The pulsation periods of long period variables (LPVs) depend on their mass and helium abundance as well as on their luminosity and metal abundance. Comparison of the observed periods of LPVs in globular clusters with models is capable of revealing the amount of mass lost on the giant branch and the helium abundance.} {We aim to determine the amount of mass loss that has occurred on the giant branches of the low metallicity globular clusters NGC 362 and NGC 2808. We also aim to see if the LPVs in NGC 2808 can tell us about helium abundance variations in this cluster.} We have used optical monitoring of NGC 362 and NGC 2808 to determine periods for the LPVs in these clusters. We have made linear pulsation models for the pulsating stars in these clusters taking into account variations in mass and helium abundance. Reliable periods have been determined for 11 LPVs in NGC 362 and 15 LPVs in NGC 2808. Comparison of the observed variables with models in the logP - K diagram shows that mass loss of ~0.15-0.2 Msun is required on the first giant branch in these clusters, in agreement with estimates from other methods. In NGC 2808, there is evidence that a high helium abundance of Y~0.4 is required to explain the periods of several of the LPVs. It would be interesting to determine periods for LPVs in other Galactic globular clusters where a helium abundance variation is suspected to see if the completely independent test for a high helium abundance provided by the LPVs can confirm the high helium abundance estimates.


We combine VI photometry from OGLE-III with VVV and 2MASS measurements of E(J-K_{s}) to resolve the longstanding problem of the non-standard optical extinction toward the Galactic bulge. We show that the extinction is well-fit by the relation A_{I} = 0.7465*E(V-I) + 1.3700*E(J-K_{s}), or, equivalently, A_{I} = 1.217*E(V-I)(1+1.126*(E(J-K_{s})/E(V-I)-0.3433)). The optical and near-IR reddening law toward the inner Galaxy approximately follows an R_{V} \approx 2.5 extinction curve with a dispersion {\sigma}_{R_{V}} \approx 0.2, consistent with extragalactic investigations of the hosts of type Ia SNe. Differential reddening is shown to be significant on scales as small as as our mean field size of 6', with the 1{\sigma} dispersion in reddening averaging 9% of total reddening for our fields. The intrinsic luminosity parameters of the Galactic bulge red clump (RC) are derived to be (M_{I,RC}, \sigma_{I,RC,0}, (V-I)_{RC,0}, \sigma_{(V-I)_{RC}}, (J-K_{s})_{RC,0}) = (-0.12, 0.09, 1.06, 0.121, 0.66). Our measurements of the RC brightness, brightness dispersion and number counts allow us to estimate several Galactic bulge structural parameters. We estimate a distance to the Galactic center of 8.20 kpc, resolving previous discrepancies in distance determinations to the bulge based on I-band observations. We measure an upper bound on the tilt {\alpha} \approx 40{\deg}. between the bar's major axis and the Sun-Galactic center line of sight, though our brightness peaks are consistent with predictions of an N-body model oriented at {\alpha} \approx 25{\deg}. The number of RC stars suggests a total stellar mass for the Galactic bulge of 2.0*10^{10} M_{\odot}, if one assumes a Salpeter IMF.


We present new analysis of 11 intermediate-age (1-2 Gyr) star clusters in the Large Magellanic Cloud based on Hubble Space Telescope imaging data. Seven of the clusters feature main sequence turnoff (MSTO) regions that are wider than can be accounted for by a simple stellar population, whereas their red giant branches indicate a single value of [Fe/H]. The star clusters cover a range in present-day mass from about 1E4 to 2E5 solar masses. We compare radial distributions of stars in the upper and lower parts of the MSTO region, and calculate cluster masses and escape velocities from the present time back to a cluster age of 10 Myr. Our main result is that for all clusters in our sample with estimated escape velocities > 15 km/s at an age of 10 Myr, the stars in the brightest half of the MSTO region are significantly more centrally concentrated than the stars in the faintest half AND more massive red giant branch and asymptotic giant branch stars. This is not the case for clusters with escape velocities < 10 km/s at an age of 10 Myr. We argue that the wide MSTO region of such clusters is mainly caused by to a 200 - 500 Myr range in the ages of cluster stars due to extended star formation within the cluster from material shed by first-generation stars featuring slow stellar winds. Dilution of this enriched material by accretion of ambient interstellar matter is deemed plausible if the spread of [Fe/H] in this ambient gas was very small when the second-generation stars were formed in the cluster.


Context. X-ray binaries are usually divided in persistent and transient sources. For ultracompact X-ray binaries (UCXBs), the mass transfer rate is expected to be a strong function of orbital period, predicting persistent sources at short periods and transients at long periods. Aims. For 14 UCXBs including two candidates, we investigate the long-term variability and average luminosity with the purpose of learning how often a source can be expected to be visible above a given luminosity, and we compare the derived luminosities with the theoretical predictions. Methods. We use data from the RXTE All-Sky Monitor because of its long-term, unbiased observations. Many UCXBs are faint, i.e., they have a count rate at the noise level for most of the time. Still, information can be extracted from the data, either by using only reliable data points or by combining the bright-end variability behavior with the time-averaged luminosity. Results. Luminosity probability distributions show the fraction of time that a source emits above a given luminosity. All UCXBs show significant variability and relatively similar behavior, though the time-averaged luminosity implies higher variability in systems with a period longer than 40 min. Conclusions. There is no large difference in the statistical luminosity behavior of what we usually call persistent and transient sources. UCXBs with a period below ~30 min have a time-averaged bolometric luminosity that is in reasonable agreement with estimates based on the theoretical mass transfer rate. Around 40 min the lower bound on the time-averaged luminosity is similar to the luminosity based on the theoretical mass transfer rate, suggesting these sources are indeed faint when not detected. Above 50 min some systems are much brighter than the theoretical mass transfer rate predicts, unless these systems have helium burning donors or lose additional angular momentum.


We present the first pilot study of jets from young stars conducted with X-shooter, on ESO/VLT. As it offers simultaneous, high quality spectra in the range 300-2500 nm X-shooter is uniquely important for spectral diagnostics in jet studies. We chose to probe the accretion/ejection mechanisms at low stellar masses examining two targets with well resolved continuous jets lying on the plane of the sky, ESO-HA 574 in Chamaleon I, and Par-Lup3-4 in Lupus III. The mass of the latter is close to the sub-stellar boundary (Mstar=0.13 Msun). A large number of emission lines probing regions of different excitation are identified, position-velocity diagrams are presented and mass outflow/accretion rates are estimated. Comparison between the two objects is striking. ESO-HA 574 is a weakly accreting star for which we estimate a mass accretion rate of log(\dot{Macc}) = -10.8 \pm 0.5 (in Msun/yr), yet it drives a powerful jet with \dot{Mout} ~ 1.5-2.7 10^-9 Msun/yr. These values can be reconciled with a magneto-centrifugal jet acceleration mechanism only assuming that the presence of the edge-on disk severely depresses the luminosity of the accretion tracers. In comparison Par-Lup3-4 with stronger mass accretion (log(\dot{Macc}) = -9.1 \pm 0.4 Msun/yr), drives a low excitation jet with about \dot{Mout} ~ 3.2 10^-10 Msun/yr in both lobes. Despite the low stellar mass, \dot{Mout} / \dot{Macc} for Par-Lup3-4 is at the upper limit of the range usually measured for young objects, but still compatible with a steady magneto-centrifugal wind scenario if all uncertainties are considered.


We present resolved Herschel images of circumbinary debris disks in the alpha CrB (HD139006) and beta Tri (HD13161) systems. We find that both disks are consistent with being aligned with the binary orbital planes. Though secular perturbations from the binary can align the disk, in both cases the alignment time at the distances at which the disk is resolved is greater than the stellar age, so we conclude that the coplanarity was primordial. Neither disk can be modelled as a narrow ring, requiring extended radial distributions. To satisfy both the Herschel and mid-IR images of the alpha CrB disk, we construct a model that extends from 1-300AU, whose radial profile is broadly consistent with a picture where planetesimal collisions are excited by secular perturbations from the binary. However, this model is also consistent with stirring by other mechanisms, such as the formation of Pluto-sized objects. The beta Tri disk model extends from 50-400AU. A model with depleted (rather than empty) inner regions also reproduces the observations and is consistent with binary and other stirring mechanisms. As part of the modelling process, we find that the Herschel PACS beam varies by as much as 10% at 70um and a few % at 100um. The 70um variation can therefore hinder image interpretation, particularly for poorly resolved objects. The number of systems in which circumbinary debris disk orientations have been compared with the binary plane is now four. More systems are needed, but a picture in which disks around very close binaries (alpha CrB, beta Tri, and HD 98800, with periods of a few weeks to a year) are aligned, and disks around wider binaries (99 Her, with a 50 yr period) are misaligned, may be emerging. This picture is qualitatively consistent with the expectation that the protoplanetary disks from which the debris emerged are more likely to be aligned if their binaries have shorter periods.


