We present high quality long slit spectra along the major and minor axes out to 1.5-2 Re (14-22 kpc) of three bright elliptical galaxies (NGC1600, NGC4125, NGC7619) obtained at the Hobby-Eberly Telescope (HET). We derive stellar kinematic profiles and Lick/IDS indices (Hbeta, Mgb, Fe5015, Fe5270, Fe5335, Fe5406). Moreover, for NGC4125 we derive gas kinematics and emission line strengths. We model the absorption line strengths using Simple Stellar Populations models that take into account the variation of [\alpha/Fe] and derive ages, total metallicity and element abundances. Overall, we find that the three galaxies have old and [\alpha/Fe] overabundant stellar populations with no significant gradients. The metallicity is supersolar at the center with a strong negative radial gradient. For NGC4125, several pieces of evidence point to a recent dissipational merger event. We calculate the broad band color profiles with the help of SSP models. All of the colors show sharp peaks at the center of the galaxies, mainly caused by the metallicity gradients, and agree well with the measured colors. Using the Schwarzschild's axisymmetric orbit superposition technique, we model the stellar kinematics to constrain the dark halos of the galaxies. We use the tight correlation between the Mgb strength and local escape velocity to set limits on the extent of the halos by testing different halo sizes. Logarithmic halos - cut at 60 kpc -minimize the overall scatter of the Mgb-Vesc relation. Larger cutoff radii are found.


A drawing of a graph is said to be a {\em straight-line drawing} if the vertices of $G$ are represented by distinct points in the plane and every edge is represented by a straight-line segment connecting the corresponding pair of vertices and not passing through any other vertex of $G$. The minimum number of slopes in a straight-line drawing of $G$ is called the slope number of $G$. We show that every cubic graph can be drawn in the plane with straight-line edges using only the four basic slopes $\{0,\pi/4,\pi/2,-\pi/4\}$. We also prove that four slopes have this property if and only if we can draw $K_4$ with them. Given a graph $G$, an {\em obstacle representation} of $G$ is a set of points in the plane representing the vertices of $G$, together with a set of obstacles (connected polygons) such that two vertices of $G$ are joined by an edge if and only if the corresponding points can be connected by a segment which avoids all obstacles. The {\em obstacle number} of $G$ is the minimum number of obstacles in an obstacle representation of $G$. We show that there are graphs on $n$ vertices with obstacle number $\Omega({n}/{\log n})$. We show that there is an $m=2n+o(n)$, such that, in the Maker-Breaker game played on $\Z^d$ where Maker needs to put at least $m$ of his marks consecutively in one of $n$ given winning directions, Breaker can force a draw using a pairing strategy. This improves the result of Kruczek and Sundberg who showed that such a pairing strategy exits if $m\ge 3n$. A simple argument shows that $m$ has to be at least $2n+1$.


ICL is believed to originate from the stars stripped from cluster galaxies. They are no longer gravitationally bound to individual galaxies, but to the cluster, and their smooth distribution potentially makes them serve as much denser tracers of the cluster dark matter than the sparsely distributed cluster galaxies. We present our study of the ICL in Cl 0024+17 using both ACS and Subaru data, where we previously reported discovery of a ringlike dark matter structure with gravitational lensing. The ACS images provide much lower sky levels than ground data, and enable us to measure relative variation of surface brightness reliably. This analysis is repeated with the Subaru images to examine if consistent features are recovered despite different reduction scheme and instrumental characteristics. We find that the ICL profile clearly resembles the peculiar mass profile, which stops decreasing at r~50" (~265 kpc) and slowly increases until it turns over at r~75" (~397 kpc). This feature is seen in both ACS and Subaru images for nearly all available passband images while the features are stronger in red filters. The consistency across different filters and instruments strongly rules out the possibility that the feature might come from any residual, uncorrected calibration errors. In addition, our re-analysis of the cluster X-ray data shows that the peculiar mass structure is also indicated by a non-negligible bump in the intracluster gas profile when the geometric center of the dark matter ring, not the peak of the X-ray emission, is chosen as the center of the radial bin. The location of the gas ring is closer to the center by ~15" (~80 kpc), raising an interesting possibility that the ring-like structure is expanding and the gas ring is lagging behind perhaps because of the ram pressure.


Stored antiproton beams at the international FAIR facility will provide unique opportunities to study hyperons as well as antihyperons in nuclear systems. Precise $\gamma$-spectroscopy of multi-strange hypernuclei will serve as a laboratory for the hyperon-hyperon interaction. Exclusive hadron-antihadron pair production close to threshold can measure the potential of a antihadron relative to that of the coincident hadrons. In the present work we explore the production of excited states in double hypernuclei following the micro-canonical break-up of an initially excited double hypernucleus which is created by the absorption and conversion of a stopped $\Xi^{-}$ hyperon. Generally the formation of excited hypernuclear states relative to ground states dominates in this model. For different initial target nuclei which absorb the $\Xi^-$, different double hypernuclei nuclei dominate. We also compare the model predictions with the correlated pion spectra measured by the E906 collaboration. In antiproton nucleus reactions the event-by-event transverse momentum correlations of hadron-antihadron pairs produced close to threshold contain information on the difference between the nuclear potential of the hadron and the associated antihadron. For produced D-meson pairs at 6.7\gevc1 the sensitivity of the transverse momenta correlation will probably be to small to deduce differences between the potentials for D$^+$ and D$^-$ mesons. However, for {\PgX\PagX} pairs produced at 2.9\gevc1 the asymmetry is sufficiently sensitive to predicted differences between the {\PgX} and {\PagX} potentials even.


We present an interesting Sunyaev-Zel'dovich (SZ) detection in the first of the Arcminute Microkelvin Imager (AMI) 'blind', degree-square fields to have been observed down to our target sensitivity of 100{\mu}Jy/beam. In follow-up deep pointed observations the SZ effect is detected with a maximum peak decrement greater than 8 \times the thermal noise. No corresponding emission is visible in the ROSAT all-sky X-ray survey and no cluster is evident in the Palomar all-sky optical survey. Compared with existing SZ images of distant clusters, the extent is large (\approx 10') and complex; our analysis favours a model containing two clusters rather than a single cluster. Our Bayesian analysis is currently limited to modelling each cluster with an ellipsoidal or spherical beta-model, which do not do justice to this decrement. Fitting an ellipsoid to the deeper candidate we find the following. (a) Assuming that the Evrard et al. (2002) approximation to Press & Schechter (1974) correctly gives the number density of clusters as a function of mass and redshift, then, in the search area, the formal Bayesian probability ratio of the AMI detection of this cluster is 7.9 \times 10^4:1; alternatively assuming Jenkins et al. (2001) as the true prior, the formal Bayesian probability ratio of detection is 2.1 \times 10^5:1. (b) The cluster mass is MT,200 = 5.5+1.2\times 10^14h-1M\odot. (c) Abandoning a physical model with num- -1.3 70 ber density prior and instead simply modelling the SZ decrement using a phenomenological {\beta}-model of temperature decrement as a function of angular distance, we find a central SZ temperature decrement of -295+36 {\mu}K - this allows for CMB primary anisotropies, receiver -15 noise and radio sources. We are unsure.


Housing and Urban Development or any public housing agency pursuant to this section. ``(2) Eviction of nonelderly tenants having drug or alcohol use problems in housing designated for elderly families.--A tenant in a project (or portion of a project) that is designated under subsection (a)(1) for occupancy by only elderly families or by only elderly and disabled families shall be evicted under this paragraph if-- ``(A) the tenant's household includes a person described in clause (i) or (ii) of subsection (a)(5)(A); and ``(B) upon termination of the tenant's tenancy in the project, the public housing agency provides rental assistance under section 8 on behalf of the tenant.''. (b) Preference for Section 8 Assistance.-- (1) Certificates.--Section 8(d)(1)(A)(i) of the United States Housing Act of 1937 (42 U.S.C. 1437f(d)(1)(A)(i)) is amended by inserting after ``income for rent,'' the following: ``are required to be evicted under section 7(c)(2) if assistance under this section is provided on behalf of the family,''. (2) Vouchers.--The first sentence of section 8(o)(3)(B) of the United States Housing Act of 1937 (42 U.S.C. 1437f(o)(3)(B)) is amended by inserting after ``displaced,'' the following: ``are required to be evicted under section 7(c)(2).


We develop a model for stochastic pre-enrichment and self-enrichment in globular clusters (GCs) during their formation process. GCs beginning their formation have an initial metallicity determined by the pre-enrichment of their surrounding protocloud, but can also undergo internal self-enrichment during formation. Stochastic variations in metallicity arise because of the finite numbers of supernova. We construct an analytic formulation of the combined effects of pre-enrichment and self-enrichment and use Monte Carlo models to verify that the model accurately encapsulates the mean metallicity and metallicity spread among real GCs. The predicted metallicity spread due to self-enrichment alone, a robust prediction of the model, is much smaller than the observed spread among real GCs. This result rules out self-enrichment as a significant contributor to the metal content in most GCs, leaving pre-enrichment as the viable alternative. Self-enrichment can, however, be important for clusters with masses well above 10^6 Msun, which are massive enough to hold in a significant fraction of their SN ejecta even without any external pressure confinement. This transition point corresponds well to the mass at which a mass-metallicity relationship ("blue tilt") appears in the metal-poor cluster sequence in many large galaxies. We therefore suggest that self-enrichment is the primary driver for the mass-metallicity relation. Other predictions from our model are that the cluster-to-cluster metallicity spread decreases amongst the highest mass clusters; and that the red GC sequence should also display a more modest mass-metallicity trend.


