor of 3.5 +- 0.3 over this redshift interval. The new data are sufficiently deep to enable us to identify companions to these hosts whose stellar masses are ten times smaller, while still yielding suitably accurate photometric redshifts to define a likely physical association. By searching for faint companions around 404 quiescent hosts within a projected physical annulus 10 < R < 30 kpc/h, we estimate the minor merger rate over the redshift range 0.4 < z < 2. After correcting for contamination from projected pairs, we find that 13-18% of quiescent hosts have likely physical companions with stellar mass ratios of 0.1 or greater. Mergers of these companions will typically increase the host mass by 6+-2% per merger timescale. We estimate the minimum growth rate necessary to explain the declining abundance of compact galaxies. Using a simple model of merging motivated by recent numerical simulations, we then assess whether mergers of the faint companions with their hosts are sufficient to explain this minimal rate. We find that mergers with mass ratios > 0.1 may explain most of the size evolution observed at z >~ 1 if a relatively short merger timescale is assumed, but the rapid growth seen at higher redshift likely requires additional physical processes.", "label": 1, "domain": "academic", "token_count": 404, "matched_pair_id": "conditionality_00380", "split": "train"}
{"id": "conditionality_train_pos_0078", "text": "Results are presented from NIR spectroscopy of a sample of BzK-selected, massive star-forming galaxies (sBzKs) at 1.5<z<2.3 that were obtained with OHS/CISCO at Subaru and with SINFONI at VLT. Among the 28 sBzKs observed, Ha emission was detected in 14 objects, and for 11 of them the [NII]6583 was also measured. Multiwavelength photometry was also used to derive stellar masses and extinction parameters, whereas Ha and [NII] have allowed us to estimate SFR, metallicities, ionization mechanisms, and dynamical masses. In order to enforce agreement between SFRs from Ha with those derived from rest-frame UV and MIR, additional obscuration for the emission lines (that originate in HII regions) was required compared to the extinction derived from the slope of the UV continuum. We have also derived the stellar mass-metallicity relation, as well as the relation between stellar mass and specific SFR, and compared them to the results in other studies. At a given stellar mass, the sBzKs appear to have been already enriched to metallicities close to those of local star-forming galaxies of similar mass. The sBzKs presented here tend to have higher metallicities compared to those of UV-selected galaxies, indicating that NIR selected galaxies tend to be a chemically more evolved population. The sBzKs show specific SFRs that are systematically higher, by up to ~2 orders of magnitude, compared to those of local galaxies of the same mass. The empirical correlations between stellar mass and metallicity, and stellar mass and specific SFR are then compared with those of population synthesis models constructed either with the simple closed-box assumption, or within an infall scenario. Within the assumptions that are built-in such models, it appears that a short timescale for the star-formation (~100 Myr) and large initial gas mass appear to be required if one wants to reproduce both relations simultaneously.", "label": 1, "domain": "academic", "token_count": 419, "matched_pair_id": "conditionality_00210", "split": "train"}
{"id": "conditionality_train_pos_0079", "text": "If you’re able to work, then you should — at least if you want food stamps. That’s what more than 80 percent of voters think, a new poll for the Foundation for Government Accountability finds. And it’s actually already the law. That’s right: Officially, the Supplemental Nutrition Assistance Program requires able-bodied adults without dependents to work, train or volunteer — at least part-time. That SNAP requirement was part of the 1996 welfare-reform package that President Bill Clinton worked out with a Republican Congress. But it was undermined from the start, since it allowed the secretary of agriculture to waive work requirements in times of need. Yet while it might make sense to give waivers in areas with high unemployment, the Clinton-era bureaucrats who wrote the enabling regulations ensured that waivers would be ridiculously easy to get. New York’s latest request cites unemployment data from several years ago to justify its waiver. Just about every state plays some game. But President Trump can have his Agriculture Department get going to write much tougher regulations, with no need to go to Congress. It’s something the public will clearly support — as it has backed sensible welfare reform for decades. And SNAP — now delivered via Electronic Benefit Cards rather than the old food-stamp coupons — has become a huge welfare program, booming under the last two presidents. Indeed, enrollment has soared to over 42 million, 13 percent of the US population. And roughly half are able-bodied adults, who account for $34 billion of the program’s benefits. That’s nuts. If ever there was a time to push these folks back into the workforce, it’s now: The economy is booming and employers are looking to hire, with 6 million jobs open across the country and unemployment at just 4.1 percent. Requiring the able-bodied to do some kind of work in exchange for federal aid doesn’t impose a hardship; it pushes them onto a path toward self-sufficiency. The 1996 reforms for regular welfare proved that. Though liberals warned the new rules would lead to mass suffering, the reverse was true: Just from 1996 to 2000, 2.4 million of Americans formerly trapped in dependency went out and found jobs. Team Trump is already offering states the chance to impose work requirements on those enrolled in Medicaid. Taking a similar step on food stamps should be a no-brainer.", "label": 1, "domain": "news", "token_count": 478, "matched_pair_id": "conditionality_00811", "split": "train"}
{"id": "conditionality_train_pos_0080", "text": "You can’t say that Warner Bros. and TellTale Games don’t know how to take advantage of the blockbuster superhero movie release schedules. Back in February, Lego Marvel Super Heroes 2 released a special Black Panther DLC pack just in time for that film’s premiere. Now they’re following suit again for the biggest Marvel movie yet. On Tuesday, you will be able to pick up the Marvel’s Avengers: Infinity War Character and Level Pack for just $2.99 — provided you already own Lego Marvel Super Heroes 2, of course. As you can see in the trailer above, the main draw is an astonishingly adorable Thanos in minifig form, with whom you’ll be able to terrorize the itty-bitty little Lego Marvel Universe. That sounds and looks way more delightful than it probably should be. From the TT Games press release: This action-packed level offers players the chance to control Thanos, one of the most dangerous Super Villains in the Marvel Universe, and his ruthless army. The Mad Titan and the Children of Thanos have invaded Attilan to take on Black Bolt and the Inhumans in an all-new original game level. Working as a team, the menacing crew must work their way through the various levels of Attilan before they are given the opportunity to break through to Black Bolt’s throne. New unlockable characters Thanos, Corvus Glaive, Cull Obsidian, Proxima Midnight, Ebony Maw, Hulkbuster 2.0, and Groot (Avengers: Infinity War) add to the main game’s roster of over 200 Super Heroes and Super Villains. While $2.99 certainly sounds like a good deal, the Season Pass option for $14.99 gives you themed DLC for the already-released Guardians of the Galaxy Vol. 2, Black Panther, Runaways, and Cloak & Dagger content, and the upcoming Champions, Out of Time, and Agents of Atlas packs. That’s a whooole lot of Marvel goodies and goodness if you’re into the Lego video game aesthetic.", "label": 1, "domain": "news", "token_count": 424, "matched_pair_id": "conditionality_00556", "split": "train"}
{"id": "conditionality_train_pos_0081", "text": "This is the second of the two related papers analysing origins and possible explanations of a paradoxical phenomenon of the quantum potential (QP). It arises in quantum mechanics'(QM) of a particle in the Riemannian $n$-dimensional configurational space obtained by various procedures of quantization of the non-relativistic natural Hamilton systems. Now, the two questions are investigated: 1)Does QP appear in the non-relativistic QM generated by the quantum theory of scalar field (QFT) non-minimally coupled to the space-time metric? 2)To which extent is it in accord with quantization of the natural systems? To this end, the asymptotic non-relativistic equation for the particle-interpretable wave functions and operators of canonical observables are obtained from the primary QFT objects. It is shown that, in the globally-static space-time, the Hamilton operators coincide at the origin of the quasi-Euclidean space coordinates in the both altenative approaches for any constant of non-minimality $\\tilde\\xi$, but a certain requirement of the Principle of Equivalence to the quantum field propagator distinguishes the unique value $\\tilde\\xi = 1/6$. Just the same value had the constant $\\xi$ in the quantum Hamiltonians arising from the traditional quantizations of the natural systems: the DeWitt canonical, Pauli-DeWitt quasiclassical, geometrical and Feynman ones, as well as in the revised Schr\\\"{o}dinger variational quantization. Thus, QP generated by mechanics is tightly related to non-minimality of the quantum scalar field. Meanwhile, an essential discrepancy exists between the non-relativistic QMs derived from the two altenative approaches: QFT generate a scalar QP, whereas various quantizations of natural mechanics, lead to PQs depending on choice of space coordinates as physical observables and non-vanishing even in the flat space if the coordinates are curvilinear.", "label": 1, "domain": "academic", "token_count": 411, "matched_pair_id": "conditionality_00410", "split": "train"}
{"id": "conditionality_train_pos_0082", "text": "Heights Half Marathon and 5K now registering HUBER HEIGHTS — The Y at the Heights is hosting the 5th Annual Heights Half Marathon & 5K Fun Run on May 19, 2018 The Half Marathon will begin at 7 a.m. followed by the 5K at 7:30 a.m. You may pick up your race packet on Friday, May 18 from Noon – 7 p.m. at the Y or Saturday, May 19 from 6-6:45 a.m. at the start line near the Aquatic Center at the Heights. All Half Marathon finishers will receive a medal and dri-fit shirt. 5K participants will receive a medal and t-shirt. For more information please visit http://www.theheightshalf.com/ Bingo offered at Huber Heights Athletic Foundation HUBER HEIGHTS — Come on out and play bingo at the Huber Heights Athletic Foundation, a volunteer run charitable Bingo located at 5367 Fishburg Road in Huber Heights. Games start at 1 p.m. on Saturday and Sunday with doors opening at 11 a.m. Ticket sales/paper sales start at 11:30 a.m. at $20 to play up to 36 faces and $5 buys three faces for the ‘Break the Bank/Callers Choice’ game for players 18 and older. No one under 18 is permitted during Bingo play/ticket sales. There are guaranteed payouts for the day from the bingo games of $4,600 and there are many Instant tickets and jackpots in addition to that to be won. All proceeds remain in Huber Heights and go to support youth in their school and athletic functions/pursuits within Huber Heights. No Bingo on holidays or if weather makes driving hazardous.", "label": 1, "domain": "news", "token_count": 364, "matched_pair_id": "conditionality_00698", "split": "train"}
{"id": "conditionality_train_pos_0083", "text": "Cold steady-state disk wind theory from near Keplerian accretion disks requires a large scale magnetic field at near equipartition strength. However the minimum magnetization has never been tested. We investigate the time evolution of an accretion disk threaded by a weak vertical magnetic field. The strength of the field is such that the disk magnetization falls off rapidly with radius. Four 2.5D numerical simulations of viscous resistive accretion disk are performed using the magnetohydrodynamic code PLUTO. In these simulations, a mean field approach is used and turbulence is assumed to give rise to anomalous transport coefficients (alpha prescription). The large scale magnetic field introduces only a small perturbation to the disk structure, with accretion driven by the dominant viscous torque. A super fast magnetosonic jet is observed to be launched from the innermost regions and remains stationary over more than 953 Keplerian orbits. The self-confined jet is launched from a finite radial zone in the disk which remains constant over time. Ejection is made possible because the magnetization reaches unity at the disk surface, due to the steep density decrease. However, no ejection is reported when the midplane magnetization becomes too small. The asymptotic jet velocity remains nevertheless too low to explain observed jets due to the negligible power carried away by the jet. Astrophysical disks with superheated surface layers could drive analogous outflows even if their midplane magnetization is low. Sufficient angular momentum would be extracted by the turbulent viscosity to allow the accretion process to continue. The magnetized outflows would be no more than byproducts, rather than a fundamental driver of accretion. However, if the midplane magnetization increases towards the center, a natural transition to an inner jet dominated disk could be achieved.", "label": 1, "domain": "academic", "token_count": 365, "matched_pair_id": "conditionality_00208", "split": "train"}
{"id": "conditionality_train_pos_0084", "text": "By Fungi Kwaramba The ruling Zanu PF party’s supreme decision-making organ in between congresses, the politburo, meets in Harare today for another crunch meeting that could end the uncertainty surrounding Saviour Kasukuwere’s future as the revolutionary party’s national political commissar. The 47-year-old Mount Darwin legislator goes into today’s potentially explosive meeting unsure whether he will keep his job, which he assumed only three years ago. Kasukuwere has been skating on thin ice ever since an insurrection against his leadership broke out in his home province of Mashonaland Central, with eight other regions throwing their weight behind calls for his ouster. Those baying for his blood accuse the party’s chief organiser and strategist of plotting a bloodless coup against the Zanu PF leader; causing mayhem in the party by interfering with party structures and imposing leaders at various levels. Also under fire is his brother Dickson Mafios, who is the acting Zanu PF chairperson for Mashonaland Central — a ruling party stronghold. Kasukuwere has his sympathisers as well, who have formed his rearguard, including Vice President Phelekezela Mphoko who believe that the brouhaha was being sponsored by a rival faction out to decimate President Robert Mugabe’s foot soldiers before launching a final assault for the high pressure job. In a bid to resolve the impasse, Mugabe set up a committee led by politburo member, Jacob Mudenda, to get to the bottom of the standoff and recommend a way forward. The committee has since finalised its report, which will be tabled at today’s crunch meeting. Zanu PF insiders said the report could be debated along factional lines hence Mugabe would, in the final analyses, be forced to take a stand. The ruling party is dominated by two factions namely Generation 40 (G40), which is sympathetic to Kasukuwere, and Team Lacoste, which has been sharpening its knives, ready to finish off the embattled political commissar. Analysts said the Zanu PF leader is caught between a rock and a hard place as he tries to balance the factional interests playing out in his party. Political analyst, Ibbo Mandaza, believes that Mugabe may not act on Kasukuwere. He said: “I am not sure if anything will be done; he thrives on chaos and confusion”.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00616", "split": "train"}
{"id": "conditionality_train_pos_0085", "text": "(Abridged) We aim to determine the degrees of CO depletion, deuterium fractionation, and ionisation in a sample of seven massive clumps associated with IRDCs. The APEX telescope was used to observe the C17O(2-1), H13CO+(3-2), DCO+(3-2), N2H+(3-2), and N2D+(3-2) transitions towards the clumps. The CO molecules do not appear to be significantly depleted in the observed clumps. The DCO+/HCO+ and N2D+/N2H+ column density ratios are about 0.0002-0.014 and 0.002-0.028, respectively. The former ratio is found to decrease as a function of gas kinetic temperature. A simple chemical analysis suggests that the lower limit to the ionisation degree is in the range x(e)~10^{-8}-10^{-7}, whereas the estimated upper limits range from a few 10^{-6} up to ~10^{-4}. Lower limits to x(e) imply the cosmic-ray ionisation rate of H2 to lie between zeta_H2~10^{-17}-10^{-15} s^{-1}. These are the first estimates of x(e) and zeta_H2 towards massive IRDCs reported so far. The finding that CO is not depleted in the observed sources conforms to the fact that they show evidence of star formation activity which is believed to release CO from the icy grain mantles back into the gas phase. The observed degree of deuteration is lower than in low-mass starless cores and protostellar envelopes. Decreasing deuteration with increasing temperature is likely to reflect the clump evolution. On the other hand, the association with young high-mass stars could enhance zeta_H2 and x(e) above the levels usually found in low-mass star-forming regions. On the scale probed by our observations, ambipolar diffusion cannot be a main driver of clump evolution unless it occurs on timescales >>10^6 yr.", "label": 1, "domain": "academic", "token_count": 426, "matched_pair_id": "conditionality_00370", "split": "train"}
{"id": "conditionality_train_pos_0086", "text": "Deflagration models poorly explain the observed diversity of SNIa. Current multidimensional simulations of SNIa predict a significant amount of, so far unobserved, carbon and oxygen moving at low velocities. It has been proposed that these drawbacks can be resolved if there is a sudden jump to a detonation (delayed detonation), but this kind of models has been explored mainly in one dimension. Here we present new three-dimensional delayed detonation models in which the deflagraton-to-detonation transition (DDT) takes place in conditions like those favored by one-dimensional models. We have used a SPH code adapted to SNIa with algorithms devised to handle subsonic as well as supersonic combustion fronts. The starting point was a C-O white dwarf of 1.38 solar masses. When the average density on the flame surface reached 2-3x10^7 g/cm^3 a detonation was launched. The detonation wave processed more than 0.3 solar masses of carbon and oxygen, emptying the central regions of the ejecta of unburned fuel and raising its kinetic energy close to the fiducial 10^51 ergs expected from a healthy Type Ia supernova. The final amount of 56Ni synthesized also was in the correct range. However, the mass of carbon and oxygen ejected is still too high. The three-dimensional delayed detonation models explored here show an improvement over pure deflagration models, but they still fail to coincide with basic observational constraints. However, there are many aspects of the model that are still poorly known (geometry of flame ignition, mechanism of DDT, properties of detonation waves traversing a mixture of fuel and ashes). Therefore, it will be worth pursuing its exploration to see if a good SNIa model based on the three-dimensional delayed detonation scenario can be obtained.", "label": 1, "domain": "academic", "token_count": 379, "matched_pair_id": "conditionality_00035", "split": "train"}
{"id": "conditionality_train_pos_0087", "text": "The Day of the Dead is a holiday observed in Mexico and other Latin American countries that celebrates and honours the memory of deceased loved ones. Falling on Nov. 1, just a day after Halloween celebrations, the holiday shares some of the sentiment of Halloween, but it is a very different occasion. Where Halloween views the dead as spooky haunts, the day known locally as Dia de los Muertos remembers them as beloved citizens of the afterlife. Through the building of altars, lively fiestas, and offerings of the departed’s favourite foods, Dia de los Muertos is a true celebration, shared between the living and the dead. And while there are many ways to celebrate, here at The Culinary Institute of America we have a habit of focusing on the dinner table. Luckily, the rich cultures surrounding the day are a wealth of traditional recipes and ingredients. Day of the Dead bread and tamales are a good place to start, but we especially love the ritual involved in creating flavourful and traditional moles, as in CIA Chef Sofia Sada’s recipe for Mole Poblano. Today, Mexico has identified more than 50 different moles, but a mole is really whatever you want your sauce to be. Of course, this traditional Mole Poblano is the most well-known variety, and so it’s a perfect representation of Mexico’s culinary tradition. If you’re looking at the ingredient list and thinking, “Wow, that’s a lot of ingredients,” you’re right. This complex sauce is not something you can throw together quickly on a Wednesday night, but for a special occasion, it is well worth the effort. Luckily, the sauce can be made well ahead of time and frozen, which means any weeknight can be that special occasion. Not all moles contain chocolate, but this recipe calls for Mexican chocolate, which is a unique ingredient that you can easily find at Latin American markets or from online retailers. Cacao, the large bean from which chocolate is produced, is native to Mexico, and chocolate has a long history in the many ancient cultures of the region. Today, Mexican chocolate is unique in that it contains cinnamon and other spices, and helps bring out the flavours of the mole. You may not use dried chilies every day, but they offer a more intense flavour than their fresh counterparts. Just like the chocolate, they are abundant at markets if you know where to look, and they store well, so keep some on hand for experimenting.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00660", "split": "train"}
{"id": "conditionality_train_pos_0088", "text": "We perform some experimental simulations in spherical symmetry and axisymmetry to understand the post-shock-revival evolution of core-collapse supernovae. Assuming that the stalled shock wave is relaunched by neutrino heating and employing the so-called light bulb approximation, we induce shock revival by raising the neutrino luminosity by hand up to the critical value, which is also de- termined by dynamical simulations. A 15M_{sun} progenitor model is employed. We incorporate nuclear network calculations with a consistent equation of state in the simulations to account for the energy release by nuclear reactions and their feedback to hydrodynamics. Varying the shock-relaunch time rather arbitrarily, we investigate the ensuing long-term evolutions systematically, paying particular attention to the explosion energy and nucleosynthetic yields as a function of this relaunch time, or equivalently the accretion rate at shock revival. We study in detail how the diagnostic explosion energy approaches the asymptotic value and which physical processes contribute to the explosion energy in what proportions as well as their dependence on the relaunch time and the dimension of dynamics. We find that the contribution of nuclear reactions to the explosion energy is comparable to or greater than that of neutrino heating. In particular, recombinations are dominant over burnings in the contributions of nuclear reactions. Interestingly 1D models studied in this paper cannot produce the appropriate explosion energy and nickel mass simultaneously, overproducing nickels, whereas this problem is resolved in 2D models if the shock is relaunched at 300-400ms after bounce.", "label": 1, "domain": "academic", "token_count": 317, "matched_pair_id": "conditionality_00497", "split": "train"}
{"id": "conditionality_train_pos_0089", "text": "Barry Manilow postpones shows to rest vocal cords Manilow postponed two concerts in Los Angeles and Chicago on doctor's orders because of sprained vocal cords. Barry Manilow's late-in-life coming-out experience was 'beautiful' Barry Manilow was touched by the public’s reaction to him coming out as gay. The 73-year-old “Copacabana” hitmaker spoke about the positive experience on the red carpet at the BMI... Barry Manilow: 'I cannot spot a hit song — even if I write it' In 1976, just as his career as a pop superstar was taking off, Barry Manilow moved into an apartment in the San Remo on Central Park West. His neighbor was... Aretha Franklin battles illness to sing for Clive Davis There are few people that Aretha Franklin would ever bow to, but on Wednesday night, she did exactly that for her mentor Clive Davis at Radio City Music Hall. The... Why Barry Manilow hid his sexuality for 40 years He said of the clandestine nature of his nearly 40-year romance with Garry Kief, “I’m so private. I always have been.” Barry Manilow joins concert to help human rights groups Proceeds will benefit the National Coalition Against Domestic Violence, Southern Poverty Law Center, National Immigration Law Center and the Sierra Club Foundation. Inside the Grammy bash that even Kanye 'begged to get in' On Grammy night, the biggest names in music gather at the Staples Center in Los Angeles — but if you look closely, most seem a bit bleary-eyed. That’s because they... Barry Manilow hospitalized for oral surgery complications It's unclear what type of oral surgery he underwent and if he'll attend Monday night's Grammy ceremony.", "label": 1, "domain": "news", "token_count": 359, "matched_pair_id": "conditionality_00825", "split": "train"}
{"id": "conditionality_train_pos_0090", "text": "If you're a gamer who grew up in the 1980s (like me), odds are you helped Link rescue Princess Zelda or Mario defeat King Bowser on a Nintendo Entertainment System (NES). Thirty-plus years later, Nintendo is helping those gamers relive their old-school victories with the NES Classic Edition. Released in November 2016, the NES Classic Edition is a pint-size version of the original system. It comes with a single two-button controller and 30 preloaded games, including old favorites like Super Mario Bros., The Legend of Zelda, Donkey Kong, Metroid and Ghosts'n Goblins. The original NES Classic Edition was discontinued in April 2017. Nintendo has said that that console will return to stores on June 29, 2018. How did Nintendo pack so much 8-bit fun into a single box? To find out, I broke out my tools. Note: This story originally ran in the Fall 2017 issue of CNET Magazine. We're publishing the story online to coincide with our Cracking Open video of the NES Classic and the original NES. Cracking open the NES Classic Edition I started with the four rubber pads, or feet, on the console's bottom. Using a thin Phillips screwdriver, I removed the pads and the tiny screw hidden underneath each one. I then lifted off the upper half of the system's plastic case to reveal the tech inside. Though it's less than a quarter the size of the original NES, the Classic Edition's interior is far less cramped. Gone are the front-loading, VCR-esque cartridge tray, the 72-pin cartridge connector that failed so often and the bulky video, audio and power circuitry. All that 1980s tech has been condensed down to a single main circuit board that's about the size of a drink coaster. After disconnecting the cables for the two game controller ports and a thin cable for the power and reset buttons, I removed a few more screws, lifted off the metal shield that covers the main circuit board and took out the board itself. Next, I removed the two controller ports, each held in place with a small bracket and single screw. To finish, I only had to disconnect a black, plastic housing that contains a small circuit board to which the contacts for the power and reset buttons are mounted along with the front LED. My teardown of the console was complete. Turning my attention to the game controller, I removed six screws from the bottom of its clam", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00501", "split": "train"}
{"id": "conditionality_train_pos_0091", "text": "Kaplanski's Zero Divisor Conjecture envisions that for a torsion-free group G and an integral domain R, the group ring R[G] does not contain non-trivial zero divisors. We define the length of an element a in R[G] as the minimal non-negative integer k for which there are ring elements r_1,...,r_k in R and group elements g_1,...,g_k in G such that a = r_1 g_1+...+r_k g_k. We investigate the conjecture when R is the field of rational numbers. By a reduction to the finite field with two elements, we show that if ab = 0 for non-trivial elements in the group ring of a torsion-free group over the rationals, then the lengths of a and b cannot be among certain combinations. More precisely, we show for various pairs of integers (i,j) that if one of the lengths is at most i then the other length must exceed j. Using combinatorial arguments we show this for the pairs (3,6) and (4,4). With a computer-assisted approach we strengthen this to show the statement holds for the pairs (3,16) and (4,7). As part of our method, we describe a combinatorial structure, which we call matched rectangles, and show that for these a canonical labeling can be computed in quadratic time. Each matched rectangle gives rise to a presentation of a group. These associated groups are universal in the sense that there is no counterexample to the conjecture among them if and only if the conjecture is true over the rationals.", "label": 1, "domain": "academic", "token_count": 336, "matched_pair_id": "conditionality_00421", "split": "train"}
{"id": "conditionality_train_pos_0092", "text": "conversion of positions identified pursuant to subparagraph (D) as described in that subparagraph. (5) Report to secretary of defense.--Not later than 180 days after the date of the enactment of this Act, the working group shall submit to the Secretary of Defense a report on the comprehensive review undertaken pursuant to paragraph (4). The report shall include the following: (A) A comprehensive description of the review and the results of the review. (B) The percentage of military technician (dual status) positions whose conversion to positions of Federal civilian employment under title 5, United States Code, would best ensure the achievement of objectives for full time support of the reserve components of the Armed Forces as an operational reserve. (C) A transition plan for implementing a new force structure for full time support of the reserve components, including for the conversion of positions as described in subparagraph (B) which mitigates any risks to readiness identified pursuant to paragraph (4)(E). (D) Recommendations for the reform of personnel management policy for military technician (dual status) positions that address-- (i) the eligibility of military technicians (dual status) for civilian retirement upon retirement from the Armed Forces; and (ii) the process for appealing employment decisions. (E) Recommendations for reforms of compensation and benefits policies for military technician (dual status) positions in order to provide military technicians (dual status) with parity in compensation and benefits with other Federal civilian employees of the Department of Defense under title 5, United States Code. (6) Transmittal of report to congress.--The Secretary shall transmit to the congressional defense committees the report of the working group under paragraph (5), together with such discussion and recommendations in connection with the report as the Secretary considers appropriate. The Secretary shall publish the report, and any such discussions and recommendations, in the Federal Register at the time of transmittal. (7) Congressional defense committees defined.--In this subsection, the term ``congressional defense committees'' has the meaning given that term in section 101(a)(16) of title 10, United States Code.", "label": 1, "domain": "government", "token_count": 423, "matched_pair_id": "conditionality_00988", "split": "train"}
{"id": "conditionality_train_pos_0093", "text": "such as striking the pleadings, dismissing the suit, or other directives of a nonmonetary nature, or, if warranted for effective deterrence, an order directing payment of a penalty into the court. TITLE IV--LAWSUIT ABUSE REDUCTION SEC. 401. SHORT TITLE. This title may be cited as the ``Lawsuit Abuse Reduction Act''. SEC. 402. ATTORNEY ACCOUNTABILITY. (a) Sanctions Under Rule 11.--Rule 11(c) of the Federal Rules of Civil Procedure is amended-- (1) in paragraph (1), by striking ``may'' and inserting ``shall''; (2) in paragraph (2), by striking ``Rule 5'' and all that follows through ``motion.'' and inserting ``Rule 5.''; and (3) in paragraph (4), by striking ``situated'' and all that follows through the end of the paragraph and inserting ``situated, and to compensate the parties that were injured by such conduct. Subject to the limitations in paragraph (5), the sanction shall consist of an order to pay to the party or parties the amount of the reasonable expenses incurred as a direct result of the violation, including reasonable attorneys' fees and costs. The court may also impose additional appropriate sanctions, such as striking the pleadings, dismissing the suit, or other directives of a nonmonetary nature, or, if warranted for effective deterrence, an order directing payment of a penalty into the court'' ; and (4) by adding at the end the following: ``(7) Appeal.--An attorney has the right to appeal a sanction under this subdivision. While such an appeal is pending, the sanction shall be stayed.''. (b) Rule of Construction for Civil Rights Claims.--Rule 11 of the Federal Rules of Civil Procedure is amended by adding at the end the following: ``(e) Rule of Construction for Civil Rights Claims.--Nothing in subdivisions (a) through (c) of this rule shall be construed to bar or impede the assertion or development of new claims or remedies under Federal, State, or local civil rights law.''. SEC. 403. PREVENTION OF INTERSTATE FORUM-SHOPPING. (a) Generally.--A person may not bring a personal injury claim in the court of a State if the person is not a resident of that State unless all or a substantial part of the acts or omissions giving rise to the claim asserted occurred in that State.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00910", "split": "train"}
{"id": "conditionality_train_pos_0094", "text": "We present the final results from our ultra-deep spectroscopic campaign with FORS2 at the ESO/VLT for the confirmation of z~7 \"z--band dropout\" candidates selected from our VLT/Hawk-I imaging survey over three independent fields. In particular we report on two newly discovered galaxies at redshift ~6.7 in the NTT deep field: both galaxies show a Ly-alpha emission line with rest-frame EWs of the order 15-20 A and luminosities of 2-4 X 10^{42} erg/s. We also present the results of ultra-deep observations of a sample of i-dropout galaxies, from which we set a solid upper limit on the fraction of interlopers. Out of the 20 z-dropouts observed we confirm 5 galaxies at 6.7 < z < 7.1. This is systematically below the expectations drawn on the basis of lower redshift observations: in particular there is a significant lack of objects with intermediate Ly-alpha EWs (between 20 and 55 A). We conclude that the trend for the fraction of Ly-alpha emission in LBGs that is constantly increasing from z~3 to z~6 is most probably reversed from z~6 to z~7. Explaining the observed rapid change in the LAE fraction among the drop-out population with reionization requires a fast evolution of the neutral fraction of hydrogen in the Universe. Assuming that the Universe is completely ionized at z=6 and adopting the semi-analytical models of Dijkstra et al. (2011), we find that our data require a change of the neutral hydrogen fraction of the order Delta chi_{HI} ~ 0.6 in a time Delta z ~ 1, provided that the escape fraction does not increase dramatically over the same redshift interval.", "label": 1, "domain": "academic", "token_count": 372, "matched_pair_id": "conditionality_00353", "split": "train"}
{"id": "conditionality_train_pos_0095", "text": "We carried out extremely sensitive Submillimeter Array (SMA) 340 GHz continuum imaging on two submillimeter galaxies (SMGs): GOODS 850-11 and GOODS 850-13. The observations reach sub-mJy rms sensitivities and, interestingly, resolve both sources into multiple, physically unrelated SMGs. GOODS 850-11 is resolved into two sources at different redshifts. GOODS 850-13 is resolved into three sources, two with different spectroscopic redshifts and one only with a photometric redshift. All the SMA sources have fluxes in the 3-5 mJy range and all are detected at 1.4 GHz. Three of them are detected by Chandra, and one is a previously unknown X-ray SMG. This is the first time that single-dish SMGs are resolved into multiple unrelated sources and also the first time that the SMA has discovered new SMGs. Our results show that identifications of SMGs at any wavelengths other than the submillimeter itself can be misleading, since such identifications usually only pick up one of the real counterparts. Using simulations that mimic our SCUBA and SMA observations, we find that the number of triple systems detected in our SMA survey is much higher than that expected from the current best-determined number counts. We tentatively attribute this to clustering. We also predict that ALMA will find ~1/3 of >5 mJy 850 um SCUBA sources to be multiple systems. Based on our SMA observations and simulations, we suggest that large samples of existing SMGs should be imaged with sensitive interferometric observations, even if the SMGs were previously thought to be securely identified.", "label": 1, "domain": "academic", "token_count": 345, "matched_pair_id": "conditionality_00287", "split": "train"}
{"id": "conditionality_train_pos_0096", "text": "If you head directly south from St. Paul, Minnesota, you'll eventually find yourself in Rochester, home of the world-renowned Mayo Clinic. For more than 100 years, the city and the hospital have been synonymous. And now, a massive economic development project backed by Mayo, the city and the state aims to transform the city of more than 100,000 into a magnet for startups and entrepreneurs in medicine and other fields. Mayo BioBusiness Center Chair Jim Rogers said Rochester’s transformation is already apparent. \"I can count — just about every building has a new business in the last four of five years, it seems,” he said. \"It's incredible what's occurring here.\" In an effort to turn the region into the “Silicon Valley of medicine,” Rogers said change is happening inside the clinic's walls, too. Recently, Mayo lifted policies that blocked employees from owning or holding an executive position with a medical company, and a business accelerator helps employees develop new products. Rogers pointed to a couple of examples: a health records system for the intensive care unit and a less-invasive procedure to treat carpal tunnel syndrome, both products of Mayo's efforts to support innovation. In the Rochester of the future, Rogers said more products like these will be developed in Discovery Square, a downtown tech park where the idea is for Mayo employees, startups and major medical firms to collaborate. \"Gone are the days where a company comes, wants to talk to a few physicians, thinks they have a good idea and they run off and develop a product that doesn't meet the patient need,” Rogers said. “Gone are the days we think we can just do it ourselves. It needs to be partnership.\" Discovery Square is part of a 20-year economic development effort to remake Rochester so Mayo can better compete for patients and top talent. The state, city and Mayo, as well as other private investors, will contribute a total of about $6.5 billion over the life of the project. The effort is also meant to help diversify southeast Minnesota's economy beyond health care. Right now, Mayo is the state's largest employer, with more than 30,000 people in the region on its payroll. But to build its reputation as something more than a medical hub, some believe Rochester's culture needs to change. \"When you have a large medical institution like the Mayo Clinic — a world renowned, top medical institution in the world — you get that way by eliminating risk,” said Jamie Sund", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00555", "split": "train"}
{"id": "conditionality_train_pos_0097", "text": "If you’re baffled by the way the Trump campaign and now administration seems to be able to weather scandal after scandal, Vox has a few answers. The American culture and politics website has put together a video looking at Donald Trump’s campaign manager/counsellor/chief defender Kellyanne Conway and her interview techniques. Host Carlos Maza (who describes the process of interviewing her as “like trying to staple Jell-O to a wall”) interviews former US national debate champion Seth Gannon to breakdown Conway’s superhuman ability to answer questions she has not been asked, and not answer questions she has. They identify four key techniques: First, Conway’s ability to detect an opening in the question that will allow her to take her answer somewhere else. She will mirror a keyword or phrase in the question at the start of her answer, to give the vague impression she’s addressing the question, before veering off onto whatever topic she’d rather discuss. This is so blatant that at one point, Conway actually pauses and winks as it’s happening. Second, as happened with much of the Trump campaign, Conway exploits the understood accord between media and politician; in this case, the natural politeness of an interviewer. She knows if she obfuscates enough times, an interviewer is more likely to move on to the next topic than appear rude. (Side note: would an interview between Conway and Jeremy Paxman ever actually end?) Third, the classic political trick of passing the buck. She has no responsibility for policy and can, in the face of tricky questions on that policy, simply say she doesn’t know. And finally, she can fall back on the fundamental Trump tactic of simply making something up. Her key role since the start of the administration has been massaging Trump statements into more palatable versions of what they are — see her re-invention of his baseless voter fraud claims as concerns around registration. The video is light-hearted, but maddening and faintly ominous, because Conway’s gymnastics and refusal to give any clarity on White House positions has not cost her or the administration their platform. As Maza says “just remember, she’s doing her job — it’s the news shows that keep booking her that are letting you down”. Something to bear in mind as Conway is inevitably trotted out on various news shows explaining the Michael Flynn situation, or whatever the most recent scandal is by the time this goes to print. — Charlie Lewis", "label": 1, "domain": "news", "token_count": 490, "matched_pair_id": "conditionality_00622", "split": "train"}
{"id": "conditionality_train_pos_0098", "text": "We present a framework to obtain photometric redshifts (photo-zs) for gamma-ray burst afterglows. Using multi-band photometry from GROND and Swift/UVOT, photo-zs are derived for five GRBs for which spectroscopic redshifts are not available. We use UV/optical/NIR data and synthetic photometry based on afterglow observations and theory to derive the photometric redshifts of GRBs and their accuracy. Taking into account the afterglow synchrotron emission properties, we investigate the application of photometry to derive redshifts in a theoretical range between z~1 and z~12. The measurement of photo-zs for GRB afterglows provides a quick, robust and reliable determination of the distance scale to the burst, particularly in those cases where spectroscopic observations in the optical/NIR range cannot be obtained. Given a sufficiently bright and mildly reddened afterglow, the relative photo-z accuracy is better than 10% between z=1.5 and z~7 and better than 5% between z=2 and z=6. We detail the approach on 5 sources without spectroscopic redshifts observed with UVOT on-board Swift and/or GROND. The distance scale to those same afterglows is measured to be $z=4.31^{+0.14}_{-0.15}$ for GRB 080825B, $z=2.13^{+0.14}_{-0.20}$ for GRB 080906, $z=3.44^{+0.15}_{-0.32}$ for GRB 081228, $z=2.03^{+0.16}_{-0.14}$ for GRB 081230 and $z=1.28^{+0.16}_{-0.15}$ for GRB 090530. Combining the response from UVOT with ground-based observatories and in particular GROND operating in the optical/NIR wavelength regime, reliable photo-zs can be obtained from z ~ 1.0 out to z ~ 10, and possibly even at higher redshifts in some favorable cases, provided that these GRBs exist, are localized quickly, have sufficiently bright afterglows and are not heavily obscured.", "label": 1, "domain": "academic", "token_count": 469, "matched_pair_id": "conditionality_00278", "split": "train"}
{"id": "conditionality_train_pos_0099", "text": "on a list of 2,746 Cubans who were alleged criminals and could be returned to the island. When the U.S. abandoned the \"wet foot, dry foot\" policy in January, the two nations agreed that the list could be revised to add other Cuban \"marielitos\" who were subject to active deportation orders. Rudy Blanco was 8 when he was brought from the port of Mariel by his parents in 1980. He now has a family and owns a home-remodeling business in Perry, Florida. But because he was convicted of attempting to sell cocaine in 1998, he wasn't allowed to become a U.S. citizen and instead received an order of deportation by mail in 2005. Blanco was allowed to stay as long as he made routine visits to ICE. However, he was arrested on May 9 and is now awaiting deportation. An ICE spokeswoman said only that the agency intends to deport him based on the 2005 order. Blanco's wife, Shelly, said that both Florida Sen. Marco Rubio and the family's congressman, Rep. Neal Dunn, have told her they are trying to gather information on the case. Both men are Republicans. Colorado Gov. John Hickenlooper, a Democrat, pardoned another Cuban immigrant for an armed robbery committed 19 years ago, in an effort to stave off his deportation. Rene Lima-Marin, 38, arrived as a toddler in the boatlift and 20 years later received a deportation order after his conviction. Apart from the Mariel list, Cuba has agreed to review deportations on a case-by-case basis. Fifty-seven Cubans have been deported since October, while 335 were arrested between Jan. 22 and April 29. Susan Eckstein, a sociology professor at Boston University, argues that Cubans' immigration privileges should end to make immigration policy more equitable for all foreign nationals. \"I would be very surprised if Trump changes Obama's policy because it is so consistent with his stance on immigration in general,\" she said.", "label": 1, "domain": "news", "token_count": 416, "matched_pair_id": "conditionality_00512", "split": "train"}
{"id": "conditionality_train_pos_0100", "text": "Recent observational studies have revealed that the Galactic bulge has cylindrical rotation and a steeper vertical metallicity gradient. We adopt two representative models for the bulge formation and thereby investigate whether the two models can explain both the observed cylindrical rotation and vertical metallicity gradient in a self-consistent manner. One is the \"pure disk scenario\" (PDS) in which the bulge is formed from a pure thin stellar disk through spontaneous bar instability. The other is the \"two-component disk scenario\" (TCDS) in which the bulge is formed from a disk composed of thin and thick disks through bar instability. Our numerical simulations show that although PDS can reproduce the cylindrical rotation, it shows a rather flatter vertical metallicity gradient that is inconsistent with observations. The derived flatter metallicity gradient is due to the vertical mixing of stars with different initial metallicities by the stellar bar. This result implies that the bulge can not be simply formed from a pure thin stellar disk. On the other hand, the bulge formed from the two-component disk in TCDS can explain both the observed cylindrical rotation and vertical metallicity gradient of the Galactic bulge reasonably well. In TCDS, more metal-poor stars at higher |z| (vertical distance) which originate from the already dynamically hotter thick disk can not be strongly influenced by vertical mixing of the bar so that they can stay in situ for longer timescales and thus keep the lower metallicity at higher |z|. Consequently, the vertical metallicity gradient of the bulge composed of initially thin and thick disk stars can not be so flattened, even if the gradient of the thin disk can be flattened significantly by the bar in TCDS.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00346", "split": "train"}
{"id": "conditionality_train_pos_0101", "text": "If Carter Phillips’ basketball career continues on the same upward path it has taken in the last year, then opponents of Catawba College are in trouble. Phillips began his senior season at North Surry as a returning All-Conference performer on a team expected to defend its Western Piedmont Athletic Conference title. Then he gunned in 41 points, along with nine rebounds and five assists, in a win over Westchester Country Day on the day after Thanksgiving. The win came in a showcase in front of dozens of talent scouts and college recruiters, and marked the 6’3” guard as a man to watch in the upcoming season. And there was plenty to watch. Phillips displayed an all-around game better than he ever had before. During the course of the season, he had six more games of 30 or more points, averaged 22.9 points and 7.9 rebounds for the season, and won WPAC Player of the Year honors even though his only real rival for the honor was a teammate. He was nominated to the AP All-State team, and ultimately led the Greyhounds all the way to the 2A state championship game. The only thing that Phillips might want to change about his senior season was the ending, when North Surry lost in the finals to Northside-Jacksonville. Still, it was a 27-5 season that featured more success than any Greyhound team had enjoyed since the 1980s. “Going to the state championship game my senior year was the highlight of my time here,” Phillips said. “We had a really good year. It would have been great to win the state championship, but we still had a good year.” It was the final chapter of a journey that began when Phillips and his partner in the North Surry backcourt, Mason Hawks, first teamed up on a youth basketball team. The two, along with fellow senior Kendal Tucker, spent all of the next several years as teammates. All three of them made the North Surry varsity as freshmen. The Hounds won just 10 games that season, but vaulted to 21-5 in their sophomore season, which saw Phillips as the third-leading scorer on the team at 10 points per game. The 2015-16 season saw another 21 wins and another conference title, with Phillips pumping in 15.6 points and leading the team in rebounding at 6.7. He would have been a Player of", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00518", "split": "train"}
{"id": "conditionality_train_pos_0102", "text": "B) Line-of-credit loans.--In guaranteeing business and industry loans, the Secretary shall guarantee line-of-credit loans in accordance with section 316(c). ``(C) Refinancing.-- ``(i) In general.--A business and industry loan may be used by a small business to refinance debt in existence as of the day before the date on which the loan was made or guaranteed, if-- ``(I) the project for which the debt was incurred is viable and will create or save jobs, as determined by the Secretary; and ``(II) as of the date of application for refinancing-- ``(aa) the underlying loan has been current for at least 1 year; and ``(bb) the lender is providing better rates and longer terms than under the original loan. ``(ii) Subordinated owner debt.-- Subordinated owner debt shall not be eligible for inclusion in debt described in clause (i). ``(D) Audit standards.--Notwithstanding any other provision of law, the Secretary-- ``(i) shall not require audited financial statements consistent with generally accepted accounting principles for business and industry loans of less than $1,000,000; and ``(ii) may waive any requirement for audited financial statements consistent with generally accepted accounting principles for business and industry loans of at least $1,000,000. ``(E) Calculation of delinquency rates.--To allow accurate comparison of delinquency rates among Federal agencies, in calculating the delinquency rate for business and industry loans, the Secretary shall use the calculation method used by the Administrator of the Small Business Administration.''. (c) Sense of Congress Relating to the Rural Microentrepreneur Assistance Program.--It is the sense of Congress that in allocating discretionary funds of the Secretary of Agriculture, the Secretary of Agriculture should give priority to the rural microentrepreneur assistance program established under section 379E of the Consolidated Farm and Rural Development Act (7 U.S.C. 2008s). (d) Budgetary Effects.--The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go-Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 485, "matched_pair_id": "conditionality_00872", "split": "train"}
{"id": "conditionality_train_pos_0103", "text": "Aims: We estimate stellar masses of galaxies in the high redshift universe with the intention of determining the influence of newly available Spitzer/IRAC infrared data on the analysis. Based on the results, we probe the mass assembly history of the universe. Methods: We use the GOODS-MUSIC catalog, which provides multiband photometry from the U--filter to the 8 mum Spitzer band for almost 15,000 galaxies with either spectroscopic (for ~7 % of the sample) or photometric redshifts, and apply a standard model fitting technique to estimate stellar masses. We then repeat our calculations with fixed photometric redshifts excluding Spitzer photometry and directly compare the outcomes to look for systematic deviations. Finally we use our results to compute stellar mass functions and mass densities up to redshift z = 5. Results: We find that stellar masses tend to be overestimated on average if further constraining Spitzer data are not included into the analysis. Whilst this trend is small up to intermediate redshifts z < 2.5 and falls within the typical error in mass, the deviation increases strongly for higher redshifts and reaches a maximum of a factor of three at redshift z = 3.5. Thus, up to intermediate redshifts, results for stellar mass density are in good agreement with values taken from literature calculated without additional Spitzer photometry. At higher redshifts, however, we find a systematic trend towards lower mass densities if Spitzer/IRAC data are included.", "label": 1, "domain": "academic", "token_count": 309, "matched_pair_id": "conditionality_00029", "split": "train"}
{"id": "conditionality_train_pos_0104", "text": "Channel polarization is a phenomenon in which a particular recursive encoding induces a set of synthesized channels from many instances of a memoryless channel, such that a fraction of the synthesized channels becomes near perfect for data transmission and the other fraction becomes near useless for this task. Mahdavifar and Vardy have recently exploited this phenomenon to construct codes that achieve the symmetric private capacity for private data transmission over a degraded wiretap channel. In the current paper, we build on their work and demonstrate how to construct quantum wiretap polar codes that achieve the symmetric private capacity of a degraded quantum wiretap channel with a classical eavesdropper. Due to the Schumacher-Westmoreland correspondence between quantum privacy and quantum coherence, we can construct quantum polar codes by operating these quantum wiretap polar codes in superposition, much like Devetak's technique for demonstrating the achievability of the coherent information rate for quantum data transmission. Our scheme achieves the symmetric coherent information rate for quantum channels that are degradable with a classical environment. This condition on the environment may seem restrictive, but we show that many quantum channels satisfy this criterion, including amplitude damping channels, photon-detected jump channels, dephasing channels, erasure channels, and cloning channels. Our quantum polar coding scheme has the desirable properties of being channel-adapted and symmetric capacity-achieving along with having an efficient encoder, but we have not demonstrated that the decoding is efficient. Also, the scheme may require entanglement assistance, but we show that the rate of entanglement consumption vanishes in the limit of large blocklength if the channel is degradable with classical environment.", "label": 1, "domain": "academic", "token_count": 325, "matched_pair_id": "conditionality_00375", "split": "train"}
{"id": "conditionality_train_pos_0105", "text": "such services that would have been made in such fiscal year if such cost limits (as those limits would otherwise be in effect on September 30, 1999) had been reduced by 15 percent; and ``(B) for such cost reporting periods that begin on or after October 1, 2002, a reduction by 15 percent in such cost limits (as so in effect). ``(2) Applicable amount defined.--In paragraph (1) the term `applicable amount' means, with respect to a fiscal year, the following amount: ``(A) For fiscal year 2000, $19,000,000,000. ``(B) For fiscal year 2001, $21,400,000,000. ``(C) For fiscal year 2002, $23,100,000,000.''. (b) Temporary Restoration of Periodic Interim Payment for Home Health Services.--Section 1815(e)(2) of the Social Security Act (42 U.S.C. 1395g(e)(2)) is amended-- (1) in subparagraph (C), by striking ``and'' at the end; (2) by redesignating subparagraph (D) as subparagraph (E); and (3) by inserting after subparagraph (C) the following: ``(D) home health services until the end of the 12-month period following the date that the prospective payment system for such services is implemented under section 1895; and''. SEC. 4. EFFECTIVE DATE. The amendments made by this Act shall take effect as if included in the enactment of the Balanced Budget Act of 1997.", "label": 1, "domain": "government", "token_count": 332, "matched_pair_id": "conditionality_00858", "split": "train"}
{"id": "conditionality_train_pos_0106", "text": "For the second week in a row, Queen Elizabeth II was a no-show at church with a bad cold that forced her to skip the New Year’s Day holiday service, according to the palace. “The Queen does not yet feel ready to attend church as she is still recuperating from a heavy cold,” Buckingham Palace said in a statement Sunday. The Queen also missed the royal family’s traditional Christmas service at St. Mary Magdalene Church on the Sandringham estate due to a cold. That was reportedly the first time in 28 years the Queen did not attend the Christmas service. On New Years Day, he stayed inside again prompting increased concerns about her health. Joe Giddens/AP Photo Princess Anne, the monarch’s daughter, reassured well-wishers who braved the cold, rainy weather Sunday outside the church that the queen was on the mend. Queen Elizabeth was last seen more than two weeks ago to pre-record her annual Christmas message. Her prolonged absence since has heightened speculation and concern about the severity and extent of her illness. The Queen: \"I wish you all a very happy Christmas\" #QueensSpeech pic.twitter.com/KHn3CWD1e4 — The Royal Family (@RoyalFamily) December 25, 2016 Royal sources are saying, however, that the palace is simply being cautious and practical given the cold weather, and that the queen is said to be up and about working inside the warmth of her home. “We’re talking about a 90-year-old woman with a lingering cold,” ABC News contributor on the royal family, Victoria Murphy, said. “She didn’t want to be standing inside a cold church for up to an hour braving that terrible rain and didn’t want to risk getting worse and she was advised by her doctors to not take the risk.” Before Christmas, the Queen and Prince Philip postponed their trip to Sandringham by 24 hours because they were ill. They later elected to take a helicopter instead of boarding the royal train in London as they typically do each year. Prince Philip, who was also suffering from a cold, according to the palace, was well enough to make the traditional walk to church with the rest of the family on Christmas while the queen remained at home. The public will have to wait one more week for a glimpse of their monarch. Her next scheduled public appearance is at church next Sunday, if she's well enough to attend.", "label": 1, "domain": "news", "token_count": 488, "matched_pair_id": "conditionality_00536", "split": "train"}
{"id": "conditionality_train_pos_0107", "text": "We study the additivity property of three multipartite entanglement measures, i.e. the geometric measure of entanglement (GM), the relative entropy of entanglement and the logarithmic global robustness. First, we show the additivity of GM of multipartite states with real and non-negative entries in the computational basis. Many states of experimental and theoretical interests have this property, e.g. Bell diagonal states, maximally correlated generalized Bell diagonal states, generalized Dicke states, the Smolin state, and the generalization of D\\\"{u}r's multipartite bound entangled states. We also prove the additivity of other two measures for some of these examples. Second, we show the non-additivity of GM of all antisymmetric states of three or more parties, and provide a unified explanation of the non-additivity of the three measures of the antisymmetric projector states. In particular, we derive analytical formulae of the three measures of one copy and two copies of the antisymmetric projector states respectively. Third, we show, with a statistical approach, that almost all multipartite pure states with sufficiently large number of parties are nearly maximally entangled with respect to GM and relative entropy of entanglement. However, their GM is not strong additive; what's more surprising, for generic pure states with real entries in the computational basis, GM of one copy and two copies, respectively, are almost equal. Hence, more states may be suitable for universal quantum computation, if measurements can be performed on two copies of the resource states. We also show that almost all multipartite pure states cannot be produced reversibly with the combination multipartite GHZ states under asymptotic LOCC, unless relative entropy of entanglement is non-additive for generic multipartite pure states.", "label": 1, "domain": "academic", "token_count": 360, "matched_pair_id": "conditionality_00198", "split": "train"}
{"id": "conditionality_train_pos_0108", "text": "Stellar kinematics in the external regions of globular clusters can be used to probe the validity of Newton's law in the low acceleration regimes without the complication of non-baryonic dark matter. Indeed, in contrast with what happens when studying galaxies, in globular clusters a systematic deviation of the velocity dispersion profile from the expected Keplerian falloff would provide indication of a breakdown of Newtonian dynamics rather than the existence of dark matter. We perform a detailed analysis of the velocity dispersion in the globular cluster omega Centauri in order to investigate whether it does decrease monotonically with distance as recently claimed by Sollima et al. (2009), or whether it converges toward a constant value as claimed by Scarpa Marconi and Gilmozzi (2003B). We combine measurements from these two works to almost double the data available at large radii, in this way obtaining an improved determination of the velocity dispersion profile in the low acceleration regime. We found the inner region of omega Centauri is clearly rotating, while the rotational velocity tend to vanish, and is consistent with no rotation at all, in the external regions. The cluster velocity dispersion at large radii from the center is found to be sensibly constant. The main conclusion of this work is that strong similarities are emerging between globular clusters and elliptical galaxies, for in both classes of objects the velocity dispersion tends to remain constant at large radii. In the case of galaxies, this is ascribed to the presence of a massive halo of dark matter, something physically unlikely in the case of globular clusters. Such similarity, if confirmed, is best explained by a breakdown of Newtonian dynamics below a critical acceleration.", "label": 1, "domain": "academic", "token_count": 340, "matched_pair_id": "conditionality_00242", "split": "train"}
{"id": "conditionality_train_pos_0109", "text": "Striking regularities are found in the northwestern arm of the M31 galaxy. Star complexes located in this arm are all spaced 1.2 kpc apart and have similar sizes of about 0.6 kpc. Within the same arm region Beck et al. (1989) detected a regular magnetic field, and we found that its wavelength is the spacing between the complexes. In this arm, groups of HII regions lie inside star complexes, which, in turn, are located inside the gas and dust lane. In contrast, the southwestern arm of M31 splits into a gas and dust lane upstream and a dense stellar arm downstream, with HII regions located mostly along the boundary between these components of the arm. The stellar density in the southwestern arm is much higher than in the northwestern arm, and the former is not fragmented into star complexes. The age gradient across this arm have been found in earlier observations. According the classical SDW theory, these drastic differences may be due due to their different pitch angles: about 0 degree for northwestern part of the arm and about 30 degree for the southwestern segment. Data on M31, M51, M74, and some other galaxies suggest that star complexes are mostly located in the arm segments that are not accompanied by a dust lane upstream, i.e. do not host spiral shock wave. The regularities in the distribution of complexes along a density wave spiral arm are most probably due to the development of the Parker-Jeans instability, which builds up star complexes if the initial SFR in the arm is low and, as a sequence, magnetic field is regular along the arm.", "label": 1, "domain": "academic", "token_count": 331, "matched_pair_id": "conditionality_00164", "split": "train"}
{"id": "conditionality_train_pos_0110", "text": "Our work is motivated by the need for impromptu (or \"as-you-go\") deployment of relay nodes (for establishing a packet communication path with a control centre) by fire-men/commandos while operating in an unknown environment. We consider a model, where a deployment operative steps along a random lattice path whose evolution is Markov. At each step, the path can randomly either continue in the same direction or take a turn \"North\" or \"East,\" or come to an end, at which point a data source (e.g., a temperature sensor) has to be placed that will send packets to a control centre at the origin of the path. A decision has to be made at each step whether or not to place a wireless relay node. Assuming that the packet generation rate by the source is very low, and simple link-by-link scheduling, we consider the problem of relay placement so as to minimize the expectation of an end-to-end cost metric (a linear combination of the sum of convex hop costs and the number of relays placed). This impromptu relay placement problem is formulated as a total cost Markov decision process. First, we derive the optimal policy in terms of an optimal placement set and show that this set is characterized by a boundary beyond which it is optimal to place. Next, based on a simpler alternative one-step-look-ahead characterization of the optimal policy, we propose an algorithm which is proved to converge to the optimal placement set in a finite number of steps and which is faster than the traditional value iteration. We show by simulations that the distance based heuristic, usually assumed in the literature, is close to the optimal provided that the threshold distance is carefully chosen.", "label": 1, "domain": "academic", "token_count": 337, "matched_pair_id": "conditionality_00483", "split": "train"}
{"id": "conditionality_train_pos_0111", "text": "connection with exposure to mustard gas or lewisite at such site and such claims were denied; and (2) submit to the appropriate committees of Congress a report on experiments conducted by the Department of Defense during World War II to assess the effects of mustard gas and lewisite on people, which shall include-- (A) a list of each location where such an experiment occurred, including locations investigated and assessed under paragraph (1); (B) the dates of each such experiment; and (C) the number of members of the Armed Forces who were exposed to mustard gas or lewisite in each such experiment. (d) Investigation and Report by Secretary of Veterans Affairs.--Not later than 180 days after the date of the enactment of this Act, the Secretary of Veterans Affairs shall-- (1) investigate and assess-- (A) the actions taken by the Secretary to reach out to individuals who had been exposed to mustard gas or lewisite in the experiments described in subsection (c)(2)(A); and (B) the claims for disability compensation under laws administered by the Secretary that were filed with the Secretary and the percentage of such claims that were denied by the Secretary; and (2) submit to the appropriate committees of Congress-- (A) a report on the findings of the Secretary with respect to the investigations and assessments carried out under paragraph (1); and (B) a comprehensive list of each location where an experiment described in subsection (c)(2)(A) was conducted. (e) Definitions.--In this section: (1) The terms ``active military, naval, or air service'', ``veteran'', and ``World War II'' have the meanings given such terms in section 101 of title 38, United States Code. (2) The term ``appropriate committees of Congress'' means-- (A) the Committee on Veterans' Affairs, the Committee on Armed Services, and the Special Committee on Aging of the Senate; and (B) the Committee on Veterans' Affairs and the Committee on Armed Services of the House of Representatives. (3) The term ``full-body exposure'', with respect to mustard gas or lewisite, has the meaning given that term by the Secretary of Defense.", "label": 1, "domain": "government", "token_count": 447, "matched_pair_id": "conditionality_00981", "split": "train"}
{"id": "conditionality_train_pos_0112", "text": "If you’ve been watching the second series of Victoria, you’ll probably have noticed that the queen’s beloved Lord Melbourne is looking a little peaky. Advertisement Now, it’s no secret that Lord M, played in the ITV drama by Rufus Sewell, retired from public life in his final years, leaving London and politics for his home, Brocket Hall in Hertfordshire. But while dizzy spells and weakness would not necessarily be a cause for concern in the modern age, for the former Prime Minister the symptoms were somewhat more sinister. Below are some details of the ex-politician’s final years – but a word of warning first. If you don’t want any spoilers, avoid reading beyond this rather lovely picture of the man in question… When did Lord Melbourne die? After leaving parliament in August 1841, Melbourne retreated from public life and suffered a stroke 14 months after his exit from politics. Weakened, he led a reclusive existence in the following years although continued to exchange letters with Victoria. He passed away on 24th November 1848, nine years after the queen had begun her reign. How did Lord Melbourne die? Lord Melbourne is reported to have died from the effects of his stroke. A clip from episode three (below) sees the former statesman trembling and the ITV drama also alludes to “weakness on his left side”, both of which would suggest the aftermath of such a condition. An article in the Liverpool Albion, announcing his death, reports: “the noble deceased had been attacked about three weeks or a month since by what was considered a bilious complaint” but that a London doctor went on to inform family members of “his fears that his lordship’s illness would prove fatal”. Melbourne died at his beloved Brockett Hall surrounded by family members including his sister, Lady Palmerston. Was he survived by any family? Lord Melbourne’s wife (who famously ran off with the poet, Lord Byron) had passed away in 1828, shortly followed by the couple’s only son, George Augustus Frederick. Their daughter, who was born premature, had also predeceased Melbourne, so on his death his titles passed on to his brother, Frederick. Did Lord Melbourne really attend the queen’s costume ball in aid of Spitalfields’ silk industry? Advertisement Episode three of the ITV drama sees Rufus Sewell’s beleaguered statesman attend the party dressed as the poet Dante. However, it is not clear", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00689", "split": "train"}
{"id": "conditionality_train_pos_0113", "text": "In this paper we study the wind accretion onto a rotating black hole in the close binary system harboring a young massive star. It is shown that the angular momentum of the accreted stellar wind material is not sufficient for the formation of an accretion disk. On the other hand, in the considered conditions the Blanford-Znajek mechanism can be activated, thus powerful jets can be launched in the direction of the rotation axis of the black hole. Importantly, no observational signatures of accretion, as typically seen from the thermal X-ray emission from the accretion disks, are expected in the suggested scenario. Here, properties of the generated jet are studied numerically in the framework of a 2D general relativity magnetohydrodynamical approach. Due to the accumulation of the magnetic flux at the black hole horizon, the jet power is expected to be modulated on a sub-second time-scale. Although the intervals between jet active phases depend on the magnetic flux escape from the black hole horizon (which can be modeled self-consistently only using a 3D code), a general estimate of the averaged jet power is obtained. It is expected that for the black hole rotation, expected in stellar binary system (the dimensionless rotation parameter a=0.5), approximately 10% of the accreted rest energy can be channeled into the jets. In the specific case of the gamma-ray binary system LS 5039, the obtained jet luminosity can be responsible for the observed GeV radiation if one invokes Doppler boosting, which can enhanced the apparent flux from the system.", "label": 1, "domain": "academic", "token_count": 327, "matched_pair_id": "conditionality_00377", "split": "train"}
{"id": "conditionality_train_pos_0114", "text": "Come January, LiAngelo Ball and LaMelo Ball will be off to Prienai, a town of about 10,000 people in southern Lithuania, to begin their respective careers as professional basketball players in Europe. The next set of circumstances for LaVar Ball’s youngest boys will be anything but glamorous, up to and including Prienai Arena, where they will play for Prienu Vytautas under head coach Virginijus Šeškus, who’s regarded by some as “the LaVar Ball of Lithuania.” Ben Brust, who played briefly in Lithuania following his four-year stint at the University of Wisconsin-Madison, passed along a less-than-impressive photo of the gym that Gelo and Melo will soon call home. The Ball’s to Lithuania is a disaster waiting to happen (I played there for a year and hated it). This is a picture of the teams gym that the Ball brothers would play at. Not exactly BIG BALLER material #BBB pic.twitter.com/STkQ57YRS5 — Ben Brust (@BenBrust) December 11, 2017 ESPN’s Adrian Wojnarowski, Jonathan Givony and Mike Schmitz added these details about the arena’s seating arrangements: The club plays in a 1,700-seat arena; 500 of those seats are reserved for team sponsors and their friends. Tickets cost around 5 euro. There’s no word yet as to how many more will need to be set aside for LaVar and his Big Baller Brand entourage. The good news is, it won’t cost them much to get in the building if the cash-strapped club can’t afford to comp them.", "label": 1, "domain": "news", "token_count": 342, "matched_pair_id": "conditionality_00514", "split": "train"}
{"id": "conditionality_train_pos_0115", "text": "As Reben told Engadget, \"the discourse around such a(n) apparatus is more important than its physical presence.\" For this project he chose to use Google Assistant, but said it could have been an Amazon Echo \"or some other input device as well.\" At the same time, the device triggered \"could have been a back massaging chair or an ice cream maker.\" But Reben chose to arm Assistant with a gun. And given the concerns raised by Google's Duplex AI since I/O earlier this month, as well as the seemingly never-ending mass shootings in America, his decision is astute. In this example, Reben was the one who told Assistant to \"activate gun.\" He is still the person responsible for the action. But in a world where machine learning has led to AI that's smart enough to anticipate our needs and cater to our comfort every day, it's not hard to imagine a day when digital assistants could kill off people who upset us, if given access to weapons. Who is responsible for the deaths then? It's easy enough to say that we should block AI access to dangerous devices. But we've already got them in our cars, in the military and in other places we probably haven't even thought about. We can demand companies make sure that their tech cannot cause harm, but it's simply impossible to plan for every eventuality, every possible way that AI might go rogue. \"Part of the message for me includes the unintended consequences of technology and the futility of considering every use case,\" Reben said. Google might not ever have imagined Assistant being used to shoot a weapon. But all it took for Reben to achieve that was parts laying around his studio. He used a control relay that usually turns on a lamp, linked it to a Google Home speaker, then connected a laundromat change-dispensing solenoid to pull a string that looped around the trigger. \"The setup was very easy,\" Reben said. He's no stranger to artwork featuring the abilities of artificial intelligence. Reben has created projects that show what AI hears and sees when exposed to \"The Joy of Painting,\" as well as hiding tiny artworks in URLs. This, however is an even more provocative piece that forces the viewer to imagine what could happen if nefarious programmers made an AI that went rogue. Now, more than ever, we need to have the discussions about how, and if, we can prevent an intelligent machine from killing us all.", "label": 1, "domain": "news", "token_count": 499, "matched_pair_id": "conditionality_00624", "split": "train"}
{"id": "conditionality_train_pos_0116", "text": "ISO, aperture, AV, TV, huh? That doesn’t looks like a TV to me. Oh what do they all mean! Which way do I twizzle this knob? Oh blinzkis! I can see only black. Oh right, the lens cap is still on. If that all sounds like a typical conversation every time you're handed a DSLR then the 800D might just be the answer. Canon's long had an app which offers users tips and tutorials to help them master photography, but it’s not always convenient to whip out your phone, fire up the app and start tapping in your ISO questions as the sun goes down. Especially when you're trying to hold a camera at the same time. The solution, according to Canon, is take the best bits from the app and put them in the camera itself, then call the whole thing the User Guide Mode. The 800D defaults to this mode, meaning that you’ll be shown handy tips on the screen as you shoot. It's a trick that Nikon has also tried in its entry-level cams, and while we don't need that kind of help ourselves, obviously, we can see how beginners might find it incredibly reassuring in use. Canon's version of it certainly looked impressive in our brief time with the camera. The instructions are clear, with plenty of simple graphics to help illustrate the points, and don't get bogged down too much in jargon. How useful they are will depend on your current level of expertise, but if you already know it all then maybe the 800D isn't the camera for you anyway.", "label": 1, "domain": "news", "token_count": 324, "matched_pair_id": "conditionality_00692", "split": "train"}
{"id": "conditionality_train_pos_0117", "text": "If one piece had to be picked to encapsulate the latest exhibition from artist Leang Seckon, it would be his work titled “Dead and Reborn Again.” Last year, the head of a pre-Angkorian statue of the Hindu deity Harihara—a fusion of Vishnu and Shiva—which had been in a French museum since the late 19th century, was sent to the National Museum in Phnom Penh to be reunited with its body, found in the 20th century, and identified in the 2010s as belonging to the head. “Harihara is a special god protecting the land,” Mr. Seckon said in an interview. Having the statue’s head and body reunited was, he said, “like a butterfly born out of the worm, Cambodia coming out of darkness.” In his painting, the statue’s head floats in the clouds with its body on the left and a whole statue on the right. This series of vast frescoes and small collages took Mr. Seckon two-and-a-half years to complete. Real and mythical people are mixed and melded, reflecting events and realities but also age-old symbols and beliefs that Cambodians may rarely discuss but which are part of their very fabric. He produced 32 works for the new show, “When Head and Body Unite,” which goes on display at the Rossi & Rossi gallery in Hong Kong next month. Done in his signature style, each work is multilayered. The large ones—some of which would fill a wall—are done on canvas and fabric with acrylic paint, collages and pieces of leather cut as finely as embroidery. The colors are warm and muted gold, soft blues and grays. Smaller collages consist of layers of painted images mixed with photographs and illustrations collected over months of research. Each one speaks of a chapter of the country’s recent history. From the “Golden Era” of the refugee camps in Thailand in the 1980s, it also includes the country’s leading figures in the early 1990s such as King Norodom Sihanouk, Prince Norodom Ranariddh and Prime Minister Hun Sen. Every work carries references well-known to Cambodians and also very personal to the artist. In “Gold Silt Creative Person,” a man stretches his arms above his head as he looks in a mirror in which his reflection shows the head of the mythical snake, naga, while his shadow is", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00623", "split": "train"}
{"id": "conditionality_train_pos_0118", "text": "If you want to keep the price on your new smartphone low, the ZTE Axon 7 has been our most recommended smartphone for $400, just edging out the OnePlus 3 in many circumstances. The OnePlus 3T costs a little more, but it’s worth it. However, the OnePlus 3T now costs more than the magic $400, and if that’s all you want to spend, the Axon 7 is the choice to make. Buyers in the U.K. may want to investigate the Honor 8 Pro, which combines a great camera with good software and other strong features, for 480 British pounds. However, all this applies to someone wanting to buy a new smartphone right this minute. The OnePlus 3T is nearly six months into its lifespan, and rumors are flying about a sequel in the near future. If you buy one, be prepared to see it replaced before the end of the summer. How long will it last? The OnePlus 3T isn’t a rugged phone, and misses out on any water resistance, so you’ll have to be careful with it if you want it to last. It should be worth it, though, because the processor is still one of the fastest out there, which enables OnePlus 3T owners to keep up with gaming and app trends, ensuring their phone will handle the best software for some time to come. Our midnight black OnePlus 3T has Android 7.1.1 Nougat installed with the March 1 Android Security Patch, so it’s nearly up to date. OnePlus has shaken up its software department recently, and promised more timely software updates in the future. The updates come to an end with Android O, but the device will continue to receive security updates. Should you buy it? Yes. The OnePlus 3T is a ridiculously good value smartphone, without any of the drawbacks you’d expect from anything labeled as “good value.” It’s beautiful to look at, great to use, takes impressive pictures, and is technically capable enough to give years of service. All for $440? Just buy one. Update: Android O will be the last major update for OnePlus 3 and 3T", "label": 1, "domain": "news", "token_count": 444, "matched_pair_id": "conditionality_00713", "split": "train"}
{"id": "conditionality_train_pos_0119", "text": "term ``principal investigator'' has the meaning given the term in section 487(a)(30)(D), as added by section 2. SEC. 4. REPORTING REQUIREMENTS FOR CERTAIN FEDERAL DEPARTMENTS AND AGENCIES. Section 1105(a)(40) of title 31, United States Code, is amended by adding at the end the following new paragraph: ``(40) in the case of a Federal department or agency authorized to award research and development grants on a competitive basis-- ``(A) the number of reports received under section 487(a)(30) of the Higher Education Act of 1965 (20 U.S.C. 1094(a)(30)), as added by the Federal Funding Accountability for Sexual Harassers Act, and disaggregated by reports received under subparagraph (A) and by reports received under subparagraph (B) of such section; and ``(B) the number of cases in which the department or agency recommended awarding such a grant for which the principal investigator (as defined in section 3(b) of the Federal Funding Accountability for Sexual Harassers Act) was an individual on which a report under section 487(a)(30)(A) of the Higher Education Act of 1965 (20 U.S.C. 1094(a)(30)(A)) had been filed during the preceding fiscal year.''. SEC. 5. STUDY AND REPORT. The Secretary of Education shall enter into a contract with the National Academy of Sciences under which the National Academy of Sciences shall-- (1) conduct a comprehensive study on the prevalence and impact of sexual harassment in higher education in science, engineering, and medical departments and programs, which shall include an evaluation of, and strategies to, address the legislative, administrative, educational, and cultural barriers to reducing the negative impacts of such sexual harassment; and (2) not later than 3 years after the date of enactment of this Act, submit to the Secretary of Education and make public a report on the results of such study, including-- (A) an evaluation of the impact of sexual harassment on the academic careers of scientists, engineers, and health care professionals; (B) a review of current institutional procedures for preventing sexual harassment with an assessment of their efficacy, with comparisons to international programs and procedures if relevant; and (C) recommendations for evidence-based strategies and policies that can reduce or eliminate sexual harassment.", "label": 1, "domain": "government", "token_count": 486, "matched_pair_id": "conditionality_00948", "split": "train"}
{"id": "conditionality_train_pos_0120", "text": "X-ray observations of unabsorbed active galactic nuclei provide an opportunity to explore the innermost regions of supermassive black hole accretion discs. Our goal in this paper is to investigate the central environment of a Seyfert 1.5 galaxy IRAS 05078+1626. We studied the time-averaged spectrum obtained with the EPIC and RGS instruments. A power-law continuum (photon index ~ 1.75) dominates the 2-10 keV energy range. A narrow iron K alpha spectral line is clearly seen, presumably originating in a distant torus, but no broad relativistic component was detected. However, the power law and the iron K alpha line alone do not provide a satisfactory fit in the soft X-ray band whose spectrum can be explained by the combination of three components: a) a cold photoelectric absorber with column density ~ 10^(21) cm^(-2). This gas could be located either in outer parts of the accretion disc, at the rim of the torus or farther out in the host galaxy; b) a warm absorber with high ionization parameter (log(xi) ~ 2.2) and column density ~ 10^(24) cm^(-2); c) an ionized reflection where the reflecting gas could be either in the inner wall of a warm absorber cone or in an ionized accretion disc. The first X-ray spectroscopic measurement of IRAS05078+1626 unveils some of the standard ingredients in Seyfert galaxies, such as a power-law primary continuum, modified by reflection from the accretion disc and by the effect of complex, multi-phase obscuration. However, data constrains the accretion disc, if present, not to extend closer than to 60 gravitational radii from the black hole.", "label": 1, "domain": "academic", "token_count": 377, "matched_pair_id": "conditionality_00185", "split": "train"}
{"id": "conditionality_train_pos_0121", "text": "she, too, was raped. It was dark when the men finally left. F managed to wriggle her wrists free of the rope and ran into a field. In the morning, she returned to search for her mother, but she had vanished. She saw at least five women lying dead on the ground, their throats cut. She has no idea what has become of her husband. And she cannot imagine returning to her homeland. “We’ve had enough torture,” she says. —— SHE DOES NOT KNOW IF HER HUSBAND IS ALIVE S was lying in bed with her husband and son after dinner in late August when around 10 soldiers burst into the house. A few took her husband outside. Five stayed behind, and one pointed his gun at her. She tried to run, but they grabbed her and kicked her back, stomach and chest. They stripped off her clothes and took her necklace and earrings. Three men raped her. Her young son began to cry. A soldier pointed his gun at the child and he screamed louder. S was in agony. After the men were finished, they took her outside, naked. Her son followed them. About two dozen other women, also naked, had been dragged outside as well. The soldiers forced the women to march toward a rice paddy, beating and kicking them as they walked. S felt blood running down her legs. Once they arrived, the men ordered them to lie down. S fought back and soldiers kicked her. She fell to the ground. Three more soldiers began to rape her. When at last the assault was over, S fled back toward her house with her son, only to find her home had been burned along with many others. She does not know if her husband is alive.", "label": 1, "domain": "news", "token_count": 354, "matched_pair_id": "conditionality_00657", "split": "train"}
{"id": "conditionality_train_pos_0122", "text": "We explore a simple model for the high luminosity of SN 2006gy involving photon diffusion of shock-deposited thermal energy. The distinguishing property of the model is that the large ``stellar'' radius of 160 AU required to prevent adiabatic losses is not the true stellar radius, but rather, the radius of an opaque, unbound circumstellar envelope, created when 10 Msun was ejected in the decade before the supernova in an eruption analogous to that of eta Carinae. The supernova light is produced primarily by diffusion of thermal energy following the passage of the blast wave through this shell. This model differs from traditional models of supernova debris interacting with external CSM in that here the shell is optically thick and the escape of radiation is delayed. We show that any model attempting to account for SN2006gy's huge luminosity with radiation emitted by ongoing CSM interaction fails for the following basic reason: the CSM density required to achieve the observed luminosity makes the same circumstellar envelope opaque, forcing a thermal diffusion solution. In our model, the weaker CSM interaction giving rise to SN2006gy's characteristic Type IIn spectrum and soft X-rays is not linked to the power source of the visual continuum; instead, it arises after the blast wave breaks free of the opaque shell into the surrounding wind. While a simple diffusion model can explain the gross properties of the early light curve of SN2006gy, it predicts that the light curve must plummet rapidly at late-times, unless an additional power source is present.", "label": 1, "domain": "academic", "token_count": 312, "matched_pair_id": "conditionality_00025", "split": "train"}
{"id": "conditionality_train_pos_0123", "text": "The frequency of heating events in the corona is an important constraint on the coronal heating mechanisms. Observations indicate that the intensities and velocities measured in active region cores are effectively steady, suggesting that heating events occur rapidly enough to keep high temperature active region loops close to equilibrium. In this paper, we couple observations of Active Region 10955 made with XRT and EIS on \\textit{Hinode} to test a simple steady heating model. First we calculate the differential emission measure of the apex region of the loops in the active region core. We find the DEM to be broad and peaked around 3\\,MK. We then determine the densities in the corresponding footpoint regions. Using potential field extrapolations to approximate the loop lengths and the density-sensitive line ratios to infer the magnitude of the heating, we build a steady heating model for the active region core and find that we can match the general properties of the observed DEM for the temperature range of 6.3 $<$ Log T $<$ 6.7. This model, for the first time, accounts for the base pressure, loop length, and distribution of apex temperatures of the core loops. We find that the density-sensitive spectral line intensities and the bulk of the hot emission in the active region core are consistent with steady heating. We also find, however, that the steady heating model cannot address the emission observed at lower temperatures. This emission may be due to foreground or background structures, or may indicate that the heating in the core is more complicated. Different heating scenarios must be tested to determine if they have the same level of agreement.", "label": 1, "domain": "academic", "token_count": 324, "matched_pair_id": "conditionality_00349", "split": "train"}
{"id": "conditionality_train_pos_0124", "text": "If you want to stick to your New Year's resolutions in 2017, don't dream big, dream reasonable.Instead of trying to lose 100 pounds or become fluent in French in 365 days, having manageable goals and a firm but flexible timeline will help keep your resolutions alive for 2017. Here are reasonable and achievable New Year's resolutions.Perhaps you've been dying to see the Eiffel Tower glowing at night or have always wanted to trek along the Great Wall of China. International travel fantasies are fun to picture but hard to turn into reality with pricey plane fares and hotels rates.Instead of trying to trot the entire globe, take a road trip to a nearby hotspot or fly to a fun, new destination in the U.S. to satisfy your New Year travel bug. You'll be able to explore somewhere new and exciting without significantly impacting your schedule or wallet.Learning a new language can be of great benefit to your personal and professional life but also requires a lot of time and dedication. Lifehacker suggests that people trying to learn a foreign language should set specific priorities and a timeline for their language goals, like knowing how to speak basic phrases at the end of a month. Online tools like Duolingo and Memrise can also keep language learners on track with their goals.It's hard not to watch a cooking show on TV and have dreams of becoming a world class chef. But with consumers spending more money at restaurants than they do at grocery stores, according to Bloomberg, fewer people are strengthening their cooking skills at home.Treat yourself to a new cookbook and then commit to trying out new recipes on a daily or weekly basis. You can also sign up for cooking classes at a community center to learn about food in a group setting.The most popular New Year's resolution in 2016 was staying fit and healthy according to Nielsen, and 2017 is almost certain to shape up the same way. Set realistic goals and commit to a regular fitness activity that you enjoy. Find a workout buddy to help motivate you and keep you on track and reward yourself when you hit milestone achievements.People love to read, with nearly eight in 10 Americans having read a book in the past year, according to the Pew Research Center. But with so many book options available in digital and print, tackling all of the year's great literary offerings can be a difficult and time-consuming task.If you want to increase your literary diet in 2017, try finishing a new book every month. If you", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00520", "split": "train"}
{"id": "conditionality_train_pos_0125", "text": "We present CaII K and TiII optical spectra of early-type stars taken mainly from the UVES Paranal Observatory Project, plus HI 21-cm spectra from the Vila-Elisa and Leiden-Dwingeloo surveys, which are employed to obtain distances to intermediate and high velocity clouds. HI emission at a velocity of -117 km/s towards the sightline HD 30677 with NHI=1.7x10^19 cm-2 has no corresponding CaII K absorption, which has a signal-to-noise (S/N) ratio of 610. The star has a spectroscopically determined distance of 2.7-kpc, and hence sets this as a firm lower distance limit towards Anti-Centre cloud ACII. Towards another sightline (HD 46185), HI at +122 km/s and NHI=1.2x10^19 cm-2 is seen. The CaII K spectrum has a S/N = 780, although no absorption is observed at the cloud velocity. This similarly places a firm lower distance limit of 2.9-kpc towards this parcel of gas that may be an intermediate velocity cloud. The lack of intermediate velocity (IV) CaII K absorption towards HD 196426 at a S/N = 500 reinforces a lower distance limit of 700-pc towards this part of Complex gp, where NHI is 1.1x10^19 cm-2 and velocity is +78 km/s. Additionally, no IV CaII K is seen in absorption in the spectrum of HD 19445, which is strong in HI with NHI=8x10^19 cm-2 at -42 km/s, placing a firm although uninteresting lower distance limit of 39-pc to this part of IV South. Finally, no HV CaII K absorption is seen towards HD 115363 at a S/N = 410, placing a lower distance of 3.2-kpc towards the HVC gas at velocity of +224 km/s and NHI=5.2x10^19 cm-2. This gas is in the same region of the sky as complex WE (Wakker 2001), but at higher velocities. The non-detection of CaII K absorption sets a lower distance of 3.2-kpc towards the HVC, which is unsurprising if this feature is indeed related to the Magellanic System.", "label": 1, "domain": "academic", "token_count": 494, "matched_pair_id": "conditionality_00002", "split": "train"}
{"id": "conditionality_train_pos_0126", "text": ",\" he said. The Brookers - who are also launching a surfing products brand to help fund more field work - have also been joined on the project by a neighbouring cafe owner and friend, Jane Fallows. She has left her daughter to run the family business while she works on the scientific side of the trial. Image caption Jane Fallows and Simon and Collin Brooker before they headed out Jane, who once worked in medical research, will be involved in gathering the data and liaising with scientists in Wales and then joining the trial to work with conservationists and oceanographers. \"I'm interested in the science side, the conservation side, and also gathering all the facts together from the experts there and using that to do the research,\" she said. \"All the field testing will be done off shore, we'll take a boat out, baiting the water and waiting for sharks to come in and then administering the chemical into the water,\" said Simon. Collin added: \"We need to look at coastal protection but it's not only protecting the humans, it's protecting the sharks.\" Image copyright Collin Brooker Image caption They have been in South Africa since the summer Image copyright Collin Brooker Image caption The Brookers hope they will be able to offer something as part of an overall conservation solution The Brookers said sharks were very much part of the eco-system, but where they have been culled, fish populations have grown out of control, which can in turn damage reefs. \"For hundreds of years fishermen have learnt to trawl a dead shark on their nets to keep sharks away- but we're commercialising that,\" said Collin. \"It's putting it into everyday use but by not using a dead shark anymore but a synthetic re-creation of that.\" Image copyright Collin Brooker The Brookers have recently started their first sea trials, which they said brought \"encouraging\" first results with one of the active ingredients. A tiny dose cleared a sea area of three shark species for five minutes, while other fish were unaffected. Eventually, if all goes to plan, the aim is to develop the device for manufacture back in south Wales, with an eye on the surfing and diving market in other parts of the world, if it takes off.", "label": 1, "domain": "news", "token_count": 456, "matched_pair_id": "conditionality_00801", "split": "train"}
{"id": "conditionality_train_pos_0127", "text": "If the seed magnetic fields exist in the early Universe, tensor components of their anisotropic stresses are not compensated prior to neutrino decoupling and the tensor metric perturbations generated from them survive passively. Consequently, due to the decay of these metric perturbations after recombination, the so-called integrated Sachs-Wolfe effect, the large-scale fluctuations of CMB radiation are significantly boosted. This kind of CMB anisotropy is called the \"tensor passive mode.\" Because these fluctuations deviate largely from the Gaussian statistics due to the quadratic dependence on the strength of the Gaussian magnetic field, not only the power spectrum but also the higher-order correlations have reasonable signals. With these motives, we compute the CMB bispectrum induced by this mode. When the magnetic spectrum obeys a nearly scale-invariant shape, we obtain an estimation of a typical value of the normalized reduced bispectrum as $\\ell_1(\\ell_1 + 1)\\ell_3(\\ell_3+1)|b_{\\ell_1\\ell_2\\ell_3}| \\sim (130-6) \\times 10^{-16} (B_{1 \\rm Mpc} / 4.7 {\\rm nG})^6$ depending on the energy scale of the magnetic field production from $10^{14}$GeV to $10^3$GeV. Here, $B_{1 {\\rm Mpc}}$ is the strength of the primordial magnetic field smoothed on $1 {\\rm Mpc}$. From the above estimation and the current observational constraint on the primordial non-Gaussianity, we get a rough constraint on the magnetic field strength as $B_{1 {\\rm Mpc}} < 2.6 - 4.4 {\\rm nG}$.", "label": 1, "domain": "academic", "token_count": 364, "matched_pair_id": "conditionality_00316", "split": "train"}
{"id": "conditionality_train_pos_0128", "text": "difference, Chaudhuri said, is that instead of calling for Medicaid to cover more people, the lawmakers propose funding more school psychologists and counselors. Included in their proposal is a way for courts to use \"extreme risk protection orders\" to temporarily remove guns from people who are deemed a danger to themselves or others. Rep. Marcia Morey, a former Durham judge, presented such orders as a step beyond domestic violence protective orders. Anyone with direct personal knowledge can ask the court to remove a gun from someone who exhibits threatening, dangerous behavior, she said, while due process rights are preserved. Their proposal would also require background checks before purchase of semi-automatic weapons such as an AR-15 from a private seller, as is already the case for people who buy handguns. Democrats are getting out ahead of a House school safety committee Republican House Speaker Tim Moore organized, which will have its first meeting this week. Republican co-chairmen of the school safety committee have promised to hear all ideas, but early on, Moore dismissed \"the gun debate\" as \"a discussion for another time.\" F. Paul Valone, president of the gun-rights group Grassroots NC, called the Democrats' proposal \"an attempt to incrementally end the private ownership of firearms.\" The proposed age restriction is a ploy to stunt the appreciation for the Second Amendment among people younger than 21, he said. And the extreme risk protection laws enacted in other states limit due process because judges can make decisions without all parties present, Valone said. \"Any of these proposals, if they come out of the General Assembly, we will vociferously oppose them by all possible means,\" Valone said. Grassroots NC tracks legislators' votes and sends out 150,000 voter guides, he said. Democrats called on the school safety committee to consider their bill. Chaudhuri said Democrats would file it even if the safety committee doesn't support it.", "label": 1, "domain": "news", "token_count": 386, "matched_pair_id": "conditionality_00782", "split": "train"}
{"id": "conditionality_train_pos_0129", "text": "We study the ground state entanglement, energy and fidelities of a two-electron system bounded by a core-shell potential, where the core width is varied continuously until it eventually vanishes. This simple system displays a rich and complex behavior: as the core width is varied, this system is characterized by two peculiar transitions where, for different reasons, it displays characteristics similar to a few-particle quantum phase transition. The first occurrence corresponds to something akin to a second order quantum phase transition, while the second transition is marked by a discontinuity, with respect to the driving parameter, in the first derivatives of quantities like energy and entanglement. The study of this system allows to shed light on the sudden variation of entanglement and energy observed in S. Abdullah et al. [Phys. Rev. B 80, 235302 (2009)]. We also compare the core-shell system with a system where a core well is absent: this shows that, even when extremely narrow, the core well has a relevant `pinning' effect. Interestingly, depending on the potential symmetry, the pinning of the wavefunction may either halve or double the system entanglement (with respect to the no-core-well system) when the ground state is already bounded to the outer (shell) well. In the process we discuss the system fidelity and show the usefulness of considering the particle density fidelity as opposed to the more commonly used -- but much more difficult to access -- wavefunction fidelity. In particular we demonstrate that -- for ground-states with nodeless spatial wavefunctions -- the particle density fidelity is zero if and only if the wavefunction fidelity is zero.", "label": 1, "domain": "academic", "token_count": 333, "matched_pair_id": "conditionality_00408", "split": "train"}
{"id": "conditionality_train_pos_0130", "text": "This fun, fluffy doc lacks guts, grit and integrity Film | by Jorge Ignacio Castillo Always at The Carlyle Studio 7 Opens July 6 Real-Life Goldfinger Donald Trump can call it “a joke” all he wants, but The Carlyle really is one of New York’s most legendary hotels. The grand old establishment is known for its classy art deco design, impressive clientele (from Jack Nicholson to the Duke and Duchess of Cambridge) and, above all, a fierce code of silence. Never mind the staff’s refusal to gossip: the documentary Always At The Carlyle has stories for days. The hosts may refuse to blab but the guests are happy to. Some of the events that took place in the hotel are the stuff of legend: Marilyn Monroe’s killer rendition of “Happy Birthday”; Paul Newman’s experiments with vinaigrette; an elevator ride including Princess Diana, Michael Jackson and Steve Jobs. And that’s just what we know. More than following a cinematic structure, the film focuses on the hotel’s most popular areas one at the time: the ridiculously expensive rooms, the Bemelmans Bar and the mythical Café Carlyle. The tone is relentlessly positive, so much so, it feels a bit like a 90-minute long infomercial. Clearly the hotel wouldn’t have been as accommodating otherwise. I have two major problems with Always At The Carlyle. As fascinating as the New York landmark is, the film feels like a celebration of the rich and famous, even though the staff (the majority of whom are immigrants) have more compelling stories than any A-listers. Of all people, Harrison Ford comes the closest to hitting the nail on the head by pointing out the irrationality of paying $1,100 a night for an hotel room. The second issue is the decision of the film’s producers to excise a Woody Allen interview. As problematic as the filmmaker may be, Woody is one of the most recognizable mainstays of the Carlyle (he’s played clarinet every Monday at the Café for decades), and a couple of passing references just don’t cut it. Of all genres, a documentary needs the courage of its convictions — even a fluffier doc like this. Regardless of my misgivings over the film I’ll be damned if I wouldn’t stay at The Carlyle given an opportunity.", "label": 1, "domain": "news", "token_count": 473, "matched_pair_id": "conditionality_00649", "split": "train"}
{"id": "conditionality_train_pos_0131", "text": "if every country puts a break on emissions that exists today, climate change will still have an impact on the world we live in today.” Obama made the connection between climate change and changes with food production and consumption across the globe. Seeds and Chips, the organization hosting the summit intended to highlight global food innovation, focuses on revolutionary ways to produce food. The organization seeks to change the ways in which food is produced, processed, distributed, communicated and consumed, according to its website. “The good news is that because of the work of many of you, the innovations you are already investing in, we’re starting to see a better way to feed a growing planet, combat hunger and malnutrition, put healthy food on the table, save our environment, and none of this is impossible,” Obama told the crowd. Barack Obama attends the Seeds and Chips - Global Food Innovation summit DANIEL DAL ZENNARO / EPA Although he never mentioned Trump by name, Obama acknowledged the current president is leading the country in a different direction when it comes to the planet warming. Despite the differences between the two presidents, Obama was optimistic that he laid the groundwork to help the United States eventually reduce emissions. “Obviously, the current administration has differences with my administration in terms of energy policy, and that’s part of what happens in democracy,” Obama said. “The good news is, in part because of what we did over the last eight years, the private sector has already made a determination that our future is in clean energy.” Claudio Lavanga reported from Milan, Kalhan Rosenblatt from New York.", "label": 1, "domain": "news", "token_count": 318, "matched_pair_id": "conditionality_00754", "split": "train"}
{"id": "conditionality_train_pos_0132", "text": ". (h) Regulatory Authority.--The President shall issue such regulations, licenses, and orders as are necessary to carry out this section. (i) Identification of Sanctionable Foreign Persons.--The Assistant Secretary of State for Democracy, Human Rights, and Labor, in consultation with the Assistant Secretary of State for Consular Affairs and other bureaus of the Department of State, as appropriate, is authorized to submit to the Secretary of State, for review and consideration, the names of foreign persons who may meet the criteria described in subsection (a). (j) Appropriate Congressional Committees Defined.--In this section, the term ``appropriate congressional committees'' means-- (1) the Committee on Banking, Housing, and Urban Affairs and the Committee on Foreign Relations of the Senate; and (2) the Committee on Financial Services and the Committee on Foreign Affairs of the House of Representatives. SEC. 4. REPORTS TO CONGRESS. (a) In General.--The President shall submit to the appropriate congressional committees, in accordance with subsection (b), a report that includes-- (1) a list of each foreign person with respect to which the President imposed sanctions pursuant to section 3 during the year preceding the submission of the report; (2) a description of the type of sanctions imposed with respect to each such person; (3) the number of foreign persons with respect to which the President-- (A) imposed sanctions under section 3(a) during that year; and (B) terminated sanctions under section 3(g) during that year; (4) the dates on which such sanctions were imposed or terminated, as the case may be; (5) the reasons for imposing or terminating such sanctions; and (6) a description of the efforts of the President to encourage the governments of other countries to impose sanctions that are similar to the sanctions authorized by section 3. (b) Dates for Submission.-- (1) Initial report.--The President shall submit the initial report under subsection (a) not later than 120 days after the date of the enactment of this Act. (2) Subsequent reports.-- (A) In general.--The President shall submit a subsequent report under subsection (a) on December 10, or the first day thereafter on which both Houses of Congress are in session, of-- (i) the calendar year in which the initial report is submitted if the initial report is submitted before December 10 of that calendar year; and (ii) each calendar year thereafter.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00849", "split": "train"}
{"id": "conditionality_train_pos_0133", "text": "The radius of neutron stars can in principle be measured via the normalisation of a blackbody fitted to the X-ray spectrum during thermonuclear (type-I) X-ray bursts, although few previous studies have addressed the reliability of such measurements. Here we examine the apparent radius in a homogeneous sample of long, mixed H/He bursts from the low-mass X-ray binaries GS 1826-24 and KS 1731-26. The measured blackbody normalisation (proportional to the emitting area) in these bursts is constant over a period of up to 60s in the burst tail, even though the flux (blackbody temperature) decreased by a factor of 60-75% (30-40%). The typical rms variation in the mean normalisation from burst to burst was 3-5%, although a variation of 17% was found between bursts observed from GS 1826-24 in two epochs. A comparison of the time-resolved spectroscopic measurements during bursts from the two epochs shows that the normalisation evolves consistently through the burst rise and peak, but subsequently increases further in the earlier epoch bursts. The elevated normalisation values may arise from a change in the anisotropy of the burst emission, or alternatively variations in the spectral correction factor, f_c, of order 10%. Since burst samples observed from systems other than GS 1826-24 are more heterogeneous, we expect that systematic uncertainties of at least 10% are likely to apply generally to measurements of neutron-star radii, unless the effects described here can be corrected for.", "label": 1, "domain": "academic", "token_count": 318, "matched_pair_id": "conditionality_00403", "split": "train"}
{"id": "conditionality_train_pos_0134", "text": "Share Bikes featuring a retro-styling seem to be all the rage these days, with even high-tech ebikes cashing in on the trend. Now, Schwinn has taken the throwback design aesthetic one step further by introducing the new Classic Cruiser, an indoor exercise machine that looks like something straight out of the 1950s, but is packed full of modern technology. At first glance, the Classic Cruiser looks like a vintage bike that had its rear tire removed. It features a bold, bright-red paint job, wide fenders, and a thick tire, along with a classic spring-loaded seat like those commonly found on traditional beach cruisers. It even has a traditional dial speedometer to let riders know how fast they are pedaling and a matching workout timer, along with a retro gear switch mounted on the handlebars within easy reach of the rider’s thumb. But when you look a bit deeper the Classic Cruiser’s tech elements begin to show. For instance, its seven-speed drive system uses electromagnetic resistance and is reportedly whisper quiet, something that is much appreciated when riding indoors. The bike even tracks speed, time, distance, and calories burned, all of which can be shared to the Schwinn Classic Cruiser smartphone app, available for both iOS and Android. That same app comes with a built-in feature that allows riders to pedal their way around a virtual 1950s town, avoiding obstacles while also delivering papers. Technology is such an important part of the Classic Cruiser that the exercise bike actually ships with a media shelf built to securely hold a tablet. The bike is also compatible with the RideSocial app (iOS/Android), which gives users even more virtual environments to explore, including cycling routes through Death Valley, Sequoia National Park, and Tibet. Other handy features include preprogrammed workouts to help riders achieve their fitness goals and compatibility with popular cycling apps, such as Zwift, for sharing exercise metrics. The Classic Cruiser even comes with built-in wheels to help move it around more easily. Available now and priced at $800, the Schwinn Classic Cruiser delivers a lot of bang for the buck, particularly if you appreciate its vintage looks.", "label": 1, "domain": "news", "token_count": 433, "matched_pair_id": "conditionality_00716", "split": "train"}
{"id": "conditionality_train_pos_0135", "text": "We characterize the changes in the longitudinal photospheric magnetic field during 38 X-class and 39 M-class flares within $65^{\\circ}$ of disk-center using 1-minute GONG magnetograms. In all 77 cases we identify at least one site in the flaring active region where clear, permanent, stepwise field changes occurred. The median duration of the field changes was about 15 minutes and was approximately equal for X-class and for M-class flares. The absolute values of the field changes ranged from the detection limit of $\\sim\\!\\!10$~G to as high as $\\sim\\!\\!450$~G in two exceptional cases. The median value was 69~G. Field changes were significantly stronger for X-class than for M-class flares and for limb flares than for disk-center flares. Longitudinal field changes less than 100~G tended to decrease longitudinal field strengths, both close to disk-center and close to the limb, while field changes greater than 100~G showed no such pattern. Likewise, longitudinal flux strengths tended to decrease during flares. Flux changes, particularly net flux changes near disk-center, correlated better than local field changes with GOES peak X-ray flux. The strongest longitudinal field and flux changes occurred in flares observed close to the limb. We estimate the change of Lorentz force associated with each flare and find that this is large enough in some cases to power seismic waves. We find that longitudinal field decreases would likely outnumber increases at all parts of the solar disk within $65^{\\circ}$ of disk-center, as in our observations, if photospheric field tilts increase during flares as predicted by Hudson et al.", "label": 1, "domain": "academic", "token_count": 346, "matched_pair_id": "conditionality_00260", "split": "train"}
{"id": "conditionality_train_pos_0136", "text": "Unemployment Insurance Act, as added by section 2006 of the Assistance for Unemployed Workers and Struggling Families Act (Public Law 111-5; 123 Stat. 445), is amended-- (1) in clause (iii)-- (A) by striking ``June 30, 2009'' and inserting ``June 30, 2010''; (B) by striking ``December 31, 2009'' and inserting ``December 31, 2010''; and (2) by adding at the end of clause (iv) the following: ``In addition to the amount appropriated by the preceding sentence, out of any funds in the Treasury not otherwise appropriated, there are appropriated $175,000,000 to cover the cost of additional extended unemployment benefits provided under this subparagraph, to remain available until expended.''. (b) Administrative Expenses.--Section 2006(b) of the Assistance for Unemployed Workers and Struggling Families Act (Public Law 111-5; 123 Stat. 445) is amended by adding at the end the following: ``In addition to funds appropriated by the preceding sentence, out of any funds in the Treasury not otherwise appropriated, there are appropriated to the Railroad Retirement Board $807,000 to cover the administrative expenses associated with the payment of additional extended unemployment benefits under section 2(c)(2)(D) of the Railroad Unemployment Insurance Act, to remain available until expended.''. (c) Effective Date.--The amendments made by this section shall take effect as if included in the enactment of the Assistance for Unemployed Workers and Struggling Families Act.", "label": 1, "domain": "government", "token_count": 328, "matched_pair_id": "conditionality_01054", "split": "train"}
{"id": "conditionality_train_pos_0137", "text": "A $t$-ruling set of a graph $G = (V, E)$ is a vertex-subset $S \\subseteq V$ that is independent and satisfies the property that every vertex $v \\in V$ is at a distance of at most $t$ from some vertex in $S$. A \\textit{maximal independent set (MIS)} is a 1-ruling set. The problem of computing an MIS on a network is a fundamental problem in distributed algorithms and the fastest algorithm for this problem is the $O(\\log n)$-round algorithm due to Luby (SICOMP 1986) and Alon et al. (J. Algorithms 1986) from more than 25 years ago. Since then the problem has resisted all efforts to yield to a sub-logarithmic algorithm. There has been recent progress on this problem, most importantly an $O(\\log \\Delta \\cdot \\sqrt{\\log n})$-round algorithm on graphs with $n$ vertices and maximum degree $\\Delta$, due to Barenboim et al. (Barenboim, Elkin, Pettie, and Schneider, April 2012, arxiv 1202.1983; to appear FOCS 2012). We approach the MIS problem from a different angle and ask if O(1)-ruling sets can be computed much more efficiently than an MIS? As an answer to this question, we show how to compute a 2-ruling set of an $n$-vertex graph in $O((\\log n)^{3/4})$ rounds. We also show that the above result can be improved for special classes of graphs such as graphs with high girth, trees, and graphs of bounded arboricity. Our main technique involves randomized sparsification that rapidly reduces the graph degree while ensuring that every deleted vertex is close to some vertex that remains. This technique may have further applications in other contexts, e.g., in designing sub-logarithmic distributed approximation algorithms. Our results raise intriguing questions about how quickly an MIS (or 1-ruling sets) can be computed, given that 2-ruling sets can be computed in sub-logarithmic rounds.", "label": 1, "domain": "academic", "token_count": 453, "matched_pair_id": "conditionality_00477", "split": "train"}
{"id": "conditionality_train_pos_0138", "text": "if other issues arise on the club, you know maybe left field is an opportunity for either one of them,’’ Cashman said. “We’ll find out over time. Clearly right field and DH work, but I think they’re athletic enough to be considered elsewhere. But the very easiest aspect of it is right field and DH, and I think both players will benefit from the DH rest. You won’t have to run somebody into the ground every day.’’ Stanton, last season’s NL MVP, has been the DH in 13 games and was enthused about the role. “I’m fine with it. I can bounce around. Wherever they need me I’m OK with that. I always liked DHing when we played the AL teams in previous years,’’ said Stanton, who has hit.333 with a 1.019 OPS in 54 at-bats as a DH. Cashman called Judge, who is a better right fielder than Stanton, before making the deal to see how the 2017 AL Rookie of the Year felt about the possibility of shifting between right, DH and possibly left. “We’re going to do everything we can to win and that’s going to make it easier in that matter,’’ Cashman said of Judge’s answer. “He said, ‘Hey, I’m pumped. This is exciting. If you could pull that off, that would be amazing.’ I didn’t talk about who we would be giving up, so he didn’t know that aspect.’’ In 11 games (10 starts) at DH, Judge has hit.294 with a 1.114 OPS in 34 at-bats. When a team has a 28-year-old and owes him $265 million for a decade, it makes sense he plays where he is comfortable, but, at least in December, the Yankees aren’t set on Stanton in right and Judge the DH full time. “We’re going to juggle it. Those are things that we’ll flesh out in spring training. Who do we believe potentially would move over to play left field in a 20-, 30-game situation. Use the DH role strategically, play different matchups that give certain guys days off depending upon the matchups,’’ new manager Aaron Boone said. “So I do feel like it’s a really good problem that we have.’’ As for Judge, Stanton and Sanchez, all right-handed hitters, batting in a row, Boone said it can be done. “Absolutely you can", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00809", "split": "train"}
{"id": "conditionality_train_pos_0139", "text": "If THIS baseball offseason gets any uglier, we might yearn for the good faith and honest dealings of Capitol Hill. Spring-training boycotts? Collusion accusations? Good grief. Ever see an implosion before? The Players Association is laying the dynamite around itself as we speak. This historically slow free-agent market reached a boiling point of sorts Friday, when Brodie Van Wagenen, one of the game’s most accomplished and respected player representatives, published a statement on Twitter that threatened a mass spurning of spring training “if behavior doesn’t change” and noted team owners’ behavior “feels coordinated, rightly or wrongly.” “There is a rising tide among players for radical change,” Van Wagenen wrote. “A fight is brewing.” A second player representative, Joshua Kusnick, backed up Van Wagenen with a tweet of his own: “[It] has certainly felt like an external force has held things up.” What in the name of Marvin Miller is going on here? What gets accomplished by this saber-rattling? First of all, don’t bet your house, or even a roll of toilet paper in your house, on a spring-training boycott, which would represent a historically outrageous violation of the collective bargaining agreement. Suffice it to say not every agent — and hence not every player — is on board with this anger. So let’s shrug off the imminent threat and pivot to the animosity, fueled further by pace-of-play negotiations, which could pose a long-term headache. Any unionized industry functions best when both sides are run competently, and baseball’s routine work stoppages of the 1970s, ’80s and ’90s can be attributed 99 percent to the stick-in-the-mud owners who wanted to destroy the Players Association rather than welcome it as a partner. Now, with Van Wagenen writing of a player population “uniting in a way that has not been seen since 1994,” the ineptitude has swung 180 degrees. It is the union that signed off on the CBA that rewarded tanking and penalized clubs that spent too much. As veteran Oakland outfielder/first baseman Brandon Moss told the MLB Network this past week: “Sooner or later, you have to take responsibility for a system you created for yourself. It’s our fault.” MLB, with that reality in mind, opted not to comment in response to Friday’s Jerry Maguire-esque outbursts. Tony Clark", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00827", "split": "train"}
{"id": "conditionality_train_pos_0140", "text": "Given a Banach space $X$, for $n\\in \\mathbb N$ and $p\\in (1,\\infty)$ we investigate the smallest constant $\\mathfrak P\\in (0,\\infty)$ for which every $f_1,...,f_n:{-1,1}^n\\to X$ satisfy \\int_{{-1,1}^n}\\Bigg|\\sum_{j=1}^n \\partial_jf_j(\\varepsilon)\\Bigg|^pd\\mu(\\varepsilon) \\leq \\mathfrak{P}^p\\int_{{-1,1}^n}\\int_{{-1,1}^n}\\Bigg\\|\\sum_{j=1}^n \\d_j\\Delta f_j(\\varepsilon)\\Bigg\\|^pd\\mu(\\varepsilon) d\\mu(\\delta), where $\\mu$ is the uniform probability measure on the discrete hypercube ${-1,1}^n$ and ${\\partial_j}_{j=1}^n$ and $\\Delta=\\sum_{j=1}^n\\partial_j$ are the hypercube partial derivatives and the hypercube Laplacian, respectively. Denoting this constant by $\\mathfrak{P}_p^n(X)$, we show that $\\mathfrak{P}_p^n(X)\\le \\sum_{k=1}^{n}\\frac{1}{k}$ for every Banach space $(X,|\\cdot|)$. This extends the classical Pisier inequality, which corresponds to the special case $f_j=\\Delta^{-1}\\partial_j f$ for some $f:{-1,1}^n\\to X$. We show that $\\sup_{n\\in \\N}\\mathfrak{P}_p^n(X)<\\infty$ if either the dual $X^*$ is a $\\mathrm{UMD}^+$ Banach space, or for some $\\theta\\in (0,1)$ we have $X=[H,Y]_\\theta$, where $H$ is a Hilbert space and $Y$ is an arbitrary Banach space. It follows that $\\sup_{n\\in \\N}\\mathfrak{P}_p^n(X)<\\infty$ if $X$ is a Banach lattice of finite cotype.", "label": 1, "domain": "academic", "token_count": 494, "matched_pair_id": "conditionality_00482", "split": "train"}
{"id": "conditionality_train_pos_0141", "text": "If the presence of a gravitational field breaks the Lorentz symmetry valid for special relativity, an \"absolute motion\" might be detectable. We summarize a scalar theory of gravity with a such \"ether\", which starts from a tentative interpretation of gravity as a pressure force. The theory also admits that our physical standards of space and time are affected by gravitation similarly as they are affected by a uniform motion. General motion is governed by an extension of Newton's second law to the curved space-time which is thus obtained. Together with the scalar field equation of the theory, this leads to a true conservation equation for the total energy. The law of motion also leads to an alternative 4-component equation governing the dynamics of a continuum in terms of its energy-momentum tensor. That new equation implies that mass conservation is obtained as a limiting behaviour for a weak and slowly varying gravitational field and/or at a low pressure. In the presence of the Lorentz force field, the new dynamical equation gives the second group of the gravitationally-modified Maxwell equations in the investigated theory. This is consistent with the geometrical optics of the theory as governed by the proposed extension of Newton's second law. The theory has the correct Newtonian limit; it predicts Schwarzschild's exterior metric of general relativity and geodesic motion in the static situation with spherical symmetry. A post-Newtonian approximation of this theory shows that no preferred-frame effect occurs for photons at the (first) post-Newtonian approximation. It is argued that the existence of preferred-frame effects in celestial mechanics, comparable in magnitude with the \"relativistic\" effects, does not a priori invalidate the theory.", "label": 1, "domain": "academic", "token_count": 337, "matched_pair_id": "conditionality_00394", "split": "train"}
{"id": "conditionality_train_pos_0142", "text": "If you worry about your privacy, you might be the type to put tape over your webcam, iSight, or FaceTime camera. Perhaps you use an app like Oversight, instead, so you can detect camera activity. There’s actually a way you can disable your Mac’s front-facing camera altogether, and it won’t leave sticky residue on the component. This works on all versions of macOS and OS X. Why Should I Disable My Mac’s Camera? This process isn’t for the average Mac user. Rather, it’s for those who want the privacy of having their cameras turned off. Security professionals, system administrators, and similar folks can benefit from this procedure. A Word of Warning Just to make sure you understand, this is an advanced tip that will fully disable the software components behind your Mac’s front-facing camera. When you follow these steps, you’ll prevent the camera from being used by any of the applications on your Mac. I’ll also show you how to enable the camera again when you need it. If, however, you aren’t comfortable modifying system files using the command line with super user privileges, you should keep going the tape-over-the-lens route. First, Disable System Integrity Protection Introduced in OS X El Capitan, System Integrity Protection, or SIP, is also called rootless mode. It prevents you from modifying certain system-level files and folders. That’s precisely what we need to do to disable the front-facing camera, so let’s disable SIP temporarily. First, back up your Mac, then proceed. Reboot your Mac into Recovery mode, and launch the Terminal from the Utilities menu. Then, issue the following command: csrutil disable Now reboot into normal mode and proceed. We’ll turn SIP back on after we’re done. Completely Disable your FaceTime Camera Now we’ll be able to issue the commands necessary to disable the Mac’s front-facing camera. Open the Terminal app from /Applications/Utilities and issue these command strings, one at a time, into the command line. Enter each command on its own line, even copying and pasting to make sure everything goes right. Terminal will ask for your password for the first one, but remember it after that. sudo chmod a-r /System/Library/Frameworks/CoreMediaIO.framework/Versions/A/Resources/VDC.plugin/Contents/MacOS/VDC sudo chmod a-r /System/Library/PrivateFrameworks/CoreMediaIOServicesPrivate.framework/Versions/A/Resources/AVC.plugin/Contents/MacOS/AVC sudo", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00570", "split": "train"}
{"id": "conditionality_train_pos_0143", "text": "We report a new technique to select 1.6<z<4.6 dusty Lyman-alpha emitters (LAEs), over a third of which are `blobs' (LABs) with emission extended on scales of 30-100kpc. Combining data from the NASA Wide-field Infrared Survey Explorer (WISE) mission with optical spectroscopy from the W.M. Keck telescope, we present a color criteria that yields a 78% success rate in identifying rare, dusty LAEs of which at least 37% are LABs. The objects have a surface density of only ~0.1 per square degree, making them rare enough that they have been largely missed in narrow surveys. We measured spectroscopic redshifts for 92 of these WISE-selected, typically radio-quiet galaxies and find that the LAEs (LABs) have a median redshift of 2.3 (2.5). The WISE photometry coupled with data from Herschel reveals that these galaxies have extreme far-infrared luminosities (L_IR>10^{13-14}L_sun) and warm colors, typically larger than submillimeter-selected galaxies (SMGs) and dust-obscured galaxies (DOGs). These traits are commonly associated with the dust being energized by intense AGN activity. We hypothesize that the combination of spatially extended Lyman-alpha, large amounts of warm IR-luminous dust, and rarity (implying a short-lived phase) can be explained if the galaxies are undergoing strong `feedback' transforming them from an extreme dusty starburst to a QSO.", "label": 1, "domain": "academic", "token_count": 331, "matched_pair_id": "conditionality_00454", "split": "train"}
{"id": "conditionality_train_pos_0144", "text": "health benefits coverage that includes coverage of abortion. SEC. 503. PROHIBITION ON TAX BENEFITS RELATING TO ABORTION. For taxable years beginning after the date of the enactment of this section, no credit shall be allowed under the internal revenue laws with respect to amounts paid or incurred for an abortion or with respect to amounts paid or incurred for a health benefits plan (including premium assistance) that includes coverage of abortion. SEC. 504. CONSTRUCTION RELATING TO SEPARATE COVERAGE. Nothing in this title shall be construed as prohibiting any individual, entity, or State or locality from purchasing separate abortion coverage or health benefits coverage that includes abortion so long as such coverage is paid for entirely using only funds not authorized or appropriated by Federal law and such coverage shall not be purchased using matching funds required for a federally subsidized program, including a State's or locality's contribution of Medicaid matching funds. SEC. 505. CONSTRUCTION RELATING TO THE USE OF NON-FEDERAL FUNDS FOR HEALTH COVERAGE. Nothing in this title shall be construed as restricting the ability of any non-Federal health benefits coverage provider from offering abortion coverage, or the ability of a State or locality to contract separately with such a provider for such coverage, so long as only funds not authorized or appropriated by Federal law are used and such coverage shall not be purchased using matching funds required for a federally subsidized program, including a State's or locality's contribution of Medicaid matching funds. SEC. 506. TREATMENT OF ABORTIONS RELATED TO RAPE, INCEST, OR PRESERVING THE LIFE OF THE MOTHER. The limitations established in this title shall not apply to an abortion-- (1) if the pregnancy is the result of an act of rape or incest; or (2) in the case where a woman suffers from a physical disorder, physical injury, or physical illness that would, as certified by a physician, place the woman in danger of death unless an abortion is performed, including a life-endangering physical condition caused by or arising from the pregnancy itself.", "label": 1, "domain": "government", "token_count": 418, "matched_pair_id": "conditionality_00886", "split": "train"}
{"id": "conditionality_train_pos_0145", "text": "If you're like literally every other phone owner on the planet, you probably need to delete some things off your phone for space. But what are you going to do with all those pictures of the kids, your going out selfies, and pictures of your pets? Don't just delete them - decor with them! Kristina Guerrero is showing you how to turn your pics into works of art with 3 different online apps that do all the hard stuff for you. 1. Keepsake Everyone loves the look of beautifully framed pictures up on a wall. But no one likes running to get pictures printed at Costco and then still go frame shopping. Luckily, there's the Keepsake app. It lets you upload photos straight from your phone, then choose what kind of frame you want the photo in and what you want the frame to look like. Once you make your choices, Keepsake sends your preprinted, pre-framed photos, right to your door - you get great looking decor pieces, without any of the gas mileage! 2. Mixtiles If you love the look of photos on canvases but don't want to pay outrageous prices for a few prints, try Mixtiles. The company makes photo board prints out of your phone's pictures and even gives you the no-damage adhesives you need to put them up. Mixtiles also won't damage your wallet - get a set of 3 prints for $49 and any additional tile is just $9. 3. Chatbooks There is something nostalgic about having a photo album, but making them can be more frustrating than fun. Now, you can reap all the photobook benefits, without all the work, with Chatbooks. The app lets you upload photos from your phone, pick the style of book you'd like, add captions; it even automatically formats the pictures to fit your book. No math required! Put together your own Chatbook for just $8 per book - or get a subscription and create a whole volume of potentially child-embarrassing memories. Do you like to print out your photos or do you prefer to keep them on your phone? Tell us on our Facebook page, @TheListShowTV.", "label": 1, "domain": "news", "token_count": 440, "matched_pair_id": "conditionality_00546", "split": "train"}
{"id": "conditionality_train_pos_0146", "text": "If you could have any superpower, would you decide to be strong, fast or invincible? Given the choice, most of us would aim for the exceptional, stretching the human form toward bigger and better limits. How many among us would choose to go in the opposite direction, to shrink down? Of course, if you were accidentally empowered with the gift to reduce in size, you would find a plethora of useful and even heroic ways to exploit your new talent. But, is it really something any of us dream of becoming? Quite different than the communities of little humanoids (such as The Borrowers or Arthur and the Invisibles ), shrinking down is often treated as disorienting and traumatic in cinema. While it certainly has heroic possibilities, it is usually a signal of a deep spiritual crisis as it relates to the fragility of the human body and soul. With the release of Ant-Man and the Wasp, let’s explore some of film history’s best examples of characters who shrink down: a strange and sometimes beguiling journey through a transformative thread at the movies. 11 Ant-Man Ant-Man is among the most palatable Marvel films, largely due to the lingering fingerprint of director Edgar Wright, who we can only presume was fired from the film for daring to lend it a personality. Paul Rudd might be one of the most charming actors working today, but still, Ant-Man just barely transcends the role of “filler character” in the Marvel universe. Despite this, the film is a rare and somewhat empowering example of celebrating the virtues of going small. 10 Downsizing In Downsizing, a Norwegian scientist presents the irreversible act of “downsizing” as the most effective way to combat climate change. Matt Damon, a hapless pushover impressed by anyone who has ever been on TV, decides to take the plunge – only to be faced with guilt and regret. While on paper, Downsizing’s skewering of Western-centric world-saving ethos is fascinating social commentary, Alexander Payne can’t seem to get his message across without using the white saviour trope. 9 Honey, I Shrunk the Kids Honey, I Shrunk the Kids stars Canadian treasure Rick Moranis, and combines state of the art effects, charming family dynamics and cute animals. This largely harmless franchise toys with power dynamics within the family unit, using the act of shrinking down (or, sometimes, being blown up) as a means of exploring interpersonal relationships. You have to hand it to the Disney", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00658", "split": "train"}
{"id": "conditionality_train_pos_0147", "text": "We provide a comprehensive description and offer an explanation for the sizes of the faintest known galaxies in the universe, the dwarf spheroidal (dSph) satellites of the Milky Way and Andromeda. After compiling a consistent data set of half-light radii (r_{1/2}) and luminosities, we describe the size-luminosity relation of dSphs by a log-normal distribution in r_{1/2} with a mean size that varies as a function of luminosity. Accounting for modest number statistics, measurement uncertainties and surface brightness limitations, we find that the size-luminosity relations of the Milky Way and Andromeda dSph populations are statistically indistinguishable, and also very similar: their mean sizes at a given stellar luminosity differ by no more than 30%. In addition, we find that the mean size, slope and scatter of this log-normal size description of Local Group dSphs matches onto the relation of more massive low-concentration galaxies. This suggests that the stellar sizes of dSphs are ultimately related to their overall initial baryonic angular momentum. To test this hypothesis we perform a series of high resolution N-body simulations that we couple with a semi-analytic model of galaxy formation. These predict the same mean size and slope as observed in dSph satellites. At the same time, these models predict that the size-luminosity distributions for satellite galaxies around similar host-halos must be similar providing a natural explanation as to why the size distributions of Milky Way and Andromeda satellites are similar. Although strong rotation is currently not observed in dSphs, this may well be consistent with our angular-momentum-based explanation for their sizes if the disks of these galaxies have become sufficiently stirred through tidal interaction.", "label": 1, "domain": "academic", "token_count": 361, "matched_pair_id": "conditionality_00350", "split": "train"}
{"id": "conditionality_train_pos_0148", "text": "This study aims at the early diagnostics of geoeffectiveness of coronal mass ejections (CMEs) from quantitative parameters of the accompanying EUV dimming and arcade events. We study events of the 23th solar cycle, in which major non-recurrent geomagnetic storms (GMS) with Dst <-100 nT are sufficiently reliably identified with their solar sources in the central part of the disk. Using the SOHO/EIT 195 A images and MDI magnetograms, we select significant dimming and arcade areas and calculate summarized unsigned magnetic fluxes in these regions at the photospheric level. The high relevance of this eruption parameter is displayed by its pronounced correlation with the Forbush decrease (FD) magnitude, which, unlike GMSs, does not depend on the sign of the Bz component but is determined by global characteristics of ICMEs. Correlations with the same magnetic flux in the solar source region are found for the GMS intensity (at the first step, without taking into account factors determining the Bz component near the Earth), as well as for the temporal intervals between the solar eruptions and the GMS onset and peak times. The larger the magnetic flux, the stronger the FD and GMS intensities are and the shorter the ICME transit time is. The revealed correlations indicate that the main quantitative characteristics of major non-recurrent space weather disturbances are largely determined by measurable parameters of solar eruptions, in particular, by the magnetic flux in dimming areas and arcades, and can be tentatively estimated in advance with a lead time from 1 to 4 days. For GMS intensity, the revealed dependencies allow one to estimate a possible value, which can be expected if the Bz component is negative.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00493", "split": "train"}
{"id": "conditionality_train_pos_0149", "text": "For Klein-Gordon fields, it is well known that there exist an infinite number of nonequivalent Fock representations of the canonical commutation relations and, therefore, of inequivalent quantum theories. A context in which this kind of ambiguities arises and prevents the derivation of robust results is, e.g., in the quantum analysis of cosmological perturbations. In these situations, typically, a suitable scaling of the field by a time dependent function leads to a description in an auxiliary static background, though the nonstationarity still shows up in a time dependent mass. For such a field description, and assuming the compactness of the spatial sections, we recently proved in three or less spatial dimensions that the criteria of a natural implementation of the spatial symmetries and of a unitary time evolution are able to select a unique class of unitarily equivalent vacua, and hence of Fock representations. In this work, we succeed to extend our uniqueness result to the consideration of all possible field descriptions that can be reached by a time dependent canonical transformation which, in particular, involves a scaling of the field by a function of time. This kind of canonical transformations modify the dynamics of the system and introduce a further ambiguity in its quantum description, exceeding the choice of a Fock representation. Remarkably, for any compact spatial manifold in less than four dimensions, we show that our criteria eliminate any possible nontrivial scaling of the field other than that leading to the description in an auxiliary static background. Besides, we show that either no time dependent redefinition of the field momentum is allowed or, if this may happen, the redefinition does not introduce any Fock representation that cannot be obtained by a unitary transformation.", "label": 1, "domain": "academic", "token_count": 342, "matched_pair_id": "conditionality_00420", "split": "train"}
{"id": "conditionality_train_pos_0150", "text": "URAL STATE INITIATIVE. (a) In General.--To address the problem of a significant portion of traffic fatalities occurring on highways in rural areas, the Secretary of Transportation shall, for each fiscal year beginning with fiscal year 2010, allocate $20 million to each State with a population density of less than 20 persons per square mile (based on the most recent decentennial census), for use by such States for projects and programs and activities eligible under 23 U.S.C. 148 and not located in an urbanized area as defined in section 134(b)(6), title 23, United States Code. (b) Such allocations shall not be considered an apportionment within the meaning of section 105 of title 23, United States Code, or considered a ``specific program'' within the meaning of said section 105. (c) Federal Share.--The Federal share of the cost of a project carried out under this section shall be determined in accordance with section 120 of title 23, United States Code. (d) Authorization of Appropriations.--There is authorized to be appropriated out of the Highway Trust Fund (other than the Mass Transit Account) such sums as may be necessary to carry out this section for each of fiscal years 2010 through 2014. (e) Applicability of Title 23.--Except as provided by subsection (b) of this section, funds made available to carry out this section shall be available for obligation in the same manner as if such funds were apportioned under chapter 1 of title 23, United States Code.", "label": 1, "domain": "government", "token_count": 321, "matched_pair_id": "conditionality_00971", "split": "train"}
{"id": "conditionality_train_pos_0151", "text": "If you like the idea of sipping home-made soda or tonic water while chilling out and listening to vinyl records, you'll be in heaven if you pay a visit to JOE. The new lounge bar, on Church Street, in Crystal Palace, makes all of its soft drinks and mixers in-house with flavours varying from week to week based on which fruits are in season. Tempting organic cordials which have featured on the menu since it opened at the end of August include pineapple and mint, fig and cinnamon and blackberry, pear and rose - with all flavours designed to be drunk alone or with a shot of your chosen liqor. A choice of tonic, soda and dandelion and burdock flavours are also available, as well as either filter or cold-brew coffee and tea. \"You can really customise the menu, just like you would for a selection of Spanish tapas,\" explained owner Joe Hirschhorn. \"When I set up here, I wanted to bring the same energy that many new restaurants bring to food to the drinks menu. \"I'd noticed that people tend to sleepwalk into the same pubs after work and have generic drinks, and I wanted to change that. \"I wanted to offer people something that was completely natural without added sugars getting in the way of you enjoying the flavours of the drinks.\" Traditional spirit and mixer combinations like gin and tonic are always available and there are also three cocktails on the menu at any one time - which can be made either with or without alcohol and are served with a glass straw. Previous offerings have included the Canadi-Asian - a mix of cold-brew coffee, maple syrup and coconut milk which can be combined with white rum for an extra kick - and the Copa Verde, which is made with avocado, agave syrup and thyme. \"We don't see them as cocktails - they are creations and they are designed to be drunk either as they are or with a spirit - the white rum really takes the Canadi-Asian to a new level,\" Joe said. \"And everyone who has tasted our gin and tonic has come back for more.\" All of the spirits, wines, ciders and craft beers at the lounge are currently ordered in, but Joe assures customers that they are high-quality and said he has not ruled out the idea of producing them in-house one day. He explained his inspiration for setting up the bar, adding: \"Part of the reason for why we are somewhere in between a", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00702", "split": "train"}
{"id": "conditionality_train_pos_0152", "text": "Medium resolution spectral analysis of candidate Faint High Latitude Carbon (FHLC) stars from Hamburg/ESO survey has given us the potential to discover objects of rare types. Two primary spectral characteristics of R Coroanae Borealis (RCB) stars are hydrogen deficiency and weaker CN bands relative to C_{2} bands. They are also characterized by their characteristic location in the J-H, H-K plane with respect to cool carbon stars. From a spectral analysis of a sample of 243 candidate FHLC stars, we have discovered a hydrogen-deficient carbon (HdC) star HE 1015-2050, at high Galactic latitude. A differential analysis of its spectrum with that of the spectrum of U Aquarii (U Aqr), a well-known cool HdC star of RCB type, provides sufficient evidence to put this object in a group same as that of U Aqr. Further, it is shown that HE 1015-2050 does not belong to any of the C-star groups CH, C-R, C-N or C-J. Cool RCB stars form a group of relatively rare astrophysical objects; approximately 51 are known in the Galaxy and some 18 in the Large Magellanic Clouds (LMC) and five in Small Magellanic Cloud (SMC). The present discovery adds a new member to this rare group. Although its spectral characteristics and its location in the J-H vs H-K plane places HE 1015-2050 in the same group to which U Aqr belongs, extended photometric observations would be useful to learn if there is any sudden decline in brightness, this being a characteristic property of HdC stars of RCB type.", "label": 1, "domain": "academic", "token_count": 346, "matched_pair_id": "conditionality_00270", "split": "train"}
{"id": "conditionality_train_pos_0153", "text": "We review current observational and theoretical constraints on the Galactic chemical evolution (GCE) of oxygen isotopes in order to explore whether GCE plays a role in explaining the lower 17O/18O ratio of the Sun, relative to the present-day interstellar medium, or the existence of distinct 16O-rich and 16O-poor reservoirs in the Solar System. Although the production of both 17O and 18O are related to the metallicity of progenitor stars, 17O is most likely produced in stars that evolve on longer timescales than those that produce 18O. Therefore the 17O/18O ratio need not have remained constant over time, contrary to preconceptions and the simplest models of GCE. An apparent linear, slope-one correlation between delta17O and delta18O in the ISM need not necessarily reflect an O isotopic gradient, and any slope-one galactocentric gradient need not correspond to evolution in time. Instead, increasing 17O/18O is consistent both with observational data from molecular clouds and with modeling of the compositions of presolar grains. Models in which the rate of star formation has decelerated over the past few Gyr or in which an enhanced period of star formation occurred shortly before solar birth (\"starburst\") can explain the solar-ISM O-isotopic difference without requiring a local input of supernova ejecta into the protosolar cloud. \"Cosmic chemical memory\" models in which interstellar dust is on average older than interstellar gas predict that primordial Solar System solids should be 16O-rich, relative to the Sun, in conflict with observations. However, scenarios in which the 16O-rich contribution of very massive stars could lead to 16O-poor solids and a 16O-rich bulk Sun, if the Solar System formed shortly after a starburst, independent of the popular scenario of photochemical self-shielding of CO.", "label": 1, "domain": "academic", "token_count": 393, "matched_pair_id": "conditionality_00484", "split": "train"}