The 8 o'clock arc is a gravitationally lensed Lyman Break Galaxy (LBG) at redshift z=2.73 that has a star-formation rate (SFR) of 270 solar-mass/year (derived from optical and near-infrared spectroscopy). Taking the magnification of the system ~12 and the SFR into account, the expected flux density of any associated radio emission at 1.4 GHz is predicted to be just 0.1 mJy. However, the lens system is found to be coincident with a radio source detected in the NRAO Very Large Array (VLA) Sky Survey with a flux density of ~5 mJy. If this flux density is attributed to the lensed LBG then it would imply a SFR ~11000 solar-mass/year, in contrast with the optical and near-infrared derived value. We want to investigate the radio properties of this system, and independently determine the SFR for the LBG from its lensed radio emission. We have carried out new high resolution imaging with the VLA ain A and B-configurations at 1.4 and 5 GHz. We find that the radio emission is dominated by a radio-loud AGN associated with the lensing galaxy. The radio-jet from the AGN partially covers the lensed arc of the LBG, and we do not detect any radio emission from the unobscured region of the arc down to a 3 sigma flux-density limit of 108 micro-Jy/beam. Using the radio data, we place a limit of <750 solar-mass/year for the SFR of the LBG, which is consistent with the results from the optical and near-infrared spectroscopy. We expect that the sensitivity of the Expanded VLA will be sufficient to detect many high redshift LBGs that are gravitationally lensed after only a few hours of observing time. The high angular resolution provided by the EVLA will also allow detailed studies of the lensed galaxies and determine if there is radio emission from the lens.


unless agreed to by the small entity, in any enforcement action brought against a small entity by a Federal agency in any Federal-- (A) court; or (B) administrative proceeding; and (2) may not be the subject of discovery in any enforcement action brought against a small entity by a Federal agency in any Federal-- (A) court; or (B) administrative proceeding. (c) Application.--For purposes of subsection (b), the evidence described in this subsection is-- (1) a voluntary self-audit made in good faith; and (2) any report, finding, opinion, or any other oral or written communication made in good faith relating to such voluntary self-audit. (d) Exceptions.--Subsection (b) shall not apply if-- (1) the act or omission that forms the basis of the enforcement action is a violation of criminal law; or (2) the voluntary self-audit or the report, finding, opinion, or other oral or written communication was prepared for the purpose of avoiding disclosure of information required for an investigative, administrative, or judicial proceeding that, at the time of preparation, was imminent or in progress. TITLE II--MISCELLANEOUS PROVISIONS SEC. 201. PERFORMANCE MEASURES. No covered agency shall establish or enforce agency personnel practices that reward agency employees, directly or indirectly, based on the number of contacts made with small entities in pursuit of enforcement actions or on the amount of fines levied against small entities to enforce agency regulations. SEC. 202. GRACE PERIOD FOR CORRECTION OF VIOLATIONS OF ENVIRONMENTAL PROTECTION AGENCY REGULATIONS. (a) In General.--Subject to subsection (b), for violations of regulations identified on or after the date of enactment of this Act, the Administrator of the Environmental Protection Agency shall afford small entities 180 days after the date on which the violation is identified to correct such violation. (b) Exception.--Subsection (a) shall not apply-- (1) if the Administrator of the Environmental Protection Agency determines that there is an imminent risk to public health or worker safety; or (2) to a violation of a regulation for which criminal liability may be imposed. SEC. 203. WAIVER OF PUNITIVE FINES FOR SMALL ENTITIES. Notwithstanding any other law, policy, or practice, a covered agency may waive all or part of a punitive fine that would otherwise be imposed on a small entity if--


if any rate of tax imposed by section 11, 511, or 831(a) or (b) (whichever applies) exceeds the alternative rate of tax under section 1201(a) (determined without regard to the last sentence of section 11(b)(1)). ``(E) Rate differential portion.--The rate differential portion of foreign source net capital gain, net capital, or the excess of net capital gain from sources within the United States over net capital gain, as the case may be, is the same proportion of such amount as-- ``(i) the excess of the highest rate of tax specified in section 11(b)(1) over the alternative rate of tax under section 1201(a), bears to ``(ii) the highest rate of tax specified in section 11(b)(1).'' (12) Subsection (d) of section 1044 of such Code is amended by striking the last sentence. (13) Section 1402(i)(1) of such Code is amended to read as follows: ``(1) In general.--In determining the net earnings from self-employment of any options dealer or commodities dealer-- ``(A) notwithstanding subsection (a)(3)(A), there shall not be excluded any gain or loss (in the normal course of the taxpayer's activity of dealing in or trading section 1256 contracts) from section 1256 contracts or property related to such contracts, and ``(B) the deduction provided by section 1202 shall not apply.'' (d) Clerical Amendment.--The table of sections for part I of subchapter P of chapter 1 of such Code is amended by adding at the end thereof the following new item: ``Sec. 1202. Deduction for capital gains.'' (e) Effective Date.--The amendments made by this section shall apply to taxable years ending after December 31, 1994.


We consider a system of many fermionic tachyons coupled to a scalar, pseudoscalar, vector and pseudovector fields. The scalar and pseudoscalar fields are responsible for the effective mass, while the pseudovector field is similar to ordinary electromagnetic field. The action of vector field $\omega_\mu$ results in tachyonic dispersion relation $\varepsilon_p=\sqrt{p^2+g^2\omega_0^2-hpg\omega_0-g\vec \sigma \cdot \nabla \omega_0-m^2} -g\vec \sigma \cdot \vec \omega$ that depends on helicity $h$ and spin $\vec \sigma$. We apply the mean field approximation and find that there appears a vector condensate with finite average $<\omega_0>$ depending on the tachyon density. The pressure and energy density of a many-tachyon system include the mean-field energy $<\varepsilon_p> =\sqrt{p^2+hpng^2/M^2+n^2g^4/M^4-m^2}$ which is real when the particle number density exceeds definite threshold which is $n>mM^2/g^2$ for right-handed and $n>\frac 2{\sqrt{3}}mM^2/g^2$ for left-handed tachyons, while all tachyons are subluminal at high density. There is visible difference in the properties of right-handed and left-handed tachyons. Interaction via the vector field $\omega_0$ may lead to stabilization of tachyon matter if its density is large enough.


If you’re looking for a hotel with a funky, quirky and new vibe then we’ve covered. Nestled in KL city’s sleepless Changkat Bukit Bintang, MOV Hotel opens its doors to urban and intrepid travelers seeking a design-conscious escape from the hectic city. Inspired by Kuala Lumpur’s exhilarating vibe and fast-paced people, MOV celebrates movement in the many daily facets of work, play and sweat. Located within the famous Bukit Bintang enclave in the heart of Kuala Lumpur it is just a few steps away from the city’s iconic shopping street and vibrant restaurants, bars and nightlife scene. Redefining innovative lodging with its innovative design, signature amenities and unique style, MOV Hotel provides you an integrated contemporary lifestyle experience with 147 stylish guestrooms and 9 lofts that’s perfect for a family vacation or couple’s weekend getaway. The hotel’s interior is a stunning showcase of modern design with harmonious use of textures both hard and soft, rough and smooth. Gleaming light fixtures lends a sense of elegance next to contemporary furniture and furnishings that are both minimal and bold. It’s clever design of the 138 standard room maximizes the use of each area, giving a sense of space. All rooms are fitted with king-sized beds (and single beds in twin rooms) guaranteeing the perfect end to a day of action. Even when static, the room ‘moves’ with you courtesy of colour changing lights their sexy curved showers. The nine lofts feature four different designs – Top Entourage for families, Top Oasis for couples, a Loft designed with a sitting area and another designed for a romantic getaway with a bathtub and soft sexy lighting. The hotel’s rooftop is a hub of activities and movement set against the stunning backdrop of the city. The 700 sq ft gym is the second home for travelling fitness junkies. Available at the gym are iPad apps mirrored on the giant TV screen for guests to work out for guided weights, guided yoga and HIIT workouts. The sleek swimming pool is the place to head to for a refreshing dip or to catch a bit of sun before hitting the streets at night. The Think Tank room gives guests a space to conduct meetings during their stay at MOV Hotel. But be warned this is no typical meeting room but with innovative seating – choose between gym balls, swings or designer chairs. Who says you can’t work those glutes while tapping on the laptop? Within the Lower Ground floor is Wurst Kuala Lumpur, an independent restaurant set


We present the results of a Hubble Space Telescope (HST) study of dwarf galaxies in the outer regions of the nearby rich Perseus Cluster, down to M_V = -12, and compare these with the dwarf population in the cluster core from our previous HST imaging. In this paper we examine how properties such as the colour magnitude relation, structure and morphology are affected by environment for the lowest mass galaxies. Dwarf galaxies are excellent tracers of the effects of environment due to their low masses, allowing us to derive their environmentally based evolution, which is more subtle in more massive galaxies. We identify 11 dwarf elliptical (dE) and dwarf spheroidal (dSph) galaxies in the outer regions of Perseus, all of which are previously unstudied. We measure the (V-I)_0 colours of our newly discovered dEs, and find that these dwarfs lie on the same red sequence as those in the cluster core. The morphologies of these dwarfs are examined by quantifying their light distributions using CAS parameters, and we find that dEs in the cluster outskirts are on average more disturbed than those in the core, with <A> =0.13\pm0.09 and <S> =0.18\pm0.08, compared to <A> =0.02\pm0.04, <S> =0.01\pm0.07 for those in the core. Based on these results, we infer that these objects are ``transition dwarfs'', likely in the process of transforming from late-type to early type galaxies as they infall into the cluster, with their colours transforming before their structures. When we compare the number counts for both the core and outer regions of the cluster, we find that below M_V = -12, the counts in the outer regions of the cluster exceed those in the core. This is evidence that in the very dense region of the cluster, dwarfs are unable to survive unless they are sufficiently massive to prevent their disruption by the cluster potential and interactions with other galaxies.