We present a spectroscopic study of Leo V, a recently discovered satellite of the Milky Way (MW). From stellar spectra obtained with the MMT/Hectochelle spectrograph we identify seven likely members of Leo V. Five cluster near the Leo V center (R < 3 arcmin) and have velocity dispersion 2.4_{-1.4}^{+2.4} km/s. The other two likely members lie near each other but far from the center (R~13 arcmin ~ 700 pc) and inflate the global velocity dispersion to 3.7_{-1.4}^{+2.3} km/s. Assuming the five central members are bound, we obtain a dynamical mass of M=3.3_{-2.5}^{+9.1} x 10^5M_{sun} (M/L_V=75_{-58}^{+230}[M/L_V]_{sun}). From the stacked spectrum of the five central members we estimate a mean metallicity of [Fe/H]=-2.0\pm 0.2 dex. Thus with respect to dwarf spheroidals of similar luminosity, Leo V is slightly less massive and slightly more metal-rich. Since we resolve the central velocity dispersion only marginally, we do not rule out the possibility that Leo V is a diffuse star cluster devoid of dark matter. The wide separation of its two outer members implies Leo V is losing mass; however, its large distance (D ~ 180 kpc) is difficult to reconcile with MW tidal stripping.


902(2) of the Trade Sanctions Reform and Export Enhancement Act of 2000 (22 U.S.C. 7201(2)) is amended-- (i) by striking subparagraph (D); and (ii) by redesignating subparagraphs (E) and (F) as subparagraphs (D) and (E), respectively. SEC. 3. FEDERAL MILK MARKETING REFORM. (a) In General.--Not later than 180 days after the date of enactment of this Act, the Secretary of Agriculture shall conduct hearings to assess the implications of transitioning Federal milk marketing orders from end-product pricing to a competitive pay pricing system. (b) Requirements.--In conducting hearings under this section, the Secretary shall-- (1) ensure that market administrators conduct a thorough analysis of the reforms to the Federal milk marketing orders proposed by the Maine Dairy Industry Advisory Council and the reforms included in title II of the Dairy Security Act of 2011; (2) analyze the implications of transitioning from a 4- class system for milk products to a 2-class system; (3) explore methods to improve signals for price discovery in the short- and long-term to allow dairy producers to better use risk management tools; (4) assess whether a 2-class competitive pay pricing system for milk products would be more or less transparent than the system in effect as of the day before the date of enactment of this Act; and (5) analyze the impact of eliminating a minimum regulated price on price volatility in dairy markets. SEC. 4. BUDGETARY EFFECTS. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee.


The development of fast and accurate methods of photometric redshift estimation is a vital step towards being able to fully utilize the data of next-generation surveys within precision cosmology. In this paper we apply a specific approach to spectral connectivity analysis (SCA; Lee & Wasserman 2009) called diffusion map. SCA is a class of non-linear techniques for transforming observed data (e.g., photometric colours for each galaxy, where the data lie on a complex subset of p-dimensional space) to a simpler, more natural coordinate system wherein we apply regression to make redshift predictions. As SCA relies upon eigen-decomposition, our training set size is limited to ~ 10,000 galaxies; we use the Nystrom extension to quickly estimate diffusion coordinates for objects not in the training set. We apply our method to 350,738 SDSS main sample galaxies, 29,816 SDSS luminous red galaxies, and 5,223 galaxies from DEEP2 with CFHTLS ugriz photometry. For all three datasets, we achieve prediction accuracies on par with previous analyses, and find that use of the Nystrom extension leads to a negligible loss of prediction accuracy relative to that achieved with the training sets. As in some previous analyses (e.g., Collister & Lahav 2004, Ball et al. 2008), we observe that our predictions are generally too high (low) in the low (high) redshift regimes. We demonstrate that this is a manifestation of attenuation bias, wherein measurement error (i.e., uncertainty in diffusion coordinates due to uncertainty in the measured fluxes/magnitudes) reduces the slope of the best-fit regression line. Mitigation of this bias is necessary.


Newborn neutron stars surrounded by hyperaccreting and neutrino-cooled disks may exist in some gamma-ray bursts (GRBs) and/or supernovae (SNe). In this paper we further study the structure of such a neutron-star disk based on the two-region (i.e., inner & outer) disk scenario following our previous work, and calculate the neutrino annihilation luminosity from the disk in various cases. We investigate the effects of the viscosity parameter, energy parameter (measuring the neutrino cooling efficiency of the inner disk) and outflow strength on the structure of the entire disk as well as the effect of emission from the neutron star surface boundary emission on the total neutrino annihilation rate. The inner disk satisfies the entropy-conservation or the advection-dominated self-similar structure depending on the energy parameter. An outflow from the disk decreases the density and pressure but increases the thickness of the disk. Moreover, compared with the black-hole disk, the neutrino annihilation luminosity above the neutron-star disk is higher, and the neutrino emission from the boundary layer could increase the neutrino annihilation luminosity by about one order of magnitude higher than the disk without boundary emission. The neutron-star disk with the advection-dominated inner disk could produce the highest neutrino luminosity while the disk with an outflow has the lowest. Although a heavily mass-loaded outflow from the neutron star surface at early times of neutron star formation prevents the outflow material from being accelerated to a high bulk Lorentz factor, an energetic ultrarelativistic jet via neutrino annihilation can be produced above the stellar polar region at late times.


In this paper, we study the average case complexity of the Unique Games problem. We propose a natural semi-random model, in which a unique game instance is generated in several steps. First an adversary selects a completely satisfiable instance of Unique Games, then she chooses an epsilon-fraction of all edges, and finally replaces ("corrupts") the constraints corresponding to these edges with new constraints. If all steps are adversarial, the adversary can obtain any (1-epsilon) satisfiable instance, so then the problem is as hard as in the worst case. In our semi-random model, one of the steps is random, and all other steps are adversarial. We show that known algorithms for unique games (in particular, all algorithms that use the standard SDP relaxation) fail to solve semi-random instances of Unique Games. We present an algorithm that with high probability finds a solution satisfying a (1-delta) fraction of all constraints in semi-random instances (we require that the average degree of the graph is Omega(log k). To this end, we consider a new non-standard SDP program for Unique Games, which is not a relaxation for the problem, and show how to analyze it. We present a new rounding scheme that simultaneously uses SDP and LP solutions, which we believe is of independent interest. Our result holds only for epsilon less than some absolute constant. We prove that if epsilon > 1/2, then the problem is hard in one of the models, the result assumes the 2-to-2 conjecture. Finally, we study semi-random instances of Unique Games that are at most (1-epsilon) satisfiable. We present an algorithm that with high probability, distinguishes between the case when the instance is a semi-random instance and the case when the instance is an (arbitrary) (1-delta) satisfiable instance.


We present the results of SiO millimeter-line observations of a sample of known SiO maser sources covering a wide dust-temperature range. A cold part of the sample was selected from the SiO maser sources found in our recent SiO maser survey of cold dusty objects. The aim of the present research is to investigate the causes of the correlation between infrared colors and SiO maser intensity ratios among different transition lines. In particular, the correlation between infrared colors and SiO maser intensity ratio among the J=1-0 v=1, 2, and 3 lines are mainly concerned in this paper. We observed in total 75 SiO maser sources with the Nobeyama 45m telescope quasi-simultaneously in the SiO J=1-0 v=0, 1, 2, 3, 4 and J=2-1 v=1, 2 lines. We also observed the sample in the 29SiO J=1-0 v=0 and J=2-1 v=0, and 30SiO J=1-0 v=0 lines, and the H2O 6(1,6)-5(2,3) line. As reported in previous papers, we confirmed that the intensity ratios of the SiO J=1-0 v=2 to v=1 lines clearly correlate with infrared colors. In addition, we found possible correlation between infrared colors and the intensity ratios of the SiO J=1-0 v=3 to v=1&2 lines. Two overlap lines of H2O (i.e., 11(6,6) nu_2=1 -> 12(7,5) nu_2=0 and 5(0,5) nu_2=2 -> 6(3,4) nu_2=1) might explain these correlation if these overlap lines become stronger with increase of infrared colors, although the phenomena also might be explained by more fundamental ways.


Then that Federal department or agency head shall publish an explanation of such continued use in the Federal Register. SEC. 4. APPLICATION. This Act shall not apply to regulations, guidelines, or recommendations related to medical research. SEC. 5. DEFINITIONS. For purposes of this Act: (1) Animal.--The term ``animal'' means any vertebrate. (2) Animal acute toxicity test.--The term ``animal acute toxicity test'' means an acute toxicity test on animals, including (but not limited to) the Draize eye or skin irritancy test, LD-50 test, approximate lethal dose test, and the limit test. (3) Federal department or agency head.--The term ``Federal department or agency head'' means the head of a Federal department or agency who-- (A) has authority to promulgate regulations, guidelines, and recommendations with respect to procedures to be used in the safety testing by manufacturers of products, including consumer products, veterinary products, and products containing hazardous or toxic substances; or (B) licenses or approves products, labeling requirements or the transportation of products based on the results of these tests. (4) Medical research.--The term ``medical research'' means research, including research performed using biotechnology, related to the causes, diagnosis, treatment, or control of physical or mental impairments of humans or animals. The term does not include the testing of a product to determine its toxicity for the purpose of complying with protocols, recommendations, or guidelines for testing required, recommended, or accepted by a Federal regulatory agency for a product introduced in commerce. (5) Nonanimal acute toxicity test.--The term ``nonanimal acute toxicity test'' means an acute toxicity test not conducted on animals. Such tests include (but are not limited to) cell culture, computer modeling, protein alteration, and chorioallantoic membrane techniques.