{"id": "conditionality_train_pos_0154", "text": "Image copyright Getty Images Drake has addressed the controversy of a photo of him appearing to be in blackface. The Canadian rapper said it was to highlight and raise frustrations about black actors \"not always getting a fair chance in the industry\". He said it was taken as part of a project while working as an actor - and not for a clothing brand shoot. The 2007 photo resurfaced after Pusha T posted it on his Instagram, along with a track taking aim at Drake. On his Instagram story, the God's Plan rapper said: \"The photos represented how African Americans were once wrongfully portrayed in entertainment.\" He said the photo was from a project that was about \"young black actors struggling to get roles, being stereotyped and type cast\". Previous reports suggested the photos were from a clothing brand shoot but Drake insisted this was wrong. Image copyright Drake/ Instagram Drake said he and his best friend at the time, actor Mazin Elsadig, were \"attempting to use our voice to bring awareness to the issues we dealt with all the time as black actors in auditions\". Pusha T has used the photo to promote The Story of Adidon - the latest in a line of diss tracks between the two rappers. He was responding to Drake's track Duppy Freestyle, which was released on Friday. Follow Newsbeat on Instagram, Facebook and Twitter. Listen to Newsbeat live at 12:45 and 17:45 every weekday on BBC Radio 1 and 1Xtra - if you miss us you can listen back here.", "label": 1, "domain": "news", "token_count": 315, "matched_pair_id": "conditionality_00802", "split": "train"}
{"id": "conditionality_train_pos_0155", "text": "6); (ii) by striking the period at the end of paragraph (7) and inserting ``; and''; and (iii) by adding at the end the following new paragraph: ``(8) in the case of prostate cancer screening services (as defined in section 1861(ll)) (other than prostate-specific antigen tests), the amounts described in section 1834(d)(1).''. (D) Section 1833(h)(1)(A) of such Act (42 U.S.C. 1395l(h)(1)(A)) is amended by striking ``The Secretary'' and inserting ``Subject to section 1834(d), the Secretary''. (E) Section 1861(s)(2)(O) of such Act (42 U.S.C. 1395x(s)(2)(O)) is amended by striking ``(jj)'' and inserting ``(kk)''. (F) Section 1862(a) of such Act (42 U.S.C. 1395y(a)) is amended-- (i) in paragraph (1)-- (I) in subparagraph (E), by striking ``and'' at the end, (II) in subparagraph (F), by striking the semicolon at the end and inserting ``, and'', and (III) by adding at the end the following new subparagraph: ``(G) in the case of prostate cancer screening services (as defined in section 1861(ll)) provided for the purpose of early detection of prostate cancer, which are performed more frequently than is covered under section 1834(d)(2);''; and (ii) in paragraph (7), by striking ``paragraph (1)(B) or under paragraph (1)(F)'' and inserting ``subparagraphs (B), (F), or (G) of paragraph (1)''. (b) Coverage of Certain Drug Treatments.--Section 1861(s)(2) of the Social Security Act (42 U.S.C. 1395x(s)(2)), as amended by subsection (a)(1), is further amended-- (1) by striking ``and'' at the end of subparagraph (Q); (2) by adding ``and'' at the end of subparagraph (R); and (3) by adding at the end the following new subparagraph: ``(S) an oral drug prescribed for the treatment of prostate cancer, if the use of the drug for such purpose is a medically accepted indication under subsection (t)(2);''.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00903", "split": "train"}
{"id": "conditionality_train_pos_0156", "text": "make a two-state solution impossible, and that a one state solution would put the future of the Jewish state in question. Trump has shied away from criticizing Netanyahu’s settlement policies as an impediment to peace, instead offering Israel some scope to build on land already under development. “The construction of new settlements or the expansion of existing settlements beyond their current borders may not be helpful in achieving that goal,” the White House said in a statement earlier this month. Saeb Erakat, a senior Palestinian official, said it was not enough for Trump to say settlements were “unhelpful” but he must order an end to new building. Netanyahu arrived in Washington on Monday, dined with US Secretary of State Rex Tillerson on Tuesday and after his White House talks with Trump on Wednesday will meet lawmakers. Aside from winning support for policies that will help him at home, the Israeli leader will also want to get the measure of Trump’s appetite for better relations with Russia. Trump has signaled his willingness to work with Russia to defeat the Daesh group in Syria. That could de facto mean furthering the goals of Russian allies Bashar Assad and Iran. Israel sees Iran and its Lebanese ally the Hezbollah militia as its greatest existential threat, a view shared by the leaders of the main Sunni Arab states of the region. Dennis Ross, a US diplomat who worked on Middle East policy under both Republican and Democratic administrations, said Netanyahu’s diplomatic goals would at first be modest. Israel wouldn’t oppose a rapprochement with Moscow in itself, but would urge Washington to use this as leverage to push Russia away from Iran. “What he’d like to see is a distancing of Russia from Iran within Syria, maybe more of a move toward Turkey and less toward Iran in Syria,” Ross told reporters on Monday. Trump appears to have back-pedaled on a campaign threat to tear up Obama’s Iran nuclear deal, which Israel bitterly opposed, but his administration has “put Iran on notice.” This appears to mean a more robust stance against military provocations and a determination to impose tough sanctions on Iran’s missile program and covert support for militants. Observers expect Trump and Netanyahu to get on well in public. Both have much to gain politically from marking a clean break from the Obama years. But, personal chemistry aside, the pair will only make the relationship a success if it overcomes the disagreement that poisoned ties under Obama.", "label": 1, "domain": "news", "token_count": 478, "matched_pair_id": "conditionality_00790", "split": "train"}
{"id": "conditionality_train_pos_0157", "text": "or after October 1, 2001, and before October 1, 2002, 50 percent; and ``(iii) with respect to cost reporting periods beginning on or after October 1, 2002, and before October 1, 2003, 25 percent.''. (b) Limit on Reductions Under Balanced Budget Act.--Section 1886(b) of the Social Security Act (42 U.S.C. 1395ww(b)) is amended by adding at the end the following: ``(8)(A) Notwithstanding the amendments made by sections 4411, 4414, 4415, and 4416 of the Balanced Budget Act of 1997, in the case of a psychiatric facility (as defined in subparagraph (B)(ii)), the amount of payment for the operating costs of inpatient hospital services for cost reporting periods beginning on or after October 1, 1998, and before October 1, 2000, shall not be less than 95 percent of the amount that would have been paid for such costs if such amendments did not apply. ``(B) For purposes of this paragraph, the term `psychiatric facility' means-- ``(i) a psychiatric hospital; and ``(ii) a psychiatric unit described in the matter following clause (v) of subsection (d)(1)(B).''. (c) Effective Date.--The amendments made by subsections (a) and (b) shall apply as if included in the enactment of the Balanced Budget Act of 1997.", "label": 1, "domain": "government", "token_count": 314, "matched_pair_id": "conditionality_00855", "split": "train"}
{"id": "conditionality_train_pos_0158", "text": "We present 0.2\" resolution near-infrared integral field spectroscopy of H-alpha emission from six star forming galaxies at z~1.6 (look-back time of ~9.6 Gyr). These observations were obtained with OSIRIS using the Keck Laser Guide Star Adaptive Optics system. All sources have a compact spatial extent of ~1\", with an average half light radius of r=2.9 kpc and average dereddened star formation rate of 22 Msolar per year. Based on H-alpha kinematics we find that these six galaxies are dynamically distinguishable, and we classify them as either merger or disk candidate systems. We find three merger systems (HDF-BX1287, HDF-BX1315, and Q1623-BX491) with varying geometries and dynamical properties. Three galaxies (HDF-BMZ1299, Q2343-BX344, and Q2343-BM145) are well-fit by an inclined-disk model with low velocity residuals (20 to 46 km/sec). An average plateau velocity of v_p=185 km/sec is achieved within 1.0 kpc. The majority of observed velocity dispersions (~88 km/sec) can be explained by the residual seeing halo, and are not intrinsic to our sources. However, one merger and one disk candidate have high velocity dispersions (> 200 km/sec) that cannot be solely explained by beam smearing. For two disk candidates, we detect [NII] emission and are able to map the [NII]/H-alpha ratio on kiloparsec scales. In both cases, [NII] emission is more concentrated than H-alpha emission (< 0.2\"), and peak ratios are best explained by the presence of an AGN. These are among the weakest known AGN at high redshift, however their emission is strong enough to impact high redshift metallicity studies that use nebular ratios. All disk candidates have likely completed only a few orbital periods, and if left unperturbed are excellent candidates to become present-day spiral galaxies.", "label": 1, "domain": "academic", "token_count": 423, "matched_pair_id": "conditionality_00093", "split": "train"}
{"id": "conditionality_train_pos_0159", "text": "A gravity theory called scalar-tensor-vector gravity (STVG) has been recently developed and succeeded in solar system, astrophysical and cosmological scales without dark matter [J. W. Moffat, J. Cosmol. Astropart. Phys. 03, 004 (2006)]. However, two assumptions have been used: (i) $B(r)=A^{-1}(r)$, where $B(r)$ and $A(r)$ are $g_{00}$ and $g_{rr}$ in the Schwarzschild coordinates (static and spherically symmetric); (ii) scalar field $G=Const.$ in the solar system. These two assumptions actually imply that the standard parametrized post-Newtonian parameter $\\gamma=1$. In this paper, we relax these two assumptions and study STVG further by using the post-Newtonian (PN) approximation approach. With abandoning the assumptions, we find $\\gamma\\neq1$ in general cases of STVG. Then, a version of modified STVG (MSTVG) is proposed through introducing a coupling function of scalar field G: $\\theta(G)$. We have derived the metric and equations of motion (EOM) in 1PN for general matter without specific equation of state and $N$ point masses firstly. Subsequently, the secular periastron precession $\\dot{\\omega}$ of binary pulsars in harmonic coordinates is given. After discussing two PPN parameters ($\\gamma$ and $\\beta$) and two Yukawa parameters ($\\alpha$ and $\\lambda$), we use $\\dot{\\omega}$ of four binary pulsars data (PSR B1913+16, PSR B1534+12, PSR J0737-3039 and PSR B2127+11C) to constrain the Yukawa parameters for MSTVG: $\\lambda=(3.97\\pm0.01)\\times10^{8}$m and $\\alpha=(2.40\\pm0.02)\\times10^{-8}$ if we fix $|2\\gamma-\\beta-1|=0$.", "label": 1, "domain": "academic", "token_count": 430, "matched_pair_id": "conditionality_00112", "split": "train"}
{"id": "conditionality_train_pos_0160", "text": "If the city moves forward with an ambitious plan to guide office and housing development in Central SoMa, Pinterest hopes to add a vertical 11-story addition to its headquarters at 505 Brannan St.A proposal filed by TMG Partners, one of the original six-story building developers, includes an 11-story addition that would add 165,000 square feet to the site and bring its height to 240 feet.The current building offers 129,450 square feet in office space and is 85 feet tall, but the site is permitted for a structure 250 feet tall, according to SF Planning documents.The addition is anticipated to cost $38 million.The project will contribute to the city's affordable housing development efforts by paying \"substantial fees to the Jobs-Housing Linkage Program,\" as well as complying with other Central SoMa neighborhood requirements, according to documents TMG filed with SF Planning.According to the city, the current Jobs-Linkage Housing fee for office space is about $26.95/gross square foot, which could add up to more than $4 million for the proposed 165,000-square-foot addition.The project would also generate about $3.4 million in fees to support public transportation, and 1 percent of the project cost would go toward public art on site or elsewhere.The Central SoMa plan, as formally introduced by Acting Mayor Mark Ferrell and District 6 Supervisor and mayoral candidate Jane Kim last month, intends to add 40,000 new jobs and 7,000 associated housing units in the area South of Market and North of Townsend between 2nd and 6th streets.The plan has been crafted over the past six years \"to take advantage of the $1.57 billion Central Subway,\" reports the. At least 33 percent of the housing will be permanently affordable and the new development in the neighborhood is expected to generate nearly half a billion dollars in funding for local and regional transit improvements, according to SF Planning.The housing stock in Eastern SoMa is currently 25 percent single-room occupancy hotels, catering to the lowest income residents in the city.According to the ordinance to be considered by the SF Planning Commission later this month, the plan aims to retain SRO hotels, which primarily serve \"elderly, disabled, and single-person households.\"SF Planning's Historic Preservation Committee is slated to consider legislation adopting the Central SoMa plan on Wednesday, March 21st, and the Planning Commission will get a briefing on the legislative package the following day", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00523", "split": "train"}
{"id": "conditionality_train_pos_0161", "text": "Breaking News Emails Get breaking news alerts and special reports. The news and stories that matter, delivered weekday mornings. SUBSCRIBE The scope of the Facebook data harvesting scandal likely extended far beyond 87 million people, according to a former Cambridge Analytica employee who described how a \"sex compass\" app was used to gather data. Brittany Kaiser, who worked for Cambridge Analytica for almost three years before leaving in January, testified before the United Kingdom's Digital, Culture, Media and Sport Committee in London on Tuesday as part of its investigation into disinformation and fake news, providing fresh information into how the secretive data analysis company operated. In addition to the \"This Is Your Digital Life\" survey developed by Cambridge University researcher Aleksandr Kogan, Kaiser said Cambridge Analytica and its partners used a wide range of surveys to collect information on Facebook users — including a \"sex compass\" app that asked people about their \"personal preferences.\" \"I do not know the specifics of these surveys or how the data was acquired or processed,\" she said. \"But I believe it is almost certain that the number of Facebook users whose data was compromised through routes similar to that used by Kogan is much greater than 87 million, and that both Cambridge Analytica and other unconnected companies and campaigns were involved in these activities.\" When she first joined the company in February 2015, Kaiser said its data science, psychology and creative teams would work together to create surveys in order to get Facebook users to provide access to their accounts. Cambridge Analytica has been under scrutiny after a whistleblower came forward alleging that the firm, which worked on President Donald Trump's campaign, used Facebook data to target U.S. voters based on personality traits. Kaiser said she would tell clients about viral personality quizzes on Facebook and how these applications could be used to harvest information from users who agreed to give the app access to their profiles. It continued to be a part of the company's sales pitch to \"commercial, political and defense clients\" even after Facebook requested that Cambridge Analytica delete the data, she said. Until 2014, Facebook's developer platform allowed connected apps to take almost any data they wanted from a user who authorized their app. The policy was so loose that it even allowed developers to gather some basic information from the profiles of a person's friends — even if those friends had not opted in to sharing their information.", "label": 1, "domain": "news", "token_count": 475, "matched_pair_id": "conditionality_00740", "split": "train"}
{"id": "conditionality_train_pos_0162", "text": "were able to gain access to Lerner Hall — amassing in the lobby and chanting, “If we don’t get no justice, then they don’t get no peace.” Many held up signs saying “Black Lives Matter,” “Dismantle White Supremacy” and “F–k Nazis.” The protesters included students, city residents and members of the anti-fascist movement, or antifa. “Punch a Nazi in the face — every nation every race,” the group chanted. “Racist, sexist, anti-gay — NYPD go away!” Cernovich was one of the biggest supporters of the Pizzagate conspiracy last year, which falsely claimed that leaders in the Democratic party were involved in a child sex trafficking ring that was being run out of a restaurant in Washington. The controversial blogger has tried to disassociate himself from the alt-right movement following the deadly events in Charlottesville — instead dubbing himself a member of the “New Right,” which is a phrase he coined last year. Other right-wing provocateurs, such as Milo Yiannopoulous, have started using the term in the attempt to distance themselves from white nationalists and alt-right leaders like Richard Spencer. Some of the Columbia students that were involved in the Cernovich protests also demonstrated outside the school earlier this month when anti-Islam activist Tommy Robinson, of the UK, was invited to speak by the CUCR. More than two dozen people managed to make it inside the venue and were able to disrupt a portion of his speech. Robinson was ultimately forced to end the event early. Social media users had been hinting that there would be spats of violence at Columbia on Monday night during Cernovich’s speech. In the days leading up to his arrival, school officials warned that anyone who disrupts the event would face disciplinary action. Several people interrupted Cernovich, though it’s unclear if they were students or if they’ll be punished.", "label": 1, "domain": "news", "token_count": 390, "matched_pair_id": "conditionality_00813", "split": "train"}
{"id": "conditionality_train_pos_0163", "text": "We model the expected X-ray polarisation induced by complex reprocessing in the active nucleus of the Seyfert-2 galaxy NGC 1068. Recent analysis of infrared interferometry observations suggests that the ionised outflows ejected by the central engine are not aligned with the symmetry axis of the obscuring torus. This conclusion was obtained by extrapolating the apparent orientation of the narrow line region to the inner parts of the ionisation cones. We show that future measurements of the soft X-ray polarisation vector unambiguously determine the orientation of the ionisation cones. Furthermore, X-ray polarimetry across a broad photon energy range may independently verify the misalignment between the ionisation cones and the axis of the torus. To model the expected polarisation percentage and position angle, we apply the radiative transfer code STOKES. Reprocessing of the primary X-ray radiation takes place in the accretion disc, the surrounding equatorial torus and the inclined, ionised outflows. We also examine additional equatorial scattering occurring in between the accretion disc and the inner surfaces of the torus. Radiative coupling between the different reprocessing components is computed coherently. The resulting polarisation properties depend on the optical depth of the reprocessing regions and on the viewing angle of the observer. We show that even under unfavourable conditions the misalignment of the outflows with respect to the torus axis can be determined from a rotation of the polarisation position angle between softer and harder X-rays. We argue that the misalignment of the outflows with respect to the torus axis in NGC 1068 may be constrained by a future X-ray mission if equipped with a broad band polarimeter.", "label": 1, "domain": "academic", "token_count": 345, "matched_pair_id": "conditionality_00295", "split": "train"}
{"id": "conditionality_train_pos_0164", "text": "if they’re a coach, they can coach however they want. If they’re a fan, they can root for a team that plays the style they like. For us, we love it. This is what gives us our edge.’’ Edge? “Every time we got a catch,’’ Baylor’s Ishmail Wainright said, “there was somebody right there.’’ Which is why South Carolina (25-10) is still here. They hadn’t danced since 2004, hadn’t won an NCAA Tournament game since 1973 and never have played in a Final Four. “It’s a good feeling when we continue to make history and I think once we got a taste of it we kind of got addicted and want to continue doing it,’’ guard Duane Notice said. “So we’re going to do everything in our power to make sure we do that.” The Gamecocks will face Florida in the region final on Sunday. If they play the same frenetic, aggressive, take-no-prisoners defense and attacking offense, there will be a dead Gator on the Garden floor. South Carolina held Baylor scoreless for seven minutes and 44 seconds in the first half, turning a 15-13 deficit into a 31-15 lead. Baylor missed 10 shots, committed four turners and not even two timeouts by coach Scott Drew could stop the onslaught. “We couldn’t, really couldn’t buy a basket,’’ said Johnathan Motley, the only Bear to finish in double figures (18 points). South Carolina’s roster — led by SEC Player of the Year Sindarius Thornwell, who had a game-high 24 points — contains players from Gabon, Australia, Canada, Gabon, Estonia and Senegal. They all speak in one tongue: defense. “It’s the best defensive team I’ve coached in college basketball as a head coach,’’ Martin said. “No doubt.”", "label": 1, "domain": "news", "token_count": 387, "matched_pair_id": "conditionality_00806", "split": "train"}
{"id": "conditionality_train_pos_0165", "text": "quite the paradise they'd imagined. Lara Vogelsberg, 23, from Cologne thinks what you see and what you get are very different. \"The beach in the film is very relaxing, there are no people to be seen, and you get this idea of a very lonely place in the middle of nowhere. \"Then you come here and you think you're in Times Square in New York.\" The beach is stunning but definitely not relaxing. There's the constant sound of the speedboat engines, their propellers churn up the water and it's hard to get a patch of the sand to yourself. The area is generally clean but there are still some pockets of litter which tourists leave behind. Image copyright Getty Images Image caption People love a selfie on Maya Bay Image caption Mel Sukonik and Ariane Benedetto (right) visited for the day with their friends from the US Tourism is one of Thailand's biggest sources of income so Maya Bay is being closed during the relatively low season, until September 30. Its Department of National Parks, Wildlife and Plant Conservation issued a notice saying it realised \"the deterioration of the ecosystem in the area of Maya Bay\". When it reopens later this year, it's thought the number of people allowed to visit the beach will be reduced. Kerri Arnold and Kendal Corgile are visiting from Atlanta, Georgia, and describe it as \"hectic but beautiful\". \"I didn't realise how busy the beach would be but shutting it temporarily is a great idea. It's crazy how many boats there are. I'm just glad I got to see it.\" Follow Newsbeat on Instagram, Facebook and Twitter. Listen to Newsbeat live at 12:45 and 17:45 every weekday on BBC Radio 1 and 1Xtra - if you miss us you can listen back here.", "label": 1, "domain": "news", "token_count": 369, "matched_pair_id": "conditionality_00793", "split": "train"}
{"id": "conditionality_train_pos_0166", "text": "Photon trapping and outflow are two key physics associated with the supercritical accretion flow. We investigate the conflict between these two processes based on two-dimensional radiation-hydrodynamic (RHD) simulation data and construct a simplified (radially) one-dimensional model. Mass loss due to outflow, which is not considered in the slim-disk model, will reduce surface density of the flow, and if very significant, it will totally suppress photon trapping effects. If the photon trapping is very significant, conversely, outflow will be suppressed because radiation pressure force will be reduced. To see what actually occurs, we examine the RHD simulation data and evaluate the accretion rate and outflow rate as functions of radius. We find that the former monotonically decreases, while the latter increases, as the radius decreases. However, the former is kept constant at small radii, inside several Schwarzschild radii, since the outflow is suppressed by the photon trapping effects. To understand the conflict between the photon trapping and outflow in a simpler way, we model the radial distribution of the accretion rate from the simulation data and build up a new (radially) one-dimensional model, which is similar to the slim-disk model but incorporates the mass loss effects due to the outflow. We find that the surface density (and, hence, the optical depth) is much reduced even inside the trapping radius, compared with the case without outflow, whereas the effective temperature distribution hardly changes. That is, the emergent spectra do not sensitively depend on the amount of mass outflow. We conclude that the slim-disk approach is valid for interpreting observations, even if the outflow is taken into account.", "label": 1, "domain": "academic", "token_count": 346, "matched_pair_id": "conditionality_00134", "split": "train"}
{"id": "conditionality_train_pos_0167", "text": "Supernova (SN) rates are potentially powerful diagnostics of metal enrichment and SN physics, particularly in galaxy clusters with their deep, metal-retaining potentials and relatively simple star-formation histories. We have carried out a survey for supernovae (SNe) in galaxy clusters, at a redshift range 0.5<z<0.9, using the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope. We reimaged a sample of 15 clusters that were previously imaged by ACS, thus obtaining two to three epochs per cluster, in which we discovered five likely cluster SNe, six possible cluster SNe Ia, two hostless SN candidates, and several background and foreground events. Keck spectra of the host galaxies were obtained to establish cluster membership. We conducted detailed efficiency simulations, and measured the stellar luminosities of the clusters using Subaru images. We derive a cluster SN rate of 0.35 SNuB +0.17/-0.12 (statistical) \\pm0.13 (classification) \\pm0.01 (systematic) [where SNuB = SNe (100 yr 10^10 L_B_sun)^-1] and 0.112 SNuM +0.055/-0.039 (statistical) \\pm0.042 (classification) \\pm0.005 (systematic) [where SNuM = SNe (100 yr 10^10 M_sun)^-1]. As in previous measurements of cluster SN rates, the uncertainties are dominated by small-number statistics. The SN rate in this redshift bin is consistent with the SN rate in clusters at lower redshifts (to within the uncertainties), and shows that there is, at most, only a slight increase of cluster SN rate with increasing redshift. The low and fairly constant SN Ia rate out to z~1 implies that the bulk of the iron mass in clusters was already in place by z~1. The recently observed doubling of iron abundances in the intracluster medium between z=1 and 0, if real, is likely the result of redistribution of existing iron, rather than new production of iron.", "label": 1, "domain": "academic", "token_count": 444, "matched_pair_id": "conditionality_00240", "split": "train"}
{"id": "conditionality_train_pos_0168", "text": "Transcript for Sen. Cory Booker on bringing America together, running in 2020 And we are back with senator %-pcory bookerwho had something to say. Just a point, we all got to this country in different ways but we're all in the same boat now. And to try to think we're going to demonize each other so bad, we need each other. There's an old saying, if you want to go fast, go alone. If you want to go far, go together. If this country is going to go far, we have to find ways to create common ground and stand together. That message that you're saying is refreshing for me, but then you have Hillary Clinton last week in India saying that she won areas that were, quote, forward thinking. Trump won places that were backward thinking on issues like race and racism. I'm from one of those states she's talking about and I just want to know from you, going forward in 2020 do you think this is an appropriate way for Democrats to speak about Republicans? We in this country -- first of all, the election is over and past and I know that Donald Trump and everyone is talking about Obama and secretary Clinton. The reality is we have to in this coming '18 election -- forget 2020 -- focus on right now. We have to begin to see each other for the truth of who we are. This idea of tolerance that we're going to stomach each other, that's a sin of state. Patriotism is love the country. Love says I see your worth, your value. I understand that my definition of worth is the same as yours. While Donald Trump seems to be intent on separating, dividing, demeaning, degrading, I want Republicans and Democrats to start a new national narrative about how we need each other. Not to pushback on you but Hillary makes me feel that way as well. Do you think this messaging is hurting our party right now? Again, secretary Clinton lost the electoral vote. She's not the president of the United States. My focus is on the future and we right now are in a state of crises. We cannot do the things we all agree upon in this country right now, whether it's dreamers or comprehensive background checks. We need to get back to a country that understands that we're not each other's enemies and if we see each other that way we're not going to be able to rise to our greatest aspirations.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00540", "split": "train"}
{"id": "conditionality_train_pos_0169", "text": "A directed graph is called Eulerian, if it contains a tour that traverses every arc in the graph exactly once. We study the problem of Eulerian extension (EE) where a directed multigraph G and a weight function is given and it is asked whether G can be made Eulerian by adding arcs whose total weight does not exceed a given threshold. This problem is motivated through applications in vehicle routing and flowshop scheduling. However, EE is NP-hard and thus we use the parameterized complexity framework to analyze it. In parameterized complexity, the running time of algorithms is considered not only with respect to input length, but also with respect to other properties of the input - called \"parameters\". Dorn et. al. proved that EE can be solved in O(4^k n^4) time, where k denotes the parameter \"number of arcs that have to be added\". In this thesis, we analyze EE with respect to the (smaller) parameters \"number c of connected components in the input graph\" and \"sum b over indeg(v) - outdeg(v) for all vertices v in the input graph where this value is positive\". We prove that there is an algorithm for EE whose running time is polynomial except for the term 4^(c log(bc^2)). To obtain this result, we make several observations about the sets of arcs that have to be added to the input graph in order to make it Eulerian. We build upon these observations to restate EE in a matching context. This matching formulation of EE might be an important tool to solve the question of whether EE can be solved within running time whose superpolynomial part depends only on c. We also consider polynomial time preprocessing routines for EE and show that these routines cannot yield instances whose size depends polynomially only on either of the parameters b, c, k unless coNP is contained in NP/poly.", "label": 1, "domain": "academic", "token_count": 381, "matched_pair_id": "conditionality_00306", "split": "train"}
{"id": "conditionality_train_pos_0170", "text": "If P \\to X is a topological principal K-bundle and \\hat K a central extension of K by Z, then there is a natural obstruction class \\delta_1(P) in \\check H^2(X,\\uline Z) in sheaf cohomology whose vanishing is equivalent to the existence of a \\hat K-bundle \\hat P over X with P \\cong \\hat P/Z. In this paper we establish a link between homotopy theoretic data and the obstruction class \\delta_1(P) which in many cases can be used to calculate this class in explicit terms. Writing \\partial_d^P \\: \\pi_d(X) \\to \\pi_{d-1}(K) for the connecting maps in the long exact homotopy sequence, two of our main results can be formulated as follows. If Z is a quotient of a contractible group by the discrete group \\Gamma, then the homomorphism \\pi_3(X) \\to \\Gamma induced by \\delta_1(P) \\in \\check H^2(X,\\uline Z) \\cong H^3_{\\rm sing}(X,\\Gamma) coincides with \\partial_2^{\\hat K} \\circ \\partial_3^P and if Z is discrete, then \\delta_1(P) \\in \\check H^2(X,\\uline Z) induces the homomorphism -\\partial_1^{\\hat K} \\circ \\partial_2^P \\: \\pi_2(X) \\to Z. We also obtain some information on obstruction classes defining trivial homomorphisms on homotopy groups.", "label": 1, "domain": "academic", "token_count": 342, "matched_pair_id": "conditionality_00371", "split": "train"}
{"id": "conditionality_train_pos_0171", "text": "If you bought an HP laptop any time in the last five years, it could be tracking your every key stroke. Over the weekend HP revealed that nearly 500 of its notebooks dating as far back as 2012 shipped with a secret keylogger installed. Alongside the announcement, HP released driver updates to eradicate the software on affected laptops. Security researcher Michael Myng discovered the keylogger when probing the Synaptics touchpad software on an HP laptop. HP’s security bulletin says the “potential security vulnerability” affects all laptops with “certain versions of Synaptics touchpad drivers”—not necessarily just HP models. The keylogger is disabled by default, however. “A party would need administrative privileges in order to take advantage of the vulnerability,” the bulletin states. “Neither Synaptics nor HP has access to customer data as a result of this issue.” HP told Myng that the keylogger was a debugging tool. The same security bulletin includes separate software updates for every HP laptop loaded with the keylogger, and HP says you should install those updates “as soon as possible.” CSO counted them all up and found a total of 475 affected laptops, with 303 being consumer laptops. Spectre, Envy, Pavilion, Omen, Compaq—they all contain the keylogger. You’ll need to know your laptop’s model number to download the correct software package. You can find HP laptop model numbers by looking for the information on a sticker on the bottom of the machine. If you don’t see the sticker, you can press Fn + Esc simultaneously to summon HP’s System Information window. You’re looking for the “product name” entry. Once you know it, head to HP’s security bulletin, press Ctrl + F, and type in your laptop’s details to quickly find the correct update for your system. You don’t want to sift through all 475 listings individually to find the right one! This isn’t the first time HP has run into keylogging trouble in 2017. In May, HP patched 30 laptops after a diagnostic update to their audio drivers accidentally resulted in every stroke being captured and saved to a local file. We’re leaving superb systems like the HP Spectre x360 on PCWorld’s list of the best laptops since the actions weren’t nefarious, but here’s hoping the company steps up its software quality assurance going forward.", "label": 1, "domain": "news", "token_count": 479, "matched_pair_id": "conditionality_00530", "split": "train"}
{"id": "conditionality_train_pos_0172", "text": "We model the mineralogy and distribution of dust around the white dwarf G29-39 using the infrared spectrum from 1-35 microns and combining a wide range of materials based on spectral studies of comets and debris disks. In order of their contribution to the mid-infrared emission, the most abundant minerals for G29-38 are amorphous carbon, amorphous and crystalline silicates, water ice, and metal sulfides. The amorphous C can be equivalently replaced by other materials (like metallic Fe) with featureless infrared spectra. The best-fitting crystalline silicate is Fe-rich pyroxene. In order to absorb enough starlight to power the observed emission, the disk must either be much thinner than the stellar radius (so that it can be heated from above and below) or it must have an opening angle wider than 2 degrees. A `moderately optically thick' torus model with mass 2x10^19 g fits the spectrum well. A physically thin (less than the white dwarf radius) and optically thick disk can contribute to the near-infrared continuum only; such a disk cannot explain the longer-wavelength continuum or strong silicate features. The silicate composition contains minerals found from cometary spectra and meteorites, but Fe-rich pyroxene is more abundant than enstatite (Mg-rich pyroxene) or forsterite (Mg-rich olivine) in G29-38, in contrast to what is found in most comet or meteorite mineralogies. Enstatite meteorites may be the most similar solar system materials to the G29-38 dust. Finally, we suggest the surviving core of a `hot jupiter' as an alternative (neither cometary nor asteroidal) origin for the debris, though further theoretical work is needed to determine if this hypothesis is viable.", "label": 1, "domain": "academic", "token_count": 382, "matched_pair_id": "conditionality_00089", "split": "train"}
{"id": "conditionality_train_pos_0173", "text": "if the employer makes an election under clause (i), notwithstanding section 2(3)(G) of the Longshore and Harbor Workers' Compensation Act (33 U.S.C. 902(3)(G)), shall be subject to that Act. ``(B) If an employer makes an election, in accordance with subparagraph (A), to participate in an authorized compensation plan under the Longshore and Harbor Workers' Compensation Act-- ``(i) a master or crew member employed by that employer shall be considered to be an employee for the purposes of that Act; and ``(ii) the liability of that employer under that Act to the master or crew member, or to any person otherwise entitled to recover damages from the employer based on the injury, disability, or death of the master or crew member, shall be exclusive and in lieu of all other liability.''. (b) Minimum Requirements.--All vessels, whether documented in the United States or not, operating in the coastwise trade of the United States shall be subject to minimum international labor standards for seafarers under international agreements in force for the United States, as determined by the Secretary of Transportation on the advice of the Secretaries of Labor and Defense. SEC. 5. REGULATIONS REGARDING VESSELS. (a) Applicable Minimum Requirements.--Except as provided in subsection (b), the minimum requirements for vessels engaging in the transportation of cargo or merchandise in the United States coastwise trade shall be the recognized international standards in force for the United States (as determined by the Secretary of the department in which the Coast Guard is operating, in consultation with any other official of the Federal Government that the Secretary determines to be appropriate). (b) Consistency in Application of Standards.--In any case in which any minimum requirement for vessels referred to in subsection (a) establishes a lower standard than a minimum that is applicable to vessels that are documented in a foreign country and that are admitted to engage in the transportation of cargo and merchandise in the United States coastwise trade, the standard applicable to such vessels that are documented in a foreign country shall be the standard to be applied to United States documented vessels. SEC. 6. ENVIRONMENTAL STANDARDS. All vessels, whether documented under the laws of the United States or not, engaging in the United States coastwise trade shall comply with all applicable United States and international environmental standards in force for the United States. SEC. 7. REQUIREMENTS FOR CERTAIN NONCITIZENS IR", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00882", "split": "train"}
{"id": "conditionality_train_pos_0174", "text": "If you woke up this morning feeling extra dry, you're not alone. Winter is notorious for stripping us of our natural moisture, whether you normally have oily skin, dry skin or even combination. We're all going through a little dry period when it comes to our faces. Whether it's bracing the wintry elements while being outside, or even being stripped of moisture because you have the heat blasting indoors, face it: It's a tough couple of months for moisture. But it's especially important to stay hydrated -- and not just on your body but on your face in particular. So along with naming our favorite face moisturizers under $70, we've also tapped a few beauty bloggers and fashion writers to tell us their favorite finds. Glossier \"Glossier’s Priming Moisturizer Rich ($35) is ballin’ on a budget. It provides a luxe experience from the packaging to the actual product quality itself. Many opt to use this during the winter months (opposed to the brand’s original priming moisturizer during spring/summer) because of its thickness and super hydrating properties, but I use it year-round because it’s that good.\" - Morgan Pitts, representative for Glossier Neutrogena \"Neutrogena Hydro Boost Water Gel ($18.99) goes on smooth and leaves your skin feeling full of moisture without any residue or heavy feel. Because it's more of a gel, it sets right into the skin and leaves it feeling bright and light!\" - Kelly McCarthy, digital reporter at ABC News IT Cosmetics \"IT Cosmetics Secret Sauce Anti-Aging moisturizer ($68) has been my go-to all winter. It works overtime to reduce discoloration, lines, and wrinkles. With key ingredients like anti-aging collagen, peptides, hyaluronic acid, vitamin C and licorice root, the secret really is in the sauce. - Ty Alexander, creator of Gorgeous in Grey Shaffali \"My facialist at HeyDay spa recommended I try Shaffali Organic Orange Blossom Facial Moisture ($48) and I see why. If you have sensitive skin like me, it's great because it's organic and offers vitamin E, vitamin A and vitamin C. Plus, I only have to apply it once a day without it feeling heavy. I use it year-round, but during the winter months, I add one drop of carrot seed oil to make it last just a bit longer. Carrot seed oil also", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00538", "split": "train"}
{"id": "conditionality_train_pos_0175", "text": "IVE OFFICE OF THE PRESIDENT. (a) Establishment.--Section 901(b)(2) of title 31, United States Code, is amended by adding at the end the following: ``(H) The Executive Office of the President.''. (b) Appointment.--The President shall appoint an individual as the Chief Financial Officer of the Executive Office of the President, pursuant to the amendment made by subsection (a), by not later than 90 days after the date of the enactment of this Act. SEC. 5. FINANCIAL MANAGEMENT ACTIVITIES WITHIN EXECUTIVE OFFICE OF THE PRESIDENT. (a) Review of Financial Management Activities Within the Executive Office of the President.--Not later than 30 days after the appointment of a Chief Financial Officer of the Executive Office of the President (in this section referred to as the ``Chief Financial Officer''), the Director of the Office of Management and Budget shall direct the Chief Financial Officer to conduct a review of the financial management activities within the Executive Office of the President for the purpose of consolidating its accounting, budgeting, and other financial management activities under the Chief Financial Officer. (b) Reorganization Proposal.--Not later than 60 days after the date the Director directs the Chief Financial Officer to conduct a review under subsection (a), and subject to all laws vesting functions in particular officers and employees of the United States, the Chief Financial Officer shall submit to the Director of the Office of Management and Budget a proposal for reorganizing the Executive Office of the President for the purpose stated in subsection (a). The proposal shall include-- (1) a description of all functions, powers, duties, personnel, property, or records which the Chief Financial Officer is proposed to have authority over, including those relating to functions that are not related to financial management activities; and (2) a detailed outline of the administrative structure of the office of the Chief Financial Officer, including a description of the responsibility and authority of financial management personnel and resources in agencies or other subdivisions as appropriate for the Executive Office of the President. (c) Review and Approval of Proposal.--Not later than 30 days after receiving a proposal from the Chief Financial Officer under subsection (c), the Director of the Office of Management and Budget shall approve or disapprove the proposal and notify the Chief Financial Officer of that approval or disapproval. The Director shall approve the proposal if it establishes a financial management structure reasonably tailored to the functions of the Executive Office of the President.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01040", "split": "train"}
{"id": "conditionality_train_pos_0176", "text": "If you do your homework, now is the time to practically steal a new sedan from your car dealer. For more than a year, sales of cars have been tanking because Americans have gone nuts over SUVs and trucks. As stockpiles of sedans such as the Chevrolet Malibu and Chrysler 200 stretch across car lots, automakers are forced to offer big discounts to move them. There are a few steps to finding the best bargain, but it boils down to this: Figure out which cars aren't selling, research discounts and don't buy until the end of the month when dealers are more desperate to sell. Brad Korner, general manager of AIS Rebate, an Ann Arbor, Michigan, firm that follows the labyrinth of automaker discounts, equates buying a car cheap with purchasing discounted baked goods. To get the good deal, you have to really look. \"You go into the store and the day-old bakery stuff is on a different shelf,\" he says. Be wary of offers that seem too good to be true, like $69 per month payments. Earl Stewart, a North Palm Beach, Florida, Toyota dealer who is critical of other dealers' sales tactics, advises people to ignore dealer advertising. \"Probably 99 percent of it is misleading,\" he says. The low-price deals often are on stripped-down models that the dealer may not even have. They also can include hefty down payments. But armed with the right information, you can navigate the new car sales maze and get 20 percent or more off a car's sticker price: FIRST: PICK A TARGET, FIND SLOW SELLERS For more than a year, many compact, midsize and large cars, gas-electric hybrids, and many lower-level luxury cars haven't sold well. So dealers have big supplies. Because they're paying interest on the cars, they're eager to sell. So figure out the size of car you want. Then look for automaker monthly sales press releases on the internet and find models with big year-over-year declines. The sales figures are released early in the month. To get the best deal, you can't be too picky about color or equipment because you need to buy what's on dealer lots. SECOND: LOOK FOR DISCOUNTS ONLINE Many websites, including those from the auto companies as well as kbb.com, truecar.com and Edmunds.com, list publicly available discounts called incentives. Say you decide on a midsize car. Sales of the Nissan Alt", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00533", "split": "train"}
{"id": "conditionality_train_pos_0177", "text": "the President, any Federal agency or official thereof, or by a court of competent jurisdiction, in the performance of functions which are transferred under this title, and (2) which are in effect at the time this title takes effect, or were final before the effective date of this title and are to become effective on or after the effective date of this title, shall continue in effect according to their terms until modified, terminated, superseded, set aside, or revoked in accordance with law by the President, the head of the transferee agency or other authorized official, a court of competent jurisdiction, or by operation of law. (b) Proceedings Not Affected.--The provisions of this title shall not affect any proceedings, including notices of proposed rulemaking, or any application for any license, permit, certificate, or financial assistance pending before the transferor agency at the time this title takes effect, with respect to functions transferred by this title but such proceedings and applications shall be continued. Orders shall be issued in such proceedings, appeals shall be taken therefrom, and payments shall be made pursuant to such orders, as if this title had not been enacted, and orders issued in any such proceedings shall continue in effect until modified, terminated, superseded, or revoked by a duly authorized official, by a court of competent jurisdiction, or by operation of law. Nothing in this subsection shall be deemed to prohibit the discontinuance or modification of any such proceeding under the same terms and conditions and to the same extent that such proceeding could have been discontinued or modified if this title had not been enacted. (c) Suits Not Affected.--The provisions of this title shall not affect suits commenced before the effective date of this title, and in all such suits, proceedings shall be had, appeals taken, and judgments rendered in the same manner and with the same effect as if this title had not been enacted. (d) Nonabatement of Actions.--No suit, action, or other proceeding commenced by or against the transferor agency, or by or against any individual in the official capacity of such individual as an officer of the transferor agency, shall abate by reason of the enactment of this title. (e) Administrative Actions Relating to Promulgation of Regulations.--Any administrative action relating to the preparation or promulgation of a regulation by the transferor agency relating to a function transferred under this title may be continued by the transferee agency with the same effect as if this title had not been enacted.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00995", "split": "train"}
{"id": "conditionality_train_pos_0178", "text": "Let $(X,T)$ be a topological dynamical system and $\\mathcal{F}$ be a Furstenberg family (a collection of subsets of $\\mathbb{Z}_+$ with hereditary upward property). A point $x\\in X$ is called an $\\mathcal{F}$-transitive one if $\\{n\\in\\mathbb{Z}_+:\\, T^n x\\in U\\}\\in\\F$ for every nonempty open subset $U$ of $X$; the system $(X,T)$ is called $\\F$-point transitive if there exists some $\\mathcal{F}$-transitive point. In this paper, we aim to classify transitive systems by $\\mathcal{F}$-point transitivity. Among other things, it is shown that $(X,T)$ is a weakly mixing E-system (resp.\\@ weakly mixing M-system, HY-system) if and only if it is $\\{\\textrm{D-sets}\\}$-point transitive (resp.\\@ $\\{\\textrm{central sets}\\}$-point transitive, $\\{\\textrm{weakly thick sets}\\}$-point transitive). It is shown that every weakly mixing system is $\\mathcal{F}_{ip}$-point transitive, while we construct an $\\mathcal{F}_{ip}$-point transitive system which is not weakly mixing. As applications, we show that every transitive system with dense small periodic sets is disjoint from every totally minimal system and a system is $\\Delta^*(\\mathcal{F}_{wt})$-transitive if and only if it is weakly disjoint from every P-system.", "label": 1, "domain": "academic", "token_count": 350, "matched_pair_id": "conditionality_00315", "split": "train"}
{"id": "conditionality_train_pos_0179", "text": "Suppose Alice wishes to send messages to Bob through a communication channel C_1, but her transmissions also reach an eavesdropper Eve through another channel C_2. The goal is to design a coding scheme that makes it possible for Alice to communicate both reliably and securely. Reliability is measured in terms of Bob's probability of error in recovering the message, while security is measured in terms of Eve's equivocation ratio. Wyner showed that the situation is characterized by a single constant C_s, called the secrecy capacity, which has the following meaning: for all $\\epsilon > 0$, there exist coding schemes of rate $R \\ge C_s - \\epsilon$ that asymptotically achieve both the reliability and the security objectives. However, his proof of this result is based upon a nonconstructive random-coding argument. To date, despite a considerable research effort, the only case where we know how to construct coding schemes that achieve secrecy capacity is when Eve's channel C_2 is an erasure channel, or a combinatorial variation thereof. Polar codes were recently invented by Arikan; they approach the capacity of symmetric binary-input discrete memoryless channels with low encoding and decoding complexity. Herein, we use polar codes to construct a coding scheme that achieves the secrecy capacity for a wide range of wiretap channels. Our construction works for any instantiation of the wiretap channel model, as long as both C_1 and C_2 are symmetric and binary-input, and C_2 is degraded with respect to C_1. Moreover, we show how to modify our construction in order to provide strong security, in the sense defined by Maurer, while still operating at a rate that approaches the secrecy capacity. In this case, we cannot guarantee that the reliability condition will be satisfied unless the main channel C_1 is noiseless, although we believe it can be always satisfied in practice.", "label": 1, "domain": "academic", "token_count": 383, "matched_pair_id": "conditionality_00186", "split": "train"}
{"id": "conditionality_train_pos_0180", "text": "We investigate the X-ray properties of the most luminous radio sources in the 3CR catalogue, in order to assess if they are similar to the most luminous radio quiet quasars, for instance in the X-ray normalization with respect to the optical luminosity, or in the distribution of the absorption column density. We have selected the (optically identified) 3CR radio sources whose 178-MHz monochromatic luminosity lies in the highest factor-of-three bin. The 4 most luminous objects had already been observed in X rays. Of the remaining 16, we observed with XMM-Newton 4 randomly chosen, optical type 1s, and 4 type 2s. All targets have been detected. The optical-to-Xray spectral index, alphaox, can be computed only for the type 1s and, in agreement with previous studies, is found to be flatter than in radio quiet quasars of similar luminosity. However, the Compton thin type 2s have an absorption corrected X-ray luminosity systematically lower than the type 1s, by a factor which makes them consistent with the radio quiet alphaox. Within the limited statistics, the Compton thick objects seem to have a reflected component more luminous than the Compton thin ones. The extra X-ray component observed in type 1 radio loud quasars is beamed for intrinsic causes, and is not collimated by the absorbing torus as is the case for the (intrinsically isotropic) disk emission. The extra component can be associated with a relativistic outflow, provided that the flow opening angle and the Doppler beaming factor are 1/5 - 1/7 radians.", "label": 1, "domain": "academic", "token_count": 352, "matched_pair_id": "conditionality_00027", "split": "train"}
{"id": "conditionality_train_pos_0181", "text": "trust funds, and an explanation of the impact any legislation the President signed into law in the preceding year will have on the plans for repaying the social security trust funds.''. SEC. 6. COMMITMENT BY THE SECRETARY OF THE TREASURY TO HONOR THE GOVERNMENT'S DEBT TO THE SOCIAL SECURITY TRUST FUNDS. Whenever the Board of Trustees of the social security trust funds submits its annual report to Congress pursuant to section 201(c) of the Social Security Act on the status of such trust funds during the preceding fiscal year and the expected operation and status during the ensuing 5 fiscal years, the Secretary of the Treasury shall submit a statement to Congress containing an affirmation that the Treasury will honor the securities in such trust funds. SEC. 7. REQUIREMENT THAT THE GOVERNMENT REPAY THE SOCIAL SECURITY TRUST FUNDS. Section 201(d) of the Social Security Act (42 U.S.C. 401(d)) is amended by inserting after the sixth sentence the following new sentence: ``Any individual who is credited with wages or self- employment income under this title may bring an action in an appropriate Federal district court to enjoin any act or practice by the Secretary of the Treasury by which the Secretary contests an obligation issued for purchase by either Trust Fund under this subsection or which constitutes a failure to provide for redemption of the obligation in accordance with the terms of such obligation or to otherwise honor the full faith and credit of the United States supporting such obligation.''. SEC. 8. GENERAL PROVISIONS. (a) Definitions.--As used in this Act-- (1) Social security trust funds.--The term ``social security trust funds'' refers to the Federal Old-Age and Survivors Insurance Trust Fund and the Federal Disability Insurance Trust Fund. (2) Other government expenditures.--The term ``other Government expenditures'' means all Government expenditures other than expenditures for the old-age, survivors, and disability insurance program under title II of the Social Security Act. Such term does not include amounts expended to pay down the Government debt. (b) Interpretation.--For purposes of this Act, amounts borrowed from the social security trust funds shall be considered to be used for other Government expenditures if there is a deficit in the non-Social Security budget.", "label": 1, "domain": "government", "token_count": 457, "matched_pair_id": "conditionality_00955", "split": "train"}
{"id": "conditionality_train_pos_0182", "text": "For closed 3-manifolds, Heegaard Floer homology is related to the Thurston norm through results due to Ozsv\\'ath and Szab\\'o, Ni, and Hedden. For example, given a closed 3-manifold Y, there is a bijection between vertices of the HF^+(Y) polytope carrying the group Z and the faces of the Thurston norm unit ball that correspond to fibrations of Y over the unit circle. Moreover, the Thurston norm unit ball of Y is dual to the polytope of \\underline{\\hfhat}(Y). We prove a similar bijection and duality result for a class of 3-manifolds with boundary called sutured manifolds. A sutured manifold is essentially a cobordism between two surfaces R_+ and R_- that have nonempty boundary. We show that there is a bijection between vertices of the sutured Floer polytope carrying the group Z and equivalence classes of taut depth one foliations that form the foliation cones of Cantwell and Conlon. Moreover, we show that a function defined by Juh\\'asz, which we call the geometric sutured function,is analogous to the Thurston norm in this context. In some cases, this function is an asymmetric norm and our duality result is that appropriate faces of this norm's unit ball subtend the foliation cones. An important step in our work is the following fact: a sutured manifold admits a fibration or a taut depth one foliation whose sole compact leaves are exactly the connected components of R_+ and R_-, if and only if, there is a surface decomposition of the sutured manifold resulting in a connected product manifold.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00445", "split": "train"}
{"id": "conditionality_train_pos_0183", "text": "In this paper, we give a model for understanding flavor physics in the lepton sector--mass hierarchy among different generations and neutrino mixing pattern. The model is constructed in the framework of supersymmetry, with a family symmetry $S4*U(1)$. There are two right-handed neutrinos introduced for seesaw mechanism, while some standard model(SM) gauge group singlet fields are included which transforms non-trivially under family symmetry. In the model, each order of contributions are suppressed by $\\delta \\sim 0.1$ compared to the previous one. In order to reproduce the mass hierarchy, $m_\\tau$ and $\\sqrt{\\Delta m_{atm}^2}$, $m_\\mu$ and $\\sqrt{\\Delta m_{sol}^2}$ are obtained at leading-order(LO) and next-to-leading-order(NLO) respectively, while electron can only get its mass through next-to-next-to-next-to-leading-order(NNNLO) contributions. For neutrino mixing angels, $\\theta_{12}, \\theta_{23}, \\theta_{13}$ are $45^\\circ, 45^\\circ, 0$ i.e. Bi-maximal mixing pattern as first approximation, while higher order contributions can make them consistent with experimental results. As corrections for $\\theta_{12}$ and $\\theta_{13}$ originate from the same contribution, there is a relation predicted for them $\\sin{\\theta_{13}}=\\displaystyle \\frac{1-\\tan{\\theta_{12}}}{1+\\tan{\\theta_{12}}}$. Besides, deviation from $\\displaystyle \\frac{\\pi}{4}$ for $\\theta_{23}$ should have been as large as deviation from 0 for $\\theta_{13}$ if it were not the former is suppressed by a factor 4 compared to the latter.", "label": 1, "domain": "academic", "token_count": 372, "matched_pair_id": "conditionality_00476", "split": "train"}
{"id": "conditionality_train_pos_0184", "text": "public golf course and this home to amazing youth programs,\" Compton wrote on Twitter. Beckham's group also wants to bring a massive technology park to the site, as well as an underground parking facility, public soccer fields, 500 new hotel rooms, a conference center, retail stores, restaurants and more. The Beckham franchise, when it gets going, will also bring a training center and an academy focused on developing local players to the Miami area. The stadium-location quest is just the latest drawn-out chapter in Beckham's five-years-and-counting marathon to bring MLS back to Miami. The Miami Fusion played from 1998-2001, folding because of poor attendance. Beckham and MLS announced in January that the franchise would be coming to Miami, but nearly every detail about the club remains unclear. There's no definitive start date — 2020 has been mentioned repeatedly, even though no new stadium could possibly be ready by then — as well as no team name, no logo, no colors, no coaching staff and no front-office personnel. More than a year ago, Miami-Dade County commissioners approved a deal to sell Beckham nearly three acres of county land for $9 million with the belief that it would be the last parcel he needed for a stadium site in the city's Overtown neighborhood. But that site was never the preferred choice for Beckham and his group anyway, with the original hope being to build on the waterfront near the Port of Miami. The Overtown site now seems all but doomed, though it's unclear what would happen if city commissioners or voters block the latest Beckham plan.", "label": 1, "domain": "news", "token_count": 320, "matched_pair_id": "conditionality_00510", "split": "train"}
{"id": "conditionality_train_pos_0185", "text": "We study the problem of $2$-dimensional orthogonal range counting with additive error. Given a set $P$ of $n$ points drawn from an $n\\times n$ grid and an error parameter $\\eps$, the goal is to build a data structure, such that for any orthogonal range $R$, it can return the number of points in $P\\cap R$ with additive error $\\eps n$. A well-known solution for this problem is the {\\em $\\eps$-approximation}, which is a subset $A\\subseteq P$ that can estimate the number of points in $P\\cap R$ with the number of points in $A\\cap R$. It is known that an $\\eps$-approximation of size $O(\\frac{1}{\\eps} \\log^{2.5} \\frac{1}{\\eps})$ exists for any $P$ with respect to orthogonal ranges, and the best lower bound is $\\Omega(\\frac{1}{\\eps} \\log \\frac{1}{\\eps})$. The $\\eps$-approximation is a rather restricted data structure, as we are not allowed to store any information other than the coordinates of the points in $P$. In this paper, we explore what can be achieved without any restriction on the data structure. We first describe a simple data structure that uses $O(\\frac{1}{\\eps}(\\log^2\\frac{1} {\\eps} + \\log n) )$ bits and answers queries with error $\\eps n$. We then prove a lower bound that any data structure that answers queries with error $\\eps n$ must use $\\Omega(\\frac{1}{\\eps}(\\log^2\\frac{1} {\\eps} + \\log n) )$ bits. Our lower bound is information-theoretic: We show that there is a collection of $2^{\\Omega(n\\log n)}$ point sets with large {\\em union combinatorial discrepancy}, and thus are hard to distinguish unless we use $\\Omega(n\\log n)$ bits.", "label": 1, "domain": "academic", "token_count": 427, "matched_pair_id": "conditionality_00480", "split": "train"}
{"id": "conditionality_train_pos_0186", "text": "A quasitoric manifold (resp. a small cover) is a $2n$-dimensional (resp. an $n$-dimensional) smooth closed manifold with an effective locally standard action of $(S^1)^n$ (resp. $(\\mathbb Z_2)^n$) whose orbit space is combinatorially an $n$-dimensional simple convex polytope $P$. In this paper we study them when $P$ is a product of simplices. A generalized Bott tower over $\\F$, where $\\F=\\C$ or $\\R$, is a sequence of projective bundles of the Whitney sum of $\\F$-line bundles starting with a point. Each stage of the tower over $\\F$, which we call a generalized Bott manifold, provides an example of quasitoric manifolds (when $\\F=\\C$) and small covers (when $\\F=\\R$) over a product of simplices. It turns out that every small cover over a product of simplices is equivalent (in the sense of Davis and Januszkiewicz \\cite{DJ}) to a generalized Bott manifold. But this is not the case for quasitoric manifolds and we show that a quasitoric manifold over a product of simplices is equivalent to a generalized Bott manifold if and only if it admits an almost complex structure left invariant under the action. Finally, we show that a quasitoric manifold $M$ over a product of simplices is homeomorphic to a generalized Bott manifold if $M$ has the same cohomology ring as a product of complex projective spaces with $\\Q$ coefficients.", "label": 1, "domain": "academic", "token_count": 342, "matched_pair_id": "conditionality_00051", "split": "train"}
{"id": "conditionality_train_pos_0187", "text": "Context. Ultracompact X-ray binaries (UCXBs) typically consist of a white dwarf donor and a neutron star or black hole accretor. The evolution of UCXBs and very low mass ratio binaries in general is poorly understood. Aims. We investigate the evolution of UCXBs in order to learn for which mass ratios and accretor types these systems can exist, and if they do, what are their orbital and neutron star spin periods, mass transfer rates and evolutionary timescales. Methods. For different assumptions concerning accretion disk behavior we calculate for which system parameters dynamical instability, thermal-viscous disk instability or the propeller effect emerge. Results. At the onset of mass transfer, the survival of the UCXB is determined by how efficiently the accretor can eject matter in the case of a super-Eddington mass transfer rate. At later times, the evolution of systems strongly depends on the binary's capacity to return angular momentum from the disk to the orbit. We find that this feedback mechanism most likely remains effective. In the case of steady mass transfer, the propeller effect can stop accretion onto recycled neutron stars completely at a sufficiently low mass transfer rate, based on energy considerations. However, mass transfer will likely be non-steady because disk instability allows for accretion of some of the transferred matter. Together, the propeller effect and disk instability cause the low mass ratio UCXBs to be visible a small fraction of the time at most, thereby explaining the lack of observations of such systems. Conclusions. Most likely UCXBs avoid late-time dynamically unstable mass transfer and continue to evolve as the age of the Universe allows. This implies the existence of a large population of low mass ratio binaries with orbital periods ~ 70 - 80 min, unless some other mechanism has destroyed these binaries.", "label": 1, "domain": "academic", "token_count": 373, "matched_pair_id": "conditionality_00391", "split": "train"}
{"id": "conditionality_train_pos_0188", "text": "We use the KOI-13 transiting star-planet system as a test case for the recently developed BEER algorithm (Faigler & Mazeh 2011), aimed at identifying non-transiting low-mass companions by detecting the photometric variability induced by the companion along its orbit. Such photometric variability is generated by three mechanisms, including the beaming effect, tidal ellipsoidal distortion, and reflection/heating. We use data from three Kepler quarters, from the first year of the mission, while ignoring measurements within the transit and occultation, and show that the planet's ephemeris is clearly detected. We fit for the amplitude of each of the three effects and use the beaming effect amplitude to estimate the planet's minimum mass, which results in M_p sin i = 9.2 +/- 1.1 M_J (assuming the host star parameters derived by Szabo et al. 2011). Our results show that non-transiting star-planet systems similar to KOI-13.01 can be detected in Kepler data, including a measurement of the orbital ephemeris and the planet's minimum mass. Moreover, we derive a realistic estimate of the amplitudes uncertainties, and use it to show that data obtained during the entire lifetime of the Kepler mission, of 3.5 years, will allow detecting non-transiting close-in low-mass companions orbiting bright stars, down to the few Jupiter mass level. Data from the Kepler Extended Mission, if funded by NASA, will further improve the detection capabilities.", "label": 1, "domain": "academic", "token_count": 313, "matched_pair_id": "conditionality_00383", "split": "train"}
{"id": "conditionality_train_pos_0189", "text": "if such deposit liability, obligation, certificate, or share is not insured by the Corporation to the extent or in the manner represented. ``(C) Authority of fdic.--The Corporation shall have-- ``(i) jurisdiction over any person that violates this paragraph, or aids or abets the violation of this paragraph; and ``(ii) for purposes of enforcing the requirements of this paragraph with regard to any person-- ``(I) the authority of the Corporation under section 10(c) to conduct investigations; and ``(II) the enforcement authority of the Corporation under subsections (b), (c), (d) and (i) of section 8, as if such person were a state nonmember insured bank. ``(D) Other actions preserved.--No provision of this paragraph shall be construed as barring any action otherwise available, under the laws of the United States or any State, to any Federal or State law enforcement agency or individual.''. (b) Enforcement Orders.--Section 8(c) of the Federal Deposit Insurance Act (12 U.S.C. 1818(c)) is amended by adding at the end the following new paragraph: ``(4) False advertising or misuse of names to indicate insured status.-- ``(A) Temporary order.-- ``(i) In general.--If a notice of charges served under subsection (b)(1) of this section specifies on the basis of particular facts that any person is engaged in conduct described in section 18(a)(4), the Corporation may issue a temporary order requiring-- ``(I) the immediate cessation of any activity or practice described, which gave rise to the notice of charges; and ``(II) affirmative action to prevent any further, or to remedy any existing, violation. ``(ii) Effect of order.--Any temporary order issued under this subparagraph shall take effect upon service. ``(B) Effective period of temporary order.--A temporary order issued under subparagraph (A) shall remain effective and enforceable, pending the completion of an administrative proceeding pursuant to subsection (b)(1) in connection with the notice of charges-- ``(i) until such time as the Corporation shall dismiss the charges specified in such notice; or ``(ii) if a cease-and-desist order is issued against such person, until the effective date of such order. ``(C) Civil money penalties.--Violations of section 18(a)(4) shall be subject to civil money penalties as set forth in subsection (i) in an amount not to exceed $1,000,000 for each day", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00962", "split": "train"}
{"id": "conditionality_train_pos_0190", "text": "The origin and composition of Ultra-High Energy Cosmic Ray Events (UHECRs) are under debate. Here we improve constraints on the source population(s) and compositions of UHECRs by accounting for UHECR deflections within existing Galactic magnetic field models (GMFs). We used Monte Carlo simulations for UHECRs detected by the Pierre Auger Observatory and AGASA in order to determine their outside-the-Galaxy arrival directions, and compared these with Galactic and extragalactic sources. The simulations, which used UHECR compositions from protons to Iron and seven models of the ordered GMF, include uncertainties in the GMF and a turbulent magnetic field. The correlation between UHECRs and nearby extended radiogalaxies (Nagar & Matulich 2008) remains valid, even strengthened, within several GMF models. Both the nearest radiogalaxy CenA, and the nearest radio-extended BL Lac, CGCG 413-019, are likely sources of multiple UHECRs. The correlation appears to be linked to the presence of the extended radio source rather than a tracer of an underlying population. It is possible, but unlikely, that all UHECRs originate in the nearby radiogalaxy CenA. For light UHECRs about a third of UHECRs can be \"matched\" to nearby galaxies with extended radio jets. The remaining UHECRs could also be explained as originating in extended radiogalaxies if one has at least one of: a large UHECR mean free path, a high cluster and/or intergalactic magnetic field, a heavy composition for two-thirds of the detected UHECRs. Several UHECRs have trajectories which pass close to Galactic magnetars and/or microquasars. If extended radiogalaxies are, or trace, UHECR sources, the most consistent models for the ordered GMF are the BS-S and BS-A models; the GMF models of Sun et al. 2008 are acceptable if a dipole component is added.", "label": 1, "domain": "academic", "token_count": 419, "matched_pair_id": "conditionality_00181", "split": "train"}
{"id": "conditionality_train_pos_0191", "text": "Single Degenerate model is the most widely accepted progenitor model of type Ia supernovae (SNe Ia), in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from a main sequence or a slightly evolved star (WD +MS) to increase its mass, and explodes when its mass approaches the Chandrasekhar mass limit. During the mass transfer phase between the two components, an optically thick wind may occur and the material lost as the wind may exist as circumstellar material (CSM). Searching the CSM around progenitor star is helpful to discriminate different progenitor models of SNe Ia. Meanwhile, the CSM is a source of color excess.The purpose of this paper is to study the color excess produced from the single-degenerate progenitor model with optically thick wind, and reproduce the distribution of color excesses of SNe Ia. Meng et al. (2009) systemically carried out binary evolution calculation of the WD +MS systems for various metallicities and showed the parameters of the systems before Roche lobe overflow and at the moment of supernova explosion in Meng & Yang (2009). With the results of Meng et al. (2009), we calculate the color excesses of SNe Ia at maximum light via a simple analytic method.We reproduces the distribution of color excesses of SNe Ia by our binary population synthesis approach if the velocity of the optically thick wind is taken to be of order of magnitude of 10 km s$^{\\rm -1}$. However, if the wind velocity is larger than 100 km s$^{\\rm -1}$, the reproduction is bad.", "label": 1, "domain": "academic", "token_count": 344, "matched_pair_id": "conditionality_00153", "split": "train"}
{"id": "conditionality_train_pos_0192", "text": "of the Tour de France in 2021 and to quality for the Giro D’Italia before that. He said that it’s great that others “are able to see a 250km, six hour race is not something that’s beyond them and that I can spread that positive message.” Professor Clodagh O’Gorman, consultant paediatrician in diabetes and endocrinology at University Hospital Limerick, said Stephen’s story gives “huge encouragement and inspiration to the children and teenagers who attend our paediatric diabetes services.” “Stephen shows that while diabetes is a lifelong condition that needs intensive management, young people with type 1 diabetes can still go on and achieve their goals whether in education, in sport or in life in general.” At UHL, about 190 children and adolescents attending their service, aged one to 18 years. “Most diabetes in young children and adolescents is type 1 diabetes mellitus and so these children require insulin injections as lifelong therapy for their diabetes,” explained Prof O’Gorman. \"It is quite different to type 2 diabetes, which is more common in adults.\" “Diabetes in children is an unremitting, life-long condition with a very high lifetime rate of complications. Intensive education, intensive management and frequent regular contact with the diabetes team are the mainstays of improving therapy to minimise the risks of complications. “We expect that modern therapies, and close attention to achieving near normal blood sugars will protect these children and adolescents from the risks of diabetes complications in their future. The young people with type 1 diabetes who attend our clinic display great courage and tenacity, facing insulin injections every day of their lives. It is wonderful to introduce them to someone like Stephen Clancy, who is proof for them that they can achieve their goals, even if they have diabetes,” said Prof O’Gorman.", "label": 1, "domain": "news", "token_count": 376, "matched_pair_id": "conditionality_00787", "split": "train"}
{"id": "conditionality_train_pos_0193", "text": "if such test result is not the first positive test result for such applicant in the benefit year, no regular compensation may be paid to such applicant during the remainder of such benefit year. ``(C) A high-risk applicant receiving benefits with respect to a benefit year shall be subject to testing for controlled substances by the State at any time during the benefit year, with limited notice provided to the applicant of such testing. ``(D) A high-risk applicant who is tested for controlled substances under-- ``(i) subparagraph (A) or (C) shall be responsible for the cost of such test if the individual tests positive for any such substance; and ``(ii) subparagraph (B)(i)(II) shall be responsible for the cost of such test. ``(2) For purposes of this subsection-- ``(A) the term `benefit year' means the benefit year as defined in the applicable State law; ``(B) the term `controlled substance'-- ``(i) means a drug or other substance selected by the State to be included in drug testing under this subsection; and ``(ii) does not include any drug or other substance used by the applicant pursuant to a valid prescription or as otherwise authorized by law; ``(C) the term `high-risk applicant', with respect to a benefit year, means an individual who is determined by the State to have a high risk of substance abuse based on the results of a substance abuse risk assessment administered under paragraph (1)(A)(i); and ``(D) the term `substance abuse risk assessment' means a screening instrument, approved by the Director of the National Institutes of Health, designed to determine whether an individual has a high risk of substance abuse.''. (b) No Merit Staffing Requirements.--Section 303(a)(1) of the Social Security Act (42 U.S.C. 503(a)(1)) shall not be construed in such a manner as to apply the merit staffing requirements in section 900.603 of title 5, Code of Federal Regulations, as in effect on October 1, 2011, to the implementation of section 303(l) of such Act (as amended by subsection (a)). (c) Funding for Substance Abuse Testing.-- (1) Funding from ipab.--Section 1899A(m) of the Social Security Act (42 U.S.C. 1395kkk(m)) is amended-- (A) in paragraph (1), in the matter preceding subparagraph (A), by striking ``to", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01018", "split": "train"}
{"id": "conditionality_train_pos_0194", "text": "Future or ongoing galaxy redshift surveys can put stringent constraints on neutrinos masses via the high-precision measurements of galaxy power spectrum, when combined with cosmic microwave background (CMB) information. In this paper we develop a method to model galaxy power spectrum in the weakly nonlinear regime for a mixed dark matter (CDM plus finite-mass neutrinos) model, based on perturbation theory (PT) whose validity is well tested by simulations for a CDM model. In doing this we carefully study various aspects of the nonlinear clustering and then arrive at a useful approximation allowing for a quick computation of the nonlinear power spectrum as in the CDM case. The nonlinear galaxy bias is also included in a self-consistent manner within the PT framework. Thus the use of our PT model can give a more robust understanding of the measured galaxy power spectrum as well as allow for higher sensitivity to neutrino masses due to the gain of Fourier modes beyond the linear regime. Based on the Fisher matrix formalism, we find that BOSS or Stage-III type survey, when combined with Planck CMB information, gives a precision of total neutrino mass constraint, sigma(m_nu,tot) 0.1eV, while Stage-IV type survey may achieve sigma(m_nu,tot) 0.05eV, i.e. more than a 1-sigma detection of neutrino masses. We also discuss possible systematic errors on dark energy parameters caused by the neutrino mass uncertainty. The significant correlation between neutrino mass and dark energy parameters is found, if the information on power spectrum amplitude is included. More importantly, for Stage-IV type survey, a best-fit dark energy model may be biased and falsely away from the underlying true model by more than the 1-sigma statistical errors, if neutrino mass is ignored in the model fitting.", "label": 1, "domain": "academic", "token_count": 372, "matched_pair_id": "conditionality_00154", "split": "train"}
{"id": "conditionality_train_pos_0195", "text": "report also predicts that raising the minimum legal age of sale of tobacco products nationwide to age 21 would result in 223,000 fewer premature deaths, 50,000 fewer deaths from lung cancer, and 4,200,000 fewer years of life lost for those born between 2000 and 2019. In addition, the report concluded that raising the minimum legal age of sale would result in near immediate reductions in preterm birth, low birth weight, and sudden infant death syndrome. SEC. 3. PROHIBITION AND ENFORCEMENT. (a) In General.--Notwithstanding any other provision of law, including any Federal regulation, it shall be unlawful to sell or distribute a tobacco product to anyone under the age of 21. (b) Enforcement.-- (1) In general.--The Secretary of Health and Human Services is authorized to enforce the prohibition under subsection (a) and shall take necessary action to enforce such prohibition, including, as appropriate-- (A) conducting undercover compliance checks, performing retailer inspections, initiating enforcement actions for noncompliance, and taking any other measures appropriate to help ensure nationwide compliance with such prohibition; and (B) establishing requirements that retailers check identification or use other methods to ensure compliance with subsection (a), or issuing guidance concerning the responsibility of retailers to ensure such compliance. (2) Enforcement authority.--In the case of a violation of subsection (a), the Secretary of Health and Human Services may apply the penalties under section 303 of the Federal Food, Drug, and Cosmetic Act (21 U.S.C. 333), as though such subsection (a) were a regulation promulgated under section 906(d)(1) of the Federal Food, Drug, and Cosmetic Act (21 U.S.C. 387f(d)(1)), notwithstanding paragraph (3)(A)(ii) of such section 906(d). (c) Definition.--In this Act, the term ``tobacco product'' has the meaning given such term in section 201(rr) of the Federal Food, Drug, and Cosmetic Act (21 U.S.C. 321(rr)). SEC. 4. NON-PREEMPTION. Nothing in this Act shall be construed to prevent a State or local governmental entity from establishing, enforcing, or maintaining a law with respect to sales of tobacco to individuals below a minimum age, provided that such State or local law is at least as restrictive as the Federal law.", "label": 1, "domain": "government", "token_count": 491, "matched_pair_id": "conditionality_01033", "split": "train"}
{"id": "conditionality_train_pos_0196", "text": "Type I planetary nebulae (PNe) have high He/H and N/O ratios and are thought to be descendants of stars with initial masses of ~3-8Msun. These characteristics indicate that the progenitor stars experienced proton-capture nucleosynthesis at the base of the convective envelope, in addition to the slow neutron capture process operating in the He-shell (the s-process). We compare the predicted abundances of elements up to Sr from models of intermediate-mass asymptotic giant branch (AGB) stars to measured abundances in Type I PNe. In particular, we compare predictions and observations for the light trans-iron elements Se and Kr, in order to constrain convective mixing and the s-process in these stars. A partial mixing zone is included in selected models to explore the effect of a 13C pocket on the s-process yields. The solar-metallicity models produce enrichments of [(Se, Kr)/Fe] < 0.6, consistent with Galactic Type I PNe where the observed enhancements are typically < 0.3 dex, while lower metallicity models predict larger enrichments of C, N, Se, and Kr. O destruction occurs in the most massive models but it is not efficient enough to account for the > 0.3 dex O depletions observed in some Type I PNe. It is not possible to reach firm conclusions regarding the neutron source operating in massive AGB stars from Se and Kr abundances in Type I PNe; abundances for more s-process elements may help to distinguish between the two neutron sources. We predict that only the most massive models would evolve into Type I PNe, indicating that extra-mixing processes are active in lower-mass stars (3-4Msun), if these stars are to evolve into Type I PNe.", "label": 1, "domain": "academic", "token_count": 367, "matched_pair_id": "conditionality_00080", "split": "train"}
{"id": "conditionality_train_pos_0197", "text": "corporation shall keep, at its principal office, a record of the names of all members having the right to vote in any proceeding of the corporation. (c) Right To Inspect Books and Records.--All books and records of the corporation may be inspected by any member having the right to vote, or by any agent or attorney of such member, for any proper purpose, at any reasonable time. (d) Application of State Law.--No provision of this section may be construed to contravene any applicable State law. SEC. 7. AUDIT OF FINANCIAL TRANSACTIONS. The first section of the Act entitled ``An Act to provide for audit of accounts of private corporations established under the Federal law'', approved August 30, 1964 (36 U.S.C. 1101), is amended by adding at the end the following: ``Ukrainian American Veterans, Incorporated.''. SEC. 8. ANNUAL REPORT. The corporation shall annually submit to the Congress a report concerning the activities of the corporation during the preceding fiscal year. The annual report shall be submitted at the same time as is the report of the audit required by section 7. The report shall not be printed as a public document. SEC. 9. RESERVATION OF RIGHT TO AMEND OR REPEAL CHAPTER. The right to amend or repeal this Act is expressly reserved to the Congress. SEC. 10. DEFINITIONS. For purposes of this Act-- (1) the term ``corporation'' means the Ukrainian American Veterans, Incorporated; and (2) the term ``State'' means any of the several States, the District of Columbia, the Commonwealth of Puerto Rico, the Commonwealth of the Northern Mariana Islands, the Virgin Islands, Guam, American Samoa, the Trust Territories of the Pacific Islands, or any other territory or possessions of the United States. SEC. 11. TAX-EXEMPT STATUS. The corporation shall maintain its status as an organization exempt from taxation as provided in the Internal Revenue Code of 1986. SEC. 12. TERMINATION. The charter granted in this Act shall expire if the corporation fails to comply with any provisions of this Act.", "label": 1, "domain": "government", "token_count": 446, "matched_pair_id": "conditionality_00843", "split": "train"}
{"id": "conditionality_train_pos_0198", "text": "Acoustic peaks in the spectrum of the cosmic microwave background in spherically symmetric inhomogeneous cosmological models are studied. At the photon-baryon decoupling epoch, the universe may be assumed to be dominated by non-relativistic matter, and thus we may treat radiation as a test field in the universe filled with dust which is described by the Lema\\^itre-Tolman-Bondi (LTB) solution. First, we give an LTB model whose distance-redshift relation agrees with that of the concordance $\\Lambda$CDM model in the whole redshift domain and which is well approximated by the Einstein-de Sitter universe at and before decoupling. We determine the decoupling epoch in this LTB universe by Gamow's criterion and then calculate the positions of acoustic peaks. Thus obtained results are not consistent with the WMAP data. However, we find that one can fit the peak positions by appropriately modifying the LTB model, namely, by allowing the deviation of the distance-redshift relation from that of the concordance $\\Lambda$CDM model at $z>2$ where no observational data are available at present. Thus there is still a possibility of explaining the apparent accelerated expansion of the universe by inhomogeneity without resorting to dark energy if we abandon the Copernican principle. Even if we do not take this extreme attitude, it also suggests that local, isotropic inhomogeneities around us may seriously affect the determination of the density contents of the universe unless the possible existence of such inhomogeneities is properly taken into account.", "label": 1, "domain": "academic", "token_count": 325, "matched_pair_id": "conditionality_00223", "split": "train"}
{"id": "conditionality_train_pos_0199", "text": "in any case in which such point of order is sustained against a conference report (or Senate amendment derived from such conference report by operation of this subsection), no further amendment shall be in order. (c) Waiver; Appeal.--A point of order under subsection (a) may be waived only by an affirmative vote of two-thirds of the Members of the Senate, duly chosen and sworn. An affirmative vote of two-thirds of the Members of the Senate, duly chosen and sworn, shall be required to sustain an appeal of the ruling of the Chair on a point of order raised under subsection (a). (d) Definitions.-- (1) Earmark.--For the purpose of this section, the term ``earmark'' means a provision or report language included primarily at the request of a Senator or Member of the House of Representatives as certified under paragraph 1(a)(1) of rule XLIV of the Standing Rules of the Senate-- (A) providing, authorizing, or recommending a specific amount of discretionary budget authority, credit authority, or other spending authority for a contract, loan, loan guarantee, grant, loan authority, or other expenditure with or to an entity, or targeted to a specific State, locality or Congressional district, other than through a statutory or administrative formula-driven or competitive award process; (B) that-- (i) provides a Federal tax deduction, credit, exclusion, or preference to a particular beneficiary or limited group of beneficiaries under the Internal Revenue Code of 1986; and (ii) contains eligibility criteria that are not uniform in application with respect to potential beneficiaries of such provision; or (C) modifying the Harmonized Tariff Schedule of the United States in a manner that benefits ten or fewer entities. (2) Determination by the senate.--In the event the Chair is unable to ascertain whether a provision with respect to which a Senator raises a point of order under subsection (a) constitutes an earmark, the question of whether the provision constitutes an earmark shall be submitted to the Senate and be decided without debate by an affirmative vote of two-thirds of the Senators, duly chosen and sworn. (e) Application.--This section shall not apply to any authorization of appropriations to a Federal entity if such authorization is not specifically targeted to a State, locality, or congressional district.", "label": 1, "domain": "government", "token_count": 463, "matched_pair_id": "conditionality_00834", "split": "train"}
{"id": "conditionality_train_pos_0200", "text": "If the individual is survived by a spouse who is living at the time of payment, the payment shall be made to such surviving spouse. (ii) If the individual is not survived by a spouse described in clause (i), the payment shall be made in equal shares to all children of the individual who are living at the time of the payment. (iii) If the individual is not survived by a person described in clause (i) or (ii), the payment shall be made in equal shares to the parents of the individual who are living at the time of payment. (iv) If the individual is not survived by a person described in clause (i), (ii), or (iii), the payment shall revert back to the Fund. (B) Filing of petition by survivor.--If an individual eligible for payment under section 102(a) dies before filing a petition under this title, a survivor of the individual may file a petition for payment under this title on behalf of the individual if the survivor may receive payment under subparagraph (A). (C) Definitions.--For purposes of this paragraph: (i) The term ``spouse'' means an individual who was lawfully married to the relevant individual at the time of death. (ii) The term ``child'' includes a recognized natural child, a stepchild who lived with the relevant individual in a regular parent-child relationship, and an adopted child. (iii) The term ``parent'' includes fathers and mothers through adoption. (3) Timing of payment.--The Secretary may not make a payment on a petition under this title before the expiration of the 120-day period beginning on the date of the enactment of this Act or after the expiration of the 5-year period beginning on the date of the enactment of this Act. (d) Action on Petitions.-- (1) In general.--The Secretary shall complete the determination required by subsection (b) regarding a petition not later than 120 days after the date the petition is filed under this title. (2) Petitions by certain individuals.--In the case of a petition filed by an individual described in section 102(a)(2)(A)(ii), the Secretary may not make a payment on such petition prior to the expiration of the period described in subsection (c)(1)(B). (e) Humanitarian Nature of Payment.--This Act does not create or admit any claim of or on behalf of the individual against the United States or against any officer, employee, or agent", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01061", "split": "train"}
{"id": "conditionality_train_pos_0201", "text": "(Abridged) A procedure is suggested to explore the value of F = alpha^2/mu, where mu = m_e/m_p is the electron-to-proton mass ratio, and alpha is the fine-structure constant. The fundamental physical constants, which are measured in different physical environments of high (terrestrial) and low (interstellar) densities of baryonic matter are supposed to vary in chameleon-like scalar field models, which predict that both masses and coupling constant may depend on the local matter density. The parameter Delta F/F = (F_obs - F_lab)/F_lab can be estimated from the radial velocity offset, Delta V = V_rot-V_fs, between the low-laying rotational transitions in carbon monoxide 13CO and the fine-structure transitions in atomic carbon [CI]. A model-dependent constraint on Delta alpha/alpha can be obtained from Delta F/F using Delta mu/mu independently measured from the ammonia method. Currently available radio astronomical datasets provide an upper limit on |Delta V| < 110 m/s (1sigma). When interpreted in terms of the spatial variation of F, this gives |Delta F/F| < 3.7*10^-{7}. An order of magnitude improvement of this limit will allow us to test independently a non-zero value of Delta mu/mu = (2.2 +/- 0.4_stat +/- 0.3_sys)*10^{-8} recently found with the ammonia method. Taking into account that the ammonia method restricts the spatial variation of mu at the level of |Delta mu/mu| <= 3*10^{-8} and assuming that Delta F/F is the same in the entire interstellar medium, one obtains that the spatial variation of alpha does not exceed the value |Delta alpha/alpha| < 2*10^{-7}. Since extragalactic gas clouds have densities similar to those in the interstellar medium, the bound on Delta alpha/alpha is also expected to be less than 2*10^{-7} at high redshift if no significant temporal dependence of alpha is present.", "label": 1, "domain": "academic", "token_count": 421, "matched_pair_id": "conditionality_00213", "split": "train"}
{"id": "conditionality_train_pos_0202", "text": "In the very last years, cosmological models where the properties of the dark components of the Universe - dark matter and dark energy - are accounted for by a single \"dark fluid\" have drawn increasing attention and interest. Amongst many proposals, Unified Dark Matter (UDM) cosmologies are promising candidates as effective theories. In these models, a scalar field with a non-canonical kinetic term in its Lagrangian mimics both the accelerated expansion of the Universe at late times and the clustering properties of the large-scale structure of the cosmos. However, UDM models also present peculiar behaviours, the most interesting one being the fact that the perturbations in the dark-matter component of the scalar field do have a non-negligible speed of sound. This gives rise to an effective Jeans scale for the Newtonian potential, below which the dark fluid does not cluster any more. This implies a growth of structures fairly different from that of the concordance LCDM model. In this paper, we demonstrate that forthcoming large-scale surveys will be able to discriminate between viable UDM models and LCDM to a good degree of accuracy. To this purpose, the planned Euclid satellite will be a powerful tool, since it will provide very accurate data on galaxy clustering and the weak lensing effect of cosmic shear. Finally, we also exploit the constraining power of the ongoing CMB Planck experiment. Although our approach is the most conservative, with the inclusion of only well-understood, linear dynamics, in the end we also show what could be done if some amount of non-linear information were included.", "label": 1, "domain": "academic", "token_count": 320, "matched_pair_id": "conditionality_00415", "split": "train"}
{"id": "conditionality_train_pos_0203", "text": "if the individual is convicted of the offense and is the parent, guardian, or custodian of the child passenger or is otherwise legally responsible for the child passenger, the law enforcement agency that charges the individual with the offense or the appropriate court to file with the appropriate State register of child abuse a report on the individual concerning the offense. ``(2) Exceptions.--The Secretary may treat a State that has enacted and is enforcing the laws described in paragraph (1) as meeting the requirements of this subsection without regard to whether any of those laws waives the application of a sanction with respect to an individual who-- ``(A) is a sibling of the child passenger; or ``(B) is under 21 years of age and is not a guardian of the child passenger. ``(c) Period of Availability of Withheld Funds; Effect of Compliance and Noncompliance.-- ``(1) Period of availability of withheld funds.--Any funds withheld under subsection (a) from apportionment to a State shall remain available for apportionment to the State until the end of the third fiscal year following the fiscal year for which the funds are authorized to be appropriated. ``(2) Apportionment of withheld funds after compliance.-- If, before the last day of the period for which funds withheld under subsection (a) from apportionment are to remain available for apportionment to a State under paragraph (1), the State meets the requirements of subsection (b), the Secretary shall, on the first day on which the State meets the requirements of subsection (b), apportion to the State the funds withheld under subsection (a) that remain available for apportionment to the State. ``(3) Period of availability of subsequently apportioned funds.--Any funds apportioned pursuant to paragraph (2)-- ``(A) shall remain available for expenditure until the end of the third fiscal year following the fiscal year in which the funds are so apportioned; and ``(B) if not apportioned at the end of that period, shall lapse. ``(4) Effect of noncompliance.--If, at the end of the period for which funds withheld under subsection (a) from apportionment are available for apportionment to a State under paragraph (1), the State does not meet the requirements of subsection (b), the funds shall lapse. ``(d) Definitions.--In this section, the following definitions apply: ``(1) Alcohol concentration.--The term `alcohol concentration' means grams of alcohol per 100", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01006", "split": "train"}
{"id": "conditionality_train_pos_0204", "text": "If David Moyes thought managing Manchester United was the biggest challenge of his career, he will soon reappraise that evaluation. This is his greatest test and, should he pass it, it will surely be his finest hour. The Scot is going to have to be a master coach, inspired motivator and transfer magician. The Scot is going to have to be a master coach, inspired motivator and transfer magician all rolled into one if he is to keep Sunderland in the Premier League. Saturday’s woeful 4-1 defeat at Burnley left the Black Cats deep in the drop zone. Injuries continue to plague the side, Lamine Kone was lost midway through the first half and, after that, the defence was lost. The departure of Victor Anichebe, also with a hamstring injury, not only robbed the team of their powerhouse forward, it drained that vital commodity from the side, confidence. Not that Big Vic’s absence cold in any way be linked to some Sunday League stuff. Sunderland’s soft centre was exposed three times by Andre Gray on 31, 51 and 53 minutes. The opener was a dreadful goal to concede, John O’Shea and Papy Djilobodji challenging each other more effectively than they did Ashley Barnes. O’Shea only succeeded in helping on Scott Arfield’s up-and-under into the path of the unmarked Gray, who strode forward and beat Vito Mannone from 18 yards, the keeper failing to keep out a shot which was pretty much straight at him. Sunderland could not deal with a hopeful ball forward for the second goal either. Gray shook off a weak attempt from Djilobodji before rounding an equally lame attempt from Mannone, who had rushed to the edge of the box to tap into the empty net. His third goal also had a comedy element. Steven Pienaar stood on he ball as he led an away counter-attack, alowing Burnley to hit their frontmen again, Barnes chesting the ball superbly before playing in Gray, who finished from seven yards. The Clarets were not finished and when Seb Larsson, ludicrously, pushed over Arfield in the box in the 67th minute, Barnes beat Mannone from the spot. Fortunately, the scoreline got no worse and Sunderland were able to pull one back in the 71st minute. Adnan Januzaj took part in a football version of the 110 metres hurdles, skipping over", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00581", "split": "train"}
{"id": "conditionality_train_pos_0205", "text": "i) In general.--All persons treated as a controlled group shall be treated as 1 person. (ii) Controlled group.--The term ``controlled group'' has the meaning given to such term by subsection (a) of section 1563 of such Code; except that for such purposes the phrase ``more than 50 percent'' shall be substituted for the phrase ``at least 80 percent'' each place it appears in such subsection. (B) Nonincorporated persons under common control.-- Under regulations prescribed by the Secretary, principles similar to the principles of subparagraph (A) shall apply to a group of persons under common control where 1 or more of such persons is not a corporation. (g) Other Law Applicable.--All provisions of law, including penalties, applicable with respect to the taxes imposed by section 4041(a)(2) of such Code in the case of special fuels; by section 4081 of such Code in the case of gasoline, diesel fuel, and kerosene; and by section 4091 of such Code in the case of aviation fuel shall, insofar as applicable and not inconsistent with the provisions of this subsection, apply with respect to the floor stock taxes imposed by subsection (a) to the same extent as if such taxes were imposed by such section 4041, 4081, or 4091. SEC. 5. PROTECTION OF HIGHWAY TRUST FUND. The amounts transferred to the Highway Trust Fund under section 9503 of the Internal Revenue Code of 1986 shall be determined as if this Act had not been acted.", "label": 1, "domain": "government", "token_count": 324, "matched_pair_id": "conditionality_00983", "split": "train"}
{"id": "conditionality_train_pos_0206", "text": "We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045 $\\le z <$ 0.78 in 8420 sq. deg. of the sky. We provide angular position, redshift, richness, core and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the $r$ band which are possible BCG candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen, Han, and Liu. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison. We find that both $\\Lambda_{200}$ and $R_{200}$ correlate well with both $L_X$ and $T_X$, with no significant difference in trend if we restrict the matches to flux-limited X-ray samples.", "label": 1, "domain": "academic", "token_count": 318, "matched_pair_id": "conditionality_00276", "split": "train"}
{"id": "conditionality_train_pos_0207", "text": "If you like a last-minute twist in a courtroom thriller, you will have left the Memorial Hall in Hathersage with a great big smile on your face after Witness for the Prosecution. The Hathersage Players’ production of Agatha Christie’s classic ran to appreciative audiences over four nights. The cast were beautifully led by Emily Upton in the titular role. Miss Upton’s smouldering portrayal of Romaine Vole (pictured) conjured up wonderful memories of Marlene Dietrich in the famous 1957 film of the same name as she coolly foiled all those around her who sought the truth. The combative Sir. Wilfrid Robarts Q.C., played by the ever-talented Denis Murphy was chiefly foiled. Mr Murphy drove the production with charm and flair, especially so bearing in mind the enormity of the script that he had committed to memory. Thereafter, the cast played in strong support, notably Rob Hall as the caddish Leonard Vole (as well as directing), Richard Morello as the steady John Mayhew, Joe Hardy as the “irritating” Mr. Myers Q.C. and Val Robinson as the truculent Janet MacKenzie. Humour was injected by some lovely moments from Alistair Cook as Carter/Mr Justice Wainwright and Gail Newsome as Greta. The scene in 1954 was set nicely using contemporary fashions, music and news items. The swift interplay between the intimate set for the Chambers of Sir. Wilfrid Robarts Q.C. and the impressively grand set for the courtroom at The Old Bailey was something of a triumph with clever lighting changes completing the task. The challenges faced when presenting a static courtroom drama were successfully overcome using an adapted script with engaging dialogue that tripped along at a good pace from well-developed characters. The gasps from the audience at the twist proved the point. Hot on the heels of last year’s sell-out sensations of Jane Eyre and Oliver!, this production marked something of an adventurous change by the ambitious Hathersage Players. However, this was a true victory and will hopefully be swiftly followed by another. STOP PRESS: Hold onto your hats! Their next production is Jessica Swale’s rip-roaring play, Nell Gwynne, a script fresh from winning the best new comedy in the West End, from Wednesday, October 11 to Saturday, October 14, 2017", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00620", "split": "train"}
{"id": "conditionality_train_pos_0208", "text": "Of the approximately 350 extrasolar planets currently known, of order 10% orbit evolved stars with radii R >~ 2.5 R_sun. These planets are of particular interest because they tend to orbit more massive hosts, and have been subjected to variable stellar insolation over their recent histories as their primaries evolved off the main sequence. Unfortunately, we have limited information about the physical properties of these planets, as they were all detected by the radial velocity method and none have been observed to transit. Here we evaluate the prospects for detecting transits of planetary companions to giant stars. We show that several of the known systems have a priori transit probabilities of >~ 10%, and about one transiting system is expected for the sample of host stars with R >= 2.5 R_sun. Although the transits are expected to have very small amplitudes (~few x 10^-4) and long durations (>~ 50 hrs), we argue that the difficulty with detecting these signals in broadband light is one of systematic errors and practicality rather than photon noise, even for modest aperture ~1m telescopes. We propose a novel method that may overcome these difficulties, which uses narrow-band measurements to isolate the thin ring of chromospheric emission expected at the limb of giant stars. The transit signals in these narrow bands are expected to be larger in magnitude and briefer in duration than in broad-band emission, and thus alleviating many of the difficulties with transit detection in broad-band emission. Finally, we point out that it may be possible to discover planetary companions to giant stars using Kepler, provided that a sufficient number of such targets are monitored.", "label": 1, "domain": "academic", "token_count": 333, "matched_pair_id": "conditionality_00122", "split": "train"}
{"id": "conditionality_train_pos_0209", "text": "or to valuations, costs or accounting, or practices relating to such rates, wages, structures, prices, appliances, services, or allowances. (5) Significant.--The term ``significant'' means increasing consumers' cost of housing by more than $100,000,000 per year. (k) Development.--Not later than 1 year after the date of the enactment of this Act, the Secretary of Housing and Urban Development shall develop model initial and final housing impact analyses under this section and shall cause such model analyses to be published in the Federal Register. The model analyses shall define the primary elements of a housing impact analysis to instruct other agencies on how to carry out and develop the analyses required under subsections (d) and (e). (l) Judicial Review.-- (1) Determination by agency.--Except as otherwise provided in paragraph (2), any determination by an agency concerning the applicability of any of the provisions of this Act to any action of the agency shall not be subject to judicial review. (2) Other actions by agency.--Any housing impact analysis prepared under subsection (d) or (e) and the compliance or noncompliance of the agency with the provisions of this Act shall not be subject to judicial review. When an action for judicial review of a rule is instituted, any housing impact analysis for such rule shall constitute part of the whole record of agency action in connection with the review. (3) Exception.--Nothing in this subsection bars judicial review of any other impact statement or similar analysis required by any other law if judicial review of such statement or analysis is otherwise provided by law.", "label": 1, "domain": "government", "token_count": 323, "matched_pair_id": "conditionality_00899", "split": "train"}
{"id": "conditionality_train_pos_0210", "text": "A path in an edge-colored graph $G$, where adjacent edges may be colored the same, is called a rainbow path if no two edges of $G$ are colored the same. For a $\\kappa$-connected graph $G$ and an integer $k$ with $1\\leq k\\leq \\kappa$, the rainbow $k$-connectivity $rc_k(G)$ of $G$ is defined as the minimum integer $j$ for which there exists a $j$-edge-coloring of $G$ such that every two distinct vertices of $G$ are connected by $k$ internally disjoint rainbow paths. Let $G$ be a complete $(\\ell+1)$-partite graph with $\\ell$ parts of size $r$ and one part of size $p$ where $0\\leq p <r$ (in the case $p=0$, $G$ is a complete $\\ell$-partite graph with each part of size $r$). This paper is to investigate the rainbow $k$-connectivity of $G$. We show that for every pair of integers $k\\geq 2$ and $r\\geq 1$, there is an integer $f(k,r)$ such that if $\\ell\\geq f(k,r)$, then $rc_k(G)=2$. As a consequence, we improve the upper bound of $f(k)$ from $(k+1)^2$ to $ck^{{3/2}}+C$, where $0<c<1$, $C=o(k^{{3/2}})$, and $f(k)$ is the integer such that if $n \\geq f(k)$ then $rc_k(K_n)=2$.", "label": 1, "domain": "academic", "token_count": 361, "matched_pair_id": "conditionality_00150", "split": "train"}
{"id": "conditionality_train_pos_0211", "text": "We present an analysis of the X-ray variability of three symbiotic X-ray binaries, GX 1+4, 4U 1700+24, and 4U 1954+31, using observations made with the Swift Burst Alert Telescope (BAT) and the Rossi X-ray Timing Explorer (RXTE) All-Sky Monitor (ASM). Observations of 4U 1954+31 with the Swift BAT show modulation at a period near 5 hours. Models to explain this modulation are discussed including the presence of an exceptionally slow X-ray pulsar in the system and accretion instabilities. We conclude that the most likely interpretation is that 4U 1954+31 contains one of the slowest known X-ray pulsars. Unlike 4U 1954+31, neither GX 1+4 nor 4U 1700+24 show any evidence for modulation on a timescale of hours. An analysis of the RXTE ASM light curves of GX 1+4, 4U 1700+24, and 4U 1954+31 does not show the presence of periodic modulation in any source, although there is considerable variability on long timescales for all three sources. There is no modulation in GX 1+4 on either the optical 1161 day orbital period or a previously reported 304 day X-ray period. For 4U 1700+24 we do not confirm the 404 day X-ray period previously proposed for this source from a shorter duration ASM light curve. We conclude that all three sources have substantial low-frequency noise in their power spectra that may give the appearance of periodic modulation if this noise is not properly accounted for, particularly if short duration light curves are examined.", "label": 1, "domain": "academic", "token_count": 356, "matched_pair_id": "conditionality_00030", "split": "train"}
{"id": "conditionality_train_pos_0212", "text": "If there was any lingering doubt that veganism is going mainstream, the existence of the McVegan should clear it up. According to Food & Wine, McDonald’s is trialling its first meatless burger. The soy-based patty is served with a schmear of vegan McFeast sauce, tomato, lettuce, onions and pickles. But there’s a catch – it’s exclusively available in Tampere, a city in southern Finland. The test-run started on October 4 and Tampere residents have until November 21 to sample the McVegan for themselves. A representative for the fast food giant told TODAY that the meatless burger “is limited to McDonald’s Finland and there are no current plans for that to change.” According to the blog Veggie Athletic, marketing director Christoffer Rönnblad confirmed that McDonald’s fries are vegan as well: “They are made here in Finland from potatoes and (fried) in vegetable oil. The fries are completely vegan.” Meatless burger options have expanded beyond the typical soy and grain-based patties recently. Products such as the Beyond Burger and Impossible Burger are redefining what a vegan burger can be. In the U.K. alone, the number of vegans has risen by 360 per cent in the past 10 years. The fact that McDonald’s is finally entering the fray with the McVegan suggests that the meatless trend is here to stay. But it may have to do better than run-of-the-mill soy to compete with innovative vegan patties that look and cook like meat.", "label": 1, "domain": "news", "token_count": 317, "matched_pair_id": "conditionality_00674", "split": "train"}
{"id": "conditionality_train_pos_0213", "text": "We present the third and final part of a census of Asymptotic Giant Branch (AGB) stars in Local Group dwarf irregular galaxies. Papers I and II presented the results for WLM and IC 1613. Included here are Phoenix, LGS 3, DDO 210, Leo A, Pegasus dIrr, and Sextans A. Spitzer photometry at 3.6, 4.5, 5.8, and 8 are presented, along with a more thorough treatment of background galaxy contamination than was presented in papers I and II. We find that at least a small population of completely optically obscured AGB stars exists in each galaxy, regardless of the galaxy's metallicity, but that higher-metallicity galaxies tend to harbor more stars with slight IR excesses. The optical incompleteness increases for the redder AGB stars, in line with the expectation that some AGB stars are not detected in the optical due to large amounts of extinction associated with in situ dust production. Overall, there is an underrepresentation of 30% - 40% in the optical AGB within the 1 sigma errors for all of the galaxies in our sample. This undetected population is large enough to affect star formation histories derived from optical color-magnitude diagrams. As measured from the [3.6] - [4.5] color excesses, we find average stellar mass-loss rates ranging from 3.1E-7 - 6.6E-6 solar masses per year, and integrated galaxy mass-loss rates ranging from 4.4E-5 - 1.4E-3 solar masses per year. The integrated mass-loss rate is sufficient to sustain the current star formation rate in only LGS 3 and DDO 210, requiring either significant non-dusty mass loss or gas accretion in Phoenix, Leo A, Pegasus dIrr, Sextans A, WLM, and IC 1613 if they are to maintain their status as gas-rich galaxies.", "label": 1, "domain": "academic", "token_count": 415, "matched_pair_id": "conditionality_00125", "split": "train"}
{"id": "conditionality_train_pos_0214", "text": "We present Kepler satellite photometry of KIC 10661783, a short-period binary star system which shows total eclipses and multi-periodic delta Scuti pulsations. A frequency analysis of the eclipse-subtracted light curve reveals at least 68 frequencies of which 55 or more can be attributed to pulsation modes. The main limitation on this analysis is the frequency resolution within the 27-day short-cadence light curve. Most of the variability signal lies in the frequency range 18 to 31 c/d, with amplitudes between 0.1 and 4 mmag. One harmonic term (2.f) and a few combination frequencies (f_i+f_j) have been detected. From a plot of the residuals versus orbital phase we assign the pulsations to the primary star in the system. The pulsations were removed from the short-cadence data and the light curve was modelled using the Wilson-Devinney code. We are unable to get a perfect fit due to the residual effects of pulsations and also to the treatment of reflection and reprocessing in the light curve model. A model where the secondary star fills its Roche lobe is favoured, which means that KIC 10661783 can be classified as an oEA system. Further photometric and spectroscopic observations will allow the masses and radii of the two stars to be measured to high precision and hundreds of delta Scuti pulsation frequencies to be resolved. This could lead to unique constraints on theoretical models of delta Scuti stars, if the evolutionary history of KIC 10661783 can be accounted for.", "label": 1, "domain": "academic", "token_count": 325, "matched_pair_id": "conditionality_00309", "split": "train"}
{"id": "conditionality_train_pos_0215", "text": "If left-right gauge theory occurs as an intermediate symmetry in a GUT then, apart from other advantages, it is possible to obtain the see-saw scale necessary to understand small neutrino masses with Majorana coupling of order unity. Barring threshold or non-renormalizable gravitational effects, or assumed presence of additional light scalar particles of unprescribed origin, all other attempts to achieve manifest one-loop gauge coupling unification in SUSY SO(10) with left-right intermediate symmetry have not been successful so far. Attributing this failure to lack of flavor symmetry in the GUT, we show how the spontaneous symmetry breaking of $SO(10)\\times S_4$ leads to such intermediate scale extending over a wide range, $M_R \\simeq 5\\times 10^{9}$ GeV to $10^{15}$ GeV. All the charged fermion masses are fitted at the see-saw scale, $M_N\\simeq M_R \\simeq 4 \\times 10^{13}$ GeV which is obtained with Majorana coupling $f_0 \\simeq 1$. Using a constrained parametrization in which CP-violation originates only from quark sector, besides other predictions made in the neutrino sector, the reactor mixing angle is found to be $\\theta_{13} \\simeq 3^{\\circ} - 5^{\\circ}$ which is in the range accessible to ongoing and planned experiments. The leptonic Dirac phase turns out to be $\\delta \\sim 2.9- 3.1$ radians with Jarlskog invariant $J \\sim 2.95 \\times 10^{-5} - 10^{-3}$.", "label": 1, "domain": "academic", "token_count": 352, "matched_pair_id": "conditionality_00062", "split": "train"}
{"id": "conditionality_train_pos_0216", "text": ") and the dollar amount in subsection (c)(4) shall be increased by an amount equal to-- ``(1) such dollar amount, multiplied by ``(2) the cost-of-living adjustment determined under section 1(f)(3) for the calendar year in which the taxable year begins, determined by substituting `calendar year 2011' for `calendar year 1992' in subparagraph (B) thereof. Any increase determined under the preceding sentence shall be rounded to the nearest multiple of $10.''. (b) Clerical Amendment.--The table of sections for part IV of subchapter A of chapter 1 of such Code is amended by inserting after the item relating to section 32 the following new item: ``Sec. 32A. Income disparity credit.''. (c) Effective Date.--The amendments made by this section shall apply to taxable years beginning after December 31, 2011. SEC. 3. ACCELERATION OF EGTRRA SUNSET. (a) In General.--Section 901 of the Economic Growth and Tax Relief Reconciliation Act of 2001 is amended by striking ``December 31, 2012'' and inserting ``December 31, 2011''. (b) Effective Date.--The amendment made by this section shall take effect as if included in the enactment of the Economic Growth and Tax Relief Reconciliation Act of 2001. SEC. 4. ACCELERATION OF JGTRRA SUNSET. (a) In General.--Section 303 of the Jobs and Growth Tax Relief Reconciliation Act of 2003 is amended by striking ``December 31, 2012'' and inserting ``December 31, 2011''. (b) Effective Date.--The amendment made by this section shall take effect as if included in the enactment of the Jobs and Growth Tax Relief Reconciliation Act of 2003.", "label": 1, "domain": "government", "token_count": 382, "matched_pair_id": "conditionality_01049", "split": "train"}
{"id": "conditionality_train_pos_0217", "text": "House Majority Whip Steve Scalise of Louisiana is in critical condition after he was was shot Wednesday morning at a congressional baseball practice, according to the MedStar Washington Hospital Center. RELATED: GOP baseball shooting: Rep. Scalise among victims in 'critical' condition The hospital released an update on Scalise's condition around 8:15 p.m. The statement reads: Congressman Steve Scalise sustained a single rifle shot to the left hip. The bullet traveled across his pelvis, fracturing bones, injuring internal organs, and causing severe bleeding. He was transported in shock to MedStar Washington Hospital Center, a Level I Trauma Center. He underwent immediate surgery, and an additional procedure to stop bleeding. He has received multiple units of blood transfusion. His condition is critical, and he will require additional operations. We will provide periodic updates. According to a statement released by Scalise's office, the congressman was taken to MedStar Washington Hospital Center and underwent surgery. The statement added he was in good spirits and spoke to his wife by phone prior to surgery. CBS News reported shortly before 10 a.m. that House Majority Leader Kevin McCarthy said Scalise was out of surgery. Rep. Mo Brooks, R-Ala., said several other people also were hit, including two law enforcement officers. The shooter is identified as James T. Hodgkinson, 66, of Belleville, Illinois. Videos claiming to be recorded during the shooting have started to appear online. WARNING: CONTENT MAY BE DISTURBING TO VIEWERS AND IT HAS NOT BEEN EDITED FOR LANGUAGE. Scalise represents the state's 1st Congressional District, which includes Jefferson, Lafourche, Orleans, Plaquemines, St. Bernard, St. Tammany, Tangipahoa and Terrebonne parishes. Gov. John Bel Edwards joined members of the Louisiana Legislature and the public in a prayer for Congressman Scalise in the Louisiana State Capitol Rotunda. The governor also spoke during the gathering. RELATED: Statements from government officials regarding congressional baseball practice shooting The Alexandria Police Department reported five people were taken to the hospital for treatment. Officials said the investigation is ongoing, but the city is safe. Police Chief Michael Brown said the shooting happened just after 7 a.m. He added the FBI will be taking over the investigation. A spokesman with the FBI said it is too early in the investigation to say if this was an act of terrorism or whether members of Congress were being directly targeted in the shooting.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00593", "split": "train"}
{"id": "conditionality_train_pos_0218", "text": "The phase of Super-Soft-Source (SSS) emission of the sixth recorded outburst of the recurrent nova RS Oph was observed twice with Chandra and once with XMM-Newton. The observations were taken on days 39.7, 54.0, and 66.9 after outburst. We confirm a 35-sec period on day 54.0 and found that it originates from the SSS emission and not from the shock. We discus the bound-free absorption by neutral elements in the line of sight, resonance absorption lines plus self-absorbed emission line components, collisionally excited emission lines from the shock, He-like intersystem lines, and spectral changes during an episode of high-amplitude variability. We find a decrease of the oxygen K-shell absorption edge that can be explained by photoionization of oxygen. The absorption component has average velocities of -1286+-267 km/s on day 39.7 and of -771+-65 km/s on day 66.9. The wavelengths of the emission line components are consistent with their rest wavelengths as confirmed by measurements of non-self absorbed He-like intersystem lines. We have evidence that these lines originate from the shock rather than the outer layers of the outflow and may be photoexcited in addition to collisional excitations. We found collisionally excited emission lines that are fading at wavelengths shorter than 15A that originate from the radiatively cooling shock. On day 39.5 we find a systematic blue shift of -526+-114 km/s from these lines. We found anomalous He-like f/i ratios which indicates either high densities or significant UV radiation near the plasma where the emission lines are formed. During the phase of strong variability the spectral hardness light curve overlies the total light curve when shifted by 1000sec. This can be explained by photoionization of neutral oxygen in the line of sight if the densities of order 10^{10}-10^{11} cm^{-3}.", "label": 1, "domain": "academic", "token_count": 403, "matched_pair_id": "conditionality_00006", "split": "train"}
{"id": "conditionality_train_pos_0219", "text": "If you thought Apple’s Face ID spelled the end of the fingerprint sensor, think again. Synaptics Inc., a company that creates touchpads and fingerprint sensors, has unveiled the next-generation Synaptics Clear ID, a fingerprint sensor that sits just under the glass of a smartphone. As smartphone manufacturers shrink the bezels around a screen, there’s less space for a fingerprint sensor on the front of the phone. Fingerprint sensors are used to unlock smartphones, and even access sensitive content like a banking app. Many Android manufacturers place these sensors on the back of the phone, so it doesn’t affect the bezel-less trend. Some — like OnePlus, LG, and Samsung — offer facial unlocking technology via the selfie camera. The sensor is two times faster than 3D facial recognition. With the iPhone X, Apple went all in on Face ID, going so far as to remove its fingerprint technology, Touch ID. The move has led analysts to believe more Android manufacturers will invest in facial-recognition 3D cameras next year. Synaptics thinks both rear fingerprint sensors and facial unlocking technology are not ideal. If your phone is sitting on a table, you have to pick it up to access the rear fingerprint sensor — the same is true to have it recognize your face. Apple’s Face ID also caused the iPhone X to have an “irregular-shaped display,” also known as the “notch,” to cram the tech in. Synaptics’ Clear ID FS9500 is a mass-production-ready sensor the company will sell to smartphone manufacturers. It works under OLED displays, which most flagship smartphones use, and it’s quite different from a traditional sensor. The fingerprint sensor on your phone now is capacitive, using electric current to capture your imprint. Clear ID is an ultra-thin optical sensor that captures your print with light emitting from the OLED panel on the smartphone. The full process works like this: The sensor detects the finger, the OLED display lights up the finger, the sensor scans the fingerprint, and the “matcher” verifies the image and confirms the imprint is yours, granting you access. The sensor can be placed anywhere on the screen the manufacturer wants, though Synaptics offers some general guidelines. The Clear ID sensor can work on rigid or flexible displays, and the company told Digital Trends it should work even if the phone has a screen protector, or if the screen is wet. Synaptics said the sensor is two times faster than 3D facial recognition, unlocking", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00710", "split": "train"}
{"id": "conditionality_train_pos_0220", "text": "corporation shall keep, at its principal office, a record of the names of all members having the right to vote in any proceeding of the corporation. (c) Right To Inspect Books and Records.--All books and records of the corporation may be inspected by any member having the right to vote, or by any agent or attorney of such member, for any proper purpose, at any reasonable time. (d) Application of State Law.--No provision of this section may be construed to contravene any applicable State law. SEC. 11. AUDIT OF FINANCIAL TRANSACTIONS. The first section of the Act entitled ``An Act to provide for audit of accounts of private corporations established under the Federal law'', approved August 30, 1964 (36 U.S.C. 1101), is amended by adding at the end of the following: ``Ukrainian American Veterans, Incorporated.''. SEC. 12. ANNUAL REPORT. The corporation shall annually submit to the Congress a report concerning the activities of the corporation during the preceding fiscal year. The annual report shall be submitted at the same time as is the report of the audit required by section 11. The report shall not be printed as a public document. SEC. 13. RESERVATION OF RIGHT TO AMEND OR REPEAL CHAPTER. The right to amend or repeal this Act is expressly reserved to the Congress. SEC. 14. DEFINITIONS. For purposes of this Act-- (1) the term ``corporation'' means the Ukrainian American Veterans, Incorporated; and (2) the term ``State'' means any of the several States, the District of Columbia, the Commonwealth of Puerto Rico, the Commonwealth of the Northern Mariana Islands, the Virgin Islands, Guam, American Samoa, the Trust Territories of the Pacific Islands, or any other territory or possessions of the United States. SEC. 15. TAX EXEMPT STATUS. The corporation shall maintain its status as an organization exempt from taxation as provided in the Internal Revenue Code of 1986. SEC. 16. TERMINATION. The charter granted in this Act shall expire if the corporation fails to comply with any provisions of this Act.", "label": 1, "domain": "government", "token_count": 446, "matched_pair_id": "conditionality_00850", "split": "train"}
{"id": "conditionality_train_pos_0221", "text": "Compact binary mergers are prime sources of gravitational waves, targeted by current and next generation detectors. The question \"what is the observable electromagnetic (EM) signature of a compact binary merger?\" is an intriguing one with crucial consequences to the quest for gravitational waves. We present a large set of numerical simulations that focus on the electromagnetic signals that emerge from the dynamically ejected sub-relativistic material. These outflows produce on a time scale of a day macronovae - short-lived IR to UV signals powered by radioactive decay. The interaction of this outflow with the surrounding matter inevitably leads to a long-lasting remnant. The expected radio signals of these remnants last longer than a year, when the sub-relativistic ejecta dominate the emission. We discuss their detectability in 1.4 GHz and 150 MHz and compare it with the detectability of short GRBs' orphan afterglows (which are produced by a different component of this outflow). Mergers with characteristics similar to those of the Galactic neutron star binary population (similar masses and typical circum-merger Galactic disk density of ~1cm^-3) taking place at the detection horizon of advanced GW detectors (300 Mpc) yield 1.4 GHz [150 MHz] signals of ~50 [300] microJy. The signal on time scales of weeks, is dominated by the mildly and/or ultra-relativistic outflow, which is not accounted for by our simulations, and is expected to be even brighter. Upcoming all sky surveys are expected to detect a few dozen, and possibly more, merger remnants at any given time thereby providing robust lower limits to the mergers rate even before the advanced GW detectorsbecome operational. Macronovae from the same distance peak in the IR to UV range at an observed magnitude that may be as bright as 22-23 about 10 hours after the merger but dimmer, redder and longer if the opacity is larger.", "label": 1, "domain": "academic", "token_count": 393, "matched_pair_id": "conditionality_00443", "split": "train"}
{"id": "conditionality_train_pos_0222", "text": "can change things, that bit of jealousy seeing your rivals raising trophies aloft. In the early 90s, Down (twice), Donegal and Derry won All-Ireland titles. Every other county in the north was supporting them. It's something unique to the northern counties and it’s something you don’t get in the other three provinces. Through the tough times of the troubles, our identity was even more important. To those looking on from over the border, we were often viewed as outcasts. My own club is on the border with Armagh, but when Derry won the All-Ireland in '93 the village was packed out for the Derry team on their way home. Tyrone looked on hoping some day it would be them. That day, thankfully did come. I mentioned earlier life skills and it’s well documented the many advantages that you can take from the various battles on the field of play. There are huge benefits for people as individuals in terms of what they can learn from playing team sports. The attributes that make you a good footballer or hurler - hard work and discipline - are things that stand to you in your work life. I would like to think that football has taught me a fair bit in how to deal with situations. You play games of football and you are faced with a lot of adversity at times. You have to learn to overcome such adversity. I know players at inter-county level have put their careers on hold because of their dedication to the game. I would counterbalance that by saying that performing at a unique level teaches you a lot about the work-related environment. Teams will sit down and set goals for the year and that's something people at work will do on a regular basis. It's not surprising that businesses bring in sports people to provide insights into how you build a successful team. So much of what they have to say is about maintaining discipline and the commitment to excel in whatever you do. After winning my All-Irelands, I was on cloud nine. Life was great. Confidence was oozing out of every pore and dealing with the likes of the media was no problem. My aim was always to try and reach my potential. You think you will never get to your potential, but you will always try to get as close as you can. My motto was to aim for perfection and if I end up a wee bit short, well it’s not so far behind to leave you disappointed.", "label": 1, "domain": "news", "token_count": 496, "matched_pair_id": "conditionality_00761", "split": "train"}
{"id": "conditionality_train_pos_0223", "text": "Spitzer spectroscopy has revealed that ~80% of submm galaxies (SMGs) are starburst (SB) dominated in the mid-infrared. Here we focus on the remaining ~20% that show signs of harboring powerful active galactic nuclei (AGN). We have obtained Spitzer-IRS spectroscopy of a sample of eight SMGs which are candidates for harboring powerful AGN on the basis of IRAC color-selection (S8/S4.5>2; i.e. likely power-law mid-infrared SEDs). SMGs with an AGN dominating (>50%) their mid-infrared emission could represent `missing link' sources in an evolutionary sequence involving a major merger. First of all, we detect PAH features in all of the SMGs, indicating redshifts from 2.5-3.4, demonstrating the power of the mid-infrared to determine redshifts for these optically faint dusty galaxies. Secondly, we see signs of both star-formation (from the PAH features) and AGN activity (from continuum emission) in our sample: 62% of the sample are AGN-dominated in the mid-infrared with a median AGN content of 56%, compared with <30% on average for typical SMGs, revealing that our IRAC color selection has successfully singled out sources with proportionately more AGN emission than typical SB-dominated SMGs. However, we find that only about 10% of these AGN dominate the bolometric emission of the SMG when the results are extrapolated to longer infrared wavelengths, implying that AGN are not a significant power source to the SMG population overall, even when there is evidence in the mid-infrared for substantial AGN activity. When existing samples of mid-infrared AGN-dominated SMGs are considered, we find that S8/S4.5>1.65 works well at selecting mid-infrared energetically dominant AGN in SMGs, implying a duty cycle of ~15% if all SMGs go through a subsequent mid-infrared AGN-dominated phase in the proposed evolutionary sequence.", "label": 1, "domain": "academic", "token_count": 427, "matched_pair_id": "conditionality_00203", "split": "train"}
{"id": "conditionality_train_pos_0224", "text": "We use the Mars Regional Atmospheric Modeling System (MRAMS) to simulate lake storms on Mars, finding that intense localized precipitation will occur for lake size >=10^3 km^2. Mars has a low-density atmosphere, so deep convection can be triggered by small amounts of latent heat release. In our reference simulation, the buoyant plume lifts vapor above condensation level, forming a 20km-high optically-thick cloud. Ice grains grow to 200 microns radius and fall near (or in) the lake at mean rates up to 1.5 mm/hr water equivalent (maximum rates up to 6 mm/hr water equivalent). Because atmospheric temperatures outside the surface layer are always well below 273K, supersaturation and condensation begin at low altitudes above lakes on Mars. In contrast to Earth lake-effect storms, lake storms on Mars involve continuous precipitation, and their vertical velocities and plume heights exceed those of tropical thunderstorms on Earth. Convection does not reach above the planetary boundary layer for lakes <<10^3 km^2 or for atmospheric pressure >O(10^2) mbar. Instead, vapor is advected downwind with little cloud formation. Precipitation occurs as snow, and the daytime radiative forcing at the land surface due to plume vapor and storm clouds is too small to melt snow directly (<+10 W/m^2). However, if orbital conditions are favorable, then the snow may be seasonally unstable to melting and produce runoff to form channels. We calculate the probability of melting by running thermal models over all possible orbital conditions and weighting their outcomes by probabilities given by Laskar et al., 2004. We determine that for an equatorial vapor source, sunlight 15% fainter than at present, and snowpack with albedo 0.28 (0.35), melting may occur with 4%(0.1%) probability. This rises to 56%(12%) if the ancient greenhouse effect was modestly (6K) greater than today.", "label": 1, "domain": "academic", "token_count": 411, "matched_pair_id": "conditionality_00298", "split": "train"}
{"id": "conditionality_train_pos_0225", "text": ". Pulaski County Circuit Judge Wendell Griffen placed a temporary restraining order on the state's ability to use the second drug in its lethal injection protocol — vecuronium bromide. Pharmaceutical company McKesson Medical-Surgical claimed the Department of Corrections essentially duped them in acquiring the drug, stating that they sold the vecuronium bromide under the pretense that it would be used for health reasons — not an execution. The state's director of the department of corrections, Wendy Kelly, disputed the charge in testimony on Thursday. But it was the judge in the pharmaceutical company's case who developed intrigue Friday evening. Soon after Griffen scheduled a hearing for Tuesday morning, he joined a protest of the executions outside the governor's mansion. To depict the inmate's experience on the Arkansas death house gurney, he strapped himself to a cot on the sidewalk outside Hutchinson's home. Judge Wendell Griffen portrays a prisoner on a gurney during a protest against executions in front of the governor's mansion in Little Rock, Ark. on April 14, 2017. Mitchell McCoy / KARK The state attorney general's office is now seeking to have him removed from the case and Republican lawmakers want him to leave the bench altogether, stating that he did not act impartially. \"As a public opponent of capital punishment, Judge Griffen should have recused himself from this case,\" said the state attorney general's spokesman, Judd Deere. Man on cot is judge who just blocked execution of seven brutal murderers. Who thinks he's impartial & fair in death-penalty cases? https://t.co/VrUOSvCcdz — Tom Cotton (@TomCottonAR) April 15, 2017 But for now, that case floats in a new state of legal limbo. McKesson, the pharmaceutical company, is seeking to drop its lawsuit and vacate the temporary restraining order against its drug after Baker's temporary injunction, but it plans to bring its lawsuit up again if the 8th Circuit dismissed the stay.", "label": 1, "domain": "news", "token_count": 412, "matched_pair_id": "conditionality_00735", "split": "train"}
{"id": "conditionality_train_pos_0226", "text": "os, undefeated? YM; Towards the end. We care about the game, like I said we wanted to win the game, but it was not about what the results showed, it was about what we did for our people in Puerto Rico. We were down (in the championship game) by seven, eight runs and you see the people in the stands chanting, screaming, dancing and having fun. That’s the point, when you play for your country and you see the people enjoying the game, being Puerto Rican that is the reason. LS: Yadier, you have been lucky playing in the biggest of games in baseball (World Series) and you have been in the World Classic games. What is the difference? YM: I have not been lucky, I have been blessed. I work hard for that and both are amazing. I play for St. Louis, but when you play in the World Classic your playing for your parents, for your cousins, for your uncles. It’s about your grandma; it’s about your grandpa, its different. Obviously you care about wining, but the classic is about your country. LS: All of you guys did so much more than many even politicians, or other leaders were able to do by bringing an entire country and people together. Congratulations. Also what do you think of Latino Sports having an award for the Latino players? YM: That’s the goal no matter where you are at to represent your country. You can be Dominican, Mexican from Venezuela wherever you come from your going to put your best and when you see the support that our people bring to us every night here in the states that is amazing. It makes you work harder, it makes you want to do the best that you can do for them. It’s an amazing feeling. LS: So hopefully, before this season ends we in Latino Sports want to make sure that you have something to take with you that your grandchildren will remember, a museum piece (both laugh. A LatinoMVP award painting by famed artist, James Fiorentino). YM: Thank you, thank you. It’s a great honor for me to be able to receive that. Hopefully, I can be there for that day, I’m going to do by best to be there, but if not, it is a great honor and I want you to know that.", "label": 1, "domain": "news", "token_count": 474, "matched_pair_id": "conditionality_00644", "split": "train"}
{"id": "conditionality_train_pos_0227", "text": "In a further development of a deterministic planet-formation model (Ida & Lin 2004), we consider the effect of type-I migration of protoplanetary embryos due to their tidal interaction with their nascent disks. During the early embedded phase of protostellar disks, although embryos rapidly emerge in regions interior to the ice line, uninhibited type-I migration leads to their efficient self-clearing. But, embryos continue to form from residual planetesimals at increasingly large radii, repeatedly migrate inward, and provide a main channel of heavy element accretion onto their host stars. During the advanced stages of disk evolution (a few Myr), the gas surface density declines to values comparable to or smaller than that of the minimum mass nebula model and type-I migration is no longer an effective disruption mechanism for mars-mass embryos. Over wide ranges of initial disk surface densities and type-I migration efficiency, the surviving population of embryos interior to the ice line has a total mass several times that of the Earth. With this reservoir, there is an adequate inventory of residual embryos to subsequently assemble into rocky planets similar to those around the Sun. But, the onset of efficient gas accretion requires the emergence and retention of cores, more massive than a few M_earth, prior to the severe depletion of the disk gas. The formation probability of gas giant planets and hence the predicted mass and semimajor axis distributions of extrasolar gas giants are sensitively determined by the strength of type-I migration. We suggest that the observed fraction of solar-type stars with gas giant planets can be reproduced only if the actual type-I migration time scale is an order of magnitude longer than that deduced from linear theories.", "label": 1, "domain": "academic", "token_count": 339, "matched_pair_id": "conditionality_00018", "split": "train"}
{"id": "conditionality_train_pos_0228", "text": "A wind energy development company is ‘disappointed’ at a decision by planners to reject its scheme for a 10-turbine wind farm on Fulbeck Airfield. South Kesteven District Council officers have refused the application for the 110m-high wind turbines under delegated powers. Should the applicant, Energiekontor, want to appeal the decision to the Planning Inspectorate it has six months to do so. Michael Briggs from Energiekontor UK, said: “We are obviously very disappointed with the council’s decision to refuse the planning application, as will be the hundreds of people who have written in to express their support for the project. “The wind farm would have delivered many benefits to the local and wider area which are now in doubt, particularly in relation to the economy, as numerous local construction companies were hoping the project would come forward. “At the same time, we fully understand the reasons why many have expressed their objections to the project and have always tried to do our best to address those concerns. “But the council was of the view that concerns in relation to landscape and cultural heritage issues were not outweighed by the benefits from the wind farm. We will need to look at the council’s reasons closely with our team before deciding what next for Fulbeck Airfield.” Planning officers said they refused the wind farm on the former wartime airfield on a number of grounds, including its potentially adverse visual and physical impact on the landscape and on the settings of numerous ‘high grade’ heritage assets. Concerns were also raised over an adverse impact on air safety through interference with aircraft radar and conflict with government policy. They further pointed to a Written Ministerial Statement from June 18, 2015, in which it states wind energy development should be in areas specified in local plans as being suitable for such development, and that wind farms should have the backing of local people. Local campaigning residents are delighted and relieved having seen a smaller project two miles away at Temple Hill rejected two years ago. Paul Miley of local anti-wind farm group reVOLT/VETO said: “Now the community asks that the developer respects local democracy and does not seek to appeal this decision.” He said: “An appeal would be an expensive and time consuming process both for the council and the community.” However, he did say ‘local people are ready to continue the fight if needed’.", "label": 1, "domain": "news", "token_count": 477, "matched_pair_id": "conditionality_00547", "split": "train"}
{"id": "conditionality_train_pos_0229", "text": "if the custodial account would, except for the fact that it is not a trust, constitute an individual investment account described in subsection (b). For purposes of this title, in the case of a custodial account treated as a trust by reason of the preceding sentence, the custodian of such account shall be treated as the trustee thereof. ``(g) Reports.--The trustee of an individual investment account shall make such reports regarding such account to the Secretary and to the individual for whose benefit the account is maintained with respect to contributions, distributions, and such other matters as the Secretary may require under regulations. The reports required by this subsection shall be filed at such time and in such manner and furnished to such individuals at such time and in such manner as may be required by those regulations.''. (b) Deduction Allowed in Arriving at Adjusted Gross Income.-- Subsection (a) of section 62 of such Code (defining adjusted gross income) is amended by inserting after paragraph (17) the following new paragraph: ``(18) Individual investment account contributions.--The deduction allowed by section 222 (relating to individual investment accounts).'' (c) Individual Investment Accounts Exempt From Estate Tax.--Part III of subchapter A of chapter 11 of such Code is amended by redesignating section 2046 as section 2047 and by inserting after section 2045 the following new section: ``SEC. 2046. INDIVIDUAL INVESTMENT ACCOUNTS. ``Notwithstanding any other provision of law, there shall be excluded from the value of the gross estate of the value of any individual investment account (as defined in section 222(b)). Section 1014 shall not apply to such accounts.'' (d) Tax on Prohibited Transactions.--Section 4975 of such Code (relating to prohibited transactions) is amended-- (1) by adding at the end of subsection (c) the following new paragraph: ``(6) Special rule for individual investment accounts.--An individual for whose benefit an individual investment account is established shall be exempt from the tax imposed by this section with respect to any transaction concerning such account (which would otherwise be taxable under this section) if, with respect to such transaction, the account ceases to be an individual investment account by reason of the application of section 222(d)(2)(A) to such account.''; and (2) in subsection (e)(1), by striking ``or'' at the end of subparagraph (E", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00918", "split": "train"}
{"id": "conditionality_train_pos_0230", "text": "Given a group G, the model \\mathcal{G}(G,p) denotes the probability space of all Cayley graphs of G where each element of the generating set is chosen independently at random with probability p. Given a family of groups (G_k) and a c \\in \\mathbb{R}_+ we say that c is the threshold for diameter 2 for (G_k) if for any \\varepsilon > 0 with high probability \\Gamma \\in \\mathcal{G}(G_k,p) has diameter greater than 2 if p \\leqslant \\sqrt{(c - \\eps)\\frac{\\log{n}}{n}} and diameter at most 2 if p \\geqslant \\sqrt{(c + \\eps)\\frac{\\log{n}}{n}}. In [5] we proved that if c is a threshold for diameter 2 for a family of groups (G_k) then c \\in [1/4,2] and provided two families of groups with thresholds 1/4 and 2 respectively. In this paper we study the question of whether every c \\in [1/4,2] is the threshold for diameter 2 for some family of groups. Rather surprisingly it turns out that the answer to this question is negative. We show that every c \\in [1/4,4/3] is a threshold but a c \\in (4/3,2] is a threshold if and only if it is of the form 4n/(3n-1) for some positive integer n.", "label": 1, "domain": "academic", "token_count": 324, "matched_pair_id": "conditionality_00422", "split": "train"}