If you’re planning to visit Knott’s Soak City water park in Buena Park, you have some options. You can carry your things or rent a locker and you can look for an open lounge chair or bench. Or you might want to rent a cabana. There are three different locations in the park with cabanas: Shore Break, with a view of the Shore Break and The Wedge attractions; Malibu, near the Malibu Run and Old Man Falls attractions; and Wavepool, overlooking Tidal Wave Bay. Each cabana has a tented private area and an outer patio area and comes with an umbrella, a table and four chairs, four lounge chairs, four inner tube rentals and waiter service. Bethany Elliott relaxes with a book inside a cabana at Knotts Soak City in Buena Park. (Photo courtesy of David Elliott). The Crismon family usually dines at the Longboard’s Grill at Knott’s Soak City in Buena Park. They liked that they could have food delivered to their cabana and that their server made sure that there was always a pitcher of cold water available. (Photo courtesy of David Crismon). Sound The gallery will resume in seconds Four-year-old Poppy Walsh hangs out in a shaded cabana at Knott’s Soak City in Buena Park on Sunday, May 13, 2018. (Photo by Mindy Schauer, Orange County Register/SCNG) Four-year-old Poppy Walsh hangs out in a shaded cabana at Knott’s Soak City in Buena Park on Sunday, May 13, 2018. (Photo by Mindy Schauer, Orange County Register/SCNG) Sisters Georgia Harper and Poppy Walsh take a walk together at Knott’s Soak City in Buena Park. (Photo courtesy of Melanie Walsh) They aren’t cheap and must be reserved in advance of your visit. Rental fees vary from $170-$245 depending on the date and are good for up to eight guests, plus include all the amenities mentioned. You may add up two additional guests for $15 each. Soak City admission is not included. But for some, it’s all worth it. Retiree David Crismon of Wildomar and his wife Cathi Crismon enjoy bringing their grandchildren, Cody Mobley, 15, and Kennedy Mobley, 12, to Soak City. This year they decided to rent


a long-term lease. For de la Cretaz, there were other perks. “It gave us housing stability, allowed us to begin saving for retirement, provided childcare help for us when we had other people living in our home, and gave friends and community members a place to live when they needed it,” she says. "The idea of what's normal has really changed." Alaina Leary, 25, works in publishing from home and opted to live in Quincy, a town in the Boston area with a lower cost of living. “It has no doubt saved me a lot of money and time. It’s time I now spend working and making money, and even the extra 2–3 hours per day five days a week has yielded thousands of extra dollars in my savings account over 2017 and early 2018,” Leary says. While these approaches are innovative, Worth says, they’re choices being made not just from a cultural standpoint, but also out of necessity. “If you look at the baby boomers, a lot of them were able to move out by their late teens even and had permanent full-time jobs with benefits in their 20s, but within one generation that’s really changed,” Worth says. “The idea of what’s normal has really changed. Young people typically look to their parents for what to expect, but nothing is the same in terms of wider social conditions around work, housing, and family life.” The nonprofit policy research organization Generation Squeeze estimates it took five years to save a 20 percent down payment in 1976, compared to 13–27 years today. Many Americans are no longer able to make a 20 percent down payment. But interestingly, Worth says, millennials seem to be less bothered by communal living situations. “One in three people surveyed responded with ‘I lived at home because I want to stay with my parents,’” she says. “That isn’t necessarily new with the millennial generation, but it’s an unreflected-upon part of why millennials live at home, this idea of generational interconnectedness and helping each other cope in times of economic stress.” “I’m taking this time of not having rent to save up some money and decide where I want to settle down long term—or if I want to settle down at all,” Brown says.


Toral introduced so-called cooperative Parrondo games, in which there are N players (3 or more) arranged in a circle. At each turn one player is randomly chosen to play. He plays either game A or game B, depending on the strategy. Game A results in a win or loss of one unit based on the toss of a fair coin. Game B results in a win or loss of one unit based on the toss of a biased coin, with the amount of the bias depending on whether none, one, or two of the player's two nearest neighbors have won their most recent games. Game A is fair, so the games are said to exhibit the Parrondo effect if game B is losing or fair and the random mixture C:=(1/2)(A+B) is winning. With mu_B (resp., mu_C) denoting the mean profit per turn to the ensemble of N players always playing game B (resp., C), we give sufficient conditions for lim mu_B (as N goes to infinity) to exist and show that lim mu_C nearly always exists, with the limits expressible in terms of a parameterized spin system on the one-dimensional integer lattice. For a particular choice of the parameters, we show that the Parrondo effect (i.e., mu_B is nonpositive and mu_C is positive) is present in the N-player model if and only if N is even. For the same choice of the parameters, we show that, with a suitable interpretation and for certain initial distributions, the Parrondo effect is present in the spin system if and only if N is even, N being the number of consecutive players whose collective profit is tracked.


This paper concerns the solution of the self-consistency equation for energy gap parameter $\Delta_{\bf k}$ in the BCS theory of superconductivity. We show that there exists a well-defined relation between the solution for energy gap parameter amplitude $|\Delta_{\bf k}|$ for a general interaction $V_{{\bf k},{\bf k}'}$ and energy gap $\Delta$ obtained by using the cut-off approximation. The relation between $|\Delta_{\bf k}|$ and $\Delta$ indicates that $\Delta$ is a weighted average over $|\Delta_{\bf k}|$ of electronic states within cut-off energy $\xi_c$ around the Fermi surface. In this interpretation for $\Delta$, $\xi_c$ is not a property of $V_{{\bf k},{\bf k}'}$, but a parameter specifying the energy range within which the weighted average over $|\Delta_{\bf k}|$ is taken. We show that the proper choice for the value of $\xi_c$ is only a few $k_BT_c$ (i.e., $\xi_c/k_BT_c$ is about 3 or 4). We also show that the cut-off approximation, even with $\xi_c/k_BT_c=\infty$, is a good approximation when it is used to calculate quantities such as the condensation energy and the specific heat, but it leads to significant overestimation for the Josephson critical current density of a Josephson junction if $\xi_c/k_BT_c \gg 1$ is assumed.


The holy grail of exoplanet searches is an exo-Earth, an Earth mass planet in the habitable zone around a nearby star. Mass is the most important parameter of a planet and can only be measured by observing the motion of the star around the planet-star center of mass. A single image of a planet, however, does not provide evidence that the planet is Earth mass or that it is in a habitable zone orbit. The planet's orbit, however, can be measured either by imaging the planet at multiple epochs or by measuring the position of the star at multiple epochs by space-based astrometry. The measurement of an exo-planet's orbit by direct imaging is complicated by a number of factors: (1) the inner working angle (IWA); (2) the apparent brightness of the planet depending on the orbital phase; (3) confusion arising from the presence of multiple planets; and (4) the planet-star contrast. In this paper we address the question: "Can a prior astrometric mission that can identify which stars have Earthlike planets significantly improve the science yield of a mission to image exo-Earths?" We find that the Occulting Ozone Observatory (a small external occulter mission that cannot measure spectra) could confirm the orbits of ~4 to ~5 times as many exo-Earths if an astrometric mission preceded it to identify which stars had such planets. We find that in the case of an internal coronagraph, a survey of the nearest ~60 stars could be done with a telescope of half the size if an astrometric mission had first identified the presence of Earth-like planets in the habitable zone and measured their orbital parameters.


in single-season leagues, let someone else take the chance on Buxton. You can find better players on the waiver wire. 2. Sam Dyson, RP, Texas Rangers: Hopefully, you didn’t draft both Britton and Dyson, because you’d really need to find saves now. Dyson has been a nightmare this year (0-2, 24.75 ERA) after posting 38 saves last year. But his strikeout rate has never been great (career 7.4 Ks per nine IP), so he was a risky pick to begin with this year. Psychologically, it’s hard to see the Rangers going back to Dyson later for saves, especially when they have better options on their roster. Drop him and find a better reliever. Someone else can take a chance on Dyson. 3. Russell Martin, C, Toronto Blue Jays: A four-time All-Star selection, Martin (and his Blue Jays) are off to a terrible start this season. However, he is a career.253 hitter, and for a catcher with his power, that’s acceptable. You know he will bounce back later along with his whole team. In the meantime, however, stash him on your bench and pick up a streaky, hot-hitting, unknown catcher. This will save your team average for now, and you’ll be able to ride the inevitable, stat-correcting run Martin goes on later this summer. 4. Jeff Samardzija, SP, San Francisco Giants: He’s now 0-3 with a 6.16 ERA and a 1.42 WHIP, although he looked a little better on Sunday against Colorado (no walks, eight Ks) despite taking the loss. However, the problem is that the Shark is the team’s No. 4 starter, and he lacks the quality stuff plus the mental fortitude (which is surprising, considering his college football days playing for Notre Dame) to overcome the San Francisco roster’s many deficiencies. He’s not Madison Bumgarner, and right now, even Bumgarner is winless for this last-place Giants team. Bench Samardzija if you must, but there are better SPs on the waiver wire.


if an equity interest in the entity is or was owned by such a foreign state, such term shall refer to the corporate entity itself and not to such foreign state. (3) Property.--The term ``property'' means any personal belongings owned or controlled by the victims of the deportations which may have been taken or confiscated in connection with the deportations, including jewelry, books, artifacts, precious metals, and currency. (4) Records.--The term ``records'' includes any documents, correspondence, memoranda, receipts, invoices, presentations, audits, and any other related materials. (5) State.--The term ``State'' means each of the several States, the District of Columbia, and any commonwealth, territory, or possession of the United States. SEC. 4. CERTAIN ENTITIES INELIGIBLE FOR FEDERALLY FUNDED HIGH-SPEED RAIL CONTRACTS. (a) In General.--Any entity that applies for a contract with any agency or instrumentality of a State or local government for any high- speed rail project (including the design, engineering, construction, manufacture, or operation of a high-speed rail network or any components thereof) that is funded, either partially or fully, by the Federal Government shall certify to such agency, in advance of submitting a formal bid to such agency, whether or not such entity had any direct involvement in the deportation of any individuals to extermination camps, death camps, or any facility used for the purpose of transiting individuals to extermination or death camps, during the period beginning on January 1, 1942, and ending on December 31, 1944. (b) Disclosures.--If an entity certifies that it had any direct involvement described in subsection (a), the entity shall certify and disclose to the agency or instrumentality of a State or local government the following: (1) Whether the entity has any records related to the deportations in its possession, custody, or control. If an entity acknowledges that it has any such records, it shall describe in detail the full contents of such records and the specific locations where such records are maintained. (2) Whether the entity has any property taken or confiscated in connection with such deportations in its possession, custody or control. If an entity acknowledges that it has any such property, it must describe in detail the specific property in its possession, custody, or control and the specific locations where such property is maintained. If such entity does not have


A quantitative evaluation of dilepton sources in heavy-ion reactions is performed taking into account both thermal and non-thermal production mechanisms. The hadronic thermal emission rate is based on an electromagnetic current-correlation function with a low-mass region (LMR, M \lsim 1 GeV) dominated by vector mesons (\rho, \omega, \phi) and an intermediate-mass region (IMR, 1 GeV \le M \le 3 GeV) characterized by (the onset of) a multi-meson continuum. A convolution of the emission rates over a thermal fireball expansion results in good agreement with experiment in the low-mass spectra, confirming the predicted broadening of the \rho meson in hadronic matter in connection with the prevalence of baryon-induced medium effects. The absolute magnitude of the LMR excess is mostly controlled by the fireball lifetime, which in turn leads to a consistent explanation of the dilepton excess in the IMR in terms of thermal radiation. The analysis of experimental transverse-momentum (q_T) spectra reveals discrepancies with thermal emission for q_T \gsim 1 GeV in noncentral In-In collisions, which we address by extending our calculations by: (i) a refined treatment of \rho decays at thermal freezeout, (ii) primordially produced \rho's subject to energy-loss, (iii) Drell-Yan annihilation, and (iv) thermal radiation from t-channel meson exchange processes. We investigate the sensitivity of dilepton spectra to the critical temperature and hadro-chemical freezeout of the fireball. The \rho broadening in the LMR turns out to be robust, while in the IMR Quark-Gluon Plasma radiation is moderate unless the critical temperature is rather low.