Observations of an optical source coincident with gravitational wave emission detected from a binary neutron star coalescence will improve the confidence of detection, provide host galaxy localisation, and test models for the progenitors of short gamma ray bursts. We employ optical observations of three short gamma ray bursts, 050724, 050709, 051221, to estimate the detection rate of a coordinated optical and gravitational wave search of neutron star mergers. Model R-band optical afterglow light curves of these bursts that include a jet-break are extrapolated for these sources at the sensitivity horizon of an Advanced LIGO/Virgo network. Using optical sensitivity limits of three telescopes, namely TAROT (m=18), Zadko (m=21) and an (8-10) meter class telescope (m=26), we approximate detection rates and cadence times for imaging. We find a median coincident detection rate of 4 yr^{-1} for the three bursts. GRB 050724 like bursts, with wide opening jet angles, offer the most optimistic rate of 13 coincident detections yr^{-1}, and would be detectable by Zadko up to five days after the trigger. Late time imaging to m=26 could detect off-axis afterglows for GRB 051221 like bursts several months after the trigger. For a broad distribution of beaming angles, the optimal strategy for identifying the optical emissions triggered by gravitational wave detectors is rapid response searches with robotic telescopes followed by deeper imaging at later times.


There are a number of areas you need to focus on to make sure all of your upgrades are in sync with each other when it comes time to push the limits of their individual capabilities. For example, if you are upgrading your suspension, the wheels and tires had better be able to handle the new g-forces the car will exhibit in the corners. Planning on adding a supercharger, turbo system, or just upping the ante in cubic inches? You’d better hope that the transmission is up to handling the task. We’re here to tell you that PerformaBuilt Transmissions has one goal in mind: to engineer and build the toughest transmission on the planet, and they’ve proved so not only with their updated designs but also through their pledge of quality, performance, and unparalleled customer service. All of their transmissions are dyno-tested at their production facility and delivered to your door ready to install with a rock-solid warranty with no exceptions for racing or mileage. On a recent visit, the team was preparing one of their Level 3 Invincible 4L60E units, which is one of their strongest models designed for extreme performance. Packed with upgrades, it features a bevy of modifications making it capable of handling up to 800 rwhp (rear-wheel horsepower), which is far more than the capabilities of a stock 4L60E, which is around 300 hp. Each unit is methodically re-engineered to overcome many of the inherent factory weaknesses by adding strength and durability. Some of the issues addressed include boosting line pressure from an OEM level of between 140-150 psi to 220 psi, and keeping the unit balanced to avoid “shift shock” (banging shifts) by tightening down clearances; this results in firm, quick shifts as driver input becomes more aggressive. From front to rear, upgrades include a BorgWarner 29-element dual-cage sprag assembly, Sonnax Smart Shell to eliminate the stripping of splines and breakage, a set of Raybestos carbon composite performance clutches with new Raybestos steels, and two Sonnax Super Hold billet servos for Second and Fourth gears for maximum hold to name but a few. Follow along and check out just what it takes to bring a stock 4L60E to the highest level of performance. CHP Source PerformaBuilt Transmissions 888.744.6542 performabuilt.com


Axed. The common thread among the three, besides zero playoff appearances? Ward, although it’s not all his fault, even if that’s a common sentiment among fans. There’s plenty of blame to go around, even beyond Eddie Lack. The Hurricanes have been too old when they needed to be younger, too young when they needed to be older and took far too long to assemble this group of talented players with untapped potential. Either way, the Hurricanes too often required something approaching perfection from Ward, and he could rarely deliver. And it was always Ward. Whether by default or design, Ward has been the main guy in net for this team for the past 11 years, in which the Hurricanes have made the playoffs once. All of the other contenders for the No. 1 job – most notably John Grahame, Anton Khudobin and Lack – turned out to be pretenders. If Lack were any good, this might have been a playoff team last spring. So now the Hurricanes try again, with Darling, whose record as a backup on one of the NHL’s best teams was stellar but who has never played more than 45 games in a season, and that when he was 19. The Hurricanes will probably need him to play at least 60, and play them well, not that Darling is taking that for granted. “Cam and I both want to play, and just because I showed up and signed here doesn’t mean, ‘Here you go, here’s 80 games,’ ” Darling said. But he will start Saturday’s opener against the Minnesota Wild, after missing his first scheduled preseason start with an undisclosed minor injury. In the two games he played after that, he was stellar: a 1.50 goals-against average and.925 save percentage. It’s foolish to draw sweeping conclusions from preseason because of the frequent talent disparity between game rosters, but those numbers are everything you’d expect from Darling. If he can deliver anything close to that in real games, it’ll be a different kind of season for the Hurricanes. And.


An election under subparagraph (A) shall-- ``(i) be made to the Settlement Trust in writing, and ``(ii) specify the percentage (not greater than 15 percent) of the distributions to be withheld. Such election may be revoked or modified with respect to distributions made after the revocation or modification. ``(6) Settlement trust.--For purposes of this section, the term `Settlement Trust' means a trust which constitutes a Settlement Trust under section 39 of the Alaska Native Claims Settlement Act (43 U.S.C. 1629e).'' (c) Reporting.--Section 6041 of such Code is amended by adding at the end the following new subsection: ``(f) Application to Alaska Settlement Trusts.--In the case of any distribution from a Settlement Trust (as defined in section 501(p)(6)) to a beneficiary, this section shall apply, except that-- ``(1) this section shall apply to such distribution without regard to the amount thereof, ``(2) the Settlement Trust shall include on any return or statement required by this section information as to the character of such distribution (if applicable) and the amount of tax imposed by chapter 1 deducted and withheld from such distribution, and ``(3) the filing of any return or statement required by this section shall satisfy any requirement to file any other form or schedule under this title with respect to distributive share information (including any form or schedule included with the trust's tax return).'' (d) Effective Dates.-- (1) In general.--The amendments made by this section shall apply to taxable years of Settlement Trusts beginning after December 31, 1996, and to contributions to such trusts after such date. (2) Requirement for election.--An election under section 501(p)(2) of the Internal Revenue Code of 1986 for a taxable year beginning in 1997 shall not be treated as failing to meet the requirements of section 501(p)(2)(B) of such Code.


We present the discovery of 5 millisecond pulsars found in the mid-Galactic latitude portion of the High Time Resolution Universe (HTRU) Survey. The pulsars have rotational periods from ~2.3 to ~7.5 ms, and all are in binary systems with orbital periods ranging from ~0.3 to ~150 d. In four of these systems, the most likely companion is a white dwarf, with minimum masses of ~0.2 Solar Masses. The other pulsar, J1731-1847, has a very low mass companion and exhibits eclipses, and is thus a member of the "black widow" class of pulsar binaries. These eclipses have been observed in bands centred near frequencies of 700, 1400 and 3000 MHz, from which measurements have been made of the electron density in the eclipse region. These measurements have been used to examine some possible eclipse mechanisms. The eclipse and other properties of this source are used to perform a comparison with the other known eclipsing and "black widow" pulsars. These new discoveries occupy a short-period and high-dispersion measure (DM) region of parameter space, which we demonstrate is a direct consequence of the high time and frequency resolution of the HTRU survey. The large implied distances to our new discoveries makes observation of their companions unlikely with both current optical telescopes and the Fermi Gamma-ray Space Telescope. The extremely circular orbits make any advance of periastron measurements highly unlikely. No relativistic Shapiro delays are obvious in any of the systems, although the low flux densities would make their detection difficult.


We analyze 2.8-yr data of 1-100 GeV photons for clusters of galaxies, collected with the Large Area Telescope onboard the Fermi satellite. By analyzing 49 nearby massive clusters located at high Galactic latitudes, we find no excess gamma-ray emission towards directions of the galaxy clusters. Using flux upper limits, we show that the Fornax cluster provides the most stringent constraints on the dark matter annihilation cross section. Stacking a large sample of nearby clusters does not help improve the limit for most dark matter models. This suggests that a detailed modeling of the Fornax cluster is important for setting robust limits on the dark matter annihilation cross section based on clusters. We therefore perform the detailed mass modeling and predict the expected dark matter annihilation signals from the Fornax cluster, by taking into account effects of dark matter contraction and substructures. By modeling the mass distribution of baryons (stars and gas) around a central bright elliptical galaxy, NGC 1399, and using a modified contraction model motivated by numerical simulations, we show that the dark matter contraction boosts the annihilation signatures by a factor of 4. For dark matter masses around 10 GeV, the upper limit obtained on the annihilation cross section times relative velocity is <\sigma v> <~ (2-3)x10^{-25} cm^3 s^{-1}, which is within a factor of 10 from the value required to explain the dark matter relic density. This effect is more robust than the annihilation boost due to substructure, and it is more important.