{"id": "conditionality_train_pos_0231", "text": "The impact of a random disorder potential on the dynamical properties of Bose Einstein condensates is a very wide research field. In microcavities, these studies are even more crucial than in the condensates of cold atoms, since random disorder is naturally present in the semiconductor structures. In this chapter, we consider a stable condensate, defined by a chemical potential, propagating in a random disorder potential, like a liquid flowing through a capillary. We analyze the interplay between the kinetic energy, the localization energy, and the interaction between particles in 1D and 2D polariton condensates. The finite life time of polaritons is taken into account as well. In the first part, we remind the results of [G. Malpuech et al. Phys. Rev. Lett. 98, 206402 (2007).] where we considered the case of a static condensate. In that case, the condensate forms either a glassy insulating phase at low polariton density (strong localization), or a superfluid phase above the percolation threshold. We also show the calculation of the first order spatial coherence of the condensate versus the condensate density. In the second part, we consider the case of a propagating non-interacting condensate which is always localized because of Anderson localization. The localization length is calculated in the Born approximation. The impact of the finite polariton life time is taken into account as well. In the last section we consider the case of a propagating interacting condensate where the three regimes of strong localization, Anderson localization, and superfluid behavior are accessible. The localization length is calculated versus the system parameters. The localization length is strongly modified with respect to the non-interacting case. It is infinite in the superfluid regime whereas it is strongly reduced if the fluid flows with a supersonic velocity.", "label": 1, "domain": "academic", "token_count": 387, "matched_pair_id": "conditionality_00439", "split": "train"}
{"id": "conditionality_train_pos_0232", "text": "Assuming that the well-confirmed non-classical rotational inertia (NCRI) effect in solid $^4$He, suggested by Leggett, indicates supersolid behavior, we make a number of remarks about both theory and experiment. (1) The long-wavelength, low-frequency (\"hydrodynamic\") part of the theory of Andreev and Lifshitz has nine variables, and thus must have nine modes. We find a new mode associated with lattice point diffusion (and thus vacancy diffusion); it may explain the absence of supersolid behavior in low-frequency pressure-driven flow. (2) The observed upper limit for the NCRI fraction (NCRIf) of about 20%, in disordered samples, is more-or-less the same as the already predicted upper limit for the superfluid fraction of a well-ordered crystal; we argue that this may not be a coincidence. (3) The negative experimental evidence for a second propagating hydrodynamic mode (expected to be fourth sound-like) may be due to the long relaxation times $\\tau$ at low temperature $T$; only for frequencies satisfying $\\omega\\tau\\ll1$ does the hydrodynamic theory apply. (4) The fundamental principles of quantum mechanics imply that Bose-Einstein condensation is not necessary to define a quantum-mechanical phase; therefore the absence of a finite condensate fraction $f_{0}$ does not necessarily imply the absence of superfluidity. (5) Just as vortices should avoid occupied lattice sites to provide a vortex-lattice interaction, the lattice should interact with the vortices to provide a lattice-vortex interaction; thus dislocations should interact with vortices, whose motion is affected by rotation. We discuss some experimental implications for the vortex liquid model, shear response, hysteresis, and relaxation.", "label": 1, "domain": "academic", "token_count": 368, "matched_pair_id": "conditionality_00143", "split": "train"}
{"id": "conditionality_train_pos_0233", "text": "By using a string-inspired modular invariant supergravity, which was proved well to explain WMAP observations appropriately, a mechanism of supersymmetry breaking (SSB) and Gravitino Production just after the end of inflation are investigated. Supersymmetry is broken mainly by F-term of the inflaton superfield and the Goldstino is identified to be inflatino in this model, which fact is shown numerically. By using the canonically normalized and diagonalized scalars, the decay rates of these fields are calculated, for both the $T$ and $Y$ into gravitinos. Non-thermal production of gravitinos is not generated from the inflaton (dilaton), since the inflaton mass is lighter than gravitino, but they are produced by the decay of modular field $T$ and scalar field $Y$. Because the reheating temperature $T_R$ is about order $\\sim O(10^{10})$ GeV and the mass of gravitino is $3.16 \\times 10^{12}$ GeV, it is not reproduced after the reheating of the universe. The gravitinos are produced almost instantly just after the end of inflation through $Y$ and $T$, not from inflaton. Because the decay time appears very rapid, gravitinos disappear before the BBN stage of the universe. The effects of the lightest supersymmetric particles (LSP) produced by gravitinos may be important to investigate more carefully, if the LSP's are the candidate of dark matter.", "label": 1, "domain": "academic", "token_count": 315, "matched_pair_id": "conditionality_00201", "split": "train"}
{"id": "conditionality_train_pos_0234", "text": "We study spontaneous symmetry breaking in a system of two parallel quasi-one-dimensional traps, equipped with optical lattices (OLs) and filled with a Bose-Einstein condensate (BEC). The cores are linearly coupled by tunneling. Analysis of the corresponding system of linearly coupled Gross-Pitaevskii equations (GPEs) reveals that spectral bandgaps of the single GPE split into subgaps. Symmetry breaking in two-component BEC solitons is studied in cases of the attractive (AA) and repulsive (RR) nonlinearity in both traps; the mixed situation, with repulsion in one trap and attraction in the other (RA), is considered too. In all the cases, stable asymmetric solitons are found, bifurcating from symmetric or antisymmetric ones (and destabilizing them), in the AA and RR systems, respectively. In either case, bi-stability is predicted, with a nonbifurcating stable branch, either antisymmetric or symmetric, coexisting with asymmetric ones. Solitons destabilized by the bifurcation tend to rearrange themselves into their stable asymmetric counterparts. The impact of a phase mismatch, between the OLs in the two cores is also studied. Also considered is a related model, for a binary BEC in a single-core trap with the OL, assuming that the two species (representing different spin states of the same atom) are coupled by linear interconversion. In that case, the symmetry-breaking bifurcations in the AA and RR models switch their character, if the inter-species nonlinear interaction becomes stronger than the intra-species nonlinearity.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00005", "split": "train"}
{"id": "conditionality_train_pos_0235", "text": "one of those bald cap masks with the Bozo hair and glasses and nose and then she walked me around the back lot. Related: Critic's Notebook: Carrie Fisher, Child of Hollywood and Droll Observer of Celebrity The lengths I would go to hear her laugh - there were no limits. I loved her and loved making her laugh. She would do these crazy things and make me do these crazy things, but I really don't think they were crazy after all. In a way, it was a defense mechanism for her. She was so off the wall, she could use it as protection. Part of what was so poignant about her was that she was vulnerable, that there was this glimmer of a little girl that was so appealing and it roused the protective nature in my personality. I'm grateful that we stayed friends and got to have this second act with the new movies. I think it was reassuring to her that I was there, the same person, that she could trust me, as critical as we could sometimes be with each other. We ran the gamut over the years, where we were in love with each other, where we hated each other's guts. \"I'm not speaking to you, you're such a judgmental, royal brat!\" We went through it all. It's like we were a family. When you were in her good graces, you couldn't have more fun with any person on the planet. She was able to make you feel like you were the most important thing in her life. I think that's a really rare quality. And then you could go 180 degrees opposite, where you were furious with one another and wouldn't speak for weeks and weeks. But that's all part of what makes a relationship complete. It's not all one sided. Like I say, she was a handful. She was high maintenance. But my life would have been so much drabber and less interesting if she hadn't been the friend that she was.", "label": 1, "domain": "news", "token_count": 402, "matched_pair_id": "conditionality_00571", "split": "train"}
{"id": "conditionality_train_pos_0236", "text": "Assuming the dark matter is made entirely from neutralinos, we re-visit the role of their annihilation on the temperature of diffuse gas in the high redshift universe. We consider neutralinos of particle mass 36 GeV and 100 GeV, respectively. The former is able to produce ~7 electron/positron particles per annihilation through the fremionic channel, and the latter ~53 particles assuming a purely bosonic channel. High energy electron/positron particles up-scatter the Cosmic Microwave Background (CMB) photons into higher energies via the inverse-Compton scattering. The process produces a power-law electron/positron energy spectrum of index -1 in the energy range of interest, independent of the initial energy distribution. The corresponding energy spectrum of the up-scattered photons is a power-law of index -1/2, if absorption by the gas is not included. The scattered photons photo-heat the gas by releasing electrons which deposit a fraction (14%)of their energy as heat into the ambient medium. For uniformly distributed neutralinos the heating is insignificant. The effect is greatly enhanced by the clumping of neutralinos into dense haloes. We use a time-dependent clumping model which takes into account the damping of density fluctuations on mass scales smaller than ~10^{-6}M_sol. With this clumping model, the heating mechanism boosts the gas temperature above that of the CMB after a redshift of z 30. By z\\approx 10 the gas temperature is nearly 100 times its temperature when no heating is invoked. Similar increase is obtained for the two neutralino masses considered.", "label": 1, "domain": "academic", "token_count": 326, "matched_pair_id": "conditionality_00021", "split": "train"}
{"id": "conditionality_train_pos_0237", "text": "The growth of the supermassive black holes (BHs) that reside at the centres of most galaxies is intertwined with the physical processes that drive the formation of the galaxies themselves. The evolution of the relations between the mass of the BH, m_BH, and the properties of its host therefore represent crucial aspects of the galaxy formation process. We use a cosmological simulation, as well as an analytical model, to investigate how and why the scaling relations for BHs evolve with cosmic time. We find that a simulation that reproduces the observed redshift zero relations between m_BH and the properties of its host galaxy, as well as the thermodynamic profiles of the intragroup medium, also reproduces the observed evolution in the ratio m_BH/m_s for massive galaxies, although the evolution of the m_BH/sigma relation is in apparent conflict with observations. The simulation predicts that the relations between m_BH and the binding energies of both the galaxy and its dark matter halo do not evolve, while the ratio m_BH/m_halo increases with redshift. The simple, analytic model of Booth & Schaye (2010), in which the mass of the BH is controlled by the gravitational binding energy of its host halo, quantitatively reproduces the latter two results. Finally, we can explain the evolution in the relations between m_BH and the mass and binding energy of the stellar component of its host galaxy for massive galaxies (m_s~10^11 M_sun) at low redshift (z<1) if these galaxies grow primarily through dry mergers.", "label": 1, "domain": "academic", "token_count": 318, "matched_pair_id": "conditionality_00225", "split": "train"}
{"id": "conditionality_train_pos_0238", "text": "Equivocation rate has been widely used as an information-theoretic measure of security after Shannon[10]. It simplifies problems by removing the effect of atypical behavior from the system. In [9], however, Merhav and Arikan considered the alternative of using guessing exponent to analyze the Shannon's cipher system. Because guessing exponent captures the atypical behavior, the strongest expressible notion of secrecy requires the more stringent condition that the size of the key, instead of its entropy rate, to be equal to the size of the message. The relationship between equivocation and guessing exponent are also investigated in [6][7] but it is unclear which is a better measure, and whether there is a unifying measure of security. Instead of using equivocation rate or guessing exponent, we study the wiretap channel in [2] using the success exponent, defined as the exponent of a wiretapper successfully learn the secret after making an exponential number of guesses to a sequential verifier that gives yes/no answer to each guess. By extending the coding scheme in [2][5] and the converse proof in [4] with the new Overlap Lemma 5.2, we obtain a tradeoff between secrecy and reliability expressed in terms of lower bounds on the error and success exponents of authorized and respectively unauthorized decoding of the transmitted messages. From this, we obtain an inner bound to the region of strongly achievable public, private and guessing rate triples for which the exponents are strictly positive. The closure of this region is equivalent to the closure of the region in Theorem 1 of [2] when we treat equivocation rate as the guessing rate. However, it is unclear if the inner bound is tight.", "label": 1, "domain": "academic", "token_count": 343, "matched_pair_id": "conditionality_00065", "split": "train"}
{"id": "conditionality_train_pos_0239", "text": "purpose of including such information in the timely reports required under this paragraph; and ``(III) ensure that when a crime of violence (as defined in section 16 of title 18, United States Code) is reported to a campus security authority, the authority reports the crime to local law police agencies; ``(ii) establish policies or procedures for training campus security authorities and the campus security authority coordinator; and ``(iii) employ or designate an individual or other entity to conduct such training using the policies or procedures established under clause (ii), upon receiving approval from the Secretary for such individual or other entity to conduct such training.''; (4) in paragraph (13)-- (A) by striking ``Upon'' and inserting ``(A) Upon''; (B) by inserting ``which distinguishes between institutional neglect and intentional misrepresentation or withholding of information,'' after ``this subsection,''; (C) by inserting ``, except that the Secretary shall impose a larger civil penalty in the case of an institution of higher education determined to have intentionally violated this subsection, as compared to an institution of higher education that violated this subsection as a result of institutional neglect. An intentional violation of this subsection by an institution of higher education shall be subject to criminal prosecution'' after ``under section 487(c)(3)(B)''; and (D) by adding at the end the following: ``(B) Prior to making a determination described in subparagraph (A) with respect to an institution of higher education, the Secretary shall-- ``(i) conduct an investigation with respect to the institution; and ``(ii) provide the institution with a timeline of the investigation and a preliminary report that includes the reasons for conducting such investigation.''; and (5) in paragraph (17), before the period insert the following: ``or any individual because such individual provided information or made a complaint to a law enforcement agency relating to the implementation of any provision of this subsection, provided that the individual acted in good faith when providing such information or making such complaint''.", "label": 1, "domain": "government", "token_count": 401, "matched_pair_id": "conditionality_00959", "split": "train"}
{"id": "conditionality_train_pos_0240", "text": "We study the quantum phase transition from a super solid phase to a solid phase of rho = 1/2 for the extended Bose-Hubbard model on the honeycomb lattice using first principles Monte Carlo calculations. The motivation of our study is to quantitatively understand the impact of theoretical input, in particular the dynamical critical exponent z, in calculating the critical exponent nu. Hence we have carried out four sets of simulations with beta = 2N^{1/2}, beta = 8N^{1/2}, beta = N/2, and beta = N/4, respectively. Here beta is the inverse temperature and N is the numbers of lattice sites used in the simulations. By applying data collapse to the observable superfluid density rho_{s2} in the second spatial direction, we confirm that the transition is indeed governed by the superfluid-insulator universality class. However we find it is subtle to determine the precise location of the critical point. For example, while the critical chemical potential (mu/V)_c occurs at (mu/V)_c = 2.3239(3) for the data obtained using beta = 2N^{1/2}, the (mu/V)_c determined from the data simulated with beta = N/2 is found to be (mu/V)_c = 2.3186(2). Further, while a good data collapse for rho_{s2}N can be obtained with the data determined using beta = N/4 in the simulations, a reasonable quality of data collapse for the same observable calculated from another set of simulations with beta = 8N^{1/2} can hardly be reached. Surprisingly, assuming z for this phase transition is determined to be 2 first in a Monte Carlo calculation, then a high quality data collapse for rho_{s2}N can be achieved for (mu/V)_c ~ 2.3184 and nu ~ 0.7 using the data obtained with beta = 8N^{1/2}. Our results imply that one might need to reconsider the established phase diagrams of some models if the accurate location of the critical point is crucial in obtaining a conclusion.", "label": 1, "domain": "academic", "token_count": 439, "matched_pair_id": "conditionality_00303", "split": "train"}
{"id": "conditionality_train_pos_0241", "text": "We have detected narrow HI 21cm and CI absorption at $z \\sim 1.4 - 1.6$ towards Q0458$-$020 and Q2337$-$011, and use these lines to test for possible changes in the fine structure constant $\\alpha$, the proton-electron mass ratio $\\mu$, and the proton gyromagnetic ratio $g_p$. A comparison between the HI 21cm and CI line redshifts yields $\\Delta X/X = [+6.8 \\pm 1.0] \\times 10^{-6}$ over $0 < <z> \\le 1.46$, where $X = g_p \\alpha^2/\\mu$, and the errors are purely statistical, from the gaussian fits. The simple line profiles and the high sensitivity of the spectra imply that statistical errors in this comparison are an order of magnitude lower than in previous studies. Further, the CI lines arise in cold neutral gas that also gives rise to HI 21cm absorption, and both background quasars are core-dominated, reducing the likelihood of systematic errors due to local velocity offsets between the hyperfine and resonance lines. The dominant source of systematic error lies in the absolute wavelength calibration of the optical spectra, which appears uncertain to $\\sim 2$ km/s, yielding a maximum error in $\\Delta X/X$ of $\\sim 6.7 \\times 10^{-6}$. Including this, we obtain $\\Delta X/X = [+6.8 \\pm 1.0 (statistical) \\pm 6.7 (max. systematic)] \\times 10^{-6}$ over $0 < <z> \\le 1.46$. Using literature constraints on $\\Delta \\mu/\\mu$, this is inconsistent with claims of a smaller value of $\\alpha$ from the many-multiplet method, unless fractional changes in $g_p$ are larger than those in $\\alpha$ and $\\mu$.", "label": 1, "domain": "academic", "token_count": 396, "matched_pair_id": "conditionality_00202", "split": "train"}
{"id": "conditionality_train_pos_0242", "text": ".''. (b) Effective Date.--The amendment made by this section shall apply to taxable years beginning after December 31, 2013. SEC. 105. LIMITATION ON DEDUCTION FOR TERTIARY INJECTANTS. (a) In General.--Section 193 of the Internal Revenue Code of 1986 is amended by adding at the end the following new subsection: ``(d) Application With Respect to Major Integrated Oil Companies.-- This section shall not apply to amounts paid or incurred by a taxpayer in any taxable year in which such taxpayer is a major integrated oil company (as defined in section 167(h)(5)(B)).''. (b) Effective Date.--The amendment made by this section shall apply to amounts paid or incurred in taxable years beginning after December 31, 2013. Subtitle B--Outer Continental Shelf Oil and Natural Gas SEC. 111. REPEAL OF OUTER CONTINENTAL SHELF DEEP WATER AND DEEP GAS ROYALTY RELIEF. (a) In General.--Sections 344 and 345 of the Energy Policy Act of 2005 (42 U.S.C. 15904, 15905) are repealed. (b) Limitation on Application.--The repeal under subsection (a) shall not affect the application of the repealed sections with respect to any lease sale for which a notice of sale is published before the date of enactment of this Act. TITLE II--BUDGETARY EFFECTS SEC. 201. DEFICIT REDUCTION. The net amount of any savings realized as a result of the enactment of this Act and the amendments made by this Act (after any expenditures authorized by this Act and the amendments made by this Act) shall be deposited in the Treasury and used for Federal budget deficit reduction or, if there is no Federal budget deficit, for reducing the Federal debt in such manner as the Secretary of the Treasury considers appropriate.", "label": 1, "domain": "government", "token_count": 392, "matched_pair_id": "conditionality_00970", "split": "train"}
{"id": "conditionality_train_pos_0243", "text": "Using Chebyshev polynomials combined with some mild combinatorics, we provide a new formula for the analytical planar limit of a random matrix model with a one-cut potential $V$. For potentials $V(x)=x^{2}/2-\\sum_{n\\ge1}a_{n}x^{n}/n$, as a power series in all $a_{n}$, the formal Taylor expansion of the analytic planar limit is exactly the formal planar limit. In the case $V$ is analytic in infinitely many variables $\\{a_{n}\\}_{n\\ge1}$ (on the appropriate spaces), the planar limit is also an analytic function in infinitely many variables and we give quantitative versions of where this is defined. Particularly useful in enumerative combinatorics are the gradings of $V$, $V_{t}(x)=x^{2}/2-\\sum_{n\\ge1}a_{n}t^{n/2}x^{n}/n$ and $V_{t}(x)=x^{2}/2-\\sum_{n\\ge3}a_{n}t^{n/2 -1}x^{n}/n$. The associated planar limits $F(t)$ as functions of $t$ count planar diagram sorted by the number of edges respectively faces. We point out a method of computing the asymptotic of the coefficients of $F(t)$ using the combination of the \\emph{wzb} method and the resolution of singularies. This is illustrated in several computations revolving around the important extreme potential $V_{t}(x)=x^{2}/2+\\log(1-\\sqrt{t}x)$ and its variants. This particular example gives a quantitive and sharp answer to a conjecture of t'Hoofts which states that if the potential is analytic, the planar limit is also analytic.", "label": 1, "domain": "academic", "token_count": 384, "matched_pair_id": "conditionality_00264", "split": "train"}
{"id": "conditionality_train_pos_0244", "text": "A new determination of the sound horizon scale in angular coordinates is presented. It makes use of ~ 0.6 x 10^6 Luminous Red Galaxies, selected from the Sloan Digital Sky Survey imaging data, with photometric redshifts. The analysis covers a redshift interval that goes from z=0.5 to z=0.6. We find evidence of the Baryon Acoustic Oscillations (BAO) signal at the ~ 2.3 sigma confidence level, with a value of theta_{BAO} (z=0.55) = (3.90 \\pm 0.38) degrees, including systematic errors. To our understanding, this is the first direct measurement of the angular BAO scale in the galaxy distribution, and it is in agreement with previous BAO measurements. We also show how radial determinations of the BAO scale can break the degeneracy in the measurement of cosmological parameters when they are combined with BAO angular measurements. The result is also in good agreement with the WMAP7 best-fit cosmology. We obtain a value of w_0 = -1.03 \\pm 0.16 for the equation of state parameter of the dark energy, Omega_M = 0.26 \\pm 0.04 for the matter density, when the other parameters are fixed. We have also tested the sensitivity of current BAO measurements to a time varying dark energy equation of state, finding w_a = 0.06 \\pm 0.22 if we fix all the other parameters to the WMAP7 best-fit cosmology.", "label": 1, "domain": "academic", "token_count": 328, "matched_pair_id": "conditionality_00326", "split": "train"}
{"id": "conditionality_train_pos_0245", "text": "from warehouse for consumption, on or after December 1, 2007. (f) Reliquidation of Entries.-- (1) In general.--Notwithstanding section 514 of the Tariff Act of 1930 (19 U.S.C. 1514) or any other provision of law and subject to the provisions of paragraph (2), the U.S. Customs and Border Protection shall, not later than 90 days after the receipt of a request described in paragraph (2), liquidate or reliquidate as applicable any entry described in paragraph (4) at the applicable rate under subchapter II of chapter 99 of the Harmonized Tariff Schedule of the United States, as amended by subsection (d). (2) Requests.--Liquidation or reliquidation may be made under paragraph (1) with respect to an entry described in paragraph (4) only if-- (A) a request therefore is filed with U.S. Customs and Border Protection not later than 90 days after the date of the enactment of this Act; and (B) the request contains sufficient information to enable U.S. Customs and Border Protection to locate the entry or reconciliation entry if it cannot be located. (3) Payment of amounts owed.--Any amounts owed by the United States pursuant to the liquidation or reliquidation of any entry under paragraph (1) shall be paid, with interest, not later than 180 days after the date of such liquidation or reliquidation. (4) Entries described.--The entries referred to in paragraph (1) are the entries, or withdrawals from warehouse for consumption, of goods to which duty-free treatment is provided by subsections (d) and (e)-- (A) that was made on or after December 1, 2007; and (B) with respect to which there would have been no duty if subsection (d) of this Act had applied to such entry or withdrawal.", "label": 1, "domain": "government", "token_count": 395, "matched_pair_id": "conditionality_01060", "split": "train"}
{"id": "conditionality_train_pos_0246", "text": "With high resolution (0.46kpc/h), adaptive mesh-refinement Eulerian cosmological hydrodynamic simulations we compute properties of O VI and O VII absorbers from the warm-hot intergalactic medium (WHIM). Our new simulations are in broad agreement with previous simulations, with ~40% of the intergalactic medium being in the WHIM at z=0. It is found (1) The amount of gas in the WHIM at temperature below and above 10^6K is about equal within uncertainties. (1) Our simulations are in excellent agreement with observed properties of O VI absorbers, with respect to the line incidence rate and Doppler width-column density relation. (2) Velocity structures within absorbing regions are a significant, and for large Doppler width clouds, a dominant contributor to the Doppler widths of both O VI and O VII absorbers. A non-negligible fraction (in number and mass) of O VI and O VII clouds can arise from gas of temperature lower than 10^5, until the Doppler width is well in excess of 100km/s. (3) Strong O VI absorbers are predominantly collisionally ionized. About (61%, 57%, 39%) of O VI absorbers in the column density ranges of log N(OVI) cm^2=(12.5-13,13-14,>14) have temperature lower than 10^5K. (4) Quantitative prediction is made for the presence of broad and shallow O VI lines, which current observations may have largely missed. Upcoming observations by COS may be able to provide a test. (5) The reported 3 sigma upper limit on the mean column density of coincidental O VII lines at the location of detected O VI lines by Yao et al is above the predicted value by a factor of 2.5-4. (6) The claimed observational detection of O VII lines by Nicastro et al, if true, is 2 sigma above what our simulations predict.", "label": 1, "domain": "academic", "token_count": 412, "matched_pair_id": "conditionality_00398", "split": "train"}
{"id": "conditionality_train_pos_0247", "text": "this act or any compact may be construed to limit the applicability of any Federal law or to diminish or to otherwise impair the jurisdiction of any action taken pursuant to any compact. ``(C) State authority preserved.--Except as expressly provided in this Act, nothing contained in this Act expands, diminishes, or otherwise affects State law. ``(3) Restricted Use of Regional Solid Waste Disposal Facilities.-- Any authority in a compact to restrict the use of regional solid waste disposal facilities under the compact to the disposal of solid waste generated within the compact region shall not take effect before each of the following occurrs: ``(1) January 1, 1995; and ``(2) the Congress by law consents to the compact. ``(4) Congressional Review.--Each compact shall: Provide, That every 5 years after the compact has taken effect the Congress may by law withdraw its consent. ``(c) Alternative Solid Waste Disposal Methods.-- ``(1) Not later than 12 months after the date of enactment of the Solid Waste Compact Act of 1993, the Environmental Protection Agency shall, in consultation with the States and other interested persons, identify potential alternative management programs for the control of solid waste, and establish and publish technical guidance regarding the implementation of such programs. ``(2) Not later than 24 months after the date of the enactment of the Solid Waste Compact Act of 1993, the Environmental Protection Agency shall, in consultation with the States and other interested persons, identify and publish all relevant technical information regarding the technologies pursuant to subsection (1) that a State or compact must provide to the Agency in order to pursue such programs, together with the requirements that such facilities must meet, in the judgment of the Agency, if pursued as an alternative to traditional solid waste management.", "label": 1, "domain": "government", "token_count": 356, "matched_pair_id": "conditionality_00891", "split": "train"}
{"id": "conditionality_train_pos_0248", "text": "who've recently resigned after allegations of sexual misconduct. Humphreys has not responded to requests from The Associated Press for comment. ___ 12:15 p.m. The president of the University of Oklahoma is distancing himself from comments made by a Board of Regents member who compared gay people to pedophiles. University President David Boren said in a statement Monday that board member and former Oklahoma City Mayor Kirk Humphreys wasn't speaking on behalf of the university. Boren also says he doesn't share Humphreys' views and that the university is a diverse and inclusive family. Humphreys made the comments during a local TV public affairs show that aired over weekend on KFOR-TV. He also compared gay people to politicians who've recently resigned after allegations of sexual misconduct. A staffer at Humphreys' office says he was out of town Monday and unavailable to comment. Humphreys also didn't immediately reply to an email seeking comment from The Associated Press. ___ 10:55 a.m. A former Oklahoma City mayor and member of the University of Oklahoma Board of Regents is being criticized for comparing gay people to pedophiles. Kirk Humphreys made the comments over the weekend on KFOR-TV's public affairs show. He also compared gay people to politicians who've recently resigned after allegations of sexual misconduct. LGBTQ advocacy group Freedom Oklahoma has called for his removal from the board if he doesn't apologize. Executive Director Troy Stevenson says Humphreys' comments were disheartening and dangerous for LGBTQ youth who are already harassed and bullied. A staffer at Humphreys' office said he was out of town Monday and unavailable to comment. Stevenson said Monday his group will protest an Oklahoma City real estate project that belongs to Humphreys' family business if he doesn't apologize.", "label": 1, "domain": "news", "token_count": 357, "matched_pair_id": "conditionality_00508", "split": "train"}
{"id": "conditionality_train_pos_0249", "text": "Angela Eagle and Imran Ahmed’s new book “The New Serfdom“, a 400-page hatchet job on the great liberal thinker Friedrich Hayek, is being lauded with praise in Labour circles, most effusively from Nick Cohen. Guido must come to Hayek’s defence in the face of their rewriting of history. The New Serfdom is a reminder that, even as the relatively moderate challenger to Corbyn, Eagle is still a liberty-hating socialist who opposes free markets and fundamentally values the state over the freedom of the individual. Even Ed Miliband’s office warned that Ahmed was “dangerously left-wing” when he became a Shadow Cabinet adviser. Their book condemns the “veneration of markets”, the “infiltration of marketisation” into the public sector, capitalism’s promotion of competition, the “toxic culture” of admiring those who succeed, and calls for a Labour government to create an “empowered state… pursuing a reinvigorated democratic socialism”. It wants to sweep back Thatcher’s trade union reforms, regulate the food and drink industry to the hilt and put taxes through the roof. It offers a depressing view of Britain today, talking the country down as “divided and resentful”, dismisses capitalist liberal democracy as a “con”, calls Hayek a “liar” with “extreme views” who inspired Thatcher and her “successor” Trump, and claims Brexit is evidence of “the extreme right on the march”. According to the respected academic Chris Hanretty, Eagle’s Wallasley seat voted 53% to Leave… The history of the last century comprehensively proved correct Hayek’s central assertion that socialism morphs into totalitarianism. He was proved right when the Keynesian post-war consensus collapsed and Thatcher used his ideas – “this is what we believe” – to turn the economy around. The New Serfdom is an unashamedly socialist critique of the last forty years of British political life, and so is as dangerous and wrong as you would expect. The key question for Eagle and Ahmed: if they truly believe in their socialist vision for Britain, why did they try to stop Corbyn becoming Prime Minister?", "label": 1, "domain": "news", "token_count": 442, "matched_pair_id": "conditionality_00580", "split": "train"}
{"id": "conditionality_train_pos_0250", "text": "If the Commission determines that both of the remaining actions for election under paragraph (1) are in the public interest, then the manufacturer, distributor, or retailer shall elect to take one of those actions.''. (b) Hazardous Substances Amendment.--Section 15(b) of the Federal Hazardous Substances Act (15 U.S.C. 1274(b)) is amended-- (1) by striking ``Refund.--If'' and inserting ``Refund.-- Except as provided in paragraph (3), if''; (2) by striking ``(1) If'' and inserting ``(A) Repair.-- If''; (3) by striking ``(2)'' and inserting ``(B) Replacment.-- ''; (4) by striking ``(3)'' and inserting ``(C) Refund.--''; (5) by redesignating subparagraphs (A) and (B) of paragraph (3) as clauses (i) and (ii), respectively; (6) by striking ``An order'' the first place it appears and inserting ``(2) An order''; (7) by striking ``paragraph (3).'' and inserting ``paragraph (1)(C)''; and (8) by adding at the end thereof the following: ``(3) If the Commission determines, after affording opportunity for an informal hearing, that the action elected by a manufacturer, distributor, or retailer under paragraph (1)(A), (B), or (C) is not in the public interest, the Commission shall order the manufacturer, distributor, or retailer to take any other action described in paragraph that the Commission determines to be in the public interest. If the Commission determines that both of the remaining actions for election under paragraph (1) are in the public interest, then the manufacturer, distributor, or retailer shall elect to take one of those actions.''. (c) Discretionary Remedial Action Under the FHSA.--Section 1274(c) of the Federal Hazardous Substances Act (15 U.S.C. 1274(c) is amended-- (1) by striking ``(2) If'' and inserting ``(2) Except as provided in paragraph (3), if''; and (2) adding at the end thereof the following: ``(3) If the Commission determines, after affording opportunity for an informal hearing, that the action elected by a manufacturer, distributor, or retailer under paragraph (2)(A), (B), or (C) is not in", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01022", "split": "train"}
{"id": "conditionality_train_pos_0251", "text": "with a comprehensive understanding of gender, consent, and the critical issues at the center of the movement. Please read through their answers and jump into the comments with your thoughtful, balanced reactions. We think this is a discussion that is important and ongoing. Unsplash Lucia When I ask my guy friends, I haven’t found anyone who understands that they have a “gender.” They all think that the only thing that makes them a man is their junk, but I’m trying to understand the idea of gender outside of genitalia. Any chance you can help me with that — in straightforward terms? Dr. Casey Brienza, sociologist and author: Sex is determined by biology, whereas gender is determined by society and culture. Does a man have to show you his “junk” to assert his gender identity? Probably not. Other cues, such as dress, hairstyle, body language, speech patterns, etc. are usually sufficient, and the very fact that these may differ in different parts the world tells us that they are not inherent. Or, for that matter, immutable. Dr. Chauntelle Tibbals, sociologist and author: In sociology and social-psychology circles, this is often discussed as a (problematic, obvs) dimension of the “default person.” The default person is male, heterosexual, able-bodied, white, etc. As a society, we spent a lot of time using that default person/experience as the neutral guide for structuring society. So, to your question, we are talking “males don’t have a gender because they are conceptualized as the social default/generic”-type of thing. A gender is something that’s added in as an extra to move a human away from the “default” experience – and within this system and process, the penis has become a sort of symbolic embodiment of that default entity. It’s interesting to me too how this taps into interlocking systems of privileges and oppression. Like, a man may have none of those other “default” characteristics, but if he’s got that dick he’s somehow still plugged into the hierarchy in a socially advantageous way.", "label": 1, "domain": "news", "token_count": 429, "matched_pair_id": "conditionality_00562", "split": "train"}
{"id": "conditionality_train_pos_0252", "text": "If magnetic activity in outer stellar atmospheres is due to an interplay between rotation and subsurface convection, as is generally presumed, then one would not expect to observe indicators of activity in stars with T_eff > 8300 K. Any X-ray or ultraviolet line emission from hotter stars must be due either to a different mechanism or to an unresolved, active, binary companion. Due to their poor spatial resolution, X-ray instruments have been especially susceptible to source confusion. At wavelengths longward of 1216 Angstroms, the near ultraviolet spectra of stars hotter than this putative dividing line are dominated by photospheric continuum. We have used FUSE to obtain spectra of the subcoronal O VI emission lines, which lie at a wavelength where the photospheric continuum of the mid- and early-A stars is relatively weak. We observed 14 stars spanning a range in T_eff from 7720 to 10,000 K. Eleven of the 14 stars showed O VI emission lines, including 6 of the 8 targets with T_eff > 8300 K. At face value, this suggests that activity does not fall off with increasing temperature. However, the emission lines are narrower than expected from the projected rotational velocities of these rapidly-rotating stars, suggesting that the emission could come from unresolved late-type companions. Furthermore, the strength of the O VI emission is consistent with that expected from an unseen active K or M dwarf binary companinon, and the high x-ray to far uv luminosity ratios observed indicate that this must be the case. Our results are therefore consistent with earlier studies that have shown a rapid drop-off in activity at the radiative/convective boundary expected at T_eff about 8300 K, in agreement with conventional stellar structure models.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00067", "split": "train"}
{"id": "conditionality_train_pos_0253", "text": "Entire Community Of Muslims Are Rounded Up And Booted Out For Terrifying Reason Nearly 40,000 Pakastani workers were deported from Saudi Arabia since October 2016. The reasons? Visa violations and terror concerns. I’m sure that nobody will have a problem calling the Saudi Arabian government “Islamophobic” for this, right? Right? From Independent.co.uk: The Kingdom of Saudi Arabia has expelled almost 40,000 Pakistani migrant workers in the last four months, local media has reported. Over 39,000 people have been deported since October 2016 over visa violations and security concerns, the Saudi Gazette reported, citing unnamed interior ministry officials. As well as crimes including drug trafficking, forgery and theft, an unknown number of those removed from the country were suspected to have links to Isis and other extremist groups, the paper said. The alleged mass deportations come after a year of strikes and other unrest in the kingdom due to unpaid wages following the oil market’s decline and subsequent blow to the Saudi economy. Official Saudi statistics say that 243,000 Pakistanis were deported between 2012 – 2015. Mass deportations of migrant workers – which Human Rights Watch and other rights organisations say often involve illegal beatings and detainment in poor conditions – are fairly common. 2010 census figures show that 8.5 million of Saudi Arabia’s 27 million strong population, or around 30 per cent, are foreign nationals. According to a 2014 European University Institute report, there are approximately 900,000 people of Pakistani nationality currently employed in Saudi Arabia’s vast construction industry and other low-paid service jobs. I’m looking forward to hearing American liberals preach to Saudi Arabia about the need for “tolerance,” Maybe if you put another “Coexist” bumper sticker on your Prius, they’ll listen.", "label": 1, "domain": "news", "token_count": 372, "matched_pair_id": "conditionality_00678", "split": "train"}
{"id": "conditionality_train_pos_0254", "text": "-time employees of the Federal Government created under such program. (2) Appropriate congressional committees defined.--In this subsection, the term ``appropriate congressional committees'' means the following: (A) In the House of Representatives: (i) The Committee on Foreign Affairs. (ii) The Committee on Homeland Security. (iii) The Committee on the Judiciary. (iv) The Committee on Appropriations. (B) In the Senate: (i) The Committee on Foreign Relations. (ii) The Committee on Homeland Security and Governmental Affairs. (iii) The Committee on the Judiciary. (iv) The Committee on Appropriations. SEC. 6. SERVICES UPON ARRIVAL. (a) In General.--Aliens provided special immigrant status and visas pursuant to section 4 shall be eligible for the same resettlement assistance, programs, and benefits as refugees admitted under section 207 of the Immigration and Naturalization Act (8 U.S.C. 1157). The Secretary of of Health and Human Services, in cooperation with the Secretary of State, shall work with nongovernmental organizations to provide such assistance, programs, and benefits and ensure that such aliens are referred to refugee resettlement agencies. (b) Computer Literacy and Vocational Training.--The Secretary of State shall utilize existing programs of the Department of State and contracts between the Department and nongovernmental organizations to make available computer literacy programs and vocational training programs to aliens provided special immigrant status pursuant to section 4. (c) Rule of Construction.--Nothing in this section shall be construed as requiring the cooperation of nongovernmental organizations. SEC. 7. TRAINING AT THE DEPARTMENT OF STATE. Not later than 180 days after the date of the enactment of this Act, the Secretary of State shall establish a program in the Department of State to provide instruction in English as a second language, vocational training, computer training, employment services, and certain counseling services for Iraqis admitted to the United States as special immigrants. SEC. 8. SENSE OF CONGRESS. It is the sense of Congress that the United States should provide an orientation into life in the United States for Iraqi special immigrants under this Act who are newly admitted to the United States and should make all reasonable efforts to provide temporary safe haven for aliens described in section 4 who are applying for special immigrant status and visas if such aliens are in imminent danger in Iraq.", "label": 1, "domain": "government", "token_count": 485, "matched_pair_id": "conditionality_00969", "split": "train"}
{"id": "conditionality_train_pos_0255", "text": "We have seen that if \\phi: M_n(\\C) \\rightarrow M_n(\\C) is a unital q-positive map and \\nu is a type II Powers weight, then the boundary weight double (\\phi, \\nu) induces a unique (up to conjugacy) type II_0 E_0-semigroup. Let \\phi: M_n(\\C) \\rightarrow M_n(\\C) and \\psi: M_{n'}(\\C) \\rightarrow M_{n'}(\\C) be unital rank one q-positive maps, so for some states \\rho \\in M_n(\\C)^* and \\rho' \\in M_{n'}(\\C)^*, we have \\phi(A)=\\rho(A)I_n and \\psi(D) = \\rho'(D)I_{n'} for all A \\in M_n(\\C) and D \\in M_{n'}(\\C). We find that if \\nu and \\eta are arbitrary type II Powers weights, then (\\phi, \\nu) and (\\psi, \\eta) induce non-cocycle conjugate E_0-semigroups if \\rho and \\rho' have different eigenvalue lists. We then completely classify the q-corners and hyper maximal q-corners from \\phi to \\psi, obtaining the following result: If \\nu is a type II Powers weight of the form \\nu(\\sqrt{I - \\Lambda(1)} B \\sqrt{I - \\Lambda(1)})=(f,Bf), then the E_0-semigroups induced by (\\phi,\\nu) and (\\psi, \\nu) are cocycle conjugate if and only if n=n' and \\phi and \\psi are conjugate.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00249", "split": "train"}
{"id": "conditionality_train_pos_0256", "text": "If you’ve ever dreamed of quitting your job and fleeing to an island in the Mediterranean, now’s your chance. There are about 200 stone houses for sale in an Italian village for just $1.50. Ollolai, located on the island of Sardinia, is partaking in a project called “Case a 1 euro,” which is aimed at preserving the history and charm of Italian villages at risk of depopulation. “My crusade is to rescue our unique traditions from falling into oblivion,” Efisio Arbau, the mayor of Ollolai, told CNN. “Pride in our past is our strength. We’ve always been tough people and won’t allow our town to die.” Though the deal is enticing — Sardinia has nearly 2,000 kilometres of coastline and picturesque beaches — it comes with conditions. The homes are in need of major renovation. Anyone that purchases a house in Ollolai will need to refurbish it within three years, and according to CNN, renovations are likely to cost around $25,000. In the past 50 years, the town’s population has shrunk from 2,250 to 1,300 people. The Municipality of Ollolai hopes that these sales will help draw in new homeowners and preserve the village’s history. “The internet has lit up from joyous dreamers who want to pack it in and live the la dolce vita,” Canadian Jennifer Avventura wrote on her blog, My Sardinian Life. But as dreamy as it sounds to move there, the realities of living on an Italian island shouldn’t be overlooked. “You will need to have a basic understanding of the Italian language to get by with day-to-day activities,” she wrote. “Remember – you’re re-building a home and will need to contact builders, plumbers, electricians, the local town hall, possibly a lawyer, a notary to notarize the billions of documents that will need to be signed, stamped and stamped again. Can you do this in Italian?” Arbau said in a statement that the town has received more requests than they have homes, and due to the overwhelming number of applications, the deadline for applications was moved up to Feb. 7 at 2 p.m. “If you can get over those small hurdles and prepare yourself for a beautiful, simple life, deep within the folds of Sardinia’s glorious mountains – then do", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00654", "split": "train"}
{"id": "conditionality_train_pos_0257", "text": "), the person engaged in, or seeking to engage in, an activity described in such subsection shall-- ``(1) inform the individual of all the purposes for which the number will be utilized and the persons to whom the number will be known; and ``(2) obtain affirmatively expressed consent in writing. ``(d) Exceptions.--Nothing in this section shall be construed to prohibit any use of social security account numbers permitted or required under section 205(c)(2) of this Act, section 7(a)(2) of the Privacy Act of 1974 (5 U.S.C. 552a note; 88 Stat. 1909), or section 6109(d) of the Internal Revenue Code of 1986. ``(e) Civil Action in United States District Court; Damages; Attorneys Fees and Costs; Nonexclusive Nature of Remedy.-- ``(1) In general.--Any individual aggrieved by any act of any person in violation of this section may bring a civil action in a United States district court to recover-- ``(A) such preliminary and equitable relief as the court determines to be appropriate; and ``(B) the greater of-- ``(i) actual damages; and ``(ii) liquidated damages of $25,000 or, in the case of a violation that was willful and resulted in profit or monetary gain, $50,000. ``(2) Attorney's fees and costs.--In the case of a civil action brought under paragraph (1) in which the aggrieved individual has substantially prevailed, the court may assess against the respondent a reasonable attorney's fee and other litigation costs and expenses (including expert fees) reasonably incurred. ``(3) Statute of limitations.--No action may be commenced under this subsection more than 3 years after the date on which the violation was or should reasonably have been discovered by the aggrieved individual. ``(4) Nonexclusive remedy.--The remedy provided under this subsection shall be in addition to any other lawful remedy available to the individual. ``(f) Civil Money Penalties.-- ``(1) In general.--Any person who the Commissioner of Social Security determines has violated this section shall be subject, in addition to any other penalties that may be prescribed by law, to-- ``(A) a civil money penalty of not more than $25,000 for each such violation, and ``(B) a civil money penalty of not more than $500,000, if violations have occurred with such frequency as to constitute a general business practice.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00857", "split": "train"}
{"id": "conditionality_train_pos_0258", "text": "Share This Video Facebook Twitter EMAIL Every day it gets harder and harder to tell if Kanye West has gone off the deep end, if he’s 100 percent sincere, or if he’s just elaborately trolling us all for attention with a ridiculous spate of GOOD Music albums supposedly on the way, but one thing is for sure: His weirdness is consistently and bizarrely captivating, entertaining, and surprising — you never know what he’ll do next. I love the way Candace Owens thinks — KANYE WEST (@kanyewest) April 21, 2018 Case in point, his latest stunt involved an unexpected response to Hot 97’s Ebro Darden after the gruff radio personality lambasted West yesterday during his show. After West tweeted in support of conservative commentator Candace Owens, Ebro and his cohosts delivered a rollicking , 16-minute explainer for his seemingly Trump-supporting tweets and why they hurt, confused, or angered many of Kanye’s longtime fans and supporters. While they weren’t exactly kind to Kanye, they weren’t totally disrespectful either, surmising that ultimately, Kanye likes Trump because Trump was nice to him at a low point in his life. Yes Kanye just called the show while we were in the middle of a break and just kept repeating \"I love you\" to Ebro…eventually he said lets meet in person off air and then talk on the air — RosenbergTelevision (@Rosenbergradio) April 24, 2018 Today, though, Kanye called into Hot 97 to speak his piece, except what actually happened is he simply kept repeating “I love you” in response to Ebro’s questions, to the confusion of the hosts. He seemed to be in good spirits, but refused to talk about the music or his tweets, offering to speak with Ebro in person before giving a radio interview. If it’s a troll, it’s one of the most masterful mind games anyone’s ever played with the rambunctious Ebro In The Morning crew, and if it was just “New” Kanye’s pacifistic way of blowing off steam, it certainly seems more productive than his old approach to radio host provocation. In either case, Kanye’s certainly built even more anticipation for his new music — if only so we can all finally get an explanation of just what he’s thinking lately.", "label": 1, "domain": "news", "token_count": 483, "matched_pair_id": "conditionality_00559", "split": "train"}
{"id": "conditionality_train_pos_0259", "text": "Netflix Even if you’re still in the middle of Lost in Space from Netflix’s April additions, the month of May is nearly upon us and the streaming giant already has a whole of new shows and films in store for its subscribers. From the fourth season of the hugely popular Unbreakable Kimmy Schmidt to a seemingly endless array of new comedy specials from Tig Notaro, John Mulaney, and more, the sheer amount of new content Netflix is putting out next month is insurmountable. Then again, to make room for it all the streamer will have to sacrifice a few expired licenses, like the Martin Scorsese classic Goodfellas. ARRIVING The fourth season of Unbreakable Kimmy Schmidt (5/30) Share This Video Facebook Twitter EMAIL We haven’t heard much from Kimmy Schmidt (Ellie Kemper) since season three dropped in May of last year. That’s all about to change at the end of May, when the popular comedy series will return to Netflix for its fourth season. Slated for a split debut on Wednesday, May 30th, the first half of season four (six episodes) will be available to watch in full. As for the second half of the new season, they will be available to watch sometime “later in 2018.” No particular reason was given by Netflix back in February, though it probably has something to do with show creator Tina Fey’s busy schedule. DEPARTING Goodfellas says goodbye (5/1) Martin Scorsese’s 1990 film Goodfellas is an all-time cinematic classic, Tommy DeVito’s (Joe Pesci) crazed outbursts notwithstanding. The film was adapted from Nicholas Pileggi’s 1986 book Wiseguy, which chronicled the rise and fall of Henry Hill (Ray Liotta), a mobster who became an informant for the FBI. Anyone with a love of Scorsese films, Robert De Niro being Robert De Niro, or crime movies will love Goodfellas. Hence why, if you haven’t seen it already, now’s your chance before Netflix removes it on Tuesday, May 1st.", "label": 1, "domain": "news", "token_count": 438, "matched_pair_id": "conditionality_00564", "split": "train"}
{"id": "conditionality_train_pos_0260", "text": "If the second Betti number b_2 of a Sasaki-Einstein manifold Y^7 does not vanish, then M-theory on AdS_4 x Y^7 possesses \"topological\" U(1)^{b_2} gauge symmetry. The corresponding Abelian gauge fields come from three-form fluctuations with one index in AdS_4 and the other two in Y^7. We find black membrane solutions carrying one of these U(1) charges. In the zero temperature limit, our solutions interpolate between AdS_4 x Y^7 in the UV and AdS_2 x R^2 x squashed Y^7 in the IR. In fact, the AdS_2 x R^2 x squashed Y^7 background is by itself a solution of the supergravity equations of motion. These solutions do not appear to preserve any supersymmetry. We search for their possible instabilities and do not find any. We also discuss the meaning of our charged membrane backgrounds in a dual quiver Chern-Simons gauge theory with a global U(1) charge density. Finally, we present a simple analytic solution which has the same IR but different UV behavior. We reduce this solution to type IIA string theory, and perform T-duality to type IIB. The type IIB metric turns out to be a product of the squashed Y^7 and the extremal BTZ black hole. We discuss an interpretation of this type IIB background in terms of the (1+1)-dimensional CFT on D3-branes partially wrapped over the squashed Y^7.", "label": 1, "domain": "academic", "token_count": 328, "matched_pair_id": "conditionality_00211", "split": "train"}
{"id": "conditionality_train_pos_0261", "text": "Assuming a spherical symmetry, the extreme UV emitted by a very hot source ionizes low pressure molecular hydrogen making a transparent bubble of H II (Protons and electrons). For an increase of radius, intensity of extreme UV and temperature decrease, so that the plasma contains more and more atoms. A spherical shell, mainly of neutral atoms (H I) appears. If this shell is optically thick at Lyman frequencies of H I, it is superradiant and a competition of modes selects modes tangent to a sphere for which many atoms are excited. Thus, a shell of plasma emits, into a given direction, tangential rays showing a ring in which selected modes are brighter. While at Lyman frequencies, absorption of rays emitted by the source excites the atoms able to amplify the superradiance, a more powerful amplification of superradiance results from an induced scattering of the radial beams, which extends to feet of lines and progressively to the whole spectrum. Thermodynamics says that the brightness of radial and tangential beams tends to be equal; if the solid angle of observation is much larger for the ring than for the source, almost the whole light emitted by the source is transferred to the rings, and the source becomes invisible. Paradoxically, a glow due to incoherent scattering and impurities around the source remains visible. As the scattering decreases with the decrease of the radial intensity, the brightness of the ring decreases with radius. These characteristics are found in supernova remnant 1987A.", "label": 1, "domain": "academic", "token_count": 306, "matched_pair_id": "conditionality_00014", "split": "train"}
{"id": "conditionality_train_pos_0262", "text": "BARNEGAT – If you see or smell smoke in Barnegat on Wednesday, it is most likely a prescribed burn performed by the New Jersey Forest Fire Service. Prescribed burns are intentional fires set to clear out easily flammable brush before a wildfire does it. The area around Cloverdale Farms, by Cloverdale Road, will be the focus of the burn. It should take place between 8 a.m. and 8 p.m. The New Jersey State Forest Fire Service conducts burns throughout the state at the end of winter every year. The burns destroy fallen trees, branches, leaves, pine needles and other debris on the forest floor. “By burning them away now, we can reduce the risk of these materials serving as tinder for wildfires later in the year,” said Bill Edwards, chief of the state fire service. “This practice also improves the overall ecological health of our forests and grasslands.” The fire service expects to burn between 10,000 and 20,000 acres of forests and grasslands this season, they said. Most burns are on state-owned property. Because of the make-up of vegetation, the Pinelands region is the focus of much of the prescribed burning activity. During burns, personnel use hand-held torches to burn away debris on the forest floor, taking into account wind, moisture and other conditions. Last year, the Forest Fire Service responded to 1,065 wildfires, but 75 percent of them were a quarter acre or smaller. The largest was a 464-acre fire in Bass River State Forest in Burlington County. Residents are advised that they might see large plumes of smoke and might smell smoke for miles around. The burns will continue through the end of March, depending on weather. For more information, go to facebook.com/newjerseyforests or call 609-292-2977. If you are unsure if it is a controlled burn or a real forest fire, call 911 or 877-WARN-DEP.", "label": 1, "domain": "news", "token_count": 399, "matched_pair_id": "conditionality_00648", "split": "train"}
{"id": "conditionality_train_pos_0263", "text": "We investigate the effect of monopolar charge disorder on the classical fluctuation-induced interactions between randomly charged net-neutral dielectric slabs and discuss various generalizations of recent results (A. Naji et al., Phys. Rev. Lett. 104, 060601 (2010)) to highly inhomogeneous dielectric systems with and without statistical disorder correlations. We shall focus on the specific case of two generally dissimilar plane-parallel slabs, which interact across vacuum or an arbitrary intervening dielectric medium. Monopolar charge disorder is considered to be present on the bounding surfaces and/or in the bulk of the slabs, may be in general quenched or annealed and may possess a finite lateral correlation length reflecting possible `patchiness' of the random charge distribution. In the case of quenched disorder, the bulk disorder is shown to give rise to an additive long-range contribution to the total force, which decays as the inverse distance between the slabs and may be attractive or repulsive depending on the dielectric constants of the slabs. We show that in the case of two dissimilar slabs the net effect due to the interplay between the disorder-induced and the pure van der Waals interactions can lead to a variety of unusual non-monotonic interaction profiles between the dielectric slabs. In particular, when the intervening medium has a larger dielectric constant than the two slabs, we find that the net interaction can become repulsive and exhibit a potential barrier, while the underlying van der Waals force is attractive. On the contrary, when the intervening medium has a dielectric constant in between that of the two slabs, the net interaction can become attractive and exhibit a free energy minimum, while the pure van der Waals force is repulsive. Therefore, the charge disorder, if present, can drastically alter the effective interaction between net-neutral objects.", "label": 1, "domain": "academic", "token_count": 378, "matched_pair_id": "conditionality_00252", "split": "train"}
{"id": "conditionality_train_pos_0264", "text": "We present a test of different error estimators for 2-point clustering statistics, appropriate for present and future large galaxy redshift surveys. Using an ensemble of very large dark matter LambdaCDM N-body simulations, we compare internal error estimators (jackknife and bootstrap) to external ones (Monte-Carlo realizations). For 3-dimensional clustering statistics, we find that none of the internal error methods investigated are able to reproduce neither accurately nor robustly the errors of external estimators on 1 to 25 Mpc/h scales. The standard bootstrap overestimates the variance of xi(s) by ~40% on all scales probed, but recovers, in a robust fashion, the principal eigenvectors of the underlying covariance matrix. The jackknife returns the correct variance on large scales, but significantly overestimates it on smaller scales. This scale dependence in the jackknife affects the recovered eigenvectors, which tend to disagree on small scales with the external estimates. Our results have important implications for the use of galaxy clustering in placing constraints on cosmological parameters. For example, in a 2-parameter fit to the projected correlation function, we find that the standard bootstrap systematically overestimates the 95% confidence interval, while the jackknife method remains biased, but to a lesser extent. The scatter we find between realizations, for Gaussian statistics, implies that a 2-sigma confidence interval, as inferred from an internal estimator, could correspond in practice to anything from 1-sigma to 3-sigma. Finally, by an oversampling of sub-volumes, it is possible to obtain bootstrap variances and confidence intervals that agree with external error estimates, but it is not clear if this prescription will work for a general case.", "label": 1, "domain": "academic", "token_count": 352, "matched_pair_id": "conditionality_00085", "split": "train"}
{"id": "conditionality_train_pos_0265", "text": "(1) or (2)'' in paragraph (1)(C) (as so redesignated) and inserting ``subparagraph (A) or (B)''; and (4) by adding at the end the following new paragraph: ``(2) Additional requirements with respect to grantor retained annuities.--For purposes of subsection (a), in the case of an interest described in paragraph (1)(A) (determined without regard to this paragraph) which is retained by the transferor, such interest shall be treated as described in such paragraph only if-- ``(A) the right to receive the fixed amounts referred to in such paragraph is for a term of not less than 10 years, ``(B) such fixed amounts, when determined on an annual basis, do not decrease relative to any prior year during the first 10 years of the term referred to in subparagraph (A), and ``(C) the remainder interest has a value greater than zero determined as of the time of the transfer.''. (b) Effective Date.--The amendments made by this section shall apply to transfers made after December 31, 2010. TITLE IV--BUDGETARY EFFECTS SEC. 401. COMPLIANCE WITH PAYGO. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 334, "matched_pair_id": "conditionality_00865", "split": "train"}
{"id": "conditionality_train_pos_0266", "text": "The peculiar motion of the Earth causes a dipole anisotropy modulation in the distant galaxy distribution due to the aberration effect. However, the amplitude and angular direction of the effect is not necessarily the same as those of the cosmic microwave background (CMB) dipole anisotropy due to the growth of cosmic structures. In other words exploring the aberration effect may give us a clue to the horizon-scale physics perhaps related to the cosmic acceleration. In this paper we develop a method to explore the dipole angular modulation from the pixelized galaxy data on the sky properly taking into account the covariances due to the shot noise and the intrinsic galaxy clustering contamination as well as the partial sky coverage. We applied the method to the galaxy catalogs constructed from the Sloan Digital Sky Survey (SDSS) Data Release 6 data. After constructing the four galaxy catalogs that are different in the ranges of magnitudes and photometric redshifts to study possible systematics, we found that the most robust sample against systematics indicates no dipole anisotropy in the galaxy distribution. This finding is consistent with the expectation from the concordance Lambda-dominated cold dark matter model. Finally we argue that an almost full-sky galaxy survey such as LSST may allow for a significant detection of the aberration effect of the CMB dipole having the precision of constraining the angular direction to ~ 20 degrees in radius. Assuming a hypothetical LSST galaxy survey, we find that this method can confirm or reject the result implied from a stacked analysis of the kinetic Sunyaev-Zel'dovich effect of X-ray luminous clusters in Kashlinsky et al. (2008,2009) if the implied cosmic bulk flow is not extended out to the horizon.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00180", "split": "train"}
{"id": "conditionality_train_pos_0267", "text": "The pulsation periods of long period variables (LPVs) depend on their mass and helium abundance as well as on their luminosity and metal abundance. Comparison of the observed periods of LPVs in globular clusters with models is capable of revealing the amount of mass lost on the giant branch and the helium abundance.} {We aim to determine the amount of mass loss that has occurred on the giant branches of the low metallicity globular clusters NGC 362 and NGC 2808. We also aim to see if the LPVs in NGC 2808 can tell us about helium abundance variations in this cluster.} We have used optical monitoring of NGC 362 and NGC 2808 to determine periods for the LPVs in these clusters. We have made linear pulsation models for the pulsating stars in these clusters taking into account variations in mass and helium abundance. Reliable periods have been determined for 11 LPVs in NGC 362 and 15 LPVs in NGC 2808. Comparison of the observed variables with models in the logP - K diagram shows that mass loss of ~0.15-0.2 Msun is required on the first giant branch in these clusters, in agreement with estimates from other methods. In NGC 2808, there is evidence that a high helium abundance of Y~0.4 is required to explain the periods of several of the LPVs. It would be interesting to determine periods for LPVs in other Galactic globular clusters where a helium abundance variation is suspected to see if the completely independent test for a high helium abundance provided by the LPVs can confirm the high helium abundance estimates.", "label": 1, "domain": "academic", "token_count": 327, "matched_pair_id": "conditionality_00318", "split": "train"}
{"id": "conditionality_train_pos_0268", "text": "We combine VI photometry from OGLE-III with VVV and 2MASS measurements of E(J-K_{s}) to resolve the longstanding problem of the non-standard optical extinction toward the Galactic bulge. We show that the extinction is well-fit by the relation A_{I} = 0.7465*E(V-I) + 1.3700*E(J-K_{s}), or, equivalently, A_{I} = 1.217*E(V-I)(1+1.126*(E(J-K_{s})/E(V-I)-0.3433)). The optical and near-IR reddening law toward the inner Galaxy approximately follows an R_{V} \\approx 2.5 extinction curve with a dispersion {\\sigma}_{R_{V}} \\approx 0.2, consistent with extragalactic investigations of the hosts of type Ia SNe. Differential reddening is shown to be significant on scales as small as as our mean field size of 6', with the 1{\\sigma} dispersion in reddening averaging 9% of total reddening for our fields. The intrinsic luminosity parameters of the Galactic bulge red clump (RC) are derived to be (M_{I,RC}, \\sigma_{I,RC,0}, (V-I)_{RC,0}, \\sigma_{(V-I)_{RC}}, (J-K_{s})_{RC,0}) = (-0.12, 0.09, 1.06, 0.121, 0.66). Our measurements of the RC brightness, brightness dispersion and number counts allow us to estimate several Galactic bulge structural parameters. We estimate a distance to the Galactic center of 8.20 kpc, resolving previous discrepancies in distance determinations to the bulge based on I-band observations. We measure an upper bound on the tilt {\\alpha} \\approx 40{\\deg}. between the bar's major axis and the Sun-Galactic center line of sight, though our brightness peaks are consistent with predictions of an N-body model oriented at {\\alpha} \\approx 25{\\deg}. The number of RC stars suggests a total stellar mass for the Galactic bulge of 2.0*10^{10} M_{\\odot}, if one assumes a Salpeter IMF.", "label": 1, "domain": "academic", "token_count": 477, "matched_pair_id": "conditionality_00487", "split": "train"}
{"id": "conditionality_train_pos_0269", "text": "We present new analysis of 11 intermediate-age (1-2 Gyr) star clusters in the Large Magellanic Cloud based on Hubble Space Telescope imaging data. Seven of the clusters feature main sequence turnoff (MSTO) regions that are wider than can be accounted for by a simple stellar population, whereas their red giant branches indicate a single value of [Fe/H]. The star clusters cover a range in present-day mass from about 1E4 to 2E5 solar masses. We compare radial distributions of stars in the upper and lower parts of the MSTO region, and calculate cluster masses and escape velocities from the present time back to a cluster age of 10 Myr. Our main result is that for all clusters in our sample with estimated escape velocities > 15 km/s at an age of 10 Myr, the stars in the brightest half of the MSTO region are significantly more centrally concentrated than the stars in the faintest half AND more massive red giant branch and asymptotic giant branch stars. This is not the case for clusters with escape velocities < 10 km/s at an age of 10 Myr. We argue that the wide MSTO region of such clusters is mainly caused by to a 200 - 500 Myr range in the ages of cluster stars due to extended star formation within the cluster from material shed by first-generation stars featuring slow stellar winds. Dilution of this enriched material by accretion of ambient interstellar matter is deemed plausible if the spread of [Fe/H] in this ambient gas was very small when the second-generation stars were formed in the cluster.", "label": 1, "domain": "academic", "token_count": 326, "matched_pair_id": "conditionality_00329", "split": "train"}
{"id": "conditionality_train_pos_0270", "text": "Context. X-ray binaries are usually divided in persistent and transient sources. For ultracompact X-ray binaries (UCXBs), the mass transfer rate is expected to be a strong function of orbital period, predicting persistent sources at short periods and transients at long periods. Aims. For 14 UCXBs including two candidates, we investigate the long-term variability and average luminosity with the purpose of learning how often a source can be expected to be visible above a given luminosity, and we compare the derived luminosities with the theoretical predictions. Methods. We use data from the RXTE All-Sky Monitor because of its long-term, unbiased observations. Many UCXBs are faint, i.e., they have a count rate at the noise level for most of the time. Still, information can be extracted from the data, either by using only reliable data points or by combining the bright-end variability behavior with the time-averaged luminosity. Results. Luminosity probability distributions show the fraction of time that a source emits above a given luminosity. All UCXBs show significant variability and relatively similar behavior, though the time-averaged luminosity implies higher variability in systems with a period longer than 40 min. Conclusions. There is no large difference in the statistical luminosity behavior of what we usually call persistent and transient sources. UCXBs with a period below ~30 min have a time-averaged bolometric luminosity that is in reasonable agreement with estimates based on the theoretical mass transfer rate. Around 40 min the lower bound on the time-averaged luminosity is similar to the luminosity based on the theoretical mass transfer rate, suggesting these sources are indeed faint when not detected. Above 50 min some systems are much brighter than the theoretical mass transfer rate predicts, unless these systems have helium burning donors or lose additional angular momentum.", "label": 1, "domain": "academic", "token_count": 377, "matched_pair_id": "conditionality_00462", "split": "train"}
{"id": "conditionality_train_pos_0271", "text": "We present the first pilot study of jets from young stars conducted with X-shooter, on ESO/VLT. As it offers simultaneous, high quality spectra in the range 300-2500 nm X-shooter is uniquely important for spectral diagnostics in jet studies. We chose to probe the accretion/ejection mechanisms at low stellar masses examining two targets with well resolved continuous jets lying on the plane of the sky, ESO-HA 574 in Chamaleon I, and Par-Lup3-4 in Lupus III. The mass of the latter is close to the sub-stellar boundary (Mstar=0.13 Msun). A large number of emission lines probing regions of different excitation are identified, position-velocity diagrams are presented and mass outflow/accretion rates are estimated. Comparison between the two objects is striking. ESO-HA 574 is a weakly accreting star for which we estimate a mass accretion rate of log(\\dot{Macc}) = -10.8 \\pm 0.5 (in Msun/yr), yet it drives a powerful jet with \\dot{Mout} ~ 1.5-2.7 10^-9 Msun/yr. These values can be reconciled with a magneto-centrifugal jet acceleration mechanism only assuming that the presence of the edge-on disk severely depresses the luminosity of the accretion tracers. In comparison Par-Lup3-4 with stronger mass accretion (log(\\dot{Macc}) = -9.1 \\pm 0.4 Msun/yr), drives a low excitation jet with about \\dot{Mout} ~ 3.2 10^-10 Msun/yr in both lobes. Despite the low stellar mass, \\dot{Mout} / \\dot{Macc} for Par-Lup3-4 is at the upper limit of the range usually measured for young objects, but still compatible with a steady magneto-centrifugal wind scenario if all uncertainties are considered.", "label": 1, "domain": "academic", "token_count": 420, "matched_pair_id": "conditionality_00345", "split": "train"}
{"id": "conditionality_train_pos_0272", "text": "We present resolved Herschel images of circumbinary debris disks in the alpha CrB (HD139006) and beta Tri (HD13161) systems. We find that both disks are consistent with being aligned with the binary orbital planes. Though secular perturbations from the binary can align the disk, in both cases the alignment time at the distances at which the disk is resolved is greater than the stellar age, so we conclude that the coplanarity was primordial. Neither disk can be modelled as a narrow ring, requiring extended radial distributions. To satisfy both the Herschel and mid-IR images of the alpha CrB disk, we construct a model that extends from 1-300AU, whose radial profile is broadly consistent with a picture where planetesimal collisions are excited by secular perturbations from the binary. However, this model is also consistent with stirring by other mechanisms, such as the formation of Pluto-sized objects. The beta Tri disk model extends from 50-400AU. A model with depleted (rather than empty) inner regions also reproduces the observations and is consistent with binary and other stirring mechanisms. As part of the modelling process, we find that the Herschel PACS beam varies by as much as 10% at 70um and a few % at 100um. The 70um variation can therefore hinder image interpretation, particularly for poorly resolved objects. The number of systems in which circumbinary debris disk orientations have been compared with the binary plane is now four. More systems are needed, but a picture in which disks around very close binaries (alpha CrB, beta Tri, and HD 98800, with periods of a few weeks to a year) are aligned, and disks around wider binaries (99 Her, with a 50 yr period) are misaligned, may be emerging. This picture is qualitatively consistent with the expectation that the protoplanetary disks from which the debris emerged are more likely to be aligned if their binaries have shorter periods.", "label": 1, "domain": "academic", "token_count": 407, "matched_pair_id": "conditionality_00489", "split": "train"}
{"id": "conditionality_train_pos_0273", "text": "The 8 o'clock arc is a gravitationally lensed Lyman Break Galaxy (LBG) at redshift z=2.73 that has a star-formation rate (SFR) of 270 solar-mass/year (derived from optical and near-infrared spectroscopy). Taking the magnification of the system ~12 and the SFR into account, the expected flux density of any associated radio emission at 1.4 GHz is predicted to be just 0.1 mJy. However, the lens system is found to be coincident with a radio source detected in the NRAO Very Large Array (VLA) Sky Survey with a flux density of ~5 mJy. If this flux density is attributed to the lensed LBG then it would imply a SFR ~11000 solar-mass/year, in contrast with the optical and near-infrared derived value. We want to investigate the radio properties of this system, and independently determine the SFR for the LBG from its lensed radio emission. We have carried out new high resolution imaging with the VLA ain A and B-configurations at 1.4 and 5 GHz. We find that the radio emission is dominated by a radio-loud AGN associated with the lensing galaxy. The radio-jet from the AGN partially covers the lensed arc of the LBG, and we do not detect any radio emission from the unobscured region of the arc down to a 3 sigma flux-density limit of 108 micro-Jy/beam. Using the radio data, we place a limit of <750 solar-mass/year for the SFR of the LBG, which is consistent with the results from the optical and near-infrared spectroscopy. We expect that the sensitivity of the Expanded VLA will be sufficient to detect many high redshift LBGs that are gravitationally lensed after only a few hours of observing time. The high angular resolution provided by the EVLA will also allow detailed studies of the lensed galaxies and determine if there is radio emission from the lens.", "label": 1, "domain": "academic", "token_count": 423, "matched_pair_id": "conditionality_00262", "split": "train"}
{"id": "conditionality_train_pos_0274", "text": "unless agreed to by the small entity, in any enforcement action brought against a small entity by a Federal agency in any Federal-- (A) court; or (B) administrative proceeding; and (2) may not be the subject of discovery in any enforcement action brought against a small entity by a Federal agency in any Federal-- (A) court; or (B) administrative proceeding. (c) Application.--For purposes of subsection (b), the evidence described in this subsection is-- (1) a voluntary self-audit made in good faith; and (2) any report, finding, opinion, or any other oral or written communication made in good faith relating to such voluntary self-audit. (d) Exceptions.--Subsection (b) shall not apply if-- (1) the act or omission that forms the basis of the enforcement action is a violation of criminal law; or (2) the voluntary self-audit or the report, finding, opinion, or other oral or written communication was prepared for the purpose of avoiding disclosure of information required for an investigative, administrative, or judicial proceeding that, at the time of preparation, was imminent or in progress. TITLE II--MISCELLANEOUS PROVISIONS SEC. 201. PERFORMANCE MEASURES. No covered agency shall establish or enforce agency personnel practices that reward agency employees, directly or indirectly, based on the number of contacts made with small entities in pursuit of enforcement actions or on the amount of fines levied against small entities to enforce agency regulations. SEC. 202. GRACE PERIOD FOR CORRECTION OF VIOLATIONS OF ENVIRONMENTAL PROTECTION AGENCY REGULATIONS. (a) In General.--Subject to subsection (b), for violations of regulations identified on or after the date of enactment of this Act, the Administrator of the Environmental Protection Agency shall afford small entities 180 days after the date on which the violation is identified to correct such violation. (b) Exception.--Subsection (a) shall not apply-- (1) if the Administrator of the Environmental Protection Agency determines that there is an imminent risk to public health or worker safety; or (2) to a violation of a regulation for which criminal liability may be imposed. SEC. 203. WAIVER OF PUNITIVE FINES FOR SMALL ENTITIES. Notwithstanding any other law, policy, or practice, a covered agency may waive all or part of a punitive fine that would otherwise be imposed on a small entity if--", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00883", "split": "train"}
{"id": "conditionality_train_pos_0275", "text": "if any rate of tax imposed by section 11, 511, or 831(a) or (b) (whichever applies) exceeds the alternative rate of tax under section 1201(a) (determined without regard to the last sentence of section 11(b)(1)). ``(E) Rate differential portion.--The rate differential portion of foreign source net capital gain, net capital, or the excess of net capital gain from sources within the United States over net capital gain, as the case may be, is the same proportion of such amount as-- ``(i) the excess of the highest rate of tax specified in section 11(b)(1) over the alternative rate of tax under section 1201(a), bears to ``(ii) the highest rate of tax specified in section 11(b)(1).'' (12) Subsection (d) of section 1044 of such Code is amended by striking the last sentence. (13) Section 1402(i)(1) of such Code is amended to read as follows: ``(1) In general.--In determining the net earnings from self-employment of any options dealer or commodities dealer-- ``(A) notwithstanding subsection (a)(3)(A), there shall not be excluded any gain or loss (in the normal course of the taxpayer's activity of dealing in or trading section 1256 contracts) from section 1256 contracts or property related to such contracts, and ``(B) the deduction provided by section 1202 shall not apply.'' (d) Clerical Amendment.--The table of sections for part I of subchapter P of chapter 1 of such Code is amended by adding at the end thereof the following new item: ``Sec. 1202. Deduction for capital gains.'' (e) Effective Date.--The amendments made by this section shall apply to taxable years ending after December 31, 1994.", "label": 1, "domain": "government", "token_count": 382, "matched_pair_id": "conditionality_00947", "split": "train"}
{"id": "conditionality_train_pos_0276", "text": "We consider a system of many fermionic tachyons coupled to a scalar, pseudoscalar, vector and pseudovector fields. The scalar and pseudoscalar fields are responsible for the effective mass, while the pseudovector field is similar to ordinary electromagnetic field. The action of vector field $\\omega_\\mu$ results in tachyonic dispersion relation $\\varepsilon_p=\\sqrt{p^2+g^2\\omega_0^2-hpg\\omega_0-g\\vec \\sigma \\cdot \\nabla \\omega_0-m^2} -g\\vec \\sigma \\cdot \\vec \\omega$ that depends on helicity $h$ and spin $\\vec \\sigma$. We apply the mean field approximation and find that there appears a vector condensate with finite average $<\\omega_0>$ depending on the tachyon density. The pressure and energy density of a many-tachyon system include the mean-field energy $<\\varepsilon_p> =\\sqrt{p^2+hpng^2/M^2+n^2g^4/M^4-m^2}$ which is real when the particle number density exceeds definite threshold which is $n>mM^2/g^2$ for right-handed and $n>\\frac 2{\\sqrt{3}}mM^2/g^2$ for left-handed tachyons, while all tachyons are subluminal at high density. There is visible difference in the properties of right-handed and left-handed tachyons. Interaction via the vector field $\\omega_0$ may lead to stabilization of tachyon matter if its density is large enough.", "label": 1, "domain": "academic", "token_count": 345, "matched_pair_id": "conditionality_00431", "split": "train"}
{"id": "conditionality_train_pos_0277", "text": "If you’re looking for a hotel with a funky, quirky and new vibe then we’ve covered. Nestled in KL city’s sleepless Changkat Bukit Bintang, MOV Hotel opens its doors to urban and intrepid travelers seeking a design-conscious escape from the hectic city. Inspired by Kuala Lumpur’s exhilarating vibe and fast-paced people, MOV celebrates movement in the many daily facets of work, play and sweat. Located within the famous Bukit Bintang enclave in the heart of Kuala Lumpur it is just a few steps away from the city’s iconic shopping street and vibrant restaurants, bars and nightlife scene. Redefining innovative lodging with its innovative design, signature amenities and unique style, MOV Hotel provides you an integrated contemporary lifestyle experience with 147 stylish guestrooms and 9 lofts that’s perfect for a family vacation or couple’s weekend getaway. The hotel’s interior is a stunning showcase of modern design with harmonious use of textures both hard and soft, rough and smooth. Gleaming light fixtures lends a sense of elegance next to contemporary furniture and furnishings that are both minimal and bold. It’s clever design of the 138 standard room maximizes the use of each area, giving a sense of space. All rooms are fitted with king-sized beds (and single beds in twin rooms) guaranteeing the perfect end to a day of action. Even when static, the room ‘moves’ with you courtesy of colour changing lights their sexy curved showers. The nine lofts feature four different designs – Top Entourage for families, Top Oasis for couples, a Loft designed with a sitting area and another designed for a romantic getaway with a bathtub and soft sexy lighting. The hotel’s rooftop is a hub of activities and movement set against the stunning backdrop of the city. The 700 sq ft gym is the second home for travelling fitness junkies. Available at the gym are iPad apps mirrored on the giant TV screen for guests to work out for guided weights, guided yoga and HIIT workouts. The sleek swimming pool is the place to head to for a refreshing dip or to catch a bit of sun before hitting the streets at night. The Think Tank room gives guests a space to conduct meetings during their stay at MOV Hotel. But be warned this is no typical meeting room but with innovative seating – choose between gym balls, swings or designer chairs. Who says you can’t work those glutes while tapping on the laptop? Within the Lower Ground floor is Wurst Kuala Lumpur, an independent restaurant set", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00566", "split": "train"}
{"id": "conditionality_train_pos_0278", "text": "We present the results of a Hubble Space Telescope (HST) study of dwarf galaxies in the outer regions of the nearby rich Perseus Cluster, down to M_V = -12, and compare these with the dwarf population in the cluster core from our previous HST imaging. In this paper we examine how properties such as the colour magnitude relation, structure and morphology are affected by environment for the lowest mass galaxies. Dwarf galaxies are excellent tracers of the effects of environment due to their low masses, allowing us to derive their environmentally based evolution, which is more subtle in more massive galaxies. We identify 11 dwarf elliptical (dE) and dwarf spheroidal (dSph) galaxies in the outer regions of Perseus, all of which are previously unstudied. We measure the (V-I)_0 colours of our newly discovered dEs, and find that these dwarfs lie on the same red sequence as those in the cluster core. The morphologies of these dwarfs are examined by quantifying their light distributions using CAS parameters, and we find that dEs in the cluster outskirts are on average more disturbed than those in the core, with <A> =0.13\\pm0.09 and <S> =0.18\\pm0.08, compared to <A> =0.02\\pm0.04, <S> =0.01\\pm0.07 for those in the core. Based on these results, we infer that these objects are ``transition dwarfs'', likely in the process of transforming from late-type to early type galaxies as they infall into the cluster, with their colours transforming before their structures. When we compare the number counts for both the core and outer regions of the cluster, we find that below M_V = -12, the counts in the outer regions of the cluster exceed those in the core. This is evidence that in the very dense region of the cluster, dwarfs are unable to survive unless they are sufficiently massive to prevent their disruption by the cluster potential and interactions with other galaxies.", "label": 1, "domain": "academic", "token_count": 419, "matched_pair_id": "conditionality_00189", "split": "train"}
{"id": "conditionality_train_pos_0279", "text": "If you’re planning to visit Knott’s Soak City water park in Buena Park, you have some options. You can carry your things or rent a locker and you can look for an open lounge chair or bench. Or you might want to rent a cabana. There are three different locations in the park with cabanas: Shore Break, with a view of the Shore Break and The Wedge attractions; Malibu, near the Malibu Run and Old Man Falls attractions; and Wavepool, overlooking Tidal Wave Bay. Each cabana has a tented private area and an outer patio area and comes with an umbrella, a table and four chairs, four lounge chairs, four inner tube rentals and waiter service. Bethany Elliott relaxes with a book inside a cabana at Knott’s Soak City in Buena Park. (Photo courtesy of David Elliott). The Crismon family usually dines at the Longboard’s Grill at Knott’s Soak City in Buena Park. They liked that they could have food delivered to their cabana and that their server made sure that there was always a pitcher of cold water available. (Photo courtesy of David Crismon). Sound The gallery will resume in seconds Four-year-old Poppy Walsh hangs out in a shaded cabana at Knott’s Soak City in Buena Park on Sunday, May 13, 2018. (Photo by Mindy Schauer, Orange County Register/SCNG) Four-year-old Poppy Walsh hangs out in a shaded cabana at Knott’s Soak City in Buena Park on Sunday, May 13, 2018. (Photo by Mindy Schauer, Orange County Register/SCNG) Sisters Georgia Harper and Poppy Walsh take a walk together at Knott’s Soak City in Buena Park. (Photo courtesy of Melanie Walsh) They aren’t cheap and must be reserved in advance of your visit. Rental fees vary from $170-$245 depending on the date and are good for up to eight guests, plus include all the amenities mentioned. You may add up two additional guests for $15 each. Soak City admission is not included. But for some, it’s all worth it. Retiree David Crismon of Wildomar and his wife Cathi Crismon enjoy bringing their grandchildren, Cody Mobley, 15, and Kennedy Mobley, 12, to Soak City. This year they decided to rent", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00577", "split": "train"}
{"id": "conditionality_train_pos_0280", "text": "a long-term lease. For de la Cretaz, there were other perks. “It gave us housing stability, allowed us to begin saving for retirement, provided childcare help for us when we had other people living in our home, and gave friends and community members a place to live when they needed it,” she says. \"The idea of what's normal has really changed.\" Alaina Leary, 25, works in publishing from home and opted to live in Quincy, a town in the Boston area with a lower cost of living. “It has no doubt saved me a lot of money and time. It’s time I now spend working and making money, and even the extra 2–3 hours per day five days a week has yielded thousands of extra dollars in my savings account over 2017 and early 2018,” Leary says. While these approaches are innovative, Worth says, they’re choices being made not just from a cultural standpoint, but also out of necessity. “If you look at the baby boomers, a lot of them were able to move out by their late teens even and had permanent full-time jobs with benefits in their 20s, but within one generation that’s really changed,” Worth says. “The idea of what’s normal has really changed. Young people typically look to their parents for what to expect, but nothing is the same in terms of wider social conditions around work, housing, and family life.” The nonprofit policy research organization Generation Squeeze estimates it took five years to save a 20 percent down payment in 1976, compared to 13–27 years today. Many Americans are no longer able to make a 20 percent down payment. But interestingly, Worth says, millennials seem to be less bothered by communal living situations. “One in three people surveyed responded with ‘I lived at home because I want to stay with my parents,’” she says. “That isn’t necessarily new with the millennial generation, but it’s an unreflected-upon part of why millennials live at home, this idea of generational interconnectedness and helping each other cope in times of economic stress.” “I’m taking this time of not having rent to save up some money and decide where I want to settle down long term—or if I want to settle down at all,” Brown says.", "label": 1, "domain": "news", "token_count": 471, "matched_pair_id": "conditionality_00632", "split": "train"}
{"id": "conditionality_train_pos_0281", "text": "Toral introduced so-called cooperative Parrondo games, in which there are N players (3 or more) arranged in a circle. At each turn one player is randomly chosen to play. He plays either game A or game B, depending on the strategy. Game A results in a win or loss of one unit based on the toss of a fair coin. Game B results in a win or loss of one unit based on the toss of a biased coin, with the amount of the bias depending on whether none, one, or two of the player's two nearest neighbors have won their most recent games. Game A is fair, so the games are said to exhibit the Parrondo effect if game B is losing or fair and the random mixture C:=(1/2)(A+B) is winning. With mu_B (resp., mu_C) denoting the mean profit per turn to the ensemble of N players always playing game B (resp., C), we give sufficient conditions for lim mu_B (as N goes to infinity) to exist and show that lim mu_C nearly always exists, with the limits expressible in terms of a parameterized spin system on the one-dimensional integer lattice. For a particular choice of the parameters, we show that the Parrondo effect (i.e., mu_B is nonpositive and mu_C is positive) is present in the N-player model if and only if N is even. For the same choice of the parameters, we show that, with a suitable interpretation and for certain initial distributions, the Parrondo effect is present in the spin system if and only if N is even, N being the number of consecutive players whose collective profit is tracked.", "label": 1, "domain": "academic", "token_count": 336, "matched_pair_id": "conditionality_00425", "split": "train"}
{"id": "conditionality_train_pos_0282", "text": "This paper concerns the solution of the self-consistency equation for energy gap parameter $\\Delta_{\\bf k}$ in the BCS theory of superconductivity. We show that there exists a well-defined relation between the solution for energy gap parameter amplitude $|\\Delta_{\\bf k}|$ for a general interaction $V_{{\\bf k},{\\bf k}'}$ and energy gap $\\Delta$ obtained by using the cut-off approximation. The relation between $|\\Delta_{\\bf k}|$ and $\\Delta$ indicates that $\\Delta$ is a weighted average over $|\\Delta_{\\bf k}|$ of electronic states within cut-off energy $\\xi_c$ around the Fermi surface. In this interpretation for $\\Delta$, $\\xi_c$ is not a property of $V_{{\\bf k},{\\bf k}'}$, but a parameter specifying the energy range within which the weighted average over $|\\Delta_{\\bf k}|$ is taken. We show that the proper choice for the value of $\\xi_c$ is only a few $k_BT_c$ (i.e., $\\xi_c/k_BT_c$ is about 3 or 4). We also show that the cut-off approximation, even with $\\xi_c/k_BT_c=\\infty$, is a good approximation when it is used to calculate quantities such as the condensation energy and the specific heat, but it leads to significant overestimation for the Josephson critical current density of a Josephson junction if $\\xi_c/k_BT_c \\gg 1$ is assumed.", "label": 1, "domain": "academic", "token_count": 317, "matched_pair_id": "conditionality_00011", "split": "train"}
{"id": "conditionality_train_pos_0283", "text": "The holy grail of exoplanet searches is an exo-Earth, an Earth mass planet in the habitable zone around a nearby star. Mass is the most important parameter of a planet and can only be measured by observing the motion of the star around the planet-star center of mass. A single image of a planet, however, does not provide evidence that the planet is Earth mass or that it is in a habitable zone orbit. The planet's orbit, however, can be measured either by imaging the planet at multiple epochs or by measuring the position of the star at multiple epochs by space-based astrometry. The measurement of an exo-planet's orbit by direct imaging is complicated by a number of factors: (1) the inner working angle (IWA); (2) the apparent brightness of the planet depending on the orbital phase; (3) confusion arising from the presence of multiple planets; and (4) the planet-star contrast. In this paper we address the question: \"Can a prior astrometric mission that can identify which stars have Earthlike planets significantly improve the science yield of a mission to image exo-Earths?\" We find that the Occulting Ozone Observatory (a small external occulter mission that cannot measure spectra) could confirm the orbits of ~4 to ~5 times as many exo-Earths if an astrometric mission preceded it to identify which stars had such planets. We find that in the case of an internal coronagraph, a survey of the nearest ~60 stars could be done with a telescope of half the size if an astrometric mission had first identified the presence of Earth-like planets in the habitable zone and measured their orbital parameters.", "label": 1, "domain": "academic", "token_count": 347, "matched_pair_id": "conditionality_00209", "split": "train"}
{"id": "conditionality_train_pos_0284", "text": "in single-season leagues, let someone else take the chance on Buxton. You can find better players on the waiver wire. 2. Sam Dyson, RP, Texas Rangers: Hopefully, you didn’t draft both Britton and Dyson, because you’d really need to find saves now. Dyson has been a nightmare this year (0-2, 24.75 ERA) after posting 38 saves last year. But his strikeout rate has never been great (career 7.4 Ks per nine IP), so he was a risky pick to begin with this year. Psychologically, it’s hard to see the Rangers going back to Dyson later for saves, especially when they have better options on their roster. Drop him and find a better reliever. Someone else can take a chance on Dyson. 3. Russell Martin, C, Toronto Blue Jays: A four-time All-Star selection, Martin (and his Blue Jays) are off to a terrible start this season. However, he is a career.253 hitter, and for a catcher with his power, that’s acceptable. You know he will bounce back later along with his whole team. In the meantime, however, stash him on your bench and pick up a streaky, hot-hitting, unknown catcher. This will save your team average for now, and you’ll be able to ride the inevitable, stat-correcting run Martin goes on later this summer. 4. Jeff Samardzija, SP, San Francisco Giants: He’s now 0-3 with a 6.16 ERA and a 1.42 WHIP, although he looked a little better on Sunday against Colorado (no walks, eight Ks) despite taking the loss. However, the problem is that the Shark is the team’s No. 4 starter, and he lacks the quality stuff plus the mental fortitude (which is surprising, considering his college football days playing for Notre Dame) to overcome the San Francisco roster’s many deficiencies. He’s not Madison Bumgarner, and right now, even Bumgarner is winless for this last-place Giants team. Bench Samardzija if you must, but there are better SPs on the waiver wire.", "label": 1, "domain": "news", "token_count": 458, "matched_pair_id": "conditionality_00528", "split": "train"}
{"id": "conditionality_train_pos_0285", "text": "if an equity interest in the entity is or was owned by such a foreign state, such term shall refer to the corporate entity itself and not to such foreign state. (3) Property.--The term ``property'' means any personal belongings owned or controlled by the victims of the deportations which may have been taken or confiscated in connection with the deportations, including jewelry, books, artifacts, precious metals, and currency. (4) Records.--The term ``records'' includes any documents, correspondence, memoranda, receipts, invoices, presentations, audits, and any other related materials. (5) State.--The term ``State'' means each of the several States, the District of Columbia, and any commonwealth, territory, or possession of the United States. SEC. 4. CERTAIN ENTITIES INELIGIBLE FOR FEDERALLY FUNDED HIGH-SPEED RAIL CONTRACTS. (a) In General.--Any entity that applies for a contract with any agency or instrumentality of a State or local government for any high- speed rail project (including the design, engineering, construction, manufacture, or operation of a high-speed rail network or any components thereof) that is funded, either partially or fully, by the Federal Government shall certify to such agency, in advance of submitting a formal bid to such agency, whether or not such entity had any direct involvement in the deportation of any individuals to extermination camps, death camps, or any facility used for the purpose of transiting individuals to extermination or death camps, during the period beginning on January 1, 1942, and ending on December 31, 1944. (b) Disclosures.--If an entity certifies that it had any direct involvement described in subsection (a), the entity shall certify and disclose to the agency or instrumentality of a State or local government the following: (1) Whether the entity has any records related to the deportations in its possession, custody, or control. If an entity acknowledges that it has any such records, it shall describe in detail the full contents of such records and the specific locations where such records are maintained. (2) Whether the entity has any property taken or confiscated in connection with such deportations in its possession, custody or control. If an entity acknowledges that it has any such property, it must describe in detail the specific property in its possession, custody, or control and the specific locations where such property is maintained. If such entity does not have", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00880", "split": "train"}
{"id": "conditionality_train_pos_0286", "text": "A quantitative evaluation of dilepton sources in heavy-ion reactions is performed taking into account both thermal and non-thermal production mechanisms. The hadronic thermal emission rate is based on an electromagnetic current-correlation function with a low-mass region (LMR, M \\lsim 1 GeV) dominated by vector mesons (\\rho, \\omega, \\phi) and an intermediate-mass region (IMR, 1 GeV \\le M \\le 3 GeV) characterized by (the onset of) a multi-meson continuum. A convolution of the emission rates over a thermal fireball expansion results in good agreement with experiment in the low-mass spectra, confirming the predicted broadening of the \\rho meson in hadronic matter in connection with the prevalence of baryon-induced medium effects. The absolute magnitude of the LMR excess is mostly controlled by the fireball lifetime, which in turn leads to a consistent explanation of the dilepton excess in the IMR in terms of thermal radiation. The analysis of experimental transverse-momentum (q_T) spectra reveals discrepancies with thermal emission for q_T \\gsim 1 GeV in noncentral In-In collisions, which we address by extending our calculations by: (i) a refined treatment of \\rho decays at thermal freezeout, (ii) primordially produced \\rho's subject to energy-loss, (iii) Drell-Yan annihilation, and (iv) thermal radiation from t-channel meson exchange processes. We investigate the sensitivity of dilepton spectra to the critical temperature and hadro-chemical freezeout of the fireball. The \\rho broadening in the LMR turns out to be robust, while in the IMR Quark-Gluon Plasma radiation is moderate unless the critical temperature is rather low.", "label": 1, "domain": "academic", "token_count": 363, "matched_pair_id": "conditionality_00032", "split": "train"}
{"id": "conditionality_train_pos_0287", "text": "If we hope to meet the moral test of our times, if we hope to eradicate child poverty or AIDS or joblessness or homelessness … then I think that we’re going to have to talk more about the empathy deficit — the ability to put ourselves in somebody else’s shoes, to see the world through somebody else’s eyes.” The Empathy Museum takes a similar tack. On its website, it defines its mission as using participatory art projects to explore “how empathy can not only transform our personal relationships, but also help tackle global challenges such as prejudice, conflict and inequality.” Founded in 2015, it has launched projects such as the Human Library, which allow visitors to “borrow” another person for a one-on-one conversation, and A Thousand and One Books, an actual library built from donations. “A Mile in My Shoes,” the exhibit I saw, fitted visitors for the shoes of a refugee or migrant and then provided them an audio recording of the person whose shoes they were literally walking in. The shoes I fit belonged to Julie Cheung Inhin, a British East Asian actress. On the audio, she spoke of the moments when someone would comment on her race and she would suddenly become conscious of her difference from the people around her, despite “feeling like everyone else.” As painful as such moments must have been for her, they also shone a problematic light on exhibit itself. No matter how much I, a white woman, could imagine what Cheung Inhin might feel in these instances, and no matter how long I walked in her shoes, other people would never perceive us in the same way. I could imagine her pain, but I would never actually suffer it, and that made the experience of walking in her shoes feel more like consumption than communication. Did I really need her to relive those experiences into the recording in order to understand she had been treated unjustly in those moments? When I returned from my intimate, meditative stroll with Julie, I saw that others were waiting for their turn with her shoes — my second empathetic failure that day. In paying careful attention to the recording, I paid too little attention to everyone else. The idea behind projects like the Empathy Museum is that that empathy, when felt truly, will prompt global change. But how? If I’m personally moved to give a bag of almonds or even my entire personal savings, that hardly seems sufficient to pass the “moral test of our times” or change the world. How can", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00682", "split": "train"}
{"id": "conditionality_train_pos_0288", "text": "the line “heaven meets earth like a sloppy wet kiss.” More recently, concerns over the “wrath of God,” as sung in the hymn “In Christ Alone,” led certain churches to alter the verse or stop singing the song altogether. The chorus of “Reckless Love,” co-written by Asbury as well as Caleb Culver and Ran Jackson with Bethel Music, goes: O, the overwhelming, never-ending, reckless love of God O, it chases me down, fights ’til I’m found, leaves the ninety-nine I couldn’t earn it, and I don’t deserve it, still, you give yourself away O, the overwhelming, never-ending, reckless love of God, yeah The song unofficially debuted last year from Bethel Music before becoming the lead single off Asbury’s album of the same name, which released in January. The singer explained, “When I use the phrase, ‘the reckless love of God,’ I’m not saying that God himself is reckless. I am, however, saying that the way he loves, is in many regards, quite so.” Assemblies of God minister and theologian Andrew Gabriel pushed back against the distinction, saying that “you can’t separate God from his attributes.” In a blog post addressing “Reckless Love,” he stated that “God loves us with clear and thoughtful intention,” not careless abandon. Even the parable of the lost sheep does not necessarily convey irresponsibility since scholars say shepherds routinely watched each other’s flocks if one went away, he said. Blogger Paul Yoo similarly made the case that the Bible does not portray such a free-wheeling Savior: “God’s love seems reckless because he is so unconcerned about himself or his well-being in the way he loves. However…the whole Bible shows us that God is not unconcerned with himself but is ultimately for himself.” CT asked Christian music experts to weigh in on “Reckless Love.” Most agreed that it’s a good thing for Christians to examine the theology beneath catchy lyrics—and said it’d be reckless not to. Wen Reagan, adjunct instructor of church history and worship at Duke Divinity School: Reckless could be taken two ways here. One is with its common implication of “thoughtlessness” or “carelessness.” I think we can all agree that’s not a very accurate description of God’s love for us, and if that was the association here, then the song would be problematic.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00830", "split": "train"}
{"id": "conditionality_train_pos_0289", "text": "Recent observations of the low-mass pre-main sequence, eccentric spectroscopic binaries DQ Tau and V773 Tau A reveal that their millimeter spectrum is occasionally dominated by flares from non-thermal emission processes. The transient activity is believed to be synchrotron in nature, resulting from powerful magnetic reconnection events when the separate magnetic structures of the binary components are capable of interacting and forced to reorganize, typically near periastron. We conducted the first systematic study of the millimeter variability toward a sample of 12 PMS spectroscopic binaries with the aim to characterize the proliferation of flares amongst sources likely to experience similar interbinary reconnection events. The source sample consists of short-period, close-separation binaries that possess either a high orbital eccentricity or a circular orbit. Using the MAMBO2 array on the IRAM 30m telescope, we carried out continuous monitoring at 1.25 mm over a 4-night period during which all of the high-eccentricity binaries approached periastron. We also obtained simultaneous optical VRI measurements, since a strong link is often observed between stellar reconnection events and optical brightenings. UZ Tau E is the only source to be detected at millimeter wavelengths: it exhibited significant variation; it is also the only source to undergo strong simultaneous optical variability. The binary possesses the largest orbital eccentricity in the current sample, a predicted factor in star-star magnetic interaction events. With orbital parameters and variable accretion activity similar to DQ Tau, the millimeter behavior of UZ Tau E draws many parallels to the DQ Tau model for colliding magnetospheres. However, on the basis of our observations alone, we cannot determine whether the variability is repetitive, or if it could also be due to variable free-free emission in an ionized wind.", "label": 1, "domain": "academic", "token_count": 370, "matched_pair_id": "conditionality_00293", "split": "train"}
{"id": "conditionality_train_pos_0290", "text": "The Galaxy hosts a widespread population of low-energy positrons revealed by successive generations of gamma-ray telescopes through a bright annihilation emission from the bulge region, with a fainter contribution from the inner disk. The exact origin of these particles remains currently unknown. We estimate the contribution to the annihilation signal of positrons generated in the decay of radioactive 26Al, 56Ni and 44Ti. We adapted the GALPROP propagation code to simulate the transport and annihilation of radioactivity positrons in a model of our Galaxy. Using plausible source spatial distributions, we explored several possible propagation scenarios to account for the large uncertainties on the transport of ~1MeV positrons in the interstellar medium. We then compared the predicted intensity distributions to the INTEGRAL/SPI observations. We obtain similar intensity distributions with small bulge-to-disk ratios, even for extreme large-scale transport prescriptions. At least half of the positrons annihilate close to their sources, even when they are allowed to travel far away. In the high-diffusion, ballistic case, up to 40% of them escape the Galaxy. In proportion, this affects bulge positrons more than disk positrons because they are injected further off the plane in a tenuous medium, while disk positrons are mostly injected in the dense molecular ring. The predicted intensity distributions are fully consistent with the observed longitudinally-extended disk-like emission, but the transport scenario cannot be strongly constrained by the current data. Nucleosynthesis positrons alone cannot account for the observed annihilation emission in the frame of our model. An additional component is needed to explain the strong bulge contribution, and the latter is very likely concentrated in the central regions if positrons have initial energies in the 100keV-1MeV range.", "label": 1, "domain": "academic", "token_count": 361, "matched_pair_id": "conditionality_00447", "split": "train"}
{"id": "conditionality_train_pos_0291", "text": "Whether you are planning to stay in your home for several years, or if you are selling in the near future, it is important to spend your money on home improvement projects that will bring you the best return on your investment (ROI). That said, here are five home improvements projects to consider for this year: Upgrade the Kitchen: One of the smartest rooms to invest in is your kitchen. While new appliances and updated cupboards and counter tops improve the value of your kitchen, do not forget about a smart, well-designed workspace. If you are renovating the kitchen, be sure to invest in a professional layout and efficient design. According to Realtor.com, a minor kitchen remodel averages over 80 percent on your ROI, and a major kitchen remodel averages over 65 percent. Spruce Up the Bathrooms: Just a few improvements to a bathroom can go a long way. For example, install new fixtures, replace the mirror, and add a fresh coat of paint. Top off the new look with decorative plush towels and accessories. Enhance Your Curb Appeal: There are several things you can do to enhance your curb appeal — add potted plants, put in a new walkway, paint and fix shutters, and repair cracks in the driveway. Additionally, replacing your front door with an updated, more attractive style is always a great idea. It can help with energy costs, and also keep your home more secure. Plus, front door replacements consistently have a high return on investment. Consider hiring a professional if a task is out of your scope of expertise, especially for more complicated and dangerous projects. Recommended Stories For You Replace Outdated Plumbing: Believe or not, an appraiser takes plumbing into consideration when assigning value to a home. So, if you have old, rusty iron pipes, you may want to consider updating the plumbing. Nowadays, re-piping is usually done with plastic tubing, which is extremely reliable and can be replaced more efficiently and easier than in years past. Add More Attic Insulation: While it might not be the most glamorous project, adding fiberglass attic insulation actually pays for itself and delivers a small profit whenever you decide to sell. Often times, adding more insulation scores the highest return on investment of all home improvements. Keep in mind that many home improvements fall under the \"Do it Yourself\" category, but some do not! So, consider hiring a professional if a task is out of your scope of expertise, especially for more complicated and dangerous projects.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00588", "split": "train"}
{"id": "conditionality_train_pos_0292", "text": "individuals, eligible under the State plan who reside in a community setting or are transitioning to a community setting, in gaining access to needed medical, social, educational, and other services. Such services may be offered by staff of non-medical programs or those who contract with non-medical programs, so long as such individuals are qualified providers under the State plan under this title and the case management services are distinct from the direct services of the non-medical program.''; (2) by redesignating clause (ii) as clause (iii); and (3) by inserting after clause (i) (as amended by paragraph (1)), the following new clause: ``(ii) For purposes of providing case management services, individuals (other than individuals who have attained age 22 but not attained age 65 and are patients in an institution for mental diseases or individuals who are inmates of public institutions) may be considered to be transitioning to a community setting for up to the last 180 days of an institutional stay.''. SEC. 205. ASSURING APPROPRIATE CASE MANAGEMENT. Section 1915(g)(4) of the Social Security Act (42 U.S.C. 1396n(g)(4)), as amended by section 202, is amended by adding at the end the following: ``(D) Nothing in this subsection shall be construed as prohibiting a State from providing case management or targeted case management services, as defined in subparagraphs (A) and (B), respectively, of paragraph (2), through multiple case managers to any individual who qualifies for medical assistance under the State plan, or to specific classes of individuals, or to individuals who reside in specified areas, selected by the State pursuant to this subsection.''. SEC. 206. EFFECTIVE DATE. The amendments made by this title shall take effect as if enacted on December 4, 2007.", "label": 1, "domain": "government", "token_count": 376, "matched_pair_id": "conditionality_00994", "split": "train"}
{"id": "conditionality_train_pos_0293", "text": "resistance on a progressive scale; and (D) the effect on the utility of ROVs used by the Armed Forces if the proposed requirements were adopted. (2) Consultation and deadline for report.--The National Academy of Sciences shall consult with the National Highway Traffic Safety Administration and the Department of Defense in carrying out the study required by this subsection. The National Academy of Sciences shall complete and transmit to the Commission a report containing the findings of the study not later than two years after the date of enactment of this Act. (3) Report to congress.--Within five days of receiving the report described in paragraph (2) from the National Academy of Sciences, the Commission shall transmit the report, along with any comments of the Commission, to the Committee on Energy and Commerce of the House of Representatives and to the Committee on Commerce, Science and Transportation of the Senate. (4) Consideration.--The Commission shall consider the results of the study in any subsequent rulemaking regarding the performance or configuration of ROVs, or the provision of point-of-sale information regarding ROV performance. (c) Definitions.--As used in this section: (1) Commission.--The term ``Commission'' means the Consumer Product Safety Commission. (2) Recreational off-highway vehicle.--The term ``recreational off-highway vehicle'' or ``ROV'' means a motorized off-highway vehicle designed to travel on four or more tires, intended by the manufacturer for recreational use by one or more persons and having the following characteristics: (A) A steering wheel for steering control. (B) Foot controls for throttle and service brake. (C) Non-straddle seating. (D) Maximum speed capability greater than 30 miles per hour. (E) Gross vehicle weight rating no greater than 3,750 pounds. (F) Less than 80 inches in overall width, exclusive of accessories. (G) Engine displacement equal to or less than 61 cubic inches for gasoline fueled engines. (H) Identification by means of a 17-character personal or vehicle information number. (3) Exclusion.--Such term does not include a prototype of a motorized, off-highway, all-terrain vehicle or other motorized, off-highway, all-terrain vehicle that is intended exclusively for research and development purposes unless the vehicle is offered for sale.", "label": 1, "domain": "government", "token_count": 471, "matched_pair_id": "conditionality_00926", "split": "train"}
{"id": "conditionality_train_pos_0294", "text": "If your Google Wifi seems to be looking a bit blue these days — as in, the light is stuck blue — you might want to check to see if it's still actually functioning. The current build for it (9202.35.8) seems to be causing issues for some users. You probably know if you've been affected since, well, your Google Wifi won't be working. Other means of detection and confirmation manifest themselves via a steady blue light on the primary hub, at which point the satellite hubs may start to flash orange signifying a disconnect of the primary hub. In the meantime it seems that restarting that primary hub fixes the issue, but only temporarily. To be very clear, this is not a universal problem. It could be related to the latest build (9202.35.8). Even then, not all users are reporting this, and the precise nature of the cause has not been reported. But, a reasonably large number of individuals on Google's forums have been experiencing this particular issue. Google has responded on the forum with some information, reassurance, and instructions for those affected, saying, \"Our team is still looking into this and working hard on getting a fix out-- we aim to have it out as soon as possible.\" More information for those who find they may be experiencing this problem is available below: The engineering team is still working on a final fix for this issue. However, over the past few days our support team has seen two workarounds that make help resolve the issue temporarily until the fix is released. These have worked in a few cases, and may be worth a try. 1. Attempt to setup GWifi from scratch using a different owner account. This can mean creating a new Google account, or using a family member's Google account to setup the Google Wifi devices through the GW app. 2. Disconnect wireless Windows 10 devices or Xbox devices (or connect them via ethernet instead). There have been a few cases in which disconnecting any Windows 10 devices or Xbox devices has brought the Google Wifi network back up again without crashes. You can also reach out to our support team (g.co/wificare or wifica...@google.com), who will be able to provide more deep-dive troubleshooting advice based on the topography of your network. As always, thank you for your patience while we work on this issue. Both of the potential fixes at this time seem a bit unfortunate; neither having to switch to a new", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00763", "split": "train"}
{"id": "conditionality_train_pos_0295", "text": "Classically, unimodular gravity is known to be equivalent to General Relativity (GR), except for the fact that the effective cosmological constant $\\Lambda$ has the status of an integration constant. Here, we explore various formulations of unimodular gravity beyond the classical limit. We first consider the non-generally covariant action formulation in which the determinant of the metric is held fixed to unity. We argue that the corresponding quantum theory is also equivalent to General Relativity for localized perturbative processes which take place in generic backgrounds of infinite volume (such as asymptotically flat spacetimes). Next, using the same action, we calculate semiclassical non-perturbative quantities, which we expect will be dominated by Euclidean instanton solutions. We derive the entropy/area ratio for cosmological and black hole horizons, finding agreement with GR for solutions in backgrounds of infinite volume, but disagreement for backgrounds with finite volume. In deriving the above results, the path integral is taken over histories with fixed 4-volume. We point out that the results are different if we allow the 4-volume of the different histories to vary over a continuum range. In this \"generalized\" version of unimodular gravity, one recovers the full set of Einstein's equations in the classical limit, including the trace, so $\\Lambda$ is no longer an integration constant. Finally, we consider the generally covariant theory due to Henneaux and Teitelboim, which is classically equivalent to unimodular gravity. In this case, the standard semiclassical GR results are recovered provided that the boundary term in the Euclidean action is chosen appropriately.", "label": 1, "domain": "academic", "token_count": 334, "matched_pair_id": "conditionality_00079", "split": "train"}
{"id": "conditionality_train_pos_0296", "text": "acquisition, land acquired by the Secretary under this Act shall be administered in accordance with the laws (including rules and regulations) generally applicable to the National Forest System. (3) Land and water conservation fund.--For purposes of section 7 of the Land and Water Conservation Fund Act of 1965 (16 U.S.C. 460l-9), the boundaries of the White River National Forest shall be deemed to be the boundaries of the White River National Forest as of January 1, 1965. (b) Revocation of Orders and Withdrawal.-- (1) Revocation of orders.--Any public orders withdrawing any of the Federal land from appropriation or disposal under the public land laws are revoked to the extent necessary to permit disposal of the Federal land. (2) Withdrawal of federal land.--On the date of enactment of this Act, if not already withdrawn or segregated from entry and appropriation under the public land laws (including the mining and mineral leasing laws) and the Geothermal Steam Act of 1970 (30 U.S.C. 1001 et seq.), the Federal land is withdrawn, subject to valid existing rights, until the date of the conveyance of the Federal land to the County. (3) Withdrawal of non-federal land.--On acquisition of the non-Federal land by the Secretary, the non-Federal land is permanently withdrawn from all forms of appropriation and disposition under the public land laws (including the mining and mineral leasing laws) and the Geothermal Steam Act of 1970 (30 U.S.C. 1001 et seq.). (c) Boundary Adjustments.--The Secretary with jurisdiction over the land and the County may agree to-- (1) minor adjustments to the boundaries of the Federal land and non-Federal land; and (2) modifications or deletions of parcels and mining claim remnants of Federal land or non-Federal land to be exchanged on Smuggler Mountain. (d) Map.--If there is a discrepancy between a map, acreage estimate, and legal or other description of the land to be exchanged under this Act, the map shall prevail unless the Secretary with jurisdiction over the land and the County agree otherwise.", "label": 1, "domain": "government", "token_count": 440, "matched_pair_id": "conditionality_00921", "split": "train"}
{"id": "conditionality_train_pos_0297", "text": "If Flowers is traded, the Giants are going to have to draft a tackle or sign one as a free agent. Odell Beckham Jr., who missed most of last season with a broken ankle, and defensive end Olivier Vernon were both at the minicamp. They skipped the minicamp a year ago. \"I think the big thing for us is our game is very simple — it's about the ball, it's about negotiating the ground and it's really about man whipping man,\" Shurmur said. The minicamp, which does not entail any hitting, is more about making sure players get to know the new systems, with some throwing and receiving mixed in. The defences can work on stripping the ball. There was speculation that Shurmur wanted to use the minicamp to see what quarterback Davis Webb could do. The third-round pick did nothing last season, so the Giants really don't know what they have with their backup to Eli Manning. \"I don't think there needs to be any anxiety on his part — get trained up, come on out here, let it rip and mistakes happen in practice and you learn from them,\" Shurmur said. \"I think that's why you practice, so I think you have to be careful about making a final evaluation on a guy in a three-day period here. He just needs to come out here and get as good as he can be.\" Most players said they felt they were entering this season with a clean slate. Cornerback Janoris Jenkins, who was suspended for a game last season after missing a practice, intends to be on his best behaviour this season. \"I promise y'all that Jackrabbit says it won't happen this year what happened last year,\" he said. \"There won't be any animosity between players, no disrespecting the coach. There will be none of that. New York Giant football is back.\" Jenkins also believes fellow cornerback and 2016 first-round draft pick Eli Apple, who also was suspended for a game, will be a different player this season. \"You have to understand that he was young,\" Jenkins said. \"It's a clean slate, new coaching staff and for him it's guys like me that have to push him and help him out because I've been in the league so long and just help him understand that adversity is going to hit you and when it hits, you've just got to keep it going.\" Beckham did not take part in the afternoon practice", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00595", "split": "train"}
{"id": "conditionality_train_pos_0298", "text": "with clients? Funke Ajomale I had an argument with somebody over this issue. She was going for a friend’s wedding and wanted to wear over the top kind of white, I told her not to wear the dress and she was upset. If it was my wedding I would have said to her not to enter. It is the bride’s day and you are meant to give her that respect and not outshine her. Where I work, we can wear whatever we choose to wear but my subconscious says to me, you are in the office. However I dress could cause me to be harassed. I am wearing a long flowing skirt and I still get harassed, so if I now wear something that would expose me what would now come from that? I believe that if you want to look expensive, cover up. I was in a church one day which was my first time, I saw a particular dressing. I asked someone if it was normal to dress that way and he said yes it is personal choice. I know that God looks at your heart and not your dressing, but how does it make the other person feel, do or say about your dressing? It now goes beyond personal rights, Is it culture confirmed? Is it culture allowed? Would people see you and insult you? If you go to the market dressed inappropriately and get stoned at or insulted, if you report the case to the police or any body, the first thing your lawyer will ask is why did you dress that way? Bukky Karibi Whyte I have a problem with that. I have heard different situations of women being sexually harassed and then it goes, why did you wear a skirt? But when dressing now breeds violence, I no longer blame dressing. It is you as a person that is displaying the violence. You have a problem. Funke Ajomale But I still feel that it is always best to erase that particular notion from the beginning. I was wearing a long dress at work and I still got harassed. It is a human right thing to wear whatever you can afford. But if I am going somewhere then I think I should be covered, it doesn’t mean I should be over the top covered but then I should be comfortable and should be able to presume the right image. Bukky Karibi Whyte When Cossy first came into the entertainment industry, a lot of us gasped. But I think if she’s outside the entertainment world, she will dress differently.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00639", "split": "train"}
{"id": "conditionality_train_pos_0299", "text": "that handles flare well and draws nice sun-stars, the sun will serve as a wonderful compositional element in your images. To get those sun-stars to appear, you would need to stop down your lens to a very small aperture such as f/11 or f/16. If you see flare and ghosting, you can use a great trick described in detail in Nasim’s article on eliminating ghosting and flare in landscape photography. If you are comfortable with image blending in post, there is another great technique to avoid over-exposure and diffraction: shoot two images – one for the sun at f/16 and one for the foreground and background at a larger aperture like f/8. Then combine the two images in post and use simple blending techniques with layers to bring those sun-stars into your image. Also, consider if filters (such as CPL, UV or ND) are helpful in any way when shooting against the sun. If not, detach them, as they could make things worse in terms of additional ghosting and flare. If you do use filters, make sure that they are of high quality and have multi-coating applied to them. For more details about lens filters, see Nasim’s article on lens filters and also check out his must-have filters for landscape photography article. 6) Make Use of Frost White frost can turn almost anything into a very attractive subject. Paradoxically, that is exactly what makes it difficult to photograph. With a thin layer of frost covering everything, landscape looks like a fairy tale, which may obscure the focus of the photographer for a good composition. I personally live in an area where the combination of freezing frost and blue sky is relatively rare. So when I got it earlier in January of this year, I got totally excited – and out of excitement I forgot to turn on VR on my lenses. When I discovered that, I was at first angry at myself, but then I took it as a good sign that I should take my time and focus on what I am doing, rather than let my excitement take over and ruin my photographs. Good composition and framing should always be your priority, but do not underestimate other variables that come into play while shooting, whether it has to do with proper exposure, focusing, depth of field or simpler things related to your camera settings. 9) Try Black and White Photography Even if I really enjoy the winter color palette, snow and frost often create handy conditions for black and white (B&W) photographs.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00610", "split": "train"}
{"id": "conditionality_train_pos_0300", "text": "We consider the potentials of the LHC and a linear e^+e^- collider (LC) for discovering supersymmetric particles in variants of the MSSM with soft supersymmetry-breaking mass parameters constrained to be universal at the GUT scale (CMSSM) or at some lower scale M_{in} (GUT-less models), as may occur in some scenarios with mirage unification. Whereas the LHC should be able to discover squarks and/or gluinos along all the CMSSM coannihilation strip where the relic neutralino LSP density lies within the range favoured for cold dark matter, many GUT-less models could escape LHC detection. In particular, if M_{in} < 10^{11} GeV, the LHC would not detect sparticles if the relic density lies within the favoured range. For any given discovery of supersymmetry at the LHC, in such GUT-less models the lightest neutralino mass and hence the threshold for sparticle pair production at a LC increases as M_{in} decreases, and the CMSSM offers the best prospects for measuring sparticles at a LC. For example, if the LHC discovers sparticles with 1 fb^{-1} of data, within the CMSSM a centre-of-mass energy of 600 GeV would suffice for a LC to to produce pairs of neutralinos, if they provide the cold dark matter, whereas over 1 TeV might be required in a general GUT-less model. These required energies increase to 800 GeV in the CMSSM and 1.4 TeV in GUT-less models if the LHC requires 10 fb^{-1} to discover supersymmetry.", "label": 1, "domain": "academic", "token_count": 348, "matched_pair_id": "conditionality_00042", "split": "train"}
{"id": "conditionality_train_pos_0301", "text": "(1) of section 402(e) of such Code (relating to alternate payee under qualified domestic relations order treated as distributee) is amended by inserting ``or a qualified child abuse order (as defined in section 414(p))'' after ``a qualified domestic relations order (as defined in section 414(p))'' each place it appears. (2) Allocation of investment in the contract.--Paragraph (10) of section 72(m) of such Code (relating to determination of investment in the contract in the case of qualified domestic relations orders) is amended-- (A) in the heading, by inserting ``and qualified child abuse orders'' after ``qualified domestic relations orders''; and (B) by inserting ``or a qualified child abuse order (as defined in section 414(p))'' after ``a qualified domestic relations order (as defined in section 414(p))''. (3) Clarification of eligibility of participant for lump sum treatment.-- (A) Subparagraph (H) of section 402(d)(4) of such Code (relating to balance to credit of employee not to include amounts payable under qualified domestic relations order) is amended-- (i) in the heading, by inserting ``or qualified child abuse order'' after ``qualified domestic relations order''; and (ii) by inserting ``or a qualified child abuse order (within the meaning of section 414(p))'' after ``a qualified domestic relations order (within the meaning of section 414(p))''. (B) Subparagraph (J) of section 402(d)(4) of such Code is amended by inserting ``, or under a qualified child abuse order (within the meaning of section 414(p)) of the balance to the credit of an alternate payee,'' after ``former spouse of the employee''. SEC. 4. EFFECTIVE DATE. The amendments made by this Act shall take effect on January 1, 1996, except that, in the case of a child abuse order entered before such date, the plan administrator-- (1) shall treat such order as a qualified child abuse order if such administrator is paying benefits pursuant to such order on such date, and (2) may treat any other such order entered before such date as a qualified child abuse order even if such order does not meet the requirements of such amendments.", "label": 1, "domain": "government", "token_count": 472, "matched_pair_id": "conditionality_00928", "split": "train"}
{"id": "conditionality_train_pos_0302", "text": "in the Treasury not otherwise appropriated, the Secretary of the Treasury shall transfer to the Secretary to carry out this paragraph $1,000,000, to remain available until expended. ``(B) Receipt and acceptance.--The Secretary shall be entitled to receive, shall accept, and shall use to carry out this paragraph the funds transferred under subparagraph (A), without further appropriation. ``(f) Study and Report.-- ``(1) In general.--The Secretary, in conjunction with the Director of the Centers for Disease Control and Prevention, shall prepare a report on the implementation, strength, and effectiveness of the local wellness policies carried out in accordance with this section. ``(2) Study of local wellness policies.--The study described in paragraph (1) shall include-- ``(A) an analysis of the strengths and weaknesses of local wellness policies and how the policies compare with model local wellness policies recommended under subsection (e)(2)(A)(ii); and ``(B) an assessment of the impact of the local wellness policies in addressing the requirements of subsection (b). ``(3) Report.--Not later than January 1, 2014, the Secretary shall submit to the Committee on Agriculture, Nutrition, and Forestry of the Senate and the Committee on Education and Labor of the House of Representatives a report that describes the findings of the study.''. SEC. 4. REPEAL. Section 204 of the Child Nutrition and WIC Reauthorization Act of 2004 (42 U.S.C. 1751 note; Public Law 108-265) is repealed. SEC. 5. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 406, "matched_pair_id": "conditionality_00870", "split": "train"}
{"id": "conditionality_train_pos_0303", "text": "provide substantial financial and technical assistance directly to CSAs from individual- or family-operated farms; ``(B) CSAs from individual- or family-operated farms; ``(C) the expansion of CSAs into underserved communities; ``(D) CSAs operated by or employing veterans (as defined in section 101 of title 38, United States Code); and ``(E) the development, improvement, or expansion of innovative delivery and distribution programs that stimulate consumer interest in CSA participation. ``(f) Funding.-- ``(1) In general.--Of the funds of the Commodity Credit Corporation, the Secretary shall use to carry out this section-- ``(A) $10,000,000 for fiscal year 2012; ``(B) $12,000,000 for each of fiscal years 2013 through 2015; and ``(C) $15,000,000 for each fiscal years 2016 through 2018. ``(2) Interdepartmental coordination.--In carrying out this subsection, the Secretary shall ensure, to the maximum extent practicable, coordination between the applicable agencies.''. SEC. 3. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 316, "matched_pair_id": "conditionality_00996", "split": "train"}
{"id": "conditionality_train_pos_0304", "text": "To study the Reynolds stresses which describe turbulent momentum transport from turbulence affected by large-scale shear and rotation. Three-dimensional numerical simulations are used to study turbulent transport under the influences of large-scale shear and rotation in homogeneous, isotropically forced turbulence. We study three cases: one with only shear, and two others where in addition to shear, rotation is present. These cases differ by the angle (0 or 90\\degr) the rotation vector makes with respect to the z-direction. Two subsets of runs are performed with both values of \\theta where either rotation or shear is kept constant. When only shear is present, the off-diagonal stress can be described by turbulent viscosity whereas if the system also rotates, nondiffusive contributions (\\Lambda-effect) to the stress can arise. Comparison of the direct simulations are made with analytical results from a simple closure model. We find that the turbulent viscosity is of the order of the first order smoothing result in the parameter regime studied and that for sufficiently large Reynolds numbers the Strouhal number, describing the ratio of correlation to turnover times, is roughly 1.5. This is consistent with the closure model based on the minimal tau-approximation which produces a reasonable fit to the simulation data for similar Strouhal numbers. In the cases where rotation is present, separating the diffusive and nondiffusive components of the stress turns out to be challenging but taking the results at face value, we can obtain nondiffusive contributions of the order of 0.1 times the turbulent viscosity. We also find that the simple closure model is able to reproduce most of the qualitative features of the numerical results provided that the Strouhal number is of the order of unity.", "label": 1, "domain": "academic", "token_count": 341, "matched_pair_id": "conditionality_00144", "split": "train"}
{"id": "conditionality_train_pos_0305", "text": "The ISM is governed by supersonic turbulence on a range of scales. We use this to develop a rigorous excursion-set model for the formation and time evolution of dense gas structures (GMCs, massive clumps, and cores). Supersonic turbulence drives the density distribution to a lognormal with dispersion increasing with Mach number; we generalize this to include scales >h (the disk scale height), and use it to construct the statistical properties of the density field smoothed on a scale R. We then compare conditions for self-gravitating collapse including thermal, turbulent, and rotational support. We show this becomes a well-defined barrier crossing problem. As such, an exact 'bound object mass function' can be derived, from scales of the sonic length to above the disk Jeans mass. This agrees remarkably well with observed GMC mass functions in the MW and other galaxies; the only inputs are the mass and size of the galaxies (to normalize the model). This explains the mass function cutoff and its power-law slope (close to, but shallower than, -2). The model also predicts the linewidth-size and size-mass relations of clouds and the dependence of their residuals on surface density/pressure. We use this to predict the spatial correlation function/clustering of clouds and star clusters; these also agree well with observations. We predict the size/mass function of ISM 'bubbles' or 'holes', and show this can account for observed HI hole distributions without any local feedback. We generalize the model to construct time-dependent 'merger/fragmentation trees' which can be used to follow cloud evolution and construct semi-analytic models for the ISM. We provide explicit recipes to construct the trees. We use a simple example to show that, if clouds are not destroyed in ~1-5 crossing times, then all ISM mass would be trapped in collapsing objects even if the large-scale turbulence were maintained.", "label": 1, "domain": "academic", "token_count": 381, "matched_pair_id": "conditionality_00387", "split": "train"}
{"id": "conditionality_train_pos_0306", "text": "and Culture shall be subject to the audit requirements of section 5134(f)(2) of title 31, United States Code, with regard to the amounts received under subsection (b). (d) Limitation.--Notwithstanding subsection (a), no surcharge may be included with respect to the issuance under this Act of any coin during a calendar year if, as of the time of such issuance, the issuance of such coin would result in the number of commemorative coin programs issued during such year to exceed the annual 2 commemorative coin program issuance limitation under section 5112(m)(1) of title 31, United States Code. The Secretary of the Treasury may issue guidance to carry out this subsection. SEC. 8. FINANCIAL ASSURANCES. The Secretary shall take such actions as may be necessary to ensure that-- (1) minting and issuing coins under this Act will not result in any net cost to the United States Government; and (2) no funds, including applicable surcharges, are disbursed to any recipient designated in section 7 until the total cost of designing and issuing all of the coins authorized by this Act is recovered by the United States Treasury, consistent with sections 5112(m) and 5134(f) of title 31, United States Code. SEC. 9. BUDGET COMPLIANCE. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Committee on the Budget of the House of Representatives, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 366, "matched_pair_id": "conditionality_00864", "split": "train"}
{"id": "conditionality_train_pos_0307", "text": "(Abridged) We demonstrate that the tenet of hierarchical structure growth leads directly to a robust, falsifiable prediction for the correlation between stellar fraction (fstar) and total system mass (M500) of galaxy groups and clusters. This prediction is relatively insensitive to the details of baryonic physics or cosmological parameters. In particular, if the fstar-M500 relation is fixed and does not evolve with redshift, CDM models predict the logarithmic slope of this relation to be b>-0.3. This constraint can be weakened if the fstar-M500 relation evolves strongly, but this implies more stars must be formed in situ in groups at low redshift. Conservatively requiring that at least half the stars in groups were formed by z=1, the constraint from evolution models is b>-0.35. Since the most massive clusters (M500=1E15 Msun) are observed to have fstar=0.01, this means that groups with M500=5E13 Msun must have fstar<0.03. Recent observations by Gonzalez et al. (2007) indicate a much steeper relation, with fstar>0.04 in groups, leading to b=-0.64. If confirmed, this would rule out hierarchical structure formation models: today's clusters could not have been built from today's groups, or even from the higher-redshift progenitors of those groups. We perform a careful analysis of these and other data to identify the most important systematic uncertainties in their measurements. Although correlated uncertainties on stellar and total masses might explain the steep observed relation, the data are only consistent with theory if the observed group masses are systematically underestimated.", "label": 1, "domain": "academic", "token_count": 340, "matched_pair_id": "conditionality_00040", "split": "train"}
{"id": "conditionality_train_pos_0308", "text": "Remember the new Play Store \"My Apps\" screen layout that we spotted in testing in a dogfood version in February? Well, that appears to be rolling out more widely now, possibly even to everyone. You may need to clear the Play Store's app data and restart it to see the change (which might revert you back to the old lime green color for a bit before it switches back to the new darker green, thought I'd warn you), but it should be working for everyone now based on the number of tips we've received and on testing with our own devices. The new \"Installed\" tab has multiple sorting methods. The new layout gives Updates their own tab in the My apps and games screen, renames All to Library, and gives you several sorting methods for the Installed apps (alphabetical, last updated, last used, and size). \"Beta\" is still there (left). \"Library\" has quick buttons to install or remove an app from your account (right). There are a couple of other benefits too. One is that it's now easier to update certain apps only, since the Update button is clickable instead of requiring you to open the app's page first then tap on update. Two is that installing apps from your account is more obvious thanks to a new Install button, so you don't need to tap and hold to select multiple apps anymore, you can just scroll and install whichever ones you want. And three is that you can refresh to check for updates instead of having to leave the Play Store and launch it again to trigger a check. It's easier to update apps one by one (left) and new refresh to check for updates button (right). Overall, there are plenty of benefits to this new layout and, as far as I can tell, no drawbacks at all. App addicts should find most of the changes very helpful. The new layout wasn't showing up for me when I opened the Play Store, but as I said at the start of the article, I cleared data and that triggered the new look. It doesn't seem to require the newest version of the Play Store either (I'm on 7.7.08) so you might as well try it with whatever version you're running now to see if it works before updating to the newest one.", "label": 1, "domain": "news", "token_count": 461, "matched_pair_id": "conditionality_00762", "split": "train"}
{"id": "conditionality_train_pos_0309", "text": "We model the dynamical structure of M87 (NGC4486) using high spatial resolution long-slit observations of stellar light in the central regions, two-dimensional stellar light kinematics out to half of the effective radius, and globular cluster velocities out to 8 effective radii. We simultaneously fit for four parameters, black hole mass, dark halo core radius, dark halo circular velocity, and stellar mass-to-light ratio. We find a black hole mass of 6.4(+-0.5)x10^9 Msun(the uncertainty is 68% confidence marginalized over the other parameters). The stellar M/L_V=6.3+-0.8. The best-fitted dark halo core radius is 14+-2 kpc, assuming a cored logarithmic potential. The best-fitted dark halo circular velocity is 715+-15 km/s. Our black hole mass is over a factor of 2 larger than previous stellar dynamical measures, and our derived stellar M/L ratio is 2 times lower than previous dynamical measures. When we do not include a dark halo, we measure a black hole mass and stellar M/L ratio that is consistent with previous measures, implying that the major difference is in the model assumptions. The stellar M/L ratio from our models is very similar to that derived from stellar population models of M87. The reason for the difference in the black hole mass is because we allow the M/L ratio to change with radius. The dark halo is degenerate with the stellar M/L ratio, which is subsequently degenerate with the black hole mass. We argue that dynamical models of galaxies that do not include the contribution from a dark halo may produce a biased result for the black hole mass. This bias is especially large for a galaxy with a shallow light profile such as M87, and may not be as severe in galaxies with steeper light profiles unless they have a large stellar population change with radius.", "label": 1, "domain": "academic", "token_count": 389, "matched_pair_id": "conditionality_00145", "split": "train"}