If we hope to meet the moral test of our times, if we hope to eradicate child poverty or AIDS or joblessness or homelessness … then I think that we’re going to have to talk more about the empathy deficit — the ability to put ourselves in somebody else’s shoes, to see the world through somebody else’s eyes.” The Empathy Museum takes a similar tack. On its website, it defines its mission as using participatory art projects to explore “how empathy can not only transform our personal relationships, but also help tackle global challenges such as prejudice, conflict and inequality.” Founded in 2015, it has launched projects such as the Human Library, which allow visitors to “borrow” another person for a one-on-one conversation, and A Thousand and One Books, an actual library built from donations. “A Mile in My Shoes,” the exhibit I saw, fitted visitors for the shoes of a refugee or migrant and then provided them an audio recording of the person whose shoes they were literally walking in. The shoes I fit belonged to Julie Cheung Inhin, a British East Asian actress. On the audio, she spoke of the moments when someone would comment on her race and she would suddenly become conscious of her difference from the people around her, despite “feeling like everyone else.” As painful as such moments must have been for her, they also shone a problematic light on exhibit itself. No matter how much I, a white woman, could imagine what Cheung Inhin might feel in these instances, and no matter how long I walked in her shoes, other people would never perceive us in the same way. I could imagine her pain, but I would never actually suffer it, and that made the experience of walking in her shoes feel more like consumption than communication. Did I really need her to relive those experiences into the recording in order to understand she had been treated unjustly in those moments? When I returned from my intimate, meditative stroll with Julie, I saw that others were waiting for their turn with her shoes — my second empathetic failure that day. In paying careful attention to the recording, I paid too little attention to everyone else. The idea behind projects like the Empathy Museum is that that empathy, when felt truly, will prompt global change. But how? If I’m personally moved to give a bag of almonds or even my entire personal savings, that hardly seems sufficient to pass the “moral test of our times” or change the world. How can


the line “heaven meets earth like a sloppy wet kiss.” More recently, concerns over the “wrath of God,” as sung in the hymn “In Christ Alone,” led certain churches to alter the verse or stop singing the song altogether. The chorus of “Reckless Love,” co-written by Asbury as well as Caleb Culver and Ran Jackson with Bethel Music, goes: O, the overwhelming, never-ending, reckless love of God O, it chases me down, fights ’til I’m found, leaves the ninety-nine I couldn’t earn it, and I don’t deserve it, still, you give yourself away O, the overwhelming, never-ending, reckless love of God, yeah The song unofficially debuted last year from Bethel Music before becoming the lead single off Asbury’s album of the same name, which released in January. The singer explained, “When I use the phrase, ‘the reckless love of God,’ I’m not saying that God himself is reckless. I am, however, saying that the way he loves, is in many regards, quite so.” Assemblies of God minister and theologian Andrew Gabriel pushed back against the distinction, saying that “you can’t separate God from his attributes.” In a blog post addressing “Reckless Love,” he stated that “God loves us with clear and thoughtful intention,” not careless abandon. Even the parable of the lost sheep does not necessarily convey irresponsibility since scholars say shepherds routinely watched each other’s flocks if one went away, he said. Blogger Paul Yoo similarly made the case that the Bible does not portray such a free-wheeling Savior: “God’s love seems reckless because he is so unconcerned about himself or his well-being in the way he loves. However…the whole Bible shows us that God is not unconcerned with himself but is ultimately for himself.” CT asked Christian music experts to weigh in on “Reckless Love.” Most agreed that it’s a good thing for Christians to examine the theology beneath catchy lyrics—and said it’d be reckless not to. Wen Reagan, adjunct instructor of church history and worship at Duke Divinity School: Reckless could be taken two ways here. One is with its common implication of “thoughtlessness” or “carelessness.” I think we can all agree that’s not a very accurate description of God’s love for us, and if that was the association here, then the song would be problematic.


Recent observations of the low-mass pre-main sequence, eccentric spectroscopic binaries DQ Tau and V773 Tau A reveal that their millimeter spectrum is occasionally dominated by flares from non-thermal emission processes. The transient activity is believed to be synchrotron in nature, resulting from powerful magnetic reconnection events when the separate magnetic structures of the binary components are capable of interacting and forced to reorganize, typically near periastron. We conducted the first systematic study of the millimeter variability toward a sample of 12 PMS spectroscopic binaries with the aim to characterize the proliferation of flares amongst sources likely to experience similar interbinary reconnection events. The source sample consists of short-period, close-separation binaries that possess either a high orbital eccentricity or a circular orbit. Using the MAMBO2 array on the IRAM 30m telescope, we carried out continuous monitoring at 1.25 mm over a 4-night period during which all of the high-eccentricity binaries approached periastron. We also obtained simultaneous optical VRI measurements, since a strong link is often observed between stellar reconnection events and optical brightenings. UZ Tau E is the only source to be detected at millimeter wavelengths: it exhibited significant variation; it is also the only source to undergo strong simultaneous optical variability. The binary possesses the largest orbital eccentricity in the current sample, a predicted factor in star-star magnetic interaction events. With orbital parameters and variable accretion activity similar to DQ Tau, the millimeter behavior of UZ Tau E draws many parallels to the DQ Tau model for colliding magnetospheres. However, on the basis of our observations alone, we cannot determine whether the variability is repetitive, or if it could also be due to variable free-free emission in an ionized wind.


The Galaxy hosts a widespread population of low-energy positrons revealed by successive generations of gamma-ray telescopes through a bright annihilation emission from the bulge region, with a fainter contribution from the inner disk. The exact origin of these particles remains currently unknown. We estimate the contribution to the annihilation signal of positrons generated in the decay of radioactive 26Al, 56Ni and 44Ti. We adapted the GALPROP propagation code to simulate the transport and annihilation of radioactivity positrons in a model of our Galaxy. Using plausible source spatial distributions, we explored several possible propagation scenarios to account for the large uncertainties on the transport of ~1MeV positrons in the interstellar medium. We then compared the predicted intensity distributions to the INTEGRAL/SPI observations. We obtain similar intensity distributions with small bulge-to-disk ratios, even for extreme large-scale transport prescriptions. At least half of the positrons annihilate close to their sources, even when they are allowed to travel far away. In the high-diffusion, ballistic case, up to 40% of them escape the Galaxy. In proportion, this affects bulge positrons more than disk positrons because they are injected further off the plane in a tenuous medium, while disk positrons are mostly injected in the dense molecular ring. The predicted intensity distributions are fully consistent with the observed longitudinally-extended disk-like emission, but the transport scenario cannot be strongly constrained by the current data. Nucleosynthesis positrons alone cannot account for the observed annihilation emission in the frame of our model. An additional component is needed to explain the strong bulge contribution, and the latter is very likely concentrated in the central regions if positrons have initial energies in the 100keV-1MeV range.


Whether you are planning to stay in your home for several years, or if you are selling in the near future, it is important to spend your money on home improvement projects that will bring you the best return on your investment (ROI). That said, here are five home improvements projects to consider for this year: Upgrade the Kitchen: One of the smartest rooms to invest in is your kitchen. While new appliances and updated cupboards and counter tops improve the value of your kitchen, do not forget about a smart, well-designed workspace. If you are renovating the kitchen, be sure to invest in a professional layout and efficient design. According to Realtor.com, a minor kitchen remodel averages over 80 percent on your ROI, and a major kitchen remodel averages over 65 percent. Spruce Up the Bathrooms: Just a few improvements to a bathroom can go a long way. For example, install new fixtures, replace the mirror, and add a fresh coat of paint. Top off the new look with decorative plush towels and accessories. Enhance Your Curb Appeal: There are several things you can do to enhance your curb appeal — add potted plants, put in a new walkway, paint and fix shutters, and repair cracks in the driveway. Additionally, replacing your front door with an updated, more attractive style is always a great idea. It can help with energy costs, and also keep your home more secure. Plus, front door replacements consistently have a high return on investment. Consider hiring a professional if a task is out of your scope of expertise, especially for more complicated and dangerous projects. Recommended Stories For You Replace Outdated Plumbing: Believe or not, an appraiser takes plumbing into consideration when assigning value to a home. So, if you have old, rusty iron pipes, you may want to consider updating the plumbing. Nowadays, re-piping is usually done with plastic tubing, which is extremely reliable and can be replaced more efficiently and easier than in years past. Add More Attic Insulation: While it might not be the most glamorous project, adding fiberglass attic insulation actually pays for itself and delivers a small profit whenever you decide to sell. Often times, adding more insulation scores the highest return on investment of all home improvements. Keep in mind that many home improvements fall under the "Do it Yourself" category, but some do not! So, consider hiring a professional if a task is out of your scope of expertise, especially for more complicated and dangerous projects.