The Secretary shall credit the account of that eligible State with an amount equal to 75% of the amount received. (ii) If the violation occurs in multiple eligible States, the Secretary shall divide the amount described in clause (i) by the number of eligible States where the violation occurred and shall credit the account of each eligible State with an equal share. (b) Requirements for Use and Redistribution of Payments.-- (1) Use of payments specified.--A payment received under this section shall be used solely for payments to local educational agencies (as defined in section 9101(26) of the Elementary and Secondary Education Act of 1965 (20 U.S.C. 7801(26))), public health care providers, and law enforcement agencies for the purpose of assisting State and local governments with meeting the costs associated with serving aliens who are unlawfully present in the United States. (2) Redistribution of payment to counties and units of local government.--An eligible State shall redistribute 66 percent of the payment received under this section, within 60 days of receipt by the State, to appropriate counties and units of local government in accordance with a system that the State shall develop that provides for opportunities for input from all counties and units of local government in the state and that targets the areas of greatest need in accordance with the purpose described in paragraph (1), based on objective criteria. (c) Definitions.--For the purposes of this section, the following definitions apply: (1) Eligible state.--The term ``eligible State'' means a State that agrees-- (A) to use the payment received under this section for the uses specified in subsection (b)(1); (B) to redistribute the payment received under this section to counties and units of local government in accordance with subsection (b)(2); (C) to require that any county or unit of local government to whom a payment is redistributed shall use the payment for the uses specified in subsection (b)(1); and (D) to submit information and assurances at such time and in such form as the Secretary may require. (2) State.--The term ``State'' includes each State, the District of Columbia, the Commonwealth of Puerto Rico, American Samoa, Guam, and the United States Virgin Islands. (3) Secretary.--The term ``Secretary'' means the Secretary of the Treasury. (d) Effective Date.--This section shall take effect at the beginning of the next fiscal year following


His drawing power sure has. The former Heisman trophy winner was paid $10,000 this season while playing for the Single-A Columbia Fireflies and St. Lucie Mets and contributed to the largest rise in minor league baseball attendance in 23 years, according to ESPN. Attendance for Fireflies games increased by 54,000 fans (21 percent) over last season during Tebow’s tenure in Columbia, and the effect was more pronounced when he joined St. Lucie at the end of June, contributing to a 37 percent rise in visitors to the ballpark. Similar results were seen during road games, where the Fireflies drew an additional 2,591 fans over the home teams’ season averages. The last time the minors saw such a spike in attendance was thanks to another popular cross-sport athlete taking a stab at professional baseball: Michael Jordan. Tebow’s numbers don’t stack up against Jordan’s, but the NBA champion was the single most recognizable sports brand in the world at the time. Add to that the fact Jordan was playing Double-A ball in larger stadiums than Tebow, and the difference in their numbers is easily explained. The point remains – Tebow was a huge draw and a tremendous boon to the clubs he played for and those he visited. A Baseball America study conducted in June placed the value of Tebow’s contribution to ticket sales, parking, concessions and other revenue at $1.6 million. In other words, the Mets organization got precisely what it wanted out of Tebow. When the erstwhile NFL quarterback announced he would try his hand at baseball, many saw the move as nothing more than a publicity stunt, a money-making venture and a distraction. All of which made him a perfect fit for the Mets’ desultory strategizing. Tebow’s .226 batting average and 126 strikeouts in 126 minor league games at the Single-A level make him an unlikely candidate to save the Mets’ floundering big league club. But putting his name on the back of a Mets jersey has clear advantages, as evidenced by the numbers. And at $10,000 a year, the bargain is too good to pass up.


Topological excitations are usually classified by the $n$th homotopy group $\pi_n$. However, for topological excitations that coexist with vortices, there are case in which an element of $\pi_n$ cannot properly describe the charge of a topological excitation due to the influence of the vortices. This is because an element of $\pi_n$ corresponding to the charge of a topological excitation may change when the topological excitation circumnavigates a vortex. This phenomenon is referred to as the action of $\pi_1$ on $\pi_n$. In this paper, we show that topological excitations coexisting with vortices are classified by the Abe homotopy group $\kappa_n$. The $n$th Abe homotopy group $\kappa_n$ is defined as a semi-direct product of $\pi_1$ and $\pi_n$. In this framework, the action of $\pi_1$ on $\pi_n$ is understood as originating from noncommutativity between $\pi_1$ and $\pi_n$. We show that a physical charge of a topological excitation can be described in terms of the conjugacy class of the Abe homotopy group. Moreover, the Abe homotopy group naturally describes vortex-pair creation and annihilation processes, which also influence topological excitations. We calculate the influence of vortices on topological excitations for the case in which the order parameter manifold is $S^n/K$, where $S^n$ is an $n$-dimensional sphere and $K$ is a discrete subgroup of $SO(n+1)$. We show that the influence of vortices on a topological excitation exists only.


Look no further than your phone. It seems emojis, those expressive pictures all over texts and Instagram, could actually help our love lives. In his new book, “The Emoji Code,” to be published in the U.S. in August by MacMillan Picador, British linguist Vyv Evans argues that emojis are making us better communicators. Evans calls emojis a “near-universal form of communication,” replacing internet slang like LOL with the popular “face with tears of joy” emoji. And while he says some see the little glyphs as “little more than an adolescent grunt,” Evans says those people couldn’t be more wrong. Evans’ research found that 72 percent of 18- to 25-year-olds find it easier to express their emotions if they’re using emojis. And 80 percent of people in the U.K. said they use them. There’s a reason for that: Digital communication has stripped away important context like gestures, facial expressions and tone of voice. Emails and texts often come across as more ambiguous — or mean-spirited — than intended. Enter the emoji. Adding a little smiley face or winking eye can convey joking or sarcasm. A text that says “Sure, go ahead!” with a kissy face could read more like “sure … go ahead” without one. A Match.com survey of singles in America found that people who use emojis went on more dates and were more likely to have sex than those who didn’t. More than half of singles who used emojis had sex in 2014, compared to 31 percent of singles who didn’t, according to the survey. NBC News / If this leaves you with a confused face, and you don’t even know how to express that in emoji, check out this quick primer of definitions from Emojipedia.


OKLAHOMA CITY — A former Oklahoma City mayor and member of the University of Oklahoma Board of Regents was rebuked Monday for comparing gay people to pedophiles and politicians who’ve recently resigned amid allegations of sexual misconduct. Kirk Humphreys made the comments during a local TV public affairs show that aired over weekend on KFOR-TV. Humphreys and others were discussing allegations against Minnesota Sen. Al Franken, who is stepping down, and President Donald Trump, when Humphreys began to ramble about other subjects. He said he was “going to make a lot of people mad today.” “Is homosexuality right or wrong? It’s not relative, there’s a right and wrong,” Humphreys said. “If it’s OK then it’s OK for everybody and, quite frankly, it’s OK for men to sleep with little boys.” LGBTQ advocacy group Freedom Oklahoma called for Humphreys’ removal from the Board of Regents if he didn’t apologize. Executive Director Troy Stevenson said Monday that Humphreys’ comments were disheartening and dangerous for LGBTQ youth who are already harassed and bullied. A staffer at Humphreys’ office said he was out of town Monday and unavailable to comment. Humphreys, 67, did not immediately reply to an email seeking comment. The president of the University of Oklahoma distanced himself from Humphreys’ comments. President David Boren noted that Humphreys was not speaking on behalf of the university, adding that the school was committed to diversity and inclusiveness. “I do not share his views on this matter,” Boren said in a statement. A state lawmaker who appeared with Humphreys pushed back at him on the show, saying it was wrong to compare sexual misconduct and crimes to the legal behaviour of consenting adults. “Mr. Humphreys’ comments were disgusting, offensive, and just plain wrong,” Rep. Emily Virgin, a Democrat from Oklahoma City, later said on her Facebook page. “I unequivocally stand with the LGBT community. Stevenson said his group planned to protest an Oklahoma City real estate project that belongs to Humphreys’ family business.


Robin Muchetu, Senior Reporter POLICE have assured the nation that they will bring the perpetrators of the bombing incident in an attempted assassination attack targeting President Emmerson Mnangagwa at White City Stadium to book saying special teams have been assigned to carry out the investigation. Addressing the media and senior officers in Bulawayo today, Police Commissioner General Thandabantu Godwin Matanga said it was work in progress for the police who he said were not going to rest until the suspects have been brought to book. He said the horrendous and nefarious act dampened the spirits of the citizens. “I assure the nation and its entire citizenry that we are fully investigating this dastardly and wicked act, which has already unnecessarily claimed two lives,” said Comm Matanga. He went on: “As the ZRP we will never rest until all those behind this heinous act have been accounted for and have had their day in court. We will do whatever it takes within the precincts of the law to ensure that this objective is met. At the risk of overemphasizing, I wish to say no stone will be left unturned,” he said. He applauded the level of cooperation and support that the joint investigation team has so far received. He said the collaborative effort was appreciated and continued to appeal for more information that may enable the force to bring to book the culprits involved. Cde Matanga further said the public must desist from acts of violence during this period and said the ZRP has since arrested 2237 people from January for engaging in various forms of violence. The ZRP said they would revitalize and reinvigorate all police patrol units with a view to assist in reducing crime through increased police visibility in all crime prone areas. The patrols, they said, help in earning public confidence from the resultant quality of their service.