{"id": "conditionality_train_pos_0310", "text": "Adele’s win over Beyoncé for Album of the Year drew criticism from a swath of viewers and artists, including Adele herself. Herbie Hancock, who won the award in 2008, is the category’s last black winner, but despite this fact—and the criticism of the Grammys that stems from it—Recording Academy President Neil Portnow said today in an interview with Pitchfork that Grammy voters don’t see race, and neither should listeners. Portnow defended the Academy’s votes, arguing that its 14,000 members are “the highest level of professionals in the industry.” Thus, he reasoned, “I don’t think there’s a race problem at all”: We don’t, as musicians, in my humble opinion, listen to music based on gender or race or ethnicity. When you go to vote on a piece of music—at least the way that I approach it—is you almost put a blindfold on and you listen. It’s a matter of what you react to and what in your mind as a professional really rises to the highest level of excellence in any given year. And that is going to be very subjective. That’s what we ask our members to do, even in the ballots. We ask that they not pay attention to sales and marketing and popularity and charts. You have to listen to the music. So of the 14,000 voters, they listen, they make up their minds, and then they vote. To further make his case, Portnow pointed to Chance the Rapper’s Best New Artist win as proof of the Academy’s diversity: “You don’t get Chance the Rapper as the Best New Artist of the year if you have a membership that isn’t diverse and isn’t open-minded and isn’t really listening to the music.” Portnow omits Chance is just one of five to win it since 1999. Lauryn Hill’s The Miseducation of Lauryn Hill won Album of the Year in 1999, the last time that award was won by a black woman. Portnow’s main argument is the Academy’s size means it is diverse. But the Academy does not release the exact demographics of its voter base, nor does it seem like it’s planning to, and one must wonder if the data really would back up his claim.", "label": 1, "domain": "news", "token_count": 464, "matched_pair_id": "conditionality_00651", "split": "train"}
{"id": "conditionality_train_pos_0311", "text": "were replaced by Westerners who were deemed to know better, and many felt that the community spirit that had fostered under communism had quickly evaporated under capitalism. \"The social cohesion from East Germany, most people here actually miss that feeling,\" according to 47-year-old Ingo Wobst, a Dresden resident who has seen many friends switch from the center-left SPD to the AfD. Ingo Wobst HC Plambeck / for NBC News \"After the fall of the wall, life in the countryside was pulsating, but then a lot of things collapsed,\" he says, sitting in a cafe across town in Dresden's trendy, graffiti-daubed Neustadt neighborhood. \"Many people lost their jobs, and today you find small towns out here where there is no supermarket, no doctor and not even a bus stop.\" The city of Dresden itself is actually flourishing, emerging as a rival tourist destination to nearby Leipzig or even Berlin. In recent years it's become known as the home of another far-right group, PEGIDA — for Patriotic Europeans Against the Islamisation of the West — which attracted 25,000 people to a demonstration in early 2015. But many of the marchers were not from Dresden but from the surrounding towns and villages, according to Richter. The AfD has found most traction in such rural areas, which are emptying out because of \"brain drain\" — the emigration of educated and trained people — and low birth rates. If East Germany were still a country, it would have the oldest population in Europe. \"In a big city you have more work and the young people come here because of it,\" says Victoria Prokudin, a 20-year-old trainee lawyer who moved to Dresden from the surrounding countryside. Victoria Prokudin HC Plambeck / for NBC News Even those who feel little nostalgia for communism balk at the idea that Germany is universally happy now that it's a single country. Later that night, around 30 minutes' drive west of Bitterfeld-Wolfen, Roi gathered with AfD compatriots in the small town of Köthen. Around half a dozen sympathizers and supporters were clustered in the unlikely setting of a restaurant called Schwarzes Ross, meaning Black Steed. A large painting of a horse dominates the back wall, accompanied by horse-themed clocks, ornamental plates and coasters — decorations that seem a bit macabre given that horse meat is on the menu.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00736", "split": "train"}
{"id": "conditionality_train_pos_0312", "text": "It is shown that if, from the starting point of a universal rank-one mass matrix long favoured by phenomenologists, one adds the assumption that it rotates (changes its orientation in generation space) with changing scale, one can reproduce, in terms of only 6 real parameters, all the 16 mass ratios and mixing parameters of quarks and leptons. Of these 16 quantities so reproduced, 10 for which data exist for direct comparison (i.e. the CKM elements including the CP-violating phase, the angles $\\theta_{12}, \\theta_{13}, \\theta_{23}$ in $\\nu$-oscillation, and the masses $m_c, m_\\mu, m_e$) agree well with experiment, mostly to within experimental errors; 4 others ($m_s, m_u, m_d, m_{\\nu_2}$), the experimental values for which can only be inferred, agree reasonably well; while 2 others ($m_{\\nu_1}, \\delta_{CP}$ for leptons), not yet measured experimentally, remain as predictions. In addition, one gets as bonuses, estimates for (i) the right-handed neutrino mass $m_{\\nu_R}$ and (ii) the strong CP angle $\\theta$ inherent in QCD. One notes in particular that the output value for $\\sin^2 2 \\theta_{13}$ from the fit agrees very well with recent experiments. By inputting the current experimental value with its error, one obtains further from the fit 2 new testable constraints: (i) that $\\theta_{23}$ must depart from its \"maximal\" value: $\\sin^2 2 \\theta_{23} \\sim 0.935 \\pm 0.021$, (ii) that the CP-violating (Dirac) phase in the PMNS would be smaller than in the CKM matrix: of order only $|\\sin \\delta_{CP}| \\leq 0.31$ if not vanishing altogether.", "label": 1, "domain": "academic", "token_count": 411, "matched_pair_id": "conditionality_00460", "split": "train"}
{"id": "conditionality_train_pos_0313", "text": ", and elsewhere to encourage an international effort to ensure readiness for the Year 2000 at banks and other financial institutions; and (2) the initiatives which the representatives of the United States to the International Monetary Fund, International Bank for Development and Reconstruction, and other international development banks are taking to engage such institutions in providing funding or technical assistance to developing countries for remedying the Year 2000 computer problem in such countries. SEC. 6. QUARTERLY PROGRESS REPORTS REQUIRED. (a) In General.--Beginning after the submission of the report on the national assessment and strategy under sections 4 and 5, the Chairperson of the Year 2000 Conversion Council shall submit a quarterly report to the Congress on the progress that has been made since the submission of the prior report in solving the Year 2000 computer problem in all critical infrastructures and key sectors of the economy and in developing a contingency plan. (b) Final Report.--The final report submitted under subsection (a) shall assess the ongoing Year 2000 and other date-related problems that will occur in the future as temporary Year 2000 renovations lapse or other fail dates occur in computer systems. (c) Sunset.--No reports shall be required under subsection (a) after December 31, 2001. SEC. 7. REVISION OF FEDERAL ACQUISITION REGULATION TO PROVIDE FOR CERTAIN PENALTIES FOR CONTRACTORS THAT VIOLATE YEAR 2000 REQUIREMENT. In the case of any person who enters into a contract with a Federal agency, and who knowingly provides goods or services to the agency under the contract that are not Year 2000 compliant (as that term is defined in section 39.002 of the Federal Acquisition Regulation, as adopted on August 22, 1997), the Federal Acquisition Regulation may be revised to provide for an appropriate period for which such person shall not be eligible for award of any contract by any Federal agency. Any restrictions developed pursuant to this section may, at the discretion of the applicable Federal agency, be waived if the new goods or services are Year 2000 compliant.", "label": 1, "domain": "government", "token_count": 431, "matched_pair_id": "conditionality_00881", "split": "train"}
{"id": "conditionality_train_pos_0314", "text": "Mayall II = G1 is one of the most luminous globular clusters (GCs) in M31. Here, we determine its age and mass by comparing multicolor photometry with theoretical stellar population synthesis models. Based on far- and near-ultraviolet GALEX photometry, broad-band UBVRI, and infrared JHK_s 2MASS data, we construct the most extensive spectral energy distribution of G1 to date, spanning the wavelength range from 1538 to 20,000 A. A quantitative comparison with a variety of simple stellar population (SSP) models yields a mean age that is consistent with G1 being among the oldest building blocks of M31 and having formed within ~1.7 Gyr after the Big Bang. Irrespective of the SSP model or stellar initial mass function adopted, the resulting mass estimates (of order $10^7 M_\\odot$) indicate that G1 is one of the most massive GCs in the Local Group. However, we speculate that the cluster's exceptionally high mass suggests that it may not be a genuine GC. We also derive that G1 may contain, on average, $(1.65\\pm0.63)\\times10^2 L_\\odot$ far-ultraviolet-bright, hot, extreme horizontal-branch stars, depending on the SSP model adopted. On a generic level, we demonstrate that extensive multi-passband photometry coupled with SSP analysis enables one to obtain age estimates for old SSPs to a similar accuracy as from integrated spectroscopy or resolved stellar photometry, provided that some of the free parameters can be constrained independently.", "label": 1, "domain": "academic", "token_count": 332, "matched_pair_id": "conditionality_00131", "split": "train"}
{"id": "conditionality_train_pos_0315", "text": "Flash memory is a non-volatile computer memory comprised of blocks of cells, wherein each cell can take on q different values or levels. While increasing the cell level is easy, reducing the level of a cell can be accomplished only by erasing an entire block. Since block erasures are highly undesirable, coding schemes - known as floating codes or flash codes - have been designed in order to maximize the number of times that information stored in a flash memory can be written (and re-written) prior to incurring a block erasure. An (n,k,t)_q flash code C is a coding scheme for storing k information bits in n cells in such a way that any sequence of up to t writes (where a write is a transition 0 -> 1 or 1 -> 0 in any one of the k bits) can be accommodated without a block erasure. The total number of available level transitions in n cells is n(q-1), and the write deficiency of C, defined as \\delta(C) = n(q-1) - t, is a measure of how close the code comes to perfectly utilizing all these transitions. For k > 6 and large n, the best previously known construction of flash codes achieves a write deficiency of O(qk^2). On the other hand, the best known lower bound on write deficiency is \\Omega(qk). In this paper, we present a new construction of flash codes that approaches this lower bound to within a factor logarithmic in k. To this end, we first improve upon the so-called \"indexed\" flash codes, due to Jiang and Bruck, by eliminating the need for index cells in the Jiang-Bruck construction. Next, we further increase the number of writes by introducing a new multi-stage (recursive) indexing scheme. We then show that the write deficiency of the resulting flash codes is O(qk\\log k) if q \\geq \\log_2k, and at most O(k\\log^2 k) otherwise.", "label": 1, "domain": "academic", "token_count": 407, "matched_pair_id": "conditionality_00137", "split": "train"}
{"id": "conditionality_train_pos_0316", "text": "If you're on a budget, chances are that you've debated a purchase between an older flagship and a newer mid-ranger. Do you want a Moto G4, or a Moto X Pure? A Galaxy Note5 or a Galaxy S7? For those of you who prefer buying powerful last-gen hardware, Newegg has got a deal for you: two Benjamins will get you a ZTE Axon Pro with a sizable 64GB of storage. When the Axon Pro was new, it packed some pretty competitive hardware: a 5.5-inch 1440p LCD display, a Snapdragon 810 (which reportedly performs decently in the Axon Pro), 4GB of RAM, 64GB of internal storage, dual rear cameras (13MP + 2MP), and a 3000mAh battery. It also has great audio, both through the headphone jack and through its front-facing speaker (only one is for audio). Virtually its only downfall in this regard is its lack of a microSD slot, but 64GB should be perfectly serviceable for most. The Axon Pro also comes with two noteworthy extras: a set of JBL E13 in-ear headphones, and ZTE's fantastic Passport 2.0 warranty, which you can see details of above. Want a 64GB Axon Pro of your very own for the low, low price of $200? Well, you're limited to the gold color (which you'll use discount code 0210CLS03 to get to from $249.99), and the discount will end around six hours from the time of this article's publishing. If you don't think you need 64GB, you can get the \"Phthalo Blue\" 32GB variant for $176 with the same code (it's probably worth it to get the 64GB variant for $24 more). Should you not need specs that powerful, you can get a lower-end 32GB Axon in that same Phthalo Blue with a 5.5\" 1080p panel, a Snapdragon 801, 2GB of RAM, and 32GB of internal storage for just $128 with the same discount code. It'll come with the same JBL headphones and the same Passport 2.0 warranty. Again, these prices will expire in roughly six hours, so don't wait up if you're interested.", "label": 1, "domain": "news", "token_count": 491, "matched_pair_id": "conditionality_00772", "split": "train"}
{"id": "conditionality_train_pos_0317", "text": "If a deer fawn is found alone in the woods, leave it there, advises a state wildlife biologist. Its mother has not abandoned it; she is probably nearby. Removing a fawn from the forest is also illegal because the animal is being taken outside the legal season for taking deer, which is the hunting season. “Many people who come upon a solitary spotted fawn in the woods or along a roadway mistakenly assume the animal has been deserted by its mother and want to take the apparently helpless creature home to care for it,” said Charles Ruth, Big Game Program coordinator for the S.C. Department of Natural Resources. “Young fawns like this have not been abandoned but are still in the care of a doe.” The apparently “helpless” deer fawns born during April, May and June in South Carolina will begin daily movements with their mothers in about three or four weeks. Human handling and disturbance of fawns can cause a doe to shy away or even desert her offspring. Also, a bleating response by the fawn can summon nearby predators. “It’s part of nature’s plan for a doe deer to leave her fawn or fawns alone for their first few weeks of life,” Ruth said. “The reason for this unusual maternal action is that the fawn at this age is better protected away from the doe. The presence of the doe nearby would attract predators because the doe lacks the protective coloration of the fawn, and the older and larger doe has a much stronger odor.” A fawn that appears abandoned is merely awaiting a visit from its mother, according to Ruth. A doe, after brief periods of feeding and grooming her fawn, will spend much of her day feeding and resting somewhat removed from her young. The fawn ordinarily stays bedded down as if sleeping, but will occasionally move short distances to new bedding sites. “Each spring and summer the SCDNR gets many calls from people who have discovered these ‘lost’ deer,” Ruth said. “Young fawns are without a doubt cute and cuddly, but if taken into captivity they grow into semi-tame adult deer that can become quite dangerous.” Adult buck deer, no matter how they were raised, are especially dangerous during the breeding season. Even does raised by humans are unpredictable. Occasionally, “tame” deer seriously injure people, according to Ruth, and in cases where the deer are a threat to humans, the deer sometimes have to be killed. People often ask the SCD", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00784", "split": "train"}
{"id": "conditionality_train_pos_0318", "text": "If the Secretary approves a plan under this section, the Secretary shall issue an order requiring implementation of such plan by the covered air carriers who submitted such plan and any other covered air carriers. If there are any covered air carriers who did not participate in development of a plan approved under this section, such carriers shall be treated under such order and plan in the same manner as carriers who did participate in development of such plan. ``(d) Regulations.--If a plan described in subsection (a) is not submitted within 180 days after the date of the enactment of this section, or if the Secretary disapproves a plan submitted in accordance with subsection (a), or if the Secretary determines that a plan approved under this section is not being implemented in a manner which provides satisfactory protection for all persons who hold airline tickets described in subsection (a), the Secretary shall issue regulations requiring all covered air carriers to provide air transportation for persons who hold such tickets. Such regulations must be issued within 90 days after the expiration of such 180-day period, the date of disapproval of such plan, or the date of such determination, as the case may be. ``(e) Definitions.--For purposes of this section-- ``(1) Airline ticket.--The term `airline ticket' means any written instrument that embodies a contract of carriage between a covered air carrier and a passenger thereof for interstate or overseas air transportation. ``(2) Covered air carrier.--The term `covered air carrier' means-- ``(A) an air carrier which provides interstate or overseas air transportation primarily with aircraft having seating for more than 60 passengers and which in the 12-month period preceding the date of the enactment of this section, enplaned more than.2 percent of the total number of passengers enplaned on all aircraft used to provide interstate and overseas air transportation in such period; and ``(B) an air carrier not described in subparagraph (A) who enters into an agreement with an air carrier who is described in subparagraph (A) to operate under or use a single air carrier designator code to provide interstate or overseas air transportation, but only with respect to those operations of the carrier not described in subparagraph (A) which are carried out under such code. ``(3) Secretary.--The term `Secretary' means the Secretary of Transportation.''. (b) Conforming Amendment to Table of Contents.--The table of contents in the first section of the Federal Aviation Act of 1958 is amended by adding at the end of the", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01046", "split": "train"}
{"id": "conditionality_train_pos_0319", "text": "in the United States. ``(5) Carryback and carryforward allowed.-- ``(A) In general.--If the credit allowable under subsection (a) for a taxable year exceeds the amount of the limitation under subsection (f)(1) for such taxable year (in this paragraph referred to as the `unused credit year'), such excess shall be a credit carryback to each of the 3 taxable years preceding the unused credit year and a credit carryforward to each of the 20 taxable years following the unused credit year. ``(B) Rules.--Rules similar to the rules of section 39 shall apply with respect to the credit carryback and credit carryforward under subparagraph (A). ``(6) Certain rules to apply.--Rules similar to the rules of subsections (c), (d), and (e) of section 52 shall apply.''. (b) Conforming Amendment.--Section 55(c)(2) of the Internal Revenue Code of 1986 is amended by inserting ``30B(f)(1),'' after ``30(b)(3),''. (c) Clerical Amendment.--The table of sections for subpart B of part IV of subchapter A of chapter 1 of the Internal Revenue Code of 1986 is amended by adding at the end of 30A the following new item: ``Sec. 30B. Employer wage credit for activated military reservists''. (d) Effective Date; Special Rule.-- (1) Effective date.--The amendments made by this section shall apply to amounts paid after September 11, 2001, in taxable years ending after such date. (2) Waiver of limitations.--If refund or credit of any overpayment of tax resulting from the amendments made by this section is prevented at any time before the close of the 1-year period beginning on the date of the enactment of this Act by the operation of any law or rule of law (including res judicata), such refund or credit may nevertheless be made or allowed if claim therefor is filed before the close of such period.", "label": 1, "domain": "government", "token_count": 413, "matched_pair_id": "conditionality_01056", "split": "train"}
{"id": "conditionality_train_pos_0320", "text": "(Abridged) Recent results from the Pierre Auger Observatory (PAO) indicate that the composition of ultra-high-energy cosmic rays (UHECRs) with energies above $10^{19}$ eV may be dominated by heavy nuclei. An important question is whether the distribution of arrival directions for such UHECR nuclei can exhibit observable anisotropy or positional correlations with their astrophysical source objects despite the expected strong deflections by intervening magnetic fields. For this purpose, we have simulated the propagation of UHECR nuclei including models for both the extragalactic magnetic field and the Galactic magnetic field. Assuming that only iron nuclei are injected steadily from sources with equal luminosity and spatially distributed according to the observed large scale structure in the local Universe, at the number of events published by the PAO so far, the arrival distribution of UHECRs would be consistent with no auto-correlation at 95% confidence if the mean number density of UHECR sources $n_s >~ 10^{-6}$ Mpc$^{-3}$, and consistent with no cross-correlation with sources within 95% errors for $n_s >~ 10^{-5}$ Mpc$^{-3}$. On the other hand, with 1000 events above $5.5 \\times 10^{19}$ eV in the whole sky, next generation experiments can reveal auto-correlation with more than 99% probability even for $n_s <~ 10^{-3}$ Mpc$^{-3}$, and cross-correlation with sources with more than 99% probability for $n_s <~ 10^{-4}$ Mpc$^{-3}$. In addition, we find that the contribution of Centaurus A is required to reproduce the currently observed UHECR excess in the Centaurus region. Secondary protons generated by photodisintegration of primary heavy nuclei during propagation play a crucial role in all cases, and the resulting anisotropy at small angular scales should provide a strong hint of the source location if the maximum energies of the heavy nuclei are sufficiently high.", "label": 1, "domain": "academic", "token_count": 424, "matched_pair_id": "conditionality_00417", "split": "train"}
{"id": "conditionality_train_pos_0321", "text": "If Jim Mora could pick a team for his former quarterback Josh Rosen to end up with Thursday night in the NFL draft, that team would be wearing green and white. “I think he’d be a fantastic fit with the Jets,” said Mora, the former UCLA coach who has served as an analyst for the NFL Network on its “Path to the Draft” program. “Josh is kind of ready to go. You give him the keys to the offense, teach it to him, and then he’s going to master it pretty quickly. He’s that type of kid. I think he’d be a tremendous fit with that coaching staff, with that city. I think it would be a great spot for him.” Mora will be tuning in to NFL Network on Thursday to see where Rosen winds up. Rosen is considered one of the top quarterbacks in this draft, but has not really been linked to the Browns or Giants (who own the top two picks) in any of the recent mock drafts. The Jets are a different story. There are people inside the Jets’ organization who like Rosen a lot. Some people around the NFL believe the Jets are debating whether to take Rosen or Oklahoma’s Baker Mayfield with the No. 3 pick. Rosen blew away members of the Jets’ coaching staff with his intelligence. He is viewed by many experts as the most ready quarterback to play immediately. “I’m hoping that’s where he ends up,” Mora said. “I’m hoping he ends up with the Giants or the Jets. I want to see him go as high as possible, but I think the Jets would be a great place for him.” Mora said he believes Rosen is cut out for being a quarterback in New York. When he said this a month ago and said Sam Darnold was a better fit for Cleveland, it caused a stir. But Mora said he did not mean that as a negative. He just believes New York fits Rosen. “He’s incredibly smart,” Mora said. “He can handle a lot of volume. He can handle being the quarterback of an NFL team in New York City with that type of scrutiny. He can handle the workload that comes with being a quarterback in the NFL. He’s been here in Los Angeles. I don’t know which one is the larger media market, but they’re both certainly very big and very prominent. He’s been under the microscope for a long time. He’s been highly scrutinized since high school", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00808", "split": "train"}
{"id": "conditionality_train_pos_0322", "text": "This paper reports Very Large Array observations at 325 and 1425 MHz (90cm and 20cm) during and near the periastron passage of HD 80606b on 2007 November 20. We obtain flux density limits (3-sigma) of 1.7 mJy and 48 microJy at 325 and 1425 MHz, respectively, equivalent to planetary luminosity limits of 2.3 x 10^{24} erg/s and 2.7 x 10^{23} erg/s. These are well above the Jovian value (at 40 MHz) of 2 x 10^{18} erg/s. The motivation for these observations was that the planetary magnetospheric emission is driven by a stellar wind-planetary magnetosphere interaction so that the planetary luminosity would be elevated. Near periastron, HD 80606b might be as much as 3000 times more luminous than Jupiter. Recent transit observations of HD 80606b provide stringent constraints on the planetary mass and radius, and, because of the planet's highly eccentric orbit, its rotation period is likely to be \"pseudo-synchronized\" to its orbital period, allowing a robust estimate of the former. We are able to make robust estimates of the emission frequency of the planetary magnetospheric emission and find it to be around 60--90 MHz. We compare HD 80606b to other high-eccentricity systems and assess the detection possibilities for both near-term and more distant future systems. Of the known high eccentricity planets, only HD 80606b is likely to be detectable, as HD 20782B b and HD 4113b are both likely to have weaker magnetic field strengths. Both the forthcoming \"EVLA low band\" system and the Low Frequency Array may be able to improve upon our limits for HD 80606b, and do so at a more optimum frequency. If the low-frequency component of the Square Kilometre Array (SKA-lo) and a future lunar radio array are able to approach their thermal noise limits, they should be able to detect an HD 80606b-like planet, unless the planet's luminosity increases by substantially less than a factor of 3000.", "label": 1, "domain": "academic", "token_count": 464, "matched_pair_id": "conditionality_00272", "split": "train"}
{"id": "conditionality_train_pos_0323", "text": "This paper discusses the approximation by %semigroups of operators of class ($\\mathscr{C}_0$) on the sphere and focuses on a class of so called exponential-type multiplier operators. It is proved that such operators form a strongly continuous semigroup of contraction operators of class ($\\mathscr{C}_0$), from which the equivalence between approximation for these operators and $K$-functionals introduced by the operators is given. As examples, the constructed $r$-th Boolean of generalized spherical Abel-Poisson operator and $r$-th Boolean of generalized spherical Weierstrass operator denoted by $\\oplus^r V_t^{\\gamma}$ and $\\oplus^r W_t^{\\kappa}$ separately ($r$ is any positive integer, $0<\\gamma,\\kappa\\leq1$ and $t>0$) satisfy that $\\|\\oplus^r V_t^{\\gamma}f - f\\|_{\\mathcal{X}}\\approx \\omega^{r\\gamma}(f,t^{1/\\gamma})_{\\mathcal{X}}$ and $\\|\\oplus^r W_t^{\\kappa}f - f\\|_{\\mathcal{X}}\\approx \\omega^{2r\\gamma}(f,t^{1/(2\\kappa)})_{\\mathcal{X}}$, for all $f\\in \\mathcal{X}$, where $\\mathcal{X}$ is a Banach space of continuous functions or $\\mathcal{L}^p$-integrable functions ($1\\leq p<\\infty$) and $\\|\\cdot\\|_{\\mathcal{X}}$ is the norm on $\\mathcal{X}$ and $\\omega^s(f,t)_{\\mathcal{X}}$ is the moduli of smoothness of degree $s>0$ for $f\\in \\mathcal{X}$. The saturation order and saturation class of the regular exponential-type multiplier operators with positive kernels are also obtained. Moreover, it is proved that $\\oplus^r V_t^{\\gamma}$ and $\\oplus^r W_t^{\\kappa}$ have the same saturation class if $\\gamma=2\\kappa$.", "label": 1, "domain": "academic", "token_count": 468, "matched_pair_id": "conditionality_00331", "split": "train"}
{"id": "conditionality_train_pos_0324", "text": "Symmetry-protected topological (SPT) phases are gapped short-range-entangled quantum phases with a symmetry $G$, which can all be smoothly connected to the trivial product states if we break the symmetry. It has been shown that a large class of interacting bosonic SPT phases can be systematically described by group cohomology theory. In this paper, we introduce a (special) group supercohomology theory which is a generalization of the standard group cohomology theory. We show that a large class of short-range interacting fermionic SPT phases can be described by the group supercohomology theory. Using the data of super cocycles, we can obtain the ideal ground state wave function for the corresponding fermionic SPT phase. We can also obtain the bulk Hamiltonian that realizes the SPT phase, as well as the anomalous (ie, non-on-site) symmetry for the boundary effective Hamiltonian. The anomalous symmetry on the boundary implies that the symmetric} boundary must be gapless for 1+1D boundary, and must be gapless or topologically ordered beyond 1+1D. As an application of this general result, we construct a new SPT phase in 3D, for interacting fermionic superconductors with coplanar spin order (which have $T^2=1$ time-reversal $Z_2^T$ and fermion-number parity $Z_2^f$ symmetries described by a full symmetry group $Z_2^T\\times Z_2^f$). Such a fermionic SPT state can neither be realized by free fermions nor by interacting bosons (formed by fermion-pairs), and thus are not included in the K-theory classification for free fermions or group cohomology description for interacting bosons. We also construct three interacting fermionic SPT phases in 2D with a full symmetry group $Z_2\\times Z_2^f$. Those 2D fermionic SPT phases all have central-charge $c=1$ gapless edge excitations, if the symmetry is not broken.", "label": 1, "domain": "academic", "token_count": 437, "matched_pair_id": "conditionality_00404", "split": "train"}
{"id": "conditionality_train_pos_0325", "text": "We present the first results of a program to characterize the disk and envelope structure of typical Class 0 protostars in nearby low-mass star forming regions. We use Spitzer IRS mid-infrared spectra, high resolution CARMA 230 GHz continuum imaging, and 2-D radiative transfer models to constrain the envelope structure, as well as the size and mass of the circum-protostellar disk in Serpens FIRS 1. The primary envelope parameters (centrifugal radius, outer radius, outflow opening angle, and inclination) are well constrained by the spectral energy distribution (SED), including Spitzer IRAC and MIPS photometry, IRS spectra, and 1.1 mm Bolocam photometry. These together with the excellent uv-coverage (4.5-500 klam) of multiple antenna configurations with CARMA allow for a robust separation of the envelope and a resolved disk. The SED of Serpens FIRS 1 is best fit by an envelope with the density profile of a rotating, collapsing spheroid with an inner (centrifugal) radius of approximately 600 AU, and the millimeter data by a large resolved disk with Mdisk~1.0 Msun and Rdisk~300 AU. These results suggest that large, massive disks can be present early in the main accretion phase. Results for the larger, unbiased sample of Class~0 sources in the Perseus, Serpens, and Ophiuchus molecular clouds are needed to determine if relatively massive disks are typical in the Class 0 stage.", "label": 1, "domain": "academic", "token_count": 320, "matched_pair_id": "conditionality_00169", "split": "train"}
{"id": "conditionality_train_pos_0326", "text": "We present deep Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) optical observations obtained as part of the ACS Nearby Galaxy Survey Treasury (ANGST) as well as early release Wide Field Camera 3 (WFC3) ultra-violet and infrared observations of the nearby dwarf starbursting galaxy NGC 4214. Our data provide a detailed example of how covering such a broad range in wavelength provides a powerful tool for constraining the physical properties of stellar populations. The deepest data reach the ancient red clump at M_F814W -0.2. All of the optical data reach the main sequence turnoff for stars younger than ~300 Myr, and the blue He burning sequence for stars younger than 500 Myr. The full CMD-fitting analysis shows that all three fields in our data set are consistent with ~75% of the stellar mass being older than 8 Gyr, in spite of showing a wide range in star formation rates at the present day. Thus, our results suggest that the scale length of NGC 4214 has remained relatively constant for many Gyr. As previously noted by others, we also find the galaxy has recently ramped up production, consistent with its bright UV luminosity and its population of UV-bright massive stars. In the central field we find UV point sources with F336W magnitudes as bright as -9.9. These are as bright as stars with masses of at least 52-56 M_sun and ages near 4 Myr in stellar evolution models. Assuming a standard IMF, our CMD is well-fitted by an increase in star formation rate beginning 100 Myr ago. The stellar populations of this late-type dwarf are compared with those of NGC 404, an early-type dwarf that is also the most massive galaxy in its local environment. The late-type dwarf appears to have a similar high fraction of ancient stars, suggesting that these dominant galaxies may form at early epochs even if they have low total mass and very different present-day morphologies.", "label": 1, "domain": "academic", "token_count": 409, "matched_pair_id": "conditionality_00321", "split": "train"}
{"id": "conditionality_train_pos_0327", "text": "A new type of neutrino mixing named bi-pair neutrino mixing is proposed to describe the current neutrino mixing pattern with a vanishing reactor mixing angle and is determined by a mixing matrix with two pairs of identical magnitudes of matrix elements. As a result, we predict \\sin^2\\theta_{12}=1-1/\\sqrt{2}(\\approx 0.293) for the solar neutrino mixing and either \\sin^2\\theta_{23}=\\tan^2\\theta_{12} or \\cos^2\\theta_{23}=\\tan^2\\theta_{12} for the atmospheric neutrino mixing. We determine flavor structure of a mass matrix M, leading to diagonal masses of m_{1,2,3}, and find that |M_{\\mu\\mu}-M_{ee}/t^2_{12}|:|M_{\\mu \\tau}|:|M_{\\tau \\tau}-M_{ee}/t^2_{12}|=t^2_{23}:|t_{23}|:1 for the normal mass hierarchy if m_1=0, where t_{ij}=\\tan\\theta_{ij} (i,j=1,2,3) and M_{ij} (i,j=e,\\mu,\\tau) stand for flavor neutrino masses. For the inverted mass hierarchy, the bi-pair mixing scheme turns out to satisfy the strong scaling ansatz requiring that |M_{\\mu\\mu}|:|M_{\\mu\\tau}|:|M_{\\tau\\tau}|=1:|t_{23}|:t^2_{23} if m_3=0.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00302", "split": "train"}
{"id": "conditionality_train_pos_0328", "text": "motorcycle in front of the office and moved to the Olomowewe area in Adiyan, where they burnt three motorcycles parked by the roadside. There was confusion everywhere. “Through the intervention of the police, the situation was brought under control on Sunday evening. Policemen have been patrolling the community.” Another resident, who did not want his name in print, said there might have been a disagreement between Olatunbosun and the vigilantes prior to the incident. “Those that killed him must be brought to book. I don’t think they beat him because he stole the dryer or not. “They probably had a disagreement with him before now and they decided to deal with him. They beat him with charms and later took him to the station,” he said. PUNCH Metro learnt that the two vigilantes were later arrested by the Agbado division. A police source said the hairdryer purportedly recovered from Olatunbosun was taken to the station. “By the time the vigilantes brought him to the station with the dryer, he had been seriously injured. “He was released to go and treat himself, but he died in the hospital,” the source added. The Ogun State Police Public Relations Officer, ASP Abimbola Oyeyemi, said the suspects were being investigated for murder and would be charged to court afterwards. “The two vigilantes in question are in custody. The Commissioner of Police, Ahmed Iliyasu, has ordered that they should be transferred to the Homicide Section of the State Criminal Investigation and Intelligence Department for proper investigation. Even if he was caught stealing, that does not mean he should be killed,” he added.", "label": 1, "domain": "news", "token_count": 340, "matched_pair_id": "conditionality_00641", "split": "train"}
{"id": "conditionality_train_pos_0329", "text": "The ISM evolution of elliptical galaxies experiencing feedback from accretion onto a central black hole was studied recently with high-resolution 1D hydrodynamical simulations including radiative heating and pressure effects, a RIAF-like radiative efficiency, mechanical input from AGN winds, and accretion-driven starbursts. Here we focus on the observational properties of the models in the X-ray band (nuclear luminosity; hot ISM luminosity and temperature; temperature and brightness profiles during quiescence and during outbursts). The nuclear bursts last for ~10^7 yr, with a duty-cycle of a few X (10^-3-10^-2); the present epoch bolometric nuclear emission is very sub-Eddington. The ISM thermal luminosity \\lx oscillates in phase with the nuclear one; this helps reproduce statistically the observed large \\lx variation. In quiescence the temperature profile has a negative gradient; thanks to past outbursts, the brightness profile lacks the steep shape typical of inflowing models. Outbursts produce disturbances in these profiles. Most significantly, a hot bubble from shocked hot gas is inflated at the galaxy center; the bubble would be conical in shape, and show radio emission. The ISM resumes a smooth appearance on a time-scale of ~200 Myr; the duty-cycle of perturbances in the ISM is of the order of 5-10%. From the present analysis, additional input physics is important in the ISM-black hole coevolution, to fully account for the properties of real galaxies, as a confining external medium and a jet. The jet will reduce further the mass available for accretion (and then the Eddington ratio $l$), and may help, together with an external pressure, to produce flat or positive temperature gradient profiles (observed in high density environments). Alternatively, $l$ can be reduced if the switch from high to low radiative efficiency takes place at a larger $l$ than routinely assumed.", "label": 1, "domain": "academic", "token_count": 409, "matched_pair_id": "conditionality_00356", "split": "train"}
{"id": "conditionality_train_pos_0330", "text": "We investigate two closely related subjects: (i) existence of a pure persistent spin current in semiconducting mesoscopic device with a spin-orbit interaction's (SOI), and (ii) the definition of the spin current in the presence of SOI. Through physical argument from four physical pictures in different aspects, we provide strong evidences that the persistent spin current does exist in a device with SOI in the absence of any magnetic materials. This persistent spin current is an analog of the persistent charge current in a mesoscopic ring threaded by a magnetic flux, and it describes the real spin motion and can be measured experimentally. We then investigate the definition of the spin current. We point out that (i) the non-zero spin current in the equilibrium SOI device is the persistent spin current, (ii) the spin current is in general not conserved, and (iii) the Onsager relation is violated for the spin transport no matter what definition of the spin current is used. These issues, the non-zero spin current in the equilibrium case, the non-conserved spin current, and the violation of the Onsager relation, are intrinsic properties of spin transport. We note that the conventional definition of the spin current has very clear physical intuition and describes the spin motion very well. Therefore we feel that the conventional definition of the spin current makes physical sense and there is no need to modify it. In addition, the relationship between the persistent spin current and transport spin current, the persistent linear and angular spin currents in the SOI region of the hybrid ring, are discussed. Finally, we show that if the spin-spin interaction is included into the Hamiltonian, the persistent spin current is automatically conserved using the conventional definition.", "label": 1, "domain": "academic", "token_count": 348, "matched_pair_id": "conditionality_00069", "split": "train"}
{"id": "conditionality_train_pos_0331", "text": "A few long gamma-ray bursts such as GRB 050421 show no afterglow emission beyond the usual initial steep decay phase. It has been suggested that these events correspond to \"naked\" bursts that occur in a very low density environment. We reconsider this possibility in the context of various scenarios for the origin of the afterglow. In the standard model where the afterglow results from the forward shock as well as in the alternative model where the afterglow comes from the reverse shock, we aim to obtain constraints on the density of the environment, the microphysics parameters, or the Lorentz factor of the ejecta, which are imposed by the absence of a detected afterglow. For the two models we compute the afterglow evolution for different values of the external density (uniform or wind medium) and various burst parameters. We then compare our results to the Swift data of GRB 050421, which is the best example of a long burst without afterglow. In the standard model we show that consistency with the data imposes that the external density does not exceed 1E-5 cm-3 or that the microphysics parameters are very small with epsilon_e <~ 1E-2 and epsilon_B <~ 1E-4. If the afterglow is caused by the reverse shock, we find that its contribution can be strongly reduced if the central source has mainly emitted fast-moving material (with less than 10 - 30 % of the kinetic energy at Gamma<100 and was located in a dense environment. The two considered scenarios therefore lead to opposite constraints on the circumburst medium. The high-density environment, favored by the reverse shock model, better corresponds to what is expected if the burst progenitor was a massive star.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00374", "split": "train"}
{"id": "conditionality_train_pos_0332", "text": "It would be an understatement to say the Ontario Progressive Conservative Party has had an unusual fortnight. A disaster is more like it. But there are welcome signs that the party is starting to gather its wits and regroup. It may still be a formidable force come this June’s provincial election. We certainly hope so. Kathleen Wynne’s tired and scandal-saddled Ontario Liberal Party has recklessly vandalized the once-envied economy of Canada’s most populous province. Recent improvements — linked to U.S. recovery, not any Liberal wisdom — cannot undo the damage that will be felt for generations thanks to the crushing debts, hydro costs and regulatory excesses that have piled up in 13 years of Liberal rule. Ontarians desperately want another option. Up until recently, the PCs seemed to be it, and were within sight of winning the next election until leader Patrick Brown was brought down by a news report of sexual misconduct. This left the party leaderless mere months before the election. The party quickly settled on Vic Fedeli as an interim leader; Fedeli, himself, despite obvious leadership ambitions of his own, wisely and graciously agreed to remove himself for consideration from the full-time job while he works to keep the party intact. The party’s executive (which also lost its president this week to sexual-assault allegations) has settled on a fast leadership race, with a high entrance fee to deter frivolous candidates. The new leader will be chosen March 10. This is the right decision. The sitting caucus members seemed to prefer simply selecting one of their own, and there’s the appeal of simplicity there. But the problem with an opposition party’s caucus is that it’s not representative of the province at large. PC members who live in ridings where there is no PC MPP deserve their say in who the next leader should be. Nor are we convinced by arguments based on fears of disruptive outsider candidates — obviously they mean Doug Ford — seizing on the chaos. Yes, the vote will cost money, and the PCs need every dollar for the upcoming general election. But democracy can’t be considered an inconvenience or a burden even amid crises. It’s the whole point, and a party that does not trust its own members should not be trusted with the entire province. Trust the members to choose, and then let Ontarians decide if they chose right.", "label": 1, "domain": "news", "token_count": 472, "matched_pair_id": "conditionality_00669", "split": "train"}
{"id": "conditionality_train_pos_0333", "text": "Happy Fourth of July! Celebrate Independence Day with this fruity star-spangled sangria from lifestyle blog Heart and Seam. Interested in 4th of July? Add 4th of July as an interest to stay up to date on the latest 4th of July news, video, and analysis from ABC News. Add Interest From fashion and beauty to wellness and recipes Heart and Seam founder Janet Cooke shares real-life experiences on her blog from her home in New Hampshire -- including her festive and tasty summer sangria recipe. Heart and Seam Lifestyle Blog \"This is a fun festive spin on a classic sangria recipe,\" Cooke told \"GMA.\" \"The best part about this recipe is that you can make it in large batches so it's perfect for a Fourth of July cookout where there will be lots of family and friends to enjoy.\" Check out the full recipe and pour this red, wine and blueberry beverage all day for friends and family. Heart and Seam Lifestyle Blog Ingredients 1 bottle red wine (I like Pinot Noir or Shiraz) 1-1/2 cups cranberry juice 1 cup brandy juice from one large orange 2 cups fresh blueberries 8 ounces fresh strawberries cut in quarters Club soda Directions To a large pitcher add wine, cranberry juice, brandy and orange juice. Add blueberries and strawberries. Chill for a few hours. To serve, fill glasses half full with ice and use a slotted spoon to add fruit from the pitcher to each glass. Pour liquid over ice and fruit, top with club soda and serve. Tips Add raspberries, blackberries and even apples to create even more of a festive drink. Be sure to add the ice to the glasses and not the pitcher itself. You will dilute the sangria if you add directly to the pitcher.", "label": 1, "domain": "news", "token_count": 365, "matched_pair_id": "conditionality_00532", "split": "train"}
{"id": "conditionality_train_pos_0334", "text": "If you liked Middle-earth: Shadow of Mordor, you’re going to be either extremely happy or a little disappointed about its sequel, Middle-earth: Shadow of War. In just about every way, developer Monolith is expanding, increasing, and doubling down on the elements that made Shadow of Mordor work, as was evident when it showed off a big chunk of the game to journalists at E3 2017. But it also feels like an expanded and deeper version of the same game, which might be a turnoff to players expecting massive overhauls. Shadow of War is bigger, more easily traversed, and most importantly, more Nemesis System-focused than its predecessor. Players of Shadow of Mordor will remember that game’s signature feature, a system in which the orcs that populate the Tolkien universe’s evil country of Mordor grow, level up, and remembered their encounters with you. A random orc that happens to strike a killing blow against the player advances up the ranks of orc society, gaining a name and traits, and popping up later in the world to menace you again. The idea is to create player-personal stories of rivalries and revenge between you and the grunts and bosses you take on throughout the game. More menacing nemeses The marketing tag line for Shadow of War is “Nothing is forgotten,” and that’s the marching order for the most interesting aspect of the game. Now the Nemesis System that lets orcs get more powerful over time is expanded, allowing you to grow an army of your own. But your captured, mentally dominated orcs remember what happens to them — and might decide to betray you if you’re a bad leader. Monolith is expanding, increasing, and doubling down on the elements that made Shadow of Mordor work. “There’s always those guys that people love to hate,” Bob Roberts, design director, explained. “Last time, it was about killing and getting revenge. And there were some people who would get to that point of feeling like this guy was important to them, but they didn’t just want to kill him, that’s the end. So there’s this whole dimension now where you make him a follower, he keeps his personality, he becomes loyal to you.” The demo we played at E3 let players roam around doing open-world activities like ambient quests and gathering collectibles, engaging in story moments, or trying to grow their army and capture territory in Mordor. It’s", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00708", "split": "train"}
{"id": "conditionality_train_pos_0335", "text": "A horse that was trapped in a mud pit in southeastern Florida has been freed, thanks to some diligent firefighters. Palm Beach County firefighters received a call early Monday morning about a horse stuck in the mud in The Acreage, Florida, an unincorporated area near West Palm Beach. When they first arrived on the scene, firefighters found the horse stuck in the mud up to its belly. #BreakingNews @PBCFR on location of horse stuck in mud in #acreage #specialoperations & Battalion 2 crews working on freeing horse pic.twitter.com/IQk1zyl9Ut — PBC Fire Rescue (@PBCFR) April 17, 2017 \"Firefighters ... started working on digging the horse from the mud using hand tools and keeping the scared horse calm during the rescue,\" Captain Albert Borroto, public information officer with the Palm Beach County Fire Rescue, told ABC News. According to firefighters, a local veterinarian sedated the horse in order to get it out safely. Horse Cmd *update* straps are around horse, #firefighters preparing to start pulling horse from mud pic.twitter.com/LvX0p7glue — PBC Fire Rescue (@PBCFR) April 17, 2017 \"Using training learned in equestrian rescue classes, the crews were able to get the rescue straps around the animal and prepare to pull it from the mud with a pulley system,\" Borroto said. Horse Cmd *update2* Vet on location has sedated horse, #firefighters pulling horse from mud pic.twitter.com/eKjWGDpYIx — PBC Fire Rescue (@PBCFR) April 17, 2017 It took about an hour to get the horse out. \"The 25-year-old horse named Skip was evaluated by the veterinarian and is doing well,\" Borroto said. Horse Cmd*update3* horse safely out of mud, sedation has worn off and he is being evaluated by veterinarian on location pic.twitter.com/YaVXz9ubNn — PBC Fire Rescue (@PBCFR) April 17, 2017 Authorities have not released how the horse became stuck in the mud or if it has been claimed by someone in the area.", "label": 1, "domain": "news", "token_count": 456, "matched_pair_id": "conditionality_00544", "split": "train"}
{"id": "conditionality_train_pos_0336", "text": "The high-frequency quasi-periodic oscillations (HF QPOs) that appear in the X-ray fluxes of low-mass X-ray binaries remain an unexplained phenomenon. Among other ideas, it has been suggested that a non-linear resonance between two oscillation modes in an accretion disc orbiting either a black hole or a neutron star plays a role in exciting the observed modulation. Several possible resonances have been discussed. A particular model assumes resonances in which the disc-oscillation modes have the eigenfrequencies equal to the radial and vertical epicyclic frequencies of geodesic orbital motion. This model has been discussed for black hole microquasar sources as well as for a group of neutron star sources. Assuming several neutron (strange) star equations of state and Hartle-Thorne geometry of rotating stars, we briefly compare the frequencies expected from the model to those observed. Our comparison implies that the inferred neutron star radius \"RNS\" is larger than the related radius of the marginally stable circular orbit \"rms\" for nuclear matter equations of state and spin frequencies up to 800Hz. For the same range of spin and a strange star (MIT) equation of state, the inferrred radius RNS is roughly equal to rms. The Paczynski modulation mechanism considered within the model requires that RNS < rms. However, we find this condition to be fulfilled only for the strange matter equation of state, masses below one solar mass, and spin frequencies above 800Hz. This result most likely falsifies the postulation of the neutron star 3:2 resonant eigenfrequencies being equal to the frequencies of geodesic radial and vertical epicyclic modes. We suggest that the 3:2 epicyclic modes could stay among the possible choices only if a fairly non-geodesic accretion flow is assumed, or if a different modulation mechanism operates.", "label": 1, "domain": "academic", "token_count": 387, "matched_pair_id": "conditionality_00250", "split": "train"}
{"id": "conditionality_train_pos_0337", "text": "If star formation proceeds by thermal fragmentation and the subsequent gravitational collapse of the individual fragments, how is it possible to form fragments massive enough for O and B stars in a typical star-forming molecular cloud where the Jeans mass is about 1Msun at the typical densities (10^4 cm^-3) and temperatures (10K)? We test the hypothesis that a first generation of low-mass stars may heat the gas enough that subsequent thermal fragmentation results in fragments >=10Msun, sufficient to form B stars. We combine ATCA and SMA observations of the massive star-forming region G8.68-0.37 with radiative transfer modeling to derive the present-day conditions in the region and use this to infer the conditions in the past, at the time of core formation. Assuming the current mass/separation of the observed cores equals the fragmentation Jeans mass/length and the region's average density has not changed, requires the gas temperature to have been 100K at the time of fragmentation. The postulated first-generation of low-mass stars would still be around today, but the number required to heat the cloud exceeds the limits imposed by the observations. Several lines of evidence suggest the observed cores in the region should eventually form O stars yet none have sufficient raw material. Even if feedback may have suppressed fragmentation, it was not sufficient to halt it to this extent. To develop into O stars, the cores must obtain additional mass from outside their observationally defined boundaries. The observations suggest they are currently fed via infall from the very massive reservoir (~1500Msun) of gas in the larger pc scale cloud around the star-forming cores. This suggests that massive stars do not form in the collapse of individual massive fragments, but rather in smaller fragments that themselves continue to gain mass by accretion from larger scales.", "label": 1, "domain": "academic", "token_count": 365, "matched_pair_id": "conditionality_00279", "split": "train"}
{"id": "conditionality_train_pos_0338", "text": "The possible existence of a continuum encompassing the diversity of explosive stellar deaths,ranging from ordinary SNe to relativistic hypernovae associated with long duration GRBs, is under intense debate. In this context, SN2008D associated with XT080109 could represent a paradigmatic case, since it might exemplify a potential borderline event. The main aim is to infer geometric information of SN2008D through the evolution of its linear optical polarization. We also report the polarization evolution of SN2007uy, and discuss the properties of the host ISM towards the XT. The final goal is to compare the polarization properties, and hence the geometries of both SNe, which shone contemporaneously in NGC2770. This fortunate coincidence brought us the opportunity to observe both SNe simultaneously, and most importantly, with identical instrumental setups. The observations span 74.9 days, starting 3.6 days after the XT and are distributed in 11 visits. In addition we performed observations in the mm range in order to identify the dominant polarization. We report positive linear polarization detections at several epochs for SN2008D at a level of ~1% and at ~1.5% for SN2007uy. SN2007uy shows constant polarization, which could be described by the host interstellar polarization plus a constant eccentricity expansion on the sky plane. A statistical analysis of the distribution of the SN2008D Stokes parametres suggests that it could show an intrinsic variable polarization component. Assuming the SN2007uy polarization is constant, we find that the evolution of the intrinsic SN2008D polarization could be explained by an aspherical axisymmetric expansion with variable eccentricity. We come to the same result even if we make no assumption on SN2007uy, although at a lower significance level. We suggest that at least the projected, if not the intrinsic, geometries of both SNe could differ.", "label": 1, "domain": "academic", "token_count": 385, "matched_pair_id": "conditionality_00091", "split": "train"}
{"id": "conditionality_train_pos_0339", "text": "of the Omnibus Budget Reconciliation Act of 1986, the provisions of such sections (as in effect before the date of the enactment of this Act) shall continue to apply with respect to such waiver until-- (i) the organization is eligible to be a provider under this Act; (ii) the Secretary issues and implements the regulations referred to in section 2(c)(1); and (iii) the organization has had a reasonable opportunity to apply to be recognized as a provider, such application has been formally considered by the Secretary, and a final determination on the application has been made. (B) Continuation of waiver until effective date.-- The waiver authority of any organization applying for recognition under subparagraph (A) shall continue until-- (i) the date that the Secretary determines that such organization is eligible to be and can actually serve as a provider under this Act; or (ii) if the Secretary determines that the organization is not eligible to be a provider under this Act, the expiration of the waiver. (C) Consideration of periods of operation prior to this act.--In determining whether an organization is eligible to be a provider under subparagraph (A), the Secretary-- (i) in determining whether the organization has successfully completed a trial period under this Act, shall consider any period before the date of the enactment of this Act during which an organization was operating under a waiver described in subparagraph (A); and (ii) shall treat the organization as eligible to be a provider under this Act for periods after the date of the enactment of this Act and before such determination if the organization meets the requirements of the regulations issued under section 2(c)(1) during such periods.", "label": 1, "domain": "government", "token_count": 336, "matched_pair_id": "conditionality_00874", "split": "train"}
{"id": "conditionality_train_pos_0340", "text": "If local workforce subcontracting requirements have not been met in any contract entered into by the General Services Administration, the report required under this subsection shall include a description of efforts made by the General Services Administration to meet the requirements in such contract. (b) GAO Report.--Not later than 180 days after submission of the first report required under subsection (a), the Comptroller General of the United States shall submit to Congress a report commenting on the findings described in such report and including recommendations for further actions to ensure compliance with local workforce subcontracting requirements. SEC. 6. ACQUISITION WORKFORCE IMPROVEMENTS. (a) Evaluation and Report.--Not later than 180 days after the date of the enactment of this Act, the head of each executive agency shall submit to Congress a report evaluating the strength and sufficiency of its acquisition workforce. (b) Content.--The report required under subsection (a) shall include-- (1) a 30-year history of the size of the acquisition agency's workforce; and (2) a description of measures the agency is implementing to address any shortage of acquisition workforce personnel. (c) Public Comment.--In preparing the report required under subsection (a), the head of each executive agency shall solicit feedback regarding the agency's acquisition workforce, including through a public comment process. SEC. 7. USE OF PROCUREMENT ASSISTANCE RESOURCES. Not later than 180 days after the date of the enactment of this Act, the Federal Acquisition Regulatory Council shall amend the Federal Acquisition Regulation to require executive agencies to take actions to encourage prospective contractors to utilize contracting assistance resources that are offered in their communities. The Federal Acquisition Regulation, as so amended, shall include a requirement that the bid solicitation documents for a contract include language encouraging the use of such resources. SEC. 8. IMPROVING OUTREACH TO SMALL BUSINESS CONCERNS. Section 15 of the Small Business Act (15 U.S.C. 644) is amended by adding at the end the following: ``(q) Small Business Outreach Program.-- ``(1) Program established.--The Administrator and the Administrator of General Services shall jointly establish an outreach program-- ``(A) to communicate with small business concerns regarding specific contracting opportunities with the Federal Government; and ``(B) to inform small business concerns about opportunities to learn about the process of contracting with the Federal Government. ``(2) Annual report to congress.--Not later than 1 year after the date of enactment of", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00904", "split": "train"}
{"id": "conditionality_train_pos_0341", "text": "If G is a finitely generated group, and A an algebraic group, then Hom(G,A) is a possibly reducible algebraic variety denoted by R_A(G). Here we define the profile function, P_d(R_A(G)), of the representation variety of G over A to be P_d(R_A(G))=(N_d(R_A(G)),...,N_0(R_A(G))), where N_i(R_A(G)) stands for the number of irreducible components of R_A(G) of dimension i, where 0\\leq i\\leq d, and d=Dim(R_A(G)). We then use this invariant in the study of fg groups and prove various results. In particular, we show that if G an orientable surface group of genus g\\geq 1, then P_d(R_{SL(2,C)}(G))\\neq P_d(R_{PSL(2,C)}(G)). We also show that the same holds for G a torus knot group with presentation <x,y;x^p=y^t> where both p,t are greater than 2, and that the same also holds when G is a the fundamental group of a compact non-orientable surface of genus g\\geq 3. Further, we show that if a group G can be n+1 generated, and presented by <x_1,...,x_n,y ; W=y^p>, where W is a non-trivial word in F_n=<x_1,...,x_n>, and A=PSL(2, C), that then Dim(R_{A}(G)) is equal to Max{3n, Dim(R_{A}(G'))+2 \\} \\leq 3n+1, where G'=<x_1,...,x_n; W=1>. We also give a condition guaranteeing that the resulting algebraic variety is reducible.", "label": 1, "domain": "academic", "token_count": 394, "matched_pair_id": "conditionality_00055", "split": "train"}
{"id": "conditionality_train_pos_0342", "text": "If you’ve not seen the previous series of Last Tango in Halifax or you’ve got a hazy memory, here’s a guide to what’s happened so far, who plays who and where you’ve seen the actors before. Advertisement Celia (Anne Reid) The Last Tango story begins with Celia, a 70-something widow, who gets in touch with childhood sweetheart Alan after she spots him on Facebook. They meet up and get on so well that it’s like they’ve never been apart. By episode two they’re engaged, much to the shock and confusion of their children. The duo are based on writer Sally Wainwright’s own mother’s experience of a meeting her teenage boyfriend 60 years later on Friends Reunited. Wait, so there is hope I could end up marrying Sam, who I fancied in year nine? Interrrrresting…. Anyway, Celia’s daughter Caroline is going out with a woman named Kate in series two and unlike Alan, Celia doesn’t take the same-sex thing well at all. In fact, she refuses to accept it and there are torrid, throw-plates-at-the-wall, rows until Celia realises she’s making her daughter miserable with her homophobia. As the Christmas special begins, Celia is happily married to Alan and is caught up in the daily chaos of her family. (Some) lessons have been learnt although her sharp tongue hasn’t lost its edge. Played by: Anne Reid, who you’ll know as Valerie in Coronation Street and Jean in dinnerladies. Alan (Derek Jacobi) Alan knows all about life’s peaks and troughs. He gets engaged to Celia and then at the end of series one he has a heart attack. It’s all ok though because he recovers and marries Celia as planned. Alan’s daughter Gillian has a complex time in the show and he’s very involved – but more about that later. The crucial thing to know about Alan is that he discovers he has a son called Gary from an affair he had in the 1980s while married to his first wife, his daughter Gillian’s mum. Alan doesn’t tell Celia about Gary because he’s worried she’ll judge him for having had an affair – and especially because Celia’s own husband was adulterous and she suffered badly. When he does tell her, she’s devastated and genuinely questions whether he’s the man she thought he was. By the time series four", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00686", "split": "train"}
{"id": "conditionality_train_pos_0343", "text": "The relation between the clustering properties of luminous matter in the form of galaxies and the underlying dark matter distribution is of fundamental importance for the interpretation of ongoing and upcoming galaxy surveys. The so called local bias model, where galaxy density is a function of local matter density, is frequently discussed as a means to infer the matter power spectrum or correlation function from the measured galaxy correlation. However, gravitational evolution generates a term quadratic in the tidal tensor and thus non-local in the density field, even if this term is absent in the initial conditions (Lagrangian space). Because the term is quadratic, it contributes as a loop correction to the power spectrum, so the standard linear bias picture still applies on large scales, however, it contributes at leading order to the bispectrum for which it is significant on all scales. Such a term could also be present in Lagrangian space if halo formation were influenced by the tidal field. We measure the corresponding coupling strengths from the matter-matter-halo bispectrum in numerical simulations and find a non-vanishing coefficient for the tidal tensor term. We find no scale dependence of the bias parameters up to k=0.1 h/Mpc and that the tidal effect is increasing with halo mass. While the Lagrangian bias picture is a better description of our results than the Eulerian bias picture, our results suggest that there might be a tidal tensor bias already in the initial conditions. We also find that the coefficients of the quadratic density term deviate quite strongly from the theoretical predictions based on the spherical collapse model and a universal mass function. Both quadratic density and tidal tensor bias terms must be included in the modeling of galaxy clustering of current and future surveys if one wants to achieve the high precision cosmology promise of these datasets.", "label": 1, "domain": "academic", "token_count": 351, "matched_pair_id": "conditionality_00409", "split": "train"}
{"id": "conditionality_train_pos_0344", "text": "Provided that there is no theoretical frame for complex engineered systems (CES) as yet, this paper claims that bio-inspired engineering can help provide such a frame. Within CES bio-inspired systems play a key role. The disclosure from bio-inspired systems and biological computation has not been sufficiently worked out, however. Biological computation is to be taken as the processing of information by living systems that is carried out in polynomial time, i.e., efficiently; such processing however is grasped by current science and research as an intractable problem (for instance, the protein folding problem). A remark is needed here: P versus NP problems should be well defined and delimited but biological computation problems are not. The shift from conventional engineering to bio-inspired engineering needs bring the subject (or problem) of computability to a new level. Within the frame of computation, so far, the prevailing paradigm is still the Turing-Church thesis. In other words, conventional engineering is still ruled by the Church-Turing thesis (CTt). However, CES is ruled by CTt, too. Contrarily to the above, we shall argue here that biological computation demands a more careful thinking that leads us towards hypercomputation. Bio-inspired engineering and CES thereafter, must turn its regard toward biological computation. Thus, biological computation can and should be taken as the ground for engineering complex non-linear systems. Biological systems do compute in terms of hypercomputation, indeed. If so, then the focus is not algorithmic or computational complexity but computation-beyond-the-Church-Turing-barrier. We claim that we need a new computational theory that encompasses biological processes wherein the Turing-Church thesis is but a particular case.", "label": 1, "domain": "academic", "token_count": 334, "matched_pair_id": "conditionality_00382", "split": "train"}
{"id": "conditionality_train_pos_0345", "text": "We apply population synthesis techniques to calculate the present day population of post-common envelope binaries (PCEBs) for a range of theoretical models describing the common envelope (CE) phase. Adopting the canonical energy budget approach we consider models where the ejection efficiency, $\\alpha_{\\rmn{CE}}$ is either a constant, or a function of the secondary mass. We obtain the envelope binding energy from detailed stellar models of the progenitor primary, with and without the thermal and ionization energy, but we also test a commonly used analytical scaling. We also employ the alternative angular momentum budget approach, known as the $\\gamma$-algorithm. We find that a constant, global value of $\\alpha_{\\rmn{CE}} \\ga 0.1$ can adequately account for the observed population of PCEBs with late spectral-type secondaries. However, this prescription fails to reproduce IK Pegasi, which has a secondary with spectral type A8. We can account for IK Pegasi if we include thermal and ionization energy of the giant's envelope, or if we use the $\\gamma$-algorithm. However, the $\\gamma$-algorithm predicts local space densities that are 1 to 2 orders of magnitude greater than estimates from observations. In contrast, the canonical energy budget prescription with an initial mass ratio distribution that favours unequal initial mass ratios gives a local space density which is in good agreement with observations, and best reproduces the observed distribution of PCEBs. Finally, all models fail to reproduce the sharp decline for orbital periods, $P_{\\rmn{orb}} \\ga 1$ d in the orbital period distribution of observed PCEBs, even if we take into account selection effects against systems with long orbital periods and early spectral-type secondaries.", "label": 1, "domain": "academic", "token_count": 361, "matched_pair_id": "conditionality_00128", "split": "train"}
{"id": "conditionality_train_pos_0346", "text": "Observations of the Lyman-alpha forest and of high-redshift galaxies at z~5-10 imply that there were just enough photons to maintain the universe in an ionized state at z~5-6, indicating a \"photon-starved\" end to reionization. The ionizing emissivity must have been larger at earlier times in order to yield the extended reionization history implied by the electron scattering optical depth constraint from WMAP. Here we address the possibility that a faint population of galaxies with host halo masses of ~1e8-1e9 Msun dominated the ionizing photon budget at redshifts of about z>9, due to their much higher escape fractions. Such faint, early galaxies, would not have formed in ionized regions due to suppression by heating from the UV background (UVB), and would therefore not contribute to the ionizing background at z<6, after reionization is complete. Our model matches: (1) the low escape fractions observed for high-redshift galaxies, (2) the WMAP constraint of tau_es~0.09, (3) the low values for the UVB at z<6, and (4) the observed star formation rate density inferred from Lyman-break galaxies. A top heavy IMF from Pop III stars is not required in this scenario. We compare our model to recent ones in the literature that were forced to introduce an escape fraction that increases strongly towards high redshift, and show that a similar evolution occurs naturally if low mass galaxies possess high escape fractions.", "label": 1, "domain": "academic", "token_count": 313, "matched_pair_id": "conditionality_00492", "split": "train"}
{"id": "conditionality_train_pos_0347", "text": "The last time we covered LineageOS, the project had started supporting seven new phones, including the Xperia Z5 Compact and LG K10. Since then, several additional devices have been added to the official build roster. These include the Sony Xperia Z5, Samsung Galaxy S6, and Redmi 3S/3X. Before we get to the new devices, there were a few developments in the LineageOS community worth mentioning. Official builds for the HTC One M9 were added back in early January, but only one version (dated January 10) was uploaded. The ROM caused hardware-encrypted One M9s to be unbootable, since only software encryption was supported. The maintainer pulled support a few days later, and as of the time of writing, it's unclear if builds will resume. On a similar note, LineageOS has also discontinued builds for the ASUS ZenFone 2. Lineage previously supported both the 1080p (Z00A) and 720p (Z008) models, and the final release was uploaded on January 27. The maintainer said on XDA, \"I'm calling it quits on these devices. My touchscreen on my last zf2 gave out and I'm done wasting money repairing these things. [...] I wanted to take a moment here to thank all of those who have participated here, supported my work and the work of crpalmer early on.\" And now, without further ado, here are the newly-supported LineageOS devices: Sony Xperia Z5 (sumire) Samsung Galaxy S6 SM-G920F (zerofltexx) Samsung Galaxy S5 Sport SM-G860P (kltesprsports) ZTE Axon 7 Mini (tulip) Xiaomi Redmi 3S/3X (land) Most of these devices have been around for a few years, so if you own one of these phones already, maybe LineageOS can extend its usefulness for a while longer.", "label": 1, "domain": "news", "token_count": 404, "matched_pair_id": "conditionality_00775", "split": "train"}
{"id": "conditionality_train_pos_0348", "text": "to administer the opioid overdose drug; and (C) the steps that need to be taken after administration of the opioid overdose drug. (b) Exception.--Subsection (a) shall not apply to a health care professional if the harm was caused by the gross negligence or reckless misconduct of the health care professional. SEC. 6. LIMITATION ON CIVIL LIABILITY FOR INDIVIDUALS WORKING FOR OR VOLUNTEERING AT A STATE OR LOCAL AGENCY OPIOID OVERDOSE PROGRAM. (a) In General.--Notwithstanding any other provision of law, except as provided in subsection (b), no individual who provides an opioid overdose drug shall be liable for harm caused by the emergency administration of an opioid overdose drug by another individual if the individual who provides such drug-- (1) works for or volunteers at an opioid overdose program; and (2) provides the opioid overdose drug as part of the opioid overdose program to an individual authorized by the program to receive an opioid overdose drug. (b) Exception.--Subsection (a) shall not apply if the harm was caused by the gross negligence or reckless misconduct of the individual who provides the drug. SEC. 7. LIMITATION ON CIVIL LIABILITY FOR INDIVIDUALS WHO ADMINISTER OPIOID OVERDOSE DRUGS. (a) In General.--Notwithstanding any other provision of law, except as provided in subsection (b), no individual shall be liable for harm caused by the emergency administration of an opioid overdose drug to an individual who has or reasonably appears to have suffered an overdose from heroin or other opioid, if-- (1) the individual who administers the opioid overdose drug-- (A) obtained the drug from a health care professional or as part of an opioid overdose program; or (B) is doing so pursuant to a prescription for an opioid overdose drug under section 505 of the Federal Food, Drug, and Cosmetic Act (21 U.S.C. 355) or is licensed under section 351 of the Public Health Service Act (42 U.S.C. 262); and (2) was educated in accordance with section 5(a)(2) by the health care professional or an opioid overdose program. (b) Exception.--Subsection (a) shall not apply to an individual if the harm was caused by the gross negligence or reckless misconduct of the individual who administers the drug.", "label": 1, "domain": "government", "token_count": 484, "matched_pair_id": "conditionality_00967", "split": "train"}
{"id": "conditionality_train_pos_0349", "text": "a copy of the State tax return of each employer making such a submission. The Secretary may, after consultation with the Interstate Conference of Employment Security Administrators, prescribe regulations requiring that additional information be submitted by such State with respect to the amount of such tax payable by such employer.'' (b) Clerical Amendment.--The table of sections for chapter 23 of such Code is amended by striking the item relating to section 3311 and inserting the following new items: ``Sec. 3311. State collection of tax. ``Sec. 3312. Short title.'' (c) Effective Date.--The amendments made by this section shall apply to taxable years beginning after December 31, 1999. SEC. 5. REQUIRED DISTRIBUTION OF STATE-SPECIFIC INFORMATION PACKETS. (a) In General.--Subsection (a) of section 3304 of the Internal Revenue Code of 1986 (relating to approval of State laws) is amended by striking ``and'' at the end of paragraph (18), by striking the period at the end of paragraph (19) and inserting ``; and'', and by adding at the end the following new paragraph: ``(20) the State will distribute to unemployed individuals State-specific information packets explaining unemployment insurance eligibility conditions.'' (b) Effective Date.--The amendment made by subsection (a) shall apply to certifications of States for 2000, except that section 3304(a)(20) of such Code, as added by subsection (a), shall not be a requirement for the State law of any State prior to July 1, 2001, if the legislature of such State does not meet in a regular session which closes during the calendar year 2000.", "label": 1, "domain": "government", "token_count": 347, "matched_pair_id": "conditionality_00853", "split": "train"}
{"id": "conditionality_train_pos_0350", "text": "Two of the dominant channels for galaxy mass assembly are cold flows (cold gas supplied via the filaments of the cosmic web) and mergers. How these processes combine in a cosmological setting, at both low and high redshift, to produce the whole zoo of galaxies we observe is largely unknown. Indeed there is still much to understand about the detailed physics of each process in isolation. While these formation channels have been studied using hydrodynamical simulations, here we study their impact on gas properties and star formation (SF) with some of the first simulations that capture the multiphase, cloudy nature of the interstellar medium (ISM), by virtue of their high spatial resolution (and corresponding low temperature threshold). In this regime, we examine the competition between cold flows and a supernovae(SNe)-driven outflow in a very high-redshift galaxy (z {\\approx} 9) and study the evolution of equal-mass galaxy mergers at low and high redshift, focusing on the induced SF. We find that SNe-driven outflows cannot reduce the cold accretion at z {\\approx} 9 and that SF is actually enhanced due to the ensuing metal enrichment. We demonstrate how several recent observational results on galaxy populations (e.g. enhanced HCN/CO ratios in ULIRGs, a separate Kennicutt Schmidt (KS) sequence for starbursts and the population of compact early type galaxies (ETGs) at high redshift) can be explained with mechanisms captured in galaxy merger simulations, provided that the multiphase nature of the ISM is resolved.", "label": 1, "domain": "academic", "token_count": 320, "matched_pair_id": "conditionality_00310", "split": "train"}
{"id": "conditionality_train_pos_0351", "text": "'' means an individual described in paragraph (2) of subsection (b) of the Policemen and Firemen's Retirement and Disability Act (sec. 5-703, D.C. Official Code), as added by subsection (a). SEC. 3. TREATMENT OF REEMPLOYED ANNUITANTS. Section 8468 of title 5, United States Code, is amended by adding at the end the following: ``(k)(1) For purposes of this section, the term `covered District of Columbia retiree' means an individual who is receiving benefits under the Policemen and Firemen's Retirement and Disability Act-- ``(A) based in whole or in part on such individual's service as an officer or member of the United States Secret Service Division or the United States Secret Service Uniformed Division; and ``(B) pursuant to an election, made under subsection (b)(2) of such Act (sec. 5-703, D.C. Official Code), to transfer to that retirement system from the retirement system under this chapter. ``(2) If a covered District of Columbia retiree becomes employed in an appointive or elective position (as referred to in subsection (a)), an amount equal to the retirement benefits which are payable under the Policemen and Firemen's Retirement and Disability Act and allocable to the period of actual employment shall be deducted from the pay of the reemployed retiree, to the same extent and in the same manner as if those retirement benefits were an annuity under this chapter. ``(3) The Director of the Office of Personnel Management shall prescribe any regulations necessary to carry out this subsection, including regulations under which an employing agency shall accept the certification of the appropriate official of the government of the District of Columbia regarding the amount of retirement benefits being paid to a covered District of Columbia retiree for a period during which such retiree is employed in the position described in paragraph (2).''. SEC. 4. PAYGO COMPLIANCE. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the House Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 485, "matched_pair_id": "conditionality_00905", "split": "train"}
{"id": "conditionality_train_pos_0352", "text": "We consider an isotropic Fermi liquid in two dimensions near the n=2 Pomeranchuk instability in the charge channel. The order parameter is a quadrupolar stress tensor with two polarizations, longitudinal and transverse to the quadrupolar momentum tensor. Longitudinal and transverse bosonic modes are characterized by dynamical exponents z_parallel=3 and z_perp=2, respectively. Previous studies have found that such a system exhibits multiscale quantum criticality with two different energy scales omega ~ xi^{-z_{parallel,perp}}, where xi is the correlation length. We study the impact of the multiple energy scales on the electron Green function. The interaction with the critical z_parallel =3 mode is known to give rise to a local self-energy that develops a non-Fermi liquid form, Sigma(omega) ~ omega^{2/3} for frequencies larger than the energy scale omega ~ xi^{-3}. We find that the exchange of transverse z_perp=2 fluctuations leads to a logarithmically singular renormalizations of the quasiparticle residue Z and the vertex Gamma. We derive and solve renormalization group equations for the flow of Z and Gamma and show that the system develops an anomalous dimension at the nematic quantum-critical point (QCP). As a result, the spectral function at a fixed omega and varying k has a non-Lorentzian form. Away from the QCP, we find that the flow of Z is cut at the energy scale omega_{FL} ~ xi^{-1}, associated with the z=1 dynamics of electrons. The z_perp=2 energy scale, omega ~ xi^{-2}, affects the flow of Z only if one includes into the theory self-interaction of transverse fluctuations.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00224", "split": "train"}
{"id": "conditionality_train_pos_0353", "text": ": ``(4) Availability of the medicare operated prescription drug plan.-- ``(A) In general.--A medicare operated prescription drug plan (as defined in section 1860D-11A(c)) shall be offered nationally in accordance with section 1860D- 11A. ``(B) Relationship to other plans.-- ``(i) In general.--Subject to clause (ii), a medicare operated prescription drug plan shall be offered in addition to any qualifying plan or fallback prescription drug plan offered in a PDP region and shall not be considered to be such a plan purposes of meeting the requirements of this subsection. ``(ii) Designation as a fallback plan.-- Notwithstanding any other provision of this part, the Secretary may designate the medicare operated prescription drug plan as the fallback prescription drug plan for any fallback service area (as defined in section 1860D-11(g)(3)) determined to be appropriate by the Secretary.''. (2) Section 1860D-13(c)(3) of such Act, as added by such section, is amended-- (A) in the heading, by inserting ``and medicare operated prescription drug plans'' after ``Fallback plans''; and (B) by inserting ``or a medicare operated prescription drug plan'' after ``a fallback prescription drug plan''. (3) Section 1860D-16(b)(1) of such Act, as added by such section, is amended-- (A) in subparagraph (C), by striking ``and'' after the semicolon at the end; (B) in subparagraph (D), by striking the period at the end and inserting ``; and''; and ``(E) payments for expenses incurred with respect to the operation of medicare operated prescription drug plans under section 1860D-11A.''. (4) Section 1860D-41(a) of such Act, as added by such section, is amended by adding at the end the following new paragraph: ``(19) Medicare operated prescription drug plan.--The term `medicare operated prescription drug plan' has the meaning given such term in section 1860D-11A(c).''. (c) Effective Date.--The amendments made by this section shall take effect as if included in the enactment of section 101 of the Medicare Prescription Drug, Improvement, and Modernization Act of 2003.", "label": 1, "domain": "government", "token_count": 478, "matched_pair_id": "conditionality_00966", "split": "train"}
{"id": "conditionality_train_pos_0354", "text": "Sgr A*, the massive black hole at the center of the Galaxy, varies in radio through X-ray emission on hourly time scales. The flare activity is thought to arise from the innermost region of an accretion flow onto Sgr A*. We present simultaneous light curves of Sgr A* in radio, sub-mm and X-rays that show a possible time delay of 110$\\pm17$ minutes between X-ray and 850 $\\mu$m suggesting that the sub-mm flare emission is optically thick. At radio wavelengths, we detect time lags of of $20.4\\pm6.8, 30\\pm12$ and 20$\\pm6$ minutes between the flare peaks observed at 13 and 7 mm (22 and 43 GHz) in three different epochs using the VLA. Linear polarization of 1$\\pm0.2$% and 0.7$\\pm0.1$% is detected at 7 and 13 mm, respectively, when averaged over the entire observation on 2006 July 17. A simple model of a bubble of synchrotron emitting electrons cooling via adiabatic expansion can explain the time delay between various wavelengths, the asymmetric shape of the light curves, and the observed polarization of the flare emission at 43 and 22 GHz. The derived physical quantities that characterize the emission give an expansion speed of v$_{exp} \\sim 0.003-0.1$c, magnetic field of B$\\sim$10-70 Gauss and particle spectral index p$\\sim$1-2. These parameters suggest that the associated plasma cannot escape from Sgr A* unless it has a large bulk motion.", "label": 1, "domain": "academic", "token_count": 344, "matched_pair_id": "conditionality_00038", "split": "train"}
{"id": "conditionality_train_pos_0355", "text": "We propose a simple model explaining two outstanding astrophysical problems related to compact objects: (1) that of stars such as G87-7 (alias EG 50) that constitute a class of relatively low-mass white dwarfs which nevertheless fall away from the C/O composition and (2) that of GRB 110328A/Swift J164449.3+57345 which showed spectacularly long-lived strong X-ray flaring, posing a challenge to standard GRB models. We argue that both these observations may have an explanation within the unified framework of a Quark-Nova occurring in a low-mass X-ray binary (neutron star- white dwarf). For LMXBs where the binary separation is sufficiently tight, ejecta from the exploding Neutron Star triggers nuclear burning in the white dwarf on impact, possibly leading to Fe-rich composition compact white dwarfs with mass 0.43M_sun < M_WD < 0.72M_sun, reminiscent of G87-7. Our results rely on the assumption, which ultimately needs to be tested by hydrodynamic and nucleosynthesis simulations, that under certain circumstances the WD can avoid the thermonuclear runaway. For heavier white dwarfs (i.e. M_WD > 0.72M_sun) experiencing the QN shock, degeneracy will not be lifted when Carbon burning begins, and a sub-Chandrasekhar Type Ia Supernovae may result in our model. Under slightly different conditions, and for pure He white dwarfs (i.e. M_WD < 0.43M_sun), the white dwarf is ablated and its ashes raining down on the Quark star leads to accretion-driven X-ray luminosity with energetics and duration reminiscent of GRB 110328A. We predict additional flaring activity towards the end of the accretion phase if the Quark star turns into a Black Hole.", "label": 1, "domain": "academic", "token_count": 392, "matched_pair_id": "conditionality_00330", "split": "train"}
{"id": "conditionality_train_pos_0356", "text": "If the research pans out, the world of mental health care may look very different in the coming decades. Psychedelic treatment won't be available for just anyone, and recreational psychedelic use may still be banned. But those with certain illnesses could seek treatment from a psychiatrist specially certified in psychedelic therapy. Just a few treatment sessions a year might be enough to provide lasting relief from their issues. People with mood disorders, including those who are unresponsive to conventional therapies, might be able to ditch their antidepressants and antianxiety medications. Those with terminal illness could enjoy their remaining days without the fear of death looming over them, while people with PTSD could return to a normal life unobstructed by paralyzing flashbacks. And rehab centers for substance use and eating disorders could empty out as more people turn to psychedelics. Again, we’re not at this point yet. But such is the promise of psychedelic medicine. SAFETY FIRST Psychedelic drugs fall into one of two categories depending on how they affect the brain. Classic psychedelics include LSD, psilocybin, and ayahuasca. They work by binding to the same receptors in the brain as serotonin, a neurotransmitter associated with feelings of wellbeing. MDMA, on the other hand, causes the release of another neurotransmitter, serotonin, in the brain. At this point, the star players in psychedelic research are psilocybin and MDMA. (LSD's hallucinogenic effects last too long, thus limiting its therapeutic value; ayahuasca is hard to standardize because it’s a brew made from two plants.) Given psychedelics’ potential for abuse — and the possibility of unpleasant hallucinations — clinical trials of the drugs follow rigid protocols. Patients for the clinical trials are screened for schizophrenia and related disorders that preclude psychedelic therapy; those who are selected undergo preliminary sessions during which they learn about the goals and nature of the treatment, as well as the particulars of the drug they’ll be trying. During treatment, patients typically don headphones for music and eyeshades and then lie down. They’re encouraged to go as \"deep\" as possible into the experience, says Charles Grob, a UCLA psychiatry professor who has done research on MDMA, psilocybin, and ayahuasca. As the session ends and the hallucinogenic effects wear off, patient and therapist discuss the experience. Follow-up psychotherapy sessions facilitate lasting results, Grob says. As experimental therapies, the sessions are conducted in", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00748", "split": "train"}
{"id": "conditionality_train_pos_0357", "text": "In multiprocessor systems, various problems are treated with Lamport's logical clock and the resultant logical time orders between operations. However, one often needs to face the high complexities caused by the lack of logical time order information in practice. In this paper, we utilize the \\emph{global clock} to infuse the so-called \\emph{pending period} to each operation in a multiprocessor system, where the pending period is a time interval that contains the performed time of the operation. Further, we define the \\emph{physical time order} for any two operations with disjoint pending periods. The physical time order is obeyed by any real execution in multiprocessor systems due to that it is part of the truly happened operation orders restricted by global clock, and it is then proven to be independent and consistent with traditional logical time orders. The above novel yet fundamental concepts enables new effective approaches for analyzing multiprocessor systems, which are named \\emph{pending period analysis} as a whole. As a consequence of pending period analysis, many important problems of multiprocessor systems can be tackled effectively. As a significant application example, complete memory consistency verification, which was known as an NP-hard problem, can be solved with the complexity of $O(n^2)$ (where $n$ is the number of operations). Moreover, the two event ordering problems, which were proven to be Co-NP-Hard and NP-hard respectively, can both be solved with the time complexity of O(n) if restricted by pending period information.", "label": 1, "domain": "academic", "token_count": 311, "matched_pair_id": "conditionality_00130", "split": "train"}
{"id": "conditionality_train_pos_0358", "text": "A local algorithm is a distributed algorithm where each node must operate solely based on the information that was available at system startup within a constant-size neighbourhood of the node. We study the applicability of local algorithms to max-min LPs where the objective is to maximise $\\min_k \\sum_v c_{kv} x_v$ subject to $\\sum_v a_{iv} x_v \\le 1$ for each $i$ and $x_v \\ge 0$ for each $v$. Here $c_{kv} \\ge 0$, $a_{iv} \\ge 0$, and the support sets $V_i = \\{v : a_{iv} > 0 \\}$, $V_k = \\{v : c_{kv}>0 \\}$, $I_v = \\{i : a_{iv} > 0 \\}$ and $K_v = \\{k : c_{kv} > 0 \\}$ have bounded size. In the distributed setting, each agent $v$ is responsible for choosing the value of $x_v$, and the communication network is a hypergraph $\\mathcal{H}$ where the sets $V_k$ and $V_i$ constitute the hyperedges. We present inapproximability results for a wide range of structural assumptions; for example, even if $|V_i|$ and $|V_k|$ are bounded by some constants larger than 2, there is no local approximation scheme. To contrast the negative results, we present a local approximation algorithm which achieves good approximation ratios if we can bound the relative growth of the vertex neighbourhoods in $\\mathcal{H}$.", "label": 1, "domain": "academic", "token_count": 335, "matched_pair_id": "conditionality_00024", "split": "train"}
{"id": "conditionality_train_pos_0359", "text": "committees of Congress a report on the operation of the Fund during the fiscal year. (2) Contents.--Each report shall include, for the fiscal year covered by the report, the following: (A) A statement of the amounts deposited into the Fund. (B) A description of the expenditures made from the Fund for the fiscal year, including the purpose of the expenditures. (C) Recommendations for additional authorities to fulfill the purpose of the Fund. (D) A statement of the balance remaining in the Fund at the end of the fiscal year. SEC. 8. EFFECTIVE DATES. (a) Prohibition on Research.--The prohibition under section (4)(a) shall take effect-- (1) on the date that is 3 years after the date of enactment of this Act for great apes assigned to an active protocol on the date of enactment of this Act; or (2) on the date of enactment of this Act for great apes not assigned to an active protocol on that date. (b) Prohibition on Housing and Funding.--The prohibitions under subsections (b) and (c) of section 4 shall take effect on the date that is 3 years after the date of enactment of this Act. (c) Other Requirements.--Any provision of this Act for which a specific effective date is not provided shall take effect on the date of enactment of this Act. SEC. 9. SEVERABILITY. In the event that any provision of this Act shall, for any reason, be held to be invalid or unenforceable in any respect, such invalidity or unenforceability shall not affect any other provision of this Act, and this Act shall be construed as if the invalid or unenforceable provision had never been included in this Act.", "label": 1, "domain": "government", "token_count": 364, "matched_pair_id": "conditionality_00862", "split": "train"}
{"id": "conditionality_train_pos_0360", "text": "require serious examination of how land reform was conducted and redistributing the land on an impartial basis right from scratch, and without favour and fear of powerful individuals or connected families. Letting go of Gushungo could include setting an uncompromising precedent in how government prosecutors deal with allegations of corruption and allegations of violence and human rights abuses in the highest echelons of power. If South Africa can charge former president Jacob Zuma over allegations of corruption, money laundering and racketeering, Zimbabwe can follow suit and arraign Gushungo – and his longtime lieutenants – if need be, and consequently, asphyxiate the blood-stained, ubiquitous storms of betrayal that have rained down on us for years. As Nyakinua states in Petals of Blood, before angry and dejected villagers decide to challenge corrupt authorities in Nairobi, “I think we should go. It is our turn to make things happen. There was a time when things happened the way we in Ilmorog wanted them to happen. We had power over the movement of our limbs. We made up our own words and sang them and we danced to them. But there came a time when this power was taken from us…. We must surround the city and demand back our share”. Likewise, we, the people, must wrestle control of our future and dance to our own democratic and economically viable song. Because, as things stand, who can prevent an exasperated clique of ZNA generals from targeting and removing the criminals around President Emmerson Mnangagwa à la Gushungo, and circumventing democracy, if need be, once again?", "label": 1, "domain": "news", "token_count": 332, "matched_pair_id": "conditionality_00617", "split": "train"}
{"id": "conditionality_train_pos_0361", "text": "Aims. The main purpose of this paper is to study time delays between the light variations in different wavebands for a sample of quasars. Measuring a reliable time delay for a large number of quasars may help constraint the models of their central engines. The standard accretion disk irradiation model predicts a delay of the longer wavelengths behind the shorter ones, a delay that depends on the fundamental quasar parameters. Since the black hole masses and the accretion rates are approximately known for the sample we use, one can compare the observed time delays with the expected ones. Methods. We applied the interpolation cross-correlation function (ICCF) method to the Giveon et al. sample of 42 quasars, monitored in two (B and R) colors, to find the time lags represented by the ICCF peaks. Different tests were performed to assess the influence of photometric errors, sampling, etc., on the final result. Results. We found that most of the objects show a delay in the red light curve behind the blue one (a positive lag), which on average for the sample is about +4 days (+3 for the median), although the scatter is significant. These results are broadly consistent with the reprocessing model, especially for the well-sampled objects. The normalized time-lag deviations do not seem to correlate significantly with other quasar properties, including optical, radio, or X-ray measurables. On the other hand, many objects show a clear negative lag, which, if real, may have important consequences for the variability models.", "label": 1, "domain": "academic", "token_count": 318, "matched_pair_id": "conditionality_00102", "split": "train"}
{"id": "conditionality_train_pos_0362", "text": "X-ray pulsations with a 6.85 s period were recently detected in the SMC and were subsequently identified as originating from the Be/X-ray binary system XTE J0103-728. The recent localization of the source of the X-ray emission has made a targeted search for radio pulsations from this source possible. The detection of pulsed radio emission from XTE J0103-728 would make it only the second system after PSR B1259-63 that is both a Be/X-ray binary and a radio pulsar. We observed XTE J0103-728 in Feb 2008 with the Parkes 64-m radio telescope soon after the identification of the source of X-ray pulsations was reported in order to search for corresponding radio pulsations. We used a continuous 6.4 hour observation with a 256 MHz bandwidth centered at 1390 MHz using the center beam of the Parkes multibeam receiver. In the subsequent data analysis, which included a folding search, a Fourier search, a fast-folding algorithm search, and a single-pulse search, no pulsed signals were found for trial dispersion measures (DMs) between 0 and 800 pc cm^-3. This DM range easily encompasses the expected values for sources in the SMC. We place an upper limit of ~45 mJy kpc^2 on the luminosity of periodic radio emission from XTE J0103-728 at the epoch of our observation, and we compare this limit to a range of luminosities measured for PSR B1259-63, the only Be/X-ray binary currently known to emit radio pulses. We also compare our limit to the radio luminosities of neutron stars having similarly long spin periods to XTE J0103-728. Since the radio pulses from PSR B1259-63 are eclipsed and undetectable during the portion of the orbit near periastron, repeated additional radio search observations of XTE J0103-728 may be valuable if it is undergoing similar eclipsing and if such observations are able to sample the orbital phase of this system well.", "label": 1, "domain": "academic", "token_count": 432, "matched_pair_id": "conditionality_00118", "split": "train"}
{"id": "conditionality_train_pos_0363", "text": "BUENA VISTA, Fla. (AP) — Fittingly, Jack Morris reached the Hall of Fame in extra innings. Morris was elected to the Hall by its Modern Era committee on Sunday along with former Detroit Tigers teammate Alan Trammell, completing a joint journey from Motown to Cooperstown. The big-game pitcher and star shortstop were picked by 16 voters who considered 10 candidates whose biggest contributions came from 1970-87. Morris got 14 votes and Trammell drew 13, one more than the minimum needed. They will be enshrined on July 29, and fitting they’ll go in together. They both began their big league careers in 1977 with Detroit and played 13 seasons alongside each other with the Tigers. “The time that I’ve spent wondering if this day would ever come seems to be vanished and erased right now because it did come, and it’s amazing,” the 62-year-old Morris said during a conference call. —— Teams can lock up as many as 5 playoff berths in Week 14 As many as five playoff berths can be locked up Sunday, and New England can clinch before taking the field Monday night. A Buffalo loss or tie against the Colts on Sunday clinches the AFC East for the Patriots, while New England can clinch Monday night by beating Miami if the Bills win. Pittsburgh clinches a berth with a Buffalo loss or tie, though the Steelers need to tie or beat Baltimore to win the AFC North. Philadelphia could clinch the NFC East if Dallas ties or loses to the Giants before the Eagles take the field in Los Angeles. Minnesota can win the NFC North by beating Carolina or if Detroit and Green Bay both tie.", "label": 1, "domain": "news", "token_count": 348, "matched_pair_id": "conditionality_00655", "split": "train"}
{"id": "conditionality_train_pos_0364", "text": "current Administration has granted discretionary compliance waivers from Obamacare to a variety of for-profit businesses, unions, and other organizations. (19) To date, the Department of Health and Human Services has granted more than 1,000 individual waiver requests for employers and insurers, excusing the employers and insurers from compliance with various aspects of the law. SEC. 3. SENSE OF THE SENATE. It is the sense of the Senate that the Food and Drug Administration should study whether contraceptives that are available with a prescription, on the date of enactment of this Act, would be safe and effective for adults if available without a prescription. SEC. 4. EMPLOYEE PROTECTION. Notwithstanding any other provision of law, an employer who is engaged in interstate commerce may not prohibit an employee from purchasing, pursuant to State prescribing and dispensing laws, a drug or medical device, including a contraceptive, that is regulated by the Food and Drug Administration. SEC. 5. EMPOWERING EMPLOYEES TO MAKE HEALTH CHOICES. (a) No Limitations Based on Whether a Drug Is Prescribed.--Section 9003 of the Patient Protection and Affordable Care Act (Public Law 111- 148), and the amendments made by such section, are repealed, and the Internal Revenue Code of 1986 shall be applied as if such section, and amendments, had never been enacted. (b) No Limitations on Health FSAs.--Sections 9005 and 10902 of the Patient Protection and Affordable Care Act (Public Law 111-148) and section 1403 of the Health Care and Education Reconciliation Act of 2010 (Public Law 111-152), and the amendments made by such sections, are repealed, and the Internal Revenue Code of 1986 shall be applied as if such section, and amendments, had never been enacted.", "label": 1, "domain": "government", "token_count": 377, "matched_pair_id": "conditionality_01005", "split": "train"}
{"id": "conditionality_train_pos_0365", "text": "This work aims to provide a first insight into the mass-metallicity (MZ) relation of star-forming galaxies at redshift z~1.4. To reach this goal, we present a first set of nine VVDS galaxies observed with the NIR integral-field spectrograph SINFONI on the VLT. Oxygen abundances are derived from empirical indicators based on the ratio between strong nebular emission-lines (Halpha, [NII]6584 and [SII]6717,6731). Stellar masses are deduced from SED fitting with Charlot & Bruzual (2007) population synthesis models, and star formation rates are derived from [OII]3727 and Halpha emission-line luminosities. We find a typical shift of 0.2-0.4 dex towards lower metallicities for the z~1.4 galaxies, compared to the MZ-relation in the local universe as derived from SDSS data. However, this small sample of eight galaxies does not show any clear correlation between stellar mass and metallicity, unlike other larger samples at different redshift (z~0, z~0.7, and z~2). Indeed, our galaxies lie just under the relation at z~2 and show a small trend for more massive galaxies to be more metallic (~0.1 logarithmic slope). There are two possible explanations to account for these observations. First, the most massive galaxies present higher specific star formation rates when compared to the global VVDS sample which could explain the particularly low metallicity of these galaxies as already shown in the SDSS sample. Second, inflow of metal-poor gas due to tidal interactions could also explain the low metallicity of these galaxies as two of these three galaxies show clear signatures of merging in their velocity fields. Finally, we find that the metallicity of 4 galaxies is lower by ~0.2 to 0.4 dex if we take into account the N/O abundance ratio in their metallicity estimate.", "label": 1, "domain": "academic", "token_count": 406, "matched_pair_id": "conditionality_00124", "split": "train"}
{"id": "conditionality_train_pos_0366", "text": "The single-degenerate channel for the progenitors of type Ia supernovae (SNe Ia) are currently accepted, in which a carbon-oxygen white dwarf (CO WD) accretes hydrogen-rich material from its companion, increases its mass to the Chandrasekhar mass limit, and then explodes as a SN Ia. Incorporating the prescription of \\citet{HAC99a} for the accretion efficiency into Eggleton's stellar evolution code and assuming that the prescription is valid for \\emph{all} metallicities, we performed binary stellar evolution calculations for more than 25,000 close WD binaries with metallicities $Z=0.06, 0.05, 0.04, 0.03, 0.02, 0.01, 0.004, 0.001, 0.0003$ and 0.0001. For our calculations, the companions are assumed to be unevolved or slightly evolved stars (WD + MS). As a result, the initial parameter spaces for SNe Ia at various $Z$ are presented in orbital period-secondary mass ($\\log P_{\\rm i}, M_{\\rm 2}^{\\rm i}$) planes. Our study shows that both the initial mass of the secondary and the initial orbital period increase with metallicity. Thus, the minimum mass of the CO WD for SNe Ia decreases with metallicity $Z$. The difference of the minimum mass may be as large as 0.24 $M_{\\odot}$ for different Z. Adopting the results above, we studied the birth rate of SNe Ia for various $Z$ via a binary population synthesis approach. If a single starburst is assumed, SNe Ia occur systemically earlier and the peak value of the birth rate is larger for a high $Z$. The Galactic birth rate from the WD + MS channel is lower than (but comparable to) that inferred from observations. Our study indicates that supernovae like SN2002ic would not occur in extremely low-metallicity environments, if the delayed dynamical-instability model in \\citet{HAN06} is appropriate.", "label": 1, "domain": "academic", "token_count": 452, "matched_pair_id": "conditionality_00048", "split": "train"}
{"id": "conditionality_train_pos_0367", "text": "Semiclassical spin-coherent kinetic equations can be derived from quantum theory with many different approaches (Liouville equation based approaches, nonequilibrium Green's functions techniques, etc.). The collision integrals turn out to be formally different, but coincide in textbook examples as well as for systems where the spin-orbit coupling is only a small part of the kinetic energy like in related studies on the spin Hall effect. In Dirac cone physics (graphene, surface states of topological insulators like Bi_{1-x}Sb_x, Bi_2Te_3 etc.), where this coupling constitutes the entire kinetic energy, the difference manifests itself in the precise value of the electron-hole coherence originated quantum correction to the Drude conductivity $\\sim e^2/h * \\ell k_F$. The leading correction is derived analytically for single and multilayer graphene with general scalar impurities. The often neglected principal value terms in the collision integral are important. Neglecting them yields a leading correction of order $(\\ell k_F)^{-1}$, whereas including them can give a correction of order $(\\ell k_F)^0$. The latter opens up a counterintuitive scenario with finite electron-hole coherent effects at Fermi energies arbitrarily far above the neutrality point regime, for example in the form of a shift $\\sim e^2/h$ that only depends on the dielectric constant. This residual conductivity, possibly related to the one observed in recent experiments, depends crucially on the approach and could offer a setting for experimentally singling out one of the candidates. Concerning the different formalisms we notice that the discrepancy between a density matrix approach and a Green's function approach is removed if the Generalized Kadanoff-Baym Ansatz in the latter is replaced by an anti-ordered version.", "label": 1, "domain": "academic", "token_count": 365, "matched_pair_id": "conditionality_00179", "split": "train"}
{"id": "conditionality_train_pos_0368", "text": "A small number of young stellar objects show signs of a halo-like structure of optically thin dust. This halo or torus is located within a few AU of the star, but its origin has not yet been understood. A dynamically excited cloud of planetesimals colliding to eventually form dust could produce such a structure. The cause of the dynamical excitation could be one or more planets. This work investigates an inwardly migrating planet that is dynamically scattering planetesimals as a possible cause for the observed structures. If this mechanism is responsible, the observed halo-like structure could be used to infer the existence of planets in these systems. We present analytical estimates on the maximum inclination reached owing to dynamical interactions between planetesimals and a migrating planet. A symplectic integrator is used to simulate the effect of a migrating planet on a population of planetesimals. It is found that an inwardly migrating planet is only able to scatter the material it encounters to highly-inclined orbits if the material is on an eccentric orbit. Such eccentric orbits can be the result of resonance trapping and eccentricity pumping. Simulations show that for a certain range of migration rates and planet masses, resonance capture combined with planetary migration indeed causes the planetesimals to reach eccentric orbits and subsequently get scattered to highly-inclined orbits. The size distribution of the resulting dust is calculated determined to find the total mass and optical depth, which are found to compare reasonably well with the observed structures. Dynamical scattering of planetesimals caused by a planet migrating in, followed by the grinding down of these planetesimals to dust grains, appears to be a promising explanation for the inferred circumstellar dust clouds. Further study is needed to see if the haloes can be used to infer the presence of planets.", "label": 1, "domain": "academic", "token_count": 357, "matched_pair_id": "conditionality_00335", "split": "train"}
{"id": "conditionality_train_pos_0369", "text": "The dust size distribution in molecular clouds can be strongly affected by ice-mantle formation and (subsequent) grain coagulation. Following previous work where the dust size distribution has been calculated from a state-of-the art collision model for dust aggregates that involves both coagulation and fragmentation (Paper I), the corresponding opacities are presented in this study. The opacities are calculated by applying the effective medium theory assuming that the dust aggregates are a mix of 0.1{\\mu}m silicate and graphite grains and vacuum. In particular, we explore how the coagulation affects the near-IR opacities and the opacity in the 9.7{\\mu}m silicate feature. We find that as dust aggregates grow to {\\mu}m-sizes both the near-IR color excess and the opacity in the 9.7 {\\mu}m feature increases. Despite their coagulation, porous aggregates help to prolong the presence of the 9.7{\\mu}m feature. We find that the ratio between the opacity in the silicate feature and the near-IR color excess becomes lower with respect to the ISM, in accordance with many observations of dark clouds. However, this trend is primarily a result of ice mantle formation and the mixed material composition of the aggregates, rather than being driven by coagulation. With stronger growth, when most of the dust mass resides in particles of size 10{\\mu}m or larger, both the near-IR color excess and the 9.7{\\mu}m silicate feature significantly diminish. Observations at additional wavelengths, in particular in the sub-mm range, are essential to provide quantitative constraints on the dust size distribution within dense cores. Our results indicate that the sub-mm index {\\beta} will increase appreciably, if aggregates grow to ~100{\\mu}m in size.", "label": 1, "domain": "academic", "token_count": 380, "matched_pair_id": "conditionality_00343", "split": "train"}
{"id": "conditionality_train_pos_0370", "text": "ig, who in 1976, on national TV, announced that he’d make the West Indies grovel. Imagine the outrage if the England captain said that today. The ECB’s corporate benefactors would be queuing up to sponsor tennis. And now an England cricketer gets filmed fighting in the streets and the footage ends up in the national newspapers. Even if the ECB wanted to be lenient to England’s star player, there’s no way the corporates are going to have that sort of thing associated with their brand. Stokes has nothing to complain about, whoever started the fight, and for whatever reasons. He is an England cricketer, well aware of the standards of behaviour his employers expect, of what is likely to happen to transgressors. He was also happy, no doubt, to pick up the sort of salary that wouldn’t be possible if ECB didn’t dip into the corporate wallet. Before Packer, in the days before smartphones with cameras, players could get away with the odd boozed-up barny. Ian Chappell got into a bar room fight with a young Ian Botham before the 1977 Centenary Test. A few months later, Botham was making his Test debut and Chappell captaining Kerry Packer’s WSC Australian team. Christmas 1980 and Botham, allegedly, got involved in a brawl in a Scunthorpe nightclub. But whilst the bow-ties at Lord’s might have raised a disapproving pink gin or three; Botham was still England captain when the team set out for the West Indies a few months later. Back then, though, there were no corporate bigwigs casting judgements about the type of chap they wanted associated with their brand. It’s not all bad change for Stokes. Suspended on full pay since the incident, he has probably earned more in the last few weeks than he would have, in an entire career, if he’d had played during those more lenient, pre-Packer days.", "label": 1, "domain": "news", "token_count": 408, "matched_pair_id": "conditionality_00516", "split": "train"}
{"id": "conditionality_train_pos_0371", "text": "If a sequence of Riemannian manifolds, $X_i$, converges in the pointed Gromov-Hausdorff sense to a limit space, $X_\\infty$, and if $E_i$ are vector bundles over $X_i$ endowed with metrics of Sasaki-type with a uniform upper bound on rank, then a subsequence of the $E_i$ converges in the pointed Gromov-Hausdorff sense to a metric space, $E_\\infty$. The projection maps $\\pi_i$ converge to a limit submetry $\\pi_\\infty$ and the fibers converge to its fibers; the latter may no longer be vector spaces but are homeomorphic to $\\R^k/G$, where $G$ is a closed subgroup of $O(k)$ ---called the {\\em wane group}--- that depends on the basepoint and that is defined using the holonomy groups on the vector bundles. The norms $\\mu_i=\\|\\cdot\\|_i$ converges to a map $\\mu_{\\infty}$ compatible with the re-scaling in $\\R^k/G$ and the $\\R$-action on $E_i$ converges to an $\\R-$action on $E_{\\infty}$ compatible with the limiting norm. In the special case when the sequence of vector bundles has a uniform lower bound on holonomy radius (as in a sequence of collapsing flat tori to a circle), the limit fibers are vector spaces. Under the opposite extreme, e.g. when a single compact $n$-dimensional manifold is re-scaled to a point, the limit fiber is $\\R^n/H$ where $H$ is the closure of the holonomy group of the compact manifold considered. An appropriate notion of parallelism is given to the limiting spaces by considering curves whose length is unchanged under the projection. The class of such curves is invariant under the $\\R$-action and each such curve preserves norms. The existence of parallel translation along rectifiable curves with arbitrary initial conditions is also exhibited. Uniqueness is not true in general, but a necessary condition is given in terms of the aforementioned wane groups $G$.", "label": 1, "domain": "academic", "token_count": 447, "matched_pair_id": "conditionality_00277", "split": "train"}
{"id": "conditionality_train_pos_0372", "text": "Two types of pseudoscalar quarkonium electromagnetic decay processes, i.e. decay to a lepton pair, and to a lepton pair plus a photon (Dalitz decay), are analyzed at the leading order in NRQCD expansion. The former type of processes, highly suppressed in the Standard Model, have been hoped to act as the sensitive probes of the possible new physics. The latter type of processes generally possess much greater decay rates than the former, owing to several conspiring factors. The recently launched BES-III program, with $10^8$ $\\eta_c$ samples to be anticipated in the coming years, may be able to observe the Dalitz decays $\\eta_c\\to e^+e^-\\gamma$ and $\\eta_c\\to \\mu^+\\mu^-\\gamma$, which have branching ratios of order $10^{-6}$. When the radiated photon becomes very soft, the Dalitz decay events will be experimentally tagged as the exclusive lepton pair events. It is found that, those quasi-two-body events that arise from $\\eta_c\\to e^+ e^-\\gamma$ with photon energy less than the minimum sensitivity of the electromagnetic calorimeter, can vastly outnumber the literal $\\eta_c\\to e^+ e^-$ events, however this amplification is still not dramatic enough for the BES-III experiment to establish these events. Consequently, the expectation of looking for new physics signature in the $\\eta_c\\to l^+l^-$ channel is obscured, unless the contamination from $\\eta_c \\to l^+l^-\\gamma$ has been taken into account carefully.", "label": 1, "domain": "academic", "token_count": 334, "matched_pair_id": "conditionality_00151", "split": "train"}
{"id": "conditionality_train_pos_0373", "text": "The intriguing observations of Swift/BAT X-ray flash XRF 060218 and the BATSE-BeppoSAX gamma-ray burst GRB 980425, both with much lower luminosity and redshift compared to other observed bursts, naturally lead to the question of how these low-luminosity (LL) bursts are related to high-luminosity (HL) bursts. Incorporating the constraints from both the flux-limited samples observed with CGRO/BATSE and Swift/BAT and the redshift-known GRB sample, we investigate the luminosity function for both LL- and HL-GRBs through simulations. Our multiple criteria, including the log N - log P distributions from the flux-limited GRB sample, the redshift and luminosity distributions of the redshift-known sample, and the detection ratio of HL- and LL- GRBs with Swift/BAT, provide a set of stringent constraints to the luminosity function. Assuming that the GRB rate follows the star formation rate, our simulations show that a simple power law or a broken power law model of luminosity function fail to reproduce the observations, and a new component is required. This component can be modeled with a broken power, which is characterized by a sharp increase of the burst number at around L < 10^47 erg s^-1}. The lack of detection of moderate-luminosity GRBs at redshift ~0.3 indicates that this feature is not due to observational biases. The inferred local rate, rho_0, of LL-GRBs from our model is ~ 200 Gpc^-3 yr^-1 at ~ 10^47 erg s^-1, much larger than that of HL-GRBs. These results imply that LL-GRBs could be a separate GRB population from HL-GRBs. The recent discovery of a local X-ray transient 080109/SN 2008D would strengthen our conclusion, if the observed non-thermal emission has a similar origin as the prompt emission of most GRBs and XRFs.", "label": 1, "domain": "academic", "token_count": 412, "matched_pair_id": "conditionality_00044", "split": "train"}
{"id": "conditionality_train_pos_0374", "text": "$500, but you can find front-loaders with over 4 cubic inches of capacity and some great features for between $600 and $700. High-efficiency top-loaders tend to be more expensive than old-school agitator models and can cost more than some front-loaders, depending on capacity and extras. However, excluding major sales, it’s hard to find a front-loader for under $600. Top-loaders look mighty tempting when you can find them on sale for under $400. The verdict If you still want a top-loader, you’re not alone. “There has been a continuing shift from top-load to front-load and the front-load market has been growing at a faster rate than top load,” Hale said. “However, the industry is still around 75 percent top-load versus 25 percent front-load. Innovation-wise, both platforms have been progressing, and both have had to change with the constantly increasing energy standards, but those changes have impacted top load more.” Some manufacturers are more outspoken about it than others, but the consensus from several we’ve spoken to is that front-loaders win in cleaning power and efficiency, especially when it comes to water use. The Energy Star program’s findings bear this out as well. The American Cleaning Institute (ACI) has found that most people unhappy with their front-loaders’ performance are actually misusing HE laundry detergent. When it comes to front-loaders, there can be some new quirks if you’ve used top-loaders your whole life, including learning to dial back the detergent. But if top-loaders fit your appliance-buying budget, they definitely have some major advantages over their water-loving counterparts.", "label": 1, "domain": "news", "token_count": 337, "matched_pair_id": "conditionality_00725", "split": "train"}
{"id": "conditionality_train_pos_0375", "text": "Let $\\ket{\\0}$ and $\\ket{\\1}$ be two states that are promised to come from known subsets of orthogonal subspaces, but are otherwise unknown. Our paper probes the question of what can be achieved with respect to the basis $\\{\\ket{\\0},\\ket{\\1}}^{\\otimes n}$ of $n$ logical qubits, given only a few copies of the unknown states $\\ket{\\0}$ and $\\ket{\\1}$. A phase-invariant operator is one that is unchanged under the relative phase-shift $\\ket{\\1} \\mapsto e^{i \\theta}\\ket{\\1}$, for any $\\theta$, of all of the $n$ qubits. We show that phase-invariant unitary operators can be implemented exactly with no copies and that phase-invariant states can be prepared exactly with at most $n$ copies each of $\\ket{\\0}$ and $\\ket{\\1}$; we give an explicit algorithm for state preparation that is efficient for some classes of states (e.g. symmetric states). We conjecture that certain non-phase-invariant operations are impossible to perform accurately without many copies. Motivated by optical implementations of quantum computers, we define ``quantum computation in a hidden basis'' to mean executing a quantum algorithm with respect to the phase-shifted hidden basis $\\{\\ket{\\0}, e^{i\\theta}\\ket{\\1}\\}$, for some potentially unknown $\\theta$; we give an efficient approximation algorithm for this task, for which we introduce an analogue of a coherent state of light, which serves as a bounded quantum phase reference frame encoding $\\theta$. Our motivation was quantum-public-key cryptography, however the techniques are general. We apply our results to quantum-public-key authentication protocols, by showing that a natural class of digital signature schemes for classical messages is insecure. We also give a protocol for identification that uses many of the ideas discussed and whose security relates to our conjecture (but we do not know if it is secure).", "label": 1, "domain": "academic", "token_count": 403, "matched_pair_id": "conditionality_00087", "split": "train"}
{"id": "conditionality_train_pos_0376", "text": "of bed her two days I just sat there reading them and trying to figure out a way. To make sure other people could read them too because they were all being. Sent to me again so I just I think they did anybody else seen all of the is so I really am retreated a lot of them. I like a lot of them and then had people look through my name my likes. And thankfully you know the New York Times picked it up. When you know on these news shows to discuss it so it did become a bigger conversation. But it was really hard I mean I went out for dinner two days after. Post in the first week. And my friends were and a really good mood you know sort of bummed out in the early let's go this is a really positive thing that you didn't think about bucket with scroll through. My Twitter feed at every time I would update at. Every second that we're still like five new stories and news stories company news stories Ford stars it was just constantly. Women sharing yeah come which was very overwhelming. It brings me to the sort of the larger question here which is you have this amazing voice. Right and you have this incredible platform yen and if there's some sort of like mission. Behind what it is he'd like to accomplish its eighty solely evolving yeah. Ole I think I'm just gonna keep doing what I'm doing now and if anything pops up today. Feel. I should contribute to you or I want to start and I well. Policy against every day's a new day on Twitter thing. NI LA Vista. Yet. Do you obviously you're cute on Twitter how do you pick that your gonna follow. Well now I am. It's mostly. New friends or. Friends and friends. Do you have favorites yet people like you can become so many people's favorite don't have any you know it looked like I have to Packers today. Having favorite I have. But this scene at the core group of people that I follow. All tweet every single day solely on a get my fill of basically like every and it's just like Twitter group more than one person that I speak. Do you follow art art Tweeter in chief. Our president. No I did until he became president and that way. Yes of course that is bold move of course an idea of course that you quit taking the Twitter questions earlier at a bunch for so coming and you would take worried. Degree in line for if you actually seizing that app.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00534", "split": "train"}
{"id": "conditionality_train_pos_0377", "text": "News analysis WHITE SULPHUR SPRINGS, W.Va. — No one knows how to run against House Minority Leader Nancy Pelosi better than Rep. Steve Stivers, R-Ohio. In 2010, he made her the central figure in his campaign to win a rematch against Mary Jo Kilroy, the Democratic incumbent who had defeated him by little more than 2,000 votes in 2008. \"Her record mirrors Pelosi's,\" Stivers said back then. \"Really, my focus is going to be on Pelosi and Kilroy.\" Across the country that year, anti-Pelosi ads were a fixture in Republican campaigns, and Stivers, who ended up winning Round 2 by a whopping 13 percentage points, became part of a freshman class that delivered the House back into GOP hands after Pelosi's four-year run as speaker. Play Facebook Twitter Embed Pence: Trump and I will stand with GOP in 2018 0:46 autoplay autoplay Copy this code to your website or blog Now, as chairman of the National Republican Congressional Committee, Stivers is charged with fending off a Democratic wave and keeping the GOP's House majority in this year's midterm elections. And he's dusting off the old playbook. \"Nancy Pelosi has stayed in the spotlight,\" Stivers explained said this week as he outlined the GOP's fall campaign plan at a news conference on the sidelines of a congressional Republican retreat here. The question is whether Pelosi is as toxic now, with Republicans in control of the White House and Congress, as she was then. Republicans are certain that she is. On Wednesday night, Vice President Mike Pence told Republicans here that Pelosi is “out of touch with the American people” because she described corporate bonuses of $1,000 as \"crumbs\" compared to the benefits the wealthy will receive under President Donald Trump's signature tax cut. The next day, in front of the same audience of House and Senate Republicans, Trump likened the remark to Hillary Clinton's formulation that half of Trump's 2016 campaign supporters were \"deplorables.\" Some Democrats fear that the prospect of Pelosi taking the speaker's gavel from Rep. Paul Ryan, R-Wis., will hurt their party's chances in swing districts. Her approval ratings have hovered just below 30 percent. And Conor Lamb, the Democratic candidate running for the House in a western Pennsylvania special election next month, has said he would not vote for Pelosi to lead the party if he's elected.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00742", "split": "train"}
{"id": "conditionality_train_pos_0378", "text": "At classical level, dynamical derivation of the properties and conservation laws for topologically non-trivial systems from Noether theorem versus the derivation of the system's properties on topological grounds are considered as distinct. We do celebrate any agreements in results derived from these two distinct approaches: i.e. the dynamical versus the topological approach. Here we consider the Corrigan-Olive-Fairlie-Nuyts solution based on which we study the stability of the 't Hooft- Polyakov outer field, known as its Higgs vacuum, and derive its stability, dynamically, from the equations of motion rather than from the familiar topological approach. Then we use our derived result of the preservation of the Higgs vacuum asymptotically to derive the stability of the 't Hooft-Polyakov monopole, even if inner core is perturbed, where we base that on observing that the magnetic charge must be conserved if the Higgs vacuum is preserved asymptotically. We also, alternatively, note stability of 't Hooft-Polyakov monopole and the conservation of its magnetic charge by again using the result of the Higgs vacuum asymptotic preservation to use Eq.(5) to show that no non-Abelian radiation allowed out of the core as long as the Higgs vacuum is preserved and restored, by the equations of motion, if perturbed. We start by deriving the asymptotic equations of motion that are valid for the monopole's field outside its core; next we derive certain constraints from the asymptotic equations of motion of the Corrigan-Olive-Fairlie-Nuyts solution to the 't Hooft-Polyakov monopole using the Lagrangian formalism of singular theories, in particular that of Gitman and Tyutin. The derived constraints will show clearly the stability of the monopole's Higgs vacuum its restoration by the equations of motion of the Higgs vacuum, if disturbed.", "label": 1, "domain": "academic", "token_count": 397, "matched_pair_id": "conditionality_00470", "split": "train"}
{"id": "conditionality_train_pos_0379", "text": "If latest speculations and media reports are to be believed, Brahmastra co-stars Ranbir Kapoor and Alia Bhatt are having a secret affair. The news of the two dating has taken the internet by storm as Ranbir and Alia have been spending a lot of quality time with each other these days. Bollywood heartthrob Ranbir Kapoor and diva Alia Bhatt, who will be seen together in Ayan Mukerji’s Brahmastra, are said to be in a secret relationship, according to latest media reports. The two have been allegedly spending a lot of quality time together even after the shooting is over. While Ranbir was rumoured to be dating Pakistani beauty Mahira Khan, it was known to all that Alia Bhatt was dating her Student of The Year co-star Sidharth Malhotra. However, if we go by the speculations, Ranbir and Alia have found love in each other. Earlier this year Ranbir and Alia were spotted chilling together. Their pictures from their outing made its way on social media thanks to their fan pages. The duo also attended the Padmaavat screening together last week. Not to forget Alia and Ranbir have been spotted together on numerous occasions in recent times. In fact, now latest reports are that that Alia and Ranbir have started meeting secretly at each other places. For the unknown, Ranbir dropped by Alia’s house on Wednesday night at around 11 pm and left only next morning at around 7 am. It will be for the first time that Ranbir and Alia would be seen sharing the screen space on the silver screen. The Dharma Productions’ film is Ayan’s third project, which comes four years after his successful romantic-comedy Yeh Jawaani Hai Deewani. The young filmmaker said he has all his hopes pinned on Brahmastra, which was announced in 2016. Besides Ranbir and Alia, megastar Amitabh Bachchan will also feature in the film and Ayan admitted that the veteran was in his mind since he conceptualised the project years ago.", "label": 1, "domain": "news", "token_count": 429, "matched_pair_id": "conditionality_00594", "split": "train"}
{"id": "conditionality_train_pos_0380", "text": "Defined as X-ray bright galaxy groups with large differences between the luminosities of their brightest and second brightest galaxies, \"fossil groups\" are believed to be some of the oldest galaxy systems in the universe. They have therefore been the subject of much recent research. In this work we present a study of 10 fossil group candidates with an average of 33 spectroscopically confirmed members per group, making this the deepest study of its type to-date. We also use this data to perform an analysis of the luminosity function of our sample of fossil groups. We confirm the high masses previously reported for many of fossil systems, finding values more similar to those of clusters than of groups. We also confirm the high dynamical mass-to-light ratios reported in many previous studies. While our results are consistent with previous studies in many ways, our interpretation is not. This is because we show that, while the luminosities of the BCGs in these systems are consistent with their high dynamical masses, their richnesses (total number of galaxies above some canonical value) are extremely low. This leads us to suggest a new interpretation of fossil systems in which the large differences between the luminosities of their brightest and second brightest galaxies are simply the result the high BCG luminosities and low richnesses, while the high masses and low richnesses also explain the high mass-to-light ratios. Our results therefore suggest that fossil systems can be characterised as cluster-like in their masses and BCG luminosities, but possessing the richnesses and optical luminosities of relatively poor groups. These findings are not predicted by any of the current models for the formation of fossil groups. Therefore, if this picture is confirmed, current ideas about the formation and evolution of fossil systems will need to be reformulated.", "label": 1, "domain": "academic", "token_count": 361, "matched_pair_id": "conditionality_00366", "split": "train"}
{"id": "conditionality_train_pos_0381", "text": "If an NFL team is high on a prospect, you can expect them to send a high-ranking official to that player's Pro Day. Bill Belichick sent himself to N.C. State on Monday. So did Tampa Bay Buccaneers general manager Jason Licht. The Carolina Panthers had defensive coordinator Eric Washington and defensive line coach Brady Hoke at the Wolfpack's practice facility, and the Super Bowl champion Philadelphia Eagles had assistant head coach/running backs coach Duce Staley there as well. Never miss a local story. Sign up today for a free 30 day free trial of unlimited digital access. SUBSCRIBE NOW There were no stats made available from N.C. State's Pro Day on Monday — scouts keep their stopwatches close to the vest — but who was there and what was said may matter more when figuring out a likely landing spot for N.C. State's prospective draftees. Who was Belichick watching? Belichick, the Patriots head coach, and New England Patriots defensive line coach Brendan Daly were getting a up-close look at N.C. State's four defensive linemen: Bradley Chubb, B.J. Hill, Justin Jones and Kentavius Street. Belichick even got hands-on in showing them some of the drills. Chubb probably won't still be on the draft board by the time the Patriots' 31st overall pick comes around but Hill and Jones have seen their stock rise as of late and may be two options New England mulls over in rounds 1-3. Where does Chubb think he'll go? Chubb was diplomatic with his answers — \"Wherever I get drafted, I'll be the happiest player. And I'll have been a fan of that team, wherever I get drafted, since I was 5 years old\" — but did say that he has extended meetings on Sunday and Monday with five of the top seven teams. (NFL draft order is: 1. Browns, 2. Giants, 3. Jets, 4. Browns, 5. Broncos, 6. Colts, 7. Buccaneers.) The Bucs pick seventh, and you would guess that would be one of the teams (otherwise why not say five of the top six?). Did Belichick look at Jaylen Samuels and Nyheim Hines? Yes, he even even gave the two some routes he wanted them to run. But Belichick didn't stay for the entirety of those drills. Take that and make it into whatever you will", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00781", "split": "train"}
{"id": "conditionality_train_pos_0382", "text": "Knowledge of the supernova (SN) delay time distribution (DTD) - the SN rate versus time that would follow a hypothetical brief burst of star formation - can shed light on SN progenitors and physics. We compile recent measurements of the Type-Ia SN (SN Ia) rate in galaxy clusters at redshifts z=0-1.45. Together with the observed iron-to-stellar mass ratio in clusters, which constrains the time-integrated number of SN Ia events in clusters, we recover the DTD of SNe Ia in cluster environments. The DTD peaks at the shortest time-delay interval we probe, 0<t<2.2 Gyr, with a low tail out to delays of ~10 Gyr, and is remarkably consistent with several recent DTD reconstructions based on different methods, in different environments. We test DTD models from the literature, requiring that they simultaneously reproduce the observed cluster SN rates and the observed iron-to-stellar mass ratios. A power-law DTD of the form t^{-1.2+/-0.3}, extending to a Hubble time, can satisfy both constraints. Shallower power laws, such as t^{-1/2} cannot, assuming a single DTD, and a single star-formation burst (either brief or extended) at high z. This implies 50-85% of SNe Ia explode within 1 Gyr of star formation. DTDs from double-degenerate (DD) models, which generically have ~t^{-1} shapes over a wide range of timescales, match the data, but only if their predictions are scaled up by factors of 5-10. Single degenerate (SD) DTDs always give poor fits to the data, due to a lack of delayed SNe and overall low numbers of SNe. The observations also permit a combination of two SN Ia populations - prompt (e.g. SD) SNe Ia that explode within a few Gyr of star formation, and produce about 60% of the iron mass in clusters, and a DD population that contributes the events seen at z<1.4. Our results support the existence of a DD progenitor channel for SNe Ia, if the overall predicted numbers can be suitably increased.", "label": 1, "domain": "academic", "token_count": 466, "matched_pair_id": "conditionality_00239", "split": "train"}
{"id": "conditionality_train_pos_0383", "text": "carried out by the Federal Government, with the full support of Congress, during the 1973-1974 energy crisis, resulting in a national speed limit on highways on the Interstate System of 55 miles per hour, which remained in effect until 1995; (D) a recognition that in 1974, when fewer than 137,000,000 cars traveled in the United States (as compared to 250,000,000 cars in 2006) and only 30 percent of United States oil was imported from foreign sources (as compared to 60 percent of oil so imported on the date of enactment of this Act), 167,000 barrels of oil per day were saved by the imposition of a national speed limit, such that greater savings are possible on the date of enactment of this Act than the savings realized in 1974; and (E) a determination of whether a limitation on the national speed limit on highways on the Interstate System similar to the limitation described in subparagraph (C) could serve as a model to generate gasoline savings, through a national speed limit on highways on the Interstate System of 60 miles per hour, given the improved fuel efficiency of automobile engines in use on the date of enactment of this Act. (b) Future Gasoline Conservation.-- (1) In general.--Not later than 60 days after the date of enactment of this Act, the Comptroller General of the United States shall conduct, and submit to the Committees on Homeland Security and Governmental Affairs, Environment and Public Works, and Energy and Natural Resources of the Senate and the Committees on House Administration, Transportation and Infrastructure, and Energy and Commerce of the House of Representatives a report describing the results of, a study to determine whether additional gasoline reduction measures by Federal departments and agencies and Congress are technically feasible. (2) Inclusion.--The report under paragraph (1) shall include a proposed schedule of future gasoline reduction measures, if the measures are determined to be technically feasible.", "label": 1, "domain": "government", "token_count": 399, "matched_pair_id": "conditionality_00961", "split": "train"}
{"id": "conditionality_train_pos_0384", "text": "In a dynamical-radiative model we recently developed to describe the physics of compact, GHz-Peaked-Spectrum (GPS) sources, the relativistic jets propagate across the inner, kpc-sized region of the host galaxy, while the electron population of the expanding lobes evolves and emits synchrotron and inverse-Compton (IC) radiation. Interstellar-medium gas clouds engulfed by the expanding lobes, and photoionized by the active nucleus, are responsible for the radio spectral turnover through free-free absorption (FFA) of the synchrotron photons. The model provides a description of the evolution of the spectral energy distribution (SED) of GPS sources with their expansion, predicting significant and complex high-energy emission, from the X-ray to the gamma-ray frequency domain. Here, we test this model with the broad-band SEDs of a sample of eleven X-ray emitting GPS galaxies with Compact-Symmetric-Object (CSO) morphology, and show that: (i) the shape of the radio continuum at frequencies lower than the spectral turnover is indeed well accounted for by the FFA mechanism; (ii) the observed X-ray spectra can be interpreted as non-thermal radiation produced via IC scattering of the local radiation fields off the lobe particles, providing a viable alternative to the thermal, accretion-disk dominated scenario. We also show that the relation between the hydrogen column densities derived from the X-ray (N_H) and radio (N_HI) data of the sources is suggestive of a positive correlation, which, if confirmed by future observations, would provide further support to our scenario of high-energy emitting lobes.", "label": 1, "domain": "academic", "token_count": 332, "matched_pair_id": "conditionality_00171", "split": "train"}
{"id": "conditionality_train_pos_0385", "text": "We show that matter yukawa couplings of the New Minimal Supersymmetric (SO(10)) GUT(NMSGUT) are subject to very significant GUT scale threshold corrections. Including these threshold effects relaxes the constraint $ y_b-y_\\tau\\simeq y_s-y_\\mu$ operative in $\\textbf{10} -\\textbf{120} $plet generated tree level MSSM matter fermion yukawas $y_f$. We find accurate fits of the MSSM fermion mass-mixing data in terms of NMSGUT superpotential couplings and 5 independent soft Susy breaking parameters $M_0, M_{1/2}, A_0, M^2_{H,\\bar{H}}$ at $M_X$. The fits generally have elevated unification scale $M_X$ near $M_{Planck}$, viable values of $\\alpha_3(M_Z)$, and are consistent with current limits on B violation, $b\\rightarrow s\\gamma$, muon magnetic moment anomaly and Standard Model $\\rho$ parameter. The associated novel and distinctive soft Susy spectra have light gauginos, a \\emph{normal} s-hierarchy and Bino LSP. The Bino LSP is accompanied by second and first generation right chiral sfermions light enough to mediate a consistent WIMP dark matter co-annihilation cosmology and to be discoverable at LHC, while third generation sfermions are in the LHC undiscoverable range of 3-50 TeV. The fits found require $|\\mu|,|A_0|\\sim 100$ TeV which imply both deep CCB/UFB minimae and stability of the MSSM standard vacuum on cosmological time scales. Our results indicate that a consistent realistic phenomenology may be specifiable in terms of SO(10) (NMS)GUT parameters at $M_X$ alone and that a new viable sector of the soft supersymmetry parameter space may exist if flavour violation constraints can be satisfied in the 43 dimensional parameter space.", "label": 1, "domain": "academic", "token_count": 429, "matched_pair_id": "conditionality_00355", "split": "train"}
{"id": "conditionality_train_pos_0386", "text": "if such country had been designated under subsection (b) of that section, subject to the provisions of this section. (2) Period of designation.--The initial period of such designation shall begin on the date of enactment of this Act and shall remain in effect for 18 months. (b) Aliens Eligible.--In applying section 244 of the Immigration and Nationality Act (8 U.S.C. 1254a) pursuant to the designation made under this section, and subject to subsection (c)(3) of such section, an alien who is a national of Haiti is deemed to meet the requirements of subsection (c)(1) of such section only if the alien-- (1) is admissible as an immigrant, except as otherwise provided under subsection (c)(2)(A) of such section, and is not ineligible for temporary protected status under subsection (c)(2)(B) of such section; and (2) registers for temporary protected status in a manner that the Secretary of Homeland Security shall establish. (c) Consent to Travel Abroad.--The Secretary of Homeland Security shall give the prior consent to travel abroad described in section 244(f)(3) of the Immigration and Nationality Act (8 U.S.C. 1254a(f)(3)) to an alien who is granted temporary protected status pursuant to the designation made under this section, if the alien establishes to the satisfaction of the Secretary of Homeland Security that emergency and extenuating circumstances beyond the control of the alien require the alien to depart for a brief, temporary trip abroad. An alien returning to the United States in accordance with such an authorization shall be treated the same as any other returning alien provided temporary protected status under section 244 of the Immigration and Nationality Act (8 U.S.C. 1254a).", "label": 1, "domain": "government", "token_count": 365, "matched_pair_id": "conditionality_00842", "split": "train"}
{"id": "conditionality_train_pos_0387", "text": "unless such loan or advance of credit, or any loan or advance of credit represented by such an obligation-- ``(A) involves a principal obligation not exceeding the sum of-- ``(i) the amount of the mortgage insurance premium paid by the borrower at the time that the loan, advance of credit, or purchase is made; and ``(ii) 95 percent of the appraised value of the manufactured home or lot on which to place a manufactured home (or both) for which the loan or advance of credit is made; and ``(B) is made to a borrower who has paid in cash or its equivalent, on account of the manufactured home or lot on which to place a manufactured home (or both) for which the loan or advance of credit is made, at least 3 percent of the Secretary's estimate of the costs of acquisition, alteration, improvements, lot preparation, or other eligible activity for which the loan or advance of credit was made (excluding the amount of the mortgage insurance premium paid by the borrower at the time that the loan or advance of credit is made).''. SEC. 5. INSURANCE BENEFITS. Section 2(b) of the National Housing Act (12 U.S.C. 1703(b)), as amended by section 4, is further amended by adding at the end the following new paragraph: ``(9) Insurance benefits for manufactured housing loans.-- ``(A) In general.--Any contract of insurance with respect to loans, advances of credit, or purchases in connection with a manufactured home or a lot on which to place a manufactured home (or both) for a financial institution that is executed under this title before or after the date of the enactment of the FHA Manufactured Housing Loan Modernization Act of 2005 by the Secretary shall be conclusive evidence of the eligibility of such financial institution for insurance, and the validity of any contract of insurance so executed shall be incontestable in the hands of the bearer from the date of the execution of such contract, except for fraud or misrepresentation on the part of such institution. ``(B) Losses.--With respect only to a loan, advance of credit, or purchase in connection with a manufactured home or a lot on which to place such a home (or both), the Secretary shall otherwise provide for the payment of insurance benefits under the provisions of this section for losses on such loans, advances, or purchases according to the same terms, conditions, procedures, and requirements applicable under section 204 to a mortgage insured", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01019", "split": "train"}
