-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.


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.


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.


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.


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.


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.


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.


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.


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


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.


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.


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.


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


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.


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.


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.


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 -.


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.


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


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.


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.


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.


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.


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.


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.


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!


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.


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.


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.


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.


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.


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?


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


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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.


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


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.


.--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.


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


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.


[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.


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.


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.