Waterford County Board chairman Paddy Joe Ryan said there was no intent in Austin Gleeson's controversial clash with Luke Meade and hopes Galway corner-back Adrian Tuohy's reprieve after a similar incident last week serves as a good omen. Gleeson and Corkman Meade tangled during yesterday's All-Ireland SHC semi-final, with Gleeson appearing to pull off his opponent's helmet. Galway's Tuohy did not face any disciplinary action following an incident with Tipperary’s Patrick Maher in the first All-Ireland semi-final. The helmet of the Tipp centre-forward came off during the first-half clash with both men competing for the ball and it was feared that retrospective action could lead him to miss next month’s decider. Speaking to RTÉ news in Dungarvan, Ryan said the Gleeson clash would not be classed as deliberate and that there was no intent by the player. He said Waterford do not want to be entangled in disciplinary matters in the weeks leading up to the All-Ireland final. "We just want this thing to take its course and hopefully we will be more or less full strength for the final," he said, adding that the Waterford County Board will look at the referee's report when it is available and that they will address any matters arising if any exist, also in relation to Conor Gleeson, who was sent off on a straight red card. Ryan revealed they'll wait and see what's in the report by referee James Owens before they decide on a course of action.


Make sure you head to Shanklin Theatre on Thursday evening. A public meeting (14th December, 7pm start) is being held to discuss the stakeholders’ response to South Western Railway’s proposals for Island Line. It’s being organised by Keep Island Line in Franchise campaign, in partnership with the IW Bus & Rail Users’ Group (IWBRUG) and the Isle of Wight Steam Railway (IWSR). The Isle of Wight Conservative MP, Bob Seely, will also be in attendance as well as a number of Isle of Wight Councillors. Your views matter The meeting is open to any members of the public with an interest in the future of railway provision on the Island. The topics being covered will include: South Western Railway’s proposals for Island Line, and the proposed consultation response on behalf of the local community (deadline 31st December 2017). Future plans for the IW Steam Railway; Improving interconnectivity between the two lines and links with cross-Solent travel (including SWR’s plans for mainland services); Possible future extensions to Newport and Ventnor, particularly in light of the Government’s announcement about previously closed lines being re-opened – and MP Bob Seely’s intervention on this topic with Transport Secretary Chris Grayling. Come along For updates and more info prior to the meeting visit KILF’s Facebook event page. Shanklin Theatre’s doors (and the bar) will open at 6:30pm, ahead of a 7pm start. Any questions about the public meeting on 14th December should be directed to kilfcampaign@gmail.com. Image: tompagenet under CC BY 2.0 Location map View the location of this story.


Searches for gravitational waves with km-scale laser interferometers often involve the long-wavelength approximation to describe the detector response. The prevailing assumption is that the corrections to the detector response due to its finite size are small and the errors due to the long-wavelength approximation are negligible. Recently, however, Baskaran and Grishchuk (2004 Class. Quantum Grav. 21 4041) found that in a simple Michelson interferometer such errors can be as large as 10 percent. For more accurate analysis, these authors proposed to use a linear-frequency correction to the long wavelength approximation. In this paper we revisit these calculations. We show that the linear-frequency correction is inadequate for certain locations in the sky and therefore accurate analysis requires taking into account the exact formula, commonly derived from the photon round-trip propagation time. Also, we extend the calculations to include the effect of Fabry-Perot resonators in the interferometer arms. Here we show that a simple approximation which combines the long-wavelength Michelson response with the single-pole approximation to the Fabry-Perot transfer function produces rather accurate results. In particular, the difference between the exact and the approximate formulae is at most 2-3 percent for those locations in the sky where the detector response is greater than half of its maximum value. We analyse the impact of such errors on detection sensitivity and parameter estimation in searches for periodic gravitational waves emitted by a known pulsar, and in searches for an isotropic stochastic gravitational-wave background. At frequencies up to 1 kHz, the effect of such errors is at most 1-2 percent. For higher frequencies, or.


Then the amount of time that has passed since the most recent common ancestor (MRCA) of all current individuals lived will change as time progresses. The resulting "MRCA age" process has been studied previously when the population has a constant large size and evolves via the diffusion limit of standard Wright--Fisher dynamics. For any population model, the sample paths of the MRCA age process are made up of periods of linear upward drift with slope +1 punctuated by downward jumps. We build other Markov processes that have such paths from Poisson point processes on $\mathbb{R}_{++}\times\mathbb{R}_{++}$ with intensity measures of the form $\lambda\otimes\mu$ where $\lambda$ is Lebesgue measure, and $\mu$ (the "family lifetime measure") is an arbitrary, absolutely continuous measure satisfying $\mu((0,\infty))=\infty$ and $\mu((x,\infty))<\infty$ for all $x>0$. Special cases of this construction describe the time evolution of the MRCA age in $(1+\beta)$-stable continuous state branching processes conditioned on nonextinction--a particular case of which, $\beta=1$, is Feller's continuous state branching process conditioned on nonextinction. As well as the continuous time process, we also consider the discrete time Markov chain that records the value of the continuous process just before and after its successive jumps. We find transition probabilities for both the continuous and discrete time processes, determine when these processes are transient and recurrent and compute stationary distributions when they exist.


Consider what Einstein said: You don't solve a problem by looking at it in the same way, try looking at things from a new angle. Agnew fits writing into her job as a primary school teacher by getting up at 5:30am to write before the school day starts. What inspired her to become a writer? Agnew "grew up in a house full of books" and her dad was a journalist who writes non-fiction, but really, she says, she "just wanted to do it." In the first session with Tania Roxborogh, Leonie Agnew and David Elliot I felt an overall theme of the elusive - of capturing the elusive writing spark, capturing the Snark, and elusive invisible friends. Another theme that came through for me was the theme of imagination: imagine if someone was trying to take your land, imagine wondrous creatures and lands, imagine how an imaginary friend would feel if they discovered they weren't real. Imagine. Session Two: Des Hunt, Jenny Cooper and Simon Pollard Des Hunt has a love of adventure stories, science, New Zealand animals and he combines all of these into his stories. Sunken Forest was inspired by a real life summer camp he went on when he was 15 at Lake Waikaremoana, a trip that was memorable partly for sparking his interest in geology. The lake was formed during an earthquake landslide that drowned the forest. Standing tree trunks eerily remain there underwater today. Also trapped there are eels which can't make their way back to sea to migrate to the Pacific islands to lay eggs. Unable to leave, they grow exponentially large. In Sunken Forest, one such eel befriends Matt, who is sent to boot camp after his father, a boy racer, is sentenced to prison. At camp, Matt has to deal with bullies and getting the blame for things he didn't do. In his talk, Des Hunt totally engaged his audience from beginning to end, by which time he had them on the edge of their seats. He cleverly demonstrated the idea of building tension in a story by blowing up a balloon... about to burst at any moment. How do you really build tension in a story? He says: Add conflict and injustice, a disaster and... Pop!... an explosive climax. While many of those who spoke at the event started writing or drawing as early as their primary school years, surprisingly Des only published his first fiction book when


1961, there are authorized to be appropriated to the President $5,000,000 for fiscal year 1999, $7,500,000 for fiscal year 2000, and $8,000,000 for fiscal year 2001 to carry out section 129 of the Foreign Assistance Act of 1961, as added by subsection (a). (2) Availability of funds.--Amounts appropriated pursuant to this subsection shall remain available until expended. (c) Effective Date.--The amendment made by subsection (a) shall take effect on October 1, 1998. SEC. 9. MULTILATERAL ASSISTANCE. (a) Funding.--Of the amounts authorized to be appropriated for fiscal years 1999, 2000, and 2001 pursuant to chapter 1 of part I of the Foreign Assistance Act of 1961, there are authorized to be appropriated to the United Nations Voluntary Fund for Victims of Torture (in this section referred to as the ``Fund'') the following amounts for the following fiscal years: (1) Fiscal year 1999.--For fiscal year 1999, $3,000,000. (2) Fiscal year 2000.--For fiscal year 2000, $3,000,000. (3) Fiscal year 2001.--For fiscal year 2001, $3,000,000. (b) Availability of Funds.--Amounts appropriated pursuant to subsection (a) shall remain available until expended. (c) Sense of Congress.--It is the sense of Congress that the President, acting through the United States Permanent Representative to the United Nations, should-- (1) request the Fund-- (A) to find new ways to support and protect treatment centers and programs that are carrying out rehabilitative services for victims of torture; and (B) to encourage the development of new such centers and programs; (2) use the voice and vote of the United States to support the work of the Special Rapporteur on Torture and the Committee Against Torture established under the Convention Against Torture and Other Cruel, Inhuman or Degrading Treatment or Punishment; and (3) use the voice and vote of the United States to establish a country rapporteur or similar procedural mechanism to investigate human rights violations in a country.


The purpose of this paper is to find optimal estimates for the Green function of a half-space of {\it the relativistic $\alpha$-stable process} with parameter $m$ on $\Rd$ space. This process has an infinitesimal generator of the form $mI-(m^{2/\alpha}I-\Delta)^{\alpha/2},$ where $0<\alpha<2$, $m>0$, and reduces to the isotropic $\alpha$-stable process for $m=0$. Its potential theory for open bounded sets has been well developed throughout the recent years however almost nothing was known about the behaviour of the process on unbounded sets. The present paper is intended to fill this gap and we provide two-sided sharp estimates for the Green function for a half-space. As a byproduct we obtain some improvements of the estimates known for bounded sets specially for balls. The advantage of these estimates is a clarification of the relationship between the diameter of the ball and the parameter $m$ of the process. The main result states that the Green function is comparable with the Green function for the Brownian motion if the points are away from the boundary of a half-space and their distance is greater than one. On the other hand for the remaining points the Green function is somehow related the Green function for the isotropic $\alpha$-stable process. For example, for $d\ge3$, it is comparable with the Green function for the isotropic $\alpha$-stable process.