individuals, eligible under the State plan who reside in a community setting or are transitioning to a community setting, in gaining access to needed medical, social, educational, and other services. Such services may be offered by staff of non-medical programs or those who contract with non-medical programs, so long as such individuals are qualified providers under the State plan under this title and the case management services are distinct from the direct services of the non-medical program.''; (2) by redesignating clause (ii) as clause (iii); and (3) by inserting after clause (i) (as amended by paragraph (1)), the following new clause: ``(ii) For purposes of providing case management services, individuals (other than individuals who have attained age 22 but not attained age 65 and are patients in an institution for mental diseases or individuals who are inmates of public institutions) may be considered to be transitioning to a community setting for up to the last 180 days of an institutional stay.''. SEC. 205. ASSURING APPROPRIATE CASE MANAGEMENT. Section 1915(g)(4) of the Social Security Act (42 U.S.C. 1396n(g)(4)), as amended by section 202, is amended by adding at the end the following: ``(D) Nothing in this subsection shall be construed as prohibiting a State from providing case management or targeted case management services, as defined in subparagraphs (A) and (B), respectively, of paragraph (2), through multiple case managers to any individual who qualifies for medical assistance under the State plan, or to specific classes of individuals, or to individuals who reside in specified areas, selected by the State pursuant to this subsection.''. SEC. 206. EFFECTIVE DATE. The amendments made by this title shall take effect as if enacted on December 4, 2007.


resistance on a progressive scale; and (D) the effect on the utility of ROVs used by the Armed Forces if the proposed requirements were adopted. (2) Consultation and deadline for report.--The National Academy of Sciences shall consult with the National Highway Traffic Safety Administration and the Department of Defense in carrying out the study required by this subsection. The National Academy of Sciences shall complete and transmit to the Commission a report containing the findings of the study not later than two years after the date of enactment of this Act. (3) Report to congress.--Within five days of receiving the report described in paragraph (2) from the National Academy of Sciences, the Commission shall transmit the report, along with any comments of the Commission, to the Committee on Energy and Commerce of the House of Representatives and to the Committee on Commerce, Science and Transportation of the Senate. (4) Consideration.--The Commission shall consider the results of the study in any subsequent rulemaking regarding the performance or configuration of ROVs, or the provision of point-of-sale information regarding ROV performance. (c) Definitions.--As used in this section: (1) Commission.--The term ``Commission'' means the Consumer Product Safety Commission. (2) Recreational off-highway vehicle.--The term ``recreational off-highway vehicle'' or ``ROV'' means a motorized off-highway vehicle designed to travel on four or more tires, intended by the manufacturer for recreational use by one or more persons and having the following characteristics: (A) A steering wheel for steering control. (B) Foot controls for throttle and service brake. (C) Non-straddle seating. (D) Maximum speed capability greater than 30 miles per hour. (E) Gross vehicle weight rating no greater than 3,750 pounds. (F) Less than 80 inches in overall width, exclusive of accessories. (G) Engine displacement equal to or less than 61 cubic inches for gasoline fueled engines. (H) Identification by means of a 17-character personal or vehicle information number. (3) Exclusion.--Such term does not include a prototype of a motorized, off-highway, all-terrain vehicle or other motorized, off-highway, all-terrain vehicle that is intended exclusively for research and development purposes unless the vehicle is offered for sale.


If your Google Wifi seems to be looking a bit blue these days — as in, the light is stuck blue — you might want to check to see if it's still actually functioning. The current build for it (9202.35.8) seems to be causing issues for some users. You probably know if you've been affected since, well, your Google Wifi won't be working. Other means of detection and confirmation manifest themselves via a steady blue light on the primary hub, at which point the satellite hubs may start to flash orange signifying a disconnect of the primary hub. In the meantime it seems that restarting that primary hub fixes the issue, but only temporarily. To be very clear, this is not a universal problem. It could be related to the latest build (9202.35.8). Even then, not all users are reporting this, and the precise nature of the cause has not been reported. But, a reasonably large number of individuals on Google's forums have been experiencing this particular issue. Google has responded on the forum with some information, reassurance, and instructions for those affected, saying, "Our team is still looking into this and working hard on getting a fix out-- we aim to have it out as soon as possible." More information for those who find they may be experiencing this problem is available below: The engineering team is still working on a final fix for this issue. However, over the past few days our support team has seen two workarounds that make help resolve the issue temporarily until the fix is released. These have worked in a few cases, and may be worth a try. 1. Attempt to setup GWifi from scratch using a different owner account. This can mean creating a new Google account, or using a family member's Google account to setup the Google Wifi devices through the GW app. 2. Disconnect wireless Windows 10 devices or Xbox devices (or connect them via ethernet instead). There have been a few cases in which disconnecting any Windows 10 devices or Xbox devices has brought the Google Wifi network back up again without crashes. You can also reach out to our support team (g.co/wificare or wifica...@google.com), who will be able to provide more deep-dive troubleshooting advice based on the topography of your network. As always, thank you for your patience while we work on this issue. Both of the potential fixes at this time seem a bit unfortunate; neither having to switch to a new


Classically, unimodular gravity is known to be equivalent to General Relativity (GR), except for the fact that the effective cosmological constant $\Lambda$ has the status of an integration constant. Here, we explore various formulations of unimodular gravity beyond the classical limit. We first consider the non-generally covariant action formulation in which the determinant of the metric is held fixed to unity. We argue that the corresponding quantum theory is also equivalent to General Relativity for localized perturbative processes which take place in generic backgrounds of infinite volume (such as asymptotically flat spacetimes). Next, using the same action, we calculate semiclassical non-perturbative quantities, which we expect will be dominated by Euclidean instanton solutions. We derive the entropy/area ratio for cosmological and black hole horizons, finding agreement with GR for solutions in backgrounds of infinite volume, but disagreement for backgrounds with finite volume. In deriving the above results, the path integral is taken over histories with fixed 4-volume. We point out that the results are different if we allow the 4-volume of the different histories to vary over a continuum range. In this "generalized" version of unimodular gravity, one recovers the full set of Einstein's equations in the classical limit, including the trace, so $\Lambda$ is no longer an integration constant. Finally, we consider the generally covariant theory due to Henneaux and Teitelboim, which is classically equivalent to unimodular gravity. In this case, the standard semiclassical GR results are recovered provided that the boundary term in the Euclidean action is chosen appropriately.


acquisition, land acquired by the Secretary under this Act shall be administered in accordance with the laws (including rules and regulations) generally applicable to the National Forest System. (3) Land and water conservation fund.--For purposes of section 7 of the Land and Water Conservation Fund Act of 1965 (16 U.S.C. 460l-9), the boundaries of the White River National Forest shall be deemed to be the boundaries of the White River National Forest as of January 1, 1965. (b) Revocation of Orders and Withdrawal.-- (1) Revocation of orders.--Any public orders withdrawing any of the Federal land from appropriation or disposal under the public land laws are revoked to the extent necessary to permit disposal of the Federal land. (2) Withdrawal of federal land.--On the date of enactment of this Act, if not already withdrawn or segregated from entry and appropriation under the public land laws (including the mining and mineral leasing laws) and the Geothermal Steam Act of 1970 (30 U.S.C. 1001 et seq.), the Federal land is withdrawn, subject to valid existing rights, until the date of the conveyance of the Federal land to the County. (3) Withdrawal of non-federal land.--On acquisition of the non-Federal land by the Secretary, the non-Federal land is permanently withdrawn from all forms of appropriation and disposition under the public land laws (including the mining and mineral leasing laws) and the Geothermal Steam Act of 1970 (30 U.S.C. 1001 et seq.). (c) Boundary Adjustments.--The Secretary with jurisdiction over the land and the County may agree to-- (1) minor adjustments to the boundaries of the Federal land and non-Federal land; and (2) modifications or deletions of parcels and mining claim remnants of Federal land or non-Federal land to be exchanged on Smuggler Mountain. (d) Map.--If there is a discrepancy between a map, acreage estimate, and legal or other description of the land to be exchanged under this Act, the map shall prevail unless the Secretary with jurisdiction over the land and the County agree otherwise.


If Flowers is traded, the Giants are going to have to draft a tackle or sign one as a free agent. Odell Beckham Jr., who missed most of last season with a broken ankle, and defensive end Olivier Vernon were both at the minicamp. They skipped the minicamp a year ago. "I think the big thing for us is our game is very simple — it's about the ball, it's about negotiating the ground and it's really about man whipping man," Shurmur said. The minicamp, which does not entail any hitting, is more about making sure players get to know the new systems, with some throwing and receiving mixed in. The defences can work on stripping the ball. There was speculation that Shurmur wanted to use the minicamp to see what quarterback Davis Webb could do. The third-round pick did nothing last season, so the Giants really don't know what they have with their backup to Eli Manning. "I don't think there needs to be any anxiety on his part — get trained up, come on out here, let it rip and mistakes happen in practice and you learn from them," Shurmur said. "I think that's why you practice, so I think you have to be careful about making a final evaluation on a guy in a three-day period here. He just needs to come out here and get as good as he can be." Most players said they felt they were entering this season with a clean slate. Cornerback Janoris Jenkins, who was suspended for a game last season after missing a practice, intends to be on his best behaviour this season. "I promise y'all that Jackrabbit says it won't happen this year what happened last year," he said. "There won't be any animosity between players, no disrespecting the coach. There will be none of that. New York Giant football is back." Jenkins also believes fellow cornerback and 2016 first-round draft pick Eli Apple, who also was suspended for a game, will be a different player this season. "You have to understand that he was young," Jenkins said. "It's a clean slate, new coaching staff and for him it's guys like me that have to push him and help him out because I've been in the league so long and just help him understand that adversity is going to hit you and when it hits, you've just got to keep it going." Beckham did not take part in the afternoon practice


with clients? Funke Ajomale I had an argument with somebody over this issue. She was going for a friend’s wedding and wanted to wear over the top kind of white, I told her not to wear the dress and she was upset. If it was my wedding I would have said to her not to enter. It is the bride’s day and you are meant to give her that respect and not outshine her. Where I work, we can wear whatever we choose to wear but my subconscious says to me, you are in the office. However I dress could cause me to be harassed. I am wearing a long flowing skirt and I still get harassed, so if I now wear something that would expose me what would now come from that? I believe that if you want to look expensive, cover up. I was in a church one day which was my first time, I saw a particular dressing. I asked someone if it was normal to dress that way and he said yes it is personal choice. I know that God looks at your heart and not your dressing, but how does it make the other person feel, do or say about your dressing? It now goes beyond personal rights, Is it culture confirmed? Is it culture allowed? Would people see you and insult you? If you go to the market dressed inappropriately and get stoned at or insulted, if you report the case to the police or any body, the first thing your lawyer will ask is why did you dress that way? Bukky Karibi Whyte I have a problem with that. I have heard different situations of women being sexually harassed and then it goes, why did you wear a skirt? But when dressing now breeds violence, I no longer blame dressing. It is you as a person that is displaying the violence. You have a problem. Funke Ajomale But I still feel that it is always best to erase that particular notion from the beginning. I was wearing a long dress at work and I still got harassed. It is a human right thing to wear whatever you can afford. But if I am going somewhere then I think I should be covered, it doesn’t mean I should be over the top covered but then I should be comfortable and should be able to presume the right image. Bukky Karibi Whyte When Cossy first came into the entertainment industry, a lot of us gasped. But I think if she’s outside the entertainment world, she will dress differently.