{"id": "conditionality_train_pos_0388", "text": "It is well known that New Physics can contribute to weak decays of heavy mesons via virtual processes during its decays. The discovery of New Physics, using such decays is made difficult due to intractable strong interaction effects needed to describe it. Modes such as B -> K^* l^+ l^- offer an advantage as they provide a multitude of observables via angular analysis. We show how the multitude of \"related observables\" obtained from B -> K^* l^+ l^-, can provide many new \"clean tests\" of the Standard Model. The hallmark of these tests is that several of them are independent of the unknown universal form factors in heavy quark effective theory. We derive a relation between observables that is free of form factors and Wilson coefficients, the violation of which will be an unambiguous signal of New Physics. We also derive relations between observables and form factors that are independent of Wilson coefficients and enable verification of hadronic estimates. We show how form factor ratios can be measured directly from helicity fraction with out any assumptions what so ever. We find that the allowed parameter space for observables is very tightly constrained in Standard Model, thereby providing clean signals of New Physics. We examine both the large-recoil and low-recoil regions of the K^* meson and point out special features and derive relations between observables valid in the two limits. In the large-recoil regions several of the relations are unaffected by corrections to all orders in \\alpha_s. We present yet another new relation involving only observables that would verify the validity of the relations between form-factors assumed in the low-recoil region. The several relations and constraints derived will provide unambiguous signals of New Physics if it contributes to these decays.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00450", "split": "train"}
{"id": "conditionality_train_pos_0389", "text": "We study in this paper three different theories of gravitation with massive gravitons - the modified Fierz-Pauli (FP) model, Massive Gravity and the bimetric theory proposed by Visser - in linear perturbation theory around a Minkowski and a flat FRW background. For the TT tensor perturbations we show that the three theories give rise to the same dynamical equations and to the same form of the Boltzmann equations for the radiative transfer in General Relativity (GR). We then analyze vector perturbations in these theories and show that they do not give the same results as in the previous case. We first show that vector perturbations in Massive Gravity present the same form as found in General Relativity, whereas in the modified FP theory the vector gravitational-wave (GW) polarization modes ($\\Psi_{3}$ amplitudes in the Newman-Penrose (NP) formalism) do not decay too fast as it happens in the former case. Rather, we show that such $\\Psi_{3}$ polarization modes give rise to an unusual vector Sachs-Wolfe effect, leaving a signature in the quadrupole form $Y_{2,\\pm 1}(\\theta,\\varphi)$ on the CMB polarization. We then derive the details for the Thomson scattering of CMB photons for these $\\Psi_{3}$ modes, and then construct the correspondent Boltzmann equations. Based upon these results we then qualitatively show that $\\Psi_{3}$-mode vector signatures - if they do exist - could clearly be distinguished on the CMB polarization from the usual $\\Psi_4$ tensor modes.", "label": 1, "domain": "academic", "token_count": 333, "matched_pair_id": "conditionality_00108", "split": "train"}
{"id": "conditionality_train_pos_0390", "text": "may make grants to demonstrate the effectiveness of outreach to populations in rural areas that do not normally seek or do not have access to health or mental health services. Grants shall be awarded to enhance linkages, integration, and cooperation in order to provide health or mental health services, to enhance services, or increase access to or utilization of health or mental health services. ``(b) Mission of the Outreach Projects.--Projects funded under subsection (a) should be designed to facilitate the integration and coordination of services in or among rural communities in order to address the needs of populations living in rural or frontier communities. ``(c) Composition of Program.-- ``(1) Consortium arrangement.--To be eligible to participate in the grant program established under subsection (a), an applicant entity shall be a consortium of three or more separate and distinct entities formed to carry out an outreach project under subsection (b). ``(2) Certain requirements.--A consortium under paragraph (1) shall be composed of three or more public or private nonprofit health care or social service providers. Consortium members may include local health departments, community or migrant health centers, community mental health centers, hospitals or private practices, or other publicly funded health or social service agencies. ``(d) Authorization of Appropriations.--For the purpose of carrying out this section, there are authorized to be appropriated $30,000,000 for fiscal year 1996, and such sums as may be necessary for each of the fiscal years 1997 through 2000.''. SEC. 4. EXTENSION OF CERTAIN PAYMENT PROVISIONS FOR MEDICARE DEPENDENT SMALL RURAL HOSPITALS. (a) In General.--Section 1886(d)(5)(G)(i) of the Social Security Act (42 U.S.C. 1395ww(d)(5)(G)(i)) is amended by striking ``October 1, 1994'' and inserting ``October 1, 1999''. (b) Payment.--Section 1886(b)(3)(D) of such Act (42 U.S.C. 1395ww(b)(3)(D)) is amended by striking ``September 30, 1994'' and inserting ``September 30, 1999''. (C) Effective Date.--The amendments made by this section shall take effect as if enacted on October 1, 1994.", "label": 1, "domain": "government", "token_count": 476, "matched_pair_id": "conditionality_00897", "split": "train"}
{"id": "conditionality_train_pos_0391", "text": "A L\\'evy noise on $\\mathbb{R}^d$ assigns a random real \"mass\" $\\Pi(B)$ to each Borel subset $B$ of $\\mathbb{R}^d$ with finite Lebesgue measure. The distribution of $\\Pi(B)$ only depends on the Lebesgue measure of $B$, and if $B_1, ..., B_n$ is a finite collection of pairwise disjoint sets, then the random variables $\\Pi(B_1), ..., \\Pi(B_n)$ are independent with $\\Pi(B_1 \\cup >... \\cup B_n) = \\Pi(B_1) + ... + \\Pi(B_n)$ almost surely. In particular, the distribution of $\\Pi \\circ g$ is the same as that of $\\Pi$ when $g$ is a bijective transformation of $\\mathbb{R}^d$ that preserves Lebesgue measure. It follows from the Hewitt--Savage zero--one law that any event which is almost surely invariant under the mappings $\\Pi \\mapsto \\Pi \\circ g$ for every Lebesgue measure preserving bijection $g$ of $\\mathbb{R}^d$ must have probability 0 or 1. We investigate whether certain smaller groups of Lebesgue measure preserving bijections also possess this property. We show that if $d \\ge 2$, the L\\'evy noise is not purely deterministic, and the group consists of linear transformations and is closed, then the invariant events all have probability 0 or 1 if and only if the group is not compact.", "label": 1, "domain": "academic", "token_count": 330, "matched_pair_id": "conditionality_00161", "split": "train"}
{"id": "conditionality_train_pos_0392", "text": "Context. LS I +61 303 is a member of the select group of gamma-ray binaries: galactic binary systems that contain a massive star and a compact object, show a changing milliarcsecond morphology and a similar broad spectral energy distribution (SED) that peaks at MeV-TeV energies and is modulated by the orbital motion. The nature of the compact object is unclear in LS I +61 303, LS 5039 and HESS J0632+057, whereas PSR B1259-63 harbours a 47.74 ms radio pulsar. Aims. A scenario in which a young pulsar wind interacts with the stellar wind has been proposed to explain the very high energy (VHE, E > 100 GeV) gamma-ray emission detected from LS I +61 303, although no pulses have been reported from this system at any wavelength. We aim to find evidence of the pulsar nature of the compact object. Methods. We performed phased array observations with the Giant Metrewave Radio Telescope (GMRT) at 1280 MHz centred at phase 0.54. Simultaneous data from the multi-bit phased array (PA) back-end with a sampling time of tsamp = 128 microsec and from the polarimeter (PMT) back-end with tsamp = 256 microsec where taken. Results. No pulses have been found in the data set, with a minimum detectable mean flux density of \\sim 0.38 mJy at 8-sigma level for the pulsed emission from a putative pulsar with period P >2 ms and duty cycle D = 10% in the direction of LS I +61 303. Conclusions. The detection of posible radio pulsations will require deep and sensitive observations at frequencies \\sim0.5-5 GHz and orbital phases 0.6-0.7. However, it may be unfeasible to detect pulses if the putative pulsar is not beamed at the Earth or if there is a strong absorption within the binary system.", "label": 1, "domain": "academic", "token_count": 422, "matched_pair_id": "conditionality_00461", "split": "train"}
{"id": "conditionality_train_pos_0393", "text": "An important result in the study of polynomial-time preprocessing shows that there is an algorithm which given an instance (G,k) of Vertex Cover outputs an equivalent instance (G',k') in polynomial time with the guarantee that G' has at most 2k' vertices (and thus O((k')^2) edges) with k' <= k. Using the terminology of parameterized complexity we say that k-Vertex Cover has a kernel with 2k vertices. There is complexity-theoretic evidence that both 2k vertices and Theta(k^2) edges are optimal for the kernel size. In this paper we consider the Vertex Cover problem with a different parameter, the size fvs(G) of a minimum feedback vertex set for G. This refined parameter is structurally smaller than the parameter k associated to the vertex covering number vc(G) since fvs(G) <= vc(G) and the difference can be arbitrarily large. We give a kernel for Vertex Cover with a number of vertices that is cubic in fvs(G): an instance (G,X,k) of Vertex Cover, where X is a feedback vertex set for G, can be transformed in polynomial time into an equivalent instance (G',X',k') such that |V(G')| <= 2k and |V(G')| <= O(|X'|^3). A similar result holds when the feedback vertex set X is not given along with the input. In sharp contrast we show that the Weighted Vertex Cover problem does not have a polynomial kernel when parameterized by the cardinality of a given vertex cover of the graph unless NP is in coNP/poly and the polynomial hierarchy collapses to the third level.", "label": 1, "domain": "academic", "token_count": 339, "matched_pair_id": "conditionality_00296", "split": "train"}
{"id": "conditionality_train_pos_0394", "text": "We use high-resolution relativistic MHD simulations coupled with a radiative transfer code to compute multiwavelength afterglow light curves of magnetized ejecta of gamma-ray bursts interacting with a uniform circumburst medium. The aim of our study is to determine how the magnetization of the ejecta at large distance from the central engine influences the afterglow emission, and to assess whether observations can be reliably used to infer the strength of the magnetic field. We find that, for typical parameters of the ejecta, the emission from the reverse shock peaks for magnetization $\\sigma_0 \\sim 0.01 - 0.1$ of the flow, and that it is greatly suppressed for higher $\\sigma_0$. The emission from the forward shock shows an achromatic break shortly after the end of the burst marking the onset of the self-similar evolution of the blast wave. Fitting the early afterglow of GRB 990123 and 090102 with our numerical models we infer respective magnetizations of $\\sigma_0 \\sim 0.01$ and $\\sigma_0 \\sim 0.1$ for these bursts. We argue that the lack of observed reverse shock emission from the majority of the bursts can be understood if $\\sigma_0 \\simmore 0.1$, since we obtain that the luminosity of the reverse shock decreases significantly for $\\sigma_0 \\sim 1$. For ejecta with $\\sigma_0 \\simmore 0.1$ our models predict that there is sufficient energy left in the magnetic field, at least during an interval of ~10 times the burst duration, to produce a substantial emission if the magnetic energy can be dissipated (for instance, due to resistive effects) and radiated away.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00219", "split": "train"}
{"id": "conditionality_train_pos_0395", "text": "We study the nonlinear growth of cosmic structure in different dark energy models, using large volume N-body simulations. We consider a range of quintessence models which feature both rapidly and slowly varying dark energy equations of state, and compare the growth of structure to that in a universe with a cosmological constant. The adoption of a quintessence model changes the expansion history of the universe, the form of the linear theory power spectrum and can alter key observables, such as the horizon scale and the distance to last scattering. We incorporate these effects into our simulations in stages to isolate the impact of each on the growth of structure. The difference in structure formation can be explained to first order by the difference in growth factor at a given epoch; this scaling also accounts for the nonlinear growth at the 15% level. We find that quintessence models that are different from $\\Lambda$CDM both today and at high redshifts $(z \\sim 1000)$ and which feature late $(z<2)$, rapid transitions in the equation of state, can have identical baryonic acoustic oscillation (BAO) peak positions to those in $\\Lambda$CDM. We find that these models have higher abundances of dark matter haloes at $z>0$ compared to $\\Lambda$CDM and so measurements of the mass function should allow us to distinguish these quintessence models from a cosmological constant. However, we find that a second class of quintessence models, whose equation of state makes an early $(z>2)$ rapid transition to $w=-1$, cannot be distinguished from $\\Lambda$CDM using measurements of the mass function or the BAO, even if these models have non-negligible amounts of dark energy at early times.", "label": 1, "domain": "academic", "token_count": 357, "matched_pair_id": "conditionality_00160", "split": "train"}
{"id": "conditionality_train_pos_0396", "text": "Protecting Your Reputation When You’re Ready to Go A top manager is preparing to leave an organization she set on a good course. What if her successors foul things up and blame her? Image Credit Glenn Harvey Send your workplace conundrums to workologist@nytimes.com, including your name and contact information (even if you want it withheld). The Workologist is a guy with well-intentioned opinions, not a professional career adviser. Letters may be edited. I’m the founding director of a nonprofit that works with local government on legal policy matters. Everyone on my small staff is competent, but all are tied in to political forces in the region. My board of directors is packed with elected officials, as well as a couple of community members. The political influence causes a lot of dysfunction, and I’m happily on my way to another position in a different field. The agency has successfully grown under my direction, but I’m worried that my colleagues will not keep the place functioning smoothly — and that their poor performance will somehow be blamed on me. Is there a checklist or some sort of parting document I can prepare to protect my reputation? LIZ Here’s one (admittedly rude) thought: Get over yourself. That’s a churlish thing to say, but I mean it in the most reassuring way possible. We’ve all had the feeling that our workplace would completely crumble in our absence. It’s rarely true. So at least consider the possibility that the organization will muddle along happily without you. More seriously, the best thing you can do is worry less about your reputation than about the organization itself. “When I think of making a checklist,” says Rebecca Zucker, a partner in the leadership development firm Next Step Partners, “I think, ‘What do I need to make sure is in place before I leave?’” Make sure you’re giving your people the information and guidance you believe they need — and responding to whatever they believe they need. In short, leave the agency “in a good position to continue on the trajectory that you’ve set it on,” Ms. Zucker adds. Even if they louse things up anyway, it’s time to move on. “There is no protecting yourself against blame once you leave a company,” says Camille Fournier, author of “The Manager’s Path” and a managing director at Two Sigma, an investment firm. Accept that this is true, she adds, even if you organize a masterful transition.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00607", "split": "train"}
{"id": "conditionality_train_pos_0397", "text": "fix of wildebeest giving birth? Are you not entertained? In our current political climate, is this not more cathartic television than anything short of Arya’s Frey Faceoff? Starting this Sunday after the Big Game (get it?), the show is airing for five straight nights. The program broadcasts game drives from Sabi Sands, South Africa, and the Maasai Mara, Kenya, zooming in on all kinds of wildlife, from big cats to bugs. It’s the circle of life and you’re all up in it. As co-founder Graham Wallington puts it, “Everything about how we build our safari experience recreates exactly what it feels like to be on the vehicle.” I’ve tagged along in the back of Mara Safari LIVE vehicle and watched an impressive amount of broadcasting, and let me tell you: watching from home has its benefits. All of the excitement of a game drive, none of the danger of tumbling-while-tipsy out of the vehicle to being eaten by lions. Note: Throughout the week of February 4th, Safari LIVE is giving normals-like-us the chance to win a full luxury African safari by playing interactive bingo.* *I, on the other hand, am offering absolutely nothing for you to play my SAFARI SUNDOWNER DRINKING GAME except the utter joy of it, so you should definitely prioritize mine. Without further ado… THE SAFARI SUNDOWNER DRINKING GAME: Unsplash Well, okay, one more ado. For our purposes, a “drink” is a sip of your favorite poison. A proper sundowner is a gin and tonic, but we’ll forgive you if your tastes run less to, um, imperialism and more to…anything else.", "label": 1, "domain": "news", "token_count": 350, "matched_pair_id": "conditionality_00558", "split": "train"}
{"id": "conditionality_train_pos_0398", "text": "adding at the end the following new subsection: ``(d) Application With Respect to Major Integrated Oil Companies.-- This section shall not apply to amounts paid or incurred by a taxpayer in any taxable year in which such taxpayer is a major integrated oil company (as defined in section 167(h)(5)(B)).''. (b) Effective Date.--The amendment made by this section shall apply to amounts paid or incurred in taxable years beginning after December 31, 2011. Subtitle B--Outer Continental Shelf Oil and Natural Gas SEC. 211. REPEAL OF OUTER CONTINENTAL SHELF DEEP WATER AND DEEP GAS ROYALTY RELIEF. (a) In General.--Sections 344 and 345 of the Energy Policy Act of 2005 (42 U.S.C. 15904, 15905) are repealed. (b) Administration.--The Secretary of the Interior shall not be required to provide for royalty relief in the lease sale terms beginning with the first lease sale held on or after the date of the enactment of this Act for which a final notice of sale has not been published. Subtitle C--Miscellaneous SEC. 221. DEFICIT REDUCTION. The net amount of any savings realized as a result of the enactment of this Act and the amendments made by this Act (after any expenditures authorized by this Act and the amendments made by this Act) shall be deposited in the Treasury and used for Federal budget deficit reduction or, if there is no Federal budget deficit, for reducing the Federal debt in such manner as the Secretary of the Treasury considers appropriate. SEC. 222. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 420, "matched_pair_id": "conditionality_01044", "split": "train"}
{"id": "conditionality_train_pos_0399", "text": "We combine new Herschel/SPIRE sub-millimeter observations with existing multiwavelength data to investigate the dust scaling relations of the Herschel Reference Survey, a magnitude-, volume-limited sample of ~300 nearby galaxies in different environments. We show that the dust-to-stellar mass ratio anti-correlates with stellar mass, stellar mass surface density and NUV-r colour across the whole range of parameters covered by our sample. Moreover, the dust-to-stellar mass ratio decreases significantly when moving from late- to early-type galaxies. These scaling relations are similar to those observed for the HI gas-fraction, supporting the idea that the cold dust is tightly coupled to the cold atomic gas component in the interstellar medium. We also find a weak increase of the dust-to-HI mass ratio with stellar mass and colour but no trend is seen with stellar mass surface density. By comparing galaxies in different environments we show that, although these scaling relations are followed by both cluster and field galaxies, HI-deficient systems have, at fixed stellar mass, stellar mass surface density and morphological type systematically lower dust-to-stellar mass and higher dust-to-HI mass ratios than HI-normal/field galaxies. This provides clear evidence that dust is removed from the star-forming disk of cluster galaxies but the effect of the environment is less strong than what is observed in the case of the HI disk. Such effects naturally arise if the dust disk is less extended than the HI and follows more closely the distribution of the molecular gas phase, i.e., if the dust-to-atomic gas ratio monotonically decreases with distance from the galactic center.", "label": 1, "domain": "academic", "token_count": 327, "matched_pair_id": "conditionality_00406", "split": "train"}
{"id": "conditionality_train_pos_0400", "text": "one or many website addresses you want to point people toward. Categories are actually quite extensive so technically you should find something to describe your business. If not, there's the ever-present Other to pick. Away Messages Away messages are automated responses that your customers will get when they try reaching you and you're not available. You can set them to on, off, or on a schedule. The message can be personalized to include any text you want (+ emoji!). As for scheduling, it's quite rudimentary now. You can set a start and end date and time, but I hope that gets improved. Recurrent options like every day or every Saturday and Sunday for example should be possible, that way you don't have to manually turn it on every night or every weekend. And that's what we've discovered so far that's different between WhatsApp Business and the regular app. For the most part, the rest of the app is unchanged, but there could be more hidden features for businesses only when you start a chat or get notifications for example. From the customer's side When your customers add your phone business' number and try to reach it, they will see a yellow briefing for end-to-end encryption (happens with regular personal chats too) as well as a pop-up and yellow briefing that they're talking to a business account and it has/hasn't been verified yet. If they check your profile, they'll see all the details you've manually applied in your business profile: image, verification status, location, category, email address, web address, and so on. So what do you think? Maybe WhatsApp Business isn't something many of you will use, but if you live in a country where everything happens on WhatsApp, you'll definitely come across businesses who use it at some point and you probably have thoughts about how they should/shouldn't handle this transition to a Business account. As a small business owner, I like what I see. I was pleasantly surprised by the landline support addition and the well thought multiple account management possibilities, but I'm expecting better analytics, better away scheduling, and more useful features in the future. You can't download WhatsApp Business right now (and neither can we) but you can sign up to test it here. Once you do, and if you're lucky enough to be accepted in the test, you should find the app on the Play Store at this address.", "label": 1, "domain": "news", "token_count": 485, "matched_pair_id": "conditionality_00770", "split": "train"}
{"id": "conditionality_train_pos_0401", "text": "If there’s one thing you should always remember about science, it’s that fact and truth are established after multiple studies converge on an answer. Even after that, further research might turn over what you thought was true of the other studies, because you were looking at it through too narrow of a lens. Single papers offer evidence, but rarely do they offer firm truths. This reality is compounded by another factor in certain fields, like nutrition and medical science. There are business interests trying to sell you a product, and proof that a product is healthy is obviously a great selling point. On the other side, if you’re an activist, proof that a product is bad can be just as useful. All of this can add bias. What the Health, a new documentary on Netflix produced by Joaquin Phoenix, takes advantage of these realities. The documentary cherry-picks studies to “prove” that any animal-based product will cause cancer or diabetes. Of course, we don’t know for sure whether giving up animal products is actually good for your health in the long run. Some studies show that vegetarians and vegans live longer, but others don’t, as Melody Ding outlines in The Conversation. Those that do suffer from a general health consciousness bias. Those folks that avoid meat and animal products could simply be living longer because they care more about their lifestyles in lots of different ways. They might also be younger and wealthier. What does that mean for you? Well, avoid meat if animal welfare or environmentalism is important to you. Otherwise, if you’re really interested in living longer (which is what everyone ultimately wants, right?) cross your fingers and hope your parents live for a long time. We use this quote a lot, but S. Jay Olshansky once told Gizmodo, “In the world of aging sciences, if you want to live a long life, choose long-lived parents.” After that, don’t smoke, and focus on a diet that minimises processed foods and includes more vegetables. Maybe eat less, get out more, and focus on a real healthy lifestyle change like biking to work every day or giving up all desserts. Past that, you might have to rely on research or expertise backed by less or less reliable data that will point you in the direction the expert thinks best reflects the existing evidence... and maybe their ethics. More Netflix Posts:", "label": 1, "domain": "news", "token_count": 476, "matched_pair_id": "conditionality_00676", "split": "train"}
{"id": "conditionality_train_pos_0402", "text": "LOS ANGELES — The Latest on a shooting following a house fire south of downtown Los Angeles (all times local): 7:35 a.m. Police say a suspect who opened fire, killing one person, after a house fire in Los Angeles appears to have suffered a self-inflicted gunshot wound. Los Angeles police say the suspect was taken into custody after holing himself up Tuesday morning for two hours inside the burned home. Police said one person had been killed but provided no additional details. Firefighters were first called to the home in the Harbor Gateway neighbourhood before dawn and reported hearing gunshots after knocking down the flames. Police and sheriff’s deputies had set up a perimeter and evacuated nearby homes. —— 7:05 a.m. Los Angeles authorities say one person was fatally shot at the scene of a house fire and a suspect is in custody after holing himself up for two hours inside the burned home. Police Officer Chris No confirmed one fatality in the shooting early Tuesday but didn’t know whether the victim is a man or woman. The Fire Department says crews heard gunshots after knocking down the flames before dawn south of downtown Los Angeles. The gunman was taken into custody shortly before 7 a.m. Several homes in the Harbor Gateway neighbourhood were evacuated as police set up a perimeter. There are no reports of injuries to firefighters or police officers. —— 6:30 a.m. Authorities say a suspect fired a weapon at the scene of a house fire south of downtown Los Angeles. The Fire Department says crews heard gunshots after dousing the flames in the Harbor Gateway neighbourhood early Tuesday. Officials say the suspect then holed up inside a home. Police and sheriff’s deputies have set up a perimeter and evacuated nearby homes. Authorities have not confirmed if anyone is hurt.", "label": 1, "domain": "news", "token_count": 358, "matched_pair_id": "conditionality_00663", "split": "train"}
{"id": "conditionality_train_pos_0403", "text": "If you’re a frequent buyer of seafood, you may be aware that more attention is being focused on how that seafood was captured. There are several certification programs meant to convey whether the fish you like to eat was taken from overfished areas. Enter another program: Fair Trade. You may know if from coffee or chocolate. In recent years, it’s expanded into seafood. And soon, the first U.S. seafood products will get that label. Is there something truly different about the Fair Trade label, or is it just another fish in the sea? If you’re a socially conscious seafood eater, you’ve got options. There’s the Marine Stewardship Council’s “Sustainable Seafood” mark, and the Monterey Bay Aquarium has a “Seafood Watch” app to help you shop. Ashley Apel, manager of the seafood program at Fair Trade USA, said her organization’s certification is different because it considers workers’ conditions and social benefits. “Other seafood certifications — at least for wild capture — really only focus on environmental sustainability of the stock,” Apel said. For U.S. scallop fishers, the premium price that comes with the label could help ease some regulatory costs. “Fishermen are still dealing with having to provide a lot of data and a lot of tracking on their vessels, and that can be very expensive,” Apel said. “So part of the premium can be used to ensure the health of the stock.” Can the marketplace sustain yet another label for responsible seafood? “If we ever got to the point where sustainability labels were competing with each other, that’d probably be a good problem to have,” said Tim Fitzgerald, who focuses on fisheries for the Environmental Defense Fund. He’s also on the advisory committee for Fair Trade’s seafood program. He said one big benefit of the label: people recognize it. “With Fair Trade getting into seafood, it puts social responsibility and environmental responsibility on the radar of just a huge amount more people,” Fitzgerald said. Still, he said price is the main factor when people choose which fish they’ll buy, and the Fair Trade scallops that’ll roll out later this month will cost a little more.", "label": 1, "domain": "news", "token_count": 436, "matched_pair_id": "conditionality_00554", "split": "train"}
{"id": "conditionality_train_pos_0404", "text": "If you think your job is more stressful than it should be, you're not alone. Americans work hard, and it takes a physical and mental toll, not to mention that it frequently cuts into personal time, according to a comprehensive survey on working conditions the nonpartisan RAND Corporation published Monday. But having a good boss and good friends on the job can make work feel less taxing. In 2015, RAND researchers, along with Harvard Medical School and the University of California, Los Angeles, began collecting data from over 3,000 people from all income and education levels who work or have worked in all types of jobs. What they discovered about how we work may help inform policymakers looking to grow the economy and employers looking to retain the best workers. This kind of data, examining workplace conditions in the U.S., has not been collected for decades. \"We have excellent data on wages, on training... but we don't know much about the conditions of work,\" says Nicole Maestas, an economist and associate health care policy professor at Harvard Medical School who is the lead researcher on this study. What the researchers found was that more than 1 in 4 Americans surveyed say they don't have enough time to do their jobs, with about half of Americans reporting that they do some work in their free time. This was most prevalent among white-collar workers. Two-thirds of all workers say they frequently work under tight deadlines or at high speed. In addition, 1 in 5 reported experiencing verbal abuse, threats, humiliating behavior or unwanted sexual attention at work in the past month; or they experienced bullying, harassment or sexual harassment in the past year. \"One thing that really struck me was the high prevalence of hostile social interactions at work,\" says Maestas. Her survey found that while such interactions were seen across the board, verbal abuse was much more common in customer service jobs and experienced at the highest rates among men who did not graduate from college. Younger women and women of \"prime age,\" defined in the survey as ages 35-49, experienced the most unwanted sexual attention. But people who have \"good\" bosses — or bosses who respect them, praise them, work with them and give feedback — were less likely to have workers who reported verbal or physical threats, Maestra notes. \"Maybe bad bosses are part of the problem,\" she says, when it comes to a hostile work environment. American workers feel, by and large, that they have a reasonable amount", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00503", "split": "train"}
{"id": "conditionality_train_pos_0405", "text": ") and (c) of section 6412 of such Code shall apply for purposes of this section. SEC. 4. FLOOR STOCKS TAX. (a) Imposition of Tax.--In the case of any liquid subject to tax under section 4091 of the Internal Revenue Code of 1986 by reason of section 4092(b)(2) of such Code and on which such tax would have been imposed but for section 2, and which is held on the suspension termination date, by any person, there is hereby imposed a floor stocks tax equal to the excess of the tax which would be imposed on such liquid had the taxable event occurred on such date over the tax previously paid (if any) on such liquid. (b) Liability for Tax and Method of Payment.-- (1) Liability for tax.--A person holding a liquid on the suspension termination date, to which the tax imposed by subsection (a) applies shall be liable for such tax. (2) Method of payment.--The tax imposed by subsection (a) shall be paid in such manner as the Secretary shall prescribe. (3) Time for payment.--The tax imposed by paragraph (1) shall be paid on or before 45 days after the suspension termination date. (c) Definitions.--For purposes of this section-- (1) Held by a person.--A liquid shall be considered as ``held by a person'' if title thereto has passed to such person (whether or not delivery to the person has been made). (2) Secretary.--The term ``Secretary'' means the Secretary of the Treasury or the Secretary's delegate. (d) Other Law Applicable.--All provisions of law, including penalties, applicable with respect to the taxes imposed by sections 4091 and 4092 of such Code shall, insofar as applicable and not inconsistent with the provisions of this section, apply with respect to the floor stock taxes imposed by subsection (a) to the same extent as if such taxes were imposed by such sections.", "label": 1, "domain": "government", "token_count": 406, "matched_pair_id": "conditionality_00943", "split": "train"}
{"id": "conditionality_train_pos_0406", "text": "Retirement Income Security Act of 1974 (29 U.S.C. 1166) is amended-- (A) in paragraph (2), by striking ``or (6)'' and inserting ``(6), or (7)''; and (B) in paragraph (4)(A), by striking ``or (6)'' and inserting ``(6), or (7)''. (4) Definition.--Section 607(3)(C) of the Employee Retirement Income Security Act of 1974 (29 U.S.C. 1167(2)) is amended by striking ``603(6)'' and inserting ``603(6) or 603(7)''. (c) Internal Revenue Code of 1986.-- (1) Period of coverage.--Section 4980B(f)(2)(B)(i) of the Internal Revenue Code of 1986 is amended by adding at the end thereof the following new subclause: ``(VI) Qualifying event involving substantial reduction or elimination of a retiree group health plan.--In the case of an event described in paragraph (3)(G), the date on which such covered qualified beneficiary becomes entitled to benefits under title XVIII of the Social Security Act.''. (2) Qualifying event.--Section 4980B(f)(3) of the Internal Revenue Code of 1986 is amended by adding at the end thereof the following new subparagraph: ``(G) The substantial reduction or elimination of group health coverage as a result of plan changes or termination with respect to a qualified beneficiary described in subsection (g)(1)(D).''. (3) Notice.--Section 4980B(f)(6) of the Internal Revenue Code of 1986 is amended-- (A) in subparagraph (B), by striking ``or (F)'' and inserting ``(F), or (G)''; and (B) in subparagraph (D)(i), by striking ``or (F)'' and inserting ``(F), or (G)''. (4) Definition.--Section 4980B(g)(1)(D) of the Internal Revenue Code of 1986 is amended by striking ``(f)(3)(F)'' and inserting ``(f)(3)(F) or (f)(3)(G)''. SEC. 3. EFFECTIVE DATE. This Act shall take effect as if enacted on January 1, 1995.", "label": 1, "domain": "government", "token_count": 486, "matched_pair_id": "conditionality_00934", "split": "train"}
{"id": "conditionality_train_pos_0407", "text": "Getty Image Jermaine Fowler was named to Variety‘s 10 comics to watch list in 2016, and in 2017, we’re all getting the chance with Fowler starring alongside Judd Hirsch in CBS’ Superior Donuts as an energetic artist/donut shop clerk and as a stand-up comic opposite Pete Holmes in HBO’s Crashing, which premieres on Sunday. Fowler was nice enough to take some time to add his answers to the Uproxx questionnaire series and to reveal that Lupe Fiasco has made him cry, Redman changed his life, and that he’d like to do the same for Nic Cage. 1. You walk into a bar. What do you order from the bartender? Pineapple juice. 2. Who’s your favorite person to follow on Twitter and/or Instagram? The Rock on Instagram and Aretha Franklin on Twitter. 3. What’s currently waiting for you on your DVR? I don’t have a DVR. Smartass. 4. It’s your last meal — what are you going out with? I’m not answering this question during Black History Month. 5. What websites do you visit on a regular basis? Forbes, Fast Company, Box Office Mojo, Complex, Fandango, Jermainefowler.com. 6. What’s the most frequently played song on your mobile device? “4r Da Squaw” by Isaiah Rashad. It used to be “LAXTasy” by Brandon DeShay until I updated my damn iPhone. I’m still pissed. 7. If you could go back and give your 18-year-old self one piece of advice what would it be? She’s gonna dump you, don’t answer the phone! 8. What’s the last thing you Googled? “is Kevin Durant a Deer?” 9. Dogs or cats? I don’t think it’s fair that I have to choose. Though, if I had to…PITBULL PUPPIES!", "label": 1, "domain": "news", "token_count": 408, "matched_pair_id": "conditionality_00563", "split": "train"}
{"id": "conditionality_train_pos_0408", "text": "We present a detailed analysis of the reliability of abundance and magnetic maps of Ap stars obtained by Zeeman Doppler mapping (ZDM). It is shown how they can be adversely affected by the assumption of a mean stellar atmosphere instead of appropriate \"local\" atmospheres corresponding to the actual abundances in a given region. The essenceof the difficulties was already shown by Chandrasekhar's picket-fence model. The results obtained with a suite of Stokes codes written in the Ada programming language and based on modern line-blanketed atmospheres are described in detail. We demonstrate that the high metallicity values claimed to have been found in chemically inhomogeneous Ap star atmospheres would lead to local temperature structures, continuum and line intensities, and line shapes that differ significantly from those predicted by a mean stellar atmosphere. Unfortunately, past applications of ZDM have consistently overlooked the intricate aspects of metallicity with their all-pervading effects. The erroneous assumption of a mean atmosphere for a spotted star can lead to phase-dependent errors of uncomfortably large proportions at varying wavelengths both in the Stokes I and V profiles, making precise mapping of abundances and magnetic field vectors largely impossible. The relation between core and wings of the H_beta line changes, too, with possible repercussions on the determination of gravity and effective temperature. Finally, a ZDM analysis of the synthetic Stokes spectra of a spotted star reveals the disturbing differences between the respective abundance maps based on a mean atmosphere on the one hand, and on appropriate \"local\" atmospheres on the other. We then discuss what this all means for published ZDMresults. Our discussion makes it clear that realistic local atmospheres must be used, especially if credible small-scale structures are to be obtained.", "label": 1, "domain": "academic", "token_count": 346, "matched_pair_id": "conditionality_00378", "split": "train"}
{"id": "conditionality_train_pos_0409", "text": "We analyzed two XMM-Newton observations of the bright atoll source 4U 1705-44, which can be considered a prototype of the class of the persistent NS LMXBs showing both hard and soft states. The first observation was performed when the source was in a hard low flux state, the second during a soft, high-flux state. Both the spectra show broad iron emission lines. We fit the spectra using a two-component model, together with a reflection model specifically suited to the case of a neutron star, where the incident spectrum has a blackbody shape. In the soft state, the reflection model, convolved with a relativistic smearing component, consistently describes the broad features present in the spectrum, and we find a clear relation between the temperature of the incident flux and the temperature of the harder X-ray component that we interpret as the boundary layer emission. In this state we find converging evidence that the boundary layer outer radius is ~ 2 times the neutron star radius. In the low flux state, we observe a change in the continuum shape of the spectrum with respect to the soft state. Still, the broad local emission features can be associated with a disk reflecting matter, but in a lower ionization state, and possibly produced in an accretion disk truncated at greater distance. Our analysis provides strong evidence that the reflection component in soft states of LMXBs comes from to hard X-ray thermal irradiation, which we identify with the boundary layer emission, also present in the continuum model. In the hard state, the broad iron line if also produced by reflection, and the continuum disk emission can be self-consistently accounted if the disk is truncated at a greater distance than the soft state.", "label": 1, "domain": "academic", "token_count": 346, "matched_pair_id": "conditionality_00217", "split": "train"}
{"id": "conditionality_train_pos_0410", "text": "roup Transactions.-- Section 355 of the Internal Revenue Code of 1986, as amended by subsection (a), is amended by adding at the end the following new subsection: ``(f) Section Not To Apply to Certain Intragroup Transactions.-- Except as provided in regulations, this section shall not apply to the distribution of stock from 1 member of an affiliated group filing a consolidated return to another member of such group, and the Secretary shall provide proper adjustments for the treatment of such distribution, including (if necessary) adjustments to-- ``(1) the adjusted basis of any stock which-- ``(A) is in a corporation which is a member of such group, and ``(B) is held by another member of such group, and ``(2) the earnings and profits of any member of such group.'' (c) Effective Date.-- (1) In general.--The amendments made by this section shall apply to distributions after April 16, 1997. (2) Transition rule for distributions followed by acquisitions.--The amendments made by subsection (a) shall not apply to any distribution after April 16, 1997, if such distribution is-- (A) made pursuant to a written agreement which was (subject to customary conditions) binding on such date and at all times thereafter, (B) described in a ruling request submitted to the Internal Revenue Service on or before such date, or (C) described on or before such date in a public announcement or in a filing with the Securities and Exchange Commission required solely by reason of the distribution. This paragraph shall not apply to any written agreement, ruling request, or public announcement or filing unless it identifies the acquirer of the distributing corporation or any controlled corporation, whichever is applicable.", "label": 1, "domain": "government", "token_count": 346, "matched_pair_id": "conditionality_00931", "split": "train"}
{"id": "conditionality_train_pos_0411", "text": "if you’ve raised over $100! If you don’t need to drop off funds or pick up a shirt, there is no need to stop by registration, you can simply enjoy our festival zone! Stroller are of course permitted along the walk route. Feel free to run the route, however please note that the March of Dimes will not be keeping time for runners. Please do not bring your bike, bikers will not be permitted on the walk route in the interest of the safety of all other walkers. Dogs ARE welcome at the Balboa Park walk, however they are not permitted at the Oceanside walk site. Together we hope for a day when all moms and babies are healthy. Families, businesses, and volunteers dedicated to the fight for the health of all moms and babies take part in March for Babies®, March of Dimes biggest annual fundraising event. All March for Babies events are non-smoking. About March of Dimes March of Dimes is the leading non-profit organization for pregnancy and baby health. If you had a heel prick test, and APGAR score, were ever given a Polio Vaccine or your mother took Folic Acid during pregnancy, chances are YOU are a March of Dimes Baby. Since 1938, March of Dimes has been actively working to fight infant disease, birth defects and premature birth across the globe. March of Dimes offers comprehensive information on pregnancy and newborn topics, such as, complications, caring for your baby, birth defects, folic acid, etc. Through marchofdimes.com you can search various pregnancy related topics and access medical references, publications, and reports.", "label": 1, "domain": "news", "token_count": 329, "matched_pair_id": "conditionality_00636", "split": "train"}
{"id": "conditionality_train_pos_0412", "text": "If you have ever spent any time in Toronto’s Kensington Market, then you have likely passed by Reg Dried Foods. The dried fruit and nut shop on Baldwin Street is a modestly sized emporium overflowing with rare spices, dried exotic fruit and nuts in every shape and variety imported from all over the world. Among the gleaming jars of saffron and green and purple tubs filled with crushed pistachios sits Reg Alex, the store’s owner and chief employee. For the past 41 years, she has watched Kensington’s lively community evolve from a livestock market in the 1970s, to a bohemian hippy paradise in the 1990s, to the gentrified arena of craft beer breweries and artisanal grocery stores that it is today. After escaping communism and emigrating from Romania in 1976, Alex opened Reg Dried Foods later that year. At 80 years old, she has never taken a vacation. She works seven days a week and 14 hours a day everyday, only taking time off for Christmas and New Year’s. Her unwavering work ethic has woven her presence into the fabric of Kensington, right next to the kaleidoscopic graffiti alleys and corners overflowing with produce stands. Decades of Toronto residents are familiar with the lady who sits outside the dried food shop and watches to make sure that you don’t accidentally pop a plump sliver of dried kiwi into your mouth before paying for your haul, but few actually know who she is. “My name is Reg,” she says, pointing to the store sign that reads Reg Dried Foods. “Reg Alex. That’s it.” As a wave of shoppers clad in trendy streetwear labels and Louis Vuitton purses pass by, one gets the sense that there is almost too much to explain about the decades she has spent watching Kensington change. “Come here, Corina,” she says eventually, getting up from her stool between the bulk bins and walking out into the street. “It’s Claudia,” I correct without realizing that, to her, I might as well be called Reporter Number 156. “Ok Corina,” she insists, grabbing my arm and forcing me to lean in before whispering into my ear. “Chickens.” She points up and down the narrow road littered with gourmet food shops, including a chocolatier selling hand-painted single origin chocolates and an artisanal sourdough bakery. “In the ’", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00662", "split": "train"}
{"id": "conditionality_train_pos_0413", "text": "If you’re a business leader, it’s likely you got to where you are through hard work, perseverance, and a determination to be the best you can be. Regardless of your success, you’re unlikely to be content with your current leadership game. Instead, you’re always seeking ways in which to advance and improve. This is no easy feat. Being a leader demands high levels of responsibility; leaders need to motivate and inspire their team, and they need to deal with fluctuating workplace demands. Moreover, what constitutes a great leader tends to evolve and change over time. What compelled Generation X to work hard won’t work with Generation Z. As our understanding of human psychology advances, we also become more knowledgeable on what inspires high levels of engagement and discretionary effort. With this article, we’ll look at modern leadership techniques and how to implement them in 2018 in order to improve individual, team, and company performance and productivity, while building a more competitive and profitable business. 1. Take the time to discover employee strengths — and allow them to use them As we move into 2018, autonomy is a key concept all leaders should keep in mind when it comes to both their leadership style and their performance management systems. Rather than rigidly controlling your employees or trying to manipulate their strengths to suit your company, you would be far more efficient and successful as a leader if you allowed your employees to play to their strengths. According to a Gallup poll, if you keep your employees' strengths in mind when constructing objectives and goals, you can make your company much stronger. Simultaneously, you can boost engagement and morale while minimizing turnover and lessening stress levels The use of employee strengths has been shown to be far more effective a motivator than even leadership exhortations. Put simply, this is because as a leader, you have taken the time to find out what truly motivates your employees, which ultimately works to your company’s advantage. In fact, even simply learning about employee strengths is known to make them 7.8% more productive, while boosting company sales and profit. So as we move into 2018, leaders should do more to focus on strengths and positives than dwelling on what employees can stand to improve. 2. Incorporate real-time feedback and more frequent one-on-ones The concept of continuous, agile performance management is no longer a revolutionary or disruptive management trend. It’s widely recognized to be a more effective means of managing behavior and performance than an annual performance review", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00614", "split": "train"}
{"id": "conditionality_train_pos_0414", "text": "The XMM-Newton survey of the Small Magellanic Cloud (SMC) was performed to study the population of X-ray sources in this neighbouring galaxy. During one of the observations, the symbiotic binary SMC3 was found at its highest X-ray luminosity observed until now. In SMC3 wind accretion from a giant donor star onto a white dwarf is believed to cause steady hydrogen burning on the white dwarf surface, making such systems candidates for supernova type Ia progenitors. It was suggested that the X-ray source is eclipsed every ~4.5 years by the companion star and its stellar wind to explain the large X-ray variability seen in ROSAT data. We use the available X-ray data to test this scenario. We present the ~20 year X-ray light curve of SMC3 and study the spectral evolution as seen with XMM-Newton/EPIC-pn to investigate possible scenarios which can reproduce the high X-ray variability. We did not find significant variations in the photo-electric absorption, as it would be expected during eclipse ingress and egress. Instead, the X-ray spectra from different intensity levels, when modelled by black-body emission, can be better explained by variations either in normalisation (by a factor of ~50) or in temperature (kT between 24 eV and 34 eV). The light curve shows maxima and minima with slow transitions between them. To explain the gradual variations in the X-ray light curve and to avoid changes in absorption by neutral gas, a predominant part of the stellar wind must be ionised by the X-ray source. Compton scattering with variable electron column density (of the order of 5 x 10^24 cm^-2) along the line of sight could then be responsible for the intensity changes. The X-ray variability of SMC3 could also be caused by temperature changes in the hydrogen burning envelope of the white dwarf, an effect which could even dominate if the stellar wind density is not sufficiently high.", "label": 1, "domain": "academic", "token_count": 406, "matched_pair_id": "conditionality_00273", "split": "train"}
{"id": "conditionality_train_pos_0415", "text": "We investigate the potential of the Square Kilometre Array (SKA) for measuring the magnetic fields in clusters of galaxies via Faraday rotation of background polarised sources. [...] We find that about 10 per cent of the sky is covered by a significant extragalactic Faraday screen. Most of it has rotation measures between 10 and 100 rad/m/m. We argue that the cluster centres should have up to about 5000 rad/m/m. We show that the proposed mid frequency aperture array of the SKA as well as the lowest band of the SKA dish array are well suited to make measurements for most of these rotation measure values, typically requiring a signal-to-noise of ten. We calculate the spacing of sources forming a grid for the purpose of measuring foreground rotation measures: it reaches a spacing of 36 arcsec for a 100 hour SKA observation per field. We also calculate the statistics for background RM measurements in clusters of galaxies. We find that a first phase of the SKA would allow us to take stacking experiments out to high redshifts (>1), and provide improved magnetic field structure measurements for individual nearby clusters. The full SKA aperture array would be able to make very detailed magnetic field structure measurements of clusters with more than 100 background sources per cluster up to a redshift of 0.5 and more than 1000 background sources per cluster for nearby clusters, and could for reasonable assumptions about future measurements of electron densities in high redshift clusters constrain the power law index for the magnetic field evolution to better than dm=0.4, if the magnetic field in clusters should follow B ~ (1+z)^m.", "label": 1, "domain": "academic", "token_count": 334, "matched_pair_id": "conditionality_00159", "split": "train"}
{"id": "conditionality_train_pos_0416", "text": "An investigation is launched into the fundamental characteristics of operations on and between sets, with a focus on compact convex sets and star sets (compact sets star-shaped with respect to the origin) in $n$-dimensional Euclidean space $\\R^n$. For example, it is proved that if $n\\ge 2$, with three trivial exceptions, an operation between origin-symmetric compact convex sets is continuous in the Hausdorff metric, GL(n) covariant, and associative if and only if it is $L_p$ addition for some $1\\le p\\le\\infty$. It is also demonstrated that if $n\\ge 2$, an operation * between compact convex sets is continuous in the Hausdorff metric, GL(n) covariant, and has the identity property (i.e., $K*\\{o\\}=K=\\{o\\}*K$ for all compact convex sets $K$, where $o$ denotes the origin) if and only if it is Minkowski addition. Some analogous results for operations between star sets are obtained. An operation called $M$-addition is generalized and systematically studied for the first time. Geometric-analytic formulas that characterize continuous and GL(n)-covariant operations between compact convex sets in terms of $M$-addition are established. The term \"polynomial volume\" is introduced for the property of operations * between compact convex or star sets that the volume of $rK*sL$, $r,s\\ge 0$, is a polynomial in the variables $r$ and $s$. It is proved that if $n\\ge 2$, with three trivial exceptions, an operation between origin-symmetric compact convex sets is continuous in the Hausdorff metric, GL(n) covariant, associative, and has polynomial volume if and only if it is Minkowski addition.", "label": 1, "domain": "academic", "token_count": 381, "matched_pair_id": "conditionality_00456", "split": "train"}
{"id": "conditionality_train_pos_0417", "text": "If $\\Omega\\subset\\R^n$ is a bounded domain, the existence of solutions ${\\bf u}\\in H^1_0(\\Omega)^n$ of ${div} {\\bf u} = f$ for $f\\in L^2(\\Omega)$ with vanishing mean value, is a basic result in the analysis of the Stokes equations. In particular it allows to show the existence of a solution $({\\bf u},p)\\in H^1_0(\\Omega)^n\\times L^2(\\Omega)$, where ${\\bf u}$ is the velocity and $p$ the pressure. It is known that the above mentioned result holds when $\\Omega$ is a Lipschitz domain and that it is not valid for arbitrary H\\\"older-$\\alpha$ domains. In this paper we prove that if $\\Omega$ is a planar simply connected H\\\"older-$\\alpha$ domain, there exist right inverses of the divergence which are continuous in appropriate weighted spaces, where the weights are powers of the distance to the boundary. Moreover, we show that the powers of the distance in the results obtained are optimal. In our results, the zero boundary condition is replaced by a weaker one. For the particular case of domains with an external cusp of power type, we prove that our weaker boundary condition is equivalent to the standard one. In this case we show the well posedness of the Stokes equations in appropriate weighted Sobolev spaces obtaining as a consequence the existence of a solution $({\\bf u},p)\\in H^1_0(\\Omega)^n\\times L^r(\\Omega)$ for some $r<2$ depending on the power of the cusp.", "label": 1, "domain": "academic", "token_count": 348, "matched_pair_id": "conditionality_00064", "split": "train"}
{"id": "conditionality_train_pos_0418", "text": "In this paper we consider a nearest-neighbor $p$-adic hard core (HC) model, with fugacity $\\lambda$, on a homogeneous Cayley tree of order $k$ (with $k + 1$ neighbors). We focus on $p$-adic Gibbs measures for the HC model, in particular on $p$-adic \"splitting\" Gibbs measures generating a $p$-adic Markov chain along each path on the tree. We show that the $p$-adic HC model is completely different from real HC model: For a fixed $k$ we prove that the $p$-adic HC model may have a splitting Gibbs measure only if $p$ divides $2^k-1$. Moreover if $p$ divides $2^k-1$ but does not divide $k+2$ then there exists unique translational invariant $p$-adic Gibbs measure. We also study $p$-adic periodic splitting Gibbs measures and show that the above model admits only translational invariant and periodic with period two (chess-board) Gibbs measures. For $p\\geq 7$ (resp. $p=2,3,5$) we give necessary and sufficient (resp. necessary) conditions for the existence of a periodic $p$-adic measure. For k=2 a $p$-adic splitting Gibbs measures exists if and only if p=3, in this case we show that if $\\lambda$ belongs to a $p$-adic ball of radius 1/27 then there are precisely two periodic (non translational invariant) $p$-adic Gibbs measures. We prove that a $p$-adic Gibbs measure is bounded if and only if $p\\ne 3$.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00360", "split": "train"}
{"id": "conditionality_train_pos_0419", "text": "Let game B be Toral's cooperative Parrondo game with (one-dimensional) spatial dependence, parameterized by N (3 or more) and p_0,p_1,p_2,p_3 in [0,1], and let game A be the special case p_0=p_1=p_2=p_3=1/2. Let mu_B (resp., mu_(1/2,1/2)) denote the mean profit per turn to the ensemble of N players always playing game B (resp., always playing the randomly mixed game (1/2)(A+B)). In previous work we showed that, under certain conditions, both sequences converge and the limits can be expressed in terms of a parameterized spin system on the one-dimensional integer lattice. Of course one can get similar results for mu_(gamma,1-gamma) corresponding to gamma A+(1-gamma)B for 0<gamma<1. In this paper we replace the random mixture with the nonrandom periodic pattern A^r B^s, where r and s are positive integers. We show that, under certain conditions, mu_[r,s], the mean profit per turn to the ensemble of N players repeatedly playing the pattern A^r B^s, converges to the same limit that mu_(gamma,1-gamma) converges to, where gamma:=r/(r+s). For a particular choice of the probability parameters, namely p_0=1, p_1=p_2 in (1/2,1), and p_3=0, we show that the Parrondo effect (i.e., mu_B is nonpositive and mu_[r,s] is positive) is present if and only if N is even, at least when s=1.", "label": 1, "domain": "academic", "token_count": 360, "matched_pair_id": "conditionality_00473", "split": "train"}
{"id": "conditionality_train_pos_0420", "text": "on Twitter suggesting the same. Paul McShane’s reaction when Liam Hood threw the ball at him suggested he was dumbfounded that, after giving himself up and not risking giving away a penalty for failing to be square, he was instead penalised for standing a good few metres behind the play-the-ball after someone chucked it at him! “I’ve seen it a few times over the weekend and it’s not something I’m a big fan of,” Hull captain Gareth Ellis said on Monday’s Super League Show. “I’d like to see it addressed.” It’s hard to disagree with Ellis. It’s essentially gamesmanship – and perhaps referees can instead penalise attacking teams for doing it so blatantly to try and win a penalty and get easy points if they believe that’s the case? Apparently, one Super League coach warned his side off doing it following the opening weekend. Hopefully it can be clamped down upon sooner rather than later – although we’ll see on Thursday with Huddersfield’s clash against Salford whether anything has changed. Perhaps it’s no surprise when you read this column and see that I picked out Castleford Tigers as the team that really caught my eye on the first weekend of the new season. The Tigers were well-held by Leigh for the opening 20 minutes of their match last Friday but in truth, once Cas got one try, the points continued to flow – and you might struggle to see as breathless a 20 minutes all season as the period Daryl Powell’s men put together in the run-up to half-time at the weekend. There were impressive performances all across the field, and while new recruits such as Zak Hardaker and Jesse Sene-Lefao will make a massive impact in 2017, having captain Michael Shenton back was like a whole new signing in itself. Shenton was back to his best on Friday night too, I thought. A winger is only as good as his centre, so the old saying goes, and whichever Cas winger is lucky enough to play outside the classy Shenton this season will have a hell of a time pocketing tries. It’s no surprise to see him straight back in England’s EPS squad after his cruel season-ending injury 12 months ago, too. He remains one of England’s most enjoyable outside backs to watch – and he will give England an extra dimension if he keeps this form up throughout 2017.", "label": 1, "domain": "news", "token_count": 484, "matched_pair_id": "conditionality_00785", "split": "train"}
{"id": "conditionality_train_pos_0421", "text": "If you could bend time … regardless of eras, what four drivers would you like to see race for the win at Daytona? Nate Ryan: Dale Earnhardt, Dale Earnhardt Jr. David Pearson and Richard Petty. When I think of winners in magical moments at Daytona, those are the four names that initially come to mind. The next question would be: Does the race happen with or without restrictor plates? Dustin Long: Richard Petty, David Pearson, Dale Earnhardt Sr. and Mario Andretti. All Daytona 500 winners and among the greats in racing. Daniel McFadin: Dale Earnhardt Jr. from 2004, Dale Earnhardt Sr. from 1991, Bill Elliott from 1988 and Brad Keselowski from today. Give them some IROC cars from 1999 and let them loose for 25 laps. Dan Beaver: Richard Petty, David Pearson, Jeff Gordon and Dale Earnhardt Sr. I’m not sure who would win, but it would certainly be spectacular. What driver currently outside a playoff spot is one you think has the best chance to win Saturday’s race at Daytona (7:30 p.m. ET on NBC)? Nate Ryan: Jamie McMurray. The two-time winner at Daytona always is a solid driver in plate races if he can avoid the wrecks and getting antsy in the draft. Dustin Long: Ryan Newman. He’s won at Daytona before and his teammate, Austin Dillon, won the Daytona 500 in February. Richard Childress Racing could make it two in a row there. Daniel McFadin: I think Paul Menard could be a sleeper. He’s finished in the top six in his last three Daytona starts. He and AJ Allmendinger are the only drivers who have finished in the top 10 in the last three Daytona races. Dan Beaver: The defending winner of this race, Ricky Stenhouse Jr., has a knack for plate racing and could get into the playoffs this week. What’s the wildest finish you’ve witnessed? Nate Ryan: The Oct. 7, 2012 race at Talladega Superspeedway. Tony Stewart attempted to throw a block off Turn 4 on the last lap, and 25 cars wrecked a few hundred yards from the finish line in a massive storm of dirt, sheet metal and smoke Dustin Long: The finish to the 2007 Daytona 500. It has Kevin Harvick and Mark Martin side-by-side", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00778", "split": "train"}
{"id": "conditionality_train_pos_0422", "text": "by adding at the end the following new subsection: ``(e) Methodology for Designating Assets.-- ``(1) In general.--In carrying out subsection (b), the Secretary may develop and implement a methodology for designating assets after the replacement plan adoption date that takes into account the value of the District Retirement Fund as of the replacement plan adoption date and the proportion of such value represented by $1.275 billion, together with the income (including returns on investments) earned on the assets of and withdrawals from and deposits to the Fund during the period between such date and the date on which the Secretary designates assets under subsection (b). In implementing a methodology under the previous sentence, the Secretary shall not be required to determine the value of designated assets as of the replacement plan adoption date. Nothing in this paragraph may be deemed to effect the entitlement of the District Retirement Fund to income (including returns on investments) earned after the replacement plan adoption date on assets designated for retention by the Fund. ``(2) Employee contributions; judicial retirement and survivors annuity fund.--The Secretary may develop and implement a methodology comparable to the methodology described in paragraph (1) in carrying out the requirements of subsection (c) and in designating assets to be transferred to the District of Columbia Judicial Retirement and Survivors Annuity Fund pursuant to section 124(c)(1) of the District of Columbia Retirement Reform Act (as amended by section 11252). ``(3) Discretion of the secretary.--The Secretary's development and implementation of methodologies for designating assets under this subsection shall be final and binding.''. SEC. 5. EFFECTIVE DATE. This Act and the amendments made by this Act shall take effect as if included in the enactment of title XI of the Balanced Budget Act of 1997.", "label": 1, "domain": "government", "token_count": 358, "matched_pair_id": "conditionality_00902", "split": "train"}
{"id": "conditionality_train_pos_0423", "text": "Using a combination of N-body simulations, semi-analytic models and radiative transfer calculations, we have estimated the theoretical cross power spectrum between galaxies and the 21cm emission from neutral hydrogen during the epoch of reionization. In accordance with previous studies, we find that the 21cm emission is initially correlated with halos on large scales (> 30 Mpc), anti-correlated on intermediate (~ 5 Mpc), and uncorrelated on small (< 3 Mpc) scales. This picture quickly changes as reionization proceeds and the two fields become anti-correlated on large scales. The normalization of the cross power spectrum can be used to set constraints on the average neutral fraction in the intergalactic medium and its shape can be a tool to study the topology of reionization. When we apply a drop-out technique to select galaxies and add to the 21cm signal the noise expected from the LOFAR telescope, we find that while the normalization of the cross power spectrum remains a useful tool for probing reionization, its shape becomes too noisy to be informative. On the other hand, for a Lyalpha Emitter (LAE) survey both the normalization and the shape of the cross power spectrum are suitable probes of reionization. A closer look at a specific planned LAE observing program using Subaru Hyper-Suprime Cam reveals concerns about the strength of the 21cm signal at the planned redshifts. If the ionized fraction at z ~ 7 is lower that the one estimated here, then using the cross power spectrum may be a useful exercise given that at higher redshifts and neutral fractions it is able to distinguish between two toy models with different topologies.", "label": 1, "domain": "academic", "token_count": 344, "matched_pair_id": "conditionality_00498", "split": "train"}
{"id": "conditionality_train_pos_0424", "text": "If the hospital or critical access hospital is not within such network or otherwise such a participating provider or supplier, the estimated amount that the hospital or critical access hospital will charge the individual for such items and services in excess of any cost sharing obligations that the individual would otherwise have under such health benefits coverage for such items and services if the hospital or critical access hospital were within such network or otherwise participating in such coverage. ``(C) Whether any of the providers of services or suppliers furnishing items or services at the hospital or critical access hospital who will furnish the items or services to the individual are not within the health care provider network or otherwise a participating provider of services or supplier with respect to such health benefits coverage of such individual. ``(D) If any of such providers of services or suppliers are not within such network or otherwise such a participating provider or supplier, the estimated amount that such providers of services or suppliers will charge the individual for such items and services in excess of any cost sharing obligations that the individual would otherwise have for such items and services if the providers of services or suppliers were within the such network or otherwise participating in such coverage. ``(3) Consent described.--For purposes of paragraph (1)(B), the consent described in this paragraph, with respect to an individual with health benefits coverage described in paragraph (1) who is to be furnished items or services by a hospital or critical access hospital (or provider of services or supplier furnishing services at such hospital or critical access hospital) that is not within the health care provider network or otherwise a participating provider of services or supplier with respect to such health benefits coverage of such individual, is a document specified by the Secretary through rulemaking that is signed by the individual (or by a representative of the individual) not less than 24 hours prior to the individual being furnished such items or services by such hospital, critical access hospital, provider of services, or supplier, respectively, and that-- ``(A) acknowledges that the individual has been-- ``(i) provided with a written estimate of the charge that the individual will be assessed for the items or services anticipated to be furnished to the individual by the hospital, critical access hospital, provider of services, or supplier that is not within such network or otherwise such a participating provider of services or supplier; and ``(ii) informed that the payment of such charge by the individual will not accrue toward any limitation that the health benefits coverage places upon the annual out-of-pocket expenses to be paid by the individual or upon the in-network", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01007", "split": "train"}
{"id": "conditionality_train_pos_0425", "text": "Assuming that inflation happened through a series of tunneling in the string theory landscape, it is argued that one can determine the structure of vacua using precise measurements of the scalar spectral index and tensor perturbations at large scales. It is shown that for a vacuum structure where the energy gap between the minima is constant, i.e. $\\epsilon_i=i m_f^4$, one obtains the scalar spectral index, $n_s$, to be $\\simeq 0.9687$, for the modes that exit the horizon 60 e-folds before the end of inflation. Alternatively, for a vacuum structure in which the energy gap increases linearly with the vacuum index, i.e. $\\epsilon_i=\\frac{i^2}{2} m_f^4$, $n_s$ turns out to be $\\simeq 0.9614$. Both these two models are motivated within the string theory landscape using flux-compactification and their predictions for scalar spectral index are compatible with WMAP results. For both these two models, the results for the scalar spectral index turn out to be independent of $m_f$. Nonetheless, assuming that inflation started at Planckian energies and that there had been successful thermalization at each step, one can constrain $m_f<2.6069\\times 10^{-5} m_P$ and $m_f<6.5396\\times 10^{-7} m_P$ in these two models, respectively. Violation of the single-field consistency relation between the tensor and scalar spectra is another prediction of chain inflation models. This corresponds to having a smaller tensor/scalar ratio at large scales in comparison with the slow-roll counterparts. Similar to slow-roll inflation, it is argued that one can reconstruct the vacuum structure using the CMB experiments.", "label": 1, "domain": "academic", "token_count": 362, "matched_pair_id": "conditionality_00196", "split": "train"}
{"id": "conditionality_train_pos_0426", "text": "d) Semiannual Reports.--Section 3013 of title 39, United States Code, is amended-- (1) in paragraph (1), by inserting ``3002b(b) or'' before ``3005''; and (2) in paragraph (3), by striking ``section 3007 of this title'' and inserting ``section 3002b(c) or section 3007, respectively,''. (e) Clerical Amendment.--The table of sections for chapter 30 of title 39, United States Code, is amended by inserting after the item relating to section 3002a the following: ``3002b. Nonmailability of certain tobacco products.''. (f) Effective Dates.-- (1) In general.--Except as provided in paragraph (2), the amendments made by this section shall take effect on the 60th day after the date of the enactment of this Act, and shall apply with respect to any mail matter mailed on or after such 60th day. (2) Semiannual reports.--The amendments made by subsection (d) shall apply beginning with the report submitted for the reporting period in which occurs the 60th day after the date of the enactment of this Act. SEC. 2. TECHNICAL CORRECTION. (a) In General.--Sections 3007(a)(1), 3012(b)(1), and 3018(f)(1) of title 39, United States Code, are amended by striking ``409(d)'' and inserting ``409(g)(2)''. (b) Effective Date.--The amendments made by subsection (a) shall take effect as if included in the enactment of the Postal Accountability and Enhancement Act (Public Law 109-435).", "label": 1, "domain": "government", "token_count": 354, "matched_pair_id": "conditionality_00848", "split": "train"}
{"id": "conditionality_train_pos_0427", "text": "If $G$ is a looped graph, then its adjacency matrix represents a binary matroid $M_{A}(G)$ on $V(G)$. $M_{A}(G)$ may be obtained from the delta-matroid represented by the adjacency matrix of $G$, but $M_{A}(G)$ is less sensitive to the structure of $G$. Jaeger proved that every binary matroid is $M_{A}(G)$ for some $G$ [Ann. Discrete Math. 17 (1983), 371-376]. The relationship between the matroidal structure of $M_{A}(G)$ and the graphical structure of $G$ has many interesting features. For instance, the matroid minors $M_{A}(G)-v$ and $M_{A}(G)/v$ are both of the form $M_{A}(G^{\\prime}-v)$ where $G^{\\prime}$ may be obtained from $G$ using local complementation. In addition, matroidal considerations lead to a principal vertex tripartition, distinct from the principal edge tripartition of Rosenstiehl and Read [Ann. Discrete Math. 3 (1978), 195-226]. Several of these results are given two very different proofs, the first involving linear algebra and the second involving set systems or delta-matroids. Also, the Tutte polynomials of the adjacency matroids of $G$ and its full subgraphs are closely connected to the interlace polynomial of Arratia, Bollob\\'{a}s and Sorkin [Combinatorica 24 (2004), 567-584].", "label": 1, "domain": "academic", "token_count": 340, "matched_pair_id": "conditionality_00364", "split": "train"}
{"id": "conditionality_train_pos_0428", "text": "Gronwall's function $G$ is defined for $n>1$ by $G(n)=\\frac{\\sigma(n)}{n \\log\\log n}$ where $\\sigma(n)$ is the sum of the divisors of $n$. We call an integer $N>1$ a \\emph{GA1 number} if $N$ is composite and $G(N) \\ge G(N/p)$ for all prime factors $p$ of $N$. We say that $N$ is a \\emph{GA2 number} if $G(N) \\ge G(aN)$ for all multiples $aN$ of $N$. In arXiv 1110.5078, we used Robin's and Gronwall's theorems on $G$ to prove that the Riemann Hypothesis (RH) is true if and only if 4 is the only number that is both GA1 and GA2. Here, we study GA1 numbers and GA2 numbers separately. We compare them with superabundant (SA) and colossally abundant (CA) numbers (first studied by Ramanujan). We give algorithms for computing GA1 numbers; the smallest one with more than two prime factors is 183783600, while the smallest odd one is 1058462574572984015114271643676625. We find nineteen GA2 numbers $\\le 5040$, and prove that a GA2 number $N>5040$ exists if and only if RH is false, in which case $N$ is even and $>10^{8576}$.", "label": 1, "domain": "academic", "token_count": 331, "matched_pair_id": "conditionality_00400", "split": "train"}
{"id": "conditionality_train_pos_0429", "text": "7. REGULATIONS. (a) In General.--Not later than 90 days after the date of the enactment of this Act, the Secretary of Defense shall revise Department of Defense regulations, and shall issue such new regulations as may be necessary, to implement section 656 of title 10, United States Code, as added by section 4(a). The Secretary of Defense shall further direct the Secretary of each military department to revise regulations of that military department in accordance with section 656 of title 10, United States Code, as added by section 4(a), not later than 180 days after the date of the enactment of this Act. Such revisions shall include the following: (1) Revision of all equal opportunity and human relations regulations, directives, and instructions to add sexual orientation nondiscrimination to the Department of Defense Equal Opportunity policy and to related human relations training programs. (2) Revision of Department of Defense and military department personnel regulations to eliminate procedures for involuntary discharges based on sexual orientation. (3) Revision of Department of Defense and military department regulations governing victims' advocacy programs to include sexual orientation discrimination among the forms of discrimination for which members of the Armed Forces and their families may seek assistance. (b) Regulation of Conduct.--The Secretary of Defense, and the Secretary of Homeland Security with respect to the Coast Guard when it is not operating as a service in the Navy, shall ensure that regulations governing the personal conduct of members of the Armed Forces shall be written and enforced without regard to sexual orientation. (c) Definition.--In this section, the term ``sexual orientation'' has the meaning given that term in section 656(f) of title 10, United States Code, as added by section 4(a).", "label": 1, "domain": "government", "token_count": 348, "matched_pair_id": "conditionality_00949", "split": "train"}
{"id": "conditionality_train_pos_0430", "text": "We present measurements of the triaxial dark matter halo shapes and alignment correlation functions in the Millennium and Millennium-2 dark matter N-body simulations. These two simulations allow us to measure the distributions of halo shapes down to 10% of the virial radius over a halo mass range of 6E9 - 2E14 M_sun/h. We largely confirm previous results on the distributions of halo axis ratios as a function of halo mass, but we find that the median angle between halo major axes at different halo radii can vary by a factor of 2 between the Millennium-1 and 2 simulations because of the different mass resolution. Thus, error in the shape determinations from limited resolution is potentially degenerate with the misalignment of halo inner and outer shapes used to constrain Brightest Cluster Galaxy alignments in previous works. We also present simplifying parameterizations for the 3-D halo-mass alignment correlation functions that are necessary ingredients for triaxial halo models of large-scale structure and models of galaxy intrinsic alignments as contaminants for cosmic shear surveys. We measure strong alignments between halos of all masses and the surrounding dark matter overdensities out to several tens of Mpc/h, in agreement with observed shear-galaxy and cluster shape correlations. We use these measurements to forecast the contribution to the weak lensing signal around galaxy clusters from correlated mass along the line-of-sight. For prolate clusters with major axes aligned with the line-of-sight the fraction of the weak lensing signal from mass external to the cluster can be twice that predicted if the excess halo alignment correlation is assumed to be zero.", "label": 1, "domain": "academic", "token_count": 322, "matched_pair_id": "conditionality_00390", "split": "train"}
{"id": "conditionality_train_pos_0431", "text": "If any streetwise academic desires to pitch into the world of “perception and deception,” there’s good news: Carleton University in Ottawa has conjured a position just for you. The university is hiring someone to establish a research and teaching program in the “conjuring arts” for graduates and undergraduates. “It is a very opportune time to have somebody like this because we’re experiencing people doing all kinds of things that are deceptive, you know,” said the school’s interim president Alastair Summerlee. “They persuade lots of people and we really don’t understand how people can be drawn into those things, so this creates an opportunity to look at that.” Whoever fills the role will have to dig in and find out what it is about our nature that makes people both good at deceiving and at being deceived. In other words, what makes deception work like magic? “Whether it’s fake news or whether it’s politicians convincing people,” Summerlee said a major theme will be “understanding something about the illusion that they created, how do they work?” So far, the Faculty of Arts and Social Science has received about 80 applicants from a variety of backgrounds, Summerlee said. The announcement is expected this summer. The chair position is named after Allan Slaight, who in addition to being one Canada’s richest people, has been an avid magic buff, even editing and helping to write a tome on the work of Stewart James, one of Canada’s most productive magicians. The job description asks Carleton’s resident sorcerer to game-plan aspects of the history of magic, the history of perception and, of course, to investigate perception and deception. Carleton is matching a $2 million grant from The Slaight Family Foundation for the new post. The money will cover everything from the chair’s salary and hiring graduates to travel to investigate magic archives around the world. Summerlee said a major task will be for the resident sorcerer to link the “enormous amount of information” that has been gathered and printed worldwide about magic, which he or she would do through a digital archive, he said. The chair position is for a five-year renewable term with the possibility of tenure. Summerlee said he wants people to explore, “what is it about our psyches that make us so gullible?” In an effort to figure out what magic can reveal about our beliefs, researchers at the University of London asked people to explain a magic trick where the solution is", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00670", "split": "train"}
{"id": "conditionality_train_pos_0432", "text": "The current paper answers an open question of abs/1007.2426 We say that a countable model M characterizes an infinite cardinal kappa, if the Scott sentence of M has a model in cardinality kappa, but no models in cardinality kappa plus. If M is linearly ordered by <, we will say that the linear ordering (M,<) characterizes kappa. It is known that if kappa is characterizable, then kappa plus is characterizable by a linear ordering. Also, if kappa is characterizable by a dense linear ordering with an increasing sequence of size kappa, then 2^kappa is characterizable. We show that if kappa is homogeneously characterizable, then kappa is characterizable by a dense linear ordering, while the converse fails. The main theorems are: 1) If kappa>2^lambda is a characterizable cardinal, lambda is characterizable by a dense linear ordering and lambda is the least cardinal such that kappa^lambda>kappa, then kappa^lambda is also characterizable, 2) if aleph_alpha and kappa^(aleph_alpha) are characterizable cardinals, then the same is true for kappa^(aleph_(alpha+beta)), for all countable beta. Combining these two theorems we get that if kappa>2^(aleph_alpha) is a characterizable cardinal, aleph_alpha is characterizable by a dense linear ordering and aleph_alpha is the least cardinal such that kappa^(aleph_alpha)>kappa, then for all beta<alpha+omega_1, kappa^(aleph_beta) is characterizable. Also if kappa is a characterizable cardinal, then kappa^(aleph_alpha) is characterizable, for all countable alpha.", "label": 1, "domain": "academic", "token_count": 353, "matched_pair_id": "conditionality_00291", "split": "train"}
{"id": "conditionality_train_pos_0433", "text": "If you were lucky enough to unwrap a DSLR or mirrorless camera kit this holiday season, you’re probably excited (and owe somebody a big thank you). But if this is your first interchangeable lens camera (ILC), you may also be unsure where things go from here. Such a camera is the centerpiece of an ecosystem of lenses and other accessories that can be as confusing as they are desirable. But before you begin adding to your kit, it’s important to know what you really want. It’s equally important to understand your current gear and what it can and can’t do. We’ve compiled a short list of next steps for the first-time DSLR or mirrorless camera owner. This list is by no means exhaustive, but it may help point you in the right direction toward a rewarding journey into the world of photography. Study and practice Bill Roberson/Digital Trends Regardless of your camera, you will get more out of it by improving your skill rather than trying to buy better gear. Today’s cameras are like supercomputers with a lens attached, and they can do much more than simply point and take a picture. Reading the manual – yes, we know it’s boring – is probably the best way to get acquainted with your particular camera’s features and controls, but it’s also worth looking elsewhere for general knowledge on photography and how cameras work. An ILC lets you control the various exposure settings. If you’re looking for a quick guide, we have one. We also recommend Bryan Peterson’s book, Understanding Exposure, which has been the go-to guide for beginning photographers for the past two-and-a-half decades. In it, you’ll learn how to take control over your camera – rather than relying on its autoexposure mode – and create better pictures as a result. Related: Get pro-quality photos with your pop-up flash by using a white balloon If book learning isn’t your thing, there are ample online video courses for studying anything from the basics of exposure to how to run a photography business. CreativeLive and Lynda.com offer a wealth of knowledge on these topics. There is also plenty of free educational content on YouTube, with channels like the Cooperative of Photography (COOPH) offering creative tips and tricks and The Camera Store TV providing more gear-centric knowledge. But nothing is more helpful than simply getting out there and shooting. Take photos of your dog, bring you camera on a hike, or ask your significant other to (begrudgingly) pose for you.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00719", "split": "train"}
{"id": "conditionality_train_pos_0434", "text": "We propose a simple model for dark energy useful for comparison with observations. It is based on the idea that dark energy and inflation should be caused by the same physical process. As motivation, we note that Linde's simple chaotic inflation $V=(1/2)m^{2}\\phi^{2}$ produces values of $n_{s}=0.967$ and $r=0.13$, which are consistent with the WMAP 1-sigma error bars. We therefore propose $V=(1/2)m_{2}^{2}\\phi_{2}^{2}+(1/2)m_{1}^{2}\\phi_{1}^{2}$ with $m_{1}\\sim10^{-5}$ and $m_{2}\\leq10^{-60}$, where $c=1=\\hbar$ and the reduced Planck mass is set to unity. The field $\\phi_{1}$ drives inflation and has damped by now ($\\phi_{1,0}=0$), while $\\phi_{2}$ is currently rolling down its potential to produce dark energy. Using this model, we derive the formula $\\delta w(z)\\equiv w(z)+1=\\delta w_{0}(H_0/H(z))^2$ via the slow-roll approximation. Our numerical results from exact and self-consistent solution of the equations of motion for $\\phi_2$ and the Friedmann equations support this formula, and it should hold for any slow-roll dark energy. Our potential can be easily realized in N-flation models with many fields, and is easily falsifiable by upcoming experiments -- for example, if Linde's chaotic inflation is ruled out. But if $r$ values consistent with Linde's chaotic inflation are detected then one should take this model seriously indeed.", "label": 1, "domain": "academic", "token_count": 362, "matched_pair_id": "conditionality_00280", "split": "train"}
{"id": "conditionality_train_pos_0435", "text": "An EMT revealed a poignant detail Friday in the police shooting death of emotionally disturbed Bronx woman Deborah Danner — testifying that he’d been about to move her to safety moments before shots rang out. Danner had calmed down and was seated on her bed as EMT Patrick Moore left the bedroom to get a chair in which to transport her out of her castle Hill apartment, he testified. Suddenly, a half-dozen cops rushed past him into the bedroom, he testified. “I heard a lot of commotion,” Moore said. “I heard yelling, ‘Get down!’ I heard the word ‘bat,’ he added. Defendant Sgt. Hugh Barry has contended through his lawyer that he shot the schizophrenic Danner, 66, as she swung a bat at him. “Then I heard gunshots,” Moore said. He heard Danner let out one scream, he said. Inside the bedroom, the dying woman was “Lying on the bed … unconscious,” he said. “There was blood spewing out of her left chest and her left arm was mangled,” he said. “The patient was taking her last agonal respirations,” he said, using the medical terms for her deep, dying breaths. There was no pulse, he said — and instead of the chair he’d intended to transport her in, Moore and his fellow EMTs carried the near-dead woman from the apartment in a stretcher. Prosecution testimony is slated to continue Monday before Bronx Supreme Court Justice Robert Neary, who is presiding over the non-jury trial. Barry faces up to life in prison if convicted of murder.", "label": 1, "domain": "news", "token_count": 331, "matched_pair_id": "conditionality_00819", "split": "train"}
{"id": "conditionality_train_pos_0436", "text": "If you are age 45 to 79, ask your PCP if you should take aspirin ever day to help lower your risk of a heart attack. Mammogram: If you are age 45 to 54, get a screening every 1 to 2 years. Talk with your PCP about your personal risk factors, together you can decide when you should start getting mammograms and how often. @ 50 years of age Colorectal Cancer: If you are age 50 to 75, get tested for colorectal cancer. You and your PCP can decide which test is best. If you have a family history of colorectal cancer, you may need to be tested before you turn 50. @ 60 years of age Vision Disorders: Starting at age 60 (age 40 if you are African American), have a full eye exam with dilated pupils at least every 2 years. This will check for glaucoma and other eye problems. If you have diabetes, you should have an eye exam each year no matter what age you are. Talk to your primary care provider (PCP) about how to prioritize preventive health screenings, and the frequency in which you should schedule them based on risk factors associated with your family history and age. About AmeriHealth Caritas AmeriHealth Caritas is part of the Independence Health Group in partnership with Blue Cross Blue Shield of Michigan. AmeriHealth Caritas is one of the nation’s leaders in health care solutions for those most in need. Operating in 16 states and the District of Columbia, AmeriHealth Caritas serves approximately 5.6 million Medicaid, Medicare and Children’s Health Insurance Program (CHIP) members through its integrated managed care products, pharmaceutical benefit management and specialty pharmacy services, behavioral health services, and other administrative services. Headquartered in Philadelphia, AmeriHealth Caritas is a mission-driven organization with more than 35 years of experience serving low-income and chronically ill populations. For more information, visit www.amerihealthcaritas.com. View source version on businesswire.com:https://www.businesswire.com/news/home/20180530006422/en/ CONTACT: AmeriHealth Caritas Jawanza Keita, 267-298-5702 jkeita@amerihealthcaritas.com KEYWORD: UNITED STATES NORTH AMERICA PENNSYLVANIA INDUSTRY KEYWORD: WOMEN HEALTH CONSUMER GENERAL HEALTH SOURCE: AmeriHealth Caritas Copyright", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00509", "split": "train"}
{"id": "conditionality_train_pos_0437", "text": "the year the percentage of such professionals employed by such agency to furnish primary care services who during such previous year completed 6 credits of continuing medical education courses relating to nutrition (as described in subsection (c)). (c) Continuing Medical Education Relating to Nutrition.--For purposes of subsections (a) and (b), continuing medical education courses relating to nutrition shall include at least courses on the role of nutrition in the prevention, management, and, as possible, reversal of obesity, cardiovascular disease, diabetes, and cancer. (d) Definitions.--For purposes of this Act: (1) Primary care health professional.--The term ``primary care health professional'' means a physician or nurse practitioner who furnishes primary care services. (2) Nurse practitioner.--The term ``nurse practitioner'' has the meaning given such term in section 1861(aa)(5) of the Social Security Act (42 U.S.C. 1395x(aa)(5)). (3) Physician.--The term ``physician'' has the meaning given such term in section 1861(r)(1) of the Social Security Act (42 U.S.C. 1395x(r)(1)). (4) Primary care services.--The term ``primary care services'' has the meaning given such term in section 1842(i)(4) of the Social Security Act (42 U.S.C. 1395u(i)(4)), but shall include such services furnished by a nurse practitioner as would otherwise be included if furnished by a physician.", "label": 1, "domain": "government", "token_count": 305, "matched_pair_id": "conditionality_01034", "split": "train"}
{"id": "conditionality_train_pos_0438", "text": "AIMS: We present the optical classification and redshift of 348 X-ray selected sources from the XMM-Newton Bright Serendipitous Survey (XBS) which contains a total of 400 objects (identification level = 87%). About 240 are new identifications. In particular, we discuss in detail the classification criteria adopted for the Active Galactic Nuclei population. METHODS: By means of systematic spectroscopic campaigns and through the literature search we have collected an optical spectrum for the large majority of the sources in the XBS survey and applied a well-defined classification ``flow-chart''. RESULTS: We find that the AGN represent the most numerous population at the flux limit of the XBS survey (~10^-13 erg cm^-2 s^-1) constituting 80% of the XBS sources selected in the 0.5-4.5 keV energy band and 95% of the ``hard'' (4.5-7.5 keV) selected objects. Galactic sources populate significantly the 0.5-4.5 keV sample (17%) and only marginally (3%) the 4.5-7.5 keV sample. The remaining sources in both samples are clusters/groups of galaxies and normal galaxies (i.e. probably not powered by an AGN). Furthermore, the percentage of type2 AGN (i.e. optically absorbed AGNs with A_V>2mag) dramatically increases going from the 0.5-4.5 keV sample (f=N_AGN2/N_AGN=7%) to the 4.5-7.5 keV sample (f=32%). We finally propose two simple diagnostic plots that can be easily used to obtain the spectral classification for relatively low redshift AGNs even if the quality of the spectrum is not good.", "label": 1, "domain": "academic", "token_count": 372, "matched_pair_id": "conditionality_00023", "split": "train"}
{"id": "conditionality_train_pos_0439", "text": "If you were walking the exhibition hangars at Sun ‘n Fun last week, you might have come across Hangarswap.com, and its creator, pilot and aviation entrepreneur Rachel Payne. What she’s up to with her site, hangarswap.com, is cool, but it could be a lot more than that, too. Payne, a hot-pink haired ball of enthusiasm for aviation, got into the airplane business when she was just 15 years old by selling used plane parts on eBay. She has turned that part time high school job into a mini empire. Her salvage yard near Orlando, Florida, is a must-visit destination for those hard-to-find parts for our GA aircraft. But for the past couple of years, Payne has been promoting a whole new kind of online experience. After getting frustrated by eBay’s high commission (10 percent and a max of $750 per sale), Payne decided to start her own dedicated auction site, hangarswap.com, that’s just now getting a facelift. The site charges only five percent commission, it has a max fee of $300 per transaction, and when you search for “Beechcraft,” it doesn’t autocorrect it to “Beach House.” Payne also insists on opening the flow of conversation among hangarswap.com buyers and sellers, a practice that eBay controls for fear of losing commissions to direct sales between the buyers and sellers. This allows easy exchange of questions and answers between the parties, so there are fewer misunderstandings, says Payne. Being smaller, Rachel and her friendly staff can also help arbitrate disputes, though she says that because her crowd is friendlier and more knowledgeable than the typical eBayers, there’s usually not much to arbitrate. Unlike eBay, hangarswap.com is run by airplane nuts, including Payne, who currently flies a Cessna 210. She admits to being a bit of a packrat when it comes to things like plane parts, vintage motorcycles and funky art, though she denies she has a problem. Her motto, and that of hangarswap.com, says it all, “It’s not hoarding if your stuff is cool.” Amen.", "label": 1, "domain": "news", "token_count": 437, "matched_pair_id": "conditionality_00779", "split": "train"}
{"id": "conditionality_train_pos_0440", "text": "The study of the broad-band emission of GHz-Peaked-Spectrum (GPS) radio galaxies is a powerful tool to investigate the physical processes taking place in the central, kpc-sized region of their active hosts, where the jets propagate and the lobes expand, interacting with the surrounding interstellar medium (ISM). We recently developed a new dynamical-radiative model to describe the evolution of the GPS phenomenon (Stawarz et al. 2008): as the relativistic jets propagate through the ISM, gradually engulfing narrow-line emitting gas clouds along their way, the electron population of the expanding lobes evolves, emitting synchrotron light, as well as inverse-Compton radiation via up-scattering of the photon fields from the host galaxy and its active nucleus. The model, which successfully reproduces the key features of the GPS radio sources as a class, provides a description of the evolution of their spectral energy distribution (SED) with the lobes' expansion, predicting significant and complex X-ray to gamma-ray emission. We apply here the model to the broad-band SED's of a sample of known, X-ray emitting GPS galaxies, and show that: (i) the free-free absorption mechanism enables us to reproduce the radio continuum at frequencies below the turnover; (ii) the lobes' non-thermal, inverse-Compton emission can account for the observed X-ray spectra, providing a viable alternative to the thermal, accretion-dominated scenario. We also show that, in our sample, the relationship between the X-ray and radio hydrogen column densitities, N_H and N_HI, is suggestive of a positive correlation, which, if confirmed, would support the scenario of high-energy emitting lobes.", "label": 1, "domain": "academic", "token_count": 350, "matched_pair_id": "conditionality_00098", "split": "train"}
{"id": "conditionality_train_pos_0441", "text": "We consider the Casimir effect of the electromagnetic field in a higher dimensional spacetime of the form $M\\times \\mathcal{N}$, where $M$ is the 4-dimensional Minkowski spacetime and $\\mathcal{N}$ is an $n$-dimensional compact manifold. The Casimir force acting on a planar piston that can move freely inside a closed cylinder with the same cross section is investigated. Different combinations of perfectly conducting boundary conditions and infinitely permeable boundary conditions are imposed on the cylinder and the piston. It is verified that if the piston and the cylinder have the same boundary conditions, the piston is always going to be pulled towards the closer end of the cylinder. However, if the piston and the cylinder have different boundary conditions, the piston is always going to be pushed to the middle of the cylinder. By taking the limit where one end of the cylinder tends to infinity, one obtains the Casimir force acting between two parallel plates inside an infinitely long cylinder. The asymptotic behavior of this Casimir force in the high temperature regime and the low temperature regime are investigated for the case where the cross section of the cylinder in $M$ is large. It is found that if the separation between the plates is much smaller than the size of $\\mathcal{N}$, the leading term of the Casimir force is the same as the Casimir force on a pair of large parallel plates in the $(4+n)$-dimensional Minkowski spacetime. However, if the size of $\\mathcal{N}$ is much smaller than the separation between the plates, the leading term of the Casimir force is $1+h/2$ times the Casimir force on a pair of large parallel plates in the 4-dimensional Minkowski spacetime, where $h$ is the first Betti number of $\\mathcal{N}$. In the limit the manifold $\\mathcal{N}$ vanishes, one does not obtain the Casimir force in the 4-dimensional Minkowski spacetime if $h$ is nonzero.", "label": 1, "domain": "academic", "token_count": 418, "matched_pair_id": "conditionality_00311", "split": "train"}
{"id": "conditionality_train_pos_0442", "text": "We present new B, V and I CCD time-series photometry for 177 variable stars in a 13'X 13' field centered on the globular cluster M54 (lying at the center of the Sagittarius dwarf spheroidal galaxy), 94 of which are newly identified variables. The total sample is composed of 2 anomalous Cepheids, 144 RR Lyrae stars (108 RR0 and 36 RR1), 3 SX Phoenicis, 7 eclipsing binaries (5 W UMA and 2 Algol binaries), 3 variables of uncertain classification and 18 long-period variables. The large majority of the RR Lyrae variables likely belong to M54. Ephemerides are provided for all the observed short-period variables. The pulsational properties of the M54 RR Lyrae variables are close to those of Oosterhoff I clusters, but a significant number of long-period ab type RR Lyrae are present. We use the observed properties of the RR Lyrae to estimate the reddening and the distance modulus of M54, E(B-V)=0.16 +/- 0.02 and (m-M)_0=17.13 +/- 0.11, respectively, in excellent agreement with the most recent estimates. The metallicity has been estimated for a subset of 47 RR Lyrae stars, with especially good quality light curves, from the Fourier parameters of the V light curve. The derived metallicity distribution has a symmetric bell shape, with a mean of <[Fe/H]>=-1.65 and a standard deviation sigma=0.16 dex. Seven stars have been identified as likely belonging to the Sagittarius galaxy, based on their too high or too low metallicity. This evidence, if confirmed, might suggest that old stars in this galaxy span a wide range of metallicities.", "label": 1, "domain": "academic", "token_count": 381, "matched_pair_id": "conditionality_00207", "split": "train"}
{"id": "conditionality_train_pos_0443", "text": "In decision problems, often, utilities and probabilities are hard to determine. In such cases, one can resort to so-called choice functions. They provide a means to determine which options in a particular set are optimal, and allow incomparability among any number of options. Applying choice functions in sequential decision problems can be highly non-trivial, as the usual properties of maximising expected utility may no longer be satisfied. In this paper, we study one of these properties: we revisit and reinterpret Selten's concept of subgame perfectness in the context of decision trees, leading us to the concept of subtree perfectness, which basically says that the optimal solution of a decision tree should not depend on any larger tree it may be embedded in. In other words, subtree perfectness excludes counterfactual reasoning, and therefore may be desirable from some philosophical points of view. Subtree perfectness is also desirable from a practical point of view, because it admits efficient algorithms for solving decision trees, such as backward induction. The main contribution of this paper is a very simple non-technical criterion for determining whether any given choice function will satisfy subtree perfectness or not. We demonstrate the theorem and illustrate subtree perfectness, or the lack thereof, through numerous examples, for a wide variety of choice functions, where incomparability amongst strategies can be caused by imprecision in either probabilities or utilities. We find that almost no choice function, except for maximising expected utility, satisfies it in general. We also find that choice functions other than maximising expected utility can satisfy it, provided that we restrict either the structure of the tree, or the structure of the choice function.", "label": 1, "domain": "academic", "token_count": 330, "matched_pair_id": "conditionality_00486", "split": "train"}
{"id": "conditionality_train_pos_0444", "text": "We calculate the emission line spectrum produced by the debris released when a white dwarf (WD) is tidally disrupted by an intermediate-mass black hole (IMBH; $M\\sim 10^{2}-10^{5}\\msun$) and we explore the possibility of using the emission lines to identify such events and constrain the properties of the IMBH. To this end, we adopt and adapt the techniques developed by Strubbe & Quataert to study the optical emission lines produced when a main sequence (MS) star is tidally disrupted by a supermassive black hole. WDs are tidally disrupted outside of the event horizon of a $< 10^{5}\\msun$ black hole, which makes these tidal disruption events good signposts of IMBHs. We focus on the optical and UV emission lines produced when the accretion flare photoionizes the stream of debris that remains unbound during the disruption. We find that the spectrum is dominated by lines due to ions of C and O, the strongest of which are \\ion{C}{4} $\\lambda$1549 at early times and [\\ion{O}{3}] $\\lambda$5007 at later times. Furthermore, we model the profile of the emission lines in the [\\ion{O}{3}] $\\lambda\\lambda$4959, 5007 doublet and find that it is highly asymmetric with velocity widths of up to $\\sim 2500 \\rm{\\;km\\;s^{-1}}$, depending on the properties of the WD-IMBH system and the orientation of the observer. Finally, we compare the models with observations of X-ray flares and optical emission lines in the cores of globular clusters and propose how future observations can test if these features are due to a WD that has been tidally disrupted by an IMBH.", "label": 1, "domain": "academic", "token_count": 374, "matched_pair_id": "conditionality_00275", "split": "train"}
{"id": "conditionality_train_pos_0445", "text": "Context. After the launch of the Swift satellite, the Gamma-Ray Burst (GRB) optical light-curve smoothness paradigm has been questioned thanks to the faster and better sampled optical follow-up, which has unveiled a very complex behaviour. This complexity is triggering the interest of the whole GRB community. The GROND multi-channel imager is used to study optical and near-infrared (NIR) afterglows of GRBs with unprecedented optical and near-infrared temporal and spectral resolution. The GRB 081029 has a very prominent optical rebrightening event and is an outstanding example of the application of the multi-channel imager to GRB afterglows. Aims. Here we exploit the rich GROND multi-colour follow-up of GRB 081029 combined with XRT observations to study the nature of late-time rebrightenings that appear in the optical-NIR light-curves of some GRB afterglows. Methods. We analyse the optical and NIR observations obtained with the seven-channel Gamma-Ray burst Optical and Near-infrared Detector (GROND) at the 2.2 m MPI/ESO telescope and the X-ray data obtained with the XRT telescope on board the Swift observatory. The multi-wavelength temporal and spectral evolution is discussed in the framework of different physical models. Results. The extremely steep optical and NIR rebrightening observed in GRB 081029 cannot be explained in the framework of the standard forward shock afterglow model. The absence of a contemporaneous X-ray rebrightening and the evidence of a strong spectral evolution in the optical-NIR bands during the rise suggest two separate components that dominate in the early and late-time lightcurves, respectively. The steepness of the optical rise cannot be explained even in the framework of the alternative scenarios proposed in the literature unless a late-time activity of the central engine is assumed.", "label": 1, "domain": "academic", "token_count": 378, "matched_pair_id": "conditionality_00328", "split": "train"}
{"id": "conditionality_train_pos_0446", "text": "if clause (i) does not apply, a portion of such dividend shall be treated as interest on a public benefit bond based on the portion of the company's gross income which consists of such interest. ``(B) Notice to shareholders.--The amount of any distribution by a regulated investment company which may be taken into account as interest on a public benefit bond for purposes of this section shall not exceed the amount so designated by the company in a written notice to its shareholders mailed not later than 45 days after the close of its taxable year. ``(C) Gross income.--For purposes of this section, the term `gross income' does not include gain from the sale or other disposition of stock or securities. ``(7) Definitions.--In this section, the following definitions apply: ``(A) Entity.--The term `entity' means an individual, corporation, partnership, joint venture, trust or governmental entity or instrumentality. ``(B) Infrastructure facility.--The term `infrastructure facility' means a road, highway, bridge, tunnel, airport, mass transportation vehicle or system, passenger rail vehicle or system, intermodal transportation facility, waterway, commercial port, drinking or waste water treatment facility, solid waste disposal facility, pollution control system, hazardous waste facility, federally designated national information highway facility, school, and any ancillary facility which forms a part of any such facility or is reasonably related to such facility, whether owned, leased or operated by a public entity or a private entity or by a combination of such entities, and the financing or refinancing of the development of which is, or will be, supported in whole or in part by user fees or other dedicated revenue sources. ``(C) Public-private partnership.--The term `public-private partnership' means any entity-- ``(i) which is undertaking the development of all or part of any infrastructure facility-- ``(I) pursuant to requirements established in 1 or more contracts between such entity and a State or an instrumentality of a State, or ``(II) the activities of which with respect to such facility are subject to regulation by a State or any instrumentality of a State, and ``(ii) which owns, leases, or operates, or will own, lease, or operate, such infrastructure facility in whole or in part, and at least 1 of the participants in such entity is a nongovernmental entity.''. (b) Conforming Amendment.--Subsection (w) of section 72 of the Internal Revenue Code of 1986", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01038", "split": "train"}
{"id": "conditionality_train_pos_0447", "text": "The theoretical need to study the properties of the Fe-based high-T_c superconductors with reliable many-body techniques requires us to determine the minimum number of orbital degrees of freedom that will capture the physics of these materials. While the shape of the Fermi surface (FS) obtained with the local density approximation (LDA) can be reproduced by a two-orbital model, it has been argued that the bands that cross the chemical potential result from the strong hybridization of three of the Fe 3d orbitals. For this reason, a three-orbital Hamiltonian obtained with the Slater-Koster formalism by considering the hybridization of the As p orbitals with the Fe d_xz,d_yz, and d_xy orbitals is discussed here. This model reproduces qualitatively the FS shape and orbital composition obtained by LDA calculations for undoped pnictides when four electrons per Fe are considered. Within a mean-field approximation, its magnetic and orbital properties in the undoped case are described. With increasing Coulomb repulsion, four regimes are obtained: (1) paramagnetic, (2) magnetic (pi,0) spin order, (3) the same (pi,0) spin order but now including orbital order, and finally (4) a magnetic and orbital ordered insulator. The spin-singlet pairing operators allowed by the lattice and orbital symmetries are also constructed. It is found that for pairs of electrons involving up to diagonal nearest-neighbors sites, the only fully gapped and purely intraband spin-singlet pairing operator is given by Delta(k)=f(k)\\sum_{alpha} d_{k,alpha,up}d_{-k,alpha,down} with f(k)=1 or f(k)=cos(k_x)cos(k_y) which would arise only if the electrons in all different orbitals couple with equal strength to the source of pairing.", "label": 1, "domain": "academic", "token_count": 385, "matched_pair_id": "conditionality_00167", "split": "train"}
{"id": "conditionality_train_pos_0448", "text": "To construct a Paley graph, we fix a finite field and consider its elements as vertices of the Paley graph. Two vertices are connected by an edge if their difference is a square in the field. We will study some important properties of the Paley graphs. In particular, we will show that the Paley graphs are connected, symmetric, and self-complementary. Also we will show that the Paley graph of order q is (q-1)/2 -regular, and every two adjacent vertices have (q-5)/4 common neighbors, and every two non-adjacent vertices have q-1/4 common neighbors, which means that the Paley graphs are strongly regular with parameters(q,q-1/2,q-5/4, q-1/4). Paley graphs are generalized by many mathematicians. In the first section of Chapter 3 we will see three examples of these generalizations and some of their basic properties. In the second section of Chapter 3 we will define a new generalization of the Paley graphs, in which pairs of elements of a finite field are connected by an edge if and only if there difference belongs to the m-th power of the multiplicative group of the field, for any odd integer m > 1, and we call them the m-Paley graphs. In the third section we will show that the m-Paley graph of order q is complete if and only if gcd(m, q - 1) = 1 and when d = gcd(m, q - 1) > 1, the m-Paley graph is q-1/d -regular. Also we will prove that the m-Paley graphs are symmetric but not self-complementary. We will show also that the m-Paley graphs of prime order are connected but the m-Paley graphs of order p^n, n > 1 are not necessary connected, for example they are disconnected if gcd(m, p^n - 1) =(p^n-1)/ 2.", "label": 1, "domain": "academic", "token_count": 406, "matched_pair_id": "conditionality_00426", "split": "train"}
{"id": "conditionality_train_pos_0449", "text": "If the credit allowable under subsection (a) for a taxable year exceeds the amount of the limitation under subsection (f)(1) for such taxable year (in this paragraph referred to as the `unused credit year'), such excess shall be a credit carryback to each of the 3 taxable years preceding the unused credit year and a credit carryforward to each of the 20 taxable years following the unused credit year. ``(B) Rules.--Rules similar to the rules of section 39 shall apply with respect to the credit carryback and credit carryforward under subparagraph (A). ``(6) Certain rules to apply.--Rules similar to the rules of subsections (c), (d), and (e) of section 52 shall apply.''. (b) Conforming Amendment.--Section 55(c)(2) of the Internal Revenue Code of 1986 is amended by inserting ``30B(f)(1),'' after ``30(b)(3),''. (c) Clerical Amendment.--The table of sections for subpart B of part IV of subchapter A of chapter 1 of the Internal Revenue Code of 1986 is amended by adding at the end 30A the following new item: ``Sec. 30B. Employer wage credit for activated military reservists.''. (d) Effective Date; Special Rule.-- (1) Effective date.--The amendments made by this section shall apply to amounts paid after September 11, 2001, in taxable years ending after such date. (2) Waiver of limitations.--If refund or credit of any overpayment of tax resulting from the amendments made by this section is prevented at any time before the close of the 1-year period beginning on the date of the enactment of this Act by the operation of any law or rule of law (including res judicata), such refund or credit may nevertheless be made or allowed if claim therefor is filed before the close of such period.", "label": 1, "domain": "government", "token_count": 392, "matched_pair_id": "conditionality_00923", "split": "train"}
{"id": "conditionality_train_pos_0450", "text": "Let $G$ be a permutation group acting on $[n]=\\{1, ..., n\\}$ and $\\mathcal{V}=\\{V_{i}: i=1, ..., n\\}$ be a system of $n$ subsets of $[n]$. When is there an element $g \\in G$ so that $g(i) \\in V_{i}$ for each $i \\in [n]$? If such $g$ exists, we say that $G$ has a $G$-marriage subject to $\\mathcal{V}$. An obvious necessary condition is the {\\it orbit condition}: for any $\\emptyset \\not = Y \\subseteq [n]$, $\\bigcup_{y \\in Y} V_{y} \\supseteq Y^{g}=\\{g(y): y \\in Y \\}$ for some $g \\in G$. Keevash (J. Combin. Theory Ser. A 111(2005), 289--309) observed that the orbit condition is sufficient when $G$ is the symmetric group $\\Sym([n])$; this is in fact equivalent to the celebrated Hall's Marriage Theorem. We prove that the orbit condition is sufficient if and only if $G$ is a direct product of symmetric groups. We extend the notion of orbit condition to that of $k$-orbit condition and prove that if $G$ is the alternating group $\\Alt([n])$ or the cyclic group $C_{n}$ where $n \\ge 4$, then $G$ satisfies the $(n-1)$-orbit condition subject to $\\V$ if and only if $G$ has a $G$-marriage subject to $\\mathcal{V}$.", "label": 1, "domain": "academic", "token_count": 362, "matched_pair_id": "conditionality_00184", "split": "train"}
{"id": "conditionality_train_pos_0451", "text": "If laughter is the best medicine, then standup veteran Mike MacDonald was a healer in the minds of many Canadian comedians. Members of Canada’s comedy scene were remembering MacDonald on Monday, not only for his ability to bring down the house with laughter, but also for the way broke down barriers by making wisecracks about his struggles with drug addiction, mental health and liver damage. MacDonald died Saturday of heart complications at the Ottawa Heart Institute, according to his brother J.P. MacDonald. He was 62. “There was always some kind of lesson buried in his comedy,” said J.P. MacDonald, who is also known by his stage name Johnny Vegas. “It was more about the message, and sort of wrapping it in a joke.” After kicking a drug problem, Mike MacDonald started joking on stage about his struggles with bipolar disorder around the early 1990s, his brother said. J.P. MacDonald said the decision temporarily deflated Mike’s career, but the comic “groundbreaker” persisted in using jokes as a vehicle to dismantle the stigma surrounding mental illness. David Granirer, founder of Stand Up For Mental Health, said Mike MacDonald headlined shows across the country to support the organization that teaches people with mental illness to perform comedy. Granirer said MacDonald would spend hours after his shows helping amateur comedians hone their humorous takes on personal hardship, a technique he helped pioneer. “Mike’s legacy is that he opened the door for a lot of other people to talk about mental health through their comedy acts,” he said. “Just the fact that someone with his stature was doing it certainly … inspired (our comics) to be able to tell their stories in a more direct way.” Coming up in Ottawa comedy clubs, comedian Ben Miner said MacDonald was a hometown hero and often credited as Canada’s first standup star, having appeared on the “Late Show with David Letterman” and the “Arsenio Hall Show” as well as several CBC and Showtime specials. While MacDonald had a larger-than-life presence on the stage, Miner said his ability to be vulnerable allowed him to connect with audiences on a deeper level, and in some cases, even help save lives. Miner, 37, pointed to a 2016 interview in which MacDonald told CBC’s “Mainstreet P.E.I.” that a member of the audience approached him after a show to tell him he had decided against committing suicide after laughing at the comedian’s jokes on the subject. “You’re never", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00673", "split": "train"}
{"id": "conditionality_train_pos_0452", "text": "if you are unable to critique the President, you've lost your prophetic witness, Christian. And, that’s a tragedy. We need to be free to critique any politician, president, or pundit when their actions are divisive, unjust, or unhelpful. Why? Because we are Christians. Prophetic Witness I don’t think everyone needs to speak up on everything, but I’m talking about those who defend that which Trump saw that he needed to correct— with him (finally) condemning racism in this instance. Christians have a prophetic witness, but we can lose that witness when we are unable to see (or speak to) the errors or failings of leaders. And, if Christians feel the need to defend even an obvious and divisive mistake (and my Twitter feed is filled with those people), they hurt the church’s witness and tying it to closely to a person, not the truth. Now, if that’s your job in the White House, I get it. You have to defend everything. But, if Christians do, it shows the world that our loyalty is to the person in the White House rather than the Person who said He is the Truth. If you are a Christian, you need to speak out against error, injustice, and the depraved strategy of silence. Many did, some said nothing, but some went to the defense of something the President two days later felt the need to correct. If you’re a Christian who thinks that President Trump can do no wrong, you’re giving the message that he’s the savior. He’s not. He is fallible, human, and makes mistakes that we, as responsible Christians and members of Christ’s household, should not be afraid to address. So, rather than defending his error, which he, himself, felt the need to correct today, search your heart and ask, have I become too connected to a secular leader? There are many godly Christians, committed to Christ and His work, who voted for and supported President Trump. They had two choices and chose now-President Trump. And, I am thankful for some of the choices and policies he has made. But, I can, must, and will critique him when his lack of words divides the nation as they did this week. As I tweeted, if you are a Christian Trump supporter, but cannot critique him when he is wrong, the world is watching and sees your primary loyalty. Furthermore, if you can’t critique, but must also defend", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00829", "split": "train"}
{"id": "conditionality_train_pos_0453", "text": "So it's a watch then, in look and feel. What it does over and above a standard £80 Timex is step and distance counting and stopwatch or timer alerts. If you’re after phone notifications, apps or GPS tracking, that’s not the Timex IQ+ Move’s bag. When you boot-up the Timex app you get to choose whether the little extra dial displays how close you are to either reaching your distance or steps goal for the day. The seconds hand can take on the same task if you don’t need the time to the second, and it can display the date too. Look carefully and you’ll see a little “1” just after the 12 o’ clock mark and a “31” just after the 6 o’ clock spot, denoting the days of the month. Subtle, right? Sure, in tech terms this is about as flashy as an abacus, but you have to appreciate how low-key it all is. You get a fitness tracker geek-out on the sly. Another neat hidden feature is the night light. Press the crown for a second and the whole screen glows blue thanks to some hidden LEDs behind it. You won’t be able to see the effects in daylight, but it means you can at least see the time in the dark. As with any fitness tracker worn on your wrist, you’re not going to judge your marathon training off the Timex IQ+ Move’s step counts. But if you find its readings way off you can set the app to nudge the totals up and down. That said, it’s been within perfectly normal reading bounds for me, so if you have an issue it may be because your gesticulate wildly with every syllable you speak.", "label": 1, "domain": "news", "token_count": 351, "matched_pair_id": "conditionality_00693", "split": "train"}
{"id": "conditionality_train_pos_0454", "text": "In South San Francisco right now, engineers are growing diamonds. We are not talking cubic zirconia - these are real diamonds. The manmade gems are virtually identical to diamonds mined from deep in the earth.High tech is now transforming high-end jewelry and a number of bay area businesses are early adopters.Husband and wife team Lindsay Reinsmith and Jason Payne started learning about manmade diamonds when they got engaged five years ago.Reinsmith did not want a traditional diamond because of the difficulty of tracking its origin. She wanted to be sure no environmental damage or human rights issues were associated with the gemstones in her engagement ring.Eventually, she and Payne settled on man-made diamonds, but they were hard to find - so the couple decided to start their own business.A few months ago they launched Ada Diamonds , an on-line business based in Sunnyvale. They sell custom jewelry using man-made diamonds.Sophisticated equipment can now grow gem quality diamonds in just a few weeks. \"It's a paragon of human achievement that we can recreate the conditions with which carbon becomes diamond\" according to Payne.Ada Diamonds sells diamonds grown in several different laboratories. Advances in technology now allow labs to grow diamonds in a wide range of colors and sizes.But is a diamond grown in a lab real? Brenda Harwick with the Gemological Institute of America says yes. Lab diamonds \"have the same physical, chemical and optical properties as a natural diamond that's grown in the earth over billions of years\" according to Harwick.Prices for manmade diamonds are generally 20 to 40 percent less than mined diamonds. But Martin Roscheisen of the Diamond Foundry in South San Francisco says it actually costs more to grow a diamond in a lab than to dig it out of the ground. Roscheisen says growing diamonds is extremely difficult which is why companies like his keep the exact details secret. Brilliant Earth in San Francisco sells both diamonds that are certified as \"ethically mined\" and lab grown diamonds. The lab diamonds are still just a tiny slice of the business, but interest is growing.Kathryn Money with Brilliant Earth says manmade gems are \"are resonating particularly well with millennials because they are beautiful, responsible and affordable.Lab-grown diamonds still have the same type of imperfections as mined diamonds. So if you are thinking of buying one, experts say you should get the same kind of independent certification that's available for natural diamonds.", "label": 1, "domain": "news", "token_count": 488, "matched_pair_id": "conditionality_00521", "split": "train"}
{"id": "conditionality_train_pos_0455", "text": "If you think the UniParty attacks upon President Trump are vitriolic now, just wait until President Trump presents his budget proposal to congress; that’s when the UniParty is really going to go bananas, and every crony-conservative pundit and radio talker will simultaneously demand Trump immediately spend more money. These politicians will demand more spending. Notice anything familiar about them? The federal fiscal year runs from October 1st to September 31st annually. The Budget and Accounting Act of 1921 requires the President to submit his budget request for the upcoming fiscal year no later than the first Monday of February. However, in the first year of the first term of each administration – congress waives the statutory deadline because so much of the election and campaign is structured around fiscal budget and tax policy. The waiver gives the incoming administration time to construct their budget after the inauguration. Historic reference: Year One Bill Clinton budget was delivered on 4/8/93 (66 days past deadline). Year One GW Bush budget was delivered on 4/9/01 (63 days past deadline). Year One Barack Obama budget was delivered on 5/11/09 (98 days past deadline). Currently President Trump is in the process of putting his budget together. Heck, the Senate hasn’t even confirmed Trump’s Office of Management and Budget (OMB) Director, Mick ‘Cantalopes‘ Mulvaney. But one thing is abundantly clear President Trump has already stated his expressed intention to bring the federal budget to balance within his first term. To comprehend the scope of this budgetary dynamic, consider the first four months of fiscal year 2017 (October 1, 2016 through Jan 31, 2017) which was just announced: ♦ Receipts through January totaled $1,084 billion [$1.08 trillion], CBO estimates—$5 billion more than the amount for the same period last year. ♦ Outlays for the first four months of fiscal year 2017 were $1,243 billion [$1.24 trillion], CBO estimates—$4 billion more than they were during the same period last year. If not for shifts in the timing of certain payments from October 2016 to September 2016 because October 1 fell on a weekend, outlays would have been $45 billion (or 4 percent) greater. The Federal Government took in a record $1.08 Trillion, and yet spent $1.24 Trillion", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00612", "split": "train"}
{"id": "conditionality_train_pos_0456", "text": "Massive stars form deeply embedded in dense molecular gas, which they stir and heat up and ionize. During an early phase, the ionization is confined to hypercompact HII regions, and the stellar radiation is entirely absorbed by dust, giving rise to a hot molecular core. To investigate the innermost structure of such high-mass star-forming regions, we observed vibrationally excited HCN (via the direct $\\ell$-type transition of v2=1, $\\Delta J$=0, J=13, which lies 1400 K above ground) toward the massive hot molecular cores G10.47+0.03, SgrB2-N, and SgrB2-M with the Very Large Array (VLA) at 7 mm, reaching a resolution of about 1000 AU (0.1\"). We detect the line both in emission and in absorption against HII regions. The latter allows to derive lower limits on the column densities of hot HCN, which are several times $10^{19}$ cm$^{-2}$. We see indication of expansion motions in G10.47+0.03 and detect velocity components in SgrB2-M at 50, 60, and 70 km/s relative to the Local Standard of Rest. The emission originates in regions of less than 0.1 pc diameter around the hypercompact HII regions G10.47+0.03 B1 and SgrB2-N K2, and reaches brightness temperatures of more than 200 K. Using the three-dimensional radiative transfer code RADMC-3D, we model the sources as dense dust cores heated by stars in the HII regions, and derive masses of hot (>300 K) molecular gas of more than 100 solar masses (for an HCN fractional abundance of 10$^{-5}$), challenging current simulations of massive star formation. Heating only by the stars in the HII regions is sufficient to produce such large quantities of hot molecular gas, provided that dust is optically thick to its own radiation, leading to high temperatures through diffusion of radiation.", "label": 1, "domain": "academic", "token_count": 427, "matched_pair_id": "conditionality_00314", "split": "train"}
{"id": "conditionality_train_pos_0457", "text": "The NSF has chosen the site for the Deep Underground Science and Engineering Laboratory (DUSEL) to be in Lead, South Dakota. In fact, the state of South Dakota has already stepped up to the plate and contributed its own funding for the proposed lab, see http://www.sanfordlaboratoryathomestake.org/index.html. The final decision by NSF for funding the Initial Suite of Experiments for DUSEL will be made early in 2009. At that time the NSF Science Board must make a decision. Of order 200 experimentalists have already expressed an interest in performing experiments at DUSEL. In order to assess the interest of the theoretical community, the Center for Cosmology and Astro-Particle Physics (CCAPP) at The Ohio State University (OSU) organized a 3-day DUSEL Theory Workshop in Columbus, Ohio from April 4 - 6, 2008. The workshop focused on the scientific case for six proposed experiments for DUSEL: long baseline neutrino oscillations, proton decay, dark matter, astrophysical neutrinos, neutrinoless double beta decay and N-Nbar oscillations. The outcome of this workshop is the DUSEL Theory White paper addressing the scientific case at a level which may be useful in the decision making process for policy makers at the NSF and in the U.S. Congress. In order to assess the physics interest in the DUSEL project we have posted the DUSEL Theory White paper on the following CCAPP link http://ccapp.osu.edu/whitepaper.html . Please read the white paper and, if you are interested, use the link to show your support by co-signing the white paper.", "label": 1, "domain": "academic", "token_count": 345, "matched_pair_id": "conditionality_00092", "split": "train"}
{"id": "conditionality_train_pos_0458", "text": "If you ask Bank of America Corp (ticker: BAC) shareholders how they feel about the past half-year or so, you're sure to get an answer that can only be described as \"hedged happiness.\" After all, BAC stock has run up some 35 percent since the November presidential election, running circles around the Standard & Poor's 500 index, which is up 12 percent since then. But the dual narrative of President Donald Trump's anti-regulation regime and Federal Reserve interest-rate hikes sending Bank of America to the moon hasn't quite materialized -- at least not nearly enough to match months' worth of hype. Bank of America, as a result, finds itself entering its first-quarter earnings report in a double-digit slide since its early March highs that has eaten all but 1 percent of its gains in 2017, versus a respectable 4 percent performance by the broader market. The question now is: What can BAC do to rekindle the kinds of go-go gains it earned in the \"Trump Bump\"? [See: 11 Ways to Buy Bank Stocks.] The headline numbers: Wall Street has some pretty optimistic views of what Bank of America will bring to the table for Tuesday's first-quarter earnings report. Revenues are expected to expand 9.6 percent from last year's quarter to $21.6 billion, while earnings should sprout by 25 percent to 35 cents per share. A beat should be... well, money in the bank. BAC has posted earnings beats for seven consecutive quarters, so it's managing expectations well on its own. But Wall Street also appears to have laid down a low bar for big-bank earnings this quarter. Citigroup ( C) and JPMorgan Chase & Co. ( JPM) beat first-quarter estimates by roughly 9 percent, and even beleaguered Wells Fargo & Co. ( WFC) managed to come in 3 percent ahead of the consensus mark. The flip side? Those three performances, all released last Thursday morning, were wasted as the U.S. dropped the \"mother of all bombs\" on Afghanistan in a strike against ISIS, sending markets (including bank stocks) into reverse. Bank of America's secret Is out: Citigroup analyst Keith Horowitz articulated the biggest problem for BAC shares going forward in an April 4 note: \"Since the election, BAC has outperformed and has substantially closed that gap with JPM.... We believe", "label": 1, "domain": "news", "token_count": 499, "matched_pair_id": "conditionality_00575", "split": "train"}
{"id": "conditionality_train_pos_0459", "text": "We consider the problem of obtaining sparse positional strategies for safety games. Such games are a commonly used model in many formal methods, as they make the interaction of a system with its environment explicit. Often, a winning strategy for one of the players is used as a certificate or as an artefact for further processing in the application. Small such certificates, i.e., strategies that can be written down very compactly, are typically preferred. For safety games, we only need to consider positional strategies. These map game positions of a player onto a move that is to be taken by the player whenever the play enters that position. For representing positional strategies compactly, a common goal is to minimize the number of positions for which a winning player's move needs to be defined such that the game is still won by the same player, without visiting a position with an undefined next move. We call winning strategies in which the next move is defined for few of the player's positions sparse. Unfortunately, even roughly approximating the density of the sparsest strategy for a safety game has been shown to be NP-hard. Thus, to obtain sparse strategies in practice, one either has to apply some heuristics, or use some exhaustive search technique, like ILP (integer linear programming) solving. In this paper, we perform a comparative study of currently available methods to obtain sparse winning strategies for the safety player in safety games. We consider techniques from common knowledge, such as using ILP or SAT (satisfiability) solving, and a novel technique based on iterative linear programming. The results of this paper tell us if current techniques are already scalable enough for practical use.", "label": 1, "domain": "academic", "token_count": 329, "matched_pair_id": "conditionality_00475", "split": "train"}
{"id": "conditionality_train_pos_0460", "text": "If nothing else, Donald Trump’s recent decision to recognize Jerusalem as Israel’s capital shows how disenthralled his administration is with traditional pieties about the Middle East. It’s about time. One piety is that “Mideast peace” is all but synonymous with Arab-Israeli peace. Seven years of upheaval, repression, terrorism, refugee crises and mass murder in Libya, Egypt, Yemen, Iraq and Syria have put paid to that notion. Another piety is that only an Israeli-Palestinian peace deal could reconcile the wider Arab world to the Jewish state. Yet relations between Jerusalem and Riyadh, Saudi Arabia; Cairo; Abu Dhabi, United Arab Emirates; and Manama, Bahrain, are flourishing as never before, even as the prospect of a Palestinian state is as remote as ever. Relations between Jerusalem and Saudi Arabia, Egypt, UAE, Bahrain are flourishing A third is that intensive mediation by the United States is essential to progress on the ground. Yet recent American involvement — whether at the Camp David summit in 2000 or John Kerry’s efforts in 2013 — has had mostly the opposite effect: diplomatic failure, followed by war. Which brings us to Jerusalem, and the piety that pretending it isn’t what it is can be a formula for anything except continued self-delusion. What Jerusalem is is the capital of Israel, both as the ancestral Jewish homeland and the modern nation-state. When Richard Nixon became the first American president to visit the country in 1974, he attended his state dinner in Jerusalem. It’s where President Anwar Sadat of Egypt spoke when he decided to make peace in 1977. It’s what Congress decided as a matter of law in 1995. When Barack Obama paid his own presidential visit to Israel in 2013, he too spent most of his time in Jerusalem. So why maintain the fiction that Jerusalem isn’t the capital? Why maintain the fiction that Jerusalem is not the capital? The original argument, from 1947, was that Jerusalem ought to be under international jurisdiction, in recognition of its religious importance. But Jews were not allowed to visit the Western Wall during the 19 years when East Jerusalem was under Jordanian occupation. Yasser Arafat denied that Solomon’s Temple was even in Jerusalem, reflecting an increasingly common Palestinian denial of history. Would Jews be allowed to visit Jewish sites, and would those sites be respected, if the city were redivided? Doubtful, considering Palestinian attacks on such", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00672", "split": "train"}
{"id": "conditionality_train_pos_0461", "text": "The Swift/XRT data of 179 GRBs (from 050124 to 070129) and the optical afterglow data of 57 pre- and post-Swift GRBs are analyzed, in order to systematically investigate the jet-like breaks in the X-ray and optical afterglow lightcurves. We find that not a single burst can be included in the ``Platinum'' sample, in which the data satisfy all the criteria of a jet break. By releasing one or more requirements to define a jet break, some candidates of various degrees could be identified. In the X-ray band, 42 out of the 103 well-sampled X-ray lightcurves have a decay slope of the post-break segment >1.5 (``Bronze'' sample), and 27 of them also satisfy the closure relations of the forward models (``Silver'' sample). The numbers of the ``Bronze'' and ``Silver'' candidates in the optical lightcurves are 27 and 23, respectively. Thirteen bursts have well-sampled optical and X-ray lightcurves, but only seven cases are consistent with an achromatic break, but even in these cases only one band satisfies the closure relations (``Gold'' sample). The observed break time in the XRT lightcurves is systematically earlier than that in the optical bands. All these raise great concerns in interpreting the jet-like breaks as jet breaks and further inferring GRB energetics from these breaks. By assuming that these breaks are jet breaks, we perform a similar analysis as previous work to calculate the jet opening angle (theta_j) and energetics (E_k) with the ``Silver'' and ``Gold'' jet break candidates. The derived E_K distribution reveals a much larger scatter than the pre-Swift sample. A tentative anti-correlation between theta_j and E_{K,iso} is found for both the pre-Swift and Swift GRBs, indicating that the E_K could still be quasi-universal, if the breaks in discussion are indeed jet breaks(abridge).", "label": 1, "domain": "academic", "token_count": 417, "matched_pair_id": "conditionality_00015", "split": "train"}
{"id": "conditionality_train_pos_0462", "text": "1) a uniform application, or set of uniform applications, to be used by an applicant to apply for assistance from multiple Federal financial assistance programs that serve similar purposes and are administered by different Federal agencies; (2) ways to streamline and simplify Federal financial assistance administrative procedures and reporting requirements for grantees; (3) a uniform system wherein an applicant may apply for, manage, and report on the use of, funding from multiple Federal financial assistance programs across different Federal agencies; (4) a process for applicants to electronically apply for, and report on the use of, funds from Federal financial assistance programs; (5) use of common rules for multiple Federal financial assistance programs across different Federal agencies; (6) improved interagency and intergovernmental coordination of information collection and sharing of data pertaining to Federal financial assistance programs, including the development of a release form to be used by grantees to facilitate the sharing of information across multiple Federal financial assistance programs; (7) a process to strengthen the information resources management capacity of State, local, and tribal governments and qualified organizations pertaining to the administration of Federal financial assistance programs; and (8) specific annual goals and objectives to further the purposes of this Act. (b) Actions Consistent With Statutory Requirements.--The actions taken by the Director under subsection (a) shall be consistent with statutory requirements relating to any applicable Federal financial assistance program. (c) Lead Agency and Working Groups.--The Director may designate a lead agency to assist the Director in carrying out the responsibilities under this section. The Director may use interagency working groups to assist in carrying out such responsibilities. (d) Review of Plans and Reports.-- (1) In general.--The Director shall-- (A) review agency plans and reports developed under section 6 for adequacy; (B) monitor the annual performance of each agency toward achieving the goals and objectives stated in the agency plan; and (C) ensure that each agency plan does not diminish standards to measure performance and accountability of financial assistance programs. (2) Report.--Not later than 3 years after the date of enactment of this Act, the Director shall report to Congress on implementation of this section. Such a report may be included as part of any of the general management reports required under law. (e) Exemptions.-- (1) In general.--The Director may exempt any Federal agency from the requirements of this Act if the Director determines that the agency does not have a significant number of Federal financial assistance programs.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00837", "split": "train"}
{"id": "conditionality_train_pos_0463", "text": "if the seller did not offer for sale the brand of vaccine on the date described in subparagraph (A), the average price of the brand of vaccine per dose offered by the seller during the 12-month period preceding such date; or (C) if the seller did not offer for sale the brand of vaccine on the date described in paragraph (1)(A) or during the period described in paragraph (1)(B), the price determined by the Secretary under paragraph (3). (2) Exception.--If the Secretary finds that the average price of a covered vaccine is substantially different at the time of a declaration of a shortage of that vaccine under subsection (c) than the average price of the vaccine during the 12-month period preceding such declaration because of factors wholly unrelated to the causes of the shortage, the Secretary may determine an appropriate baseline price of the vaccine. (3) Timing of determinations by secretary.--At the time of declaring a shortage of a covered vaccine under subsection (c), the Secretary shall determine an appropriate baseline price of the vaccine per dose for purposes of paragraph (1)(C) and, if applicable, for purposes of paragraph (2). (e) Penalties.-- (1) In general.--Any person who violates subsection (a) shall be imprisoned for not more than 30 days, fined in the amount described in paragraph (2), or both. Each violation of subsection (a) respecting a separate dose of a covered vaccine constitutes a separate offense. (2) Amount.--The amount of a fine under paragraph (1) shall be, for each dose of covered vaccine sold at a price in violation of this section, 3 times the amount of the difference between such price and the applicable baseline price. (f) Citizen Suits.-- (1) In general.--Except as provided in paragraph (2), any person may commence a civil action on his own behalf to compel compliance with subsection (a) against any person (including the United States and any other governmental instrumentality or agency to the extent permitted by the Eleventh Amendment to the Constitution) for any alleged violation of subsection (a). The United States district courts shall have jurisdiction, without regard to the amount in controversy or the citizenship of the parties, to compel compliance with such subsection. (2) Notice required.--No action may be commenced under this subsection-- (A) prior to 30 days after the plaintiff has given notice of the alleged violation (in such manner as the Secretary may require) to the", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00911", "split": "train"}
{"id": "conditionality_train_pos_0464", "text": "The long term time evolution of tidal dwarf satellite galaxies with two different initial densities orbiting a host galaxy that resembles the Milky Way has been studied using a large set of Newtonian N-Body simulations. From the simulations two maps of the orbital conditions that lead to quasi-equilibrium objects were constructed. It has been found that several orbits of the satellites allow for the existence, for about 1 Gyr or more, of out-of-equilibrium bodies with high apparent mass-to-light ratios. Within this framework the satellites in the quasi-stable phase reproduce the observed satellite properties for about 16% of the orbit for high density progenitors, and for about 66% for progenitors with lower densities An additional simulation for a single satellite with initial mass of 10^7 Msun and Plummer radius of 0.15 kpc leads to remnants in the quasi- equilibrium phase that simultaneously reproduce remarkably well the observational quantities of the UFDGs of the Milky Way. This satellite in the quasi-stable phase reproduces the observed satellite properties for about 42% of the orbit. The results suggest that a fraction of the observed satellites could plausibly be galaxies without dark matter that have true M/L ratios much lower than those measured. The inflated M/L ratios arise because they are observed at the right time, along the right orbit and during the quasi-equilibrium phase of their evolution. This is a viable explanation for the high M/L ratios observed in all satellites as long as the satellites are preferentially on certain orbits and are observed at certain times. This could arise within the TDG scenario if all satellites are created at the same time along a few specific orbits that are particularly susceptible to the quasi-equilibrium phase.", "label": 1, "domain": "academic", "token_count": 344, "matched_pair_id": "conditionality_00457", "split": "train"}
{"id": "conditionality_train_pos_0465", "text": "If you want the best possible picture from an LG TV, you’re going to want to look at its OLED models, but they’re fairly expensive and not everyone wants to spend that kind of money on a TV — even a really good one. LG is aware of this, and is constantly working to improve its LCD models. The latest result of the company’s efforts to that end is the SJ9500 Super UHD TV, which LG says provides its best 4K LCD picture quality ever. To achieve this, LG uses a quantum dot film developed by the company’s display division that it calls Nano Cell, which allows for more accurate colors, deeper blacks, and a wider viewing angle. While conventional LCD displays can lose nearly 60 percent of their color and contrast when viewed from off to the side, LG says the SJ9500 maintains 95 percent at the same angles, meaning you don’t have to fight over the best seat in the house, at least not for picture-related reasons. More: LG debuts Tone Free headset and Tone Studio wearable speaker ahead of CES As expected in a premium TV these days, the SJ9500 supports high dynamic range (HDR), with both the HDR10 and Dolby Vision formats supported. The TV features Active HDR, which LG says analyzes and optimizes HDR10 content on a scene-by-scene basis, making for an even better HDR experience. The new models also include support for Advanced HDR, developed by Technicolor, as well as a feature LG calls HDR Effect. This feature has the further ability to process standard dynamic range content in order to simulate HDR, making for a more colorful picture, even with older content. The SJ9500 doesn’t use a front cover, which helps keep the thickness of the bezel down, making for a nearly edge-to-edge look. As LG’s premium UHD LCD TV, it uses a metal design and uniquely shaped stand that allow it to maintain an impressive look without dominating your living room — at least not until it’s turned on. More: LG’s levitating PJ9 Bluetooth speaker expected to take off at CES Alongside the SJ9500, the company is also introducing two other series, the SJ8500 and SJ8000. These offer the same type of display technology and features, though they aren’t quite as thin and lights as the SJ9500, which is just 6.9 mm thick at its thinnest point. As of yet, there is no word on the", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00718", "split": "train"}