The DAMA/NaI and DAMA/LIBRA annual modulation data, which may be interpreted as a signal for the existence of weakly interacting dark matter (WIMPs) in our galactic halo, are examined in light of null results from other experiments. We use the energy spectrum of the combined DAMA modulation data given in 36 bins, and include the effect of channeling. Several statistical tools are implemented in our study: likelihood ratio with a global fit and with raster scans in the WIMP mass and goodness-of-fit (g.o.f.). These approaches allow us to differentiate between the preferred (global best fit) and allowed (g.o.f.) parameter regions. It is hard to find WIMP masses and couplings consistent with all existing data sets. For spin-independent (SI) interactions, the best fit DAMA regions are ruled out to the 3$\sigma$ C.L., even with channeling taken into account. However, for WIMP masses of ~8 GeV some parameters outside these regions still yield a moderately reasonable fit to the DAMA data and are compatible with all 90% C.L. upper limits from negative searches, when channeling is included. For spin-dependent (SD) interactions with proton-only couplings, a range of masses below 10 GeV is compatible with DAMA and other experiments, with and without channeling, when SuperK indirect detection constraints are included; without the SuperK constraints, masses as high as ~20 GeV are compatible. For SD neutron-only couplings we find no parameters compatible with all the experiments. Mixed SD couplings are examined: e.g. ~8 GeV mass WIMPs with a_n = +/- a_p are found to be consistent with all experiments. In short, there are surviving regions at low mass for both SI and SD interactions;.


You may not know who Harvey Weinstein is. But if you do, then you’ll know he’s something of a Hollywood kingpin, a super-producer with six Oscars to his name, and movies like Pulp Fiction, Good Will Hunting and Shakespeare in Love dotting his resumé. You’ll also know he’s been dodging rumours of sexual harassment for over three decades. In an explosive report by The New York Times published Thursday after The Hollywood Reporter revealed Wednesday that Weinstein was preparing to file a lawsuit against the paper, details of countless allegations of sexual harassment against him were revealed, backed up by legal records, emails and internal documents from his companies. Many of his former employees revealed they were aware of his behaviour for years. The women making the allegations range from their 20s to 40s, all in different cities (Weinstein is known to flit from New York to London to Paris). Several said they didn’t report Weinstein because they were afraid of retaliation, because there weren’t witnesses, or simply because they felt embarrassed. Weinstein, who has been married to designer Georgina Chapman for 10 years (with whom he has two children), has reached at least eight settlements with different women. A follow-up report on Weinstein is set to be published by The New Yorker in the coming weeks, but for now, here are the biggest takeaways from the NYT: Ashley Judd comes forward In 1997, while she was filming Kiss the Girls (a Weinstein Company movie), Weinstein invited actress Ashley Judd to his Beverly Hills hotel room, wearing nothing but a bathrobe. He asked her if she would either give him a massage or watch him shower. When she declined, he asked her for a shoulder rub (she declined again). Countless actresses reported Weinstein making the same requests of them over the decades. He would often tell them he’d “boost” their career if they accepted his advances, and would also boast about famous actresses he claimed to have slept with. Speaking to the NYT, Judd said, “Women have been talking about Harvey amongst ourselves for a long time, and it’s simply beyond time to have the conversation publicly.” In 1997, Weinstein reached a US$100,000 settlement with actress Rose McGowan, 23 at the time, “after an episode in a hotel room” at the Sundance Film Festival. His legal team noted that the settlement


The effective potential in the Grumiller's modified gravity [D. Grumiller, Phys. Rev. Lett {\bf 105}, 211303 (2010)] includes the Newtonian potential and a Rindler term. The fitting to the rotation curve data of eight galaxies suggests a universal Rindler acceleration $a\approx 0.30\times 10^{-10}$ m s$^{-2}$. We do a two-parameter fit first, with the mass-to-light ratio ($\Upsilon_*$) and the Rindler acceleration ($a$) as free parameters. It is found that the data of six out of the eight galaxies fit well with the prediction of theory in the range $0\lesssim r \lesssim 40$ kpc, although the theoretical curves show a tendency of arising beyond this range. The Rindler accelerations of the six well-fitted galaxies have the same magnitude, with an average value $\bar{a}\approx0.30\times 10^{-10}$ m s$^{-2}$. Inspired by this fact, we then carry out a one-parameter ($\Upsilon_*$) fit to the six galaxies, with $a$ fixed at $\bar{a}$, and find that the theory can still reproduce the observation. The value of Rindler acceleration we get here is a quarter of that of Milgrom's MOND. For the rest two galaxies, NGC5055 and DDO154, the fitting results are significantly improved.


We present parameter-free predictions of the nuclear modification factor, R_{AA}^pi(p_T,s), of high p_T pions produced in Pb+Pb collisions at sqrt{s}_{NN}=2.76 and 5.5 ATeV based on the WHDG/DGLV (radiative+elastic+geometric fluctuation) jet energy loss model. The initial quark gluon plasma (QGP) density at LHC is constrained from a rigorous statistical analysis of PHENIX/RHIC pi^0 quenching data at sqrt{s}_{NN}=0.2 ATeV and the charged particle multiplicity at ALICE/LHC at 2.76 ATeV. Our perturbative QCD tomographic theory predicts significant differences between jet quenching at RHIC and LHC energies, which are qualitatively consistent with the p_T-dependence and normalization---within the large systematic uncertainty---of the first charged hadron nuclear modification factor, R^{ch}_{AA}, data measured by ALICE. However, our constrained prediction of the central to peripheral pion modification, R^pi_{cp}(p_T), for which large systematic uncertainties associated with unmeasured p+p reference data cancel, is found to be over-quenched relative to the charged hadron ALICE R^{ch}_{cp} data in the range 5<p_T<20 GeV/c. The discrepancy challenges the two most basic jet tomographic assumptions: (1) that the energy loss scales linearly with the initial local comoving QGP density, rho_0, and (2) that \rho_0 \propto dN^{ch}(s,C)/dy is proportional to the observed global charged particle multiplicity per unit rapidity as a function of sqrt{s} and centrality class, C. Future LHC identified (h=pi,K,p) hadron R^h_{AA} data (together with precise p+p, p+Pb, and Z boson and direct photon Pb+Pb control data) are needed to assess.


Aims. We search for transiting circumbinary (CB) planets around eclipsing binaries (EBs). Methods. CB-BLS is a recently-introduced algorithm for the detection of transiting CB planets around EBs.We describe progress in search sensitivity, generality and capability of CB-BLS, and detection tests of CB-BLS on simulated data. We also describe an analytical approach for the determination of CB-BLS detection limits, and a method for the correct detrending of intrinsically-variable stars. Results. We present some blind-tests with simulated planets injected to real CoRoT data. The presented upgrades to CB-BLS allowed it to detect all the blind tests successfully, and these detections were in line with the detection limits analysis. We also correctly detrend bright eclipsing binaries from observations by the TrES planet search, and present some of the first results of applying CB-BLS to multiple real light curves from a wide-field survey. Conclusions. CB-BLS is now mature enough for its application to real data, and the presented processing scheme will serve as the template for our future applications of CB-BLS to data from wide-field surveys such as CoRoT. Being able to put constraints even on non-detection will help to determine the correct frequency of CB planets, contributing to the understanding of planet formation in general. Still, searching for transiting CB planets is still a learning experience, similarly to the state of transiting planets around single stars only a few years ago. The recent rapid progress in this front, coupled with the exquisite quality of space-based photometry, allows to realistically expect that.


An alien may be eligible to be granted the status of having been lawfully admitted for permanent residence under this section shall not preclude the alien from seeking such status under any other provision of law for which the alien may be eligible. SEC. 3. AMENDMENTS TO NICARAGUAN ADJUSTMENT AND CENTRAL AMERICAN RELIEF ACT. (a) Elimination of Limitations on Judicial Review.-- (1) Adjustment of status of certain nicaraguans and cubans.--Section 202(f) of the Nicaraguan Adjustment and Central American Relief Act is amended to read as follows: ``(f) Judicial Review.--A determination by the Attorney General as to whether the status of any alien should be adjusted under this section is subject to judicial review in accordance with chapter 7 of title 5, United States Code.''. (2) Special rule for certain aliens granted temporary protection from deportation.--Section 309(c)(5)(C)(ii) of the Illegal Immigration Reform and Immigrant Responsibility Act of 1996, as added by section 203(a)(1) of the Nicaraguan Adjustment and Central American Relief Act, is amended to read as follows: ``(ii) Judicial review.--A determination by the Attorney General as to whether an alien satisfies the requirements of clause (i) is subject to judicial review in accordance with chapter 7 of title 5, United States Code. Nothing in the preceding sentence shall be construed as limiting the application of section 242(a)(2)(B) of the Immigration and Nationality Act (as in effect after the title III-A effective date) to other eligibility determinations pertaining to discretionary relief under this Act.''. (b) Elimination of Temporary Reductions in Visas.--Section 203 of the Nicaraguan Adjustment and Central American Relief Act is amended-- (1) by striking subsections (d) and (e); and (2) by redesignating subsection (f) as subsection (d). (c) Effective Date.--The amendments made by this section-- (1) shall take effect upon the enactment of the Nicaraguan Adjustment and Central American Relief Act; and (2) shall be effective as.