that handles flare well and draws nice sun-stars, the sun will serve as a wonderful compositional element in your images. To get those sun-stars to appear, you would need to stop down your lens to a very small aperture such as f/11 or f/16. If you see flare and ghosting, you can use a great trick described in detail in Nasim’s article on eliminating ghosting and flare in landscape photography. If you are comfortable with image blending in post, there is another great technique to avoid over-exposure and diffraction: shoot two images – one for the sun at f/16 and one for the foreground and background at a larger aperture like f/8. Then combine the two images in post and use simple blending techniques with layers to bring those sun-stars into your image. Also, consider if filters (such as CPL, UV or ND) are helpful in any way when shooting against the sun. If not, detach them, as they could make things worse in terms of additional ghosting and flare. If you do use filters, make sure that they are of high quality and have multi-coating applied to them. For more details about lens filters, see Nasim’s article on lens filters and also check out his must-have filters for landscape photography article. 6) Make Use of Frost White frost can turn almost anything into a very attractive subject. Paradoxically, that is exactly what makes it difficult to photograph. With a thin layer of frost covering everything, landscape looks like a fairy tale, which may obscure the focus of the photographer for a good composition. I personally live in an area where the combination of freezing frost and blue sky is relatively rare. So when I got it earlier in January of this year, I got totally excited – and out of excitement I forgot to turn on VR on my lenses. When I discovered that, I was at first angry at myself, but then I took it as a good sign that I should take my time and focus on what I am doing, rather than let my excitement take over and ruin my photographs. Good composition and framing should always be your priority, but do not underestimate other variables that come into play while shooting, whether it has to do with proper exposure, focusing, depth of field or simpler things related to your camera settings. 9) Try Black and White Photography Even if I really enjoy the winter color palette, snow and frost often create handy conditions for black and white (B&W) photographs.


We consider the potentials of the LHC and a linear e^+e^- collider (LC) for discovering supersymmetric particles in variants of the MSSM with soft supersymmetry-breaking mass parameters constrained to be universal at the GUT scale (CMSSM) or at some lower scale M_{in} (GUT-less models), as may occur in some scenarios with mirage unification. Whereas the LHC should be able to discover squarks and/or gluinos along all the CMSSM coannihilation strip where the relic neutralino LSP density lies within the range favoured for cold dark matter, many GUT-less models could escape LHC detection. In particular, if M_{in} < 10^{11} GeV, the LHC would not detect sparticles if the relic density lies within the favoured range. For any given discovery of supersymmetry at the LHC, in such GUT-less models the lightest neutralino mass and hence the threshold for sparticle pair production at a LC increases as M_{in} decreases, and the CMSSM offers the best prospects for measuring sparticles at a LC. For example, if the LHC discovers sparticles with 1 fb^{-1} of data, within the CMSSM a centre-of-mass energy of 600 GeV would suffice for a LC to to produce pairs of neutralinos, if they provide the cold dark matter, whereas over 1 TeV might be required in a general GUT-less model. These required energies increase to 800 GeV in the CMSSM and 1.4 TeV in GUT-less models if the LHC requires 10 fb^{-1} to discover supersymmetry.


(1) of section 402(e) of such Code (relating to alternate payee under qualified domestic relations order treated as distributee) is amended by inserting ``or a qualified child abuse order (as defined in section 414(p))'' after ``a qualified domestic relations order (as defined in section 414(p))'' each place it appears. (2) Allocation of investment in the contract.--Paragraph (10) of section 72(m) of such Code (relating to determination of investment in the contract in the case of qualified domestic relations orders) is amended-- (A) in the heading, by inserting ``and qualified child abuse orders'' after ``qualified domestic relations orders''; and (B) by inserting ``or a qualified child abuse order (as defined in section 414(p))'' after ``a qualified domestic relations order (as defined in section 414(p))''. (3) Clarification of eligibility of participant for lump sum treatment.-- (A) Subparagraph (H) of section 402(d)(4) of such Code (relating to balance to credit of employee not to include amounts payable under qualified domestic relations order) is amended-- (i) in the heading, by inserting ``or qualified child abuse order'' after ``qualified domestic relations order''; and (ii) by inserting ``or a qualified child abuse order (within the meaning of section 414(p))'' after ``a qualified domestic relations order (within the meaning of section 414(p))''. (B) Subparagraph (J) of section 402(d)(4) of such Code is amended by inserting ``, or under a qualified child abuse order (within the meaning of section 414(p)) of the balance to the credit of an alternate payee,'' after ``former spouse of the employee''. SEC. 4. EFFECTIVE DATE. The amendments made by this Act shall take effect on January 1, 1996, except that, in the case of a child abuse order entered before such date, the plan administrator-- (1) shall treat such order as a qualified child abuse order if such administrator is paying benefits pursuant to such order on such date, and (2) may treat any other such order entered before such date as a qualified child abuse order even if such order does not meet the requirements of such amendments.


in the Treasury not otherwise appropriated, the Secretary of the Treasury shall transfer to the Secretary to carry out this paragraph $1,000,000, to remain available until expended. ``(B) Receipt and acceptance.--The Secretary shall be entitled to receive, shall accept, and shall use to carry out this paragraph the funds transferred under subparagraph (A), without further appropriation. ``(f) Study and Report.-- ``(1) In general.--The Secretary, in conjunction with the Director of the Centers for Disease Control and Prevention, shall prepare a report on the implementation, strength, and effectiveness of the local wellness policies carried out in accordance with this section. ``(2) Study of local wellness policies.--The study described in paragraph (1) shall include-- ``(A) an analysis of the strengths and weaknesses of local wellness policies and how the policies compare with model local wellness policies recommended under subsection (e)(2)(A)(ii); and ``(B) an assessment of the impact of the local wellness policies in addressing the requirements of subsection (b). ``(3) Report.--Not later than January 1, 2014, the Secretary shall submit to the Committee on Agriculture, Nutrition, and Forestry of the Senate and the Committee on Education and Labor of the House of Representatives a report that describes the findings of the study.''. SEC. 4. REPEAL. Section 204 of the Child Nutrition and WIC Reauthorization Act of 2004 (42 U.S.C. 1751 note; Public Law 108-265) is repealed. SEC. 5. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.


provide substantial financial and technical assistance directly to CSAs from individual- or family-operated farms; ``(B) CSAs from individual- or family-operated farms; ``(C) the expansion of CSAs into underserved communities; ``(D) CSAs operated by or employing veterans (as defined in section 101 of title 38, United States Code); and ``(E) the development, improvement, or expansion of innovative delivery and distribution programs that stimulate consumer interest in CSA participation. ``(f) Funding.-- ``(1) In general.--Of the funds of the Commodity Credit Corporation, the Secretary shall use to carry out this section-- ``(A) $10,000,000 for fiscal year 2012; ``(B) $12,000,000 for each of fiscal years 2013 through 2015; and ``(C) $15,000,000 for each fiscal years 2016 through 2018. ``(2) Interdepartmental coordination.--In carrying out this subsection, the Secretary shall ensure, to the maximum extent practicable, coordination between the applicable agencies.''. SEC. 3. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee, provided that such statement has been submitted prior to the vote on passage.


To study the Reynolds stresses which describe turbulent momentum transport from turbulence affected by large-scale shear and rotation. Three-dimensional numerical simulations are used to study turbulent transport under the influences of large-scale shear and rotation in homogeneous, isotropically forced turbulence. We study three cases: one with only shear, and two others where in addition to shear, rotation is present. These cases differ by the angle (0 or 90\degr) the rotation vector makes with respect to the z-direction. Two subsets of runs are performed with both values of \theta where either rotation or shear is kept constant. When only shear is present, the off-diagonal stress can be described by turbulent viscosity whereas if the system also rotates, nondiffusive contributions (\Lambda-effect) to the stress can arise. Comparison of the direct simulations are made with analytical results from a simple closure model. We find that the turbulent viscosity is of the order of the first order smoothing result in the parameter regime studied and that for sufficiently large Reynolds numbers the Strouhal number, describing the ratio of correlation to turnover times, is roughly 1.5. This is consistent with the closure model based on the minimal tau-approximation which produces a reasonable fit to the simulation data for similar Strouhal numbers. In the cases where rotation is present, separating the diffusive and nondiffusive components of the stress turns out to be challenging but taking the results at face value, we can obtain nondiffusive contributions of the order of 0.1 times the turbulent viscosity. We also find that the simple closure model is able to reproduce most of the qualitative features of the numerical results provided that the Strouhal number is of the order of unity.