{"id": "conditionality_train_pos_0466", "text": "has its own names for many of its missiles. Determining what missiles are fired by North Korea after explosive launch failures can be an imprecise science. For example, officials said that no determination has been made for a North Korean missile that was fired on March 21 and exploded moments later. A description of the missile launched on April 4 has also been revised several times. It was initially described by a U.S. Pacific Command press release as a KN-15, a new land-based, multi-stage, medium-range missile that uses solid fuel. The new KN-15 designation was created to distinguish it from the KN-11, North Korea’s solid-fueled, submarine-launched missile, which the country tested last summer. However, the day after the launch, U.S. officials revised their assessment and described the missile as a SCUD missile with an existing range. Days later, it was re-designated again as the new KN-17 because it was different than existing single-stage SCUD missiles. Two of North Korea's five missile launches this year have involved failures shortly after liftoff. These failures have been similar to the series of explosions that occurred with the intermediate-range Musudan missile in 2016. Last year, North Korea conducted eight tests of the Musudan missile, but only one of the missiles achieved flight. The vast majority of the Musudan tests ended in failure. According to a New York Times report, the U.S. military sabotaged North Korea's missile program by using cyber and electronic strikes that caused missiles to explode seconds after launch in March. According to the Times, the Obama administration signed off on the Pentagon's use of so-called \"left of launch\" techniques. These are techniques that could electronically affect North Korean missiles before launch or as they lift off. The report has gained traction in the wake of Saturday's failed launch, although it remains unclear if such a program actually exists.", "label": 1, "domain": "news", "token_count": 390, "matched_pair_id": "conditionality_00539", "split": "train"}
{"id": "conditionality_train_pos_0467", "text": "In Kaluza-Klein models, we investigate soliton solutions of Einstein equation. We obtain the formulas for perihelion shift, deflection of light, time delay of radar echoes and PPN parameters. We find that the solitonic parameter k should be very big: |k|\\geq 2.3\\times10^4. We define a soliton solution which corresponds to a point-like mass source. In this case the soliton parameter k=2, which is clearly contrary to this restriction. Similar problem with the observations takes place for static spherically symmetric perfect fluid with the dust-like equation of state in all dimensions. The common for both of these models is the same equations of state in our three dimensions and in the extra dimensions. All dimensions are treated at equal footing. To be in agreement with observations, it is necessary to break the symmetry between the external/our and internal spaces. It takes place for black strings which are particular examples of solitons with k\\to \\infty. For such k, black strings are in concordance with the observations. Moreover, we show that they are the only solitons which are at the same level of agreement with the observations as in general relativity. Black strings can be treated as perfect fluid with dust-like equation of state p_0=0 in the external/our space and very specific equation of state p_1=-(1/2)\\epsilon in the internal space. The latter equation is due to negative tension in the extra dimension. We also demonstrate that dimension 3 for the external space is a special one. Only in this case we get the latter equation of state. We show that the black string equations of state satisfy the necessary condition of the internal space stabilization. Therefore, black strings are good candidates for a viable model of astrophysical objects (e.g., Sun) if we can provide a satisfactory explanation of negative tension for particles constituting these objects.", "label": 1, "domain": "academic", "token_count": 397, "matched_pair_id": "conditionality_00274", "split": "train"}
{"id": "conditionality_train_pos_0468", "text": "Let $\\mathcal{L}$ be a subspace lattice on a Banach space $X$ and let $\\delta:\\mathrm{Alg}\\mathcal{L}\\rightarrow B(X)$ be a linear mapping. If $\\vee\\{L\\in \\mathcal{L}: L_-\\nsupseteq L\\}=X$ or $\\wedge\\{L_-:L\\in \\mathcal{L}, L_-\\nsupseteq L\\}=(0)$, we show that the following three conditions are equivalent: (1) $\\delta(AB)=\\delta(A)B+A\\delta(B)$ whenever $AB=0$; (2) $\\delta(AB+BA)=\\delta(A)B+A\\delta(B)+\\delta(B)A+B\\delta(A)$ whenever $AB+BA=0$; (3) $\\delta$ is a generalized derivation and $\\delta(I)\\in (\\mathrm{Alg}\\mathcal{L})^\\prime$. If $\\vee\\{L\\in \\mathcal{L}: L_-\\nsupseteq L\\}=X$ or $\\wedge\\{L_-:L\\in \\mathcal{L}, L_-\\nsupseteq L\\}=(0)$ and $\\delta$ satisfies $\\delta(AB+BA)=\\delta(A)B+A\\delta(B)+\\delta(B)A+B\\delta(A)$ whenever $AB=0$, we obtain that $\\delta$ is a generalized derivation and $\\delta(I)A\\in(\\mathrm{Alg}\\mathcal{L})^\\prime$ for every $A\\in \\mathrm{Alg}\\mathcal{L}$. We also prove that if $\\vee\\{L\\in \\mathcal{L}: L_-\\nsupseteq L\\}=X$ and $\\wedge\\{L_-:L\\in \\mathcal{L}, L_-\\nsupseteq L\\}=(0)$, then $\\delta$ is a local generalized derivation if and only if $\\delta$ is a generalized derivation.", "label": 1, "domain": "academic", "token_count": 433, "matched_pair_id": "conditionality_00347", "split": "train"}
{"id": "conditionality_train_pos_0469", "text": "irtles and the Charmanders and the Bulbasaurs.\" She points to Nintendo's recent ventures into mobile development as evidence of a continued push to expand its player base. \"Pokemon Go became this transitory nostalgic thing that brought people back into Pokemania,\" Samantha says. \"They [Nintendo] saw a surge of new players that maybe hadn't picked up a Pokemon game for 20 years and wanted to get back in.\" Let's Go includes significant crossovers with Pokemon Go, which has received over 750 million mobile downloads to date. Players will be able to transfer caught Pokémon from the mobile game into the Switch experience. \"I think Nintendo saw the success of Pokemon Go and wanted to cash in on it,\" Samantha says. Nintendo also confirmed that an \"all-new core series\" title is in development, which will continue the tradition of in-depth Pokemon RPGs begun by Red and Blue in 1996. Some Pokemon fans have reacted positively to the news online, but those who are passingly familiar with the brand will have to be convinced to buy a Nintendo Switch to play. Skip Twitter post by @Koil1990 Not hyped for the new Pokemon game on the switch, I want a proper Pokemon game ;( — Kyle (@Koil1990) May 30, 2018 Report The decision to release these new Pokemon games aims to dismantle any barriers to entry for those without a Switch by tempting them to purchase a Switch ahead of the core RPG launch next year. \"Pokemon Let's Go Eevee and Pikachu have the Pokemon you know,\" Samantha says. \"My Mum even knows who Pikachu is - she can't spell it, but she knows who Pikachu is - and that's the sort of experience they want to deliver people sort of to wean them back into the experience and maybe even get a few more people playing on Switch too.\" Nintendo remains tight-lipped on how Let's Go will actually play for now, with more information expected in the coming months. Follow Newsbeat on Instagram, Facebook and Twitter. Listen to Newsbeat live at 12:45 and 17:45 every weekday on BBC Radio 1 and 1Xtra - if you miss us you can listen back here.", "label": 1, "domain": "news", "token_count": 451, "matched_pair_id": "conditionality_00797", "split": "train"}
{"id": "conditionality_train_pos_0470", "text": "If you've ever wondered why so many companies are making moves toward the cloud, the answer may surprise you: It's fear of missing out. According to recent report from Commvault and CITO Research, 81% of business leaders are embracing the cloud because they're concerned about missing out on cloud advancements. So, just how many executives are making that move? According to the report, 93% of respondents said that at least some of their processes were being moved to the cloud. Additionally, 56% said that they had already moved, or intended to move, all of their processes to the cloud. \"The survey unequivocally confirms that Cloud FOMO is real and on the mind of C-level and other IT leaders who are grappling with bringing the value of this new frontier to their organizations, from increasing IT outcomes to being a strategic driver for increased business agility,\" Dan Woods, CTO of CITO Research, said in the release. \"The research indicates the migration toward the cloud is underway in full force, even as companies struggle to understand cloud capabilities. Data protection and recovery was highlighted as a fundamental area where the cloud is having significant business impact.\" SEE: Special report: The cloud v. data center decision (free PDF) Don Foster, senior director of solutions marketing for Commvault, said in the report that cloud technologies are still seen as a key driver for digital transformation. As such, it makes sense that these business leaders would be concerned about getting to the cloud quickly. The most important cloud projects cited by the respondents were data protection and backup, and data recovery, as noted by 75% of the respondents and 63% respectively. However, there are some challenges holding these companies back from realizing their cloudy dreams. The sheer volume of data was cited by 68% of those surveyed as a key barrier, while 65% pointed to a struggle with skills and talent, and 55% said policies were the biggest barrier. These business leaders are putting their money on the line, too. Some 87% plan on putting more money in their budget for cloud investments. The reasons for why these respondents wanted to move to the cloud were varied. Of those surveyed, 33% noted that \"customer focus through business agility\" was their primary reason for moving to the cloud. Cost savings were the primary reason for 22% of respondents and 20% said \"innovation and development of new apps, products and services\" was the driving force behind their", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00500", "split": "train"}
{"id": "conditionality_train_pos_0471", "text": "Model independent reconstructions of dark energy have received some attention. The approach that addresses the reconstruction of the dimensionless coordinate distance and its two first derivatives using a polynomial fit in different redshift windows is well developed \\cite{DalyDjorgovski1,DalyDjorgovski2,DalyDjorgovski3}. In this work we offer new insights into the problem by focusing on two types of observational probes: SNeIa and GRBs. Our results allow to highlight some of the intrinsic weaknesses of the method. One of the directions we follow is to consider updated observational samples. Our results indicate than conclusions on the main dark energy features as drawn from this method are intimately related to the features of the samples themselves (which are not quite ideal). This is particularly true of GRBs, which manifest themselves as poor performers in this context. In contrast to original works, we conclude they cannot be used for cosmological purposes, and the state of the art does not allow to regard them on the same quality basis as SNeIa. The next direction we contribute to is the question of how the adjusting of some parameters (window width, overlap, selection criteria) affect the results. We find again there is a considerable sensitivity to these features. Then, we try to establish what is the current redshift range for which one can make solid predictions on dark energy evolution. Finally, we strengthen the former view that this model is modest in the sense it provides only a picture of the global trend. But, on the other hand, we believe it offers an interesting complement to other approaches given that it works on minimal assumptions.", "label": 1, "domain": "academic", "token_count": 330, "matched_pair_id": "conditionality_00419", "split": "train"}
{"id": "conditionality_train_pos_0472", "text": "We use a semi-analytical model to study the impact of reionization, and the associated radiative feedback, on galaxy formation. Two feedback models have been considered: (i) a standard prescription, according to which star formation is totally suppressed in galaxies with circular velocity below a critical threshold (model CF06) and (ii) a characterization based on the filtering scale (model G00), allowing for a gradual reduction of the gas available for star formation in low-mass galaxies. In model CF06 reionization starts at z ~ 15-20, is 85% complete by z ~ 10; at the same z, the ionized fraction is 16% in model G00. The models match SDSS constraints on the evolution of the neutral hydrogen fraction at z < 7, but predict different Thomson optical depths, tau_e = 0.1017 (CF06), and 0.0631 (G00); such values are within 1 sigma of the WMAP 3-yr determination. Both models are in remarkable good agreement with additional existing data (evolution of Lyman-limit systems, cosmic star formation history, high-z galaxy counts, IGM thermal history), which therefore cannot be used to discriminate among different feedback models. Deviations among radiative feedback prescriptions emerge when considering the expected HI 21 cm background signal, where a ~ 15 mK absorption feature in the range 75-100 MHz is present in model G00 and a global shift of the emission feature preceding reionization towards larger frequencies occurs in the same model. Single dish observations with existing or forthcoming low-frequency radio telescopes can achieve mK sensitivity, allowing the identification of these features provided that foregrounds can be accurately subtracted.", "label": 1, "domain": "academic", "token_count": 353, "matched_pair_id": "conditionality_00036", "split": "train"}
{"id": "conditionality_train_pos_0473", "text": "competent jurisdiction; (4) to a consumer reporting agency, as defined in section 603 of the Fair Credit Reporting Act for inclusion in a consumer report that may be released to a third party only for a purpose permissible under section 604 of that Act; or (5) that is not personally identifiable. SEC. 4. CIVIL LIABILITY FOR NONCOMPLIANCE. (a) In General.--Any individual whose rights under this Act have been knowingly or negligently violated may bring a civil action to recover-- (1) such preliminary and equitable relief as the court determines to be appropriate; and (2) the greater of compensatory damages or liquidated damages of $5,000. (b) Punitive Damages.--In any action brought under this section in which the individual has prevailed because of a knowing violation of a provision of this Act, the court may, in addition to any relief awarded under subsection (a), award such punitive damages as may be warranted. (c) Attorney's Fees.--In the case of a civil action brought under subsection (a) in which the individual has substantially prevailed, the court may assess against the respondent a reasonable attorney's fee and other litigation costs and expenses (including expert fees) reasonably incurred. (d) Limitation.--No action may be commenced under this section more than 3 years after the date on which the violation was or should reasonably have been discovered. (e) Agency.--A principal is jointly and severally liable with the principal's agent for damages under this section for the actions of the principal's agent acting within the scope of the agency. (f) Additional Remedies.--The equitable relief or damages that may be available under this section shall be in addition to any other lawful remedy or award available. SEC. 5. RELATION TO STATE LAWS. (a) In General.--This Act shall not be construed as superseding, altering, or affecting the statutes, regulations, orders, or interpretations in effect in any State, except to the extent that such statutes, regulations, orders, or interpretations are inconsistent with the provisions of this Act, and then only to the extent of the inconsistency. (b) Greater Protection Under State Law.--For purposes of this Act, a State statute, regulation, order, or interpretation is not inconsistent with the provisions of this subtitle if the protection such statute, regulation, order, or interpretation affords any person is greater than the protection provided under this Act.", "label": 1, "domain": "government", "token_count": 498, "matched_pair_id": "conditionality_00879", "split": "train"}
{"id": "conditionality_train_pos_0474", "text": "on a map entitled `Lewis Fork Addition and Little Wilson Creek Additions', dated March 23, 2005, and which are hereby incorporated in the Little Wilson Creek Wilderness; ``(19) certain lands in the Jefferson National Forest, which comprise approximately 2,456 acres, as generally depicted on a map entitled `Shawvers Run Additions', dated March 23, 2005, and which are hereby incorporated in the Shawvers Run Wilderness; ``(20) certain lands in the Jefferson National Forest, which comprise approximately 1,203 acres, as generally depicted on a map entitled `Peters Mountain Addition', dated March 23, 2005, and which are hereby incorporated in the Peters Mountain Wilderness; and ``(21) certain lands in the Jefferson National Forest, which comprise approximately 612 acres, as generally depicted on a map entitled `Kimberling Creek Additions', dated March 23, 2005, and which are hereby incorporated in the Kimberling Creek Wilderness;''. SEC. 3. SENG MOUNTAIN AND BEAR CREEK SCENIC AREAS, JEFFERSON NATIONAL FOREST, VIRGINIA. (a) Establishment of Scenic Areas.-- (1) Establishment.--The following National Forest System lands in the State of Virginia are hereby designated as National Scenic Areas (in this section referred to as the ``scenic areas''): (A) Certain lands in the Jefferson National Forest, which comprise approximately 6,455 acres, as generally depicted on a map entitled ``Seng Mountain and Raccoon Branch'', dated March 23, 2005, and which shall be known as the Seng Mountain National Scenic Area. (B) Certain lands in the Jefferson National Forest, which comprise approximately 5,503 acres, as generally depicted on a map entitled ``Bear Creek'' dated March 23, 2005, and which shall be known as the Bear Creek National Scenic Area. (2) Maps and descriptions.--As soon as practicable after the date of the enactment of this Act, the Secretary of Agriculture shall file a map and boundary description of the scenic areas with the Committee on Agriculture, Nutrition, and Forestry of the Senate and the Committee on Agriculture and the Committee on Resources of the House of Representatives. The map and description shall have the same force and effect as if included in this Act, except that the Secretary may correct clerical and typographical errors in the map and description.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00894", "split": "train"}
{"id": "conditionality_train_pos_0475", "text": "'. (b) Definition of Siblings.--Section 475 of the Social Security Act (42 U.S.C. 675) is amended by adding at the end the following: ``(9) The term `siblings' means individuals who satisfy at least one of the following conditions: ``(A) The individuals are considered by State law to be siblings. ``(B) The individuals would have been considered siblings under State law but for termination of parental rights or other disruption of parental rights, such as the death of a parent.''. SEC. 9. EFFECTIVE DATE. (a) In General.--Except as provided in subsection (b), the amendments made this Act shall take effect on October 1, 2013. (b) Delay Permitted if State Legislation Required.--In the case of a State plan approved under part B or E of title IV of the Social Security Act which the Secretary of Health and Human Services determines requires State legislation (other than legislation appropriating funds) in order for the plan to meet the additional requirements imposed by this Act, the State plan shall not be regarded as failing to comply with the requirements of such part solely on the basis of the failure of the plan to meet such additional requirements before the 1st day of the 1st calendar quarter beginning after the close of the 1st regular session of the State legislature that ends after the 1-year period beginning with the date of the enactment of this Act. For purposes of the preceding sentence, in the case of a State that has a 2-year legislative session, each year of the session is deemed to be a separate regular session of the State legislature. SEC. 10. DETERMINATION OF BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 431, "matched_pair_id": "conditionality_00978", "split": "train"}
{"id": "conditionality_train_pos_0476", "text": "We present deep Keck spectroscopy for 17 morphologically-selected field spheroidals in the redshift range 1.05<z<1.60 in order to investigate the continuity in physical properties between the claimed massive compact red galaxies (\"nuggets\") at z~2 and well-established data for massive spheroidal galaxies below z~1. By combining Keck-based stellar velocity dispersions with HST-based sizes, we find that the most massive systems (Mdyn > 10^11 Msol) grew in size over 0<z<1.6 as (1+z)^(-0.75 +- 0.10) (i.e., x2 since z=1.5) whereas intermediate mass systems (10^11 Msol > Mdyn > 10^10 Msol) did not grow significantly. These trends are consistent with a picture in which more massive spheroidals formed at higher redshift via \"wetter\" mergers involving greater dissipation. To examine growth under the favored \"dry\" merger hypothesis, we also examine size growth at a fixed velocity dispersion. This test, uniquely possible with our dynamical data, allows us to consider the effects of \"progenitor bias.\" Above our completeness limit (sigma > 200 km/s), we find size growth consistent with that inferred for the mass-selected sample, thus ruling out strong progenitor bias. To maintain continuity in the growth of massive galaxies over the past 10 Gyr, our new results imply that size evolution over 1.3<z<2.3, a period of 1.9 Gyr, must have been even more dramatic than hitherto claimed if the red sources at z>2 are truly massive and compact.", "label": 1, "domain": "academic", "token_count": 356, "matched_pair_id": "conditionality_00215", "split": "train"}
{"id": "conditionality_train_pos_0477", "text": "We give a generalization of the classical Bombieri--Schneider--Lang criterion in transcendence theory. We give a local notion of $LG$--germ, which is similar to the notion of $E$-- function and Gevrey condition, and which generalize (and replace) the condition on derivatives in the theorem quoted above. Let $K\\subset \\Bbb C$ be a number field and $X$ a quasi--projective variety defined over $K$. Let $\\gamma\\colon M\\to X$ be an holomorphic map of finite order from a parabolic Riemann surface to $X$ such that the Zariski closure of the image of it is strictly bigger then one. Suppose that for every $p\\in X(K)\\cap\\gamma(M)$ the formal germ of $M$ near $P$ is an $LG$-- germ, then we prove that $X(K)\\cap\\gamma(M)$ is a finite set. Then we define the notion of conformally parabolic Kh\\\"aler varieties; this generalize the notion of parabolic Riemann surface. We show that on these varieties we can define a value distribution theory. The complementary of a divisor on a compact Kh\\\"aler manifold is conformally parabolic; in particular every quasi projective variety is. Suppose that $A$ is conformally parabolic variety of dimension $m$ over $\\Bbb C$ with Kh\\\"aler form $\\omega$ and $\\gamma\\colon A\\to X$ is an holomorphic map of finite order such that the Zariski closure of the image is strictly bigger then $m$. Suppose that for every $p\\in X(K)\\cap \\gamma (A)$, the image of $A$ is an $LG$--germ. then we prove that there exists a current $T$ on $A$ of bidegree $(1,1)$ such that $\\int_AT\\wedge\\omega^{m-1}$ explicitly bounded and with Lelong number bigger or equal then one on each point in $\\gamma^{-1}(X(K))$. In particular if $A$ is affine $\\gamma^{-1}(X(K))$ is not Zariski dense.", "label": 1, "domain": "academic", "token_count": 453, "matched_pair_id": "conditionality_00099", "split": "train"}
{"id": "conditionality_train_pos_0478", "text": "Let $A$ be a finite dimensional hereditary algebra over an algebraically closed field $k$, $T_2(A)=(\\begin{array}{cc}A&0 A&A\\end{array})$ be the triangular matrix algebra and $A^{(1)}=(\\begin{array}{cc}A&0 DA&A\\end{array})$ be the duplicated algebra of $A$ respectively. We prove that ${\\rm rep.dim}\\ T_2(A)$ is at most three if $A$ is Dynkin type and ${\\rm rep.dim}\\ T_2(A)$ is at most four if $A$ is not Dynkin type. Let $T$ be a tilting A-$\\module$ and $\\ol{T}=T\\oplus\\ol{P}$ be a tilting $A^{(1)}$-$\\module$. We show that $\\End_{A^{(1)}} \\ol{T}$ is representation finite if and only if the full subcategory $\\{(X,Y,f)\\ |\\ X\\in {\\rm mod}\\ A, Y\\in\\tau^{-1}\\mathscr{F}(T_A)\\cup{\\rm add}\\ A\\}$ of ${\\rm mod \\ T_2(A)}$ is of finite type, where $\\tau$ is the Auslander-Reiten translation and $\\mathscr{F}(T_A)$ is the torsion-free class of ${\\rm mod}\\ A$ associated with $T$. Moreover, we also prove that ${\\rm rep.dim\\ End}_{A^{(1)}}\\ {\\ol T}$ is at most three if $A$ is Dynkin type.", "label": 1, "domain": "academic", "token_count": 339, "matched_pair_id": "conditionality_00358", "split": "train"}
{"id": "conditionality_train_pos_0479", "text": "Motivated by the discovery of extremely bright supernovae SNe1999as and 2006gy, we have investigated how much 56Ni mass can be synthesized in core-collapse massive supernovae (SNe). We calculate the evolution of several very massive stars with initial masses M <~ 100 Msun from the main-sequence to the beginning of the Fe-core collapse and simulate their explosions and nucleosynthesis. In order to avoid complications associated with strong mass-loss, we only consider metal-poor stars with initial metallicity Z = Zsun/200. However, our results are applicable to higher metallicity models with similar C+O core masses. The C+O core mass for the 100Msun model is M_CO = 42.6Msun and this is the heaviest model in the literature for which Fe-core collapse SN is explored. The synthesized 56Ni mass increases with the increasing explosion energy and progenitor mass. For the explosion energy of E_51 = E/10^{51} erg =30, for example, the 56Ni masses of M(56Ni) = 2.2, 2.3, 5.0, and 6.6 Msun can be produced for the progenitors with initial masses of 30, 50, 80 and 100 Msun (or C+O core masses M_CO = 11.4, 19.3, 34.0 and 42.6 Msun), respectively. We find that producing M(56Ni) ~ 4Msun as seen in SN1999as is possible for M_CO >~ 34 Msun and E_{51} >~ 20. Producing M(56Ni) ~ 13Msun as suggested for SN2006gy requires a too large explosion energy for M_CO <~ 43Msun, but it may be possible with a reasonable explosion energy if M_CO >~ 60Msun.", "label": 1, "domain": "academic", "token_count": 404, "matched_pair_id": "conditionality_00013", "split": "train"}
{"id": "conditionality_train_pos_0480", "text": "If left always on, I think there is a fair chance at some point people will determine that cellular Apple Watches cause cancer. Apple should investigate this possibility and do what it can to mitigate. Airplane Mode is Your Friend For a little perspective, don’t go running with your hair on fire to throw your Apple Watch into the trash. I own an Apple Watch. I even wear it every day. However, my Apple Watch is always in Airplane mode. Why? Well, first, because then I can wear it for long periods of time without needing to recharge it—it lasts 3 days between charges in Airplane mode. Second, because I find most Apple Watch apps useless. But third, and most importantly, I believe it is inevitable that people will discover that wireless technology causes cancer. The Math of: No it Doesn’t, Yes it Does In fact, I believe that this is more a math problem than it is a debate of scientific studies. The bottom line is, the more exposed you are to RF radiation, the more likely you are to have a random DNA-bit flipped that spawns a mutation, i.e., cancerous growth. Now there have been dozens of “yes, cellphones cause cancer”, “no, cellphones do not cause cancer” studies. To me, that sounds amazingly like what happened with the tobacco industry for decades. That includes one recent study by the US National Toxicology Program (NTP) that shows an increase in tumors in rats exposed to cellphone radiation (albeit at exposures which are at greater levels than most cell phone users experience). However, I think that there is something people are not paying attention to. The Apple Watch 3 now sports a cellular transceiver strapped to your arm as much as 24 hours a day. Every day. This seems beyond NTP rat-like exposure, and perhaps even beyond the long exposures that caused many Connecticut cops to contract testicular and brain cancer from their radar guns. With many radiation safety protocols, you reduce radiation injury by increasing distance, decreasing time exposed, and increasing shielding, whereas the Apple Watch seems to be doing the opposite. In my totally non-expert, non-learned, non-medically-trained, non-scientific, monkey-at-best opinion, it is a near certainty and inevitability that such constant close contact and exposure will increase the odds of a radiation-induced-DNA-bit-flip and cause cancer. [Update: Even the CDC is noting that the “International Agency for Research", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00568", "split": "train"}
{"id": "conditionality_train_pos_0481", "text": "Using deep infrared observations conducted with the MOIRCS on the Subaru Telescope in GOODS-N combined with public surveys in GOODS-S, we investigate the dependence on stellar mass, M_*, and galaxy type of the close pair fraction (5 kpc < r < 20 kpc) and implied merger rate. In common with some recent studies we find that the fraction of paired systems that could result in major mergers is low (~4%) and does not increase significantly with redshift to z~1.2, with (1+z)^{1.6 \\pm 1.6}. Our key finding is that massive galaxies with M_* > 1E11 Msun are more likely to host merging companions than less massive systems (M_* ~ 1E10 Msun). We find evidence for a higher pair fraction for red, spheroidal hosts compared to blue, late-type systems, in line with expectations based on clustering at small scales. So-called \"dry\" mergers between early-type galaxies represent nearly 50% of close pairs with M_* > 3E10 Msun at z~0.5, but less than 30% at z~1. This result can be explained by the increasing abundance of red, early-type galaxies at these masses. We compare the volumetric merger rate of galaxies with different masses to mass-dependent trends in galaxy evolution, finding that major mergers cannot fully account for the formation of spheroidal galaxies since z~1. In terms of mass assembly, major mergers contribute little to galaxy growth below M_* ~ 3E10 Msun but are more significant among galaxies with M_* > 1E11 Msun, 30% of which have undergone mostly dry mergers over the observed redshift range. Overall, the relatively more rapid coalescence of high mass galaxies mirrors the expected hierarchical growth of halos and is consistent with recent model predictions, even if the downsizing of star formation and morphological evolution involves additional physical processes.", "label": 1, "domain": "academic", "token_count": 403, "matched_pair_id": "conditionality_00119", "split": "train"}
{"id": "conditionality_train_pos_0482", "text": "area -- just that he hadn't performed or flown there.This time around, the same prosecution team faced off against an entirely new defense team, led by celebrity attorney Tom Mesereau, who mounted a far more aggressive strategy in defending Cosby than the previous team by focusing on attacking the credibility of Constand.It remains to be seen whether that more muscular strategy will pay off or backfire.The primary difference between Cosby's first trial and his second was that at last summer's trial the judge in the case, O'Neill, allowed only one additional accuser to testify and support Constand's account, based on the prosecution's argument that it needed to show a common scheme or pattern to Cosby's alleged assault of Constand.This time around, the judge allowed five such women to take the stand.Another new element in this year's trial was O'Neill's decision to allow the testimony of Marguerite \"Margo\" Jackson, a former colleague of Constand's at Temple, who testified that Constand once mused about framing a celebrity. The judge had rejected her testimony in the first trial as hearsay. Constand has denied Jackson's claims.Unlike last summer, when a parade of Cosby accusers turned up inside and outside the courthouse, just three steadfast accusers -- Victoria Valentino, Therese Serignese and Lili Bernard -- sat quietly in the back of the court for virtually every moment of the lengthy pre-trial motions process, the jury selection and the trial.Cosby faces up to 10 years in prison for each count, if convicted.", "label": 1, "domain": "news", "token_count": 312, "matched_pair_id": "conditionality_00522", "split": "train"}
{"id": "conditionality_train_pos_0483", "text": "The distance dependence and atomic-scale contrast observed in nominal contact potential difference (CPD) signals recorded by KPFM on surfaces of insulating and semiconducting samples, have stimulated theoretical attempts to explain such effects. We attack this problem in two steps. First, the electrostatics of the macroscopic tip-cantilever-sample system is treated by a finite-difference method on an adjustable nonuniform mesh. Then the resulting electric field under the tip apex is inserted into a series of atomistic wavelet-based density functional theory (DFT) calculations. Results are shown for a realistic neutral but reactive silicon nano-scale tip interacting with a NaCl(001) sample. Bias-dependent forces and resulting atomic displacements are computed to within an unprecedented accuracy. Theoretical expressions for amplitude modulation (AM) and frequency modulation (FM) KPFM signals and for the corresponding local contact potential differences (LCPD) are obtained by combining the macroscopic and atomistic contributions to the electrostatic force component generated at the voltage modulation frequency, and evaluated for several tip oscillation amplitudes A up to 10 nm. Being essentially constant over a few Volts, the slope of atomistic force versus bias is the basic quantity which determines variations of the atomic-scale LCPD contrast. Already above A = 0.1 nm, the LCPD contrasts in both modes exhibit almost the same spatial dependence as the slope. In the AM mode, this contrast is approximately proportional to $A^{-1/2}$, but remains much weaker than the contrast in the FM mode, which drops somewhat faster as A is increased. These trends are a consequence of the macroscopic contributions to the KPFM signal, which are stronger in the AM-mode and especially important if the sample is an insulator even at sub-nanometer separations where atomic-scale contrast appears.", "label": 1, "domain": "academic", "token_count": 374, "matched_pair_id": "conditionality_00432", "split": "train"}
{"id": "conditionality_train_pos_0484", "text": "If you are looking for “edgy” art, Bill Herndon, 83, of Acton is your man. He is a custom knife-maker. Herndon’s passion for creating art in steel began at his father’s side. His father’s hobby was photography and his job was engineering. Earning a degree in engineering, he then earned a degree one in illustrative design after serving as a photographer in the U.S. military while stationed in Germany in the 1950’s. After a lifetime in photography and career of selling movie film stock in San Francisco, he retired to Acton in 1997 where he began creating custom knives in his garage. “When I first started out, I sharpened everything in sight” Herndon said. He sharpened his lawn mower blades and then quickly cut off three toes with it. Creating his own steel Herndon wipes the sweat off his face as he stands in front of the 3,000-degree furnace roaring in his back yard. He is creating a piece of “Damascus” steel, a tedious process perfected in the Third Century in India and the Middle East. The process welds thin layers of steel together and creates distinctive design patterns in a blank of steel that will become a knife blade. After removing the glowing billet of steel from the white hot mouth of the forge, borax is added to bind the layers. Then 30 tons of force is applied in the nearby press, fusing the strips into one slab of steel. After repeating the process many times, he moves the blank blade to his power hammer. Activating the six foot tall, clanking, belt driven monster with his foot, Herndon pummels the steel with 50 pounds of pressure at a deafening 250 beats per minute to coax the steel to the thickness of a knife blade. “Using the power hammer saves my old arms,” he laughs. Heating the blade again, he then taps the edge with a blacksmith’s hammer on an anvil to give the blade the familiar curve of a bowie knife. Work continues in the machine shop Herndon weaves through the narrow isles between rows of grinders, band saws and drill presses in his garage. His workshop is literally “cutting edge,” with each piece of machinery focused on a specific task in creating his knives. “Don’t call it a hobby – it’s a vocation,” he said. Herndon pulls on his scratched glasses, tattered leather gloves", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00726", "split": "train"}
{"id": "conditionality_train_pos_0485", "text": "If budget-cutters in Washington decided to eliminate food stamps for New Yorkers, city politicians would be denouncing the cruelty of the “Republican war on the poor.” Yet Mayor de Blasio and the City Council are inflicting the same sort of pain on low-income New Yorkers by denying them access to one of the nation’s most effective anti-poverty programs: Walmart. When he was mayor, Michael Bloomberg supported Walmart’s efforts to open a store in New York, but the company faced unremitting resistance from unions and elected officials, and it gave up the fight once de Blasio moved into Gracie Mansion. “I have been adamant that I don’t think Walmart — the company, the stores — belong in New York City,” de Blasio said. Walmart’s benefits are obvious to shoppers and to economists like Jason Furman, who served in the Clinton administration and was chairman of the Council of Economic Advisers under President Barack Obama. In a paper, “Walmart: A Progressive Success Story,” Furman cited estimates that Walmart, by driving down prices, saved the typical American family more than $2,300 annually. That was about the same amount that a family on food stamps then received from the federal government. How could any progressive with a conscience oppose an organization that confers such benefits? How could de Blasio and the council effectively take money out of the pockets of the poorest families in New York? Because, though they would deny it, they care a lot more about pleasing powerful labor interests, especially the United Food and Commercial Workers, which helped lead the long fight to keep Walmart out of the five boroughs. Labor activists have been spreading horror stories for more than a decade about Walmart’s purported mistreatment of workers, yet somehow they haven’t dissuaded thousands of people in other cities from lining up for jobs whenever a Walmart opens. Often there are five or 10 applicants for each job. As the economist Richard Vedder has noted, the pay at Walmart is comparable with that of other large retailers. Some argue that Walmart exerts downward pressure on retail wages, but even if that’s true — and it’s debatable — the effect is tiny compared with the savings at the cash register. According to Furman, Walmart lowered American retail workers’ pay by less than $5 billion while saving shoppers more than $250 billion with lower prices. Anti-Walmart agitators complain about the government subsidies that some of the company’s workers receive for health insurance, which, they argue, burden taxpayers.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00824", "split": "train"}
{"id": "conditionality_train_pos_0486", "text": "A mobile robot represented by a point moving in the plane has to explore an unknown terrain with obstacles. Both the terrain and the obstacles are modeled as arbitrary polygons. We consider two scenarios: the unlimited vision, when the robot situated at a point p of the terrain explores (sees) all points q of the terrain for which the segment pq belongs to the terrain, and the limited vision, when we require additionally that the distance between p and q be at most 1. All points of the terrain (except obstacles) have to be explored and the performance of an exploration algorithm is measured by the length of the trajectory of the robot. For unlimited vision we show an exploration algorithm with complexity O(P + D?k), where P is the total perimeter of the terrain (including perimeters of obstacles), D is the diameter of the convex hull of the terrain, and k is the number of obstacles. We do not assume knowledge of these parameters. We also prove a matching lower bound showing that the above complexity is optimal, even if the terrain is known to the robot. For limited vision we show exploration algorithms with complexity O(P + A + ?Ak), where A is the area of the terrain (excluding obstacles). Our algorithms work either for arbitrary terrains, if one of the parameters A or k is known, or for c-fat terrains, where c is any constant (unknown to the robot) and no additional knowledge is assumed. (A terrain T with obstacles is c-fat if R/r ? c, where R is the radius of the smallest disc containing T and r is the radius of the largest disc contained in T .) We also prove a matching lower bound ?(P + A + ?Ak) on the complexity of exploration for limited vision, even if the terrain is known to the robot.", "label": 1, "domain": "academic", "token_count": 363, "matched_pair_id": "conditionality_00187", "split": "train"}
{"id": "conditionality_train_pos_0487", "text": "If you fired up Pokemon Go yesterday just to find that you weren't able to connect, there's one potentially good reason behind it. It appears that Google recently updated how their SafetyNet detections work, and the new changes are able to pick up some previous root-hiding methods. If you are using Magisk, the current workaround is to set it to operate in \"core only\" mode via settings in Magisk Manager. Magisk developer topjohnwu issued a statement on the subject earlier today, in which he waxed for a bit on the perpetual cat-and-mouse game of hiding from SafetyNet checks. He stated that he has found a workaround for the new detection policy, but to wait for the next beta. It appears that the most likely method for detection now is app based. Rather than checking if su is present when it shouldn't be or if it can be invoked, it appears that Google might just be checking to see if a root manager application is installed. It's such a simple check that it's difficult to prevent since any app can call up a list of apps on the device, and technically it doesn't even check if a device has been modified or tampered with since a root manager can be present without having root. He could easily fix that by simply tweaking the name of his application, but that's not an ideal fix, as detection could just as easily change the name it looks for. Chainfire's suhide seems to be able to escape package name detection for the time being, as it uses another method to work, though the downloads page for suhide says it isn't currently working. So in the meantime, if you've been hiding root, right now you'll have to move Magisk over into core only mode for the time being if you still want to pass SafetyNet checks. We've reached out to topjohnwu for more information about a future workaround for the SafetyNet changes, or a release schedule for any fixes, and we will add any relevant information to this post when we get it.", "label": 1, "domain": "news", "token_count": 410, "matched_pair_id": "conditionality_00765", "split": "train"}
{"id": "conditionality_train_pos_0488", "text": "31, 2013. (2) Expansion of election to accelerate amt credits in lieu of bonus depreciation.-- (A) In general.--The amendment made by subsection (c) (other than so much of such amendment as relates to section 168(k)(4)(D)(iii) of such Code, as added by such amendment) shall apply to taxable years ending after December 31, 2013. (B) Transitional rule.--In the case of a taxable year beginning before January 1, 2014, and ending after December 31, 2013, the bonus depreciation amount determined under section 168(k)(4) of such Code for such year shall be the sum of-- (i) such amount determined without regard to the amendments made by this section and-- (I) by taking into account only property placed in service before January 1, 2014, and (II) by multiplying the limitation under section 168(k)(4)(C)(ii) of such Code (determined without regard to the amendments made by this section) by a fraction the numerator of which is the number of days in the taxable year before January 1, 2014, and the denominator of which is the number of days in the taxable year, and (ii) such amount determined after taking into account the amendments made by this section and-- (I) by taking into account only property placed in service after December 31, 2013, and (II) by multiplying the limitation under section 168(k)(4)(B)(ii) of such Code (as amended by this section) by a fraction the numerator of which is the number of days in the taxable year after December 31, 2013, and the denominator of which is the number of days in the taxable year. (3) Technical amendment.--The amendment made by subsection (e) shall take effect as if included in the provision of the American Taxpayer Relief Act of 2012 to which it relates.", "label": 1, "domain": "government", "token_count": 405, "matched_pair_id": "conditionality_00986", "split": "train"}
{"id": "conditionality_train_pos_0489", "text": "We present a {\\it Chandra} observation of IRAS 19254--7245, a nearby ULIRG also known as {\\it the Superantennae}. The high spatial resolution of {\\it Chandra} allows us to disentangle for the first time the diffuse starburst emission from the embedded Compton-thick AGN. The 2-10 keV spectrum of the AGN emission is fitted by a flat power-law $\\Gamma=1.3$) and a He-like Fe K$\\alpha$ line with EW$\\sim$1.5 keV, consistent with previous observations. The Fe K$\\alpha$ line profile could be resolved as a blend of a neutral 6.4 keV line and an ionized 6.7 keV (He-like) or 6.9 keV (H-like) line. Variability is detected compared with the previous {\\it XMM-Newton} and {\\it suzaku} observations, demonstrating the compact size of the iron line emission. We fit the spectrum of the galaxy-scale extended emission excluding the AGN and other bright point sources with a soft thermal component with kT~0.8 keV. The luminosity of the extended emission is about one order of magnitude lower than that of the AGN. The basic physical and structural properties of the extended emission are fully consistent with a galactic wind being driven by the starburst (no contribution to the feedback by the AGN is required). A candidate ultra-luminous X-ray source is detected 8\\arcsec\\ south of the southern nucleus. The 0.3-10 keV luminosity of this off-nuclear point source is ~$6\\times 10^{40}$ erg s$^{-1}$ if the emission is isotropic and the source is associated with the Superantennae.", "label": 1, "domain": "academic", "token_count": 377, "matched_pair_id": "conditionality_00444", "split": "train"}
{"id": "conditionality_train_pos_0490", "text": "If you were hoping to snag a ticket to Easton's most celebrity-packed retirement party, you might be out of luck. The State Theatre announced Monday that \"Boak's Bash,\" the Jan. 6 tribute concert for C.F. Martin and Co.'s retiring Director of Museum and Archives Dick Boak, sold out before tickets became available to the general public. The show, first announced on Dec. 4, is slated to feature Boak's celebrity friends and clients like iconic blues rocker Steve Miller and blues/pop star John Mayer. State Theatre members did get a chance to grab a seat: Tickets, which cost $85 to $184, went on sale to the venue's members on Tuesday, Dec. 5. But the sale for the general public, which had been announced for Dec. 12 at 10 a.m., has been scrapped because of the sell-out. In the initial announcement for the show, the State Theatre cautioned that \"limited tickets\" had been made available to the venue for the event. Other stars scheduled to appear at the event include country legend Marty Stuart, former Wings lead guitarist Laurence Juber, former Jefferson Airplane guitarist Jorma Kaukonen, singer-songwriter David Bromberg, local musician Craig Thatcher and guitarist Trevor Gordon Hall. Boak earned these high-profile fans throughout a career at Martin Guitar that spanned four decades and included a number of different roles. He is known for launching the company's signature guitar series. A retrospective art show looking back on Boak's career in the State Theatre's Easton Hospital Gallery will accompany the concert. Proceeds from the concert will benefit the State Theatre. Andrew Doerfler may be reached at adoerfler@njadvancemedia.com. Follow him on Twitter @adoerfler or on Facebook.", "label": 1, "domain": "news", "token_count": 368, "matched_pair_id": "conditionality_00650", "split": "train"}
{"id": "conditionality_train_pos_0491", "text": "We combine the CfA3 supernova Type Ia (SN Ia) sample with samples from the literature to calculate improved constraints on the dark energy equation of state parameter, w. The CfA3 sample is added to the Union set of Kowalski et al. (2008) to form the Constitution set and, combined with a BAO prior, produces 1+w=0.013 +0.066/-0.068 (0.11 syst), consistent with the cosmological constant. The CfA3 addition makes the cosmologically-useful sample of nearby SN Ia between 2.6 and 2.9 times larger than before, reducing the statistical uncertainty to the point where systematics play the largest role. We use four light curve fitters to test for systematic differences: SALT, SALT2, MLCS2k2 (R_V=3.1), and MLCS2k2 (R_V=1.7). SALT produces high-redshift Hubble residuals with systematic trends versus color and larger scatter than MLCS2k2. MLCS2k2 overestimates the intrinsic luminosity of SN Ia with 0.7 < Delta < 1.2. MLCS2k2 with R_V=3.1 overestimates host-galaxy extinction while R_V=1.7 does not. Our investigation is consistent with no Hubble bubble. We also find that, after light-curve correction, SN Ia in Scd/Sd/Irr hosts are intrinsically fainter than those in E/S0 hosts by 2 sigma, suggesting that they may come from different populations. We also find that SN Ia in Scd/Sd/Irr hosts have low scatter (0.1 mag) and reddening. Current systematic errors can be reduced by improving SN Ia photometric accuracy, by including the CfA3 sample to retrain light-curve fitters, by combining optical SN Ia photometry with near-infrared photometry to understand host-galaxy extinction, and by determining if different environments give rise to different intrinsic SN Ia luminosity after correction for light-curve shape and color.", "label": 1, "domain": "academic", "token_count": 444, "matched_pair_id": "conditionality_00116", "split": "train"}
{"id": "conditionality_train_pos_0492", "text": "if there is no display, at the point of sale. Such information shall also include information on recycling old televisions and other consumer electronics. ``(3) Other devices.--For devices other than television sets that are included in section 303(s) and that contain an analog tuner, but not a digital tuner, the Commission shall require the clear and conspicuous placement of a comparable consumer advisory label on such devices, as well as on the outside of the retail packaging of such devices. ``(4) Additional disclosures.-- ``(A) Announcements and notices required.--From November 1, 2007, through March 31, 2009-- ``(i) each television broadcaster shall air, at a minimum, 120 seconds per day of public service announcements between the hours of 6 a.m. and 11:35 p.m., at variable time slots throughout the week, with at least half aired between the hours of 5 p.m. and 11:35 p.m.; and ``(ii) any multichannel video program distributor shall include a notice in or with each periodic bill. ``(B) Content of announcements and notices.--The announcements and notices required by this paragraph shall educate consumers about the deadline for termination of analog television broadcasting and the equipment options consumers have after such termination. Announcements aired and notices distributed after January 1, 2008, shall also educate consumers about the need for and availability of the converter box voucher program and the steps to redeem the voucher. ``(5) Advisory committee.-- ``(A) Establishment.--The Commission shall, after consultation with the National Telecommunications and Information Administration and the Federal Trade Commission, create a DTV Transition Federal Advisory Committee to lead the effort to educate the public about the digital television transition and to ensure that the public knows the information described in paragraph (3)(B). Such consumer education shall commence no later than September 1, 2007. ``(B) Composition.--The committee shall be composed of representatives from the following groups: commercial broadcasters, noncommercial broadcasters, cable operators, satellite providers, retailers and manufacturers of consumer electronics equipment, electronic recyclers, minority groups, Hispanic Americans, Americans whose primary language is not English, Americans with disabilities, Americans living in rural communities, general business, senior citizens, commercial advertising, and consumers in general. ``(C) Advisory committee role.--The committee shall-- ``(i) develop a comprehensive education plan for consumers regarding the digital television transition which includes-- ``(I) specific and targeted messages to reach", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00863", "split": "train"}
{"id": "conditionality_train_pos_0493", "text": "We calculate the masses of bottom mesons using an improved relativistic action for the b-quarks and the RBC/UKQCD Iwasaki gauge configurations with 2+1 flavors of dynamical domain-wall light quarks. We analyze configurations with two lattice spacings: a^{-1} = 1.729 GeV (a ~ 0.11 fm) and a^{-1} = 2.281 GeV (a ~ 0.086 fm). We use an anisotropic, clover-improved Wilson action for the b-quark, and tune the three parameters of the action nonperturbatively such that they reproduce the experimental values of the B_s and B_s* heavy-light meson states. The masses and mass-splittings of the low-lying bottomonium states (such as the eta_b and Upsilon) can then be computed with no additional inputs, and comparison between these predictions and experiment provides a test of the validity of our method. We obtain bottomonium masses with total uncertainties of ~0.5-0.6% and fine-structure splittings with uncertainties of ~35-45%; for all cases we find good agreement with experiment. The parameters of the relativistic heavy-quark action tuned for b-quarks presented in this work can be used for precise calculations of weak matrix elements such as B-meson decay constants and mixing parameters with lattice discretization errors that are of the same size as in light pseudoscalar meson quantities. This general method can also be used for charmed meson masses and matrix elements if the parameters of the heavy-quark action are appropriately tuned.", "label": 1, "domain": "academic", "token_count": 331, "matched_pair_id": "conditionality_00465", "split": "train"}
{"id": "conditionality_train_pos_0494", "text": "The article was published electronically by a peer-reviewed scientific journal, the Proceedings of the National Academy of Sciences. The researchers did some mathematical modeling and computer simulations to determine how likely people were to come close to a hypothetical infectious passenger sitting in an aisle seat on the 14th row of a single-aisle airplane. They concluded that on average, only one person on a flight of about 150 passengers would be infected. Researchers who were not involved said it would be difficult to use the relatively small study to make any general conclusions about the risks of an airline passenger getting a cold or flu, let alone other diseases like measles or tuberculosis. But it’s a novel study about a subject that hasn’t been well researched, they said. Studies have looked at how respiratory viruses spread in labs and in homes, but “this is the first time I’ve seen it done for airplanes,” said Seema Lakdawala, a University of Pittsburgh biologist who studies how flu spreads. She and others not involved in the research were intrigued by the study’s findings about how people moved about the cabin and came in contact with each other. It found: About 38 percent of passengers never left their seat, 38 percent left once, 13 percent left twice, and 11 percent left more than twice. Not surprisingly, a lot of the people getting up had an aisle seat. About 80 percent of people sitting on the aisle moved at least once during their flights, compared with 62 percent in middle seats and 43 percent in window seats. The 11 people sitting closest to a person with a cold or flu are at the highest risk. That included two people sitting to their left, the two to their right, and people in the row immediately in front of them and those in the row behind. A lot of frequent fliers will be interested in the study’s results, said Edward Pizzarello, an investor in a Washington-area venture-capital firm who also writes a travel blog. “It’s absolutely a fear I hear from people all the time. They just believe that they’re going to get sick from going on an airplane, or they got sick from being on an airplane,” he said. Pizzarello said he’s an aisle person, because he doesn’t want to feel trapped in the window seat if he needs to get up. Will he now go for the window? Maybe, he said, if a sick person sits next to him.", "label": 1, "domain": "news", "token_count": 493, "matched_pair_id": "conditionality_00815", "split": "train"}
{"id": "conditionality_train_pos_0495", "text": "Low temperature specific heat, C, in magnetic fields up to Hc2 is reported for underdoped Ba(Fe0.955Co0.045)2As2 (Tc=8 K) and for three overdoped samples Ba(Fe1-xCox)2As2 (x=0.103, 0.13, and 0.15, Tc=17.2, 16.5, and 11.7 K respectively). Previous measurements of thermal conductivity (as a function of temperature and field) and penetration depth on comparable composition samples gave some disagreement as to whether there was fully gapped/nodal behavior in the under-/overdoped materials respectively. The present work shows that the measured behavior of the specific heat gamma (proportional to C/T as T->0, i. e. a measure of the electronic density of states at the Fermi energy) as a function of field approximately obeys gamma proportional to H**(0.5 +- 0.1), similar to the Volovik effect for nodal superconductors, for both the underdoped and the most overdoped Co samples. However, for the two overdoped compositions x=0.103 and 0.13, the low field (H < 10 T) data show a Volovik-like behavior of gamma proportional to H**(0.3-0.4), followed by an inflection point, followed at higher fields by gamma proportional to H**1. We argue that within the 2-band theory of superconductivity, an inflection point may occur if the interband coupling is dominant.", "label": 1, "domain": "academic", "token_count": 333, "matched_pair_id": "conditionality_00472", "split": "train"}
{"id": "conditionality_train_pos_0496", "text": "We present the first results from a near-IR spectroscopic campaign of the Cl1604 supercluster at z~0.9 and the cluster RX J1821.6+6827 at z~0.82 to investigate the nature of [OII] 3727A emission in cluster galaxies at high redshift. Of the 401 members in the two systems, 131 galaxies have detectable [OII] emission with no other signs of current star-formation, as well as strong absorption features indicative of a well-established older stellar population. The combination of these features suggests that the primary source of [OII] emission in these galaxies is not the result of star-formation, but rather due to the presence of a LINER or Seyfert component. Using the NIRSPEC spectrograph on the Keck II 10-m telescope, 19 such galaxies were targeted, as well as six additional [OII]-emitting cluster members that exhibited other signs of ongoing star-formation. Nearly half (~47%) of the 19 [OII]-emitting, absorption-line dominated galaxies exhibit [OII] to Ha equivalent width ratios higher than unity, the typical value for star-forming galaxies. A majority (~68%) of these 19 galaxies are classified as LINER/Seyfert based on the emission-line ratio of [NII] and Ha, increasing to ~85% for red [OII]-emitting, absorption-line dominated galaxies. The LINER/Seyfert galaxies exhibit L([OII])/L(Ha) ratios significantly higher than that observed in populations of star-forming galaxies, suggesting that [OII] is a poor indicator of star-formation in a large fraction of high-redshift cluster members. We estimate that at least ~20% of galaxies in high-redshift clusters contain a LINER/Seyfert component that can be revealed with line ratios. We also investigate the effect this population has on the star formation rate of cluster galaxies and the post-starburst fraction, concluding that LINER/Seyferts must be accounted for if these quantities are to be meaningful.", "label": 1, "domain": "academic", "token_count": 429, "matched_pair_id": "conditionality_00205", "split": "train"}
{"id": "conditionality_train_pos_0497", "text": "If there’s one thing casual photographers are guilty of, it’s leaving their images on a memory card. Sure, memory card capacities are so large that you may never have to offload them, but they end up becoming digital graveyards for your photos and videos. Canon has created a new device, called the Connect Station, that’s designed to put all that content on the big screen, and share it. The company debuted the new product category at the 2015 International CES Show. First previewed at Photokina in 2014 (codenamed Cross Media Station), the Connect Station CS100 ($300) is essentially a network-attached storage (NAS) device, a 1TB portable hard drive connected to a home network that lets you archive, display, and share images and videos taken with a digital camera and camcorder. Updated on February 14, 2017: Canon issued a firmware update that adds support for non-Canon cameras, improves smartphone compatibility, and allows for playback of videos that have been edited on a computer, making the device a bit more flexible. Updated on July 14, 2016: Canon released a new mobile app for the CS100 that would allow users to view and back-up images from their phones or tablets. This article, originally published on January 5, 2015, has been updated to reflect the changes. The idea for such a product isn’t new, as there are other similar media storage and sharing drives available (in fact, Canon had a prototype of it five years ago, although that early version used different technologies). But the CS100, with near-field communication (NFC) and Wi-Fi built in, was designed to help Canon camera and camcorder owners get content off their media cards and give them a viewing experience they can enjoy. The CS100 is a standalone product that doesn’t require a computer to function, although it does need to be connected to a TV in order to view content and menus; it supports Full HD displays via HDMI. To add content, you can transfer photos and videos wirelessly from Wi-Fi-enabled Canon cameras and camcorders (NFC helps to facilitate the pairing and download processes quickly); directly off an SD or Compact Flash card through the built-in card reader; or from a compatible camera or flash drive through the USB port. Although it uses the 802.11n Wi-Fi protocol, it’s much faster to insert a memory card. The CS100 also", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00724", "split": "train"}
{"id": "conditionality_train_pos_0498", "text": "We take deep images of four ultra faint dwarf (UFD) galaxies, Canes Venatici I (CVn I), Bootes I (Boo I), Canes Venatici II (CVn II), and Leo IV using the Suprime-Cam on the Subaru Telescope. The colour-magitude diagrams (CMDs) extend below the main sequence turn-offs (MSTOs) and yield measurements of the ages of stellar populations. The stellar populations of faint three galaxies, Boo I, CVn II and Leo IV dwarf spheroidal galaxies (dSphs) are estimated as old as a Galactic globular cluster M92. We confirm that Boo I dSph has no intrinsic colour spread in the MSTO, and no spatial difference in the CMD morphology, which indicates that Boo I dSph is composed of an old single stellar population. One of the brightest UFDs, CVn I dSph, shows a relatively younger age (-12.6 Gyr) with respect to Boo I, CVn II, and Leo IV dSphs, and the distribution of red horizontal branch (HB) stars is more concentrated toward the centre than that of blue HB stars, suggesting that the galaxy contains complex stellar populations. Boo I and CVn I dSphs show the elongated and distorted shapes. CVn II dSph has the smallest tidal radius as a Milky Way satellite and has distorted shape, while Leo IV dSph shows less concentrated spherical shape. The simple stellar population of faint UFDs indicates that the gases in their progenitors were removed more effectively than those of brighter dSphs at an occurrence of their initial star formation. This is reasonable if the progenitors of UFDs belong to the less massive halos than those of brighter dSphs.", "label": 1, "domain": "academic", "token_count": 371, "matched_pair_id": "conditionality_00381", "split": "train"}
{"id": "conditionality_train_pos_0499", "text": "This work provides a statistical analysis of the massive star binary characteristics in the Cygnus OB2 Association using radial velocity information of 114 B3-O3 primary stars and orbital properties for the 24 known binaries. We compare these data to a series of Monte Carlo simulations to infer the intrinsic binary fraction and distributions of mass ratios, periods, and eccentricities. We model the distribution of mass ratio, log-period, and eccentricity as power-laws and find best fitting indices of alpha=0.1+/-0.5, beta=0.2+/-0.4, and gamma=-0.6+/-0.3 respectively. These distributions indicate a preference for massive companions, short periods, and low eccentricities. Our analysis indicates that the binary fraction of the cluster is 44+/-8% if all binary systems are (artificially) assumed to have P<1000 days; if the power-law period distribution is extrapolated to 10^4 years, a plausible upper limit for bound systems, the binary fraction is ~90+/-10%. Of these binary (or higher order) systems, ~45% will have companions close enough to interact during pre- or post-main-sequence evolution (semi-major axis ~/<4.7 AU). The period distribution for P<27 days is not well reproduced by any single power-law owing to an excess of systems with periods around 3-5 days (0.08-0.31 AU) and a relative shortage of systems with periods around 7-14 days (0.14-0.62 AU). We explore the idea that these longer-period systems evolved to produce the observed excess of short-period systems. The best fitting binary parameters imply that secondaries generate, on average, ~16% of the V-band light in young massive populations. This means that photometrically based distance measurements for young massive clusters & associations will be systematically low by ~8% (0.16 mag in the distance modulus) if the luminous contributions of unresolved secondaries are not taken into account.", "label": 1, "domain": "academic", "token_count": 418, "matched_pair_id": "conditionality_00427", "split": "train"}
{"id": "conditionality_train_pos_0500", "text": "of 2003, is amended to read as follows: ``(3) Qualifying plan defined.--For purposes of this section, the term `qualifying plan' means a prescription drug plan offered by a PDP sponsor.''. SEC. 6. REPEAL OF MA REGIONAL PLAN STABILIZATION FUND. (a) In General.--Section 1858 of the Social Security Act, as added by section 221(c) of the Medicare Prescription Drug, Improvement, and Modernization Act of 2003, is amended-- (1) by striking subsection (e); (2) by redesignating subsections (f), (g), and (h) as subsections (e), (f), and (g), respectively; and (3) in subsection (e), as so redesignated, by striking ``subject to subsection (e),''. (b) Conforming Amendment.--Section 1851(i)(2) of the Social Security Act (42 U.S.C. 1395w-21(i)(2)), as amended by section 221(d)(5) of the Medicare Prescription Drug, Improvement, and Modernization Act of 2003, is amended by striking ``1858(h)'' and inserting ``1858(g)''. SEC. 7. REPEAL OF HEALTH SAVINGS ACCOUNTS. Section 1201 of the Medicare Prescription Drug, Improvement, and Modernization Act of 2003, and the amendments made by such section, are repealed. SEC. 8. EFFECTIVE DATE. (a) In General.--The amendments made by this Act shall take effect as if included in the enactment of the Medicare Prescription Drug, Improvement, and Modernization Act of 2003. (b) Application of Laws.--If any amendment to any provision of any Act is repealed by this Act, such provision shall be applied and administered as if the amendment had never been enacted.", "label": 1, "domain": "government", "token_count": 390, "matched_pair_id": "conditionality_00963", "split": "train"}
{"id": "conditionality_train_pos_0501", "text": "Using a one-dimensional height integrated model, we calculate the evolution of an unequal mass binary black hole with a coplanar gas disk that contains a gap due to the presence of the secondary black hole. Viscous evolution of the outer circumbinary disk initially hardens the binary, while the inner disk drains onto the primary (central) black hole. As long as the inner disk remains cool and thin at low $\\dot{M}_{\\rm ext}$ (rather than becoming hot and geometrically thick), the mass of the inner disk reaches an asymptotic mass typically $\\sim 10^{-3}-10^{-4}\\Msun$. Once the semimajor axis shrinks below a critical value, angular momentum losses from gravitational waves dominate over viscous transport in hardening the binary. The inner disk then no longer responds viscously to the inspiraling black holes. Instead, tidal interactions with the secondary rapidly drive the inner disk into the primary. Tidal and viscous dissipation in the inner disk lead to a late time brightening in luminosity $L\\propto t_{\\rm minus}^{5/4}$, where $t_{\\rm minus}$ is the time prior to the final merger. This late time brightening peaks $\\sim 1$ day prior to the final merger at $\\sim 0.1 L_{\\rm Edd}$. This behavior is relatively robust because of self regulation in the coupled viscous-gravitational evolution of such binary systems. It constitutes a unique electromagnetic signature of a binary supermassive black hole merger and may allow the host galaxy to be identified if used in conjunction with the Laser Interferometric Space Antenna (LISA) localization.", "label": 1, "domain": "academic", "token_count": 343, "matched_pair_id": "conditionality_00141", "split": "train"}
{"id": "conditionality_train_pos_0502", "text": "if applicable), adjusted under section 8462. ``(3) A reduction under this section-- ``(A) shall become effective as of the effective date of the election under subsection (b) or (c) of section 8416 or section 8417(b), as the case may be; ``(B) shall not be terminated on account of a change in marital status or for any other reason; and ``(C) shall be in addition to any reduction under section 8419(a) or 8420. ``(c) Subsections (a) and (b) shall not apply with respect to an election under section 8416 or 8417(b) if-- ``(1) the employee or Member makes such election after having made an election under section 8420; and ``(2) the election under section 8420 becomes void under section 8416 (b)(3) or (c)(2). ``(d) That the total amount withheld under this section from the annuity of an employee or Member, as of time of death or other annuity- terminating event, is less than the amount described in subsection (a) (including interest) shall not affect either the entitlement of such employee's or Member's survivor to receive the annuity elected for such survivor under section 8416 (b) or (c) or section 8417 (as the case may be) or the amount of such survivor annuity.''. (b) Technical and Conforming Amendments.--(1) Section 8416(b)(2) of title 5, United States Code, is amended by striking ``be effective'' and inserting ``become effective''. (2) The first sentence of section 8416(c)(2) of title 5, United States Code, is amended to read as follows: ``The election and reduction shall become effective the first day of the second month after the election is received by the Office, but not less than 9 months after the date of the marriage.''. (3) Section 8417(b)(2) of title 5, United States Code, is amended to read as follows: ``(2) An election under this subsection-- ``(A) shall be made at the time of retirement or, if the marriage is dissolved after the date of retirement, within 2 years after the date on which the marriage of the former spouse to the employee or Member is dissolved; and ``(B) shall become effective the first day", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00984", "split": "train"}
{"id": "conditionality_train_pos_0503", "text": "Supernovae Ib/c are likely to be associated to long GRBs, therefore it is important to compare the SN rate in galaxies with the GRB rate. To do that we computed Type Ib/c SN rates in galaxies of different morphological type by assuming different histories of star formation and different supernova Ib/c progenitors. We included some recent suggestions about the dependence of the minimum mass of single Wolf-Rayet (WR) stars upon the stellar metallicity and therefore upon galactic chemical evolution. We adopted several cosmic star formation rates as functions of cosmic time, either observationally or theoretically derived, including the one computed with our galaxy models. Then we computed the cosmic Type Ib/c SN rates. We derived the following conclusions: i) the ratio cosmic GRB - Type Ib/c rate varies in the range 10^{-2}-10^{-4} in the whole redshift range, thus suggesting that only a small fraction of all the Type Ib/c SNe gives rise to GRBs. ii) The metallicity dependence of Type Ib/c SN progenitors produces lower cosmic SN Ib/c rates at early times, for any chosen cosmic star formation rate. iii) Different theoretical cosmic star formation rates, computed under different scenarios of galaxy formation, produce SN Ib/c cosmic rates which differ mainly at very high redshift. However, it is difficult to draw firm conclusions on the high redshift trend because of the large uncertainties in the data. iv) GRBs can be important tracers of star formation at high redshift if their luminosity function does not vary with redshift and they can help in discriminating among different galaxy formation models.", "label": 1, "domain": "academic", "token_count": 327, "matched_pair_id": "conditionality_00440", "split": "train"}
{"id": "conditionality_train_pos_0504", "text": "We have studied formation of planetesimals at a radial pressure bump in a protoplanetary disk created by radially inhomogeneous magnetorotational instability (MRI), through three-dimensional resistive MHD simulations including dust particles. In our previous papers, we showed that the inhomogeneous MRI developing in non-uniform structure of magnetic field or magnetic resistivity can transform the local gas flow in the disk to a quasi-steady state with local rigid rotation that is no more unstable against the MRI. Since the outer part of the rigid rotation is super-Keplerian flow, a quasi-static pressure bump is created and dust concentration is expected there. In this paper, we perform simulations of the same systems, adding dust particles that suffer gas drag and modulate gas flow via the back-reaction of the gas drag (dust drag). We use O(10^7) super-particles, each of which represents many dust particles with sizes of centimeter to meter. We have found that the dust drag suppresses turbulent motion to decrease the velocity dispersion of the dust particles while it broadens the dust concentrated regions to limit peaky dust concentration, compared with the simulation without the dust drag. We found that reduction in the velocity dispersion) is dominated over the suppression in particle concentration. For meter-size particles with the friction time ~1/Omega, where Omega is Keplerian frequency, the gravitational instability of the dust particles that may lead to planetesimal formation is expected. For such a situation, we further introduced the self-gravity of dust particles to the simulation to demonstrate that several gravitationally bound clumps are actually formed. Through analytical arguments, we found that the planetesimal formation from meter-sized dust particles can be possible at ~5AU, if dust spatial density is a few times larger than that in the minimum mass solar nebula.", "label": 1, "domain": "academic", "token_count": 369, "matched_pair_id": "conditionality_00399", "split": "train"}
{"id": "conditionality_train_pos_0505", "text": "The possibility of inducing topological superconductivity with cuprate high-temperature superconductors (HTSC) is studied for various heterostructures. We first consider a ballistic planar junction between a HTSC and a metallic ferromagnet. We assume that inversion symmetry breaking at the tunnel barrier gives rise to Rashba spin-orbit coupling in the barrier and allows equal-spin triplet superconductivity to exist in the ferromagnet. Bogoliubov-de Gennes equations are obtained by explicitly modeling the barrier, and taking account of the transport anisotropy in the HTSC. By making use of the self-consistent boundary conditions and solutions for the barrier and HTSC regions, an effective equation of motion for the ferromagnet is obtained where Andreev scattering at the barrier is incorporated as a boundary condition for the ferromagnetic region. For a ferromagnet layer deposited on a (100) facet of the HTSC, triplet p-wave superconductivity is induced. For the layer deposited on a (110) facet, the induced gap does not have the p-wave orbital character, but has an even orbital symmetry and an odd dependence on energy. For the layer on the (001) facet, an exotic f-wave superconductivity is induced. We also consider the induced triplet gap in a one-dimensional half-metallic nanowire deposited on a (001) facet of a HTSC. We find that for a wire axis along the a-axis, a robust triplet p-wave gap is induced. For a wire oriented 45 degrees away from the a-axis the induced triplet p-wave gap vanishes. For the appropriately oriented wire, the induced p-wave gap should give rise to Majorana fermions at the ends of the half-metallic wire. Based on our result, topological superconductivity in a semi-conductor nanowire may also be possible given that it is oriented along the a-axis of the HTSC.", "label": 1, "domain": "academic", "token_count": 390, "matched_pair_id": "conditionality_00468", "split": "train"}
{"id": "conditionality_train_pos_0506", "text": "SGR 0418+5729 is a transient Soft Gamma-ray Repeater which underwent a major outburst in June 2009, during which the emission of short bursts was observed. Its properties appeared quite typical of other sources of the same class until long-term X-ray monitoring failed to detect any period derivative. The present upper limit on $\\dot P$ implies that the surface dipole field is $B_p\\lesssim 7.5\\times 10^{12}\\ {\\rm G}$ (Rea et al 2010), well below those measured in other Soft Gamma-ray Repeaters (SGRs) and in the Anomalous X-ray Pulsars (AXPs), a group of similar sources. Both SGRs and AXPs are currently believed to be powered by ultra-magnetized neutron stars (magnetars, $B_p\\approx 10^{14}$--$10^{15}\\ {\\rm G}$). SGR 0418+5729 hardly seems to fit in such a picture. We show that the magneto-rotational properties of SGR 0418+5729 can be reproduced if this is an aged magnetar, $\\approx 1\\ {\\rm Myr}$ old, which experienced substantial field decay. The large initial toroidal component of the internal field required to match the observed properties of SGR 0418+5729 ensures that crustal fractures, and hence bursting activity, can still occur at present time. The thermal spectrum observed during the outburst decay is compatible with the predictions of a resonant compton scattering model (as in other SGRs/AXPs) if the field is low and the magnetospheric twist moderate.", "label": 1, "domain": "academic", "token_count": 347, "matched_pair_id": "conditionality_00363", "split": "train"}
{"id": "conditionality_train_pos_0507", "text": "If you know anything about Odyssey already, it’s probably that it’s the Mario game with actual humans in it. These people - as opposed to whatever kind of being the moustached one is - all reside in New Donk City: which marries New York with a litany of Donkey Kong references both obvious and obscure. For example, the mayor of city is the same Pauline that Jumpman (a.k.a. Mario) tried to rescue way back in 1981. While we didn’t catch sight of ol’ DK himself, it seems impossible that he won’t turn up in the final game. In the meantime, we were contented ourselves with collecting Power Moons that fuel Mario’s ship - the Odyssey - and further his quest to rescue the kidnapped Princess Peach from Bowser planned wedding to her. While it’s a shame that the most revolutionary Mario game yet is still happy to stick with Peach as a damsel-in-distress, the idea of scattering a load of collectables across one huge world is a good one. Even in our brief time with Odyssey, we found loads Power Moons scattered around New Donk City. From secret levels below manholes to the top of the Empire State Building, this game makes a great effort to reward your curiosity and the same went for our time in the sunny climes of the Sand Kingdom. That you can go from playing an 8-bit, 2D side-scrolling section to leaping about on a Sphinx-like taxi called a Jaxi in the space of a minute speaks volumes of the creativity that’s been crammed into the game. Better still, each world we delved into had its own unique art style and challenges. Rather than sticking to the usual formula of fire world, ice world, water world, it seems as though Nintendo has done its utmost to break conventions and confound expectations. Having gone into our time with Odyssey with some degree of suspicion how everything would fit together, we came out of it wanting to see just how ludicrous it might get.", "label": 1, "domain": "news", "token_count": 411, "matched_pair_id": "conditionality_00690", "split": "train"}
{"id": "conditionality_train_pos_0508", "text": "The magnetic flux periodicity in superconducting loops is reviewed. Whereas quantization of the magnetic flux with hc/2e prevails in sufficiently thick loops with current free interior, the supercurrent in narrow loops is either hc/2e or hc/e periodic with the external magnetic flux. The periodicity depends on the properties of the condensate state, in particular on the Doppler shift of the energy spectrum. For an s-wave superconductor in a loop with diameter larger than the coherence length, the Doppler shift is small with respect to the energy gap, and the hc/2e periodic behavior of its flux dependent thermodynamic properties is maintained. However, for smaller s-wave loops and, more prominently, narrow d-wave loops of any diameter R, the Doppler shift has a strong effect on the supercurrent carrying state; as a consequence, the fundamental flux periodicity is in fact hc/e. It is shown analytically and numerically that the hc/e periodic component in the supercurrent decays only algebraically as 1/R for large d-wave loops. For nodal superconductors the discrete nature of the eigenergies close to the Fermi energy has to be respected in the evaluation of the Doppler shift. Furthermore, we investigate, whether the Doppler shift modifies the supercurrent through Josephson junctions with d-wave superconductors. For transparent junctions, the Josephson current behaves similar to the persistent supercurrent in a loop. These distinct physical phenomena can be compared, if the magnetic flux in units of hc/e is identified with the phase variation of the order parameter divided by 4 pi.", "label": 1, "domain": "academic", "token_count": 330, "matched_pair_id": "conditionality_00222", "split": "train"}
{"id": "conditionality_train_pos_0509", "text": "If you're after a computer close to the size of the tiny Raspberry Pi but approaching the power of the MacBook, then you may want to check out the LattePanda Alpha. However, it's worth noting the LattePanda Alpha is not a Pi competitor. While the Pi costs just $35, the LattePanda Alpha starts at $289. The difference is reflected in the specs, with the LattePanda Alpha having more in common with a laptop than a low-cost board like the Pi. The LattePanda Alpha uses the same class of Intel processor as found in this year's 12-inch MacBook, a 7th generation, Intel Core m3. Backing up this processor is 8GB of DDR3 memory and 64GB Flash storage, alongside Gigabit Ethernet, 802.11ac Wi-Fi and USB 3.0 ports, a USB Type-C port, 4K video out. While the board's makers DFRobot say the Alpha will ship with Windows 10 Pro, they add it will also be compatible with a range of Linux-based OSes. The board—which is about 70% the length of the iPhone 7 Plus—is designed to be used to be used by developers working in a wide range of fields, from robotics to internet of things, and as such has the necessary electronics for adding a wide-range of custom hardware to the board. SEE: Hardware spotlight: The Raspberry Pi The Alpha has 2 x 50-Pin headers for hooking up hardware, as well as an Arduino Leonardo co-processor. Alongside the Alpha, the board's makers will also release a version of the board without the eMMC storage for $269, as well as the lower-specced LattePanda Delta, which starts at $129. The Delta runs on an Intel Celeron N4100 processor, has 4GB of RAM but still keeps many of the advantages of the Alpha board, such as 802.11ac Wi-Fi and 3 x USB 3.0 ports. Both boards are being crowdfunded via Kickstarter, and as of publication have passed their £72,611 funding target, with just shy of £97,000 raised with 56 days left to go. DFRobot estimate that the boards, which are also available with a 7-inch touchscreen display, will ship in May next year. It is not the first Windows 10-based, developer board", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00502", "split": "train"}
{"id": "conditionality_train_pos_0510", "text": "Astrometric measurements of stellar systems are becoming significantly more precise and common, with many ground and space-based instruments and missions approaching 1 microarcsecond precision. We examine the multi-wavelength astrometric orbits of exoplanetary systems via both analytical formulae and numerical modeling. Exoplanets have a combination of reflected and thermally emitted light that cause the photocenter of the system to shift increasingly farther away from the host star with increasing wavelength. We find that, if observed at long enough wavelengths, the planet can dominate the astrometric motion of the system, and thus it is possible to directly measure the orbits of both the planet and star, and thus directly determine the physical masses of the star and planet, using multi-wavelength astrometry. In general, this technique works best for, though is certainly not limited to, systems that have large, high-mass stars and large, low-mass planets, which is a unique parameter space not covered by other exoplanet characterization techniques. Exoplanets that happen to transit their host star present unique cases where the physical radii of the planet and star can be directly determined via astrometry alone. Planetary albedos and day-night contrast ratios may also be probed via this technique due to the unique signature they impart on the observed astrometric orbits. We develop a tool to examine the prospects for near-term detection of this effect, and give examples of some exoplanets that appear to be good targets for detection in the K to N infrared observing bands, if the required precision can be achieved.", "label": 1, "domain": "academic", "token_count": 316, "matched_pair_id": "conditionality_00424", "split": "train"}
{"id": "conditionality_train_pos_0511", "text": "We investigate the quantitative constraint on the triple-alpha reaction rate based on stellar evolution theory, motivated by the recent significant revision of the rate proposed by nuclear physics calculations. Targeted stellar models were computed in order to investigate the impact of that rate in the mass range of 0.8 < M / Msun < 25 and in the metallicity range between Z = 0 and Z = 0.02. The revised rate has a significant impact on the evolution of low- and intermediate-mass stars, while its influence on the evolution of massive stars (M >~ 10 Msun) is minimal. We find that employing the revised rate suppresses helium shell flashes on AGB phase for stars in the initial mass range 0.8 < M / Msun < 6, which is contradictory to what is observed. The absence of helium shell flashes is due to the weak temperature dependence of the revised triple-alpha reaction cross section at the temperature involved. In our models, it is suggested that the temperature dependence of the cross section should have at least nu > 10 at T = 1 - 1.2 x 10^8 K where the cross section is proportional to T^{nu}. We also derive the helium ignition curve to estimate the maximum cross section to retain the low-mass first red giants. The semi-analytically derived ignition curves suggest that the reaction rate should be less than ~ 10^{-29} cm^6 s^{-1} mole^{-2} at ~ 10^{7.8} K, which corresponds to about three orders of magnitude larger than that of the NACRE compilation. In an effort to compromise with the revised rates, we calculate and analyze models with enhanced CNO cycle reaction rates to increase the maximum luminosity of the first giant branch. However, it is impossible to reach the typical RGB tip luminosity even if all the reaction rates related to CNO cycles are enhanced by more than ten orders of magnitude.", "label": 1, "domain": "academic", "token_count": 398, "matched_pair_id": "conditionality_00361", "split": "train"}
{"id": "conditionality_train_pos_0512", "text": "If the activity of active galactic nuclei (AGNs) is predominantly induced by major galaxy mergers, then a significant fraction of AGNs should harbor binary massive black holes in their centers. We study the mass function of binary massive black holes in nearby AGNs based on the observed AGN black-hole mass function and theory of evolution of binary massive black holes interacting with a massive circumbinary disk in the framework of coevolution of massive black holes and their host galaxies. The circumbinary disk is assumed to be steady, axisymmetric, geometrically thin, self-regulated, self-gravitating but non-fragmenting with a fraction of Eddington accretion rate, which is typically one tenth of Eddington value. The timescale of orbital decay is {then} estimated as ~10^8yr for equal mass black-hole, being independent of the black hole mass, semi-major axis, and viscosity parameter but dependent on the black-hole mass ratio, Eddington ratio, and mass-to-energy conversion efficiency. This makes it possible for any binary massive black holes to merge within a Hubble time by the binary-disk interaction. We find that (1.8+-0.6%) for the equal mass ratio and (1.6+-0.4%) for the one-tenth mass ratio of the total number of nearby AGNs have close binary massive black holes with orbital period less than ten years in their centers, detectable with on-going highly sensitive X-ray monitors such as Monitor of All-sky X-ray Image and/or Swift/Burst Alert Telescope. Assuming that all binary massive black holes have the equal mass ratio, about 20% of AGNs with black hole masses of 10^{6.5-7}M_sun has the close binaries and thus provides the best chance to detect them.", "label": 1, "domain": "academic", "token_count": 369, "matched_pair_id": "conditionality_00192", "split": "train"}
{"id": "conditionality_train_pos_0513", "text": "5,000,000 for fiscal year 1999, $7,500,000 for fiscal year 2000, and $9,000,000 for fiscal year 2001 to carry out section 129 of the Foreign Assistance Act, as added by subsection (a). (2) Availability of funds.--Amounts appropriated pursuant to this subsection shall remain available until expended. (c) Effective Date.--The amendment made by subsection (a) shall take effect on October 1, 1998. SEC. 9. MULTILATERAL ASSISTANCE. (a) Funding.--Of the amounts authorized to be appropriated for fiscal years 1999, 2000, and 2001 pursuant to chapter 1 of part I of the Foreign Assistance Act of 1961, there are authorized to be appropriated to the United Nations Voluntary Fund for Victims of Torture (in this section referred to as the ``Fund'') the following amounts for the following fiscal years: (1) Fiscal year 1999.--For fiscal year 1999, $3,000,000. (2) Fiscal year 2000.--For fiscal year 2000, $3,000,000. (3) Fiscal year 2001.--For fiscal year 2001, $3,000,000. (b) Availability of Funds.--Amounts appropriated pursuant to subsection (a) shall remain available until expended. (c) Sense of Congress.--It is the sense of Congress that the President, acting through the United States Permanent Representative to the United Nations, should-- (1) request the Fund-- (A) to find new ways to support and protect treatment centers and programs that are carrying out rehabilitative services for victims of torture; and (B) to encourage the development of new such centers and programs; (2) use the voice and vote of the United States to support the work of the Special Rapporteur on Torture and the Committee Against Torture established under the Convention Against Torture and Other Cruel, Inhuman or Degrading Treatment or Punishment; and (3) use the voice and vote of the United States to establish a country rapporteur or similar procedural mechanism to investigate human rights violations in a country if either the Special Rapporteur or the Committee Against Torture indicates that a systematic practice of torture is prevalent in that country.", "label": 1, "domain": "government", "token_count": 482, "matched_pair_id": "conditionality_01062", "split": "train"}
{"id": "conditionality_train_pos_0514", "text": "This dissertation focuses on phenomenological studies for possible signals for supersymmetric events at the Large Hadron Collider (LHC). We have divided our endeavours into three separate projects. First, we consider SUSY models where the gluino production at the LHC should be rich in top and bottom quark jets. Requiring $b$-jets in addition to missing energy $\\eslt$ should, therefore, enhance the supersymmetry signal relative to Standard Model backgrounds. We quantify the increase in the supersymmetry reach of the LHC from $b$-tagging in a variety of well-motivated models of supersymmetry. We also explore $top$-tagging at the LHC. Second, we explore the prospects for detecting the direct production of third generation squarks in models with an inverted squark mass hierarchy. This is signalled by $b$-jets + $\\eslt$ events harder than in the Standard Model, but softer than those from the production of gluinos and heavier squarks. We find that these events can be readily separated from SM background (for third generation squark masses in the 200-400 GeV range), and the contamination from the much heavier gluinos and squarks although formidable can effectively be suppressed. Third, we attempt to extract model-independent information about neutralino properties from LHC data. assuming only the particle content of the MSSM and that all two-body neutralino decays are kinematically suppressed, with the neutralino inclusive production yielding a sufficient cross section. We show that the Lorentz invariant dilepton mass distribution encodes clear information about the relative sign of the mass eigenvalues of the parent and daughter neutralinos. We show that we can extract most neutralino mass matrix parameters if there is a double mass edge.", "label": 1, "domain": "academic", "token_count": 363, "matched_pair_id": "conditionality_00448", "split": "train"}
{"id": "conditionality_train_pos_0515", "text": "With the legacy of Spitzer and current advances in (sub)mm astronomy, a large number of 'transitional' disks has been identified which are believed to contain gaps or have developped large inner holes, some filled with dust. This may indicate that complex geometries may be a key feature in disk evolution that has to be understood and modeled correctly. The disk around LkCa 15 is such a disk, with a gap ranging from ~5 - 50 AU, as identified by Espaillat et al. (2007) using 1+1D radiative transfer modelling. To fit the SED, they propose 2 possible scenarios for the inner (<5 AU) disk - optically thick or optically thin - and one scenario for the outer disk. We use the gapped disk of LkCa 15 as a showcase to illustrate the importance of 2D radiative transfer in transitional disks, by showing how the vertical dust distribution in dust-filled inner holes determines not only the radial optical depth but also the outer disk geometry. We use MCMax, a 2D radiative transfer code with a self-consistent vertical structure, to model the SED. We identify two possible geometries for the inner and outer disk, that are both different from those in Espaillat et al. (2007). An inner disk in hydrostatic equilibrium reprocesses enough starlight to fit the near infrared flux, but also casts a shadow on the inner rim of the outer disk. This requires the outer disk scale height to be large enough to rise out of the shadow. An optically thin inner disk does not cast such a shadow, and the SED can be fitted with a smaller outer disk scale height. For the dust in the inner regions to become optically thin however, the scale height would have to be so much larger than its hydrostatic equilibrium value that it effectively becomes a dust shell. It is currently unclear if a physical mechanism exists which could provide for such a configuration.", "label": 1, "domain": "academic", "token_count": 407, "matched_pair_id": "conditionality_00190", "split": "train"}
{"id": "conditionality_train_pos_0516", "text": "Clean Energy Leadership Act of 2009 is amended in the second sentence-- (1) in paragraph (6), by striking ``and'' after the semicolon at the end; (2) in paragraph (7), by striking the period at the end and inserting ``; and''; and (3) by adding at the end the following: ``(8) hydroelectric power technology.''. SEC. 14. REPORT ON MEMORANDUM OF UNDERSTANDING ON HYDROPOWER. Not later than 18 months after the date of enactment of this Act, the President shall submit to the Committee on Energy and Natural Resources of the Senate and the Committee on Energy and Commerce of the House of Representatives a report on actions taken by the Department of Energy, the Department of the Interior, and the Corps of Engineers to carry out the memorandum of understanding on hydropower entered into on March 24, 2010, with particular emphasis on actions taken by the agencies to work together and investigate ways to efficiently and responsibly facilitate the Federal permitting process for Federal and non-Federal hydropower projects at Federal facilities, within existing authority. SEC. 15. NONAPPLICATION TO FEDERAL POWER MARKETING ADMINISTRATIONS. (a) In General.--This Act and the amendments made by this Act shall not-- (1) apply to a hydroelectric project that provides power marketed by a Federal Power Marketing Administration; or (2) impact any additions, improvements, or replacements of hydroelectric generation at Federal projects carried out by a Federal Power Marketing Administration; (b) Modifications.--Nothing in this Act limits the authority under existing law of a Federal Power Marketing Administrator in the event that operations at Federal projects with hydropower facilities are modified. SEC. 16. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 444, "matched_pair_id": "conditionality_00951", "split": "train"}
{"id": "conditionality_train_pos_0517", "text": "if this group can bounce back, Quenneville had a short answer: \"We're going to have to.\" Chicago captain Jonathan Toews called it a very disappointing loss. His personal goal drought is now 12 straight postseason games, though he did have an assist. \"We got to find a way to put pressure on them, got to make them realize that winning a fourth game is the toughest for any team in any series,\" Toews said. Fiala finally converted on his third chance in overtime. Crawford got a glove on a puck nearly midway through the extra period off Fiala's shot from the high slot. Crawford also got his left toe on a shot from Fiala in the slot with 6:00 left. Then James Neal found Fiala with a pass, and he beat Crawford to send fans home shortly after midnight local time. \"It was a great save by Crawford,\" Fiala said of the toe save by the Chicago goalie. \"I was pretty angry, I could have finished it there, but never mind, we won.\" The Predators brought out the star power with country singer Carrie Underwood, married to Nashville captain Mike Fisher, to sing the national anthem. Five catfish also were tossed onto the ice before the puck dropped and combined with a late start for a very loud standing-room only crowd of 17,204. Nashville outshot Chicago 49-36. Rinne's shutout streak ended when Rasmussen scored the first postseason goal of his career 65 seconds into the second period. He beat Rinne glove-side off an assist from Marcus Kruger. The goal also snapped a scoreless skid for Chicago that spanned 177:45 back to their first-round loss to St. Louis last postseason. Then the Blackhawks quickly made it a 2-0 lead with a power-play goal by Kane. He scored the 50th postseason goal of his career with a wrister from the right circle at 11:15 of the second, taking advantage of Marcus Kruger standing in front of Rinne. Forsberg started the rally. He scored on a wrister hitting the puck in the air past Crawford, who was caught having turned around in the crease, at 4:24. Blackhawks forward Richard Panik argued the puck went off the netting, but the play was called a good goal after a review. \"It went off the shoulder and then off the glass and then straight in,", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00696", "split": "train"}
{"id": "conditionality_train_pos_0518", "text": "the lesser of-- ``(i) 50 percent of the portion of lifetime income payments (within the meaning of section 72(c)(5), applied with the substitutions described in subparagraph (B)) otherwise includible in gross income under this section (determined without regard to this paragraph), or ``(ii) the amount in effect under section 72(b)(5)(A). ``(B) Recapture and other special rules.--For purposes of this paragraph, rules similar to the rules of subparagraphs (D) and (E) of section 72(b)(5) and section 72(x) shall be applied by substituting `beneficiary of the life insurance contract' for `annuitant' and `life insurance contract' for `annuity contract' therein.''. (2) Conforming amendment.--Paragraph (1) of section 101(d) of such Code is amended by inserting ``or paragraph (3)'' after ``to the extent not excluded by the preceding sentence''. (e) Effective Date.-- (1) In general.--The amendments made by this section shall apply to amounts received in calendar years beginning after the date of the enactment of this Act. (2) Special rule for existing contracts.--In the case of a contract in force on the date of the enactment of this Act that does not satisfy the requirements of section 72(c)(5)(A) of the Internal Revenue Code of 1986 (as added by this section), any modification to such contract (including a change in ownership) or to the payments thereunder that is made to satisfy the requirements of such section shall not result in the recognition of any gain or loss, any amount being included in gross income, or any addition to tax that otherwise might result from such modification, but only if the modification is completed prior to the date that is 2 years after the date of the enactment of this Act.", "label": 1, "domain": "government", "token_count": 381, "matched_pair_id": "conditionality_00977", "split": "train"}
{"id": "conditionality_train_pos_0519", "text": "Unless you’re willing to spend upwards of £4000 on a Nikon D5 or Sony A9, this camera has the best feature set of any DSLR around. While those two full-frame rivals tend to be used more for action and sports than landscape, macro or portrait shots (largely due to their lower resolution sensors), the D850 is a genuine all-rounder, and a great one at that. You get both a super high resolution sensor, and a camera which copes reasonably well with fast-moving subjects. That’s thanks to an upgrade in frame rate – it can now shoot at 7.5fps (or 9fps if you attach the additional D850 grip), and the AF system is the same used in the fantastic D5. The D850 is capable of locking onto your subject very quickly and easily, even in lower light conditions. Moving subjects are also dealt with easily, especially for ones that have a reasonably predictable pattern of movement. The only complaint we have about autofocus is that all of the AF points are grouped towards the centre of the frame - that means that there will be occasions when you need to focus and recompose. To facilitate fast frame rates, the D850 has two memory card slots. One for SD, which is compatible with the fast UHS-II format. The other is for the even faster XQD format, though cards of this type can set you back upwards of £70 for 32GB, as right now they’re made by very few manufacturers. One of the downsides of having such a high resolution sensor is massive file sizes. In short, if you’re shooting both JPEGs and RAW files, you’re gonna need a bigger hard drive. Still, if you’re a professional working in the field who needs to get shots of a football match or a news event across quickly, you’ll be pleased to know that you can shoot in lower resolution modes and still have access to raw files. You can also use the great DX crop mode, which essentially works with the central part of the sensor as if you were using an APS-C sensor. If you’re wondering why you might want this, it basically means that your long lenses can appear even longer and get you closer to the action. Since you have all those extra megapixels to play with, effectively cropping into the image still leaves you with an incredibly useable 19 megapixels. Silent shooting is another feature that’s very useful in certain situations, such as", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00694", "split": "train"}
{"id": "conditionality_train_pos_0520", "text": "will have to play at Dallas anyway – not that the Cowboys are the end-all, be-all of the NFC. Winning at the Georgia Dome isn’t exactly an easy task either. (Getty Images) Getty Images/Getty Images The only game that matters is the one in front of you, but if you’re the look-ahead type (like all those Redskins fans who spent this week figuring out where they’d travel as that No. 6 seed) the scenario looks like this: No. 4 Green Bay: vs. Giants, at Cowboys or Falcons No. 6 Detroit: at Seahawks, at Cowboys (Getty Iages) Getty Images/Stacy Revere I’m taking the “worse” draw every time. The Packers are on a six-game winning streak and Aaron Rodgers may have just clinched the MVP with a four-touchdown night in Detroit. Who or where they play may be irrelevant. But it’s now the NFL playoffs and nothing will come easy nor will anything be handed to you. The Green Bay Packers were going to have a tough ride to their ultimate destination – Houston on Feb. 5 for Super Bowl LI – no matter what happened on Sunday night. It just so happens that the tougher ride came with the spoils of victory. So if Green Bay lost by winning, did Detroit win by losing? Eh, not so much. The Lions have lost three straight games and didn’t defeat a single team in the 2016 playoff field. At this point, I’m not sure I’d pick them to win their wild-card game even if they somehow got to host the Browns.", "label": 1, "domain": "news", "token_count": 322, "matched_pair_id": "conditionality_00728", "split": "train"}
{"id": "conditionality_train_pos_0521", "text": "The association of an electromagnetic signal with the merger of a pair of supermassive black holes would have many important implications. For example, it would provide new information about gas and magnetic field interactions in dynamical spacetimes as well as a combination of redshift and luminosity distance that would enable precise cosmological tests. A proposal first made by Bode & Phinney (2007) is that because radiation of gravitational waves during the final inspiral and merger of the holes is abrupt and decreases the mass of the central object by a few percent, there will be waves in the disk that can steepen into shocks and thus increase the disk luminosity in a characteristic way. We evaluate this process analytically and numerically. We find that shocks only occur when the fractional mass loss exceeds the half-thickness (h/r) of the disk, hence significant energy release only occurs for geometrically thin disks which are thus at low Eddington ratios. This strongly limits the effective energy release, and in fact our simulations show that the natural variations in disk luminosity are likely to obscure this effect entirely. However, we demonstrate that the reduction of luminosity caused by the retreat of the inner edge of the disk following mass loss is potentially detectable. This decrease occurs even if the disk is geometrically thick, and lasts for a duration on the order of the viscous time of the modified disk. Observationally, the best prospect for detection would be a sensitive future X-ray instrument with a field of view of on the order of a square degree, or possibly a wide-field radio array such as the Square Kilometer Array, if the disk changes produce or interrupt radio emission from a jet.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00106", "split": "train"}
{"id": "conditionality_train_pos_0522", "text": "Ponoka RCMP are looking for this man alleged to have taken some items from Main Street Hardware in Ponoka without paying. When asked, the man told the clerk he was ‘borrowing’ the items. RCMP photo Ponoka RCMP are looking for a man claiming he was ‘borrowing’ items from Main Street Hardware. Police were called to the hardware store March 17 after the man allegedly left the store with several items without paying. It appears that the suspect left the store with a hammer and scraper. When asked by the clerk to pay for them he said he was borrowing the items. “The store manager explained that the items had to be paid for before leaving but the male left with the merchandise,” say police. Investigators say they are looking for a Caucasian man in his 30s. At the time he was wearing a black hoodie. Ponoka man arrested for impaired driving Police charged a 56-year-old Ponoka man with impaired driving last week. At about 10 a.m. on March 16 witnesses called the police of an erratic driver heading westbound into Ponoka on Highway 53. Police say two witnesses reported a white Dodge Ram driving erratically into oncoming traffic. Police say he travelled at a high rate of speed through the Mecca Glen school zone and almost hit the ditch. “RCMP located the vehicle at the intersection of Highway 2A and Highway 53 and proceeded to observe the occupant’s driving pattern,” states a Ponoka RCMP release. He was arrested and charged with impaired driving. A court date is yet to be set. -Heyden-Kaye If you have information, please call the Ponoka RCMP at 403-783-4472. If you want to remain anonymous, you can contact Crime Stoppers by phone at 1-800-222-8477 (TIPS), or by internet at www.tipsubmit.com. You do not have to reveal your identity to Crime Stoppers, and if you provide information to Crime Stoppers that leads to an arrest(s), you may be eligible for a cash reward.", "label": 1, "domain": "news", "token_count": 418, "matched_pair_id": "conditionality_00705", "split": "train"}
{"id": "conditionality_train_pos_0523", "text": "the video below [COARSE LANGUAGE WARNING]: Angry homosexual kicks Christian customers out of coffee shop. WARNING! This video includes extremely graphic, hate-filled, blasphemous language.Watch and Share before Facebook takes it down! And let us know what YOU think. Posted by Abolish Human Abortion on Sunday, October 1, 2017 So can someone explain to me why Christian bakers are taken to court and publicly demeaned because they refuse to service a homosexual wedding, but when a gay liberals kicks a group of Christians out of their coffee shop, nobody in the mainstream media is reporting on it? Does anyone else see the double standard here? I still hold the belief that anyone in just about any business (except the healthcare profession and other emergency services) and choose who they do and don’t serve based on any factor, because the market will take care of itself. If a white guy walks into a shop, and the owner says “Get out, I don’t serve white people,” he should have that right, but as the guy has the right to go on social media and blast her and convince people to stop spending their money there. The owner will then have to decide if he wants to serve white people, or lose his business. That’s the way it should be in a free market. I think this guy has every right to do what he did, but the fact is that we’re living in a society that gives one person a pass while demonizing the other. Liberals wouldn’t tolerate it if it were the other way around, so why are we letting this happen?", "label": 1, "domain": "news", "token_count": 321, "matched_pair_id": "conditionality_00680", "split": "train"}
{"id": "conditionality_train_pos_0524", "text": "We investigate the magnetic field dependence of the physical properties of f^2-configuration systems with a crystalline-electric field (CEF) singlet ground state, which gives rise to a non- Fermi liquid (NFL) fixed point due to the competition between the Kondo-Yosida singlet and CEF singlet states. On the basis of the numerical renormalization group method, we find that the magnetic field breaks this NFL fixed point via two mechanisms: one causing the polarization of f-electrons and the other giving the \"channel\" anisotropy. These two mechanisms induce a difference in the magnetic field dependence of the characteristic temperature T_F^{*}(H), the crossover temperature from NFL to Fermi-liquid behavior. While the polarization of f-electrons gives T_F^{*}(H) \\propto H^x (x\\sim2.0), the \"channel\" anisotropy gives the H-independent T_F^{*}(H). These two mechanisms cross over continuously at approximately the crossover magnetic field H_c, where an anomalous H-dependence of T_F^{*}(H) appears. Such T_F^{*}(H) well reproduces the NFL behaviors observed in Th_{1-x}U_xRu_2Si_2. We also find that the H-dependence of the resistivity and the magnetic susceptibility are in good agreement with the experimental results of this material. These results suggest that the NFL behaviors observed in Th_{1-x}U_xRu_2Si_2 can be understood if this material is located in the CEF singlet side near the critical phase boundary between the two singlet states.", "label": 1, "domain": "academic", "token_count": 336, "matched_pair_id": "conditionality_00388", "split": "train"}
{"id": "conditionality_train_pos_0525", "text": "the United States Government if the agency-- (1) demonstrates through a business case that it can provide the administrative service more efficiently; and (2) agrees to provide the administrative service to all other International Cooperative Administrative Support Services customer agencies at the overseas post. SEC. 6. REPORTING REQUIREMENTS. (a) Biennial Report.-- (1) In general.--Not later than 1 year after the date of the enactment of this Act, and every 2 years thereafter, the Secretary of State, in consultation with the International Cooperative Administrative Support Services Executive Board, shall submit to the appropriate congressional committees a report on the International Cooperative Administrative Support Services system. (2) Content.--The report required under paragraph (1) shall-- (A) establish performance goals to define the level of performance to be achieved in providing efficient, effective, and equitable administrative services to International Cooperative Administrative Support Services customer agencies; (B) establish a balanced set of performance indicators to be used in measuring or assessing progress toward each performance goal; (C) describe how the International Cooperative Administrative Support Services system ensures the accuracy and reliability of the data used to measure progress; and (D) identify strategies and the resources required to achieve performance goals. (b) Comptroller General Review.-- (1) In general.--Not later than 2 years after the date of the enactment of this Act, the Comptroller General of the United States shall submit to the appropriate congressional committees a review of the International Cooperative Administrative Support Services system. (2) Content.--The review required under paragraph (1) shall include-- (A) an evaluation of whether requiring agencies to participate in the International Cooperative Administrative Support Services system for household furniture, furnishings, and appliance pools services and motor pools services has increased cost-efficiency and reduced administrative redundancies; (B) recommendations, if warranted, for further consolidation of services in the International Cooperative Administrative Support Services system; (C) an evaluation of how implementation of this Act is affecting the performance of International Cooperative Administrative Support Services customer agencies; and (D) recommendations, if warranted, for improving the International Cooperative Administrative Support Services system and implementing this Act.", "label": 1, "domain": "government", "token_count": 431, "matched_pair_id": "conditionality_01043", "split": "train"}
{"id": "conditionality_train_pos_0526", "text": "a violation of this subsection as a claim or defense in a judicial proceeding. ``(4) Remedies.-- ``(A) Federal jurisdiction.--The Federal courts shall have jurisdiction to prevent and redress actual or threatened violations of this subsection by granting all forms of legal or equitable relief, including, but not limited to, injunctive relief, declaratory relief, damages, costs, and attorney fees. ``(B) Initiating party.--An action under this subsection may be instituted by the Attorney General of the United States, or by any person or entity having standing to complain of a threatened or actual violation of this subsection, including, but not limited to, any actual or prospective plan sponsor, issuer, or other entity offering a plan, any actual or prospective purchaser or beneficiary of a plan, and any individual or institutional health care provider. ``(C) Interim relief.--Pending final determination of any action under this subsection, the court may at any time enter such restraining order or prohibitions, or take such other actions, as it deems necessary. ``(5) Administration.--The Office for Civil Rights of the Department of Health and Human Services is designated to receive complaints of discrimination based on this subsection and coordinate the investigation of such complaints. ``(6) Definition.--For purposes of this subsection, the term `entity' includes a group health plan, a health insurance issuer offering group or individual health insurance coverage, and an employer or other sponsor of such plan or coverage.''. (b) Effective Date.--The amendment made by subsection (a) shall be effective as if included in the enactment of Public Law 111-148.", "label": 1, "domain": "government", "token_count": 324, "matched_pair_id": "conditionality_00953", "split": "train"}
{"id": "conditionality_train_pos_0527", "text": "We investigate the formation and evolution of satellite galaxies using smoothed particle hydrodynamics (SPH) simulations of a Milky Way(MW)-like system, focussing on the best resolved examples, analogous to the classical MW satellites. Comparing with a pure dark matter simulation, we find that the condensation of baryons has had a relatively minor effect on the structure of the satellites' dark matter halos. The stellar mass that forms in each satellite agrees relatively well over three levels of resolution (a factor of ~64 in particle mass) and scales with (sub)halo mass in a similar way in an independent semi-analytical model. Our model provides a relatively good match to the average luminosity function of the MW and M31. To establish whether the potential wells of our satellites are realistic, we measure their masses within observationally determined half-light radii, finding that the most massive examples have somewhat higher mass-to-light ratios than those derived for the MW dSphs from stellar kinematic data. A statistical test yields a ~9 percent probability that the simulated and observationally derived distributions of masses are consistent. Our results may suggest that either the MW halo is less massive than assumed in our simulations (~1.4e12 M_sun) or that there is substantial scatter in the satellite luminosity function or distribution of mass-to-light ratios at fixed host halo mass. Alternatively, feedback processes not properly captured by our simulations may have reduced the central densities of (sub)halos, or the subhalos may have initially formed with lower concentrations as would be the case, for example, if the dark matter were made of warm, rather than cold particles.", "label": 1, "domain": "academic", "token_count": 336, "matched_pair_id": "conditionality_00333", "split": "train"}
{"id": "conditionality_train_pos_0528", "text": "For extrasolar planets with orbital periods, P>10 days, radial velocity surveys find non-circular orbital eccentricities are common, <e>~0.3. Future surveys for extrasolar planets using the transit technique will also have sensitivity to detect these longer period planets. Orbital eccentricity affects the detection of extrasolar planets using the transit technique in two opposing ways: an enhancement in the probability for the planet to transit near pericenter and a reduction in the detectability of the transit due to a shorter transit duration. For an eccentricity distribution matching the currently known extrasolar planets with P>10 day, the probability for the planet to transit is ~1.25 times higher than the equivalent circular orbit and the average transit duration is ~0.88 times shorter than the equivalent circular orbit. These two opposing effects nearly cancel for an idealized field transit survey with independent photometric measurements that are dominated by Poisson noise. The net effect is a modest ~4% increase in the transiting planet yield compared to assuming all planets have circular orbits. When intrinsic variability of the star or correlated photometric measurements are the dominant source of noise, the transit detectability is independent of the transit duration. In this case the transit yield is ~25% higher than that predicted under the assumption of circular orbits. Since the Kepler search for Earth-sized planets in the habitable zone of a Solar-type star is limited by intrinsic variability, the Kepler mission is expected to have a ~25% higher planet yield than that predicted for circular orbits if the Earth-sized planets have an orbital eccentricity distribution similar to the currently known Jupiter-mass planets.", "label": 1, "domain": "academic", "token_count": 327, "matched_pair_id": "conditionality_00043", "split": "train"}
{"id": "conditionality_train_pos_0529", "text": "Consider the use of $\\ell_{1}/\\ell_{\\infty}$-regularized regression for joint estimation of a $\\pdim \\times \\numreg$ matrix of regression coefficients. We analyze the high-dimensional scaling of $\\ell_1/\\ell_\\infty$-regularized quadratic programming, considering both consistency in $\\ell_\\infty$-norm, and variable selection. We begin by establishing bounds on the $\\ell_\\infty$-error as well sufficient conditions for exact variable selection for fixed and random designs. Our second set of results applies to $\\numreg = 2$ linear regression problems with standard Gaussian designs whose supports overlap in a fraction $\\alpha \\in [0,1]$ of their entries: for this problem class, we prove that the $\\ell_{1}/\\ell_{\\infty}$-regularized method undergoes a phase transition--that is, a sharp change from failure to success--characterized by the rescaled sample size $\\theta_{1,\\infty}(n, p, s, \\alpha) = n/\\{(4 - 3 \\alpha) s \\log(p-(2- \\alpha) s)\\}$. An implication of this threshold is that use of $\\ell_1 / \\ell_{\\infty}$-regularization yields improved statistical efficiency if the overlap parameter is large enough ($\\alpha > 2/3$), but has \\emph{worse} statistical efficiency than a naive Lasso-based approach for moderate to small overlap ($\\alpha < 2/3$). These results indicate that some caution needs to be exercised in the application of $\\ell_1/\\ell_\\infty$ block regularization: if the data does not match its structure closely enough, it can impair statistical performance relative to computationally less expensive schemes.", "label": 1, "domain": "academic", "token_count": 369, "matched_pair_id": "conditionality_00135", "split": "train"}
{"id": "conditionality_train_pos_0530", "text": "CAL83 is a prototype of the class of Super Soft X-ray Sources (SXS). It is a binary consisting of a low mass secondary that is transferring mass onto a white dwarf primary and is the only known SXS surrounded by an ionisation nebula, made up of the interstellar medium (ISM) ionised by the source itself. With the VIMOS IFU we obtained spectra over a 25\\times25\" field of view, encompassing one quarter of the nebula. Emission line maps - H I, He II, [O III], [N II], and [S II] - are produced in order to study the morphology of the ionised gas. We include CAL83 on diagrams of various diagnostic ion ratios to compare it to other X-ray ionised sources. Finally we computed some simple models of the ionised gas around CAL83 and compare the predicted to the observed spectra. CAL83 appears to have a fairly standard ionisation nebula as far as the morphology goes: the edges where H is recombining are strong in the low stage ionisation lines and the central, clumpy regions are stronger in the higher stage ionisation lines. But the He II emission is unusual in being confined to one side of CAL83 rather than being homogeneously distributed as with the other ions. We model the CAL83 nebula with cloudy using model parameters for SXSs found in the literature. The He II emission does not fit in with model predictions; in fact none of the models is able to fit the observed spectrum very well. The spectral line images of the region surrounding CAL83 are revealing and instructive. However, more modelling of the spectrum of the ionised gas is necessary, and especially for the high-ionisation level emission from CAL83. In particular, we wish to know if the He II emission and the other nebular lines are powered by the same ionising source.", "label": 1, "domain": "academic", "token_count": 386, "matched_pair_id": "conditionality_00466", "split": "train"}
{"id": "conditionality_train_pos_0531", "text": "In this paper we report the results of high-resolution circular spectropolarimetric monitoring of the Herbig Ae star V380 Ori, in which we discovered a magnetic field in 2005. A careful study of the intensity spectrum reveals the presence of a cool spectroscopic companion. By modelling the binary spectrum we infer the effective temperature of both stars: $10500\\pm 500$ K for the primary, and $5500\\pm500$ K for the secondary, and we argue that the high metallicity ($[M/H] = 0.5$), required to fit the lines may imply that the primary is a chemically peculiar star. We observe that the radial velocity of the secondary's lines varies with time, while that of the the primary does not. By fitting these variations we derive the orbital parameters of the system. We find an orbital period of $104\\pm5$ d, and a mass ratio ($M_{\\rm P}/M_{\\rm S}$) larger than 2.9. The intensity spectrum is heavily contaminated with strong, broad and variable emission. A simple analysis of these lines reveals that a disk might surround the binary, and that a wind occurs in the environment of the system. Finally, we performed a magnetic analysis using the Least-Squares Deconvolved (LSD) profiles of the Stokes $V$ spectra of both stars, and adopting the oblique rotator model. From rotational modulation of the primary's Stokes $V$ signatures, we infer its rotation period $P=4.31276\\pm0.00042$ d, and find that it hosts a centred dipole magnetic field of polar strength $2.12\\pm0.15$ kG, with a magnetic obliquity $\\beta = 66\\pm5^{\\circ}$, and a rotation axis inclination $i=32\\pm5^{\\circ}$. However, no magnetic field is detected in the secondary, and if it hosts a dipolar magnetic field, its strength must be below about 500 G, to be consistent with our observations.", "label": 1, "domain": "academic", "token_count": 426, "matched_pair_id": "conditionality_00157", "split": "train"}
{"id": "conditionality_train_pos_0532", "text": "If only Alberto Nisman were alive to see justice finally being pursued. Three years ago, Mr. Nisman was set to testify to the country’s Congress on Ms. Kirchner’s role in the cover up. The day before his testimony, on Jan. 18, 2015, he was found dead in his apartment in Buenos Aires, with a bullet in his head. This, despite the fact that he had a 10-man security detail paid to protect him. Within hours, Ms. Kirchner announced that Mr. Nisman had committed suicide. In the days that followed, she strangely claimed his death was part of a lovers’ spat. Finally, she changed her story once more: His death may have been the result of rogue intelligence operatives. When we heard the news of Mr. Nisman’s death and of Ms. Kirchner’s suspected cover-up, we were horrified, but not entirely shocked. Anyone who had followed Mr. Nisman’s pursuit of this case knew that he was assuming grave risks by taking on both a terrorist state and his own government. Through a decade of investigation, Mr. Nisman received death threats against not only him but his children as well. One email he told us about had a picture of bloodied and brutalized bodies lying on the ground, with a note saying this would be the fate of his young daughters if he did not cease his investigation. Newsletter Sign Up Continue reading the main story Sign Up for the Opinion Today Newsletter Every weekday, get thought-provoking commentary from Op-Ed columnists, the Times editorial board and contributing writers from around the world. Please verify you're not a robot by clicking the box. Invalid email address. Please re-enter. You must select a newsletter to subscribe to. Sign Up You agree to receive occasional updates and special offers for The New York Times's products and services. Thank you for subscribing. An error has occurred. Please try again later. View all New York Times newsletters. None of it stopped him. Fearless and resolute, Mr. Nisman and his team had determined that former Iranian and Hezbollah officials planned the AMIA attack. He was able to show definitively that the plan included no less than Iran’s former president, Ali Akbar Hashemi Rafsanjani; its minister of intelligence; its foreign minister; the head of Iran’s Islamic Revolutionary Guard Corps; the head of the corps’ elite Quds force; the Iranian cultural attaché in Argentina; and the third", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00608", "split": "train"}
{"id": "conditionality_train_pos_0533", "text": "Relay networks having $n$ source-to-destination pairs and $m$ half-duplex relays, all operating in the same frequency band in the presence of block fading, are analyzed. This setup has attracted significant attention and several relaying protocols have been reported in the literature. However, most of the proposed solutions require either centrally coordinated scheduling or detailed channel state information (CSI) at the transmitter side. Here, an opportunistic relaying scheme is proposed, which alleviates these limitations. The scheme entails a two-hop communication protocol, in which sources communicate with destinations only through half-duplex relays. The key idea is to schedule at each hop only a subset of nodes that can benefit from \\emph{multiuser diversity}. To select the source and destination nodes for each hop, it requires only CSI at receivers (relays for the first hop, and destination nodes for the second hop) and an integer-value CSI feedback to the transmitters. For the case when $n$ is large and $m$ is fixed, it is shown that the proposed scheme achieves a system throughput of $m/2$ bits/s/Hz. In contrast, the information-theoretic upper bound of $(m/2)\\log \\log n$ bits/s/Hz is achievable only with more demanding CSI assumptions and cooperation between the relays. Furthermore, it is shown that, under the condition that the product of block duration and system bandwidth scales faster than $\\log n$, the achievable throughput of the proposed scheme scales as $\\Theta ({\\log n})$. Notably, this is proven to be the optimal throughput scaling even if centralized scheduling is allowed, thus proving the optimality of the proposed scheme in the scaling law sense.", "label": 1, "domain": "academic", "token_count": 349, "matched_pair_id": "conditionality_00037", "split": "train"}
{"id": "conditionality_train_pos_0534", "text": "We present the first detections of the 3um water ice and 3.4um amorphous hydrocarbon (HAC) absorption features in z~2 ULIRGs. These are based on deep rest-frame 2-8um Spitzer IRS spectra of 11 sources selected for their appreciable silicate absorption. The HAC-to-silicate ratio for our z~2 sources is typically higher by a factor of 2-5 than that observed in the Milky Way. This HAC `excess' suggests compact nuclei with steep temperature gradients as opposed to predominantly host obscuration. Beside the above molecular absorption features, we detect the 3.3um PAH emission feature in one of our sources with three more individual spectra showing evidence for it. Stacking analysis suggests that water ice, hydrocarbons, and PAH are likely present in the bulk of this sample even when not individually detected. The most unexpected result of our study is the lack of clear detections of the 4.67um CO gas absorption feature. Only three of the sources show tentative signs of this feature and at significantly lower levels than has been observed in local ULIRGs. Overall, we find that the closest local analogs to our sources, in terms of 3-4um color, HAC-to-silicate and ice-to-silicate ratios, as well as low PAH equivalent widths are sources dominated by deeply obscured nuclei. Such sources form only a small fraction of ULIRGs locally and are commonly believed to be dominated by buried AGN. Our sample suggests that, in absolute number, such buried AGN are at least an order of magnitude more common at z~2 than today. The presence of PAH suggests that significant levels of star-formation are present even if the obscured AGN typically dominate the power budget.", "label": 1, "domain": "academic", "token_count": 371, "matched_pair_id": "conditionality_00158", "split": "train"}
{"id": "conditionality_train_pos_0535", "text": "heath Gardens, in Addiscombe, on October 6 when he saw a moped “driving at about 20pmh” approach him. Kouebitra and a then 15-year-old boy were on the moped. This youth, who is now 16 and cannot be named because of his age, has pleaded guilty to wounding with intent and admitted he was on the moped, but denied he was involved in the stabbing. Mr Dunham said: “[The youth] drove Kouebitra to Long Heath Gardens and when they arrived, Kouebitra chased him through the estate before cornering him and stabbed him with a machete four times to the chest, his side, his leg and arm.” He added: “Gadd was a close associate of Jack Harvey, who killed Daryl Kouebitra’s brother [Scotty]. One of the stab wounds was to the chest and if you stab someone to the chest, what could you possibly by trying to do?” Two men, who were on the estate at the time of the stabbing, desperately tried to help Kallum by applying pressure to his wounds before the emergency services were called. When helping him they asked him if he knew who had stabbed him, to which Kallum replied “Yes, Selhurst”. Kallum was taken to hospital, where he remained for five days, before coming home with “no significant disabilities” and made a “good recovery”. Kouebitra had previously been at a police custody suite earlier that day, for an unrelated crime. The court was told that he then left, changed his clothes and was picked up by the youth to go and collect a knife. Kouebitra denied attempting to kill Kallum, having pleaded not guilty at an earlier hearing. The jury unanimously found Kouebitra guilty of attempted murder and guilty of possessing an offensive weapon. They could not reach a verdict on a charge relating to wounding with intent, however. He will be sentenced at the same court on Thursday (May 31). It is not currently clear if the 16-year-old has already been sentenced.", "label": 1, "domain": "news", "token_count": 427, "matched_pair_id": "conditionality_00704", "split": "train"}
{"id": "conditionality_train_pos_0536", "text": "If North Korea's nukes don’t scare you, take a look at its biological weapons The Four Horsemen of the Apocalypse — Pestilence, War, Famine and Death — gallop through the Book of Revelation, and they’ve put in plenty of grim appearances elsewhere. Lately they’ve... North Korea soldier who defected had immunity to anthrax A North Korean soldier who defected to the South was found to have antibodies to anthrax — triggering concerns that the rogue regime has weaponized the deadly bacteria, according to... More than 100 hippos dead in suspected anthrax outbreak A sudden hippo die-off has sparked fears of an anthrax outbreak in Namibia. “Over 100 hippos died in the past week. The cause of death is unknown but the signs... Anthrax outbreak in Russia kills child, sends dozens to hospital MOSCOW — A child has died of anthrax in Siberia in the first fatal outbreak of the bacterial disease reported in Russia in 75 years, the regional governor’s office said... CDC mishandled bioterror germs A laboratory operated by the Centers for Disease Control and Prevention (CDC) had its permit suspended for three years for violating federal safety rules in its handling of bioterror pathogens,... Oops! Pentagon accidentally shipped more live anthrax than they thought The number of shipments of potentially live anthrax spores sent by mistake over the past decade now stands at 51. US shipped live anthrax to nine states The US Department of Defense inadvertently shipped live anthrax spores to as many as nine labs across the country, but officials insisted Wednesday that no one would be harmed by... Bacteria-filled subways leave riders feeling queasy Straphangers are worried sick over a new study that found traces of the bubonic plague and other bacteria — including ones that cause meningitis and staph infections — in the... Scientist finds lost vials of 'extinct' smallpox virus ATLANTA — A government scientist cleaning out an old storage room at a research center near Washington made a startling discovery last week — decades-old vials of smallpox packed away...", "label": 1, "domain": "news", "token_count": 427, "matched_pair_id": "conditionality_00814", "split": "train"}
{"id": "conditionality_train_pos_0537", "text": "if we were to completely ban this kind of \"research\" in the United States, it would still progress in other industrialized nations all over the planet. The genetic modification of humans and animals is part of a larger trend we are currently witnessing. In the scientific community, there is a tremendous amount of excitement about the fact that humans can finally \"take control of their own evolution.\" Many scientists believe we can use various forms of technology to give ourselves superhuman powers and radically extend our lifespans. And as technology continues to increase at an exponential rate, these scientists believe we will be able to ultimately create a \"post-human society\" where all sickness, disease, poverty and war are eradicated. So they aren't concerned about the potential dangers of these new technologies because they believe we are right on the verge of achieving immortality and transforming this planet into a technological utopia that will be perfect in every way. In other words, they believe humanity will no longer need \"god\" because we will be our own gods. Unfortunately for all the rest of us, in their relentless pursuit of this very foolish dream they are racing toward genetic Armageddon and they are opening up a Pandora's box of horrors that they simply do not understand. Michael Snyder is the founder and publisher of End Of The American Dream. Michael’s controversial new book about Bible prophecy entitled \"The Rapture Verdict\" is available in paperback and for the Kindle on Amazon.com. Leaders are readers! Subscribe now and get 3 magazines for the price of 1. Get Ministry Today, Charisma and SpiritLed Woman all for $24. YES - Sign me up! 3 Reasons Why you should read Life in the Spirit. 1) Get to know the Holy Spirit. 2) Learn to enter God's presence 3) Hear God's voice clearly! Click Here to draw closer to God! - See an error in this article? This email address is being protected from spambots. You need JavaScript enabled to view it.", "label": 1, "domain": "news", "token_count": 404, "matched_pair_id": "conditionality_00621", "split": "train"}
{"id": "conditionality_train_pos_0538", "text": "We report observations of a possible young transiting planet orbiting a previously known weak-lined T-Tauri star in the 7-10 Myr old Orion-OB1a/25-Ori region. The candidate was found as part of the Palomar Transient Factory (PTF) Orion project. It has a photometric transit period of 0.448413 +- 0.000040 days, and appears in both 2009 and 2010 PTF data. Follow-up low-precision radial velocity (RV) observations and adaptive optics imaging suggest that the star is not an eclipsing binary, and that it is unlikely that a background source is blended with the target and mimicking the observed transit. RV observations with the Hobby-Eberly and Keck telescopes yield an RV that has the same period as the photometric event, but is offset in phase from the transit center by approximately -0.22 periods. The amplitude (half range) of the RV variations is 2.4 km/s and is comparable with the expected RV amplitude that stellar spots could induce. The RV curve is likely dominated by stellar spot modulation and provides an upper limit to the projected companion mass of M_p sin i_orb < 4.8 +- 1.2 M_Jup; when combined with the orbital inclination, i orb, of the candidate planet from modeling of the transit light curve, we find an upper limit on the mass of the planetary candidate of M_p < 5.5 +- 1.4 M_Jup. This limit implies that the planet is orbiting close to, if not inside, its Roche limiting orbital radius, so that it may be undergoing active mass loss and evaporation.", "label": 1, "domain": "academic", "token_count": 349, "matched_pair_id": "conditionality_00463", "split": "train"}
{"id": "conditionality_train_pos_0539", "text": "Within the framework of the scalar-tensor theory (STT), its second post-Newtonian (2PN) approximation is obtained with Chandrasekhar's approach. By focusing on an $N$-point-masses system as the first step, we reduce the metric to its 2PN form for light propagation. Unlike previous works, at 2PN order, we abandon the hierarchized hypothesis and do not assume two parametrized post-Newtonian (PPN) parameters $\\gamma$ and $\\beta$ to be unity. We find that although there exist $\\gamma$ and $\\beta$ in the 2PN metric, only $\\gamma$ appears in the 2PN equations of light. As a simple example for applications, a gauge-invariant angle between the directions of two incoming photons for a differential measurement is investigated after the light trajectory is solved in a static and spherically symmetric spacetime. It shows the deviation from the general relativity (GR) $\\delta\\theta_{\\mathrm{STT}}$ does \\emph{not} depend on $\\beta$ even at 2PN level in this circumstance, which is consistent with previous results. A more complicated application is light deflection in a 2-point-masses system. We consider a case that the light propagation time is much less than the time scale of its orbital motion and thus treat it as a static system. The 2-body effect at 2PN level originating from relaxing the hierarchized hypothesis is calculated. Our analysis shows the 2PN 2-body effect in the Solar System is one order of magnitude less than future $\\sim 1$ nas experiments, while this effect could be comparable with 1PN component of $\\delta\\theta_{\\mathrm{STT}}$ in a binary system with two Sun-like stars and separation by $\\sim 0.1$ AU if an experiment would be able to measure $\\gamma-1$ down to $\\sim 10^{-6}$.", "label": 1, "domain": "academic", "token_count": 404, "matched_pair_id": "conditionality_00478", "split": "train"}
{"id": "conditionality_train_pos_0540", "text": "If the Secretary determines that a State has failed to submit a report by the deadline specified by subsection (c), or finds that the State has not implemented and provided adequate enforcement of the standards established under subsection (a) or (b), the Secretary shall notify the State and provide the State a period of 60 days in which to submit the report. ``(2) Implementation of alternative enforcement mechanism.-- ``(A) In general.--If, after the 60-day period, the Secretary finds that such a failure has not been corrected, the Secretary shall within 30 days provide for a mechanism for the implementation and enforcement of such standards in the State as the Secretary determines to be appropriate. ``(B) Civil penalty.--Under any implementation and enforcement mechanism established by the Secretary pursuant to this paragraph, the Secretary shall have the authority to impose on an insurer a civil monetary penalty in the amount of $10,000 for each day during which such insurer violates the requirements described in section 2701, or the standards developed under this section. Liability for such penalty shall begin to accrue on the 30th day after the Secretary has provided such insurer with notice of its noncompliance, if the insurer has failed to correct the deficiency by such date. ``(C) Effective period.--Any such implementation and enforcement mechanism established by the Secretary shall take effect with respect to insurers, and health insurance coverage offered or renewed, on or after 3 months after the date of the Secretary's finding under paragraph (1), and until the date the Secretary finds that such a failure has been corrected. ``(3) Federal civil right of action.-- ``(A) In general.--Any individual aggrieved as a result of conduct prohibited by section 2701 may bring a civil action in the appropriate United States district court against the insurer. ``(B) Relief.--Upon proof of such conduct by a preponderance of the evidence, the insurer shall be subject to a civil penalty that may include temporary, preliminary, or permanent injunctive relief and compensatory and punitive damages, as well as the costs of suit and reasonable fees for the aggrieved individual's attorneys. With respect to compensatory damages, the aggrieved individual may elect, at any time prior to the rendering of final judgment, to recover in lieu of actual damages, an award of statutory damages in the amount of $5,000 for each violation. ``SEC. 2703. APPLICATION TO GROUP HEALTH PLANS AND ENFORCEMENT. ``(a) Application.--Subject", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00914", "split": "train"}
{"id": "conditionality_train_pos_0541", "text": "In Montgomery (2009a), we show that accretion discs in binary systems could retrogradely precess by tidal torques like the Moon and the Sun on a tilted, spinning, non-spherical Earth. In addition, we show that the state of matter and the geometrical shape of the celestial object could significantly affect the precessional value. For example, a Cataclysmic Variable (CV) Dwarf Novae (DN) non-magnetic system that shows negative superhumps in its light curve can be described by a retrogradely precessing, differentially rotating, tilted disc. Because the disc is a fluid and because the gas stream overflows the tilted disc and particles can migrate into inner disc annuli, coupled to the disc could be a retrogradely precessing inner ring that is located near the innermost annuli of the disc. However, numerical simulations by Bisikalo et al. (2003, 2004) and this work show that an inner spiral density wave can be generated instead of an inner ring. Therefore, we show that retrograde precession in non-magnetic, spinning, tilted CV DN systems can equally be described by a retrogradely precessing and differentially rotating disc with an attached retrogradely precessing inner spiral density wave so long as the wave appears at the same radius as the ring and within the plane of the tilted disc. We find that the theoretical results generated in this work agree well with the theoretical results presented in Montgomery (2009a) and thus with the numerical simulations and select CV DN systems in Montgomery (2009b) that may have a main sequence secondary. Therefore, pressure effects do need to be considered in CV DN systems that exhibit negative superhumps if the accretion discs are tilted and have an inner spiral density wave that is in the plane of the disc.", "label": 1, "domain": "academic", "token_count": 380, "matched_pair_id": "conditionality_00282", "split": "train"}
{"id": "conditionality_train_pos_0542", "text": "We examine the dynamical destruction of binary systems in star clusters of different densities. We find that at high densities (10^4 - 10^5 Msun pc^-3) almost all binaries with separations > 10^3 AU are destroyed after a few crossing times. At low densities (order(10^2) Msun pc^-3) many binaries with separations > 10^3 AU are destroyed, and no binaries with separations > 10^4 AU survive after a few crossing times. Therefore the binary separations in clusters can be used as a tracer of the dynamical age and past density of a cluster. We argue that the central region of the Orion Nebula Cluster was around 100 times denser in the past with a half-mass radius of only 0.1 - 0.2 pc as (a) it is expanding, (b) it has very few binaries with separations > 10^3 AU, and (c) it is well-mixed and therefore dynamically old. We also examine the origin of the field binary population. Binaries with separations < 10^2 AU are not significantly modified in any cluster, therefore at these separations the field reflects the sum of all star formation. Binaries with separations in the range 10^2 - 10^4 AU are progressively more and more heavily affected by dynamical disruption in increasingly dense clusters. If most star formation is clustered, these binaries must be over-produced relative to the field. Finally, no binary with a separation > 10^4 AU can survive in any cluster and so must be produced by isolated star formation, but only if all isolated star formation produces extremely wide binaries.", "label": 1, "domain": "academic", "token_count": 348, "matched_pair_id": "conditionality_00138", "split": "train"}
{"id": "conditionality_train_pos_0543", "text": "Following the notion that the Titius-Bode rule (TBR) may also be applicable to some extra-solar planetary systems, although this number could be relatively small, it is applied to 55 Cancri, which is a G-type main-sequence star currently known to host five planets. Following a concise computational process, we tentatively identify four new hypothetical planetary positions given as 0.081, 0.41, 1.51 and 2.95 AU from the star. The likelihood that these positions are occupied by real existing planets is significantly enhanced for the positions of 1.51 and 2.95 AU in the view of previous simulations on planet formation and planetary orbital stability. For example, Raymond et al. (2008) [ApJ 689, 478] argued that additional planets would be possible between 55 Cnc f and 55 Cnc d, which would include planets situated at 1.51 and 2.95 AU. If two additional planets are assumed to exist between 55 Cnc f and 55 Cnc d, the deduced domains of stability would be given as 1.3-1.6 and 2.2-3.3 AU. The possible planet near 1.5 AU appears to be located at the outskirts of the stellar habitable zone, which is however notably affected by the stellar parameters as well as the adopted model of circumstellar habitability. We also compute the distance of the next possible outer planet in the 55 Cnc system, which if existing is predicted to be located between 10.9 and 12.2 AU, which is consistent with orbital stability constraints. The inherent statistical significance of the TBR is evaluated following the method by Lynch (2003) [MNRAS 341, 1174]. Yet it is up to future planetary search missions to verify or falsify the applicability of the TBR to the 55 Cnc system, and to attain information on additional planets, if existing.", "label": 1, "domain": "academic", "token_count": 410, "matched_pair_id": "conditionality_00362", "split": "train"}
{"id": "conditionality_train_pos_0544", "text": "The Director of the Office of Management and Budget, at such time or times as the Director shall provide, is authorized and directed to make such determinations as may be necessary with regard to the functions, entities or programs, or portions thereof transferred by this Act, and to make such additional incidental dispositions of personnel, assets, liabilities, grants, contracts, property, records, and unexpended balances of appropriations, authorizations, allocations, and other funds held, used, arising from, available to, or to be made available in connection with such functions, entities or programs, or portions thereof, as may be necessary to carry out the provisions of this Act. The Director shall provide for the termination of the affairs of all entities and programs terminated by this Act and for such further measures and dispositions as may be necessary to effectuate the purposes of this Act. (B) Transfer of positions within senior executive service.--After consultation with the Director of the Office of Personnel Management, the Director of the Office of Management and Budget is authorized, at such time as the Director of the Office of Management and Budget provides, to make such determinations as may be necessary with regard to the transfer of positions within the Senior Executive Service in connection with functions and entities and programs transferred by this Act. (c) Savings Provisions.-- (1) Completed administrative actions.-- (A) In general.--Completed administrative actions of an entity or program shall not be affected by the enactment of this Act or the transfer of the functions of such entity or program to the Agency under section 4(c), but shall continue in effect according to their terms until amended, modified, superseded, terminated, set aside, or revoked in accordance with law by an officer of the United States or a court of competent jurisdiction, or by operation of law. (B) Definition.--For purposes of subparagraph (A), the term ``completed administrative action'' includes orders, determinations, rules, regulations, personnel actions, permits, agreements, grants, contracts, certificates, licenses, registrations, and privileges. (2) Pending civil actions.--Subject to the authority of the Under Secretary under this Act, pending civil actions shall continue notwithstanding the enactment of this Act or the transfer of the functions of an entity or program to the Agency under section 4(c), and in such civil actions, proceedings shall be had, appeals taken, and judgments rendered and enforced in the same manner and with the same effect as if such enactment or transfer had not occurred.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00839", "split": "train"}