Get daily updates directly to your inbox + Subscribe Thank you for subscribing! Could not subscribe, try again later Invalid Email Students at Helsby High School took part in a range of activities with the theme All Different, All Equal. The school held a non-uniform day when children and staff had to wear something blue to support the cause and raise awareness for anti-bullying week. They raised £1,200 in donations, which will go to the charity Bullying UK. Year 11 student leaders produced a video clip, which is hosted on the school’s YouTube channel, which sees students from all year groups contributing. This video clip was played in assemblies and in form time. Students from all form classes held class discussions on four main questions: 1. What is bullying? 2. Who can you go to for help? 3. Why is it important to stop bullying? 4. Is there anything we could do at Helsby High School to help prevent it? (Image: UGC) Each form class was then given the opportunity to contribute to the anti-bullying board. The next step is for this information to be collated and shared with the student leaders and pastoral leaders. A set of action points will then be created. At Helsby High School, they take any reporting of alleged bullying very seriously. As a school community they do not tolerate any form of bullying. Each and every member of the school community has a part to play in this by either reporting or helping to resolve any alleged bullying. All students are expected to treat fellow students with respect and consideration by following the school’s Code of Conduct. The school strives that.


In a recent article, Kholmetskii, Missevitch and Yarmin ["On the classical analysis of spin-orbit coupling in hydrogenlike atoms," Am. J. Phys. 78(4), April 2010 (428-432)] examine in detail the spin-orbit coupling in the semiclassical hydrogenic atom, and identify a need to account for non-Coulomb forces not included in the standard analysis. Kholmetskii, et al., showed that the experimentally-measured coupling continues to be obtained when the new forces are incorporated in the analysis. This requires that the change in orbital radius due to non-Coulomb forces is also properly accounted for. In response to a comment, Kholmetskii, et al., showed that the experimentally-measured coupling continues to be obtained when so-called "hidden momentum" forces are also included. However it has been postulated that when hidden momentum is nonvanishing, a corresponding hidden energy must also be present, that was not included in the total energy by Kholmetskii, et al. Hidden energy is postulated necessary to obtaining a relativistically covariant description. Inclusion of hidden energy leads to disagreement with the experimentally-determined spin-orbit coupling magnitude if the Bohr postulate, that orbital angular momentum is quantized in whole multiples of the reduced Planck constant, is assumed to apply to kinetic momentum alone. The empirical result may be recovered in the semiclassical picture and using the general approach developed by Kholmetskii, et al..


And this home to amazing youth programs,” Compton wrote on Twitter. Beckham’s group also wants to bring a massive technology park to the site, as well as an underground parking facility, public soccer fields, 500 new hotel rooms, a conference centre, retail stores, restaurants and more. The Beckham franchise, when it gets going, will also bring a training centre and an academy focused on developing local players to the Miami area. The stadium-location quest is just the latest drawn-out chapter in Beckham’s five-years-and-counting marathon to bring MLS back to Miami. The Miami Fusion played from 1998-2001, folding because of poor attendance. Beckham and MLS announced in January that the franchise would be coming to Miami, but nearly every detail about the club remains unclear. There’s no definitive start date — 2020 has been mentioned repeatedly, even though no new stadium could possibly be ready by then — as well as no team name, no logo, no colours, no coaching staff and no front-office personnel. More than a year ago, Miami-Dade County commissioners approved a deal to sell Beckham nearly three acres of county land for $9 million with the belief that it would be the last parcel he needed for a stadium site in the city’s Overtown neighbourhood. But that site was never the preferred choice for Beckham and his group anyway, with the original hope being to build on the waterfront near the Port of Miami. The Overtown site now seems all but doomed, though it’s unclear what would happen.


Several experimental studies show the existence of leader neurons in population bursts of 2D living neural networks. A leader neuron is, basically, a neuron which fires at the beginning of a burst (respectively network spike) more often that we expect by looking at its whole mean neural activity. This means that leader neurons have some burst triggering power beyond a simple statistical effect. In this study, we characterize these leader neuron properties. This naturally leads us to simulate neural 2D networks. To build our simulations, we choose the leaky integrate and fire (lIF) neuron model. Our lIF model has got stable leader neurons in the burst population that we simulate. These leader neurons are excitatory neurons and have a low membrane potential firing threshold. Except for these two first properties, the conditions required for a neuron to be a leader neuron are difficult to identify and seem to depend on several parameters involved in the simulations themself. However, a detailed linear analysis shows a trend of the properties required for a neuron to be a leader neuron. Our main finding is: A leader neuron sends a signal to many excitatory neurons as well as to a few inhibitory neurons and a leader neuron receives only a few signals from other excitatory neurons. Our linear analysis exhibits five essential properties for leader neurons with relative importance. This means that considering a given neural network with a fixed mean number of connections per neuron, our analysis gives us a way of predicting which neuron can be a good leader neuron and which cannot. Our prediction formula gives us a good statistical prediction even.


Recent publications claim that there is no convincing evidence for measurements of the baryonic acoustic (BAO) feature in galaxy samples using either monopole or radial information. Different claims seem contradictory: data is either not consistent with the BAO model or data is consistent with both the BAO model and featureless models without BAO. We investigate this point with a set of 216 realistic mock galaxy catalogs extracted from MICE7680, one of the largest volume dark matter simulation run to date, with a volume of 1300 cubical gigaparsecs. Our mocks cover similar volume, densities and bias as the real galaxies and provide 216 realizations of the Lambda or w=-1 Cold Dark Matter (wCDM) BAO model. We find that only 20% of the mocks show a statistically significant (3 sigma) preference for the true (input) wCDM BAO model as compared to a featureless (non-physical) model without BAO. Thus the volume of current galaxy samples is not yet large enough to claim that the BAO feature has been detected. Does this mean that we can not locate the BAO position? Using a simple (non optimal) algorithm we show that in 50% (100%) of the mocks we can find the BAO position within 5% (20%) of the true value. These two findings are not in contradiction: the former is about model selection, the later is about parameter fitting within a model. We conclude that current monopole and radial BAO measurements can be used as standard rulers.


2 of the meetings each year shall take place in person at the Department's headquarters in the District of Columbia. Participants should make every effort within reason to attend these meetings in person. (4) Agenda.--Each meeting shall be conducted in accordance with an agenda formulated by the chairman of the Committee, with input from other Committee members. (5) Department representation.--Each meeting of the Committee shall be attended by the Secretary or the Secretary's designee. (f) Compensation and Travel Expenses.--Each member of the Committee who is not a full-time employee of the United States shall-- (1) be entitled to receive compensation at a rate not to exceed the daily equivalent of the annual rate of basic pay in effect for a position at level V of the Executive Schedule under section 5316 of title 5, United States Code, for each day during which the member is engaged in the actual performance of the duties of the Committee; and (2) while away from the home or regular place of business of the member in the performance of services for the Committee, be allowed travel expenses, including per diem in lieu of subsistence, in the same manner as persons employed intermittently in the Government service are allowed expenses under section 5703 of title 5, United States Code. (g) Staff.--The Department shall make available to the Committee such staff as the chairman of the Committee determines are necessary to carry out the functions of the Committee. (h) Review by Department.--The Department shall-- (1) review the findings and recommendations of the Committee; and (2) each time the Committee submits a finding or recommendation to the Department, promptly, but no more than 60 days after submission, issue a public statement, a copy of which shall be delivered to Committee members-- (A) assessing the finding or recommendation of the Committee; and (B) disclosing the action.


TiVo is (cleverly) turning things upside down for Super Bowl LII with introduction of GameSkip. This first-time feature for TiVo DVRs flips the company’s SkipMode—which skips commercials in some shows—on its head. With GameSkip, TiVo users can skip the game and get right to the important bits—Super Bowl commercials and the Halftime Show. Firstly, TiVo’s website is oh-so-careful not to mention the Super Bowl by name. I’m not sure why, since the whole point of the event is to submerse us in a marketing bath, but it’s notable in TiVo’s description: This coming Sunday, February 4, is the day TV fans wait all year for. Sure, the big game’s great and all, but for those who tune in for the multi-million-dollar commercials and the world’s biggest halftime show, we’ve got the perfect solution: TiVo GameSkip. This first-time feature turns SkipMode™ upside-down. After recording the big game, look for the on-screen SKIP icon next to the recording. Then hit play, press the SKIP button1 and your TiVo will jump to the beginning of the next commercial break! Kind of makes you want to give us a high-five, right? I’ll admit that I love and hate this. I haven’t had time for sports in a long, long time. So, you know, lolfunny. At the same time, there’s a part of me appalled at how commercial advertising has become content in and of itself. It’s perverse, and yet another step towards a cyberpunk future where we’re all slaves to the Corp. Then again, I enjoy watching, writing, and talking about Apple’s advertising, so my I may need a hand getting up on my high horse on this topic. And while we’re at it, you can just watch teasers for the commercials on TiVo’s site. So there’s that, too. Anyhoo…TiVo is giving its customers an interesting choice this year with GameSkip. I’d love to hear.