The ISM is governed by supersonic turbulence on a range of scales. We use this to develop a rigorous excursion-set model for the formation and time evolution of dense gas structures (GMCs, massive clumps, and cores). Supersonic turbulence drives the density distribution to a lognormal with dispersion increasing with Mach number; we generalize this to include scales >h (the disk scale height), and use it to construct the statistical properties of the density field smoothed on a scale R. We then compare conditions for self-gravitating collapse including thermal, turbulent, and rotational support. We show this becomes a well-defined barrier crossing problem. As such, an exact 'bound object mass function' can be derived, from scales of the sonic length to above the disk Jeans mass. This agrees remarkably well with observed GMC mass functions in the MW and other galaxies; the only inputs are the mass and size of the galaxies (to normalize the model). This explains the mass function cutoff and its power-law slope (close to, but shallower than, -2). The model also predicts the linewidth-size and size-mass relations of clouds and the dependence of their residuals on surface density/pressure. We use this to predict the spatial correlation function/clustering of clouds and star clusters; these also agree well with observations. We predict the size/mass function of ISM 'bubbles' or 'holes', and show this can account for observed HI hole distributions without any local feedback. We generalize the model to construct time-dependent 'merger/fragmentation trees' which can be used to follow cloud evolution and construct semi-analytic models for the ISM. We provide explicit recipes to construct the trees. We use a simple example to show that, if clouds are not destroyed in ~1-5 crossing times, then all ISM mass would be trapped in collapsing objects even if the large-scale turbulence were maintained.


and Culture shall be subject to the audit requirements of section 5134(f)(2) of title 31, United States Code, with regard to the amounts received under subsection (b). (d) Limitation.--Notwithstanding subsection (a), no surcharge may be included with respect to the issuance under this Act of any coin during a calendar year if, as of the time of such issuance, the issuance of such coin would result in the number of commemorative coin programs issued during such year to exceed the annual 2 commemorative coin program issuance limitation under section 5112(m)(1) of title 31, United States Code. The Secretary of the Treasury may issue guidance to carry out this subsection. SEC. 8. FINANCIAL ASSURANCES. The Secretary shall take such actions as may be necessary to ensure that-- (1) minting and issuing coins under this Act will not result in any net cost to the United States Government; and (2) no funds, including applicable surcharges, are disbursed to any recipient designated in section 7 until the total cost of designing and issuing all of the coins authorized by this Act is recovered by the United States Treasury, consistent with sections 5112(m) and 5134(f) of title 31, United States Code. SEC. 9. BUDGET COMPLIANCE. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Committee on the Budget of the House of Representatives, provided that such statement has been submitted prior to the vote on passage.


(Abridged) We demonstrate that the tenet of hierarchical structure growth leads directly to a robust, falsifiable prediction for the correlation between stellar fraction (fstar) and total system mass (M500) of galaxy groups and clusters. This prediction is relatively insensitive to the details of baryonic physics or cosmological parameters. In particular, if the fstar-M500 relation is fixed and does not evolve with redshift, CDM models predict the logarithmic slope of this relation to be b>-0.3. This constraint can be weakened if the fstar-M500 relation evolves strongly, but this implies more stars must be formed in situ in groups at low redshift. Conservatively requiring that at least half the stars in groups were formed by z=1, the constraint from evolution models is b>-0.35. Since the most massive clusters (M500=1E15 Msun) are observed to have fstar=0.01, this means that groups with M500=5E13 Msun must have fstar<0.03. Recent observations by Gonzalez et al. (2007) indicate a much steeper relation, with fstar>0.04 in groups, leading to b=-0.64. If confirmed, this would rule out hierarchical structure formation models: today's clusters could not have been built from today's groups, or even from the higher-redshift progenitors of those groups. We perform a careful analysis of these and other data to identify the most important systematic uncertainties in their measurements. Although correlated uncertainties on stellar and total masses might explain the steep observed relation, the data are only consistent with theory if the observed group masses are systematically underestimated.


Remember the new Play Store "My Apps" screen layout that we spotted in testing in a dogfood version in February? Well, that appears to be rolling out more widely now, possibly even to everyone. You may need to clear the Play Store's app data and restart it to see the change (which might revert you back to the old lime green color for a bit before it switches back to the new darker green, thought I'd warn you), but it should be working for everyone now based on the number of tips we've received and on testing with our own devices. The new "Installed" tab has multiple sorting methods. The new layout gives Updates their own tab in the My apps and games screen, renames All to Library, and gives you several sorting methods for the Installed apps (alphabetical, last updated, last used, and size). "Beta" is still there (left). "Library" has quick buttons to install or remove an app from your account (right). There are a couple of other benefits too. One is that it's now easier to update certain apps only, since the Update button is clickable instead of requiring you to open the app's page first then tap on update. Two is that installing apps from your account is more obvious thanks to a new Install button, so you don't need to tap and hold to select multiple apps anymore, you can just scroll and install whichever ones you want. And three is that you can refresh to check for updates instead of having to leave the Play Store and launch it again to trigger a check. It's easier to update apps one by one (left) and new refresh to check for updates button (right). Overall, there are plenty of benefits to this new layout and, as far as I can tell, no drawbacks at all. App addicts should find most of the changes very helpful. The new layout wasn't showing up for me when I opened the Play Store, but as I said at the start of the article, I cleared data and that triggered the new look. It doesn't seem to require the newest version of the Play Store either (I'm on 7.7.08) so you might as well try it with whatever version you're running now to see if it works before updating to the newest one.


We model the dynamical structure of M87 (NGC4486) using high spatial resolution long-slit observations of stellar light in the central regions, two-dimensional stellar light kinematics out to half of the effective radius, and globular cluster velocities out to 8 effective radii. We simultaneously fit for four parameters, black hole mass, dark halo core radius, dark halo circular velocity, and stellar mass-to-light ratio. We find a black hole mass of 6.4(+-0.5)x10^9 Msun(the uncertainty is 68% confidence marginalized over the other parameters). The stellar M/L_V=6.3+-0.8. The best-fitted dark halo core radius is 14+-2 kpc, assuming a cored logarithmic potential. The best-fitted dark halo circular velocity is 715+-15 km/s. Our black hole mass is over a factor of 2 larger than previous stellar dynamical measures, and our derived stellar M/L ratio is 2 times lower than previous dynamical measures. When we do not include a dark halo, we measure a black hole mass and stellar M/L ratio that is consistent with previous measures, implying that the major difference is in the model assumptions. The stellar M/L ratio from our models is very similar to that derived from stellar population models of M87. The reason for the difference in the black hole mass is because we allow the M/L ratio to change with radius. The dark halo is degenerate with the stellar M/L ratio, which is subsequently degenerate with the black hole mass. We argue that dynamical models of galaxies that do not include the contribution from a dark halo may produce a biased result for the black hole mass. This bias is especially large for a galaxy with a shallow light profile such as M87, and may not be as severe in galaxies with steeper light profiles unless they have a large stellar population change with radius.


Adele’s win over Beyoncé for Album of the Year drew criticism from a swath of viewers and artists, including Adele herself. Herbie Hancock, who won the award in 2008, is the category’s last black winner, but despite this fact—and the criticism of the Grammys that stems from it—Recording Academy President Neil Portnow said today in an interview with Pitchfork that Grammy voters don’t see race, and neither should listeners. Portnow defended the Academy’s votes, arguing that its 14,000 members are “the highest level of professionals in the industry.” Thus, he reasoned, “I don’t think there’s a race problem at all”: We don’t, as musicians, in my humble opinion, listen to music based on gender or race or ethnicity. When you go to vote on a piece of music—at least the way that I approach it—is you almost put a blindfold on and you listen. It’s a matter of what you react to and what in your mind as a professional really rises to the highest level of excellence in any given year. And that is going to be very subjective. That’s what we ask our members to do, even in the ballots. We ask that they not pay attention to sales and marketing and popularity and charts. You have to listen to the music. So of the 14,000 voters, they listen, they make up their minds, and then they vote. To further make his case, Portnow pointed to Chance the Rapper’s Best New Artist win as proof of the Academy’s diversity: “You don’t get Chance the Rapper as the Best New Artist of the year if you have a membership that isn’t diverse and isn’t open-minded and isn’t really listening to the music.” Portnow omits Chance is just one of five to win it since 1999. Lauryn Hill’s The Miseducation of Lauryn Hill won Album of the Year in 1999, the last time that award was won by a black woman. Portnow’s main argument is the Academy’s size means it is diverse. But the Academy does not release the exact demographics of its voter base, nor does it seem like it’s planning to, and one must wonder if the data really would back up his claim.


were replaced by Westerners who were deemed to know better, and many felt that the community spirit that had fostered under communism had quickly evaporated under capitalism. "The social cohesion from East Germany, most people here actually miss that feeling," according to 47-year-old Ingo Wobst, a Dresden resident who has seen many friends switch from the center-left SPD to the AfD. Ingo Wobst HC Plambeck / for NBC News "After the fall of the wall, life in the countryside was pulsating, but then a lot of things collapsed," he says, sitting in a cafe across town in Dresden's trendy, graffiti-daubed Neustadt neighborhood. "Many people lost their jobs, and today you find small towns out here where there is no supermarket, no doctor and not even a bus stop." The city of Dresden itself is actually flourishing, emerging as a rival tourist destination to nearby Leipzig or even Berlin. In recent years it's become known as the home of another far-right group, PEGIDA — for Patriotic Europeans Against the Islamisation of the West — which attracted 25,000 people to a demonstration in early 2015. But many of the marchers were not from Dresden but from the surrounding towns and villages, according to Richter. The AfD has found most traction in such rural areas, which are emptying out because of "brain drain" — the emigration of educated and trained people — and low birth rates. If East Germany were still a country, it would have the oldest population in Europe. "In a big city you have more work and the young people come here because of it," says Victoria Prokudin, a 20-year-old trainee lawyer who moved to Dresden from the surrounding countryside. Victoria Prokudin HC Plambeck / for NBC News Even those who feel little nostalgia for communism balk at the idea that Germany is universally happy now that it's a single country. Later that night, around 30 minutes' drive west of Bitterfeld-Wolfen, Roi gathered with AfD compatriots in the small town of Köthen. Around half a dozen sympathizers and supporters were clustered in the unlikely setting of a restaurant called Schwarzes Ross, meaning Black Steed. A large painting of a horse dominates the back wall, accompanied by horse-themed clocks, ornamental plates and coasters — decorations that seem a bit macabre given that horse meat is on the menu.