{"id": "conditionality_train_pos_0545", "text": "Recent analysis of five gamma-ray burst (GRB) afterglow spectra reveal the absence of molecular hydrogen absorption lines, a surprising result in light of their large neutral hydrogen column densities and the detection of H$_2$ in similar, more local star-forming regions like 30 Doradus in the Large Magellanic Cloud (LMC). Observational evidence further indicates that the bulk of the neutral hydrogen column in these sight lines lies 100 pc beyond the progenitor and that H$_2$ was absent prior to the burst, suggesting that direct flux from the star, FUV background fields, or both suppressed its formation. We present one-dimensional radiation hydrodynamical models of GRB host galaxy environments, including self-consistent radiative transfer of both ionizing and Lyman-Werner photons, nine-species primordial chemistry with dust formation of H$_2$, and dust extinction of UV photons. We find that a single GRB progenitor is sufficient to ionize neutral hydrogen to distances of 50 - 100 pc but that a galactic Lyman-Werner background is required to dissociate the molecular hydrogen in the ambient ISM. Intensities of 0.1 - 100 times the Galactic mean are necessary to destroy H$_2$ in the cloud, depending on its density and metallicity. The minimum radii at which neutral hydrogen will be found in afterglow spectra is insensitive to the mass of the progenitor or the initial mass function (IMF) of its cluster, if present.", "label": 1, "domain": "academic", "token_count": 308, "matched_pair_id": "conditionality_00046", "split": "train"}
{"id": "conditionality_train_pos_0546", "text": "If $w=u\\alpha$ for $\\alpha\\in \\Sigma=\\{1,2\\}$ and $u\\in \\Sigma^*$, then $w$ is said to be a \\textit{simple right extension}of $u$ and denoted by $u\\prec w$. Let $k$ be a positive integer and $P^k(\\epsilon)$ denote the set of all $C^\\infty$-words of height $k$. Set $u_{1},\\,u_{2},..., u_{m}\\in P^{k}(\\epsilon)$, if $u_{1}\\prec u_{2}\\prec ...\\prec u_{m}$ and there is no element $v$ of $P^{k}(\\epsilon)$ such that $v\\prec u_{1}\\text{or} u_{m}\\prec v$, then $u_{1}\\prec u_{2}\\prec...\\prec u_{m}$ is said to be a \\textit{maximal right smooth extension (MRSE) chains}of height $k$. In this paper, we show that \\textit{MRSE} chains of height $k$ constitutes a partition of smooth words of height $k$ and give the formula of the number of \\textit{MRSE} chains of height $k$ for each positive integer $k$. Moreover, since there exist the minimal height $h_1$ and maximal height $h_2$ of smooth words of length $n$ for each positive integer $n$, we find that \\textit{MRSE} chains of heights $h_1-1$ and $h_2+1$ are good candidates to be used to establish the lower and upper bounds of the number of smooth words of length $n$ respectively, which is simpler and more intuitionistic than the previous methods.", "label": 1, "domain": "academic", "token_count": 382, "matched_pair_id": "conditionality_00299", "split": "train"}
{"id": "conditionality_train_pos_0547", "text": "Former Chicago Police Chief Slams BLM… Blames Them For Violent Crime Wave [AUDIO] A former Chicago police chief has finally said what the rest of us are thinking and called out the Black Lives Matter movement. Since the rise of this famous group, we’ve seen a rise in the amount of police-targeted crimes. While many are afraid to call it what it is for fear of being labeled “racist” or a “bigot,” Garry McCarthy took to the airwaves to prove that not everyone will be bullied into silence. Coming from Chicago, he’s seen more than his fair share of crime, so if anyone would know the effect of BLM on police interaction with the public, it would be him. While speaking with John Catsimatidis on AM 970 in New York, McCarthy blamed the movement for the “political atmosphere of anti-police sentiment.” McCarthy explained that the movement has created an environment that has “emboldened” violent criminals, while “hamstringing” police officers, which McCarthy said contributes to increased “lawlessness” and violent crime. “So what’s happening, and this is ironic, is that a movement with the goal of saving black lives at this point is getting black lives taken, because 80 percent of our murder victims here in Chicago are male blacks,” he explained. “Less than half of 1 percent of all the shootings in this city involve police officers shooting civilians.” McCarthy went on to explain that the murder rate has skyrocketed 90 percent in Chicago over the past two years, which he said is “simply unacceptable.” “We are very clearly going down the wrong path,” he added. Listen to the audio below: I’m hoping that Trump’s election with embolden the police to go after criminals and stop being afraid of the media’s reaction to their difficult decisions. There is no reason an officer should feel like they couldn’t do their job because people would harass them and their family if the media portrays what they did as a bad thing.", "label": 1, "domain": "news", "token_count": 407, "matched_pair_id": "conditionality_00681", "split": "train"}
{"id": "conditionality_train_pos_0548", "text": "if it involves murder (relating to possessing a dangerous weapon in a Federal facility), 956 (relating to conspiracy to injure property of a foreign government), 1030(a)(1), 1030(a)(5)(A), or 1030(a)(7) (relating to protection of computers), 1362 (relating to destruction of communication lines, stations, or systems), 1366 (relating to destruction of an energy facility), 1992 (relating to trainwrecking), 2152 (relating to injury of fortifications, harbor defenses, or defensive sea areas), 2155 (relating to destruction of national defense materials, premises, or utilities), 2156 (relating to production of defective national defense materials, premises, or utilities), 2280 (relating to violence against maritime navigation), 2281 (relating to violence against maritime fixed platforms), 2339A (relating to providing material support to terrorists), 2339B (relating to providing material support to terrorist organizations), or 2340A (relating to torture). ``(2) Any of the following provisions of title 49: the second sentence of section 46504 (relating to assault on a flight crew with a dangerous weapon), section 46505(b)(3), (relating to explosive or incendiary devices, or endangerment of human life by means of weapons, on aircraft), section 46506 if homicide or attempted homicide is involved, or section 60123(b) (relating to destruction of interstate gas or hazardous liquid pipeline facility) of title 49.''. (b) Clerical Amendment.--The table of sections at the beginning of chapter 213 of title 18, United States Code, is amended by amending the item relating to section 3286 to read as follows: ``3286. Terrorism offenses.''. (c) Application.--The amendments made by this section shall apply to the prosecution of any offense committed before, on, or after the date of enactment of this section. SEC. 402. ALTERNATIVE MAXIMUM PENALTIES FOR TERRORISM CRIMES. Section 3559 of title 18, United States Code, is amended by adding after subsection (d) the following: ``(e) Authorized Terms of Imprisonment for Terrorism Crimes.--A person convicted of any Federal terrorism offense may be sentenced to imprisonment for any term of", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00999", "split": "train"}
{"id": "conditionality_train_pos_0549", "text": "The characteristic mass M_c in the stellar initial mass function (IMF) is about constant for most star-forming regions. Numerical simulations consistently show a proportionality between M_c and the thermal Jeans mass M_J at the time of cloud fragmentation, but no models have explained how it can be the same in diverse conditions. Here we show that M_J depends weakly on density, temperature, metallicity, and radiation field in three environments: the dense cores where stars form, larger star-forming regions ranging from GMCs to galactic disks, and the interiors of HII regions and super star clusters. In dense cores, the quantity T^{3/2}n^{-1/2} that appears in M_J scales with core density as n^{0.25} or with radiation density as U^{0.1} at the density where dust and gas come into thermal equilibrium. On larger scales, this quantity varies with ambient density as n^{-0.05} and ambient radiation field as U^{-0.033} when the Kennicutt-Schmidt law of star formation determines U(n). In super star clusters with ionization and compression of pre-stellar globules, M_J varies as the 0.13 power of the cluster column density. These weak dependencies on n, U, and column density imply that most environmental variations affect the thermal Jeans mass by at most a factor of ~2. Cosmological increases in M_J, which have been suggested by observations, may be explained if the star formation efficiency is systematically higher at high redshift for a given density and pressure, if dust grains are smaller at lower metallicity, and so hotter for a given radiation field, or if small pre-stellar cores are more severely ionized in extreme starburst conditions.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00053", "split": "train"}
{"id": "conditionality_train_pos_0550", "text": "; and ``(C) any other information necessary to enable the public to accurately compute the Federal retirement benefits of each Member based on various assumptions of years of service and age of separation from service by reason of retirement.''. (b) Effective Date.--This section shall take effect 1 year after the date of the enactment of this Act. SEC. 4. ELIMINATION OF AUTOMATIC ANNUITY ADJUSTMENTS FOR MEMBERS OF CONGRESS. The portion of the annuity of a Member of Congress which is based solely on service as a Member of Congress shall not be subject to a cost-of-living adjustment under section 8340 or 8462 of title 5, United States Code. SEC. 5. ELIMINATION OF AUTOMATIC PAY ADJUSTMENTS FOR MEMBERS OF CONGRESS. (a) Pay Adjustments.--Paragraph (2) of section 601(a) of the Legislative Reorganization Act of 1946 (2 U.S.C. 31) is repealed. (b) Conforming Amendment.--Section 601(a)(1) of such Act is amended-- (1) by striking ``(a)(1)'' and inserting ``(a)''; (2) by redesignating subparagraphs (A), (B), and (C) as paragraphs (1), (2), and (3), respectively; and (3) by striking ``, as adjusted by paragraph (2) of this subsection''. SEC. 6. ROLLCALL VOTE FOR ANY CONGRESSIONAL PAY RAISE. It shall not be in order in the Senate or the House of Representatives to dispose of any amendment, bill, resolution, motion, or other matter relating to the pay of Members of Congress unless the matter is decided by a rollcall vote.", "label": 1, "domain": "government", "token_count": 361, "matched_pair_id": "conditionality_00860", "split": "train"}
{"id": "conditionality_train_pos_0551", "text": ", rule, or regulation, each individual occupying a Senior Executive Service position (as that term is defined in section 3132(a)(2) of title 5, United States Code) on the date of enactment of this Act shall, beginning on the first day of the first pay period beginning after the date that the applicable appointing authority makes the determination under section 5383(a) of title 5, United States Code (as amended by subsection (a)), receive the rate of pay applicable to such position, as determined by the appointing authority under such section. SEC. 3. SEMIANNUAL REPORTS ON TRANSFERS OF SENIOR EXECUTIVES OF DEPARTMENT OF VETERANS AFFAIRS. (a) Semiannual Reports.--On a semiannual basis, the Secretary of Veterans Affairs shall submit to the Committees on Veterans' Affairs of the House of Representatives and the Senate a report on covered senior executives who transfer from one senior executive position in the Department of Veterans Affairs to another senior executive position in the Department during the period covered by the report. (b) Matters Included.--Each report under subsection (a) shall include, with respect to each covered senior executive who transfers from one senior executive position in the Department to another senior executive position in the Department during the period covered by the report, the following: (1) The name of the covered senior executive. (2) A description of the senior executive position from which the covered senior executive transferred, including the annual rate of basic pay received by the covered senior executive in such position. (3) A description of the senior executive position to which the covered senior executive transferred, including the annual rate of basic pay received by the covered senior executive in such position. (4) A description of the purpose of the transfer. (5) Justification for any increase or decrease in the annual rate of basic pay received by the covered senior executive by reason of such transfer. (6) Information regarding any relocation expenses and any incentives provided to the covered senior executive as part of such transfer. (c) Definitions.--In this section: (1) The term ``covered senior executive'' means an individual (as such term is defined in section 713(g)(1) of title 38, United States Code). (2) The term ``senior executive position'' has the meaning given that term in section 713(g)(3) of title 38, United States Code.", "label": 1, "domain": "government", "token_count": 493, "matched_pair_id": "conditionality_01048", "split": "train"}
{"id": "conditionality_train_pos_0552", "text": "two years after the date of the enactment of this section and at least once every five years thereafter (or more frequently as appropriate), the Inspector General of the Peace Corps shall perform an audit of Peace Corps implementation of safety and security protocols, including the status of any Inspector General findings and recommendations from previous audits that have not been adequately remediated or implemented. SEC. 6. PORTFOLIO REVIEWS. (a) In General.--The Director of the Peace Corps shall, at least once every three years (or more frequently as appropriate), perform a review to evaluate the allocation and delivery of resources across the countries the Peace Corps serves or is considering for service. Such portfolio reviews shall at a minimum include the following with respect to each such country: (1) An evaluation of the country's commitment to the Peace Corps program. (2) An analysis of the safety and security of volunteers. (3) An evaluation of the country's need for assistance. (4) An analysis of country program costs. (5) An evaluation of the effectiveness of management of each post within a country. (6) An evaluation of the country's congruence with the Peace Corps' mission and strategic priorities. (b) Report.--The Director of the Peace Corps shall prepare a report on each portfolio review required under subsection (a). Each such report shall discuss performance measures and sources of data used (such as project status reports, volunteer surveys, impact studies, reports of Inspector General of the Peace Corps, and any relevant external sources) in making such review's findings and conclusions. The Director shall make each such report available upon request to the Chairman and Ranking Member of the Committee on Foreign Affairs of the House of Representatives and the Committee on Foreign Relations of the Senate in a manner consistent with the protection of classified information if determined necessary to protect sensitive information.", "label": 1, "domain": "government", "token_count": 369, "matched_pair_id": "conditionality_01035", "split": "train"}
{"id": "conditionality_train_pos_0553", "text": "nothing preventing local NHS organisations from setting their own limit.\" Image caption Greg says he lost his hair 'overnight' Greg Burnet, who's 26, completely lost his hair when he was 13. \"I scratched my head in music class and some hair came out and I remember the girl next to me being like 'What the hell?' \"It was an overnight thing,\" he says. Despite seeing multiple doctors, dermatologists and specialists over the years, no-one has ever offered to prescribe him a wig. \"I would've been a different person. The alopecia has completely changed me and if I had an option of a wig it might not have done. \"Whether it's for better or worse - I wasn't given a choice and that's not fair.\" Image copyright Greg Burnet Image caption Greg says he wishes he'd been given the option of a wig Human hair wigs can cost several hundred pounds and the charity says it's heard from people who've had to cut back on essentials just to afford theirs. Jen, who has alopecia herself, used to get real hair wigs prescribed to her on the NHS - but in recent years she says the service has been cut. \"I remember when they told me - I just couldn't hold it together and I burst into tears,\" she says. Image copyright Getty Images The British Association of Dermatologists has echoed the call for a consistent NHS wig policy. \"Wig provision should be equal across the NHS, regardless of where you live. \"Alopecia can have an enormous impact on quality of life and should not be considered a cosmetic issue.\" Both NHS England and the body that represents CCGs (NHSCC) have refused to comment. Catch me up hide Follow Newsbeat on Instagram, Facebook and Twitter. Listen to Newsbeat live at 12:45 and 17:45 every weekday on BBC Radio 1 and 1Xtra - if you miss us you can listen back here.", "label": 1, "domain": "news", "token_count": 399, "matched_pair_id": "conditionality_00796", "split": "train"}
{"id": "conditionality_train_pos_0554", "text": "We present high quality long slit spectra along the major and minor axes out to 1.5-2 Re (14-22 kpc) of three bright elliptical galaxies (NGC1600, NGC4125, NGC7619) obtained at the Hobby-Eberly Telescope (HET). We derive stellar kinematic profiles and Lick/IDS indices (Hbeta, Mgb, Fe5015, Fe5270, Fe5335, Fe5406). Moreover, for NGC4125 we derive gas kinematics and emission line strengths. We model the absorption line strengths using Simple Stellar Populations models that take into account the variation of [\\alpha/Fe] and derive ages, total metallicity and element abundances. Overall, we find that the three galaxies have old and [\\alpha/Fe] overabundant stellar populations with no significant gradients. The metallicity is supersolar at the center with a strong negative radial gradient. For NGC4125, several pieces of evidence point to a recent dissipational merger event. We calculate the broad band color profiles with the help of SSP models. All of the colors show sharp peaks at the center of the galaxies, mainly caused by the metallicity gradients, and agree well with the measured colors. Using the Schwarzschild's axisymmetric orbit superposition technique, we model the stellar kinematics to constrain the dark halos of the galaxies. We use the tight correlation between the Mgb strength and local escape velocity to set limits on the extent of the halos by testing different halo sizes. Logarithmic halos - cut at 60 kpc -minimize the overall scatter of the Mgb-Vesc relation. Larger cutoff radii are found if the dark matter density profile is decreasing more steeply at large radii.", "label": 1, "domain": "academic", "token_count": 359, "matched_pair_id": "conditionality_00220", "split": "train"}
{"id": "conditionality_train_pos_0555", "text": "A drawing of a graph is said to be a {\\em straight-line drawing} if the vertices of $G$ are represented by distinct points in the plane and every edge is represented by a straight-line segment connecting the corresponding pair of vertices and not passing through any other vertex of $G$. The minimum number of slopes in a straight-line drawing of $G$ is called the slope number of $G$. We show that every cubic graph can be drawn in the plane with straight-line edges using only the four basic slopes $\\{0,\\pi/4,\\pi/2,-\\pi/4\\}$. We also prove that four slopes have this property if and only if we can draw $K_4$ with them. Given a graph $G$, an {\\em obstacle representation} of $G$ is a set of points in the plane representing the vertices of $G$, together with a set of obstacles (connected polygons) such that two vertices of $G$ are joined by an edge if and only if the corresponding points can be connected by a segment which avoids all obstacles. The {\\em obstacle number} of $G$ is the minimum number of obstacles in an obstacle representation of $G$. We show that there are graphs on $n$ vertices with obstacle number $\\Omega({n}/{\\log n})$. We show that there is an $m=2n+o(n)$, such that, in the Maker-Breaker game played on $\\Z^d$ where Maker needs to put at least $m$ of his marks consecutively in one of $n$ given winning directions, Breaker can force a draw using a pairing strategy. This improves the result of Kruczek and Sundberg who showed that such a pairing strategy exits if $m\\ge 3n$. A simple argument shows that $m$ has to be at least $2n+1$ if Breaker is only allowed to use a pairing strategy, thus the main term of our bound is optimal.", "label": 1, "domain": "academic", "token_count": 405, "matched_pair_id": "conditionality_00372", "split": "train"}
{"id": "conditionality_train_pos_0556", "text": "ICL is believed to originate from the stars stripped from cluster galaxies. They are no longer gravitationally bound to individual galaxies, but to the cluster, and their smooth distribution potentially makes them serve as much denser tracers of the cluster dark matter than the sparsely distributed cluster galaxies. We present our study of the ICL in Cl 0024+17 using both ACS and Subaru data, where we previously reported discovery of a ringlike dark matter structure with gravitational lensing. The ACS images provide much lower sky levels than ground data, and enable us to measure relative variation of surface brightness reliably. This analysis is repeated with the Subaru images to examine if consistent features are recovered despite different reduction scheme and instrumental characteristics. We find that the ICL profile clearly resembles the peculiar mass profile, which stops decreasing at r~50\" (~265 kpc) and slowly increases until it turns over at r~75\" (~397 kpc). This feature is seen in both ACS and Subaru images for nearly all available passband images while the features are stronger in red filters. The consistency across different filters and instruments strongly rules out the possibility that the feature might come from any residual, uncorrected calibration errors. In addition, our re-analysis of the cluster X-ray data shows that the peculiar mass structure is also indicated by a non-negligible bump in the intracluster gas profile when the geometric center of the dark matter ring, not the peak of the X-ray emission, is chosen as the center of the radial bin. The location of the gas ring is closer to the center by ~15\" (~80 kpc), raising an interesting possibility that the ring-like structure is expanding and the gas ring is lagging behind perhaps because of the ram pressure if both features in mass and gas share the same dynamical origin.", "label": 1, "domain": "academic", "token_count": 365, "matched_pair_id": "conditionality_00227", "split": "train"}
{"id": "conditionality_train_pos_0557", "text": "Stored antiproton beams at the international FAIR facility will provide unique opportunities to study hyperons as well as antihyperons in nuclear systems. Precise $\\gamma$-spectroscopy of multi-strange hypernuclei will serve as a laboratory for the hyperon-hyperon interaction. Exclusive hadron-antihadron pair production close to threshold can measure the potential of a antihadron relative to that of the coincident hadrons. In the present work we explore the production of excited states in double hypernuclei following the micro-canonical break-up of an initially excited double hypernucleus which is created by the absorption and conversion of a stopped $\\Xi^{-}$ hyperon. Generally the formation of excited hypernuclear states relative to ground states dominates in this model. For different initial target nuclei which absorb the $\\Xi^-$, different double hypernuclei nuclei dominate. We also compare the model predictions with the correlated pion spectra measured by the E906 collaboration. In antiproton nucleus reactions the event-by-event transverse momentum correlations of hadron-antihadron pairs produced close to threshold contain information on the difference between the nuclear potential of the hadron and the associated antihadron. For produced D-meson pairs at 6.7\\gevc1 the sensitivity of the transverse momenta correlation will probably be to small to deduce differences between the potentials for D$^+$ and D$^-$ mesons. However, for {\\PgX\\PagX} pairs produced at 2.9\\gevc1 the asymmetry is sufficiently sensitive to predicted differences between the {\\PgX} and {\\PagX} potentials even if the momentum and density dependence of the the potential are taken into account.", "label": 1, "domain": "academic", "token_count": 355, "matched_pair_id": "conditionality_00304", "split": "train"}
{"id": "conditionality_train_pos_0558", "text": "We present an interesting Sunyaev-Zel'dovich (SZ) detection in the first of the Arcminute Microkelvin Imager (AMI) 'blind', degree-square fields to have been observed down to our target sensitivity of 100{\\mu}Jy/beam. In follow-up deep pointed observations the SZ effect is detected with a maximum peak decrement greater than 8 \\times the thermal noise. No corresponding emission is visible in the ROSAT all-sky X-ray survey and no cluster is evident in the Palomar all-sky optical survey. Compared with existing SZ images of distant clusters, the extent is large (\\approx 10') and complex; our analysis favours a model containing two clusters rather than a single cluster. Our Bayesian analysis is currently limited to modelling each cluster with an ellipsoidal or spherical beta-model, which do not do justice to this decrement. Fitting an ellipsoid to the deeper candidate we find the following. (a) Assuming that the Evrard et al. (2002) approximation to Press & Schechter (1974) correctly gives the number density of clusters as a function of mass and redshift, then, in the search area, the formal Bayesian probability ratio of the AMI detection of this cluster is 7.9 \\times 10^4:1; alternatively assuming Jenkins et al. (2001) as the true prior, the formal Bayesian probability ratio of detection is 2.1 \\times 10^5:1. (b) The cluster mass is MT,200 = 5.5+1.2\\times 10^14h-1M\\odot. (c) Abandoning a physical model with num- -1.3 70 ber density prior and instead simply modelling the SZ decrement using a phenomenological {\\beta}-model of temperature decrement as a function of angular distance, we find a central SZ temperature decrement of -295+36 {\\mu}K - this allows for CMB primary anisotropies, receiver -15 noise and radio sources. We are unsure if the cluster system we observe is a merging system or two separate clusters.", "label": 1, "domain": "academic", "token_count": 438, "matched_pair_id": "conditionality_00294", "split": "train"}
{"id": "conditionality_train_pos_0559", "text": "Housing and Urban Development or any public housing agency pursuant to this section. ``(2) Eviction of nonelderly tenants having drug or alcohol use problems in housing designated for elderly families.--A tenant in a project (or portion of a project) that is designated under subsection (a)(1) for occupancy by only elderly families or by only elderly and disabled families shall be evicted under this paragraph if-- ``(A) the tenant's household includes a person described in clause (i) or (ii) of subsection (a)(5)(A); and ``(B) upon termination of the tenant's tenancy in the project, the public housing agency provides rental assistance under section 8 on behalf of the tenant.''. (b) Preference for Section 8 Assistance.-- (1) Certificates.--Section 8(d)(1)(A)(i) of the United States Housing Act of 1937 (42 U.S.C. 1437f(d)(1)(A)(i)) is amended by inserting after ``income for rent,'' the following: ``are required to be evicted under section 7(c)(2) if assistance under this section is provided on behalf of the family,''. (2) Vouchers.--The first sentence of section 8(o)(3)(B) of the United States Housing Act of 1937 (42 U.S.C. 1437f(o)(3)(B)) is amended by inserting after ``displaced,'' the following: ``are required to be evicted under section 7(c)(2) if assistance under this section is provided on behalf of the family,''.", "label": 1, "domain": "government", "token_count": 328, "matched_pair_id": "conditionality_01008", "split": "train"}
{"id": "conditionality_train_pos_0560", "text": "We develop a model for stochastic pre-enrichment and self-enrichment in globular clusters (GCs) during their formation process. GCs beginning their formation have an initial metallicity determined by the pre-enrichment of their surrounding protocloud, but can also undergo internal self-enrichment during formation. Stochastic variations in metallicity arise because of the finite numbers of supernova. We construct an analytic formulation of the combined effects of pre-enrichment and self-enrichment and use Monte Carlo models to verify that the model accurately encapsulates the mean metallicity and metallicity spread among real GCs. The predicted metallicity spread due to self-enrichment alone, a robust prediction of the model, is much smaller than the observed spread among real GCs. This result rules out self-enrichment as a significant contributor to the metal content in most GCs, leaving pre-enrichment as the viable alternative. Self-enrichment can, however, be important for clusters with masses well above 10^6 Msun, which are massive enough to hold in a significant fraction of their SN ejecta even without any external pressure confinement. This transition point corresponds well to the mass at which a mass-metallicity relationship (\"blue tilt\") appears in the metal-poor cluster sequence in many large galaxies. We therefore suggest that self-enrichment is the primary driver for the mass-metallicity relation. Other predictions from our model are that the cluster-to-cluster metallicity spread decreases amongst the highest mass clusters; and that the red GC sequence should also display a more modest mass-metallicity trend if it can be traced to similarly high mass.", "label": 1, "domain": "academic", "token_count": 331, "matched_pair_id": "conditionality_00110", "split": "train"}
{"id": "conditionality_train_pos_0561", "text": "We present a spectroscopic study of Leo V, a recently discovered satellite of the Milky Way (MW). From stellar spectra obtained with the MMT/Hectochelle spectrograph we identify seven likely members of Leo V. Five cluster near the Leo V center (R < 3 arcmin) and have velocity dispersion 2.4_{-1.4}^{+2.4} km/s. The other two likely members lie near each other but far from the center (R~13 arcmin ~ 700 pc) and inflate the global velocity dispersion to 3.7_{-1.4}^{+2.3} km/s. Assuming the five central members are bound, we obtain a dynamical mass of M=3.3_{-2.5}^{+9.1} x 10^5M_{sun} (M/L_V=75_{-58}^{+230}[M/L_V]_{sun}). From the stacked spectrum of the five central members we estimate a mean metallicity of [Fe/H]=-2.0\\pm 0.2 dex. Thus with respect to dwarf spheroidals of similar luminosity, Leo V is slightly less massive and slightly more metal-rich. Since we resolve the central velocity dispersion only marginally, we do not rule out the possibility that Leo V is a diffuse star cluster devoid of dark matter. The wide separation of its two outer members implies Leo V is losing mass; however, its large distance (D ~ 180 kpc) is difficult to reconcile with MW tidal stripping unless the orbit is very radial.", "label": 1, "domain": "academic", "token_count": 326, "matched_pair_id": "conditionality_00121", "split": "train"}
{"id": "conditionality_train_pos_0562", "text": "902(2) of the Trade Sanctions Reform and Export Enhancement Act of 2000 (22 U.S.C. 7201(2)) is amended-- (i) by striking subparagraph (D); and (ii) by redesignating subparagraphs (E) and (F) as subparagraphs (D) and (E), respectively. SEC. 3. FEDERAL MILK MARKETING REFORM. (a) In General.--Not later than 180 days after the date of enactment of this Act, the Secretary of Agriculture shall conduct hearings to assess the implications of transitioning Federal milk marketing orders from end-product pricing to a competitive pay pricing system. (b) Requirements.--In conducting hearings under this section, the Secretary shall-- (1) ensure that market administrators conduct a thorough analysis of the reforms to the Federal milk marketing orders proposed by the Maine Dairy Industry Advisory Council and the reforms included in title II of the Dairy Security Act of 2011; (2) analyze the implications of transitioning from a 4- class system for milk products to a 2-class system; (3) explore methods to improve signals for price discovery in the short- and long-term to allow dairy producers to better use risk management tools; (4) assess whether a 2-class competitive pay pricing system for milk products would be more or less transparent than the system in effect as of the day before the date of enactment of this Act; and (5) analyze the impact of eliminating a minimum regulated price on price volatility in dairy markets. SEC. 4. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 404, "matched_pair_id": "conditionality_00990", "split": "train"}
{"id": "conditionality_train_pos_0563", "text": "The development of fast and accurate methods of photometric redshift estimation is a vital step towards being able to fully utilize the data of next-generation surveys within precision cosmology. In this paper we apply a specific approach to spectral connectivity analysis (SCA; Lee & Wasserman 2009) called diffusion map. SCA is a class of non-linear techniques for transforming observed data (e.g., photometric colours for each galaxy, where the data lie on a complex subset of p-dimensional space) to a simpler, more natural coordinate system wherein we apply regression to make redshift predictions. As SCA relies upon eigen-decomposition, our training set size is limited to ~ 10,000 galaxies; we use the Nystrom extension to quickly estimate diffusion coordinates for objects not in the training set. We apply our method to 350,738 SDSS main sample galaxies, 29,816 SDSS luminous red galaxies, and 5,223 galaxies from DEEP2 with CFHTLS ugriz photometry. For all three datasets, we achieve prediction accuracies on par with previous analyses, and find that use of the Nystrom extension leads to a negligible loss of prediction accuracy relative to that achieved with the training sets. As in some previous analyses (e.g., Collister & Lahav 2004, Ball et al. 2008), we observe that our predictions are generally too high (low) in the low (high) redshift regimes. We demonstrate that this is a manifestation of attenuation bias, wherein measurement error (i.e., uncertainty in diffusion coordinates due to uncertainty in the measured fluxes/magnitudes) reduces the slope of the best-fit regression line. Mitigation of this bias is necessary if we are to use photometric redshift estimates produced by computationally efficient empirical methods in precision cosmology.", "label": 1, "domain": "academic", "token_count": 370, "matched_pair_id": "conditionality_00142", "split": "train"}
{"id": "conditionality_train_pos_0564", "text": "Newborn neutron stars surrounded by hyperaccreting and neutrino-cooled disks may exist in some gamma-ray bursts (GRBs) and/or supernovae (SNe). In this paper we further study the structure of such a neutron-star disk based on the two-region (i.e., inner & outer) disk scenario following our previous work, and calculate the neutrino annihilation luminosity from the disk in various cases. We investigate the effects of the viscosity parameter, energy parameter (measuring the neutrino cooling efficiency of the inner disk) and outflow strength on the structure of the entire disk as well as the effect of emission from the neutron star surface boundary emission on the total neutrino annihilation rate. The inner disk satisfies the entropy-conservation or the advection-dominated self-similar structure depending on the energy parameter. An outflow from the disk decreases the density and pressure but increases the thickness of the disk. Moreover, compared with the black-hole disk, the neutrino annihilation luminosity above the neutron-star disk is higher, and the neutrino emission from the boundary layer could increase the neutrino annihilation luminosity by about one order of magnitude higher than the disk without boundary emission. The neutron-star disk with the advection-dominated inner disk could produce the highest neutrino luminosity while the disk with an outflow has the lowest. Although a heavily mass-loaded outflow from the neutron star surface at early times of neutron star formation prevents the outflow material from being accelerated to a high bulk Lorentz factor, an energetic ultrarelativistic jet via neutrino annihilation can be produced above the stellar polar region at late times if the disk accretion rate and the neutrino emission luminosity from the surface boundary layer are sufficiently high.", "label": 1, "domain": "academic", "token_count": 355, "matched_pair_id": "conditionality_00107", "split": "train"}
{"id": "conditionality_train_pos_0565", "text": "In this paper, we study the average case complexity of the Unique Games problem. We propose a natural semi-random model, in which a unique game instance is generated in several steps. First an adversary selects a completely satisfiable instance of Unique Games, then she chooses an epsilon-fraction of all edges, and finally replaces (\"corrupts\") the constraints corresponding to these edges with new constraints. If all steps are adversarial, the adversary can obtain any (1-epsilon) satisfiable instance, so then the problem is as hard as in the worst case. In our semi-random model, one of the steps is random, and all other steps are adversarial. We show that known algorithms for unique games (in particular, all algorithms that use the standard SDP relaxation) fail to solve semi-random instances of Unique Games. We present an algorithm that with high probability finds a solution satisfying a (1-delta) fraction of all constraints in semi-random instances (we require that the average degree of the graph is Omega(log k). To this end, we consider a new non-standard SDP program for Unique Games, which is not a relaxation for the problem, and show how to analyze it. We present a new rounding scheme that simultaneously uses SDP and LP solutions, which we believe is of independent interest. Our result holds only for epsilon less than some absolute constant. We prove that if epsilon > 1/2, then the problem is hard in one of the models, the result assumes the 2-to-2 conjecture. Finally, we study semi-random instances of Unique Games that are at most (1-epsilon) satisfiable. We present an algorithm that with high probability, distinguishes between the case when the instance is a semi-random instance and the case when the instance is an (arbitrary) (1-delta) satisfiable instance if epsilon > c delta.", "label": 1, "domain": "academic", "token_count": 378, "matched_pair_id": "conditionality_00323", "split": "train"}
{"id": "conditionality_train_pos_0566", "text": "We present the results of SiO millimeter-line observations of a sample of known SiO maser sources covering a wide dust-temperature range. A cold part of the sample was selected from the SiO maser sources found in our recent SiO maser survey of cold dusty objects. The aim of the present research is to investigate the causes of the correlation between infrared colors and SiO maser intensity ratios among different transition lines. In particular, the correlation between infrared colors and SiO maser intensity ratio among the J=1-0 v=1, 2, and 3 lines are mainly concerned in this paper. We observed in total 75 SiO maser sources with the Nobeyama 45m telescope quasi-simultaneously in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines. We also observed the sample in the 29SiO J=1-0 v=0 and J=2-1 v=0, and 30SiO J=1-0 v=0 lines, and the H2O 6(1,6)-5(2,3) line. As reported in previous papers, we confirmed that the intensity ratios of the SiO J=1-0 v=2 to v=1 lines clearly correlate with infrared colors. In addition, we found possible correlation between infrared colors and the intensity ratios of the SiO J=1-0 v=3 to v=1&2 lines. Two overlap lines of H2O (i.e., 11(6,6) nu_2=1 -> 12(7,5) nu_2=0 and 5(0,5) nu_2=2 -> 6(3,4) nu_2=1) might explain these correlation if these overlap lines become stronger with increase of infrared colors, although the phenomena also might be explained by more fundamental ways if we take into account the variation of opacity from object to object.", "label": 1, "domain": "academic", "token_count": 427, "matched_pair_id": "conditionality_00009", "split": "train"}
{"id": "conditionality_train_pos_0567", "text": "If a Federal department or agency head determines that such use is justified, then that Federal department or agency head shall publish an explanation of such continued use in the Federal Register. SEC. 4. APPLICATION. This Act shall not apply to regulations, guidelines, or recommendations related to medical research. SEC. 5. DEFINITIONS. For purposes of this Act: (1) Animal.--The term ``animal'' means any vertebrate. (2) Animal acute toxicity test.--The term ``animal acute toxicity test'' means an acute toxicity test on animals, including (but not limited to) the Draize eye or skin irritancy test, LD-50 test, approximate lethal dose test, and the limit test. (3) Federal department or agency head.--The term ``Federal department or agency head'' means the head of a Federal department or agency who-- (A) has authority to promulgate regulations, guidelines, and recommendations with respect to procedures to be used in the safety testing by manufacturers of products, including consumer products, veterinary products, and products containing hazardous or toxic substances; or (B) licenses or approves products, labeling requirements or the transportation of products based on the results of these tests. (4) Medical research.--The term ``medical research'' means research, including research performed using biotechnology, related to the causes, diagnosis, treatment, or control of physical or mental impairments of humans or animals. The term does not include the testing of a product to determine its toxicity for the purpose of complying with protocols, recommendations, or guidelines for testing required, recommended, or accepted by a Federal regulatory agency for a product introduced in commerce. (5) Nonanimal acute toxicity test.--The term ``nonanimal acute toxicity test'' means an acute toxicity test not conducted on animals. Such tests include (but are not limited to) cell culture, computer modeling, protein alteration, and chorioallantoic membrane techniques.", "label": 1, "domain": "government", "token_count": 388, "matched_pair_id": "conditionality_00861", "split": "train"}
{"id": "conditionality_train_pos_0568", "text": "Observations of an optical source coincident with gravitational wave emission detected from a binary neutron star coalescence will improve the confidence of detection, provide host galaxy localisation, and test models for the progenitors of short gamma ray bursts. We employ optical observations of three short gamma ray bursts, 050724, 050709, 051221, to estimate the detection rate of a coordinated optical and gravitational wave search of neutron star mergers. Model R-band optical afterglow light curves of these bursts that include a jet-break are extrapolated for these sources at the sensitivity horizon of an Advanced LIGO/Virgo network. Using optical sensitivity limits of three telescopes, namely TAROT (m=18), Zadko (m=21) and an (8-10) meter class telescope (m=26), we approximate detection rates and cadence times for imaging. We find a median coincident detection rate of 4 yr^{-1} for the three bursts. GRB 050724 like bursts, with wide opening jet angles, offer the most optimistic rate of 13 coincident detections yr^{-1}, and would be detectable by Zadko up to five days after the trigger. Late time imaging to m=26 could detect off-axis afterglows for GRB 051221 like bursts several months after the trigger. For a broad distribution of beaming angles, the optimal strategy for identifying the optical emissions triggered by gravitational wave detectors is rapid response searches with robotic telescopes followed by deeper imaging at later times if an afterglow is not detected within several days of the trigger.", "label": 1, "domain": "academic", "token_count": 323, "matched_pair_id": "conditionality_00327", "split": "train"}
{"id": "conditionality_train_pos_0569", "text": "If you’re building a performance car, there are a number of areas you need to focus on to make sure all of your upgrades are in sync with each other when it comes time to push the limits of their individual capabilities. For example, if you are upgrading your suspension, the wheels and tires had better be able to handle the new g-forces the car will exhibit in the corners. Planning on adding a supercharger, turbo system, or just upping the ante in cubic inches? You’d better hope that the transmission is up to handling the task. We’re here to tell you that PerformaBuilt Transmissions has one goal in mind: to engineer and build the toughest transmission on the planet, and they’ve proved so not only with their updated designs but also through their pledge of quality, performance, and unparalleled customer service. All of their transmissions are dyno-tested at their production facility and delivered to your door ready to install with a rock-solid warranty with no exceptions for racing or mileage. On a recent visit, the team was preparing one of their Level 3 Invincible 4L60E units, which is one of their strongest models designed for extreme performance. Packed with upgrades, it features a bevy of modifications making it capable of handling up to 800 rwhp (rear-wheel horsepower), which is far more than the capabilities of a stock 4L60E, which is around 300 hp. Each unit is methodically re-engineered to overcome many of the inherent factory weaknesses by adding strength and durability. Some of the issues addressed include boosting line pressure from an OEM level of between 140-150 psi to 220 psi, and keeping the unit balanced to avoid “shift shock” (banging shifts) by tightening down clearances; this results in firm, quick shifts as driver input becomes more aggressive. From front to rear, upgrades include a BorgWarner 29-element dual-cage sprag assembly, Sonnax Smart Shell to eliminate the stripping of splines and breakage, a set of Raybestos carbon composite performance clutches with new Raybestos steels, and two Sonnax Super Hold billet servos for Second and Fourth gears for maximum hold to name but a few. Follow along and check out just what it takes to bring a stock 4L60E to the highest level of performance. CHP Source PerformaBuilt Transmissions 888.744.6542 performabuilt.com", "label": 1, "domain": "news", "token_count": 493, "matched_pair_id": "conditionality_00590", "split": "train"}
{"id": "conditionality_train_pos_0570", "text": "axed. The common thread among the three, besides zero playoff appearances? Ward, although it’s not all his fault, even if that’s a common sentiment among fans. There’s plenty of blame to go around, even beyond Eddie Lack. The Hurricanes have been too old when they needed to be younger, too young when they needed to be older and took far too long to assemble this group of talented players with untapped potential. Either way, the Hurricanes too often required something approaching perfection from Ward, and he could rarely deliver. And it was always Ward. Whether by default or design, Ward has been the main guy in net for this team for the past 11 years, in which the Hurricanes have made the playoffs once. All of the other contenders for the No. 1 job – most notably John Grahame, Anton Khudobin and Lack – turned out to be pretenders. If Lack were any good, this might have been a playoff team last spring. So now the Hurricanes try again, with Darling, whose record as a backup on one of the NHL’s best teams was stellar but who has never played more than 45 games in a season, and that when he was 19. The Hurricanes will probably need him to play at least 60, and play them well, not that Darling is taking that for granted. “Cam and I both want to play, and just because I showed up and signed here doesn’t mean, ‘Here you go, here’s 80 games,’ ” Darling said. But he will start Saturday’s opener against the Minnesota Wild, after missing his first scheduled preseason start with an undisclosed minor injury. In the two games he played after that, he was stellar: a 1.50 goals-against average and.925 save percentage. It’s foolish to draw sweeping conclusions from preseason because of the frequent talent disparity between game rosters, but those numbers are everything you’d expect from Darling. If he can deliver anything close to that in real games, it’ll be a different kind of season for the Hurricanes. And if he can’t, it’ll look all too familiar.", "label": 1, "domain": "news", "token_count": 429, "matched_pair_id": "conditionality_00780", "split": "train"}
{"id": "conditionality_train_pos_0571", "text": "An election under subparagraph (A) shall-- ``(i) be made to the Settlement Trust in writing, and ``(ii) specify the percentage (not greater than 15 percent) of the distributions to be withheld. Such election may be revoked or modified with respect to distributions made after the revocation or modification. ``(6) Settlement trust.--For purposes of this section, the term `Settlement Trust' means a trust which constitutes a Settlement Trust under section 39 of the Alaska Native Claims Settlement Act (43 U.S.C. 1629e).'' (c) Reporting.--Section 6041 of such Code is amended by adding at the end the following new subsection: ``(f) Application to Alaska Settlement Trusts.--In the case of any distribution from a Settlement Trust (as defined in section 501(p)(6)) to a beneficiary, this section shall apply, except that-- ``(1) this section shall apply to such distribution without regard to the amount thereof, ``(2) the Settlement Trust shall include on any return or statement required by this section information as to the character of such distribution (if applicable) and the amount of tax imposed by chapter 1 deducted and withheld from such distribution, and ``(3) the filing of any return or statement required by this section shall satisfy any requirement to file any other form or schedule under this title with respect to distributive share information (including any form or schedule included with the trust's tax return).'' (d) Effective Dates.-- (1) In general.--The amendments made by this section shall apply to taxable years of Settlement Trusts beginning after December 31, 1996, and to contributions to such trusts after such date. (2) Requirement for election.--An election under section 501(p)(2) of the Internal Revenue Code of 1986 for a taxable year beginning in 1997 shall not be treated as failing to meet the requirements of section 501(p)(2)(B) of such Code if such election is filed with the return of tax for the first taxable year after such taxable year.", "label": 1, "domain": "government", "token_count": 418, "matched_pair_id": "conditionality_00992", "split": "train"}
{"id": "conditionality_train_pos_0572", "text": "We present the discovery of 5 millisecond pulsars found in the mid-Galactic latitude portion of the High Time Resolution Universe (HTRU) Survey. The pulsars have rotational periods from ~2.3 to ~7.5 ms, and all are in binary systems with orbital periods ranging from ~0.3 to ~150 d. In four of these systems, the most likely companion is a white dwarf, with minimum masses of ~0.2 Solar Masses. The other pulsar, J1731-1847, has a very low mass companion and exhibits eclipses, and is thus a member of the \"black widow\" class of pulsar binaries. These eclipses have been observed in bands centred near frequencies of 700, 1400 and 3000 MHz, from which measurements have been made of the electron density in the eclipse region. These measurements have been used to examine some possible eclipse mechanisms. The eclipse and other properties of this source are used to perform a comparison with the other known eclipsing and \"black widow\" pulsars. These new discoveries occupy a short-period and high-dispersion measure (DM) region of parameter space, which we demonstrate is a direct consequence of the high time and frequency resolution of the HTRU survey. The large implied distances to our new discoveries makes observation of their companions unlikely with both current optical telescopes and the Fermi Gamma-ray Space Telescope. The extremely circular orbits make any advance of periastron measurements highly unlikely. No relativistic Shapiro delays are obvious in any of the systems, although the low flux densities would make their detection difficult unless the orbits were fortuitously edge-on.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00307", "split": "train"}
{"id": "conditionality_train_pos_0573", "text": "We analyze 2.8-yr data of 1-100 GeV photons for clusters of galaxies, collected with the Large Area Telescope onboard the Fermi satellite. By analyzing 49 nearby massive clusters located at high Galactic latitudes, we find no excess gamma-ray emission towards directions of the galaxy clusters. Using flux upper limits, we show that the Fornax cluster provides the most stringent constraints on the dark matter annihilation cross section. Stacking a large sample of nearby clusters does not help improve the limit for most dark matter models. This suggests that a detailed modeling of the Fornax cluster is important for setting robust limits on the dark matter annihilation cross section based on clusters. We therefore perform the detailed mass modeling and predict the expected dark matter annihilation signals from the Fornax cluster, by taking into account effects of dark matter contraction and substructures. By modeling the mass distribution of baryons (stars and gas) around a central bright elliptical galaxy, NGC 1399, and using a modified contraction model motivated by numerical simulations, we show that the dark matter contraction boosts the annihilation signatures by a factor of 4. For dark matter masses around 10 GeV, the upper limit obtained on the annihilation cross section times relative velocity is <\\sigma v> <~ (2-3)x10^{-25} cm^3 s^{-1}, which is within a factor of 10 from the value required to explain the dark matter relic density. This effect is more robust than the annihilation boost due to substructure, and it is more important unless the mass of the smallest subhalos is much smaller than that of the Sun.", "label": 1, "domain": "academic", "token_count": 337, "matched_pair_id": "conditionality_00401", "split": "train"}
{"id": "conditionality_train_pos_0574", "text": "If the violation occurs in a single eligible State, the Secretary shall credit the account of that eligible State with an amount equal to 75% of the amount received. (ii) If the violation occurs in multiple eligible States, the Secretary shall divide the amount described in clause (i) by the number of eligible States where the violation occurred and shall credit the account of each eligible State with an equal share. (b) Requirements for Use and Redistribution of Payments.-- (1) Use of payments specified.--A payment received under this section shall be used solely for payments to local educational agencies (as defined in section 9101(26) of the Elementary and Secondary Education Act of 1965 (20 U.S.C. 7801(26))), public health care providers, and law enforcement agencies for the purpose of assisting State and local governments with meeting the costs associated with serving aliens who are unlawfully present in the United States. (2) Redistribution of payment to counties and units of local government.--An eligible State shall redistribute 66 percent of the payment received under this section, within 60 days of receipt by the State, to appropriate counties and units of local government in accordance with a system that the State shall develop that provides for opportunities for input from all counties and units of local government in the state and that targets the areas of greatest need in accordance with the purpose described in paragraph (1), based on objective criteria. (c) Definitions.--For the purposes of this section, the following definitions apply: (1) Eligible state.--The term ``eligible State'' means a State that agrees-- (A) to use the payment received under this section for the uses specified in subsection (b)(1); (B) to redistribute the payment received under this section to counties and units of local government in accordance with subsection (b)(2); (C) to require that any county or unit of local government to whom a payment is redistributed shall use the payment for the uses specified in subsection (b)(1); and (D) to submit information and assurances at such time and in such form as the Secretary may require. (2) State.--The term ``State'' includes each State, the District of Columbia, the Commonwealth of Puerto Rico, American Samoa, Guam, and the United States Virgin Islands. (3) Secretary.--The term ``Secretary'' means the Secretary of the Treasury. (d) Effective Date.--This section shall take effect at the beginning of the next fiscal year following", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00932", "split": "train"}
{"id": "conditionality_train_pos_0575", "text": "If Tim Tebow’s stat line has not justified even his meager salary, his drawing power sure has. The former Heisman trophy winner was paid $10,000 this season while playing for the Single-A Columbia Fireflies and St. Lucie Mets and contributed to the largest rise in minor league baseball attendance in 23 years, according to ESPN. Attendance for Fireflies games increased by 54,000 fans (21 percent) over last season during Tebow’s tenure in Columbia, and the effect was more pronounced when he joined St. Lucie at the end of June, contributing to a 37 percent rise in visitors to the ballpark. Similar results were seen during road games, where the Fireflies drew an additional 2,591 fans over the home teams’ season averages. The last time the minors saw such a spike in attendance was thanks to another popular cross-sport athlete taking a stab at professional baseball: Michael Jordan. Tebow’s numbers don’t stack up against Jordan’s, but the NBA champion was the single most recognizable sports brand in the world at the time. Add to that the fact Jordan was playing Double-A ball in larger stadiums than Tebow, and the difference in their numbers is easily explained. The point remains – Tebow was a huge draw and a tremendous boon to the clubs he played for and those he visited. A Baseball America study conducted in June placed the value of Tebow’s contribution to ticket sales, parking, concessions and other revenue at $1.6 million. In other words, the Mets organization got precisely what it wanted out of Tebow. When the erstwhile NFL quarterback announced he would try his hand at baseball, many saw the move as nothing more than a publicity stunt, a money-making venture and a distraction. All of which made him a perfect fit for the Mets’ desultory strategizing. Tebow’s .226 batting average and 126 strikeouts in 126 minor league games at the Single-A level make him an unlikely candidate to save the Mets’ floundering big league club. But putting his name on the back of a Mets jersey has clear advantages, as evidenced by the numbers. And at $10,000 a year, the bargain is too good to pass up.", "label": 1, "domain": "news", "token_count": 451, "matched_pair_id": "conditionality_00818", "split": "train"}
{"id": "conditionality_train_pos_0576", "text": "Topological excitations are usually classified by the $n$th homotopy group $\\pi_n$. However, for topological excitations that coexist with vortices, there are case in which an element of $\\pi_n$ cannot properly describe the charge of a topological excitation due to the influence of the vortices. This is because an element of $\\pi_n$ corresponding to the charge of a topological excitation may change when the topological excitation circumnavigates a vortex. This phenomenon is referred to as the action of $\\pi_1$ on $\\pi_n$. In this paper, we show that topological excitations coexisting with vortices are classified by the Abe homotopy group $\\kappa_n$. The $n$th Abe homotopy group $\\kappa_n$ is defined as a semi-direct product of $\\pi_1$ and $\\pi_n$. In this framework, the action of $\\pi_1$ on $\\pi_n$ is understood as originating from noncommutativity between $\\pi_1$ and $\\pi_n$. We show that a physical charge of a topological excitation can be described in terms of the conjugacy class of the Abe homotopy group. Moreover, the Abe homotopy group naturally describes vortex-pair creation and annihilation processes, which also influence topological excitations. We calculate the influence of vortices on topological excitations for the case in which the order parameter manifold is $S^n/K$, where $S^n$ is an $n$-dimensional sphere and $K$ is a discrete subgroup of $SO(n+1)$. We show that the influence of vortices on a topological excitation exists only if $n$ is even and $K$ includes a nontrivial element of $O(n)/SO(n)$.", "label": 1, "domain": "academic", "token_count": 381, "matched_pair_id": "conditionality_00379", "split": "train"}
{"id": "conditionality_train_pos_0577", "text": "If you’re seeking relationship bliss circa 2017, look no further than your phone. It seems emojis, those expressive pictures all over texts and Instagram, could actually help our love lives. In his new book, “The Emoji Code,” to be published in the U.S. in August by MacMillan Picador, British linguist Vyv Evans argues that emojis are making us better communicators. Evans calls emojis a “near-universal form of communication,” replacing internet slang like LOL with the popular “face with tears of joy” emoji. And while he says some see the little glyphs as “little more than an adolescent grunt,” Evans says those people couldn’t be more wrong. Evans’ research found that 72 percent of 18- to 25-year-olds find it easier to express their emotions if they’re using emojis. And 80 percent of people in the U.K. said they use them. There’s a reason for that: Digital communication has stripped away important context like gestures, facial expressions and tone of voice. Emails and texts often come across as more ambiguous — or mean-spirited — than intended. Enter the emoji. Adding a little smiley face or winking eye can convey joking or sarcasm. A text that says “Sure, go ahead!” with a kissy face could read more like “sure … go ahead” without one. A Match.com survey of singles in America found that people who use emojis went on more dates and were more likely to have sex than those who didn’t. More than half of singles who used emojis had sex in 2014, compared to 31 percent of singles who didn’t, according to the survey. NBC News / If this leaves you with a confused face, and you don’t even know how to express that in emoji, check out this quick primer of definitions from Emojipedia.", "label": 1, "domain": "news", "token_count": 376, "matched_pair_id": "conditionality_00741", "split": "train"}
{"id": "conditionality_train_pos_0578", "text": "OKLAHOMA CITY — A former Oklahoma City mayor and member of the University of Oklahoma Board of Regents was rebuked Monday for comparing gay people to pedophiles and politicians who’ve recently resigned amid allegations of sexual misconduct. Kirk Humphreys made the comments during a local TV public affairs show that aired over weekend on KFOR-TV. Humphreys and others were discussing allegations against Minnesota Sen. Al Franken, who is stepping down, and President Donald Trump, when Humphreys began to ramble about other subjects. He said he was “going to make a lot of people mad today.” “Is homosexuality right or wrong? It’s not relative, there’s a right and wrong,” Humphreys said. “If it’s OK then it’s OK for everybody and, quite frankly, it’s OK for men to sleep with little boys.” LGBTQ advocacy group Freedom Oklahoma called for Humphreys’ removal from the Board of Regents if he didn’t apologize. Executive Director Troy Stevenson said Monday that Humphreys’ comments were disheartening and dangerous for LGBTQ youth who are already harassed and bullied. A staffer at Humphreys’ office said he was out of town Monday and unavailable to comment. Humphreys, 67, did not immediately reply to an email seeking comment. The president of the University of Oklahoma distanced himself from Humphreys’ comments. President David Boren noted that Humphreys was not speaking on behalf of the university, adding that the school was committed to diversity and inclusiveness. “I do not share his views on this matter,” Boren said in a statement. A state lawmaker who appeared with Humphreys pushed back at him on the show, saying it was wrong to compare sexual misconduct and crimes to the legal behaviour of consenting adults. “Mr. Humphreys’ comments were disgusting, offensive, and just plain wrong,” Rep. Emily Virgin, a Democrat from Oklahoma City, later said on her Facebook page. “I unequivocally stand with the LGBT community. Stevenson said his group planned to protest an Oklahoma City real estate project that belongs to Humphreys’ family business if he doesn’t apologize.", "label": 1, "domain": "news", "token_count": 436, "matched_pair_id": "conditionality_00671", "split": "train"}
{"id": "conditionality_train_pos_0579", "text": "Robin Muchetu, Senior Reporter POLICE have assured the nation that they will bring the perpetrators of the bombing incident in an attempted assassination attack targeting President Emmerson Mnangagwa at White City Stadium to book saying special teams have been assigned to carry out the investigation. Addressing the media and senior officers in Bulawayo today, Police Commissioner General Thandabantu Godwin Matanga said it was work in progress for the police who he said were not going to rest until the suspects have been brought to book. He said the horrendous and nefarious act dampened the spirits of the citizens. “I assure the nation and its entire citizenry that we are fully investigating this dastardly and wicked act, which has already unnecessarily claimed two lives,” said Comm Matanga. He went on: “As the ZRP we will never rest until all those behind this heinous act have been accounted for and have had their day in court. We will do whatever it takes within the precincts of the law to ensure that this objective is met. At the risk of overemphasizing, I wish to say no stone will be left unturned,” he said. He applauded the level of cooperation and support that the joint investigation team has so far received. He said the collaborative effort was appreciated and continued to appeal for more information that may enable the force to bring to book the culprits involved. Cde Matanga further said the public must desist from acts of violence during this period and said the ZRP has since arrested 2237 people from January for engaging in various forms of violence. The ZRP said they would revitalize and reinvigorate all police patrol units with a view to assist in reducing crime through increased police visibility in all crime prone areas. The patrols, they said, help in earning public confidence from the resultant quality of their service if the deployments were well planned and adequately supervised.", "label": 1, "domain": "news", "token_count": 385, "matched_pair_id": "conditionality_00549", "split": "train"}
{"id": "conditionality_train_pos_0580", "text": "Waterford County Board chairman Paddy Joe Ryan said there was no intent in Austin Gleeson's controversial clash with Luke Meade and hopes Galway corner-back Adrian Tuohy's reprieve after a similar incident last week serves as a good omen. Gleeson and Corkman Meade tangled during yesterday's All-Ireland SHC semi-final, with Gleeson appearing to pull off his opponent's helmet. Galway's Tuohy did not face any disciplinary action following an incident with Tipperary’s Patrick Maher in the first All-Ireland semi-final. The helmet of the Tipp centre-forward came off during the first-half clash with both men competing for the ball and it was feared that retrospective action could lead him to miss next month’s decider. Speaking to RTÉ news in Dungarvan, Ryan said the Gleeson clash would not be classed as deliberate and that there was no intent by the player. He said Waterford do not want to be entangled in disciplinary matters in the weeks leading up to the All-Ireland final. \"We just want this thing to take its course and hopefully we will be more or less full strength for the final,\" he said, adding that the Waterford County Board will look at the referee's report when it is available and that they will address any matters arising if any exist, also in relation to Conor Gleeson, who was sent off on a straight red card. Ryan revealed they'll wait and see what's in the report by referee James Owens before they decide on a course of action, if any is required.", "label": 1, "domain": "news", "token_count": 318, "matched_pair_id": "conditionality_00759", "split": "train"}
{"id": "conditionality_train_pos_0581", "text": "If you’re a user of Island Line trains or have an interest in the future of the line, make sure you head to Shanklin Theatre on Thursday evening. A public meeting (14th December, 7pm start) is being held to discuss the stakeholders’ response to South Western Railway’s proposals for Island Line. It’s being organised by Keep Island Line in Franchise campaign, in partnership with the IW Bus & Rail Users’ Group (IWBRUG) and the Isle of Wight Steam Railway (IWSR). The Isle of Wight Conservative MP, Bob Seely, will also be in attendance as well as a number of Isle of Wight Councillors. Your views matter The meeting is open to any members of the public with an interest in the future of railway provision on the Island. The topics being covered will include: South Western Railway’s proposals for Island Line, and the proposed consultation response on behalf of the local community (deadline 31st December 2017). Future plans for the IW Steam Railway; Improving interconnectivity between the two lines and links with cross-Solent travel (including SWR’s plans for mainland services); Possible future extensions to Newport and Ventnor, particularly in light of the Government’s announcement about previously closed lines being re-opened – and MP Bob Seely’s intervention on this topic with Transport Secretary Chris Grayling. Come along For updates and more info prior to the meeting visit KILF’s Facebook event page. Shanklin Theatre’s doors (and the bar) will open at 6:30pm, ahead of a 7pm start. Any questions about the public meeting on 14th December should be directed to kilfcampaign@gmail.com. Image: tompagenet under CC BY 2.0 Location map View the location of this story.", "label": 1, "domain": "news", "token_count": 368, "matched_pair_id": "conditionality_00583", "split": "train"}
{"id": "conditionality_train_pos_0582", "text": "Searches for gravitational waves with km-scale laser interferometers often involve the long-wavelength approximation to describe the detector response. The prevailing assumption is that the corrections to the detector response due to its finite size are small and the errors due to the long-wavelength approximation are negligible. Recently, however, Baskaran and Grishchuk (2004 Class. Quantum Grav. 21 4041) found that in a simple Michelson interferometer such errors can be as large as 10 percent. For more accurate analysis, these authors proposed to use a linear-frequency correction to the long wavelength approximation. In this paper we revisit these calculations. We show that the linear-frequency correction is inadequate for certain locations in the sky and therefore accurate analysis requires taking into account the exact formula, commonly derived from the photon round-trip propagation time. Also, we extend the calculations to include the effect of Fabry-Perot resonators in the interferometer arms. Here we show that a simple approximation which combines the long-wavelength Michelson response with the single-pole approximation to the Fabry-Perot transfer function produces rather accurate results. In particular, the difference between the exact and the approximate formulae is at most 2-3 percent for those locations in the sky where the detector response is greater than half of its maximum value. We analyse the impact of such errors on detection sensitivity and parameter estimation in searches for periodic gravitational waves emitted by a known pulsar, and in searches for an isotropic stochastic gravitational-wave background. At frequencies up to 1 kHz, the effect of such errors is at most 1-2 percent. For higher frequencies, or if more accuracy is required, one should use the exact formula for the response.", "label": 1, "domain": "academic", "token_count": 349, "matched_pair_id": "conditionality_00076", "split": "train"}
{"id": "conditionality_train_pos_0583", "text": "If we follow an asexually reproducing population through time, then the amount of time that has passed since the most recent common ancestor (MRCA) of all current individuals lived will change as time progresses. The resulting \"MRCA age\" process has been studied previously when the population has a constant large size and evolves via the diffusion limit of standard Wright--Fisher dynamics. For any population model, the sample paths of the MRCA age process are made up of periods of linear upward drift with slope +1 punctuated by downward jumps. We build other Markov processes that have such paths from Poisson point processes on $\\mathbb{R}_{++}\\times\\mathbb{R}_{++}$ with intensity measures of the form $\\lambda\\otimes\\mu$ where $\\lambda$ is Lebesgue measure, and $\\mu$ (the \"family lifetime measure\") is an arbitrary, absolutely continuous measure satisfying $\\mu((0,\\infty))=\\infty$ and $\\mu((x,\\infty))<\\infty$ for all $x>0$. Special cases of this construction describe the time evolution of the MRCA age in $(1+\\beta)$-stable continuous state branching processes conditioned on nonextinction--a particular case of which, $\\beta=1$, is Feller's continuous state branching process conditioned on nonextinction. As well as the continuous time process, we also consider the discrete time Markov chain that records the value of the continuous process just before and after its successive jumps. We find transition probabilities for both the continuous and discrete time processes, determine when these processes are transient and recurrent and compute stationary distributions when they exist.", "label": 1, "domain": "academic", "token_count": 337, "matched_pair_id": "conditionality_00103", "split": "train"}
{"id": "conditionality_train_pos_0584", "text": "if you're stuck, consider what Einstein said: You don't solve a problem by looking at it in the same way, try looking at things from a new angle. Agnew fits writing into her job as a primary school teacher by getting up at 5:30am to write before the school day starts. What inspired her to become a writer? Agnew \"grew up in a house full of books\" and her dad was a journalist who writes non-fiction, but really, she says, she \"just wanted to do it.\" In the first session with Tania Roxborogh, Leonie Agnew and David Elliot I felt an overall theme of the elusive - of capturing the elusive writing spark, capturing the Snark, and elusive invisible friends. Another theme that came through for me was the theme of imagination: imagine if someone was trying to take your land, imagine wondrous creatures and lands, imagine how an imaginary friend would feel if they discovered they weren't real. Imagine. Session Two: Des Hunt, Jenny Cooper and Simon Pollard Des Hunt has a love of adventure stories, science, New Zealand animals and he combines all of these into his stories. Sunken Forest was inspired by a real life summer camp he went on when he was 15 at Lake Waikaremoana, a trip that was memorable partly for sparking his interest in geology. The lake was formed during an earthquake landslide that drowned the forest. Standing tree trunks eerily remain there underwater today. Also trapped there are eels which can't make their way back to sea to migrate to the Pacific islands to lay eggs. Unable to leave, they grow exponentially large. In Sunken Forest, one such eel befriends Matt, who is sent to boot camp after his father, a boy racer, is sentenced to prison. At camp, Matt has to deal with bullies and getting the blame for things he didn't do. In his talk, Des Hunt totally engaged his audience from beginning to end, by which time he had them on the edge of their seats. He cleverly demonstrated the idea of building tension in a story by blowing up a balloon... about to burst at any moment. How do you really build tension in a story? He says: Add conflict and injustice, a disaster and... Pop!... an explosive climax. While many of those who spoke at the event started writing or drawing as early as their primary school years, surprisingly Des only published his first fiction book when", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00611", "split": "train"}
{"id": "conditionality_train_pos_0585", "text": "1961, there are authorized to be appropriated to the President $5,000,000 for fiscal year 1999, $7,500,000 for fiscal year 2000, and $8,000,000 for fiscal year 2001 to carry out section 129 of the Foreign Assistance Act of 1961, as added by subsection (a). (2) Availability of funds.--Amounts appropriated pursuant to this subsection shall remain available until expended. (c) Effective Date.--The amendment made by subsection (a) shall take effect on October 1, 1998. SEC. 9. MULTILATERAL ASSISTANCE. (a) Funding.--Of the amounts authorized to be appropriated for fiscal years 1999, 2000, and 2001 pursuant to chapter 1 of part I of the Foreign Assistance Act of 1961, there are authorized to be appropriated to the United Nations Voluntary Fund for Victims of Torture (in this section referred to as the ``Fund'') the following amounts for the following fiscal years: (1) Fiscal year 1999.--For fiscal year 1999, $3,000,000. (2) Fiscal year 2000.--For fiscal year 2000, $3,000,000. (3) Fiscal year 2001.--For fiscal year 2001, $3,000,000. (b) Availability of Funds.--Amounts appropriated pursuant to subsection (a) shall remain available until expended. (c) Sense of Congress.--It is the sense of Congress that the President, acting through the United States Permanent Representative to the United Nations, should-- (1) request the Fund-- (A) to find new ways to support and protect treatment centers and programs that are carrying out rehabilitative services for victims of torture; and (B) to encourage the development of new such centers and programs; (2) use the voice and vote of the United States to support the work of the Special Rapporteur on Torture and the Committee Against Torture established under the Convention Against Torture and Other Cruel, Inhuman or Degrading Treatment or Punishment; and (3) use the voice and vote of the United States to establish a country rapporteur or similar procedural mechanism to investigate human rights violations in a country if either the Special Rapporteur or the Committee Against Torture indicates that a systematic practice of torture is prevalent in that country.", "label": 1, "domain": "government", "token_count": 499, "matched_pair_id": "conditionality_00898", "split": "train"}
{"id": "conditionality_train_pos_0586", "text": "The purpose of this paper is to find optimal estimates for the Green function of a half-space of {\\it the relativistic $\\alpha$-stable process} with parameter $m$ on $\\Rd$ space. This process has an infinitesimal generator of the form $mI-(m^{2/\\alpha}I-\\Delta)^{\\alpha/2},$ where $0<\\alpha<2$, $m>0$, and reduces to the isotropic $\\alpha$-stable process for $m=0$. Its potential theory for open bounded sets has been well developed throughout the recent years however almost nothing was known about the behaviour of the process on unbounded sets. The present paper is intended to fill this gap and we provide two-sided sharp estimates for the Green function for a half-space. As a byproduct we obtain some improvements of the estimates known for bounded sets specially for balls. The advantage of these estimates is a clarification of the relationship between the diameter of the ball and the parameter $m$ of the process. The main result states that the Green function is comparable with the Green function for the Brownian motion if the points are away from the boundary of a half-space and their distance is greater than one. On the other hand for the remaining points the Green function is somehow related the Green function for the isotropic $\\alpha$-stable process. For example, for $d\\ge3$, it is comparable with the Green function for the isotropic $\\alpha$-stable process, provided that the points are close enough.", "label": 1, "domain": "academic", "token_count": 310, "matched_pair_id": "conditionality_00010", "split": "train"}
{"id": "conditionality_train_pos_0587", "text": "The DAMA/NaI and DAMA/LIBRA annual modulation data, which may be interpreted as a signal for the existence of weakly interacting dark matter (WIMPs) in our galactic halo, are examined in light of null results from other experiments. We use the energy spectrum of the combined DAMA modulation data given in 36 bins, and include the effect of channeling. Several statistical tools are implemented in our study: likelihood ratio with a global fit and with raster scans in the WIMP mass and goodness-of-fit (g.o.f.). These approaches allow us to differentiate between the preferred (global best fit) and allowed (g.o.f.) parameter regions. It is hard to find WIMP masses and couplings consistent with all existing data sets. For spin-independent (SI) interactions, the best fit DAMA regions are ruled out to the 3$\\sigma$ C.L., even with channeling taken into account. However, for WIMP masses of ~8 GeV some parameters outside these regions still yield a moderately reasonable fit to the DAMA data and are compatible with all 90% C.L. upper limits from negative searches, when channeling is included. For spin-dependent (SD) interactions with proton-only couplings, a range of masses below 10 GeV is compatible with DAMA and other experiments, with and without channeling, when SuperK indirect detection constraints are included; without the SuperK constraints, masses as high as ~20 GeV are compatible. For SD neutron-only couplings we find no parameters compatible with all the experiments. Mixed SD couplings are examined: e.g. ~8 GeV mass WIMPs with a_n = +/- a_p are found to be consistent with all experiments. In short, there are surviving regions at low mass for both SI and SD interactions; if indirect detection limits are relaxed, some SD proton-only couplings at high masses also survive.", "label": 1, "domain": "academic", "token_count": 389, "matched_pair_id": "conditionality_00075", "split": "train"}
{"id": "conditionality_train_pos_0588", "text": "Unless you happen to be a film buff or just like reading the odd tabloid, you may not know who Harvey Weinstein is. But if you do, then you’ll know he’s something of a Hollywood kingpin, a super-producer with six Oscars to his name, and movies like Pulp Fiction, Good Will Hunting and Shakespeare in Love dotting his resumé. You’ll also know he’s been dodging rumours of sexual harassment for over three decades. In an explosive report by The New York Times published Thursday after The Hollywood Reporter revealed Wednesday that Weinstein was preparing to file a lawsuit against the paper, details of countless allegations of sexual harassment against him were revealed, backed up by legal records, emails and internal documents from his companies. Many of his former employees revealed they were aware of his behaviour for years. The women making the allegations range from their 20s to 40s, all in different cities (Weinstein is known to flit from New York to London to Paris). Several said they didn’t report Weinstein because they were afraid of retaliation, because there weren’t witnesses, or simply because they felt embarrassed. Weinstein, who has been married to designer Georgina Chapman for 10 years (with whom he has two children), has reached at least eight settlements with different women. A follow-up report on Weinstein is set to be published by The New Yorker in the coming weeks, but for now, here are the biggest takeaways from the NYT: Ashley Judd comes forward In 1997, while she was filming Kiss the Girls (a Weinstein Company movie), Weinstein invited actress Ashley Judd to his Beverly Hills hotel room, wearing nothing but a bathrobe. He asked her if she would either give him a massage or watch him shower. When she declined, he asked her for a shoulder rub (she declined again). Countless actresses reported Weinstein making the same requests of them over the decades. He would often tell them he’d “boost” their career if they accepted his advances, and would also boast about famous actresses he claimed to have slept with. Speaking to the NYT, Judd said, “Women have been talking about Harvey amongst ourselves for a long time, and it’s simply beyond time to have the conversation publicly.” In 1997, Weinstein reached a US$100,000 settlement with actress Rose McGowan, 23 at the time, “after an episode in a hotel room” at the Sundance Film Festival. His legal team noted that the settlement", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00665", "split": "train"}
{"id": "conditionality_train_pos_0589", "text": "The effective potential in the Grumiller's modified gravity [D. Grumiller, Phys. Rev. Lett {\\bf 105}, 211303 (2010)] includes the Newtonian potential and a Rindler term. The fitting to the rotation curve data of eight galaxies suggests a universal Rindler acceleration $a\\approx 0.30\\times 10^{-10}$ m s$^{-2}$. We do a two-parameter fit first, with the mass-to-light ratio ($\\Upsilon_*$) and the Rindler acceleration ($a$) as free parameters. It is found that the data of six out of the eight galaxies fit well with the prediction of theory in the range $0\\lesssim r \\lesssim 40$ kpc, although the theoretical curves show a tendency of arising beyond this range. The Rindler accelerations of the six well-fitted galaxies have the same magnitude, with an average value $\\bar{a}\\approx0.30\\times 10^{-10}$ m s$^{-2}$. Inspired by this fact, we then carry out a one-parameter ($\\Upsilon_*$) fit to the six galaxies, with $a$ fixed at $\\bar{a}$, and find that the theory can still reproduce the observation. The value of Rindler acceleration we get here is a quarter of that of Milgrom's MOND. For the rest two galaxies, NGC5055 and DDO154, the fitting results are significantly improved if the photometric scale length ($h$) is included as another free parameter.", "label": 1, "domain": "academic", "token_count": 328, "matched_pair_id": "conditionality_00494", "split": "train"}
{"id": "conditionality_train_pos_0590", "text": "We present parameter-free predictions of the nuclear modification factor, R_{AA}^pi(p_T,s), of high p_T pions produced in Pb+Pb collisions at sqrt{s}_{NN}=2.76 and 5.5 ATeV based on the WHDG/DGLV (radiative+elastic+geometric fluctuation) jet energy loss model. The initial quark gluon plasma (QGP) density at LHC is constrained from a rigorous statistical analysis of PHENIX/RHIC pi^0 quenching data at sqrt{s}_{NN}=0.2 ATeV and the charged particle multiplicity at ALICE/LHC at 2.76 ATeV. Our perturbative QCD tomographic theory predicts significant differences between jet quenching at RHIC and LHC energies, which are qualitatively consistent with the p_T-dependence and normalization---within the large systematic uncertainty---of the first charged hadron nuclear modification factor, R^{ch}_{AA}, data measured by ALICE. However, our constrained prediction of the central to peripheral pion modification, R^pi_{cp}(p_T), for which large systematic uncertainties associated with unmeasured p+p reference data cancel, is found to be over-quenched relative to the charged hadron ALICE R^{ch}_{cp} data in the range 5<p_T<20 GeV/c. The discrepancy challenges the two most basic jet tomographic assumptions: (1) that the energy loss scales linearly with the initial local comoving QGP density, rho_0, and (2) that \\rho_0 \\propto dN^{ch}(s,C)/dy is proportional to the observed global charged particle multiplicity per unit rapidity as a function of sqrt{s} and centrality class, C. Future LHC identified (h=pi,K,p) hadron R^h_{AA} data (together with precise p+p, p+Pb, and Z boson and direct photon Pb+Pb control data) are needed to assess if the QGP produced at LHC is indeed less opaque to jets than predicted by constrained extrapolations from RHIC.", "label": 1, "domain": "academic", "token_count": 443, "matched_pair_id": "conditionality_00325", "split": "train"}
{"id": "conditionality_train_pos_0591", "text": "Aims. We search for transiting circumbinary (CB) planets around eclipsing binaries (EBs). Methods. CB-BLS is a recently-introduced algorithm for the detection of transiting CB planets around EBs.We describe progress in search sensitivity, generality and capability of CB-BLS, and detection tests of CB-BLS on simulated data. We also describe an analytical approach for the determination of CB-BLS detection limits, and a method for the correct detrending of intrinsically-variable stars. Results. We present some blind-tests with simulated planets injected to real CoRoT data. The presented upgrades to CB-BLS allowed it to detect all the blind tests successfully, and these detections were in line with the detection limits analysis. We also correctly detrend bright eclipsing binaries from observations by the TrES planet search, and present some of the first results of applying CB-BLS to multiple real light curves from a wide-field survey. Conclusions. CB-BLS is now mature enough for its application to real data, and the presented processing scheme will serve as the template for our future applications of CB-BLS to data from wide-field surveys such as CoRoT. Being able to put constraints even on non-detection will help to determine the correct frequency of CB planets, contributing to the understanding of planet formation in general. Still, searching for transiting CB planets is still a learning experience, similarly to the state of transiting planets around single stars only a few years ago. The recent rapid progress in this front, coupled with the exquisite quality of space-based photometry, allows to realistically expect that if transiting CB planets exist - then they will soon be found.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00139", "split": "train"}
{"id": "conditionality_train_pos_0592", "text": "an alien may be eligible to be granted the status of having been lawfully admitted for permanent residence under this section shall not preclude the alien from seeking such status under any other provision of law for which the alien may be eligible. SEC. 3. AMENDMENTS TO NICARAGUAN ADJUSTMENT AND CENTRAL AMERICAN RELIEF ACT. (a) Elimination of Limitations on Judicial Review.-- (1) Adjustment of status of certain nicaraguans and cubans.--Section 202(f) of the Nicaraguan Adjustment and Central American Relief Act is amended to read as follows: ``(f) Judicial Review.--A determination by the Attorney General as to whether the status of any alien should be adjusted under this section is subject to judicial review in accordance with chapter 7 of title 5, United States Code.''. (2) Special rule for certain aliens granted temporary protection from deportation.--Section 309(c)(5)(C)(ii) of the Illegal Immigration Reform and Immigrant Responsibility Act of 1996, as added by section 203(a)(1) of the Nicaraguan Adjustment and Central American Relief Act, is amended to read as follows: ``(ii) Judicial review.--A determination by the Attorney General as to whether an alien satisfies the requirements of clause (i) is subject to judicial review in accordance with chapter 7 of title 5, United States Code. Nothing in the preceding sentence shall be construed as limiting the application of section 242(a)(2)(B) of the Immigration and Nationality Act (as in effect after the title III-A effective date) to other eligibility determinations pertaining to discretionary relief under this Act.''. (b) Elimination of Temporary Reductions in Visas.--Section 203 of the Nicaraguan Adjustment and Central American Relief Act is amended-- (1) by striking subsections (d) and (e); and (2) by redesignating subsection (f) as subsection (d). (c) Effective Date.--The amendments made by this section-- (1) shall take effect upon the enactment of the Nicaraguan Adjustment and Central American Relief Act; and (2) shall be effective as if included in the enactment of such Act.", "label": 1, "domain": "government", "token_count": 451, "matched_pair_id": "conditionality_00900", "split": "train"}
{"id": "conditionality_train_pos_0593", "text": "Get daily updates directly to your inbox + Subscribe Thank you for subscribing! Could not subscribe, try again later Invalid Email Students at Helsby High School took part in a range of activities with the theme All Different, All Equal. The school held a non-uniform day when children and staff had to wear something blue to support the cause and raise awareness for anti-bullying week. They raised £1,200 in donations, which will go to the charity Bullying UK. Year 11 student leaders produced a video clip, which is hosted on the school’s YouTube channel, which sees students from all year groups contributing. This video clip was played in assemblies and in form time. Students from all form classes held class discussions on four main questions: 1. What is bullying? 2. Who can you go to for help? 3. Why is it important to stop bullying? 4. Is there anything we could do at Helsby High School to help prevent it? (Image: UGC) Each form class was then given the opportunity to contribute to the anti-bullying board. The next step is for this information to be collated and shared with the student leaders and pastoral leaders. A set of action points will then be created. At Helsby High School, they take any reporting of alleged bullying very seriously. As a school community they do not tolerate any form of bullying. Each and every member of the school community has a part to play in this by either reporting or helping to resolve any alleged bullying. All students are expected to treat fellow students with respect and consideration by following the school’s Code of Conduct. The school strives that if a student is experiencing bullying or has witnessed bullying, they are able to voice their concerns without fear or prejudice.", "label": 1, "domain": "news", "token_count": 358, "matched_pair_id": "conditionality_00684", "split": "train"}
{"id": "conditionality_train_pos_0594", "text": "In a recent article, Kholmetskii, Missevitch and Yarmin [\"On the classical analysis of spin-orbit coupling in hydrogenlike atoms,\" Am. J. Phys. 78(4), April 2010 (428-432)] examine in detail the spin-orbit coupling in the semiclassical hydrogenic atom, and identify a need to account for non-Coulomb forces not included in the standard analysis. Kholmetskii, et al., showed that the experimentally-measured coupling continues to be obtained when the new forces are incorporated in the analysis. This requires that the change in orbital radius due to non-Coulomb forces is also properly accounted for. In response to a comment, Kholmetskii, et al., showed that the experimentally-measured coupling continues to be obtained when so-called \"hidden momentum\" forces are also included. However it has been postulated that when hidden momentum is nonvanishing, a corresponding hidden energy must also be present, that was not included in the total energy by Kholmetskii, et al. Hidden energy is postulated necessary to obtaining a relativistically covariant description. Inclusion of hidden energy leads to disagreement with the experimentally-determined spin-orbit coupling magnitude if the Bohr postulate, that orbital angular momentum is quantized in whole multiples of the reduced Planck constant, is assumed to apply to kinetic momentum alone. The empirical result may be recovered in the semiclassical picture and using the general approach developed by Kholmetskii, et al., if the Bohr postulate is reinterpreted to apply to orbital angular momentum that consists of hidden as well as kinetic momentum.", "label": 1, "domain": "academic", "token_count": 333, "matched_pair_id": "conditionality_00257", "split": "train"}
{"id": "conditionality_train_pos_0595", "text": "and this home to amazing youth programs,” Compton wrote on Twitter. Beckham’s group also wants to bring a massive technology park to the site, as well as an underground parking facility, public soccer fields, 500 new hotel rooms, a conference centre, retail stores, restaurants and more. The Beckham franchise, when it gets going, will also bring a training centre and an academy focused on developing local players to the Miami area. The stadium-location quest is just the latest drawn-out chapter in Beckham’s five-years-and-counting marathon to bring MLS back to Miami. The Miami Fusion played from 1998-2001, folding because of poor attendance. Beckham and MLS announced in January that the franchise would be coming to Miami, but nearly every detail about the club remains unclear. There’s no definitive start date — 2020 has been mentioned repeatedly, even though no new stadium could possibly be ready by then — as well as no team name, no logo, no colours, no coaching staff and no front-office personnel. More than a year ago, Miami-Dade County commissioners approved a deal to sell Beckham nearly three acres of county land for $9 million with the belief that it would be the last parcel he needed for a stadium site in the city’s Overtown neighbourhood. But that site was never the preferred choice for Beckham and his group anyway, with the original hope being to build on the waterfront near the Port of Miami. The Overtown site now seems all but doomed, though it’s unclear what would happen if city commissioners or voters block the latest Beckham plan.", "label": 1, "domain": "news", "token_count": 317, "matched_pair_id": "conditionality_00668", "split": "train"}
{"id": "conditionality_train_pos_0596", "text": "Several experimental studies show the existence of leader neurons in population bursts of 2D living neural networks. A leader neuron is, basically, a neuron which fires at the beginning of a burst (respectively network spike) more often that we expect by looking at its whole mean neural activity. This means that leader neurons have some burst triggering power beyond a simple statistical effect. In this study, we characterize these leader neuron properties. This naturally leads us to simulate neural 2D networks. To build our simulations, we choose the leaky integrate and fire (lIF) neuron model. Our lIF model has got stable leader neurons in the burst population that we simulate. These leader neurons are excitatory neurons and have a low membrane potential firing threshold. Except for these two first properties, the conditions required for a neuron to be a leader neuron are difficult to identify and seem to depend on several parameters involved in the simulations themself. However, a detailed linear analysis shows a trend of the properties required for a neuron to be a leader neuron. Our main finding is: A leader neuron sends a signal to many excitatory neurons as well as to a few inhibitory neurons and a leader neuron receives only a few signals from other excitatory neurons. Our linear analysis exhibits five essential properties for leader neurons with relative importance. This means that considering a given neural network with a fixed mean number of connections per neuron, our analysis gives us a way of predicting which neuron can be a good leader neuron and which cannot. Our prediction formula gives us a good statistical prediction even if, considering a single given neuron, the success rate does not reach hundred percent.", "label": 1, "domain": "academic", "token_count": 326, "matched_pair_id": "conditionality_00221", "split": "train"}
{"id": "conditionality_train_pos_0597", "text": "Recent publications claim that there is no convincing evidence for measurements of the baryonic acoustic (BAO) feature in galaxy samples using either monopole or radial information. Different claims seem contradictory: data is either not consistent with the BAO model or data is consistent with both the BAO model and featureless models without BAO. We investigate this point with a set of 216 realistic mock galaxy catalogs extracted from MICE7680, one of the largest volume dark matter simulation run to date, with a volume of 1300 cubical gigaparsecs. Our mocks cover similar volume, densities and bias as the real galaxies and provide 216 realizations of the Lambda or w=-1 Cold Dark Matter (wCDM) BAO model. We find that only 20% of the mocks show a statistically significant (3 sigma) preference for the true (input) wCDM BAO model as compared to a featureless (non-physical) model without BAO. Thus the volume of current galaxy samples is not yet large enough to claim that the BAO feature has been detected. Does this mean that we can not locate the BAO position? Using a simple (non optimal) algorithm we show that in 50% (100%) of the mocks we can find the BAO position within 5% (20%) of the true value. These two findings are not in contradiction: the former is about model selection, the later is about parameter fitting within a model. We conclude that current monopole and radial BAO measurements can be used as standard rulers if we assume wCDM type of models.", "label": 1, "domain": "academic", "token_count": 328, "matched_pair_id": "conditionality_00281", "split": "train"}
{"id": "conditionality_train_pos_0598", "text": "2 of the meetings each year shall take place in person at the Department's headquarters in the District of Columbia. Participants should make every effort within reason to attend these meetings in person. (4) Agenda.--Each meeting shall be conducted in accordance with an agenda formulated by the chairman of the Committee, with input from other Committee members. (5) Department representation.--Each meeting of the Committee shall be attended by the Secretary or the Secretary's designee. (f) Compensation and Travel Expenses.--Each member of the Committee who is not a full-time employee of the United States shall-- (1) be entitled to receive compensation at a rate not to exceed the daily equivalent of the annual rate of basic pay in effect for a position at level V of the Executive Schedule under section 5316 of title 5, United States Code, for each day during which the member is engaged in the actual performance of the duties of the Committee; and (2) while away from the home or regular place of business of the member in the performance of services for the Committee, be allowed travel expenses, including per diem in lieu of subsistence, in the same manner as persons employed intermittently in the Government service are allowed expenses under section 5703 of title 5, United States Code. (g) Staff.--The Department shall make available to the Committee such staff as the chairman of the Committee determines are necessary to carry out the functions of the Committee. (h) Review by Department.--The Department shall-- (1) review the findings and recommendations of the Committee; and (2) each time the Committee submits a finding or recommendation to the Department, promptly, but no more than 60 days after submission, issue a public statement, a copy of which shall be delivered to Committee members-- (A) assessing the finding or recommendation of the Committee; and (B) disclosing the action, if any, the Department intends to take with respect to the finding or recommendation.", "label": 1, "domain": "government", "token_count": 394, "matched_pair_id": "conditionality_00913", "split": "train"}
{"id": "conditionality_train_pos_0599", "text": "TiVo is (cleverly) turning things upside down for Super Bowl LII with introduction of GameSkip. This first-time feature for TiVo DVRs flips the company’s SkipMode—which skips commercials in some shows—on its head. With GameSkip, TiVo users can skip the game and get right to the important bits—Super Bowl commercials and the Halftime Show. Firstly, TiVo’s website is oh-so-careful not to mention the Super Bowl by name. I’m not sure why, since the whole point of the event is to submerse us in a marketing bath, but it’s notable in TiVo’s description: This coming Sunday, February 4, is the day TV fans wait all year for. Sure, the big game’s great and all, but for those who tune in for the multi-million-dollar commercials and the world’s biggest halftime show, we’ve got the perfect solution: TiVo GameSkip. This first-time feature turns SkipMode™ upside-down. After recording the big game, look for the on-screen SKIP icon next to the recording. Then hit play, press the SKIP button1 and your TiVo will jump to the beginning of the next commercial break! Kind of makes you want to give us a high-five, right? I’ll admit that I love and hate this. I haven’t had time for sports in a long, long time. So, you know, lolfunny. At the same time, there’s a part of me appalled at how commercial advertising has become content in and of itself. It’s perverse, and yet another step towards a cyberpunk future where we’re all slaves to the Corp. Then again, I enjoy watching, writing, and talking about Apple’s advertising, so my I may need a hand getting up on my high horse on this topic. And while we’re at it, you can just watch teasers for the commercials on TiVo’s site. So there’s that, too. Anyhoo…TiVo is giving its customers an interesting choice this year with GameSkip. I’d love to hear if you’d use it, or not, and why.", "label": 1, "domain": "news", "token_count": 435, "matched_pair_id": "conditionality_00567", "split": "train"}
{"id": "conditionality_train_pos_0600", "text": "job. Is there a misconception where these skilled jobs have to be dirty and dangerous? MR: The problem isn't that so much has changed in that world; the problem in my view is that higher ed needed a PR campaign in the ’50s and ’60s. We actually needed more people to enthusiastically matriculate through universities. Society really could benefit from more liberal arts classical thought and more people with a broad-based understanding of stuff. And so the push for college in my view was legitimate. Unfortunately, the push for college came at the expense of other forms of education. And this is just a classic trap in most forms of advocacy and PR. You promote one thing not to the betterment of itself but at the expense of the other. So the proposition became “if you don't go to a four-year school, you're going to wind up over here in this shit hole. But if you wind up over there, then the kind of job you're going to get is going to make you want to kill yourself. So the whole transaction became fraught with false consequences. That's how we promote it. I still have a poster that was in my guidance counselor’s office that was really one of the first attempts to broadly promote college with a platitude, and the platitude was “Work smart, not hard.” And that's really where a lot of people just assume it's a logical thing with regard to heightened efficiency and of course it is. But that caption appeared on a photo of a kid holding a diploma next to a skilled worker holding a wrench and looking like he just won a vocational consolation prize. mikeRoweWORKS When you start telling kids that if you don't work smart, you'll have no choice but to work hard, you're giving them this \"Let's Make a Deal” choice, where behind the curtain is nothing but a box of Borax or a brand new, shiny Corvette. It's not fair, it's not right, it's not sensible. But that basic notion has infected and informed a big chunk of our culture, and consequently you've got well over $1 trillion in student loans on the books and you've got over 6 million jobs that are currently open, many in manufacturing, many in the skilled trades — and few of which require a four-year degree. So that's your disconnect in a nutshell. Today we have this notion that if you're unhappy in your work it's because your work is making you unhappy.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00613", "split": "train"}
{"id": "conditionality_train_pos_0601", "text": "unemployment account was established before the date of enactment of this Act, the Temporary Extended Unemployment Compensation Act of 2002 (as amended by this Act) shall be applied subject to the following: (A) Any amounts deposited in the individual's temporary extended unemployment compensation account by reason of section 203(c) of such Act (commonly known as ``TEUC-X amounts'') before the date of enactment of this Act shall be treated as amounts deposited by reason of section 203(b) of such Act (commonly known as ``TEUC amounts''), as deemed to have been amended by subsection (c)(1). (B) For purposes of determining whether the individual is eligible for any TEUC-X amounts under such Act, as deemed to be amended by this section-- (i) any determination made under section 203(c) of such Act before the application of the amendment described in subsection (c)(2) shall be disregarded; and (ii) any such determination shall instead be made by applying section 203(c) of such Act, as deemed to be amended by subsection (c)(2)-- (I) as of the time that all amounts established in such account in accordance with section 203(b) of such Act (as deemed to be amended under this section, and including any amounts described in subparagraph (A)) are in fact exhausted, except that (II) if such individual's account was both augmented by and exhausted of all TEUC-X amounts before the date of enactment of this Act, such determination shall be made as if exhaustion (as described in section 203(c)(1) of such Act) had not occurred until such date of enactment.", "label": 1, "domain": "government", "token_count": 339, "matched_pair_id": "conditionality_00885", "split": "train"}
{"id": "conditionality_train_pos_0602", "text": "Study.--Not later than 180 days after the date of enactment of this Act, the Secretary shall conduct a study to determine the effectiveness and feasibility of establishing 1 or more propane storage facilities, to be operated separately from the Strategic Petroleum Reserve established under part B of title I of the Energy Policy and Conservation Act (42 U.S.C. 6231 et seq.). (b) Plan.--Following completion of the study under subsection (a), the Secretary may submit to Congress and the President a plan describing-- (1) the proposed acquisition of storage and related facilities or storage services for, including-- (A) the potential use of storage facilities not currently in use; and (B) a determination of the combination of primary, secondary, and tertiary storage facilities that will be used; (2) the proposed acquisition of propane for storage; (3) the proposed methods of disposition of propane; (4) the estimated costs of establishment, maintenance, and operation; (5) the efforts the Secretary will make-- (A) to minimize any potential need for future drawdowns; and (B) to ensure that distributors and importers are not discouraged from maintaining and increasing supplies of propane; (6) the proposed actions to ensure the quality of the propane; and (7) the proposed accounts and funding structures required for acquisition of propane and propane storage facilities. SEC. 7. STORAGE FACILITY LOANS FOR PROPANE STORAGE. Section 1614(a) of the Food, Conservation, and Energy Act of 2008 (7 U.S.C. 8789(a)) is amended by inserting ``, including facilities for propane that is used for drying and heating'' before the period at the end. SEC. 8. STUDY OF JURISDICTION. Not later than 1 year after the date of enactment of this Act, the Comptroller General of the United States shall complete a study of facilities appurtenant to propane pipelines (such as terminals and storage facilities) that are not subject to the jurisdiction of the Commission (as of the date on which the study commences) to determine-- (1) whether the nonjurisdictional nature of the facilities is injurious to shippers or consumers; and (2)(A) whether the facilities can be placed under the jurisdiction of the Commission; or (B) if not, whether changes in law to place the facilities under the jurisdiction of the Commission are in the public interest.", "label": 1, "domain": "government", "token_count": 494, "matched_pair_id": "conditionality_01025", "split": "train"}
{"id": "conditionality_train_pos_0603", "text": "We investigate the orientation correlation of giant elliptical galaxies by measuring the intrinsic ellipticity correlation function of 83,773 luminous red galaxies (LRGs) at redshifts 0.16 -- 0.47 from the Sloan Digital Sky Survey. We have accurately determined the correlation up to 30 $h^{-1}$Mpc. Luminosity dependence of the ellipticity correlation is also detected although the error bars are large, while no evidence is found for its redshift evolution between $z=0.2$ and $z=0.4$. Then we use a cosmological $N$-body simulation to examine misalignment between the central LRGs and their parent dark matter halos. Central and satellite galaxies are assigned to simulated halos by employing a halo occupation distribution model for the LRGs. The ellipticity correlation is predicted to have the same shape as but an amplitude about 4 times higher than our observation if the central LRGs are perfectly aligned with their host halos. This indicates that the central LRG galaxies are preferentially but not perfectly aligned with their host halos. With the assumption that there is a misalignment angle between a central LRG and its host halo which follows a Gaussian distribution with a zero mean and a width $\\sigma_\\theta$, we obtain a tight constraint on the misalignment parameter, $\\sigma_\\theta={35.4}^{+4.0}_{-3.3}$ deg. This type of intrinsic ellipticity correlation, if not corrected, can lead to contamination at 5% level to the shear power spectrum in weak lensing surveys of limiting magnitude $R_{AB}=24.5$ if the source central galaxies follow the same misalignment distribution as the LRGs.", "label": 1, "domain": "academic", "token_count": 355, "matched_pair_id": "conditionality_00084", "split": "train"}
{"id": "conditionality_train_pos_0604", "text": "If the gas in filaments and halos shares the same velocity field than the luminous matter, it will generate measurable temperature anisotropies due to the Kinematic Sunyaev-Zeldovich effect. We compute the distribution function of the KSZ signal produced by a typical filament and show it is highly non-gaussian. The combined contribution of the Thermal and Kinematic SZ effects of a filament of size $L\\simeq 5$Mpc and electron density $n_e\\simeq 10^3m^{-3}$ could explain the cold spots of $\\delta\\sim -200\\mu$K on scales of 30' found in the Corona Borealis Supercluster by the VSA experiment. PLANCK, with its large resolution and frequency coverage, could provide the first evidence of the existence of filaments in this region. The KSZ contribution of the network of filaments and halo structures to the radiation power spectrum peaks around $l\\sim 400$, a scale very different from that of clusters of galaxies, with a maximum amplitude $l(l+1)C_l/2\\pi\\sim 10-25 (\\mu K)^2$, depending on model parameters, i.e., $\\sigma_8$ and the Jeans length. About 80% of the signal comes from filaments with redshift $z\\le 0.1$. Adding this component to the intrinsic Cosmic Microwave Background temperature anisotropies of the concordance model improves the fit to WMAP 3yr data by $\\Delta\\chi^2\\simeq 1$. The improvement is not statistically significant but a more systematic study could demonstrate that gas could significantly contribute to the anisotropies measured by WMAP.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00041", "split": "train"}
{"id": "conditionality_train_pos_0605", "text": "If Amazon does acquire a pharmaceutical company, it could cause buyer's remorse for CVS, Mr. Coker said. The retail pharmacy chain intends to finance the transaction with $45 billion in debt. \"This Aetna deal could be boneheaded if CVS's goal is to shore up its defenses against an inevitable entry against Amazon into the market,\" he said. \"Health insurers are part of why drugs are so expensive. Amazon approaches markets by eliminating the middleman. It seems that CVS is making a bet that health insurers are going to continue to be the dominate intermediary between a consumer and drugmaker.\" Investors also appear to have doubts about how much the drugstore chain was willing to pay for Aetna: CVS Health Corp.'s stock fell $3.41, or nearly 5 percent, to $71.69 on the New York Stock Exchange, although the Dow Jones index was up strongly for most of the day. Joel Espelien, a senior research analyst at The Diffusion Group, agreed that Amazon will put pressure on CVS and Aetna after the deal is completed. \"CVS didn't want to just be a distributor, so it bought a health plan,\" he said. \"But disruption can change how business is done in that industry. Amazon will force CVS and Aetna to dramatically up their game.\" Even if Amazon's first step in the health care industry is offering prescriptions through its website, Mr. Espelien said, that could create fierce competition in the sector. He predicts prescriptions will be delivered via drones within minutes along with other supply advantages that only Amazon can offer. \"It doesn't mean CVS can't compete with Amazon, but if they can't match what Amazon is doing, they will be in serious trouble,\" he said. The time is right for Amazon to enter the health care industry because of its proven ability to reduce costs in an industry that has long struggled to keep expenses down and prices competitive. \"When I look at a retail pharmacy, it strikes me as fairly inefficient,\" Mr. Coker said. \"They have to maintain that expensive floor space, expensive pharmacist, cash register. Maybe you can achieve greater economies of scale by moving that to a call center in India like Amazon did with the book industry.\" © 2017 Washington Times under contract with NewsEdge/Acquire Media. All rights reserved. Image credit: CVS/iStock/Artist's concept.", "label": 1, "domain": "news", "token_count": 485, "matched_pair_id": "conditionality_00629", "split": "train"}
{"id": "conditionality_train_pos_0606", "text": "or 4091 of such Code shall, insofar as applicable and not inconsistent with the provisions of this subsection, apply with respect to the floor stocks taxes imposed by paragraph (1) to the same extent as if such taxes were imposed by such section 4081 or 4091, as the case may be. (e) Effective Dates.-- (1) Fuel taxes.--The amendments made by subsection (a) shall apply to periods beginning on or after the 7th day after the date of the enactment of this Act. (2) Ticket taxes.-- (A) In general.--The amendments made by subsection (b) shall apply to transportation beginning on or after such 7th day. (B) Exception for certain payments.--Except as provided in subparagraph (C), the amendments made by subsection (b) shall not apply to any amount paid before such 7th day. (C) Payments of property transportation tax within controlled group.--In the case of the tax imposed by section 4271 of the Internal Revenue Code of 1986, subparagraph (B) shall not apply to any amount paid by 1 member of a controlled group for transportation furnished by another member of such group. For purposes of the preceding sentence, all persons treated as a single employer under subsection (a) or (b) of section 52 of the Internal Revenue Code of 1986 shall be treated as members of a controlled group. (f) Application of Look-Back Safe Harbor for Deposits.--Nothing in the look-back safe harbor prescribed in Treasury Regulation section 40.6302(c)-1(c)(2) shall be construed to permit such safe harbor to be used with respect to any tax unless such tax was imposed throughout the look-back period.", "label": 1, "domain": "government", "token_count": 353, "matched_pair_id": "conditionality_00893", "split": "train"}
{"id": "conditionality_train_pos_0607", "text": "if we need it at all, if we do, we then enact democratic legislation that will ensure there is transparency and accountability in the appointment process and execution of duty, which conduct must be guided by the Constitution. “For many years the Censorship Board has assumed the notorious character of a morality police as well as an unchecked gatekeeper who decides what content is right or wrong for Zimbabweans. “They have banned some plays with political satire and films that reflect badly on the ruling elite all on flimsy grounds that they were not suitable for the majority of the people. “And now that Chombo says the new board will extend its control tentacles to the social media, it’s clear it’s not about the contested moral righteousness but policing citizens’ artistic freedoms, freedom of expression, generation and access to information online and offline,” said Ngwenya. He added that Zimbabwe does not need another body or layer of repression under the guise of promoting morality; it needs democratic laws and institutions that will ensure constitutionalism goes beyond simply flaunting the Constitution. Playwright and actor Slyvanos Mudzvova said this board has actually been put to silence mainly artists dealing with human rights-related artistic products. “The board consists of people who have no experience in dealing with artistic products at all. Their agenda is so simple — ban anything that is critical to President Robert Mugabe and his regime. “Serious artists will not submit anything to this board as a way of protest for its composition,” said Mudzvova. Social commentator Rejoice Ngwenya said: “With the drastic modernisation of the creative industry (e-ntertainment, e-reading, the drone and virtual creations), it’s surprising that Mugabe can appoint dinosaurs, drunken with conservative stupour, to preside over 21st Century creativity. “It shows Mugabe views everything through the partisan prism, with an eye on 2018. What these human fossils do not know is that the IOT (internet of things) no longer allows political hoodlums clad in statutory censorship clothes to poison creativity.” Theatre producer Mthabisi Phili believes any sinking man will catch at a straw. “They are catching at straws now; I think Zanu PF is strengthening its censorship and control muscle ahead of the upcoming elections. “It’s more of a political move than just the employment of people. The true colours that we are under a dictatorship are really coming out through the rampant nepotism and focus", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00618", "split": "train"}
{"id": "conditionality_train_pos_0608", "text": "We present observations of the O VI system at z_abs = 0.495096 toward PKS 0405-123 (z_em = 0.5726) obtained with FUSE and STIS. In addition to strong O VI, with log N(O VI) = 14.47+/-0.02, and moderate H I this absorber shows C III, N IV, O IV, and O V, with upper limits for another seven ions. The large number of available ions allows us to test ionization models usually adopted with far less contraints. We find the ionic column densities cannot be matched by collisional ionization models, in or out of equilibrium. Photoionization models can match the observed column densities, including O VI. If one assumes photoionization by a UV background dominated by QSOs, the metallicity of the gas is [O/H] = -0.15, while a model for the UV background with contributions from ionizing photons escaping from galaxies gives [O/H] = -0.62. Both give [N/O] ~ -0.6 and [C/H] ~ -0.2 to -0.1. The choice of ionizing spectrum is poorly constrained. Multiphase models with a contribution from both photoionized gas (at T~10^4 K) and collisionally ionized gas (at T~(1-3)x10^5 K) can also match the observations giving very similar metallicities. The O VI in this system is not necessarily a reliable tracer of WHIM matter. We do not detect Ne VIII or Mg X absorption. The limit on Ne VIII/O VI < 0.21 (3 sigma), the lowest yet observed. Thus this absorber shows no firm evidence of the \"warm-hot intergalactic medium\" at T~(0.5-3)x10^6 K thought to contain a significant fraction of the baryons at low redshift. We present limits on the total column of warm-hot gas in this absorber as a function of temperature. This system would be unlikely to provide detectable X-ray absorption in the ions O VII or O VIII even if it resided in front of the brighter X-ray sources in the sky.", "label": 1, "domain": "academic", "token_count": 461, "matched_pair_id": "conditionality_00126", "split": "train"}
{"id": "conditionality_train_pos_0609", "text": "We examine the Lagrangian divergence of the displacement field, arguably a more natural object than the density in a Lagrangian description of cosmological large-scale structure. This quantity, which we denote \\psi, quantifies the stretching and distortion of the initially homogeneous lattice of dark-matter particles in the universe. \\psi\\ encodes similar information as the density, but the correspondence has subtleties. It corresponds better to the log-density A than the overdensity \\delta. A Gaussian distribution in \\psi\\ produces a distribution in A with slight skewness; in \\delta, we find that in many cases the skewness is further increased by 3. A local spherical-collapse-based (SC) fit found by Bernardeau gives a formula for \\psi's particle-by-particle behavior that works quite well, better than applying Lagrangian perturbation theory (LPT) at first or second (2LPT) order. In 2LPT, there is a roughly parabolic relation between initial and final \\psi\\ that can give overdensities in deep voids, so low-redshift, high-resolution 2LPT realizations should be used with caution. The SC fit excels at predicting \\psi\\ until streams cross; then, for particles forming haloes, \\psi\\ plummets as in a waterfall to -3. This gives a new method for producing N-particle realizations. Compared to LPT realizations, such SC realizations give reduced stream-crossing, and better visual and 1-point-PDF correspondence to the results of full gravity. LPT, on the other hand, predicts large-scale flows and the large-scale power-spectrum amplitude better, unless an empirical correction is added to the SC formula.", "label": 1, "domain": "academic", "token_count": 354, "matched_pair_id": "conditionality_00438", "split": "train"}
{"id": "conditionality_train_pos_0610", "text": "We consider a Hamiltonian action of n-dimensional torus, T^n, on a compact symplectic manifold (M,\\omega) with d isolated fixed points. For every fixed point p there exists (though not unique) a class a_p in H^*_{T}(M; Q) such that the collection {a_p}, over all fixed points, forms a basis for H^*_{T}(M; Q) as an H^*(BT; Q) module. The map induced by the inclusion, \\iota^*:H^*_{T}(M; Q) \\rightarrow H^*_{T}(M^{T}; Q)= \\oplus_{j=1}^{d}Q[x_1, ..., x_n] is injective. We use such classes {a_p} to give necessary and sufficient conditions for f=(f_1, ...,f_d) in \\oplus_{j=1}^{d}Q[x_1, ..., x_n] to be in the image of \\iota^*, i.e. to represent an equiviariant cohomology class on M. In the case when T is a circle and present these conditions explicitly. We explain how to combine this 1-dimensional solution with Chang-Skjelbred Lemma in order to obtain the result for a torus T of any dimension. Moreover, for a GKM T-manifold M our techniques give combinatorial description of H^*_{K}(M; Q), for a generic subgroup K \\hookrightarrow T, even if M is not a GKM K-manifold.", "label": 1, "domain": "academic", "token_count": 327, "matched_pair_id": "conditionality_00253", "split": "train"}
{"id": "conditionality_train_pos_0611", "text": "If you live in a region where temperatures routinely dip below freezing this time of year, you know that vehicle maintenance requirements shift along with the weather. While keeping up with your customers’ maintenance needs is always essential for business, there are some areas of the country where winter maintenance takes on a whole new level of importance. In America’s coldest cities, poor vehicle maintenance isn’t just a repair issue — it’s a safety issue. Being stranded with a broken-down car in extreme temperatures isn’t an option. So, how do shops in some of America’s coldest climates keep their customers’ cars running through even the worst winter conditions? The answer, it turns out, is just a little preparation. Setting Up Seasonal Inspections It’s nice to have proactive customers who want to take care of maintenance issues before something goes wrong. Unfortunately, not all customers have this kind of foresight. Whether or not the temperature drops to 50 below where you live, the arrival of winter weather puts the onus on shops to be more direct in selling winter inspections. Talk to your customers about the importance of being more proactive in servicing their vehicles during winter. While they may be familiar with the recommended service intervals in their owner’s manuals, you need to be conservative when it comes to winter maintenance. ”You need to offer your experience when thinking about maintenance intervals,” said Mike Simard, owner, Simard Automotive in Fairbanks, AK. “The independent industry does roughly 80% of all maintenance work in this country; so, we’ve learned a thing or two about vehicles that are no longer under warranty. Essentially, we want to take the manufacturer’s recommendation and pair that with our years of experience to make an appropriate recommendation on winter maintenance.” Fluids Vehicles using contaminated fluids or fluids that are mixed in the wrong concentration are especially susceptible to failure during winter. That’s because fluids don’t give off many warning signs when they need to be changed. They also are rarely checked by most drivers. Check the motor oil on every inspection. If your shop is in a region where temperatures routinely drop below freezing, you might consider switching to a lower viscosity oil. Regardless of what oil you’re using, recommend an oil change to help the customer’s engine run easier upon startup. “We recommend oil changes after most tune-ups and battery replacements that were done after a vehicle failed to start,” said Jason Emrick, ASE Master/L1 technician, Lloyd’s Automotive in St. Paul, MN. “At a", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00756", "split": "train"}
{"id": "conditionality_train_pos_0612", "text": "If you’ve never found yourself on the powerless end of a longterm relationship that’s falling apart before your eyes, well—I haven’t either, but I imagine it’s awful. Of the many Magnetic Fields songs that document such resignation, “You’re My Only Home” has stuck with me the longest because of its despairing chorus: “When you cancel dinner plans/when you cross the street and you don’t take my hand/ when you make impossible demands/I wish I didn’t understand.” Bracketed by earnest declarations of devotion, the song’s center reveals its narrator to be a realist, someone who understands that whatever relationship he’s in is already over—that even if he isn’t technically alone, he’s on his own. Also, the way Stephen Merritt drops his voice when he croons “street” makes me grin every time. — TAYLOR BERMAN NSYNC, “Tearin’ Up My Heart” This is the first song about heartbreak I remember really being affected by. There’s never been a point in my life since its release that I haven’t been able to sing its chorus, and the damaged sweetness of boy band vocals are particularly good at conveying this sort of infinite internal turmoil. — JORDAN SARGENT Aaliyah, “We Need a Resolution” ft. Timbaland In which Timbaland the No Good, fed up with the drama, decides to abandon his girl for a night out, as he justifies himself with a charismatically corny verse—“I’m tired of these scars!”—that rides off the defense of wounded masculinity. I suppose confronting that hurt would be the noble course of action here, but this verse consoles me because of its moral: Life is too short not to be petty. It’s an easy mantra to remember when an ex removes you from Facebook or what-have-you. I will keep shining, boo. — BRIAN JOSEPHS The Mountain Goats, “Game Shows Touch Our Lives” Tallahassee is a devastating album about the death throes of a married couple’s relationship, but no song locates the heartbreaking mix of tenderness and bitterness involved with a protracted breakup like “Game Shows Touch Our Lives,” in which the couple watches game shows while getting stupid drunk. Darnielle’s narrator hands his soon-to-be-ex-wife a bottle of liquor, and delivers a heartbreaking, unadorned line: “People say friends don’t destroy one", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00652", "split": "train"}
{"id": "conditionality_train_pos_0613", "text": "and inserting ``4''. (b) Effective Date.--The amendments made by subsection (a) shall apply to weeks of unemployment beginning 6 months or more after the date of the enactment of this Act. SEC. 102. INCREASE AND DECREASE IN EARNINGS CREDITED TO STATE ACCOUNTS WHEN STATES MEET OR FAIL TO MEET FUNDING GOALS. (a) In General.--Section 904 of the Social Security Act (42 U.S.C. 1104) is amended by adding at the end the following new subsection: ``(h) Increase and Decrease in Amount of Earnings Allocated to State Accounts When States Meet or Fail To Meet Funding Goals.--(1) If the average daily balance in a State account in the Unemployment Trust Fund for any calendar quarter exceeds the funding goal of such State, the amount otherwise creditable to such account under subsection (e) for such quarter shall be increased by the interest premium on such excess. If the average daily balance in such a State account for any calendar quarter is less than the funding goal of such State, the amount otherwise creditable to such account under subsection (e) for such quarter shall be decreased by the interest penalty. ``(2) Paragraph (1) shall not apply with respect to any interest premium or interest penalty to the extent that such application would result in an increase or decrease of more than $2,500,000 in the amount creditable to any State account for any calendar quarter. ``(3) For purposes of this subsection, the term `interest premium' means, for any calendar quarter-- ``(A) with respect to the State with the largest percentage value of excess of the average daily balance in the State account in the Unemployment Trust Fund over the funding goal of such State, one-half of one percent of the amount of such excess, and ``(B) with respect to each other State, the product of-- ``(i) the amount of the excess of the average daily balance in the State account in the Unemployment Trust Fund over the funding goal of such State, and ``(ii) the percentage which bears the same ratio to one-half of one percent as-- ``(I) the percentage value of such excess, bears to ``(II) the percentage value of the excess of the State referred to in subparagraph (A). The Secretary shall make appropriate adjustments in the interest premium for any calendar quarter if the aggregate interest premiums payable for such quarter exceed the aggregate interest penalties for such quarter.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00933", "split": "train"}
{"id": "conditionality_train_pos_0614", "text": "The non-local thermodynamic equilibrium (NLTE) line formation of neutral boron in the atmospheres of cool stars are investigated. Our results confirm that NLTE effects for the B I resonance lines, which are due to a combination of overionization and optical pumping effects, are most important for hot, metalpoor, and low-gravity stars; however, the amplitude of departures from LTE found by this work are smaller than that of previous studies. In addition, our calculation shows that the line formation of B I will get closer to LTE if the strength of collisions with neutral hydrogen increases, which is contrary to the result of previous studies. The NLTE line formation results are applied to the determination of boron abundances for a sample of 16 metal-poor stars with the method of spectrum synthesis of the B I 2497 A resonance lines using the archived HST/GHRS spectra. Beryllium and oxygen abundances are also determined for these stars. The abundances of the nine stars which are not depleted in Be or B show that, no matter the strength of collisions with neutral hydrogen may be, both Be and B increase with O quasi-linearly in the logarithmic plane, which confirms the conclusions that Be and B are mainly produced by primary process in the early Galaxy. The most noteworthy result of this work is that B increases with Fe or O at a very similar speed as, or a bit faster than Be does, which is in accord with the theoretical models. The B/Be ratios remain almost constant over the metallicity range investigated here. Our average B/Be ratio falls in the interval [13+-4, 17+-4], which is consistent with the predictions of spallation process. The contribution of B from the nu-process may be required if the 11B/10B isotopic ratios in metal-poor stars are the same as the meteoric value.", "label": 1, "domain": "academic", "token_count": 385, "matched_pair_id": "conditionality_00200", "split": "train"}
{"id": "conditionality_train_pos_0615", "text": "We present a study of the chemistry of a dense photon-dominated region (PDR) using a time-dependent chemical model. Our major interest is to study the spatial distribution of complex molecules such as hydrocarbons and cyanopolyynes in the cool dense material bordering regions where star formation has taken place. Our standard model uses a homogeneous cloud of density 2x10e4 cm-3 and temperature T=40 K, which is irradiated by a far-ultraviolet radiation field of intermediate intensity, given by X=100. We find that over a range of times unsaturated hydrocarbons (e.g., C2H, C4H, C3H2) have relatively high fractional abundances in the more external layers of the PDR, whereas their abundances in the innermost layers are several orders of magnitudes lower. On the other hand, molecules that are typical of late-time chemistry are usually more abundant in the inner parts of the PDR. We also present results for models with different density, temperature, intensity of the radiation field and initial fractional abundances. Our results are compared with both high- and moderate-angular resolution observations of the Horsehead nebula. Our standard model is partially successful in reproducing the observations. Additional models run with different physical parameters are able to reproduce the abundance of many of the observed molecules, but we do not find a single model that fits all the observations at the same time. We discuss the suitability of a time-dependent model of a dense PDR such as ours as an estimator of the age of a PDR, provided that enough observational data exist.", "label": 1, "domain": "academic", "token_count": 324, "matched_pair_id": "conditionality_00083", "split": "train"}
{"id": "conditionality_train_pos_0616", "text": "If things go as planned, Kris Aquino will join the cast of the Warner Brothers movie of the bestseller “Crazy Rich Asians”—the first Filipino woman to be cast in this Hollywood movie. Aquino flew to Los Angeles on Easter Sunday to meet with the producers and sign the contract, sources say. About six Filipino actresses, according to sources, had auditioned, but apparently only Aquino had landed a role, so far. ADVERTISEMENT 2013 bestseller The movie is based on Kevin Kwan’s 2013 bestseller about an old-wealth Singaporean family, its matriarch Eleanor Young (to be played by Michelle Yeoh), and its heir apparent—the Ivy-League-educated Nick Young, who flies home to Singapore for a friend’s wedding with his New Yorker girlfriend in tow. Kwan gives readers a jaw-dropping glimpse of the lives—and secrets—of the rich and the chi-chi set. Kwan followed up this bestseller with “China Rich Girlfriend” (2015) and just this year, “Rich People Problems.” Kwan was in Manila about two years ago and met the lifestyle set—and apparently drew inspiration from some of its characters. “Rich People Problems” has characters whose names curiously sound like those of Metro Manila’s A-listers, such as Diego San Antonio (Inquirer columnist Anton San Diego?) and Doris Hoh (business leader Doris Magsaysay-Ho). Obviously Kwan and the movie producers have had Aquino on their radar. According to our sources—and which Aquino confirmed in her Instragram post—Grammy and Tony award-winning producer Jhett Tolentino tried to contact Aquino through intermediaries—specifically Nene Chan and Rep. Len Alonte. Instagram post In her Instagram post, Aquino wrote she had only a few days to prepare an audition reel, so she got a suite at Peninsula Manila to mount the audition shoot, tapping her network that included director Ricky Villabona, Jules Dacanay and makeup artist Juan Sarte. The team then did rush editing and color grading of her audition reel and video biography. Director Jon Chu (“Step Up,” “GI Joe”) and the producers liked the reels, said our sources, and thus Aquino got the part of an Asian princess—a minor yet significant part. “At this particular point in my life, to have the Hollywood door open is God-sent,” Aquino said. ADVERTISEMENT And the suspense", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00551", "split": "train"}
{"id": "conditionality_train_pos_0617", "text": "If Flowers is traded, the Giants are going to have to draft a tackle or sign one as a free agent. Odell Beckham Jr., who missed most of last season with a broken ankle, and defensive end Olivier Vernon were both at the minicamp. They skipped the minicamp a year ago. “I think the big thing for us is our game is very simple — it’s about the ball, it’s about negotiating the ground and it’s really about man whipping man,” Shurmur said. The minicamp, which does not entail any hitting, is more about making sure players get to know the new systems, with some throwing and receiving mixed in. The defences can work on stripping the ball. There was speculation that Shurmur wanted to use the minicamp to see what quarterback Davis Webb could do. The third-round pick did nothing last season, so the Giants really don’t know what they have with their backup to Eli Manning. “I don’t think there needs to be any anxiety on his part — get trained up, come on out here, let it rip and mistakes happen in practice and you learn from them,” Shurmur said. “I think that’s why you practice, so I think you have to be careful about making a final evaluation on a guy in a three-day period here. He just needs to come out here and get as good as he can be.” Most players said they felt they were entering this season with a clean slate. Cornerback Janoris Jenkins, who was suspended for a game last season after missing a practice, intends to be on his best behaviour this season. “I promise y’all that Jackrabbit says it won’t happen this year what happened last year,” he said. “There won’t be any animosity between players, no disrespecting the coach. There will be none of that. New York Giant football is back.” Jenkins also believes fellow cornerback and 2016 first-round draft pick Eli Apple, who also was suspended for a game, will be a different player this season. “You have to understand that he was young,” Jenkins said. “It’s a clean slate, new coaching staff and for him it’s guys like me that have to push him and help him out because I’ve been in the league so long and just help him understand that adversity is going to hit you and when it hits, you’ve just got to keep it going.” Beckham did not take part in the afternoon practice", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00667", "split": "train"}
{"id": "conditionality_train_pos_0618", "text": "`Small Business Protection Account' means a trust created or organized in the United States for the exclusive benefit of the taxpayer, but only if the written governing instrument creating the trust meets the following requirements: ``(A) No contribution will be accepted for any taxable year in excess of the amount allowed as a deduction under subsection (a) for such year. ``(B) The trustee is a bank (as defined in section 408(n)) or another person who demonstrates to the satisfaction of the Secretary that the manner in which such person will administer the trust will be consistent with the requirements of this section. ``(C) The assets of the trust consist entirely of cash or of obligations which have adequate stated interest (as defined in section 1274(c)(2)) and which pay such interest not less often than annually. ``(D) All income of the trust is distributed currently to the grantor. ``(E) The assets of the trust will not be commingled with other property except in a common trust fund or common investment fund. ``(2) Account taxed as grantor trust.--The grantor of a Small Business Protection Account shall be treated for purposes of this title as the owner of such Account and shall be subject to tax thereon in accordance with subpart E of part I of subchapter J of this chapter (relating to grantors and others treated as substantial owners). ``(e) Inclusion of Amounts Distributed.-- ``(1) In general.--Except as provided in paragraph (2), there shall be includible in the gross income of the taxpayer for any taxable year-- ``(A) any amount distributed from a Small Business Protection Account of the taxpayer during such taxable year, and ``(B) any deemed distribution under-- ``(i) subsection (f)(1) (relating to deposits not distributed within 5 years), ``(ii) subsection (f)(2) (relating to cessation in eligible small business), and ``(iii) subparagraph (A) or (B) of subsection (f)(3) (relating to prohibited transactions and pledging account as security). ``(2) Exceptions.--Paragraph (1)(A) shall not apply to-- ``(A) any distribution to the extent attributable to income of the Account, and ``(B) the distribution of any contribution paid during a taxable year to a Small Business Protection Account to the extent that such contribution exceeds the limitation applicable under subsection (b) if requirements similar to the requirements of section 408(d)(4) are met.", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00841", "split": "train"}
{"id": "conditionality_train_pos_0619", "text": "if any, opportunities for diversion, storage, or other uses of water occurring outside such lands that would adversely affect the wilderness or other values of such lands; (B) the lands designated as wilderness by this Act generally are not suitable for use for development of new water resource facilities, or for the expansion of existing facilities; (C) it is possible to provide for proper management and protection of the wilderness and other values of such lands in ways different from those utilized in other legislation designating as wilderness lands not sharing the attributes of the lands designated as wilderness by this Act. (2) Statutory construction.-- (A) Nothing in this Act shall constitute or be construed to constitute either an express or implied reservation of any water or water rights with respect to the lands designated as a national conservation area or as wilderness by this Act. (B) Nothing in this Act shall affect any conditional or absolute water rights in the State of Colorado existing on the date of the enactment of this Act. (C) Nothing in this subsection shall be construed as establishing a precedent with regard to any future national conservation area or wilderness designations. (D) Nothing in this Act shall be construed as limiting, altering, modifying, or amending any of the interstate compacts or equitable apportionment decrees that apportion water among and between the State of Colorado and other States. (3) Colorado water law.--The Secretary shall follow the procedural and substantive requirements of the law of the State of Colorado in order to obtain and hold any new water rights with respect to the Conservation Area and the Wilderness. (4) New projects.-- (A) As used in this paragraph, the term ``water resource facility'' means irrigation and pumping facilities, reservoirs, water conservation works, aqueducts, canals, ditches, pipelines, wells, hydropower projects, and transmission and other ancillary facilities, and other water diversion, storage, and carriage structures. Such term does not include any such facilities related to or used for the purpose of livestock grazing. (B) Except as otherwise provided by section 6(g) or other provisions of this Act, on and after the date of the enactment of this Act, neither the President nor any other officer, employee, or agent of the United States shall fund, assist, authorize, or issue a license or permit for the development of any new water resource facility within the wilderness area designated by this Act. (C) Except as provided in this paragraph, nothing in this Act", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_01020", "split": "train"}
{"id": "conditionality_train_pos_0620", "text": "A British judge heard a new appeal Tuesday from the parents of a terminally ill British toddler who want to take him to Italy for treatment — something British courts have ruled isn't in the child's interest. The Christian Legal Centre, which is supporting the parents of 23-month-old Alfie Evans, said lawyers would repeat a request to judge Anthony Hayden to allow the boy to be cared for at the Vatican's hospital in Rome. The judge appeared to rule that out at an emergency court hearing in Manchester, but asked whether there might be \"other options\" that involved Alfie's parents taking their son home. The hearing was adjourned while the hospital considered the question. Doctors say Alfie is in a \"semi-vegetative state\" as a result of a degenerative neurological condition that medics have been unable to identify precisely. Doctors treating him at Alder Hey Children's Hospital say he has little brain function and further treatment is futile. But his parents have refused to accept the decision and fought to prevent Alfie's life support being switched off. He was taken off life support Monday after a series of court rulings blocked further medical treatment. Alfie's father Tom Evans said earlier Tuesday that Alfie survived for six hours with no assistance, and that doctors had subsequently resumed providing oxygen and hydration. In court, the family's lawyer, Paul Diamond, read a statement from Tom Evans saying his son was doing \"significantly better\" than previously believed. Evans, 21, and Alfie's mother Kate James, 20, want to take Alfie to the Vatican's Bambino Gesu Pediatric Hospital. Doctors at Alder Hey Hospital in Liverpool, northwest England, believe that would not be in the boy'ss best interests, and British courts have agreed. Emotions have run high over the case, with a band of supporters known as \"Alfie's Army\" protesting regularly outside the hospital. They have blocked roads and on Monday tried to storm a door of the hospital before being pushed back by police. The case has also drawn the attention of Pope Francis, who during a Sunday blessing in St. Peter's Square this month offered prayers for Alfie and others who are suffering from serious infirmities. Francis has made appeals for the boy to be kept alive, saying only God can decide who dies. The head of the Vatican's Bambino Gesu Pediatric Hospital said the Italian defense ministry had a plane ready to transport Alfie to Italy if he were allowed.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00545", "split": "train"}
{"id": "conditionality_train_pos_0621", "text": "If it hadn’t been for Kerry Packer, World Series Cricket and the smartphone, England’s Ben Stokes might well be out in Australia defending the Ashes, this winter, rather than waiting at home to see if he’ll be charged with actual bodily harm, after that brawl in Bristol, last September. Crispin Andrews is a freelance cricket expert who writes for the Cricketer, Cricinfo, Inside Cricket and the Nightwatchman. World Series Cricket began,forty years ago, this December. Australian media tycoon, Packer, was refused international broadcast rights by the Australian Cricket Board, so he signed up the world’s best players on lucrative contracts and put on his own contests.Two years later, the ACB gave Packer his TV deal and the players returned to their international sides. Before World Series Cricket, international cricketers were paid peanuts. Ever since, cricket boards have been increasingly aware that if they don’t pay their best players what the players think they’re worth; someone else will, these days most probably a T20 franchise. To raise money to pay their stars, and of course their own salaries, cricket board executives turn to corporate sponsors. ECB made £1.1bn from their last TV deal alone. Corporates sponsor cricket teams because they think it will help them sell more of whatever they sell. They like their chosen teams to be full of well spoken, nicely turned out lads. The sort the company CEO might hire as an office junior, or even invite home to meet his or her, daughter. What the corporates don’t want are charismatic, colourful types who can’t be trusted to say the right things at the right time. People like Kevin Pietersen, and Tony Greig, who in 1976, on national TV, announced that he’d make the West Indies grovel. Imagine the outrage if the England captain said that today. The ECB’s corporate benefactors would be queuing up to sponsor tennis. And now an England cricketer gets filmed fighting in the streets and the footage ends up in the national newspapers. Even if the ECB wanted to be lenient to England’s star player, there’s no way the corporates are going to have that sort of thing associated with their brand. Stokes has nothing to complain about, whoever started the fight, and for whatever reasons. He is an England cricketer, well aware of the standards of behaviour his employers expect, of what is likely to happen to", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00515", "split": "train"}