It is shown that if, from the starting point of a universal rank-one mass matrix long favoured by phenomenologists, one adds the assumption that it rotates (changes its orientation in generation space) with changing scale, one can reproduce, in terms of only 6 real parameters, all the 16 mass ratios and mixing parameters of quarks and leptons. Of these 16 quantities so reproduced, 10 for which data exist for direct comparison (i.e. the CKM elements including the CP-violating phase, the angles $\theta_{12}, \theta_{13}, \theta_{23}$ in $\nu$-oscillation, and the masses $m_c, m_\mu, m_e$) agree well with experiment, mostly to within experimental errors; 4 others ($m_s, m_u, m_d, m_{\nu_2}$), the experimental values for which can only be inferred, agree reasonably well; while 2 others ($m_{\nu_1}, \delta_{CP}$ for leptons), not yet measured experimentally, remain as predictions. In addition, one gets as bonuses, estimates for (i) the right-handed neutrino mass $m_{\nu_R}$ and (ii) the strong CP angle $\theta$ inherent in QCD. One notes in particular that the output value for $\sin^2 2 \theta_{13}$ from the fit agrees very well with recent experiments. By inputting the current experimental value with its error, one obtains further from the fit 2 new testable constraints: (i) that $\theta_{23}$ must depart from its "maximal" value: $\sin^2 2 \theta_{23} \sim 0.935 \pm 0.021$, (ii) that the CP-violating (Dirac) phase in the PMNS would be smaller than in the CKM matrix: of order only $|\sin \delta_{CP}| \leq 0.31$ if not vanishing altogether.


, and elsewhere to encourage an international effort to ensure readiness for the Year 2000 at banks and other financial institutions; and (2) the initiatives which the representatives of the United States to the International Monetary Fund, International Bank for Development and Reconstruction, and other international development banks are taking to engage such institutions in providing funding or technical assistance to developing countries for remedying the Year 2000 computer problem in such countries. SEC. 6. QUARTERLY PROGRESS REPORTS REQUIRED. (a) In General.--Beginning after the submission of the report on the national assessment and strategy under sections 4 and 5, the Chairperson of the Year 2000 Conversion Council shall submit a quarterly report to the Congress on the progress that has been made since the submission of the prior report in solving the Year 2000 computer problem in all critical infrastructures and key sectors of the economy and in developing a contingency plan. (b) Final Report.--The final report submitted under subsection (a) shall assess the ongoing Year 2000 and other date-related problems that will occur in the future as temporary Year 2000 renovations lapse or other fail dates occur in computer systems. (c) Sunset.--No reports shall be required under subsection (a) after December 31, 2001. SEC. 7. REVISION OF FEDERAL ACQUISITION REGULATION TO PROVIDE FOR CERTAIN PENALTIES FOR CONTRACTORS THAT VIOLATE YEAR 2000 REQUIREMENT. In the case of any person who enters into a contract with a Federal agency, and who knowingly provides goods or services to the agency under the contract that are not Year 2000 compliant (as that term is defined in section 39.002 of the Federal Acquisition Regulation, as adopted on August 22, 1997), the Federal Acquisition Regulation may be revised to provide for an appropriate period for which such person shall not be eligible for award of any contract by any Federal agency. Any restrictions developed pursuant to this section may, at the discretion of the applicable Federal agency, be waived if the new goods or services are Year 2000 compliant.


Mayall II = G1 is one of the most luminous globular clusters (GCs) in M31. Here, we determine its age and mass by comparing multicolor photometry with theoretical stellar population synthesis models. Based on far- and near-ultraviolet GALEX photometry, broad-band UBVRI, and infrared JHK_s 2MASS data, we construct the most extensive spectral energy distribution of G1 to date, spanning the wavelength range from 1538 to 20,000 A. A quantitative comparison with a variety of simple stellar population (SSP) models yields a mean age that is consistent with G1 being among the oldest building blocks of M31 and having formed within ~1.7 Gyr after the Big Bang. Irrespective of the SSP model or stellar initial mass function adopted, the resulting mass estimates (of order $10^7 M_\odot$) indicate that G1 is one of the most massive GCs in the Local Group. However, we speculate that the cluster's exceptionally high mass suggests that it may not be a genuine GC. We also derive that G1 may contain, on average, $(1.65\pm0.63)\times10^2 L_\odot$ far-ultraviolet-bright, hot, extreme horizontal-branch stars, depending on the SSP model adopted. On a generic level, we demonstrate that extensive multi-passband photometry coupled with SSP analysis enables one to obtain age estimates for old SSPs to a similar accuracy as from integrated spectroscopy or resolved stellar photometry, provided that some of the free parameters can be constrained independently.


Flash memory is a non-volatile computer memory comprised of blocks of cells, wherein each cell can take on q different values or levels. While increasing the cell level is easy, reducing the level of a cell can be accomplished only by erasing an entire block. Since block erasures are highly undesirable, coding schemes - known as floating codes or flash codes - have been designed in order to maximize the number of times that information stored in a flash memory can be written (and re-written) prior to incurring a block erasure. An (n,k,t)_q flash code C is a coding scheme for storing k information bits in n cells in such a way that any sequence of up to t writes (where a write is a transition 0 -> 1 or 1 -> 0 in any one of the k bits) can be accommodated without a block erasure. The total number of available level transitions in n cells is n(q-1), and the write deficiency of C, defined as \delta(C) = n(q-1) - t, is a measure of how close the code comes to perfectly utilizing all these transitions. For k > 6 and large n, the best previously known construction of flash codes achieves a write deficiency of O(qk^2). On the other hand, the best known lower bound on write deficiency is \Omega(qk). In this paper, we present a new construction of flash codes that approaches this lower bound to within a factor logarithmic in k. To this end, we first improve upon the so-called "indexed" flash codes, due to Jiang and Bruck, by eliminating the need for index cells in the Jiang-Bruck construction. Next, we further increase the number of writes by introducing a new multi-stage (recursive) indexing scheme. We then show that the write deficiency of the resulting flash codes is O(qk\log k) if q \geq \log_2k, and at most O(k\log^2 k) otherwise.


If you're on a budget, chances are that you've debated a purchase between an older flagship and a newer mid-ranger. Do you want a Moto G4, or a Moto X Pure? A Galaxy Note5 or a Galaxy S7? For those of you who prefer buying powerful last-gen hardware, Newegg has got a deal for you: two Benjamins will get you a ZTE Axon Pro with a sizable 64GB of storage. When the Axon Pro was new, it packed some pretty competitive hardware: a 5.5-inch 1440p LCD display, a Snapdragon 810 (which reportedly performs decently in the Axon Pro), 4GB of RAM, 64GB of internal storage, dual rear cameras (13MP + 2MP), and a 3000mAh battery. It also has great audio, both through the headphone jack and through its front-facing speaker (only one is for audio). Virtually its only downfall in this regard is its lack of a microSD slot, but 64GB should be perfectly serviceable for most. The Axon Pro also comes with two noteworthy extras: a set of JBL E13 in-ear headphones, and ZTE's fantastic Passport 2.0 warranty, which you can see details of above. Want a 64GB Axon Pro of your very own for the low, low price of $200? Well, you're limited to the gold color (which you'll use discount code 0210CLS03 to get to from $249.99), and the discount will end around six hours from the time of this article's publishing. If you don't think you need 64GB, you can get the "Phthalo Blue" 32GB variant for $176 with the same code (it's probably worth it to get the 64GB variant for $24 more). Should you not need specs that powerful, you can get a lower-end 32GB Axon in that same Phthalo Blue with a 5.5" 1080p panel, a Snapdragon 801, 2GB of RAM, and 32GB of internal storage for just $128 with the same discount code. It'll come with the same JBL headphones and the same Passport 2.0 warranty. Again, these prices will expire in roughly six hours, so don't wait up if you're interested.


If a deer fawn is found alone in the woods, leave it there, advises a state wildlife biologist. Its mother has not abandoned it; she is probably nearby. Removing a fawn from the forest is also illegal because the animal is being taken outside the legal season for taking deer, which is the hunting season. “Many people who come upon a solitary spotted fawn in the woods or along a roadway mistakenly assume the animal has been deserted by its mother and want to take the apparently helpless creature home to care for it,” said Charles Ruth, Big Game Program coordinator for the S.C. Department of Natural Resources. “Young fawns like this have not been abandoned but are still in the care of a doe.” The apparently “helpless” deer fawns born during April, May and June in South Carolina will begin daily movements with their mothers in about three or four weeks. Human handling and disturbance of fawns can cause a doe to shy away or even desert her offspring. Also, a bleating response by the fawn can summon nearby predators. “It’s part of nature’s plan for a doe deer to leave her fawn or fawns alone for their first few weeks of life,” Ruth said. “The reason for this unusual maternal action is that the fawn at this age is better protected away from the doe. The presence of the doe nearby would attract predators because the doe lacks the protective coloration of the fawn, and the older and larger doe has a much stronger odor.” A fawn that appears abandoned is merely awaiting a visit from its mother, according to Ruth. A doe, after brief periods of feeding and grooming her fawn, will spend much of her day feeding and resting somewhat removed from her young. The fawn ordinarily stays bedded down as if sleeping, but will occasionally move short distances to new bedding sites. “Each spring and summer the SCDNR gets many calls from people who have discovered these ‘lost’ deer,” Ruth said. “Young fawns are without a doubt cute and cuddly, but if taken into captivity they grow into semi-tame adult deer that can become quite dangerous.” Adult buck deer, no matter how they were raised, are especially dangerous during the breeding season. Even does raised by humans are unpredictable. Occasionally, “tame” deer seriously injure people, according to Ruth, and in cases where the deer are a threat to humans, the deer sometimes have to be killed. People often ask the SCD