{"id": "conditionality_train_pos_0622", "text": "the prior month. ``(2) Publication.--The Secretary shall make the information reported under paragraph (1) available to the public on the first reporting day of the each month, not later than 10:00 a.m. Central Time, categorized by location and product characteristics.''; and (3) in subsection (d) (as redesignated by paragraph (2))-- (A) in paragraph (3), by adding at the end the following: ``(C) Cold storage survey.-- ``(i) In general.--For purposes of the cold storage survey of the National Agricultural Statistics Service, each facility storing dairy products shall report to the Secretary each month information on the quantity of dairy products stored. ``(ii) Audit.--Subject to the availability of appropriations, the Secretary shall take such measures as are necessary to audit the survey described in clause (i) and ensure compliance with the reporting requirement. ``(D) Dairy products survey.-- ``(i) In general.--For purposes of the dairy products survey of the National Agricultural Statistics Service, each manufacturer storing dairy products shall report to the Secretary each month information on the quantity of dairy products stored. ``(ii) Audit.--The Secretary shall take such measures as are necessary to audit the survey described in clause (i) and ensure compliance with the reporting requirement.''; and (B) by adding at the end the following ``(7) Survey products.--In carrying out this section, the Secretary shall require each manufacturer and other appropriate person to report to the Secretary, at a periodic interval determined by the Secretary, information on the products in the cold storage survey and the dairy products survey of the National Agricultural Statistics Service. ``(8) Exemption.--The Secretary may exempt from all reporting requirements under this section any manufacturer or facility that stores less than an average of 10,000 pounds monthly on an annual basis. ``(9) Collection and publication of data.--The Secretary shall collect and publish data on actual milk prices paid by dairy processors.''. SEC. 7. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 488, "matched_pair_id": "conditionality_00887", "split": "train"}
{"id": "conditionality_train_pos_0623", "text": "members of which are public officials, and (iii) not more than one-third of the members of which are individuals who are or were at any time within 5 years before the beginning of a term of membership on the board, an employee of, independent contractor with respect to, officer of, director of, or held a material financial interest in, a commercial forest products enterprise with which the qualified organization has a contractual or other financial arrangement, (D) the bylaws of which require at least two-thirds of the members of the board of directors to vote affirmatively to approve the qualified conservation plan and any change thereto, and (E) upon dissolution, is required to dedicate its assets to-- (i) an organization described in section 501(c)(3) of such Code which is organized and operated for conservation purposes, or (ii) a governmental unit described in section 170(c)(1) of such Code. (4) Unrelated person.--The term ``unrelated person'' means a person who is not a related person. (5) Related person.--A person shall be treated as related to another person if-- (A) such person bears a relationship to such other person described in section 267(b) (determined without regard to paragraph (9) thereof), or 707(b)(1), of such Code, determined by substituting ``25 percent'' for ``50 percent'' each place it appears therein, and (B) in the case such other person is a non-profit organization, if such person controls directly or indirectly more than 25 percent of the governing body of such organization.", "label": 1, "domain": "government", "token_count": 325, "matched_pair_id": "conditionality_00927", "split": "train"}
{"id": "conditionality_train_pos_0624", "text": "We reexamine the 1/S-correction to the self-energy of the gapless magnon of a D-dimensional quantum Heisenberg antiferromagnet in a uniform magnetic field h using a hybrid approach between 1/S-expansion and non-linear sigma model, where the Holstein-Primakoff bosons are expressed in terms of Hermitian field operators representing the uniform and the staggered components of the spin-operators [N. Hasselmann and P. Kopietz, Europhys. Lett. {\\bf{74}}, 1067 (2006)]. By integrating over the field associated with the uniform spin-fluctuations we obtain the effective action for the staggered spin-fluctuations on the lattice, which contains fluctuations on all length scales and does not have the cutoff ambiguities of the non-linear sigma model. We show that in dimensions D <= 3 the magnetic field dependence of the spin-wave velocity c(h) is non-analytic in h^2, with c(h) - c(0) proportional to h^2 \\ln | h | in D=3, and c(h) - c(0) proportional to | h | in D=2. The frequency dependent magnon self-energy is found to exhibit an even more singular magnetic field dependence, implying a strong momentum dependence of the quasi-particle residue of the gapless magnon. We also discuss the problem of spontaneous magnon decay and show that in D > 1 dimensions the damping of magnons with momentum k is proportional to |k|^{2D -1} if spontaneous magnon decay is kinematically allowed.", "label": 1, "domain": "academic", "token_count": 331, "matched_pair_id": "conditionality_00059", "split": "train"}
{"id": "conditionality_train_pos_0625", "text": "If $\\Sigma=(X,\\sigma)$ is a topological dynamical system, where $X$ is a compact Hausdorff space and $\\sigma$ is a homeomorphism of $X$, then a crossed product Banach $\\sp{*}$-algebra $\\ell^1(\\Sigma)$ is naturally associated with these data. If $X$ consists of one point, then $\\ell^1(\\Sigma)$ is the group algebra of the integers. The commutant $C(X)'_1$ of $C(X)$ in $\\ell^1(\\Sigma)$ is known to be a maximal abelian subalgebra which has non-zero intersection with each non-zero closed ideal, and the same holds for the commutant $C(X)'_*$ of $C(X)$ in $C^*(\\Sigma)$, the enveloping $C^*$-algebra of $\\ell^1(\\Sigma)$. This intersection property has proven to be a valuable tool in investigating these algebras. Motivated by this pivotal role, we study $C(X)'_1$ and $C(X)'_*$ in detail in the present paper. The maximal ideal space of $C(X)'_1$ is described explicitly, and is seen to coincide with its pure state space and to be a topological quotient of $X\\times\\mathbb{T}$. We show that $C(X)'_1$ is hermitian and semisimple, and that its enveloping $C^*$-algebra is $C(X)'_*$. Furthermore, we establish necessary and sufficient conditions for projections onto $C(X)'_1$ and $C(X)'_*$ to exist, and give explicit formulas for such projections, which we show to be unique. In the appendix, topological results for the periodic points of a homeomorphism of a locally compact Hausdorff space are given.", "label": 1, "domain": "academic", "token_count": 388, "matched_pair_id": "conditionality_00340", "split": "train"}
{"id": "conditionality_train_pos_0626", "text": "if you do something bad, you can die. So nature has kind of tuned us to look at the negative side because if you get a bit more food, a bit more money or whatever, there’s a positive expected value but it’s limited. Whereas on the negative side, you can lose a lot. So because of that we just attune more to losses. Image source: Getty Images. Rana Pritanjali:What do you think are some of the most important traits of successful investors? Dan Ariely:Maybe not follow your emotions. Human emotions get us to buy high and sell low, so we have to fight those. And being systematic. Looking forward rather than backward. Thinking about what you want to do moving forward and not looking at what’s happened to the stock in the past. Not being impulsive is important, and not following the herd. And then the other one, I would say, is that it’s about setting up processes that help us to do things in a more systematic way. So if you basically create a system where you say, “Here are my rules. I’m going to sell when it hits this number. I’m going to buy when it hits this number. I’m going to do X, Y, and Z.” If you stick to your rules, you’re probably going to do OK. But what happens is that most of us create rules and then we don’t stick to them, because we are tempted at the moment, so sticking to our rules is important. Rana Pritanjali:Do you believe in “information overload?” How is this affecting us as investors? Dan Ariely:Absolutely. It’s very hard for us to deal with lots and lots of information. Of course, today we’re getting lots and lots of information, so what do we do when we get too much information? We simplify. We use heuristics. We rely on only part of the information. On the most salient information. And that, of course, means that the most salient information is probably the information everybody else knows, as well; so we become less independent in our opinions from other investors. If everybody is in information overload, and we all do simplifications, then what happens is that we follow the simplest source of information, which is probably common to everybody. Rana Pritanjali:What human characteristics will be hardest for robots (or artificial intelligence)to replicate? Dan Ariely:I think ser", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00730", "split": "train"}
{"id": "conditionality_train_pos_0627", "text": "If it looks like a duck and quacks like a duck, it might be a goose. That's how George E. Burns, commissioner for the Financials Department of the State of Nevada, Department of Business & Industry, described the types of depository institutions in the state. They all handle money and extend loans, but they are not all the same. The state of Nevada charters four such institutions: commercial banks, credit unions, savings banks, and industrial loan companies. Each has its own focus, ownership, and regulations, said Burns, who has been in the financial industry for 28 years in both giant and small financial institutions. He was appointed commissioner for the Nevada Department of Business & Industry in 2007. Commercial banks are traditional banks, insured by the FDIC — what people traditionally think of as a bank, he said. They offer a broad range of financial services including saving deposits, loans, mortgages, checks and debit cards. Savings banks evolved from the savings and loan industry, which collapsed in the 1980s and 1990s. Their primary focus is on savings accounts, retirement savings, certificates of deposit and mortgages. Industrial loan companies are owned by non-financial companies and generally provide loans for specific industries. For instance, in Nevada, Toyota Savings provides loans for Toyota products, and Eagle Mark provides loans for Harley Davidson products. Some industrial banks also issue credit cards, and offer mortgages or small business loans. They are state chartered and FDIC insured. Recommended Stories For You Credit unions are similar to commercial banks, except that they are membership-owned nonprofits. As such, they don't pay taxes and because they don't pay taxes, they have more restrictions. For credit unions, their field of membership (FOM) used to be very specific. Over time they expanded, Burns said. Ten credit unions operate in Nevada and each has a different FOM. Members must be individuals, not businesses, and that's where some of the restrictions come in. Originally, credit unions could only offer loans to individuals. Now they can offer loans to members for a members' business, but no more than 1.75 percent of the credit union's net worth. \"The amount they can loan (for a business purpose) is limited,\" Burns said. \"If the focus of a credit union is membership as individuals, they can't go out and make a loan to say, MGM. \"It's being debated in congress whether or not to expand the limit", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00589", "split": "train"}
{"id": "conditionality_train_pos_0628", "text": "if enough time has been given to know whether they work. Since the summer of 2015, farmers in the western basin have been required to meet new regulations for applying manure, and since September 30, 2017, all farmers who apply fertilizer to more than 50 acres must be state certified. Farmers helped form both regulations, but are concerned about what lies ahead. Know the science Joe Cornely, communications director for Ohio Farm Bureau Federation, said it’s important that state regulators not get ahead of the science. He said a lot is still being determined, like how and why nutrients move. “Basing decisions on admittedly inadequate amounts of data is a problem,” he said. Cornely said the state’s approach so far has recognized that improvement takes time, and that more information is needed. In recent years, the Farm Bureau has partnered with state and federal leaders to research new farming practices through the use of demonstration farms and edge-of-field testing — hoping to find solutions that work for farmers and the nonfarm public. He said there has definitely been a sudden “change of tenor” from the state, and that he has “real concerns about the whole ready, fire, aim approach.” Even with the impairment designation, Butler said he doesn’t believe the state will be required to form new Total Daily Maximum Load limits for nutrients, because similar nutrient tracking has already been done. New law Butler is hopeful that a bill will soon be introduced into the state legislature that will lay out the framework for what is expected of agriculture. The bill would include lower phosphorus discharge levels and would also expand the definition of agriculture pollution to include fertilizer. This would allow the EPA to declare parts of watersheds in distress, and focus on specific areas. Butler said the bill has not been popular with farmers and so far a sponsor has not been found. Related coverage:", "label": 1, "domain": "news", "token_count": 374, "matched_pair_id": "conditionality_00631", "split": "train"}
{"id": "conditionality_train_pos_0629", "text": "If the balance has gone awry and coach Alain Vigneault thinks his Rangers are getting away from their high-paced, high-skill game in favor of a more physical brand of hockey needed in the playoffs and enforced by the Canadiens, then a lineup change certainly could help alleviate that. And he did his part in stoking those flames when he had talented 22-year-old Russian winger Pavel Buchnevich rotating in during Monday’s practice at the Garden, as well as having him on the first power-play unit. Buchnevich has been a scratch for the opening three games of this first-round playoff series, the best-of-seven contest in which the Rangers trail, 2-1, heading into Tuesday night’s pivotal Game 4 at the Garden. They are coming off another postseason no-show on Broadway with Game 3’s 3-1 loss Sunday night, when their offense sputtered and their handling of the puck was negligent. But that wasn’t changing Vigneault’s philosophy, even if he does change the lineup in hopes of getting more skill plays. “We’ve been playing a certain style this season that’s permitted us to get into the playoffs that, in my estimation, when we play it, we’re a hard team to play against,” Vigneault said. “I think we’ve shown in this series, in moments when we’ve played that way, we’re a hard team to play against. And from game to game, there’s different things that a certain team might do that’s making them a little harder to handle. “So if you make minor adjustment as far as making a read or a puck decision, it could help your game. But as far as changing the overall way of how we play and how we have success, obviously that’s not going to happen.” Yet inserting Buchnevich in place of Tanner Glass certainly would change the makeup of Vigneault’s lineup, even if Glass has been one of the team’s best forwards through the first three games and one of the only legitimate physical presences on the roster. The two polar opposites took turns rotating on a line with Chris Kreider and Mika Zibanejad, both of whom have struggled. That would be a very skilled line with Buchnevich on the right, and also one that had some success in the preseason and very early in the regular season. But as the grind wore on, Buchnevich missed a lot of time with a core/back issue and never", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00810", "split": "train"}
{"id": "conditionality_train_pos_0630", "text": "We present an analytic model for the interaction between planetary atmospheres and stellar winds from main sequence M stars, with the purpose of obtaining a quick test-model that estimates the timescale for total atmospheric mass loss due to this interaction. Planets in the habitable zone of M dwarfs may be tidally locked and may have weak magnetic fields, because of this we consider the extreme case of planets with no magnetic field. The model gives the planetary atmosphere mass loss rate as a function of the stellar wind and planetary properties (mass, atmospheric pressure and orbital distance) and an entrainment efficiency coefficient $\\alpha$. We use a mixing layer model to explore two different cases: a time-independent stellar mass loss and a stellar mass loss rate that decreases with time. For both cases we consider planetary masses within the range of $1\\to10$ M$_{\\oplus}$ and atmospheric pressures with values of 1, 5 and 10 atm. For the time dependent case, planets without magnetic field in the habitable zone of M dwarfs with initial stellar mass losses of $\\leq \\dot{M}_{w} < 10^{-11}$ M$_{\\odot}$ yr$^{-1}$, may retain their atmospheres for at least 1 Gyr. This case may be applied to early spectral type M dwarfs (earlier than M5). Studies have shown that late type M dwarfs (later than M5) may be active for long periods of time ($\\geq 4$Gyr), and because of that our model with constant stellar mass loss rate may be more accurate. For these stars most planets may have lost their atmospheres in 1 Gyr or less because most of the late type M dwarfs are expected to be active. We emphasize that our model only considers planets without magnetic fields. Clearly we must expect a higher resistance to atmospheric erosion if we include the presence of a magnetic field.", "label": 1, "domain": "academic", "token_count": 388, "matched_pair_id": "conditionality_00234", "split": "train"}
{"id": "conditionality_train_pos_0631", "text": "If a system undergoes symmetric dynamics, then the final state of the system can only break the symmetry in ways in which it was broken by the initial state, and its measure of asymmetry can be no greater than that of the initial state. It follows that for the purpose of understanding the consequences of symmetries of dynamics, in particular, complicated and open-system dynamics, it is useful to introduce the notion of a state's asymmetry properties, which includes the type and measure of its asymmetry. We demonstrate and exploit the fact that the asymmetry properties of a state can also be understood in terms of information-theoretic concepts, for instance in terms of the state's ability to encode information about an element of the symmetry group. We show that the asymmetry properties of a pure state psi relative to the symmetry group G are completely specified by the characteristic function of the state, defined as chi_psi(g)=<psi|U(g)|psi> where g\\in G and U is the unitary representation of interest. For a symmetry described by a compact Lie group G, we show that two pure states can be reversibly interconverted one to the other by symmetric operations if and only if their characteristic functions are equal up to a 1-dimensional representation of the group. Characteristic functions also allow us to easily identify the conditions for one pure state to be converted to another by symmetric operations (in general irreversibly) for the various paradigms of single-copy transformations: deterministic, state-to-ensemble, stochastic and catalyzed.", "label": 1, "domain": "academic", "token_count": 311, "matched_pair_id": "conditionality_00320", "split": "train"}
{"id": "conditionality_train_pos_0632", "text": "If you’re looking for a new budget handset, then it’s likely you’ve watched the Moto G6 with great interest since its reveal. Motorola’s new addition to the Moto G range is set to take the lower-priced market by storm with a brand-new design, more power, and some of the best value for the money that you’re likely to find. But just because it’s a budget phone doesn’t mean it should be going out into the world unprotected. A good protective case can reduce the risk of scratching the Moto G6’s body, shattering the screen, or inflicting any other sort of damage on it. We’ve scoured the internet to find some of the best cases to help keep your Moto G6 looking great all the way to your next upgrade and beyond. Spigen Rugged Armor ($20) We’re starting this list off with one of the best phone case manufacturers out there. Spigen‘s Rugged Armor case is one of the most popular cases around, and it’s easy to see why. Made from shock-absorbent and flexible TPU, the soft surface provides plenty of grip for your fingers, along with great protection from bumps, drops, scratches, and dings. A raised lip around the edges keeps your display and camera lenses elevated from surfaces, and the carbon fiber-style panels at either end of the back lend a cool, futuristic look. Buy one now from: Spigen TopAce Clear Case ($8) Sticking a case over the top of your phone isn’t for everyone — after all, don’t you want to look at the phone you just bought? If you’re that sort of person, but you still want some protection for your Moto G6, then a clear case might be for you. This case from TopAce is made from flexible TPU that adds shock absorbency and a soft surface for your fingers to grip. While this thin case won’t be as protective as a bulkier case, it should still protect well against scratches and bumps, and will offer some resistance to bigger drops and bangs. It’s not a bad little case if you want your phone’s beauty to shine through. Buy one now from: Amazon Dretal Shock Absorbing Magnetic Armor ($9) Looking for a little more protection? Dretal’s Magnetic Armor case is made from a combination of rigid polycarbonate plastic (PC) and soft TPU, giving it a hard backbone, as well as adequate shock-absorbency.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00714", "split": "train"}
{"id": "conditionality_train_pos_0633", "text": "We study the impact of a running index $\\alpha_t$ on the spectrum of relic gravitational waves (RGWs) over the whole range of frequency $(10^{-18}\\sim 10^{10})$ Hz and reveal its implications in RGWs detections and in cosmology. Analytical calculations show that, although the spectrum of RGWs on low frequencies is less affected by $\\alpha_t\\ne 0$, but, on high frequencies, the spectrum is modified substantially. Investigations are made toward potential detections of the $\\alpha_t$-modified RGWs for several kinds of current and planned detectors. The Advanced LIGO will likely be able to detect RGWs with $\\alpha_t\\ge 0$ for inflationary models with the inflation index $\\beta=-1.956$ and the tensor-scalar ratio $r= 0.55$. The future LISA can detect RGWs for a much broader range of ($\\alpha_t$, $\\beta$, $r$), and will have a better chance to break a degeneracy between them. Constraints on $\\alpha_t$ are estimated from several detections and cosmological observations. Among them, the most stringent one is from the bound of the Big Bang nucleosynthesis (BBN), and requires $\\alpha_t < 0.008$ rather conservatively for any reasonable ($\\beta$, $r$), preferring a nearly power-law spectrum of RGWs. In light of this result, one would expect the scalar running index $\\alpha_s$ to be of the same magnitude as $\\alpha_t$, if both RGWs and scalar perturbations are generated by the same scalar inflation.", "label": 1, "domain": "academic", "token_count": 328, "matched_pair_id": "conditionality_00165", "split": "train"}
{"id": "conditionality_train_pos_0634", "text": "If Reese Gullenheimer looks a bit overwhelmed, there's a good reason. #UCBerkeley #abc7now He's moving in for Freshman year. pic.twitter.com/PoCPsRumkr — Wayne Freedman (@WayneFreedman) August 14, 2017 Its a madhouse outside the #UCBerkeley dorms today. Traffic jams. Parents. #abc7now Freshmen moving in. pic.twitter.com/K06VAE4vWc — Wayne Freedman (@WayneFreedman) August 14, 2017 Whether #UCBerkeley or any college/university, this is a lifetime experience. 2nd maybe to 1st day of school. Rough on parents. #ABC7now pic.twitter.com/vxhomY5lZs — Wayne Freedman (@WayneFreedman) August 14, 2017 I have done this day with my own daughter. Was an emotional wreck. #abc7now pic.twitter.com/qSG4ywq6Xo — Wayne Freedman (@WayneFreedman) August 14, 2017 Reese going 6500 new freshmen from all 50 states, 54 countries. 69 percent of #UCBerkeley frosh from California. Average GPA. 3.88. #abc7now pic.twitter.com/Y1EI1tofgF — Wayne Freedman (@WayneFreedman) August 14, 2017 Average #UCBerkely tuition and board for Cal residents will be $34,400. #abc7now pic.twitter.com/q4A7aSI8RK — Wayne Freedman (@WayneFreedman) August 14, 2017 The first night without your kid under your roof is the toughest, Dad. #UCBerkeley #abc7now pic.twitter.com/itI8oDvRtV — Wayne Freedman (@WayneFreedman) August 14, 2017 If the sound of hard wheels rolling across bricks doesn't give it away, then the sight of bins filled with bedding and microwaves, will. Or else, all of those parents having awkward goodbyes with their kids.\"I'm going to cry later,\" said Carl Gullenheimer, a single father, as he dropped off his first-born son Reese for freshman year at UC Berkeley.\"What were you thinking those last few days with him at home?\"", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00525", "split": "train"}
{"id": "conditionality_train_pos_0635", "text": "If a team like the Yankees, who have been above the luxury tax threshold for three consecutive seasons, blows past next season’s $197 million threshold, the tax could be as high as 95 cents for every dollar over the limit that a team spends. The worst offenders will also be docked more valuable draft picks if they sign free agents, will be slotted down 10 spots for their first pick in the draft and could lose as much as $1 million in international pool money. Dipping below the luxury tax threshold will allow them to shed their status as repeat offenders and drastically reduce their tax bill — and their cost in draft picks — if they exceed the threshold again next year, when two young, prized free agents will hit the market: Washington Nationals outfielder Bryce Harper and Baltimore Orioles third baseman Manny Machado. With a raft of expensive, lengthy and burdensome contracts expiring over the last two seasons, the Yankees showed a rare discipline in constructing their roster. They mostly resisted splurging on splashy and pricey free agents, instead focusing on developing and acquiring inexpensive young talent. Photo But when the Yankees failed to even get an audience with the affordable Japanese star Shohei Ohtani, they pivoted in a familiar way — they landed slugger Giancarlo Stanton, the newly minted National League most valuable player. Acquiring Stanton, who is three years into a record-setting 13-year, $325 million contract from the Miami Marlins that is heavily backloaded may not jeopardize the Yankees’ ability to duck below the luxury tax threshold. But it will test their newfound fiscal discipline. Stanton’s charge against the payroll will be $22 million — the average per-year cost of his contract ($25 million) minus the $3 million per year offset from the $30 million the Marlins have agreed to pay the Yankees if Stanton does not opt out of his contract after the 2020 season. But the Yankees also saved $8.5 million by sending second baseman Starlin Castro to the Marlins. Newsletter Sign Up Continue reading the main story Please verify you're not a robot by clicking the box. Invalid email address. Please re-enter. You must select a newsletter to subscribe to. Sign Up You agree to receive occasional updates and special offers for The New York Times's products and services. Thank you for subscribing. An error has occurred. Please try again later. View all New York Times newsletters. According to Cot’s Contracts, which tracks major league payroll tax estimates, the Yankees", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00604", "split": "train"}
{"id": "conditionality_train_pos_0636", "text": "if that collaboration extends to the 5-nanometer technology generation, then Qualcomm would be another company that would make use of such bleeding-edge technology (for both its high-end mobile chips as well as its server processor ambitions). Another company that could benefit from this technology would be graphics specialist NVIDIA (NASDAQ: NVDA), and I wouldn’t be surprised if TSMC sought NVIDIA’s input — at least for a “high-performance” version — for the definition of 5 nanometer. Graphics processors are generally used for applications that require high-performance computing capabilities (it’s not just graphics). Although NVIDIA has said it doesn’t aim to be the first company to new manufacturing technologies, it wants to adopt them shortly after the first-movers (i.e., the Apples of the world) do. 10 stocks we like better than Taiwan Semiconductor Manufacturing When investing geniuses David and Tom Gardner have a stock tip, it can pay to listen. After all, the newsletter they have run for over a decade, Motley Fool Stock Advisor, has tripled the market.* David and Tom just revealed what they believe are the 10 best stocks for investors to buy right now… and Taiwan Semiconductor Manufacturing wasn’t one of them! That’s right — they think these 10 stocks are even better buys. Click here to learn about these picks! *Stock Advisor returns as of April 3, 2017 Ashraf Eassa owns shares of Qualcomm. The Motley Fool owns shares of and recommends Apple, Nvidia, and Qualcomm. The Motley Fool has a disclosure policy.", "label": 1, "domain": "news", "token_count": 316, "matched_pair_id": "conditionality_00727", "split": "train"}
{"id": "conditionality_train_pos_0637", "text": "The signature of a path provides a top down description of the path in terms of its effects as a control [Differential Equations Driven by Rough Paths (2007) Springer]. The signature transforms a path into a group-like element in the tensor algebra and is an essential object in rough path theory. The expected signature of a stochastic process plays a similar role to that played by the characteristic function of a random variable. In [Chevyrev (2013)], it is proved that under certain boundedness conditions, the expected value of a random signature already determines the law of this random signature. It becomes of great interest to be able to compute examples of expected signatures and obtain the upper bounds for the decay rates of expected signatures. For instance, the computation for Brownian motion on $[0,1]$ leads to the ``cubature on Wiener space'' methodology [Lyons and Victoir, Proc. R. Soc. Lond. Ser. A Math. Phys. Eng. Sci. 460 (2004) 169-198]. In this paper we fix a bounded domain $\\Gamma$ in a Euclidean space $E$ and study the expected signature of a Brownian path starting at $z\\in\\Gamma$ and stopped at the first exit time from $\\Gamma$. We denote this tensor series valued function by $\\Phi_{\\Gamma}(z)$ and focus on the case $E=\\mathbb{R}^d$. We show that $\\Phi_{\\Gamma}(z)$ satisfies an elliptic PDE system and a boundary condition. The equations determining $\\Phi_{\\Gamma}$ can be recursively solved; by an iterative application of Sobolev estimates we are able, under certain smoothness and boundedness condition of the domain $\\Gamma$, to prove geometric bounds for the terms in $\\Phi_{\\Gamma}(z)$. However, there is still a gap and we have not shown that $\\Phi_{\\Gamma}(z)$ determines the law of the signature of this stopped Brownian motion even if $\\Gamma$ is a unit ball.", "label": 1, "domain": "academic", "token_count": 417, "matched_pair_id": "conditionality_00308", "split": "train"}
{"id": "conditionality_train_pos_0638", "text": "Let $\\mathcal{F} $ be a pointwise almost periodic decomposition of a compact metrizable space $X$. Then $\\mathcal{F} $ is $R$-closed if and only if $\\hat{\\mathcal{F}} $ is usc. Moreover, if there is a finite index normal subgroup $H$ of an $R$-closed flow $G$ on a compact manifold such that the orbit closures of $H$ consist of codimension $k$ compact connected elements and \"few singularities\" for $k = 1$ or 2, then the orbit class space of $G$ is a compact $k$-dimensional manifold with conners. In addition, let $v$ be a nontrivial $R$-closed vector field on a connected compact 3-manifold $M$. Then one of the following holds: 1) The orbit class space $M/ \\hat{v}$ is $[0,1]$ or $S^1$ and each interior point of $M/ \\hat{v}$ is two dimensional. 2) $\\mathrm{Per}(v)$ is open dense and $M = \\mathrm{Sing}(v) \\sqcup \\mathrm{Per}(v)$. 3) There is a nontrivial non-toral minimal set. On the other hand, let $G$ be a flow on a compact metrizable space and $H$ a finite index normal subgroup. Then we show that $G$ is $R$-closed if and only if so is $H$.", "label": 1, "domain": "academic", "token_count": 326, "matched_pair_id": "conditionality_00491", "split": "train"}
{"id": "conditionality_train_pos_0639", "text": "of conscience in this paragraph constitute the protection of individual rights and create a private cause of action for those persons or entities protected. Any person or entity may assert a violation of this paragraph as a claim or defense in a judicial proceeding. ``(F) Remedies.-- ``(i) Federal jurisdiction.--The Federal courts shall have jurisdiction to prevent and redress actual or threatened violations of this paragraph by granting all forms of legal or equitable relief, including, but not limited to, injunctive relief, declaratory relief, damages, costs, and attorney fees. ``(ii) Initiating party.--An action under this paragraph may be instituted by the Attorney General of the United States, or by any person or entity having standing to complain of a threatened or actual violation of this paragraph, including, but not limited to, any actual or prospective plan sponsor, issuer, or other entity offering a plan, any actual or prospective purchaser or beneficiary of a plan, and any individual or institutional health care provider. ``(iii) Interim relief.--Pending final determination of any action under this paragraph, the court may at any time enter such restraining order or prohibitions, or take such other actions, as it deems necessary. ``(G) Administration.--The Office for Civil Rights of the Department of Health and Human Services is designated to receive complaints of discrimination based on this paragraph and coordinate the investigation of such complaints. ``(H) Actuarial equivalence.--Nothing in this paragraph shall prohibit the Secretary from issuing regulations or other guidance to ensure that health plans excluding specific items or services under this paragraph shall have an aggregate actuarial value at least equivalent to that of plans at the same level of coverage that do not exclude such items or services.''. (b) Effective Date.--The amendment made by subsection (a) shall be effective as if included in the enactment of Public Law 111-148.", "label": 1, "domain": "government", "token_count": 374, "matched_pair_id": "conditionality_00919", "split": "train"}
{"id": "conditionality_train_pos_0640", "text": "In a 2011 paper published in the journal \"Asian Journal of Algebra\"(see reference[1]), the authors consider, among other equations,the diophantine equations 2xy=n(x+y) and 3xy=n(x+y). For the first equation, with n being an odd positive integer, they give the solution x=(n+1)/2, y=n(n+1)/2. For the second equation they present the particular solution, x=(n+1)/3,y=n(n+1)/3, where is n is a positive integer congruent to 2modulo3. If in the above equations we assume n to be prime, then these two equations become special cases of the diophantine equation, nxy=p(x+y) (1), with p being a prime and n a positive integer greater than or equal to 2. This 2-variable symmetric diophantine equation is the subject matter of this article; with the added condition that the intager n is not divisible by the prime p. Observe that this equation can be written in fraction form: n/p= 1/x + 1/y(See [2] for more details) In this work we prove the following result, Theorem1(stated on page2 of this paper):Let p be a prime, n a positive integer at least2, and not divisible by p. Then, 1)If n=2 and p is an odd prime, equation (1) has exactly three distinct positive integer solutions:x=p, y=p ; x=p(p+1)/2, y=(p+1)/2 ; x=(p+1)/2, y=p(p+1)/2 2)If n is greater than or equal to 3, and n is a divisor of p+1. Then equation (1) has exactly two distinct solutions: x=p(p+1)/n, y=(p+1)/n ; x=(p+1)/n, y=p(p+1)/n 3) if n is not a divisor of p+1. Then equation (1) has no positive integer solution. The proof of this result is elementary, and only uses Euclid's Lemma from number theory,and basic divisor arguments(such that if a prime divides a product of two integers; it must divide at least one of them).", "label": 1, "domain": "academic", "token_count": 479, "matched_pair_id": "conditionality_00423", "split": "train"}
{"id": "conditionality_train_pos_0641", "text": "If the supermassive black hole (SMBH) at the center of our Galaxy grew adiabatically, then a dense \"spike\" of dark matter is expected to have formed around it. Assuming that dark matter is composed primarily of weakly interacting massive particles (WIMPs), a star orbiting close enough to the SMBH can capture WIMPs at an extremely high rate. The stellar luminosity due to annihilation of captured WIMPs in the stellar core may be comparable to or even exceed the luminosity of the star due to thermonuclear burning. The model thus predicts the existence of unusual stars, i.e. \"WIMP burners\", in the vicinity of an adiabatically grown SMBH. We find that the most efficient WIMP burners are stars with degenerate electron cores, e.g. white dwarfs (WD) or degenerate cores with envelopes. If found, such stars would provide evidence for the existence of particle dark matter and could possibly be used to establish its density profile. In our previous paper we computed the luminosity from WIMP burning for a range of dark matter spike density profiles, degenerate core masses, and distances from the SMBH. Here we compare our results with the observed stars closest to the Galactic center and find that they could be consistent with WIMP burners in the form of degenerate cores with envelopes. We also cross-check the WIMP burner hypothesis with the EGRET observed flux of gamma-rays from the Galactic center, which imposes a constraint on the dark matter spike density profile and annihilation cross-section. We find that the EGRET data is consistent with the WIMP burner hypothesis. New high precision measurements by GLAST will confirm or set stringent limits on a dark matter spike at the Galactic center, which will in turn support or set stringent limits on the existence of WIMP burners at the Galactic center.", "label": 1, "domain": "academic", "token_count": 382, "matched_pair_id": "conditionality_00003", "split": "train"}
{"id": "conditionality_train_pos_0642", "text": "assuming the obligation to repay, pursuant to subsection (c), a loan made, insured or guaranteed under this part or part D (excluding loans made under sections 428B and 428C) for any new borrower after October 1, 1994, who completes a degree in early childhood education and obtains full-time employment in a child care facility. ``(2) Award basis; priority.-- ``(A) Award basis.--Subject to subparagraph (B), loan repayment under this section shall be on a first- come, first-served basis and subject to the availability of appropriations. ``(B) Priority.--The Secretary shall give priority in providing loan repayment under this section for a fiscal year to student borrowers who received loan repayment under this section for the preceding fiscal year. ``(3) Regulations.--The Secretary is authorized to prescribe such regulations as may be necessary to carry out the provisions of this section. ``(c) Loan Repayment.-- ``(1) In general.--The Secretary shall assume the obligation to repay 15 percent of the total amount of all loans made after October 1, 1994, to a student under this part or part D for each complete year of employment described in subsection (b)(1). ``(2) Construction.--Nothing in this section shall be construed to authorize the refunding of any repayment of a loan made under this part or part D. ``(3) Interest.--If a portion of a loan is repaid by the Secretary under this section for any year, the proportionate amount of interest on such loan which accrues for such year shall be repaid by the Secretary. ``(4) Special rule.--In the case where a student borrower who is not participating in loan repayment pursuant to this section returns to an institution of higher education after graduation from an institution of higher education for the purpose of obtaining a degree in early childhood education, the Secretary is authorized to assume the obligation to repay the total amount of loans made under this part or part D incurred for a maximum of two academic years in returning to an institution of higher education for the purpose of obtaining a degree in early childhood education. Such loans shall only be repaid for borrowers who qualify for loan repayment pursuant to the provisions of this section, and shall be repaid in accordance with the provisions of paragraph (1). ``(5) Ineligibility of national service award recipients.-- No student borrower may, for the same volunteer service, receive a benefit under both this section and subtitle D of title I of the National and Community", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00929", "split": "train"}
{"id": "conditionality_train_pos_0643", "text": "The evolutionary stage of the delta Scuti star 44 Tau has been unclear. Recent asteroseismic studies have claimed models on the main sequence, as well as in the expansion phase of the post-main sequence evolution. However, these models could not reproduce all of the observed frequencies, the mode instability range, and the fundamental stellar parameters simultaneously. A recent photometric study has increased the number of detected independent modes in 44 Tau to 15, and a newly found gravity mode at 5.30 c/d extends the observed frequency range. Aims. One of the possible evolutionary stages of 44 Tau has not yet been considered: the overall contraction phase after the main sequence. We computed asteroseismic models to examine whether models in this evolutionary stage provide a better fit of the observed frequency spectrum. Methods. We used Dziembowski's pulsation code to compute nonadiabatic frequencies of radial and nonradial modes. Observation of two radial modes and an avoided crossing of dipole modes put strong constraints on the models. A two-parametric overshooting routine is utilized to determine the efficiency of element mixing in the overshoot layer above the convective core. Results. We find that pulsation models in the post-MS contraction phase successfully reproduce the observed frequency range, as well as the frequency values of all individual radial and nonradial modes. The theoretical frequencies of the mixed modes at 7.79 c/d and 9.58 c/d are in better agreement with the observations if efficient element mixing in a small overshoot layer is assumed.", "label": 1, "domain": "academic", "token_count": 313, "matched_pair_id": "conditionality_00176", "split": "train"}
{"id": "conditionality_train_pos_0644", "text": "Curt Schilling: I’d be in the Hall of Fame if I bashed Donald Trump The 2017 Baseball Hall of Fame inductees will be announced later this month, and Curt Schilling is once again expected to come up short. The former Cy Young Award winner is convinced that has much more to do with his political opinions than what he accomplished in his career. And he’s probably right. In an interview with TMZ this week, Schilling said he believes nearly all of the 400-plus voters would give him a thumbs up if he bashed Donald Trump rather than supporting the president elect. “They’re not hiding the fact that they’ve stopped voting for me because of the things I’ve said on social media,” the 50-year-old said. “That’s their prerogative as voters. … If I had said lynch Trump, I’d be getting in with about 90 percent of the votes this year.” A few months ago, Schilling shared a photo on social media of a man wearing a shirt encouraging people to lynch journalists and described it as “awesome.” Schilling added that many of the voters are hypocrites for keeping him out of the Hall because of his character, noting that there’s a tendency to “pick and choose” which players to apply the character clause to. “The people who have said they’re not going to vote for me are not going to vote for me because of the character clause,” he said. “There are some of the worst human beings I’ve ever known voting. There are scumbags all across — if they don’t believe my baseball talents merit me getting into the Hall of Fame, so be it.” Schilling is one of only 16 pitchers with 3,000-plus strikeouts in his career. His 216 wins are a bit low for some people, but he ranks third all-time in strikeout-to-walk ratio. The strongest case Schilling can make for Cooperstown is his 11-2 record and 2.23 ERA in the playoffs, where he was downright dominant. Are many voters keeping Schilling off their ballots because he has made unpopular remarks like this? Most likely, but he still has a few years to get in. It’d be a surprise if he doesn’t eventually get to the Hall.", "label": 1, "domain": "news", "token_count": 465, "matched_pair_id": "conditionality_00758", "split": "train"}
{"id": "conditionality_train_pos_0645", "text": "if the State program or other State entity authorized to make such determinations certifies to the Secretary, in accordance with the procedures established under subsection (b), that the State program complies with the following requirements: (1) State program design.--The State program is established and authorized by State law as an earthquake insurance program that offers residential property insurance coverage for insured losses to property, contents, and additional living expenses, and which is not a State program that requires insurers to pool resources to provide property insurance coverage for earthquakes. (2) Operation.--The State program shall meet the following requirements: (A) A majority of the members of the governing body of the State program shall be public officials or appointed by public officials. (B) The State shall have a financial interest in the State program. (C) If the State has at any time appropriated amounts from the State program's funds for any purpose other than payments for losses insured under the State program, or payments made in connection with any of the State program's authorized activities, the State shall have returned such amounts to the State fund, together with interest on such amounts. (3) Tax status.--The State program shall have received from the Secretary (or the Secretary's designee) a written determination, within the meaning of section 6110(b) of the Internal Revenue Code of 1986, that the State program either-- (A) constitutes an ``integral part'' of the State that has created it; or (B) is otherwise exempt from Federal income taxation. (4) Earnings.--The State program may not provide for any distribution of any part of any net profits of the State program to any insurer that participates in the State program. (5) Loss prevention and mitigation.-- (A) Mitigation of losses.--The State program shall include provisions designed to encourage and support programs to mitigate losses for which the State insurance program was established to provide insurance. (B) Operational requirements.--The State program shall operate in a State that-- (i) has in effect and enforces, or the appropriate local governments within the State have in effect and enforce, nationally recognized building, seismic-design, and safety codes and consensus-based standards; and (ii) has taken actions to establish an insurance rate structure that takes into account measures to mitigate insured losses. (6) Requirements regarding coverage.--The State program-- (A) may not, except for charges or assessments related to post-event financing or bonding, involve cross-subsidization", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00912", "split": "train"}
{"id": "conditionality_train_pos_0646", "text": "Assuming that the universe is homogenous and isotropic and applying Gauss' flux theorem for gravity, it follows that the gravitational field of the visible universe can be calculated as if the entire mass of the visible universe is located in one point. Taking into account that the mass of the visible universe is M=2x10^{53} kg, it appears that the entire visible universe is inside a {\\it photon sphere} of radius R_{ps} = 14.3 Gpc. The current model for the visible universe must be corrected to account for the fact that measured horizon distance of 14.0 \\pm 0.2 Gpc is not a straight line. Rather it is an arc of a circle with that length, because all photons are inside the photon sphere. Our model interprets the visible universe as a surface of a sphere (or an inside of a sphere shell) with radius 4.46 \\pm 0.06 Gpc and an event horizon, located on that sphere (shell), with size of 14.0 \\pm 0.2 Gpc. The model predicts CMB redshift and time dilatation of Type Ia supernovae by gravitation. It explains, without inflation theory, the isotropy and uniformity of the CMB. It predicts the correct value for the Hubble constant H_0 = 67.26 \\pm 0.90 km/s/Mpc, the cosmic expansion rate H(z) in agreement with observations, and the speed of the event horizon. Through relativistic energy correction, our model also provides an explanation for critical density without use of dark matter. It explains that Type Ia supernovae redshifts are not related to the accelerated expansion of the universe and dark energy. It explains the reason for the established discrepancy between the non-covariant version of the holographic principle and the calculated dimensionless entropy (S/k) for the visible universe, which exceeds the entropy of a black hole. The model is in agreement with the distribution of radio sources in space, Type Ia data, and data from the HUDF optical and near-infrared survey.", "label": 1, "domain": "academic", "token_count": 434, "matched_pair_id": "conditionality_00230", "split": "train"}
{"id": "conditionality_train_pos_0647", "text": "ALBUQUERQUE, NM (CNN) – A New Mexico woman has been taken to a mental hospital after a shocking find at her home. Authorities found her husband’s mummified body inside a bedroom closet. There’s now a sign on the garage of the Foothills home warning trespassers to keep out as the house is in foreclosure. When deputies showed up to evict the owners last month they were shocked at what they found “I never would have imagined that he would be laying in the closet into a mummified state,” said Thomas Huerta, the dead man’s son. Police found the body of Huerta’s father on a mattress in the closet, with a pillow propped under his head, and he was tucked in under blankets. The man’s wife told police he died in April of 2015, more than two years earlier. “I try not to think about it. It is very difficult,” said Huerta. Huerta says he is still trying to let the news sink in. He lives in California now, but visited Albuquerque last October to introduce his father to his pregnant girlfriend. “Not only she was in there, but so was his mummified corpse,” said Huerta. According to a report, neighbors noticed the man hadn’t been around, but when they asked his wife, she only told them he was preparing for the ministry. The woman told police her husband suffered from chronic back pain so he often slept in that closet. He had been coughing up bile, but refused to go the hospital. Tom tells me he never imagined his father’s life would end like this. “It is horrible to think that that was his destiny,” said Huerta. Authorities are now trying to determine how the man died. It’s unclear if the woman will face criminal charges.", "label": 1, "domain": "news", "token_count": 367, "matched_pair_id": "conditionality_00519", "split": "train"}
{"id": "conditionality_train_pos_0648", "text": "lights when you get home. Smart Cameras Canary is an all-in-one home security system trained to send intelligent alerts to a user's smartphone when it detects activity. You can also open your Canary app to see live video and audio of what's happening in your home at that moment and replay video clips. The all-in-one security system can even let you sound a 90+ decibel alarm if you see shady activity unfolding live on your app, hopefully scaring the thief away and alerting neighbors. One device starts at $169, with deals for multi-packs. Another option is the Nest Cam Indoor, which can be placed in an inconspicuous place in your home and record video that can be stored in the cloud for 30 days. If there's a suspicious sound in your home, Nest will also send an alert to your phone, so you're immediately in the know. It can also send \"person alerts,\" letting you see who's in your home. The indoor camera starts at $199, but there are deals if you buy multiple devices to cover more areas of your home. Where Did That Thing Go? If losing your favorite bag or coat is a worry, consider putting a Tile tracker in it. The tiny device pairs to your smartphone and will let you know where your item is, as long as the Tile is still inside of it. More often than not, it's likely your housekeeper moved that bag to vacuum and you'll find it somewhere in your house. If you're having trouble locating an item, you can also reach out to the customer service representatives from whichever platform you used. They can ask the service provider if they saw a specific item — and more often than not, quickly tell you where it is in your home.", "label": 1, "domain": "news", "token_count": 354, "matched_pair_id": "conditionality_00744", "split": "train"}
{"id": "conditionality_train_pos_0649", "text": "If Cristiano Ronaldo can teach us anything about fame, perhaps it’s that the more famous you get, the more haters you get. Ronaldo has revealed that even his son’s classmates are among the Real Madrid star’s critics and they tell Cristiano Jr. that there are better players than the four-time Ballon d’Or winner. “There are people who sometimes say to him that ‘there is another player who is better than your father,’ but he knows how to deal with that,” Ronaldo told ON TV in Egypt. “He is a smart boy, like me. I often tell him ‘be yourself and be polite,’” he added. “I know that he will go through periods of adversity as there are jealous people out there, but I see him as a happy child.” Ronaldo did not specify who his son’s classmates think is better. But, hmm, wonder who the other player could be? We can’t say for sure … but it’s definitely Lionel Messi. While Ronaldo’s son for now must defend his father’s honor at the school yard, the Portuguese also said he wouldn’t mind if his son followed in his footsteps and carried on his legacy as an attacking player — but he won’t pressure him too much. “Of course I would like it if he became a footballer,” he admitted. “I know that it is a challenge and that it isn’t easy, but he can be whatever he wants to be as I won’t pressure him.” “I might be pushing him a little in the direction of becoming a footballer,” he added, “but not to be a goalkeeper as I want him to be a forward.” Let the bids for Cristiano Jr.’s 2028 rights begin. MORE FROM FOX SOCCER", "label": 1, "domain": "news", "token_count": 350, "matched_pair_id": "conditionality_00734", "split": "train"}
{"id": "conditionality_train_pos_0650", "text": "Recently Shukurov et al [Phys Rev \\textbf{E} (2008)] presented a numerical solution of a Moebius strip dynamo flow, to investigate its use in modelling dynamo flows in Perm torus of liquid sodium dynamo experiments. Here, by analogy one presents an electric dynamo on a twisted torus or Klein bottle topology. An exact solution in the form of flat Klein bottle dynamo flow is obtained. It is shown that even in the absence of magnetic dynamos initial electric fields can be amplified in distinct points of the Klein bottle. In this case diffusion is taken as ${\\eta}\\approx{5.0{\\times}10^{-3}{\\Omega}-m}$ the electric potential is obtained. The difference of electric fields at the beginning of plasma flow profile is ${\\Delta}E_{Dyn}\\approx{468\\frac{V}{m}}$, which is stronger than the electric dynamo field obtained in the magnetic axis of spheromaks, which is of the order of $E_{Dyn}\\approx{200\\frac{V}{m}}$. The potential of the dynamo at the surface of the Earth computed by Boozer [Phys Fluids \\textbf{B} (1993)] of ${\\Phi}\\approx{160V}$, is used to obtain the magnetic vector constant $A_{0}\\approx{10^{6}V}$. In general the associated magnetic dynamo is shown to be a fast dynamo in force-free plasmas in Klein bottle. Of course if the magnetic dynamo growth is turned on the electric dynamo shall be able to sustain itself along the Klein bottle.", "label": 1, "domain": "academic", "token_count": 338, "matched_pair_id": "conditionality_00178", "split": "train"}
{"id": "conditionality_train_pos_0651", "text": "Binary radio pulsars are generally believed to have been spun up to millisecond periods (i.e. recycling) via mass accretion from their donor stars, and they are the descendants of neutron star low-mass X-ray binaries. However, some studies indicate that the formation of pulsars from the accretion-induced collapse (AIC) of accreting white dwarfs (WDs) cannot be excluded. In this work, we use a population synthesis code to examine if the AIC channel can produce eccentric binary millisecond pulsars (BMSPs) in the Galaxy. Our simulated results indicate that, only when the natal MSPs receive a relatively strong kick ($\\ga100\\rm km\\,s^{-1}$), can the AIC channel produce $\\sim 10-180$ eccentric ($e>0.1$) BMSPs in the Galaxy, most of which are accompanied by a Helium star. Such a kick seems to be highly unlikely in the conventional AIC process, hence the probability of forming eccentric BMSPs via the AIC channel can be ruled out. Even if a high kick is allowed, the AIC channel cannot produce eccentric BMSPs with an orbital period of $\\ga 20$ days. Therefore, we propose that the peculiar BMSP PSR J1903+0327 cannot be formed by the AIC channel. However, the AIC evolutionary channel may produce some fraction of isolated millisecond pulsars, and even sub-millisecond pulsars if they really exist.", "label": 1, "domain": "academic", "token_count": 310, "matched_pair_id": "conditionality_00255", "split": "train"}
{"id": "conditionality_train_pos_0652", "text": "receiving a grant under this subsection, each grant recipient shall agree to cooperate in an evaluation by the Secretary of the program carried out using grant funds. ``(7) Technical assistance.--The Secretary shall provide technical assistance and information to assist eligible schools, State and local agencies, Indian tribal organizations, and nonprofit entities-- ``(A) to facilitate the coordination and sharing of information and resources in the Department that may be applicable to the farm to school program; ``(B) to collect and share information on best practices; and ``(C) to disseminate research and data on existing farm to school programs and the potential for programs in underserved areas. ``(8) Funding.-- ``(A) In general.--On October 1, 2010, out of any funds in the Treasury not otherwise appropriated, the Secretary of the Treasury shall transfer to the Secretary to carry out this subsection $50,000,000, to remain available until expended. ``(B) Receipt and acceptance.--The Secretary shall be entitled to receive, shall accept, and shall use to carry out this subsection the funds transferred under subparagraph (A), without further appropriation. ``(h) Pilot Program for High-Poverty Schools.-- ``(1) In general.--''; and (3) in subsection (h) (as redesignated by paragraph (2))-- (A) in subparagraph (F) of paragraph (1) (as so redesignated), by striking ``in accordance with paragraph (1)(H)'' and inserting ``carried out by the Secretary''; and (B) by redesignating paragraph (4) as paragraph (2). SEC. 3. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the House Budget Committee, provided that such statement has been submitted prior to the vote on passage.", "label": 1, "domain": "government", "token_count": 417, "matched_pair_id": "conditionality_01039", "split": "train"}
{"id": "conditionality_train_pos_0653", "text": "If the Higgs does not propagate into an otherwise universal extra dimension, then tree-level Kaluza-Klein number is not conserved in the Yukawa interactions. This leads to mixing between zero-mode fermions and their associated Kaluza-Klein excitations. The effect can be quite large for the top quark, since its mass (171.4 plus or minus 2.1 GeV) is approximately one-half the current Tevatron mass bound (about 350-400 GeV) for Kaluza-Klein excitations of quarks with one universal extra dimension. In contrast to the SM, the bi-unitary transformation that diagonalizes the mass matrix does not diagonalize the effective 4D Yukawa coupling matrix because of the presence of the 5D kinetic terms. This leads to violation of tree-level Kaluza-Klein number conservation in the gauge sector due to a unique feature of the 5D theory. This allows Kaluza-Klein excitations of the fermions to be produced singly, and opens up new decay channels in the gauge sector. We compute the cross section for the production of the lowest-lying Kaluza-Klein excitations of the top and bottom quarks in the non-universal Higgs model at the Large Hadron Collider, and consider their subsequent decays. The effect is quite large: For example, pair production of Kaluza-Klein excitations of the bottom quark will lead to a pair of top quarks plus a pair of charged weak gauge bosons. Since the production is via the strong interaction, such final states stand out well against the Standard Model background, and are observable at the LHC for a wide range of compactification scales. Finally, we discuss the effects that such a model has on the T- parameter, and propose a model with maximal mixing where the compactification scale may be as large as a universal extra dimension.", "label": 1, "domain": "academic", "token_count": 388, "matched_pair_id": "conditionality_00016", "split": "train"}
{"id": "conditionality_train_pos_0654", "text": "Fight fans watching this one might be better served looking PAST this match-up. Ramirez is getting a chance, with this ESPN exposure for an expected highlight reel performance, to put his name at the very top of the division… Jose Ramirez (22-0, 16 KOs) makes the first defense of his WBC junior welterweight title this Saturday against Danny O’Connor (30-3, 11 KOs) at the Save Mart Center in Fresno, California (broadcast live on ESPN and ESPN Deportes at 10:30 p.m. ET)—and it probably won’t be the least bit competitive. Fight fans watching this one might be better served looking PAST this match-up while tuning in. The 140 lb. division is quickly and quietly becoming packed with top tier talent and it’ll be interesting to see how bright Ramirez’s star shines when given the opportunity to slam through a relative “gimme” of a defense. Awaiting Ramirez at 140 are mega-talents Regis Prograis and Josh Taylor, as well as tough, top-tier opposition like Kiryl Relikh, Maurice Hooker, Terry Flanagan, Antonio Orozco, Alex Saucedo, Sergey Lipinets, Viktor Postol, and Ivan Baranchyk (among others). Ramirez is getting a chance, with this ESPN exposure for an expected highlight reel performance, to put his name at the very top of the division when it comes to asking price and negotiating leverage. The popular Fresno-area attraction and 2012 US Olympian is an ultra-confident and tenacious pressure fighter whose best weapons are a dogged body attack and a solid overhand right. Not gifted with truly heavy hands or with elite-level athleticism, there’s reason to believe that Ramirez may falter when stacked up against an opponent gifted with high-end speed and reflexes. In his March contest with Amir Imam for the vacant title, Ramirez outworked and out-pointed his foe, but clearly struggled to walk his way into range against the quicker, more mobile opponent. The 25-year-old’s flimsy résume and relative lack of pro seasoning certainly don’t help in this area, nor did a long-time association with trainer Freddie Roach (who has since been replaced by Robert Garcia). Ramirez’s ability to will his way past opposition and simply outwork them won’t likely carry him too far into increasingly deep divisional waters if he doesn’t make some essential tweaks to his game.", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00586", "split": "train"}
{"id": "conditionality_train_pos_0655", "text": "We report a photometric and spectroscopic study of the peculiar cataclysmic variable SDSS 1507+52. The star shows very deep eclipses on the 67 minute orbital period, and those eclipses are easily separable into white-dwarf and hot-spot components. This leads to tight constraints on binary parameters, with M_1=0.83(8) solar masses, M_2=0.057(8) solar masses, R_1=0.0097(9) solar radii, R_2=0.097(4) solar radii, q=0.069(2), and i=83.18(13) degrees. Such numbers suggest possible membership among the WZ Sge stars, a common type of dwarf nova. The spectroscopic behavior (strong and broad H emission, double-peaked and showing a classic rotational disturbance during eclipse) is also typical. But the star's orbital period is shockingly below the \"period minimum\" of approximately 77 min which is characteristic of hydrogen-rich CVs; producing such a strange binary will require some tinkering with the theory of cataclysmic-variable evolution. The proper motion is also remarkably high for a star of its distance, which we estimate from photometry and trigonometric parallax as 230 +- 40 pc. This suggests a transverse velocity of 164 +- 30 km/s - uncomfortably high if the star belongs to a Galactic-disk population. These difficulties with understanding its evolution and space velocity can be solved if the star belongs to a Galactic-halo population.", "label": 1, "domain": "academic", "token_count": 324, "matched_pair_id": "conditionality_00052", "split": "train"}
{"id": "conditionality_train_pos_0656", "text": "if we tried to modify the environment,\" she said. \"Geese like very flat green grass so if you start to plant spiky grass its not as hospitable for them. \"More experimentally in America, they are starting to use drones to try and scare the geese away. \"It's about balancing the very real health and safety risk with animal welfare and I really think that if we try to prevent the geese from landing here, rather than destroying their eggs, it will be much better. \"It's very important that people who use the park know that this is going on so that they can voice their opinions on it.\" Image caption Greylag geese can often be seen on the grass beside the water in Victoria Park Belfast City Airport has held a licence to carry out egg pricking since 2002. In a freedom of information request the Northern Ireland environment agency revealed that since 2002, 1,775 greylag goose eggs have been oiled and pricked. The numbers involved vary each year, ranging from fewer than 50 to more than 250. In recent years, an average of 100 eggs have been pricked. Hazardous wildlife A spokesman for the airport said: \"In order to control the feral geese population in Victoria Park, the oiling and pricking of eggs is undertaken by a biologist under licence from the Northern Ireland Environment Agency and with the permission of Belfast City Council. \"The airport has a legal obligation to reduce the number of hazardous wildlife in the vicinity of the airport and does this through consultation with local authorities and wildlife experts. \"Earlier this year, Belfast City Airport was named Northern Ireland's Responsible Company of the Year by Business in the Community and, like all airports, is committed to managing its operations in an environmentally sensitive manner whilst ensuring air safety.\" Image caption Planes regularly fly over Victoria Park and the geese throughout the day A spokesperson for the council said: \"Public health and safety is paramount to Belfast City Council. \"Due to concerns over the number of greylag geese in Victoria Park, and their potential threat to landing or taking off aircrafts at George Best Belfast City Airport, Belfast City Council has an agreement with the airport granting them access to Victoria Park to carryout egg pricking.\"", "label": 1, "domain": "news", "token_count": 460, "matched_pair_id": "conditionality_00798", "split": "train"}
{"id": "conditionality_train_pos_0657", "text": "KANSAS CITY, Mo. — Brett Veach has made so many manoeuvrs involving draft picks since taking over as the Kansas City Chiefs' general manager that it's hard to believe he's never led an actual draft. That changes this week. The young front office boss, who took over when John Dorsey was let go last summer, heads into the three-day draft Thursday without a first-round pick. But Veach has one in the second round and two more in the third, giving him ample opportunity to shore up a leaky defence on an otherwise deep roster. \"I am looking forward to it. I've been working up to it, been doing this for 12 years,\" he said last week. \"I've been going to the draft room for a long time. Certainly, it will be different as a GM. I am surrounded by a lot of great people and trust those guys.\" The Chiefs clearly trust him. Dorsey did a good job of acquiring talent after taking over a 2-14 franchise, but his inability to manage the salary cap ultimately led to his ouster. Veach has quickly balanced the books, using draft choices to help the process. He sent a fourth-round pick next year to Buffalo to grab middle linebacker Reggie Ragland, who started right away last season, and a fifth-rounder this year to Cleveland for swing offensive tackle Cam Erving. Then, he dealt quarterback Alex Smith to Washington for cornerback Kendall Fuller and a third-round pick this year, and cornerback Marcus Peters and a sixth-round pick this year to the Los Angeles Rams for a fourth-round pick this year and a second-round selection next season. Got all that? The upshot is that, while nobody is quite sure what Veach will do when he runs his own draft, the safe assumption is that he will move aggressively to nab a player he likes. \"That's just kind of who I am. I have a group of guys up there who are worried that I'm going to be too aggressive,\" he said, \"so I'm glad I have those guys. Everyone does this, and we've done this the last five years, you go through mock drafts just like you see online. We kind of just play that game ourselves in regards to what do we do if, or what about if this guy slides.", "label": 1, "domain": "news", "token_count": 470, "matched_pair_id": "conditionality_00597", "split": "train"}
{"id": "conditionality_train_pos_0658", "text": "Understanding space usage and resource selection is a primary focus of many studies of animal populations. Usually, such studies are based on location data obtained from telemetry, and resource selection functions (RSF) are used for inference. Another important focus of wildlife research is estimation and modeling population size and density. Recently developed spatial capture-recapture (SCR) models accomplish this objective using individual encounter history data with auxiliary spatial information on location of capture. SCR models include encounter probability functions that are intuitively related to RSFs, but to date, no one has extended SCR models to allow for explicit inference about space usage and resource selection. We develop a statistical framework for jointly modeling space usage, resource selection, and population density by integrating SCR data, such as from camera traps, mist-nets, or conventional catch-traps, with resource selection data from telemetered individuals. We provide a framework for estimation based on marginal likelihood, wherein we estimate simultaneously the parameters of the SCR and RSF models. Our method leads to increases in precision for estimating population density and parameters of ordinary SCR models. Importantly, we also find that SCR models alone can estimate parameters of resource selection functions and, as such, SCR methods can be used as the sole source for studying space-usage; however, precision will be higher when telemetry data are available. Finally, we find that SCR models using standard symmetric and stationary encounter probability models produce biased estimates of density when animal space usage is related to a landscape covariate. Therefore, it is important that space usage be taken into consideration, if possible, in studies focused on estimating density using capture-recapture methods.", "label": 1, "domain": "academic", "token_count": 323, "matched_pair_id": "conditionality_00479", "split": "train"}
{"id": "conditionality_train_pos_0659", "text": "Based on the intensity and rates of various kinds of intense ionizing radiation events such as supernovae and gamma-ray bursts, it is likely that the Earth has been subjected to one or extinction level events during the Phanerozoic. These induce changes in atmospheric chemistry so that the level of Solar ultraviolet-B radiation reaching the surface and near-surface waters may be doubled for up to a decade. This UVB level is known from experiment to be more than enough to kill off many kinds of organisms, particularly phytoplankton. It could easily induce a crash of the photosynthetic-based food chain in the oceans. Regularities in the latitudinal distribution of damage are apparent in simulations of the atmospheric changes. We previously proposed that the late Ordovician extinction is a plausible candidate for a contribution from an ionizing radiation event, based on environmental selectivity in trilobites. To test a null hypothesis based on this proposal, we confront latitudinal differential extinction rates predicted from the simulations with data from a published analysis of latitudinal gradients in the Ordovician extinction. The pattern of UVB damage always shows a strong maximum at some latitude, with substantially lower intensity to the north and south of this maximum. We find that the pattern of damage predicted from our simulations is consistent with the data assuming a burst approximately over the South Pole, and no further north than -75 degrees. We predict that any land mass (such as parts of north China, Laurentia, and New Guinea) which then lay north of the equator should be a refuge from UVB effects, and show a different pattern of extinction in the first strike of the end-Ordovician extinction, if induced by such a radiation event.", "label": 1, "domain": "academic", "token_count": 348, "matched_pair_id": "conditionality_00078", "split": "train"}
{"id": "conditionality_train_pos_0660", "text": "A celebrated result of Chv\\'atal, R\\\"odl, Szemer\\'edi and Trotter states (in slightly weakened form) that, for every natural number $\\Delta$, there is a constant $r_\\Delta$ such that, for any connected $n$-vertex graph $G$ with maximum degree $\\Delta$, the Ramsey number $R(G,G)$ is at most $r_\\Delta n$, provided $n$ is sufficiently large. In 1987, Burr made a strong conjecture implying that one may take $r_\\Delta = \\Delta$. However, Graham, R\\\"odl and Ruci\\'nski showed, by taking $G$ to be a suitable expander graph, that necessarily $r_\\Delta > 2^{c\\Delta}$ for some constant $c>0$. We show that the use of expanders is essential: if we impose the additional restriction that the bandwidth of $G$ be at most some function $\\beta (n) = o(n)$, then $R(G,G) \\le (2\\chi(G)+4)n\\leq (2\\Delta+6)n$, i.e., $r_\\Delta = 2\\Delta +6$ suffices. On the other hand, we show that Burr's conjecture itself fails even for $P_n^k$, the $k$th power of a path $P_n$. Brandt showed that for any $c$, if $\\Delta$ is sufficiently large, there are connected $n$-vertex graphs $G$ with $\\Delta(G)\\leq\\Delta$ but $R(G,K_3)>cn$. We show that, given $\\Delta$ and $H$, there are $\\beta>0$ and $n_0$ such that, if $G$ is a connected graph on $n\\ge n_0$ vertices with maximum degree at most $\\Delta$ and bandwidth at most $\\beta n$, then we have $R(G,H)=(\\chi(H)-1)(n-1)+\\sigma(H)$, where $\\sigma(H)$ is the smallest size of any part in any $\\chi(H)$-partition of $H$. We also show that the same conclusion holds without any restriction on the maximum degree of $G$ if the bandwidth of $G$ is at most $\\epsilon(H) \\log n/\\log\\log n$.", "label": 1, "domain": "academic", "token_count": 486, "matched_pair_id": "conditionality_00269", "split": "train"}
{"id": "conditionality_train_pos_0661", "text": "and Records.--All books and records of the corporation may be inspected by any member having the right to vote in any proceeding of the corporation, or by any agent or attorney of such member, for any proper purpose at any reasonable time. (d) Application of State Law.--This section may not be construed to contravene any applicable State law. SEC. 11. AUDIT OF FINANCIAL TRANSACTIONS. The first section of the Act entitled ``An Act to provide for audit of accounts of private corporations established under Federal law'', approved August 30, 1964 (36 U.S.C. 1101), is amended by adding at the end the following: ``VietNow.''. SEC. 12. ANNUAL REPORT. The corporation shall annually submit to the Congress a report concerning the activities of the corporation during the preceding fiscal year. The annual report shall be submitted on the same date as the report of the audit required by section 11. The annual report may not be printed as a public document. SEC. 13. DEFINITIONS. For purposes of this Act: (1) The term ``corporation'' means VietNow. (2) The term ``State'' means each of the several States, the District of Columbia, the Commonwealth of Puerto Rico, the Commonwealth of the Northern Mariana Islands, the Virgin Islands, Guam, American Samoa, the Trust Territories of the Pacific Islands, and any other territory or possession of the United States. SEC. 134. TAX-EXEMPT STATUS. The corporation shall maintain its status as an organization exempt from taxation as provided in the Internal Revenue Code of 1986. SEC. 15. TERMINATION. The charter granted in this Act shall expire if the corporation fails to comply with any of the provisions of this Act.", "label": 1, "domain": "government", "token_count": 366, "matched_pair_id": "conditionality_00930", "split": "train"}
{"id": "conditionality_train_pos_0662", "text": ") In this subsection: ``(A) The term `child' means an individual who has not attained 18 years of age. ``(B) The term `adult' means an individual who has attained 18 years of age.''. (b) Penalties.--Section 924(a) of such title is amended by adding at the end the following: ``(7) Whoever violates section 922(bb) in a State shall be punished in accordance with the laws of the State that apply to persons convicted of child abandonment.''. SEC. 7. GRANTS FOR GUN SAFETY EDUCATION PROGRAMS. (a) Program Authority.--The Attorney General is authorized to provide grants to units of local government to enable law enforcement agencies to develop and sponsor gun safety classes for parents and their children. (b) Application.-- (1) In general.--Any unit of local government that desires to receive a grant award under this section shall submit an application to the Attorney General at such time, in such manner and containing such information as the Attorney General may reasonably require. (2) Contents.--Each application referred to in paragraph (1) shall include an assurance that-- (A) funds received under this section shall be used only to provide funds to law enforcement agencies to provide gun safety classes; and (B) gun safety classes will be offered at times convenient to parents, including evenings and weekends. (c) Regulations.--The Attorney General shall issue any regulations necessary to carry out this section. SEC. 8. EDUCATION: NATIONWIDE FIREARMS SAFETY PROGRAMS. It is the sense of Congress that-- (1) each school district should provide or participate in a firearms safety program for students in grades kindergarten through 12 and should consult with a certified firearms instructor before establishing the curriculum for the program; and (2) participation by students in a firearms safety program should not be mandatory if the district receives written notice from a parent of the student to exempt the student from the program.", "label": 1, "domain": "government", "token_count": 400, "matched_pair_id": "conditionality_00942", "split": "train"}
{"id": "conditionality_train_pos_0663", "text": "As part of a JCMT Legacy Survey of star formation in the Gould Belt, we present early science results for Taurus. CO J=3-2 maps have been secured along the north-west ridge and bowl, collectively known as L 1495, along with deep 13CO and C18O J=3-2 maps in two sub-regions. With these data we search for molecular outflows, and use the distribution of flows, HH objects and shocked H2 line emission features, together with the population of young stars, protostellar cores and starless condensations to map star formation across this extensive region. In total 21 outflows are identified. It is clear that the bowl is more evolved than the ridge, harbouring a greater population of T Tauri stars and a more diffuse, more turbulent ambient medium. By comparison, the ridge contains a much younger, less widely distributed population of protostars which, in turn, is associated with a greater number of molecular outflows. We estimate the ratio of the numbers of prestellar to protostellar cores in L 1495 to be ~ 1.3-2.3, and of gravitationally unbound starless cores to (gravitationally bound) prestellar cores to be ~ 1. If we take previous estimates of the protostellar lifetime of ~ 5 x 10^5 yrs, this indicates a prestellar lifetime of 9(+/-3) x 10^5 yrs. From the number of outflows we also crudely estimate the star formation efficiency in L 1495, finding it to be compatible with a canonical value of 10-15 %. We note that molecular outflow-driving sources have redder near-IR colours than their HH jet-driving counterparts. We also find that the smaller, denser cores are associated with the more massive outflows, as one might expect if mass build-up in the flow increases with the collapse and contraction of the protostellar envelope.", "label": 1, "domain": "academic", "token_count": 405, "matched_pair_id": "conditionality_00197", "split": "train"}
{"id": "conditionality_train_pos_0664", "text": "program, including-- (A) developing and disseminating an online survey instrument (designed to establish baseline data, including data on need for services) to veterans attending the institutions of higher education described in paragraph (1) of this subsection; (B) developing and disseminating (not earlier than 18 months after the start of the pilot program) a follow-up online survey instrument (designed to gather data, including data to assess engagement with peer- support, experience accessing services, and adjustment to higher education) other on the possible impact of the program); and (C) tabulating-- (i) the number of veterans who meet on an individual basis with such peer; (ii) the number of referrals such individual makes; and (iii) the outcome of such referrals. (d) Duration.-- The authority of the Secretary to provide services under the pilot program under this section shall terminate on the later of the following dates: (1) The date that is three years after the date of the commencement of the pilot program. (2) The date of the last day of the academic year that ends not more than 180 days after the date that is three years after the date of the commencement of the pilot program. (e) Report.--Not later than nine months after the completion of the pilot program under this section, the Secretary shall submit to the Committees on Veterans' Affairs of the Senate and the House of Representatives a report on the pilot program. The report shall include the following: (1) A description of the implementation and operation of the program. (2) An evaluation of effectiveness of then peer-outreach services provided under the program in-- (A) reducing the prevalence of veterans failing to continue higher education pursuits using their entitlement to educational assistance under chapter 33 of title 38, United States Code; (B) improving other outcomes related to higher education for veterans using such entitlement; and (C) the use by such veterans of needed behavioral health and other services. (3) An analysis of the costs and benefits of the program. (4) The Secretary's recommendations, if any, regarding an extension or expansion of the program.", "label": 1, "domain": "government", "token_count": 433, "matched_pair_id": "conditionality_00868", "split": "train"}
{"id": "conditionality_train_pos_0665", "text": "We present constraints on the values of $\\Omega_m$, $n$, $\\sigma_8$, obtained from measurements of the X-ray luminosity function of galaxy clusters as compiled in EMSS, RDCS and BCS galaxy cluster samples. The values obtained $\\Omega_m=0.25^{+0.15}_{-0.05}$, $n=-1^{+0.05}_{-0.05}$, and $\\sigma_8=0.8^{+0.1}_{-0.1}$ are in agreement with WMAP data. We then put constraints on the quoted parameters and the dark-energy equation-of-state parameter, $w$, using Chandra observations of 37 clusters with $<z>$=0.55 derived from 400 deg$^2$ ROSAT serendipitous survey and 49 brightest $z \\simeq 0.05$ clusters detected in the All-Sky Survey. In the case of $\\Lambda$CDM model, we get $\\Omega_m=0.25^{+0.1}_{-0.08}$ and $\\sigma_8=0.75^{+0.08}_{-0.05}$, while in the case of the $w$CDM model, we get $\\Omega_m=0.28^{+0.10}_{-0.10}$, $w=-1.25^{+0.30}_{-0.35}$, and $\\sigma_8=0.8^{+0.09}_{-0.09}$. Our results are consistent with those from recent analyses of type Ia supernovae, cosmic microwave background anisotropies, the X-ray gas mass fraction of relaxed galaxy clusters, baryon acoustic oscillations and cosmic shear. The improvement in data quality from EMSS, RDCS, and BCS to Chandra observations leads to an improvement in the constraints even if not of the same entity of the improvement in data.", "label": 1, "domain": "academic", "token_count": 403, "matched_pair_id": "conditionality_00149", "split": "train"}
{"id": "conditionality_train_pos_0666", "text": "the amendments made by such subtitles) shall not apply until the date on which the last of the collective bargaining agreements relating to the coverage terminates. Any coverage amendment made pursuant to a collective bargaining agreement relating to the coverage which amends the coverage solely to conform to any requirement added by this subtitle or subtitle A (or amendments) shall not be treated as a termination of such collective bargaining agreement. ``(e) Definition.--In this title, the term `grandfathered health plan' means any group health plan or health insurance coverage to which this section applies.''. (b) Effective Date.--The amendment made by subsection (a) shall take effect as if included in the Patient Protection and Affordable Care Act (Public Law 111-148). SEC. 6. ESSENTIAL HEALTH BENEFITS. (a) In General.--Subsections (a) and (b) of section 1302 of the Patient Protection and Affordable Care Act (42 U.S.C. 18022) are amended to read as follows: ``(a) Essential Health Benefits Package.--In this title, the term `essential health benefits package' means, with respect to any health plan, coverage that provide for benefits and cost sharing as required in the States in which such plan is offered. ``(b) Essential Health Benefits.--Essential health benefits shall be defined to include those required by the State in which a health plan is offered.''. (b) Effective Date.--The amendment made by subsection (a) shall take effect as if included in the Patient Protection and Affordable Care Act (Public Law 111-148).", "label": 1, "domain": "government", "token_count": 320, "matched_pair_id": "conditionality_01023", "split": "train"}
{"id": "conditionality_train_pos_0667", "text": "if the work is to be performed there. ``(2) For purposes of this section, the term `helper' means a semi- skilled worker (rather than a skilled journeyman mechanic) who-- ``(A) works under the direction of and assists a journeyman, ``(B) under the direction and supervision of the journeyman, performs a variety of duties to assist the journeyman, such as-- ``(i) preparing, carrying, and furnishing materials, tools, equipment, and supplies and maintaining them in order, ``(ii) cleaning and preparing work areas, ``(iii) lifting, positioning, and holding materials or tools, and ``(iv) other related semi-skilled tasks as directed by the journeyman, and ``(C) may use tools of the trade which are under the direction and supervision of the journeyman.''. SEC. 7. PROHIBITION ON CONTRACT-SPLITTING. Section 1 (40 U.S.C. 276a) (as amended by section 6) is further amended by adding at the end thereof the following new subsections: ``(d) Any person entering into a contract under which wages are to be determined in accordance with this Act shall not divide any project into contracts of $500,000 or less if the project would not have been so divided but for the purpose of avoiding the application of this Act. ``(e) Whenever the Secretary of Labor determines that a division for such purpose as described in subsection (d) has occurred, the Secretary may-- ``(1) require that the contracts, grants, or other instruments providing Federal financing or assistance be amended so as to incorporate retroactively all the provisions which would have been required under this Act or other applicable prevailing wage statute, and ``(2) require the contracting or assisting agency, the recipient of Federal financing or assistance, or any other entity which awarded the contract or instrument providing Federal financing or assistance in violation of this section, to compensate the contractor, the grantee, or other recipient of Federal assistance, as appropriate, for payment to each affected laborer, mechanic, and helper, of an amount equal to the difference between the rate received and the applicable prevailing wage rate, with interest on wages due at the rate specified in section 6621(c) of the Internal Revenue Code of 1986, from the date the work was performed by such laborers, mechanics, and helpers. ``(f) The Secretary shall make a determination that a division for such purpose as described in subsection (", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00965", "split": "train"}
{"id": "conditionality_train_pos_0668", "text": "The cost of the state's newborn health screening would nearly triple under a budget provision aimed at expanding the number of health conditions included in the screening. The fee would increase from $44 to $128 to cover the equipment and personnel costs of the expanded screening. \"We're pretty excited about this provision being in there and what the implications are,\" said Rep. Nelson Dollar, a Wake County Republican, adding that the fee is covered by insurance or Medicaid for most families. \"The sooner you can treat this babies, the better their health outcomes are going to be.\" But the provision, in a state spending plan released Monday and scheduled for votes this week, drew criticism from Gov. Roy Cooper's administration. SIGN UP Help us deliver journalism that makes a difference in our community. Our journalism takes a lot of time, effort, and hard work to produce. If you read and enjoy our journalism, please consider subscribing today. SUBSCRIBE TODAY \"Republicans tripling a birth tax on new mothers while giving more tax breaks to corporations and those earning more than $200,000 per year epitomizes the priorities we need to change,\" Ford Porter, a spokesman for the Democratic governor, said in an email. Republicans aren't allowing changes to the budget, so the fee is likely to become law. During a committee hearing, Rep. Carla Cunningham, a Mecklenburg County Democrat, questioned whether parents could opt out of the new elements of the screening and pay a lower fee. \"The screening panel is not like a cafeteria style,\" replied Rep. Greg Murphy, a Pitt County Republican and the legislature's only doctor. The new conditions being added to the screening are Pompe disease, Mucopolysaccharidosis Type I (MPS I), and X-Linked Adrenoleukodystrophy (X-ALD). Murphy noted that Duke University has developed a cure for Pompe disease, but doctors have to catch it early. \"Yes, it costs more, but in the long run it'll save lives,\" Murphy said of the increased fee. The provision allows the Department of Health and Human Services to expand the conditions tested in the future to match a federal list, with the ability to increase fees to cover future additions to the testing cost. Parents are allowed to opt out of the screening if they file a written request with their doctor.", "label": 1, "domain": "news", "token_count": 469, "matched_pair_id": "conditionality_00783", "split": "train"}
{"id": "conditionality_train_pos_0669", "text": "if any, under existing law for the cleanup of hazardous or solid wastes on the property, nor shall the United States or Shishmaref Native Corporation become liable for the cleanup of the property solely by virtue of acquiring title from the State or from the United States. SEC. 9. PURCHASE OF SETTLEMENT COMMON STOCK OF COOK INLET REGION. (a) In General.--Section 7(h) of the Alaska Native Claims Settlement Act (43 U.S.C. 1606(h)) is amended by adding at the end the following new paragraph: ``(4)(A) As used in this paragraph, the term `Cook Inlet Regional Corporation' means Cook Inlet Region, Incorporated. ``(B) The Cook Inlet Regional Corporation may, by an amendment to its articles of incorporation made in accordance with the voting standards under section 36(d)(1), purchase Settlement Common Stock of the Cook Inlet Regional Corporation and all rights associated with the stock from the shareholders of Cook Inlet Regional Corporation in accordance with any provisions included in the amendment that relate to the terms, procedures, number of offers to purchase, and timing of offers to purchase. ``(C) Subject to subparagraph (D), and notwithstanding paragraph (1)(B), the shareholders of Cook Inlet Regional Corporation may, in accordance with an amendment made pursuant to subparagraph (B), sell the Settlement Common Stock of the Cook Inlet Regional Corporation to itself. ``(D) No sale or purchase may be made pursuant to this paragraph without the prior approval of the board of directors of Cook Inlet Regional Corporation. Except as provided in subparagraph (E), each sale and purchase made under this paragraph shall be made pursuant to an offer made on the same terms to all holders of Settlement Common Stock of the Cook Inlet Regional Corporation. ``(E) To recognize the different rights that accrue to any class or series of shares of Settlement Common Stock owned by stockholders who are not residents of a Native village (referred to in this paragraph as `non-village shares'), an amendment made pursuant to subparagraph (B) shall authorize the board of directors (at the option of the board) to offer to purchase-- ``(i) the non-village shares, including the right to share in distributions made to shareholders pursuant to subsections (j) and (m) (referred to in this paragraph as `nonresident distribution rights'), at a price that includes a premium, in addition to the amount that is offered for the purchase of", "label": 1, "domain": "government", "token_count": 500, "matched_pair_id": "conditionality_00973", "split": "train"}
{"id": "conditionality_train_pos_0670", "text": "The study of the interplay between the testability of properties of Boolean functions and the invariances acting on their domain which preserve the property was initiated by Kaufman and Sudan (STOC 2008). Invariance with respect to F_2-linear transformations is arguably the most common symmetry exhibited by natural properties of Boolean functions on the hypercube. Hence, an important goal in Property Testing is to describe necessary and sufficient conditions for the testability of linear-invariant properties. This direction was explicitly proposed for investigation in a recent survey of Sudan. We obtain the following results: 1. We show that every linear-invariant property that can be characterized by forbidding induced solutions to a (possibly infinite) set of linear equations can be tested with one-sided error. 2. We show that every linear-invariant property that can be tested with one-sided error can be characterized by forbidding induced solutions to a (possibly infinite) set of systems of linear equations. We conjecture that our result from item (1) can be extended to cover systems of linear equations. We further show that the validity of this conjecture would have the following implications: 1. It would imply that every linear-invariant property that is closed under restrictions to linear subspaces is testable with one-sided error. Such a result would unify several previous results on testing Boolean functions, such as the testability of low-degree polynomials and of Fourier dimensionality. 2. It would imply that a linear-invariant property P is testable with one-sided error if and only if P is closed under restrictions to linear subspaces, thus resolving Sudan's problem.", "label": 1, "domain": "academic", "token_count": 329, "matched_pair_id": "conditionality_00268", "split": "train"}
{"id": "conditionality_train_pos_0671", "text": "We solve two-dimensional large-N QCD in the presence of a nonzero baryon number B, and for arbitrary quark mass m and volume L. We fully treat the dynamics of the gluonic zero modes and check how this affects results from previous studies of the B=0 and B=1 systems. For a finite density of baryons, and for any m>0, we find that the ground state contains a baryon crystal with expectation values for psi-bar gamma_mu psi that have a helix-like spatial structure. We study how these evolve with B and see that the volume integral of psi-bar psi strongly changes with the baryon density. We compare this emerging crystal structure with the sine-Gordon crystal, which is expected to be a good approximation for light quarks, and find that it is a very good approximation for surprisingly heavy quarks. We also calculate the way the ground state energy E changes as a function of the baryon number B, and find that for sufficiently large densities the function E(B) is well described by the equation of state for free massless quarks, thus suggesting a quark-Hadron continuity. From dE(B)/dB we calculate the quark chemical potential mu as a function of B and see that the baryons repel each other. The way mu depends on B also allows us to translate our findings to the grand-canonical ensemble. The resulting phase structure along the mu-axis contains a phase transition that occurs at a value of mu equal to the baryon mass divided in N, and that separates a mu-independent phase with intact translation symmetry from a mu-dependent phase with spontaneously broken translation symmetry. Finally, our calculations confirm the presence of a partial large-N Eguchi-Kawai volume independence, as described in Phys.Rev.D79:105021, that arises only if one treats the gluonic zero modes correctly.", "label": 1, "domain": "academic", "token_count": 381, "matched_pair_id": "conditionality_00114", "split": "train"}
{"id": "conditionality_train_pos_0672", "text": "We investigate the mean electromotive force in the kinematic framework, that is, ignoring the back-reaction of the magnetic field on the fluid velocity, under the assumption of axisymmetric turbulence determined by the presence of either rotation, density stratification, or both. We use an analogous approach for the mean passive scalar flux. As an alternative to convection, we consider forced turbulence in an isothermal layer. When using standard ansatzes, the mean magnetic transport is then determined by nine, and the mean passive scalar transport by four coefficients. We give results for all these transport coefficients. We use the test-field method and the test-scalar method, where transport coefficients are determined by solving sets of equations with properly chosen mean magnetic fields or mean scalars. These methods are adapted to mean fields which may depend on all three space coordinates. We find the anisotropy of turbulent diffusion to be moderate in spite of rapid rotation or strong density stratification. Contributions to the mean electromotive force determined by the symmetric part of the gradient tensor of the mean magnetic field, which were ignored in several earlier investigations, turn out to be important. In stratified rotating turbulence, the $\\alpha$ effect is strongly anisotropic, suppressed along the rotation axis on large length scales, but strongly enhanced at intermediate length scales. Also the $\\OO\\times\\meanJJ$ effect is enhanced at intermediate length scales. The turbulent passive scalar diffusivity is typically almost twice as large as the turbulent magnetic diffusivity. Both magnetic and passive scalar diffusion are slightly enhanced along the rotation axis, but decreased if there is gravity.", "label": 1, "domain": "academic", "token_count": 322, "matched_pair_id": "conditionality_00368", "split": "train"}
{"id": "conditionality_train_pos_0673", "text": "NGC 3147 is so far the most convincing case of a \"true\" Seyfert 2 galaxy, i.e. a source genuinely lacking the Broad Line Regions. We obtained a Suzaku observation with the double aim to study in more detail the iron line complex, and to check the Compton-thick hypothesis for the lack of observed optical broad lines. The Suzaku XIS and HXD/PIN spectra of the source were analysed in detail. The line complex is composed of at least two unresolved lines, one at about 6.45 keV and the other one at about 7 keV, most likely identified with Fe XVII/XIX, the former, and Fe XXVI, the latter. The high-ionization line can originate either in a photoionized matter or in an optically thin thermal plasma. In the latter case, an unusually high temperature is implied. In the photoionized model case, the large equivalent width can be explained either by an extreme iron overabundance or by assuming that the source is Compton-thick. In the Compton-thick hypothesis, however, the emission above 2 keV is mostly due to a highly ionized reflector, contrary to what is usually found in Compton-thick Seyfert 2s, where reflection from low ionized matter dominates. Moreover, the source flux varied between the XMM-Newton and the Suzaku observations, taken 3.5 years apart, confirming previous findings and indicating that the size of the emitting region must be smaller than a parsec. The hard X-ray spectrum is also inconclusive on the Compton-thick hypothesis. Weighting the various arguments, a \"true\" Seyfert 2 nature of NGC 3147 seems to be still the most likely explanation, even if the \"highly ionized reflector\" Compton-thick hypothesis cannot at present be formally rejected.", "label": 1, "domain": "academic", "token_count": 386, "matched_pair_id": "conditionality_00437", "split": "train"}
{"id": "conditionality_train_pos_0674", "text": "We present the results of daily monitoring of 6.7 GHz methanol maser in Cepheus A (Cep A) using Yamaguchi 32-m radio telescope as well as the results of imaging observations conducted with the JVN (Japanese VLBI Network). We indentified five spectral features, which are grouped into red-shifted (-1.9 and -2.7 km/s) and blue-shifted (-3.8, -4.2, and -4.9 km/s), and we detected rapid variabilities of these maser features within a monitoring period of 81 days. The red-shifted features decreased in flux density to 50% of its initial value, while the flux density of the blue-shifted features rapidly increased within a 30 days. The time variation of these maser features showed two remarkable properties; synchronization and anti-correlation between the red-shifted and the blue-shifted. The spatial distribution of the maser spots obtained by the JVN observation showed an arclike structure with a scale of $\\sim$1400 AU, and separations of the five maser features were found to be larger than 100 AU. The absolute position of the methanol maser was also obtained based on the phase-referencing observations, and the arclike structure were found to be associated with the Cep A-HW2 object, with the elongation of the arclike structure nearly perpendicularly to the radio continuum jet from the Cep A-HW2 object. These properties of the masers, namely, the synchronization of flux variation, and the spectral and spatial isolation of features, suggest that the collisional excitation by shock wave from a common exciting source is unlikely. Instead, the synchronized time variation of the masers can be explained if all the maser features are excited by infrared radiation from dust which is heated by a common exciting source with a rapid variability.", "label": 1, "domain": "academic", "token_count": 391, "matched_pair_id": "conditionality_00063", "split": "train"}
{"id": "conditionality_train_pos_0675", "text": "Protoplanet eccentricities of e >~ H/r can slow or reverse migration, but previous 2D studies have shown that gravitational scattering cannot maintain significant planet eccentricities against disc-induced damping. We simulate the evolution of low-mass protoplanetary swarms in three dimensions. The aim is to examine both protoplanet survival rates and the dynamical structure of the resulting planetary systems, and to compare them with 2D simulations. We present results from a 3D hydrodynamic simulation of eight protoplanets embedded in a protoplanetary disc. We also present a suite of simulations performed using an N-body code, modified to include prescriptions for planetary migration and for eccentricity and inclination damping. These prescriptions were obtained by fitting analytic formulae to hydrodynamic simulations of planets embedded in discs with initially eccentric and/or inclined orbits. As was found in two dimensions, differential migration produces groups of protoplanets in stable, multiple mean-motion resonances that migrate in lockstep, preventing prolonged periods of gravitational scattering. In almost all simulations, this leads to large-scale migration of the protoplanet swarm into the central star in the absence of a viable stopping mechanism. The evolution involves mutual collisions, occasional instances of large-scale scattering, and the frequent formation of the long-lived, co-orbital planet systems that arise in > 30% of all runs. Disc-induced damping overwhelms eccentricity and inclination growth due to planet-planet interactions. Co-orbital planets are a natural outcome of dynamical relaxation in a strongly dissipative environment, and if observed in nature would imply that such a period of evolution commonly arises during planetary formation.", "label": 1, "domain": "academic", "token_count": 329, "matched_pair_id": "conditionality_00101", "split": "train"}
{"id": "conditionality_train_pos_0676", "text": "if that person isn’t available to sue (for example, an individual too young to sue). The court, however, said that PETA didn’t have a significant relationship with the monkey, which is required in next friend lawsuits. After all, Slater and PETA can’t even agree on the monkey’s name — and try tracking down an individual monkey in an Indonesian jungle. The judges even went as far as accusing PETA of using the monkey as a pawn: “Puzzlingly, while representing to the world that ‘animals are not ours to eat, wear, experiment on, use for entertainment, or abuse in any other way,’… PETA seems to employ Naruto as an unwitting pawn in its ideological goals. Yet this is precisely what is to be avoided by requiring next friends to have a significant relationship with, rather than an institutional interest in, the competent party…” a footnote in the published decision reads. “I thank the judges for their decision today, that comes at a legal cost of berating a previous precedent about animals having at least some Constitutional rights in the USA,” Slater wrote in a Facebook post. “My case may indeed be a catalyst at overturning a previous but limited animal rights victory that granted animals, at least, some U.S. Constitutional respect … I so hope that wild animals are granted more and more fundamental rights in the future — like rights to dignity, survival, homeland, and their evolutionary privileges. They accept us as part of their landscape, with a big smile.” Along with dismissing the lawsuit, the judges also approved Slater’s request for attorney fees.", "label": 1, "domain": "news", "token_count": 319, "matched_pair_id": "conditionality_00707", "split": "train"}
{"id": "conditionality_train_pos_0677", "text": "Facebook is making it harder to see what your friends are liking and commenting on right this minute — the ticker feed recently joined Facebook’s list of axed features. A Facebook representative confirmed through a help forum last week that the ticker, which showed friend activity in real time from status updates to likes and comments, was removed after users started asking where the option was. The ticker is about as old as Facebook’s algorithms that determine what content you see first. The tool launched back in 2011 as a real-time alternative to news feed algorithms. While the feed chooses top stories based on past likes and other data, the ticker showed everything as it happened, including not just status updates but likes and comments on other posts as well. While Facebook only recently confirmed the feature got the ax, users have been reporting the tool missing for several weeks before that. The platform appeared to either test a ticker-free feed first or may have simply gradually removed the feature. Facebook’s decision to remove the feature likely wasn’t on a whim — the platform tested the removal of the real-time tracker in 2013, creating a panic (or in some cases, excitement) when the feature was part of an outage. Facebook returned the feature after the temporary outage. The removal of the ticker has mixed reactions for Facebook users. Many inside the Facebook help forums are reporting that they used the tool often and liked being able to have both an algorithmic feed and a real-time option. Others have different names for the feature, including “creeper feed” because of the tool’s inclusion of not just status updates but all activity on the platform. Without the ticker, Facebook’s right-hand sidebar on desktop browsers is divided into different sections with Stories at the top, followed by event invited, trending topics, Instant games, and a list of episodes (if you follow any) as part of Facebook’s new push for original video content. And of course, some ads. With only a one-line response inside a help forum confirming that the ticker is no longer available, it is unclear why Facebook decided to remove the feature. Users could previously remove the ticker from their sidebar and then turn it back on again later if they changed their mind.", "label": 1, "domain": "news", "token_count": 440, "matched_pair_id": "conditionality_00715", "split": "train"}
{"id": "conditionality_train_pos_0678", "text": "A polytropic quark star model is suggested in order to establish a general framework in which theoretical quark star models could be tested by observations. The key difference between polytropic quark stars and the polytropic model studied previously for normal (i.e., non-quarkian) stars is related to two issues: (i) a constant term representing the contribution of vacuum energy may be added in the energy density and the pressure for a quark star, but not for a normal star; (ii) the quark star models with non-vanishing density at the stellar surface are not avoidable due to the strong interaction between quarks. The first one implies that the vacuum inside a quark star is different from that outside, while the second one is relevant to the effect of color confinement. The polytropic equations of state are stiffer than that derived in conventional realistic models (e.g., the bag model) for quark matter, and pulsar-like stars calculated with a polytropic equation of state could then have high maximum masses (> 2 M_sun). Quark stars can also be very low massive, and be still gravitationally stable even if the polytropic index, n, is greater than 3. All these would result in different mass-radius relations, which could be tested by observations. In addition, substantial strain energy would develop in a solid quark star during its accretion/spindown phase, and could be high enough to take a star-quake. The energy released during star-quakes could be as high as ~ 10^{47} ergs if the tangential pressure is ~ 10^{-6} higher than the radial one.", "label": 1, "domain": "academic", "token_count": 343, "matched_pair_id": "conditionality_00056", "split": "train"}
{"id": "conditionality_train_pos_0679", "text": "SAN FRANCISCO (AP) — Amid record-setting heat in the state's south, California's water managers will measure the Sierra Nevada snowpack, which supplies water to millions. Department of Water Resources officials will trek to the mountains Thursday to check the snow depth, one gauge of the state's water supply. Electronic sensors show snow levels are about one-third of normal. At the peak of California's recently ended five-year drought, Gov. Jerry Brown ordered 25 percent water conservation in cities and towns and declared a drought emergency. Heavy rains in Northern California last year finally snapped the drought, and Brown declared the emergency over in April. But the drought never really seemed to end in some Southern California areas, said Daniel Swain, a climate scientist with the University of California, Los Angeles. Los Angeles received only one significant rain in almost the last 12 months. In Ventura and Santa Barbara counties, which are about 100 miles (161 kilometers) north of Los Angeles, the lack of rain and dry vegetation were perfect fuel for a December wildfire that grew to be the largest recorded in state history. When it finally rained, the scorched earth turned into deadly mudslides. The most recent weekly U.S. drought monitor, a product of the federal government and others, shows only small patches of the state, in Southern California, in the mildest form of drought. That compares to 2014 and 2015, some of the driest years in history in California, when much of the state was rated as in the most severe categories of drought. In the middle of the state's winter rain and snow season, no rain is in the forecast. In Southern California, \"it really is pretty grim,\" said Swain, who has tracked the stubborn weather patterns blocking rain from the state's south for years. Doug Carlson, spokesman for the state's Department of Water Resources, which carries out the snowpack surveys, said the dry weather is a growing concern, although reservoirs are still fuller than usual thanks to last year's rain in Northern California. Considerations of what constitutes a drought vary, and include: rainfall, the state of waterways, soil dryness, and other measures. Any decision to declare a new drought emergency if the winter remains dry, or later, would be up to Brown.", "label": 1, "domain": "news", "token_count": 464, "matched_pair_id": "conditionality_00504", "split": "train"}
{"id": "conditionality_train_pos_0680", "text": "Neutrinoless double beta decay, which is a very old and yet elusive process, is reviewed. Its observation will signal that lepton number is not conserved and the neutrinos are Majorana particles. More importantly it is our best hope for determining the absolute neutrino mass scale at the level of a few tens of meV. To achieve the last goal certain hurdles have to be overcome involving particle, nuclear and experimental physics. Nuclear physics is important for extracting the useful information from the data. One must accurately evaluate the relevant nuclear matrix elements, a formidable task. To this end, we review the sophisticated nuclear structure approaches recently been developed, which give confidence that the needed nuclear matrix elements can be reliably calculated. From an experimental point of view it is challenging, since the life times are long and one has to fight against formidable backgrounds. If a signal is found, it will be a tremendous accomplishment. Then, of course, the real task is going to be the extraction of the neutrino mass from the observations. This is not trivial, since current particle models predict the presence of many mechanisms other than the neutrino mass, which may contribute or even dominate this process. We will, in particular, consider the following processes: (i)The neutrino induced, but neutrino mass independent contribution. (ii)Heavy left and/or right handed neutrino mass contributions. (iii)Intermediate scalars (doubly charged etc). (iv)Supersymmetric (SUSY) contributions. We will show that it is possible to disentangle the various mechanisms and unambiguously extract the important neutrino mass scale, if all the signatures of the reaction are searched in a sufficient number of nuclear isotopes.", "label": 1, "domain": "academic", "token_count": 346, "matched_pair_id": "conditionality_00446", "split": "train"}
{"id": "conditionality_train_pos_0681", "text": "this clause for payment to the first physician; and (ii) payment may be made to a physician for physicians' services (and services incident to such services) which that physician pays a second physician on a per diem or other fee- for-time basis to provide to individuals who are patients of the first physician if (I) the first physician is unavailable to provide the services, (II) the services are not provided by the second physician over a continuous period of longer than 90 days (or such longer period as the Secretary may provide), and (III) the claim form submitted to the carrier includes the second physician's unique identifier (provided under the system established under subsection (r)) and indicates that the claim meets the requirements of this clause for payment to the first physician''. (2) Effective date.--The amendment made by paragraph (1) shall apply to services furnished on or after the first day of the first month beginning more than 60 days after the date of the enactment of this Act. (b) Medicaid Program.-- (1) In general.--Section 1902(a)(32)(C) of the Social Security Act (42 U.S.C. 1396a(a)(32)(C)) is amended to read as follows: ``(C) payment may be made to a physician for services furnished by a substitute physician under the circumstances described in subparagraph (D) of section 1842(b)(6), except that, for purposes of this subparagraph, any reference in such subparagraph to `a carrier' or `the system established under subsection (r)' is deemed a reference to the State (or other fiscal agent under the State plan) and to the system established under subsection (x) of this section, respectively.''. (2) Effective date.--(A) The amendment made by paragraph (1) shall apply to services furnished on or after the date of the enactment of this Act. (B) Until the first day of the first calendar quarter beginning more than 60 days after the date the Secretary of Health and Human Services establishes the physician identifier system under section 1902(x) of the Social Security Act, the requirement under section 1902(a)(32)(C) of such Act that a claim form submitted must include the second physician's unique identifier is deemed to be satisfied if the claim form identifies (in a manner specified by the Secretary of Health and Human Services) the second physician.", "label": 1, "domain": "government", "token_count": 486, "matched_pair_id": "conditionality_00906", "split": "train"}
{"id": "conditionality_train_pos_0682", "text": "We study the effect of Coulomb drag between two closely positioned graphene monolayers. In the limit of weak electron-electron interaction and small inter-layer spacing ($\\mu_{1(2)}, T\\ll v/d$) the drag is described by a universal function of the chemical potentials of the layers $\\mu_{1(2)}$ measured in the units of temperature $T$. When both layers are tuned close to the Dirac point, then the drag coefficient is proportional to the product of the chemical potentials $\\rho_D\\propto\\mu_1\\mu_2$. In the opposite limit of low temperature the drag is inversely proportional to both chemical potentials $\\rho_D\\propto T^2/(\\mu_1\\mu_2)$. In the mixed case where the chemical potentials of the two layers belong to the opposite limits $\\mu_1\\ll T\\ll\\mu_2$ we find $\\rho_D\\propto \\mu_1/\\mu_2$. For stronger interaction and larger values of $d$ the drag coefficient acquires logarithmic corrections and can no longer be described by a power law. Further logarithmic corrections are due to the energy dependence of the impurity scattering time in graphene (for $\\mu_{1(2)}\\gg T$ these are small and may be neglected). In the case of strongly doped (or gated) graphene $\\mu_{1(2)}\\gg v/d\\gg T$ the drag coefficient acquires additional dependence on the inter-layer spacing and we recover the usual Fermi-liquid result if the screening length is smaller than $d$.", "label": 1, "domain": "academic", "token_count": 330, "matched_pair_id": "conditionality_00384", "split": "train"}
{"id": "conditionality_train_pos_0683", "text": "Let $i_t(G)$ denote the number of independent sets of size $t$ in a graph $G$. Levit and Mandrescu have conjectured that for all bipartite $G$ the sequence $(i_t(G))_{t \\geq 0}$ (the {\\em independent set sequence} of $G$) is unimodal. We provide evidence for this conjecture by showing that is true for almost all equibipartite graphs. Specifically, we consider the random equibipartite graph $G(n,n,p)$, and show that for any fixed $p\\in(0,1]$ its independent set sequence is almost surely unimodal, and moreover almost surely log-concave except perhaps for a vanishingly small initial segment of the sequence. We obtain similar results for $p=\\tilde{\\Omega}(n^{-1/2})$. We also consider the problem of estimating $i(G)=\\sum_{t \\geq 0} i_t(G)$ for $G$ in various families. We give a sharp upper bound on the number of independent sets in an $n$-vertex graph with minimum degree $\\delta$, for all fixed $\\delta$ and sufficiently large $n$. Specifically, we show that the maximum is achieved uniquely by $K_{\\delta, n-\\delta}$, the complete bipartite graph with $\\delta$ vertices in one partition class and $n-\\delta$ in the other. We also present a weighted generalization: for all fixed $x>0$ and $\\delta >0$, as long as $n=n(x,\\delta)$ is large enough, if $G$ is a graph on $n$ vertices with minimum degree $\\delta$ then $\\sum_{t \\geq 0} i_t(G)x^t \\leq \\sum_{t \\geq 0} i_t(K_{\\delta, n-\\delta})x^t$ with equality if and only if $G=K_{\\delta, n-\\delta}$.", "label": 1, "domain": "academic", "token_count": 419, "matched_pair_id": "conditionality_00467", "split": "train"}
{"id": "conditionality_train_pos_0684", "text": "Why it matters to you Paying for data, especially on monthly subscription plans, can get expensive pretty quickly. But Ultra Mobile wants to offer an affordable prepaid plan that can compete with the big dogs. Forget about what you think you know about prepaid phone plans. Ultra Mobile wants to give you a whole new look at what it means to pay before you talk, text, and otherwise use your smartphone. On Monday, the mobile carrier announced the launch of two new high data plans, which give users 10GB or 20GB of data every month for the relatively low price of $45 and $54, respectively. This marks the largest amount of data ever offered to Ultra Mobile customers. The company, which is focused on folks with international needs, said that these higher data plans were created to appease customers who, now more than ever, are demanding high-speed data. Citing a recent Ericcson’s Mobility Report, Ultra Mobile noted that the average data consumption for 2016 was 5GB, but many other service providers “put international calling at a premium over large data allotments.” Ultra Mobile, however, has the international component built into its plans, allowing customers to pay less for what could amount to more. “Our customers and retail partners continue to request larger data offerings and we’ve listened by rounding out our portfolio with these new data plans,” said Tyler Leshney, president of Ultra Mobile. “At Ultra Mobile, we are always looking for the next best way to service our rapidly growing customer base and with these new data plans, we truly see an opportunity to satisfy the needs of a growing customer base while also offering our current subscribers additional upgrade options. As our international customer base grows we will continue to innovative and provide valuable service to our users.” Ultra is also working to expand its unlimited calling list to more than 60 countries around the world. Some existing plans, like the New $19, already allow for unlimited talk and text across the U.S., along with 100 MB 4G LTE data and calling to over 60 countries for $19 a month. So if you have friends and family aplenty abroad, you may want to take a closer look at Ultra and its latest offerings.", "label": 1, "domain": "news", "token_count": 447, "matched_pair_id": "conditionality_00720", "split": "train"}
{"id": "conditionality_train_pos_0685", "text": "threshold' is-- ``(i) $50,000 in the case of a committee which is an authorized committee of a candidate for the office of President or for nomination to such office; and ``(ii) $15,000 in the case of any other committee. In determining whether the amount of bundled contributions provided to a committee by a person exceeds the applicable threshold, there shall be excluded any contribution made to the committee by the person or the person's spouse.''; and (B) in subparagraph (B), by striking ``the amount'' each place it appears and inserting ``each amount''; (4) in paragraph (5), by striking ``described in paragraph (7)'' each place it appears in subparagraphs (C) and (D); (5) by striking paragraph (7) and inserting the following: ``(7) Separate reporting for certain persons.--Each committee required to include a schedule under paragraph (1) shall also include a separate schedule setting forth the name, address, and employer of each person listed on the schedule required under paragraph (1) who, at the time a contribution is forwarded to a committee as described in paragraph (8)(A)(i) or is received by a committee as described in paragraph (8)(A)(ii), is-- ``(A) a current registrant under section 4(a) of the Lobbying Disclosure Act of 1995; ``(B) an individual who is listed on a current registration filed under section 4(b)(6) of such Act or a current report under section 5(b)(2)(C) of such Act; or ``(C) a political committee established or controlled by such a registrant or individual. The schedule required under the preceding sentence shall also include the aggregate amount of bundled contributions provided by each such person during the covered period.''; and (6) in paragraph (8)(A)-- (A) by striking ``and a person described in paragraph (7)''; and (B) by adding at the end the following flush sentence: ``The term `bundled contribution' shall not include any contribution forwarded by or credited to (through records, designations, or other means of recognizing a certain amount of money has been raised) a person who is a regularly paid employee of the committee.''. (b) Effective Date.--The amendments made by this section shall take effect as if included in section 204 of the Honest Leadership and Open Government Act of 2007.", "label": 1, "domain": "government", "token_count": 498, "matched_pair_id": "conditionality_00997", "split": "train"}
{"id": "conditionality_train_pos_0686", "text": "We study opinion dynamics in a population of interacting adaptive agents voting on a set of complex multidimensional issues. We consider agents which can classify issues into for or against. The agents arrive at the opinions about each issue in question using an adaptive algorithm. Adaptation comes from learning and the information for the learning process comes from interacting with other neighboring agents and trying to change the internal state in order to concur with their opinions. The change in the internal state is driven by the information contained in the issue and in the opinion of the other agent. We present results in a simple yet rich context where each agent uses a Boolean Perceptron to state its opinion. If there is no internal clock, so the update occurs with asynchronously exchanged information among pairs of agents, then the typical case, if the number of issues is kept small, is the evolution into a society thorn by the emergence of factions with extreme opposite beliefs. This occurs even when seeking consensus with agents with opposite opinions. The curious result is that it is learning from those that hold the same opinions that drives the emergence of factions. This results follows from the fact that factions are prevented by not learning at all from those agents that hold the same opinion. If the number of issues is large, the dynamics becomes trapped and the society does not evolve into factions and a distribution of moderate opinions is observed. We also study the less realistic, but technically simpler synchronous case showing that global consensus is a fixed point. However, the approach to this consensus is glassy in the limit of large societies if agents adapt even in the case of agreement.", "label": 1, "domain": "academic", "token_count": 317, "matched_pair_id": "conditionality_00097", "split": "train"}
{"id": "conditionality_train_pos_0687", "text": "Given linear matrix inequalities (LMIs) L_1 and L_2, it is natural to ask: (Q1) when does one dominate the other, that is, does L_1(X) PsD imply L_2(X) PsD? (Q2) when do they have the same solution set? Such questions can be NP-hard. This paper describes a natural relaxation of an LMI, based on substituting matrices for the variables x_j. With this relaxation, the domination questions (Q1) and (Q2) have elegant answers, indeed reduce to constructible semidefinite programs. Assume there is an X such that L_1(X) and L_2(X) are both PD, and suppose the positivity domain of L_1 is bounded. For our \"matrix variable\" relaxation a positive answer to (Q1) is equivalent to the existence of matrices V_j such that L_2(x)=V_1^* L_1(x) V_1 + ... + V_k^* L_1(x) V_k. As for (Q2) we show that, up to redundancy, L_1 and L_2 are unitarily equivalent. Such algebraic certificates are typically called Positivstellensaetze and the above are examples of such for linear polynomials. The paper goes on to derive a cleaner and more powerful Putinar-type Positivstellensatz for polynomials positive on a bounded set of the form {X | L(X) PsD}. An observation at the core of the paper is that the relaxed LMI domination problem is equivalent to a classical problem. Namely, the problem of determining if a linear map from a subspace of matrices to a matrix algebra is \"completely positive\".", "label": 1, "domain": "academic", "token_count": 360, "matched_pair_id": "conditionality_00204", "split": "train"}
{"id": "conditionality_train_pos_0688", "text": "Many models of shallow water waves admit peaked solitary waves. However, it is an open question whether or not the widely accepted peaked solitary waves can be derived from the fully nonlinear wave equations. In this paper, a unified wave model (UWM) based on the symmetry and the fully nonlinear wave equations is put forward for progressive waves with permanent form in finite water depth. Different from traditional wave models, the flows described by the UWM are not necessarily irrotational at crest, so that it is more general. The unified wave model admits not only the traditional progressive waves with smooth crest, but also a new kind of solitary waves with peaked crest that include the famous peaked solitary waves given by the Camassa-Holm equation. Besides, it is proved that Kelvin's theorem still holds everywhere for the newly found peaked solitary waves. Thus, the UWM unifies, for the first time, both of the traditional smooth waves and the peaked solitary waves. In other words, the peaked solitary waves are consistent with the traditional smooth ones. So, in the frame of inviscid fluid, the peaked solitary waves are as acceptable and reasonable as the traditional smooth ones. It is found that the peaked solitary waves have some unusual and unique characteristics. First of all, they have a peaked crest with a discontinuous vertical velocity at crest. Especially, the phase speed of the peaked solitary waves has nothing to do with wave height. In addition, the kinetic energy of the peaked solitary waves either increases or almost keeps the same from free surface to bottom. All of these unusual properties show the novelty of the peaked solitary waves, although it is still an open question whether or not they are reasonable in physics if the viscosity of fluid and surface tension are considered.", "label": 1, "domain": "academic", "token_count": 347, "matched_pair_id": "conditionality_00441", "split": "train"}
{"id": "conditionality_train_pos_0689", "text": "If it seems there are a lot more animals in airports — and on airplanes — these days, you're not imagining it. More than 30 airports around the country now have regular programs that bring certified pet therapy dogs and their handlers into the terminals to mingle with passengers and help ease the stress of traveling. At both Mineta San Jose International Airport (the first airport to have an official pet therapy program) and Dallas/Fort Worth International Airport, they're called the K9 crew. At Los Angeles International Airport the PUP (Pets Unstressing Passengers) team roams the concourses. And at Denver International Airport it's the Canine Airport Therapy Squad (CATS) that welcomes passengers to hug, hang out and get their pictures taken with dogs wearing \"Pet Me\" vests. During 2016, some airport pet therapy teams broadened their membership beyond dogs. Last summer, when passengers were encountering excessively long lines at security checkpoints at many airports around the country, Cincinnati/Northern Kentucky International Airport began welcoming miniature therapy horses and their handlers to visit several times a month. And as the winter holiday travel season went into high gear, two airports announced that pigs were joining their pet therapy teams. LiLou, a Juliana-breed pig, joined San Francisco International Airport's Wag Brigade to add \"more moments of surprise and delight for guests at our airport,\" said Christopher Birch, SFO's Director-Guest Experience, on LiLou's first day on the job. Lilou, the pig will be at #sfo on 12/26/16 at 12 pm in T3. Please be patient, give her space, and always ask her mom before touching LiLou. pic.twitter.com/nekpaxYxXh — flySFO (@flySFO) December 26, 2016 And a pot-bellied pig named Bacon Bits is now part of Albany International Airport's Canine Ambassador program. More animals in the air Of course, not all the animals you see in airport terminals these days are just there to be petted. According to the American Pet Products Association, there are around 77 million pet dogs and 85 million pet cats in the United States — and a growing number of their owners take them along when they travel by air. And when they fly as carry-on passengers in the cabin, those pets need to have tickets. On Alaska Airlines and JetBlue, the domestic fee for a pet in the cabin is $100 each", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00737", "split": "train"}
{"id": "conditionality_train_pos_0690", "text": "In a prior study, I introduced a simple economic growth model designed to be consistent with general thermodynamic laws. Unlike traditional economic models, civilization is viewed only as a well-mixed global whole with no distinction made between individual nations, economic sectors, labor, or capital investments. At the model core is an observationally supported hypothesis that the global economy's current rate of primary energy consumption is tied through a constant to a very general representation of its historically accumulated wealth. Here, this growth model is coupled to a linear formulation for the evolution of globally well-mixed atmospheric CO2 concentrations. While very simple, the coupled model provides faithful multi-decadal hindcasts of trajectories in gross world product (GWP) and CO2. Extending the model to the future, the model suggests that the well-known IPCC SRES scenarios substantially underestimate how much CO2 levels will rise for a given level of future economic prosperity. For one, global CO2 emission rates cannot be decoupled from wealth through efficiency gains. For another, like a long-term natural disaster, future greenhouse warming can be expected to act as an inflationary drag on the real growth of global wealth. For atmospheric CO2 concentrations to remain below a \"dangerous\" level of 450 ppmv, model forecasts suggest that there will have to be some combination of an unrealistically rapid rate of energy decarbonization and nearly immediate reductions in global civilization wealth. Effectively, it appears that civilization may be in a double-bind. If civilization does not collapse quickly this century, then CO2 levels will likely end up exceeding 1000 ppmv; but, if CO2 levels rise by this much, then the risk is that civilization will gradually tend towards collapse.", "label": 1, "domain": "academic", "token_count": 344, "matched_pair_id": "conditionality_00261", "split": "train"}
{"id": "conditionality_train_pos_0691", "text": "and white as some people make it out to be.\" He could think of only one time he was genuinely worried about his game. McIlroy was 19 and in his first full year as a pro in 2008. He had only two top 10s all year on the European Tour. He wasn't eligible for any of the majors. He had missed three straight cuts in Sweden, Holland and Scotland. He was concerned he might lose his card. And then he lost in a playoff in Switzerland, lost in another playoff in Hong Kong and won his first pro event early in the next year. \"And I was off and running,\" he said. McIlroy reached No. 50 with that playoff loss in Hong Kong, and he hasn't fallen out since then. He's had a few dips, sure, \"but it's not as if I've had to panic.\" Palmer and McIlroy share one other connection, at least for now. They are one leg short of the Grand Slam. Palmer never won the PGA Championship. McIlroy needs the Masters. When they had dinner at Bay Hill in 2015 — right before McIlroy's first crack at the fourth leg of the slam — the topic never came up. \"It's amazing to think, all that Arnold did in the game, he never won that Grand Slam,\" McIlroy said. McIlroy at the Masters, Phil Mickelson at the U.S. Open and Jordan Spieth at the PGA Championship each have a chance at the career slam this year. \"I'm glad to be part of that conversation, get the first shot at it in a few weeks,\" McIlroy said. \"So we'll see how we go.\" His game is never far away, even if it doesn't look like it at times.", "label": 1, "domain": "news", "token_count": 369, "matched_pair_id": "conditionality_00511", "split": "train"}
{"id": "conditionality_train_pos_0692", "text": "if there weren't some out-there tech on the way. This year, much of the mobile news will revolve around the buzzwords that dominated 2016. Case in point: Huawei. When its CEO delivers his keynote on January 5th, he'll unveil a mobile strategy that centers around \"artificial intelligence, virtual reality and connected technologies.\" Expect many, many other companies to take a similarly trendy focus. ASUS, meanwhile, could continue its history of boundary-pushing CES launches by introducing the second phone to use Google's Tango depth-sensing technology for augmented reality. Even though 5G data won't be ready for the real world in 2017, we should hear a lot about the forthcoming technology at CES. It's close enough that device makers and carriers are envisioning what they can do with that much bandwidth, such as smarter self-driving cars and robots. You should see some bread-and-butter phone updates, of course. Many companies use CES for launches that would otherwise be overshadowed at Mobile World Congress a month later. That's not to say that they'll be pedestrian, though. Take LG's 2017 mid-range lineup as an example -- the company is making a point of including features that were previously reserved for higher-end devices, like fingerprint readers. Sony, in turn, is rumored to be reviving its 4K smartphone dreams now that the technology is more mature. In some ways, these could be the most important introductions at CES. They won't revolutionize the mobile landscape, but they should make once-exotic technology more commonplace. TV / home theater Richard Lawler Coming into CES 2017, several of the big players in home theater are holding their cards closer to the vest than usual. Of course, even without a slew of pre-event reveals, we have some ideas about what's in store for TVs and the devices that surround them. OLED is well-known for offering up the best display quality out there -- so what comes next? Price cuts, for one: LG's has made its series of 4K OLED TVs much more affordable while keeping the quality up, but it will need to go further to match LCD for value. As for the competition, we're waiting to see if anyone else will try the technology on for size. Panasonic and Sony are good candidates for OLED TVs in 2017, even if they end up using LG's panels. There's no indication yet that Samsung will switch gears on its display", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00626", "split": "train"}
{"id": "conditionality_train_pos_0693", "text": "If you like the hustle and bustle of a modern city in the run-up to Christmas, but with all the attractions within walking distance of each other, then Nottingham is right up your street. Hotels to meet every budget, bars, a plethora of ever-evolving restaurants catering for every cuisine and attractions for all ages and tastes, the choice is seemingly endless. Plus, at this time of year, there is an endless selection of festive fun from an ice-rink at the heart of the city among the Winter Wonderland to a Christmas fairground, ski chalet bar and a huge amount of festive cheer and shopping choices. Gone are previous misconceptions about the city, which greatly benefits from the redevelopment of the famed ‘Slab’ Square, or Old Market Square, at its heart. And because Nottingham is so compact, it has a great buzz and atmosphere as people scurry between the designer shops, independent retailers and eateries peppered everywhere. During a recent visit to the city we enjoyed an overnight stay at the wonderful St James Hotel on Rutland Street. The view from the balcony in Delilah Having undergone a full redevelopment in 2014, it has a real boutique feel that is clear to all from the public areas, such as the sparkling and spacious reception with mirrored furniture. You are immediately taken by the No 6 restaurant which is packed with books and artwork — and where you can enjoy a chance to relax in a comfy armchair with a cocktail from the extensive menu. Rooms on offer include crash pads, classic rooms, executive rooms (our choice), four-poster rooms and even a penthouse. Walkways on each of the floors have a decadent feel and that extended to our room, which was sumptuous and even had an extra seating area, plus a very comfortable super kingsize bed. Cocktails at Revolucion De Cuba Once checked in it was off into the city to sample some of the lunch delights offered by the deli Delilah. The original Delilah opened in 2005 on Middle Pavement with a dream to provide a venue for artisan foods. But since then it has grown and now has a huge home on Victoria Street. On the ground floor is a feast for the senses and tastebuds with everything from cheeses and olives to fine wines on sale. There is also a coffee bar area where you can grab a relaxed mocha and a light lunch. Upstairs, in what was a former HSBC bank, is the restaurant", "label": 1, "domain": "news", "token_count": 500, "matched_pair_id": "conditionality_00619", "split": "train"}
{"id": "conditionality_train_pos_0694", "text": "We present a Differential Emission Measure (DEM) analysis of the quiet solar corona on disk using data obtained by the Extreme-ultraviolet Imaging Spectrometer (EIS) on {\\it Hinode}. We show that the expected quiet Sun DEM distribution can be recovered from judiciously selected lines, and that their average intensities can be reproduced to within 30%. We present a subset of these selected lines spanning the temperature range $\\log$ T = 5.6 to 6.4 K that can be used to derive the DEM distribution reliably. The subset can be used without the need for extensive measurements and the observed intensities can be reproduced to within the estimated uncertainty in the pre-launch calibration of EIS. Furthermore, using this subset, we also demonstrate that the quiet coronal DEM distribution can be recovered on size scales down to the spatial resolution of the instrument (1$\"$ pixels). The subset will therefore be useful for studies of small-scale spatial inhomogeneities in the coronal temperature structure, for example, in addition to studies requiring multiple DEM derivations in space or time. We apply the subset to 45 quiet Sun datasets taken in the period 2007 January to April, and show that although the absolute magnitude of the coronal DEM may scale with the amount of released energy, the shape of the distribution is very similar up to at least $\\log$ T $\\sim$ 6.2 K in all cases. This result is consistent with the view that the {\\it shape} of the quiet Sun DEM is mainly a function of the radiating and conducting properties of the plasma and is fairly insensitive to the location and rate of energy deposition. This {\\it universal} DEM may be sensitive to other factors such as loop geometry, flows, and the heating mechanism, but if so they cannot vary significantly from quiet Sun region to region.", "label": 1, "domain": "academic", "token_count": 374, "matched_pair_id": "conditionality_00140", "split": "train"}
{"id": "conditionality_train_pos_0695", "text": "specifying the method for determining a significant increase in the price of kerosene under section 7(b)(10)(A)(iv)(II) of the Small Business Act, as added by this Act. SEC. 7. REPORTS. (a) Small Business Administration.--Not later than 12 months after the date on which the Administrator issues guidelines under section 6, and annually thereafter until the date that is 12 months after the end of the effective period of section 7(b)(10) of the Small Business Act, as added by this Act, the Administrator shall submit to the Committee on Small Business and Entrepreneurship of the Senate and the Committee on Small Business of the House of Representatives, a report on the effectiveness of the assistance made available under section 7(b)(10) of the Small Business Act, as added by this Act, including-- (1) the number of small business concerns that applied for a loan under such section and the number of those that received such loans; (2) the dollar value of those loans; (3) the States in which the small business concerns that received such loans are located; (4) the type of heating fuel or energy that caused the significant increase in the cost for the participating small business concerns; and (5) recommendations for ways to improve the assistance provided under such section 7(b)(10), if any. (b) Department of Agriculture.--Not later than 12 months after the date on which the Secretary of Agriculture issues guidelines under section 6, and annually thereafter until the date that is 12 months after the end of the effective period of the amendments made to section 321(a) of the Consolidated Farm and Rural Development Act (7 U.S.C. 1961(a)) by this Act, the Secretary shall submit to the Committee on Small Business and Entrepreneurship and the Committee on Agriculture, Nutrition, and Forestry of the Senate and the Committee on Small Business and the Committee on Agriculture of the House of Representatives, a report that-- (1) describes the effectiveness of the assistance made available under section 321(a) of the Consolidated Farm and Rural Development Act (7 U.S.C. 1961(a)); and (2) contains recommendations for ways to improve the assistance provided under such section 321(a), if any.", "label": 1, "domain": "government", "token_count": 468, "matched_pair_id": "conditionality_01030", "split": "train"}
{"id": "conditionality_train_pos_0696", "text": "We show that we can obtain a good fit to the present day stellar mass functions (MFs) of a large sample of young and old Galactic clusters in the range 0.1 - 10 Msolar with a tapered power law distribution function with an exponential truncation of the form dN/dm \\propto m^alpha [1 - exp-(m/m_c)^beta]. The average value of the power-law index alpha is -2, that of beta is 2.5, whereas the characteristic mass m_c is in the range 0.1 - 0.8 Msolar and does not seem to vary in any systematic way with the present cluster parameters such as metal abundance, total cluster mass or central concentration. However, m_c shows a remarkable correlation with the dynamical age of the cluster, namely m_c/Msolar ~ 0.15 + 0.5 tau_dyn^0.75, where tau_dyn is the dynamical age taken as the ratio of cluster age and dissolution time. The small scatter seen around this correlation is consistent with the uncertainties on the estimated value of tau_dyn. We attribute the observed trend to the onset of mass segregation via two-body relaxation in a tidal environment, causing the preferential loss of low-mass stars from the cluster and hence a drift of the characteristic mass m_c towards higher values. If dynamical evolution is indeed at the origin of the observed trend, it would seem plausible that high-concentration globular clusters, now with median m_c ~ 0.33 Msolar, were born with a stellar MF very similar to that measured today in the youngest Galactic clusters and with a value of m_c ~ 0.15 Msolar. This hypothesis is consistent with the absence of a turn-over in the MF of the Galactic bulge down to the observational limit at ~0.2 Msolar and, if correct, it would carry the implication that the characteristic mass is not set by the thermal Jeans mass of the cloud.", "label": 1, "domain": "academic", "token_count": 402, "matched_pair_id": "conditionality_00231", "split": "train"}
{"id": "conditionality_train_pos_0697", "text": "and ``(2) the testimony, or the record, document, or other object obstructed, tampered, or retaliated against by the defendant need not be admissible in evidence or free of a claim of privilege. ``(g) Intent.--In a prosecution for an offense under this section, the state of mind need not be proved with respect to-- ``(1) a State official proceeding before a judge, court, magistrate judge, or grand jury being before a judge or court of a State or political subdivision thereof; ``(2) a judge being a judge of a State or political subdivision thereof; or ``(3) a law enforcement officer being an officer or employee of the State or political subdivision thereof. ``(h) Venue.--A prosecution brought under this section may be brought-- ``(1) in the district in which the State official proceeding (whether or not pending or about to be instituted) was intended to be affected; or ``(2) in the district which the conduct constituting the alleged offense occurred.''. (b) Technical and Conforming Amendment.--The table of contents for chapter 73 of title 18, United States Code, is amended by adding at the end the following: ``1522. State and local witness tampering and retaliation.''. SEC. 3. SENTENCING GUIDELINES ENHANCEMENT. Pursuant to its authority under section 994 of title 28, United States Code, and in accordance with this section, the United States Sentencing Commission shall amend the Federal Sentencing Guidelines to increase the guideline range for Obstruction of Justice, Sec. 2J1.2, as follows-- (1) by 2 levels if the defendant threatened or harmed 1 or more individuals on more than 1 occasion; (2) by 2 levels if the defendant accepted or paid a bribe or payoff as part of a scheme to obstruct justice; (3) by 2 levels if the defendant destroyed or caused the destruction of documents on a computer; and (4) by 6 levels if the offense resulted in substantial interference with the administration of justice.", "label": 1, "domain": "government", "token_count": 424, "matched_pair_id": "conditionality_00987", "split": "train"}
{"id": "conditionality_train_pos_0698", "text": "The Latest on the announcement that Prime Minister Theresa will make a surprise statement (all times local): 10:45 a.m. The British pound has fallen amid mounting speculation that Prime Minister Theresa May is planning to call an early general election. In the wake of an announcement that May will make an unexpected statement in Downing Street at 11:15 a.m. (1015GMT), the pound was down 0.3 percent at $1.2525. May’s office says she will speak after the weekly meeting of her Cabinet. FXTM Vice President of Market Research, Jameel Ahmad says that “truth be told, nobody is really that aware of what is going on but this uncertainty has caused a reaction.” ___ 10:30 a.m. British Prime Minister Theresa May is due to make an unexpected statement in Downing Street, triggering speculation that she plans to call an early election. May’s office says she will speak at 11:15 a.m. (1015GMT) Tuesday, after the weekly meeting of her Cabinet. Such statements are generally reserved for major news, such as resignations and election calls. May, who took office in July after predecessor David Cameron stepped down, could be tempted to go to the polls to secure her own mandate as she negotiates Britain’s withdrawal from the European Union. But she has previously said she will stay in office until the next scheduled national election, in 2020. Under Britain’s Fixed-Term Parliaments Act, the prime minister can call an election if two-thirds of lawmakers vote for it.", "label": 1, "domain": "news", "token_count": 315, "matched_pair_id": "conditionality_00731", "split": "train"}
{"id": "conditionality_train_pos_0699", "text": "We have carried out calculations of the triple-differential cross section for one-photon double ionization of molecular hydrogen for a central photon energy of $75$~eV, using a fully {\\it ab initio}, nonperturbative approach to solve the time-dependent \\Schro equation in prolate spheroidal coordinates. The spatial coordinates $\\xi$ and $\\eta$ are discretized in a finite-element discrete-variable representation. The wave packet of the laser-driven two-electron system is propagated in time through an effective short iterative Lanczos method to simulate the double ionization of the hydrogen molecule. For both symmetric and asymmetric energy sharing, the present results agree to a satisfactory level with most earlier predictions for the absolute magnitude and the shape of the angular distributions. A notable exception, however, concerns the predictions of the recent time-independent calculations based on the exterior complex scaling method in prolate spheroidal coordinates [Phys.~Rev.~A~{\\bf 82}, 023423 (2010)]. Extensive tests of the numerical implementation were performed, including the effect of truncating the Neumann expansion for the dielectronic interaction on the description of the initial bound state and the predicted cross sections. We observe that the dominant escape mode of the two photoelectrons dramatically depends upon the energy sharing. In the parallel geometry, when the ejected electrons are collected along the direction of the laser polarization axis, back-to-back escape is the dominant channel for strongly asymmetric energy sharing, while it is completely forbidden if the two electrons share the excess energy equally.", "label": 1, "domain": "academic", "token_count": 312, "matched_pair_id": "conditionality_00301", "split": "train"}