Job. Is there a misconception where these skilled jobs have to be dirty and dangerous? MR: The problem isn't that so much has changed in that world; the problem in my view is that higher ed needed a PR campaign in the ’50s and ’60s. We actually needed more people to enthusiastically matriculate through universities. Society really could benefit from more liberal arts classical thought and more people with a broad-based understanding of stuff. And so the push for college in my view was legitimate. Unfortunately, the push for college came at the expense of other forms of education. And this is just a classic trap in most forms of advocacy and PR. You promote one thing not to the betterment of itself but at the expense of the other. So the proposition became “if you don't go to a four-year school, you're going to wind up over here in this shit hole. But if you wind up over there, then the kind of job you're going to get is going to make you want to kill yourself. So the whole transaction became fraught with false consequences. That's how we promote it. I still have a poster that was in my guidance counselor’s office that was really one of the first attempts to broadly promote college with a platitude, and the platitude was “Work smart, not hard.” And that's really where a lot of people just assume it's a logical thing with regard to heightened efficiency and of course it is. But that caption appeared on a photo of a kid holding a diploma next to a skilled worker holding a wrench and looking like he just won a vocational consolation prize. mikeRoweWORKS When you start telling kids that if you don't work smart, you'll have no choice but to work hard, you're giving them this "Let's Make a Deal” choice, where behind the curtain is nothing but a box of Borax or a brand new, shiny Corvette. It's not fair, it's not right, it's not sensible. But that basic notion has infected and informed a big chunk of our culture, and consequently you've got well over $1 trillion in student loans on the books and you've got over 6 million jobs that are currently open, many in manufacturing, many in the skilled trades — and few of which require a four-year degree. So that's your disconnect in a nutshell. Today we have this notion that.


Unemployment account was established before the date of enactment of this Act, the Temporary Extended Unemployment Compensation Act of 2002 (as amended by this Act) shall be applied subject to the following: (A) Any amounts deposited in the individual's temporary extended unemployment compensation account by reason of section 203(c) of such Act (commonly known as ``TEUC-X amounts'') before the date of enactment of this Act shall be treated as amounts deposited by reason of section 203(b) of such Act (commonly known as ``TEUC amounts''), as deemed to have been amended by subsection (c)(1). (B) For purposes of determining whether the individual is eligible for any TEUC-X amounts under such Act, as deemed to be amended by this section-- (i) any determination made under section 203(c) of such Act before the application of the amendment described in subsection (c)(2) shall be disregarded; and (ii) any such determination shall instead be made by applying section 203(c) of such Act, as deemed to be amended by subsection (c)(2)-- (I) as of the time that all amounts established in such account in accordance with section 203(b) of such Act (as deemed to be amended under this section, and including any amounts described in subparagraph (A)) are in fact exhausted, except that (II) if such individual's account was both augmented by and exhausted of all TEUC-X amounts before the date of enactment of this Act, such determination shall be made as.


Study.--Not later than 180 days after the date of enactment of this Act, the Secretary shall conduct a study to determine the effectiveness and feasibility of establishing 1 or more propane storage facilities, to be operated separately from the Strategic Petroleum Reserve established under part B of title I of the Energy Policy and Conservation Act (42 U.S.C. 6231 et seq.). (b) Plan.--Following completion of the study under subsection (a), the Secretary may submit to Congress and the President a plan describing-- (1) the proposed acquisition of storage and related facilities or storage services for, including-- (A) the potential use of storage facilities not currently in use; and (B) a determination of the combination of primary, secondary, and tertiary storage facilities that will be used; (2) the proposed acquisition of propane for storage; (3) the proposed methods of disposition of propane; (4) the estimated costs of establishment, maintenance, and operation; (5) the efforts the Secretary will make-- (A) to minimize any potential need for future drawdowns; and (B) to ensure that distributors and importers are not discouraged from maintaining and increasing supplies of propane; (6) the proposed actions to ensure the quality of the propane; and (7) the proposed accounts and funding structures required for acquisition of propane and propane storage facilities. SEC. 7. STORAGE FACILITY LOANS FOR PROPANE STORAGE. Section 1614(a) of the Food, Conservation, and Energy Act of 2008 (7 U.S.C. 8789(a)) is amended by inserting ``, including facilities for propane that is used for drying and heating'' before the period at the end. SEC. 8. STUDY OF JURISDICTION. Not later than 1 year after the date of enactment of this Act, the Comptroller General of the United States shall complete a study of facilities appurtenant to propane pipelines (such as terminals and storage facilities) that are not subject to the jurisdiction of the Commission (as of the date on which the study commences) to determine-- (1) whether the nonjurisdictional nature of the facilities is injurious to shippers or consumers; and (2)(A) whether the facilities can be placed under the jurisdiction of the Commission; or (B).


We investigate the orientation correlation of giant elliptical galaxies by measuring the intrinsic ellipticity correlation function of 83,773 luminous red galaxies (LRGs) at redshifts 0.16 -- 0.47 from the Sloan Digital Sky Survey. We have accurately determined the correlation up to 30 $h^{-1}$Mpc. Luminosity dependence of the ellipticity correlation is also detected although the error bars are large, while no evidence is found for its redshift evolution between $z=0.2$ and $z=0.4$. Then we use a cosmological $N$-body simulation to examine misalignment between the central LRGs and their parent dark matter halos. Central and satellite galaxies are assigned to simulated halos by employing a halo occupation distribution model for the LRGs. The ellipticity correlation is predicted to have the same shape as but an amplitude about 4 times higher than our observation if the central LRGs are perfectly aligned with their host halos. This indicates that the central LRG galaxies are preferentially but not perfectly aligned with their host halos. With the assumption that there is a misalignment angle between a central LRG and its host halo which follows a Gaussian distribution with a zero mean and a width $\sigma_\theta$, we obtain a tight constraint on the misalignment parameter, $\sigma_\theta={35.4}^{+4.0}_{-3.3}$ deg. This type of intrinsic ellipticity correlation, if not corrected, can lead to contamination at 5% level to the shear power spectrum in weak lensing surveys of limiting magnitude $R_{AB}=24.5$.


It will generate measurable temperature anisotropies due to the Kinematic Sunyaev-Zeldovich effect. We compute the distribution function of the KSZ signal produced by a typical filament and show it is highly non-gaussian. The combined contribution of the Thermal and Kinematic SZ effects of a filament of size $L\simeq 5$Mpc and electron density $n_e\simeq 10^3m^{-3}$ could explain the cold spots of $\delta\sim -200\mu$K on scales of 30' found in the Corona Borealis Supercluster by the VSA experiment. PLANCK, with its large resolution and frequency coverage, could provide the first evidence of the existence of filaments in this region. The KSZ contribution of the network of filaments and halo structures to the radiation power spectrum peaks around $l\sim 400$, a scale very different from that of clusters of galaxies, with a maximum amplitude $l(l+1)C_l/2\pi\sim 10-25 (\mu K)^2$, depending on model parameters, i.e., $\sigma_8$ and the Jeans length. About 80% of the signal comes from filaments with redshift $z\le 0.1$. Adding this component to the intrinsic Cosmic Microwave Background temperature anisotropies of the concordance model improves the fit to WMAP 3yr data by $\Delta\chi^2\simeq 1$. The improvement is not statistically significant but a more systematic study could demonstrate that gas could significantly contribute to the anisotropies measured by WMAP.


It could cause buyer's remorse for CVS, Mr. Coker said. The retail pharmacy chain intends to finance the transaction with $45 billion in debt. "This Aetna deal could be boneheaded if CVS's goal is to shore up its defenses against an inevitable entry against Amazon into the market," he said. "Health insurers are part of why drugs are so expensive. Amazon approaches markets by eliminating the middleman. It seems that CVS is making a bet that health insurers are going to continue to be the dominate intermediary between a consumer and drugmaker." Investors also appear to have doubts about how much the drugstore chain was willing to pay for Aetna: CVS Health Corp.'s stock fell $3.41, or nearly 5 percent, to $71.69 on the New York Stock Exchange, although the Dow Jones index was up strongly for most of the day. Joel Espelien, a senior research analyst at The Diffusion Group, agreed that Amazon will put pressure on CVS and Aetna after the deal is completed. "CVS didn't want to just be a distributor, so it bought a health plan," he said. "But disruption can change how business is done in that industry. Amazon will force CVS and Aetna to dramatically up their game." Even if Amazon's first step in the health care industry is offering prescriptions through its website, Mr. Espelien said, that could create fierce competition in the sector. He predicts prescriptions will be delivered via drones within minutes along with other supply advantages that only Amazon can offer. "It doesn't mean CVS can't compete with Amazon, but if they can't match what Amazon is doing, they will be in serious trouble," he said. The time is right for Amazon to enter the health care industry because of its proven ability to reduce costs in an industry that has long struggled to keep expenses down and prices competitive. "When I look at a retail pharmacy, it strikes me as fairly inefficient," Mr. Coker said. "They have to maintain that expensive floor space, expensive pharmacist, cash register. Maybe you can achieve greater economies of scale by moving that to a call center in India like Amazon did with the book industry." © 2017 Washington Times under contract with NewsEdge/Acquire Media. All rights reserved. Image credit: CVS/iStock/Artist's concept.


Or 4091 of such Code shall, insofar as applicable and not inconsistent with the provisions of this subsection, apply with respect to the floor stocks taxes imposed by paragraph (1) to the same extent as if such taxes were imposed by such section 4081 or 4091, as the case may be. (e) Effective Dates.-- (1) Fuel taxes.--The amendments made by subsection (a) shall apply to periods beginning on or after the 7th day after the date of the enactment of this Act. (2) Ticket taxes.-- (A) In general.--The amendments made by subsection (b) shall apply to transportation beginning on or after such 7th day. (B) Exception for certain payments.--Except as provided in subparagraph (C), the amendments made by subsection (b) shall not apply to any amount paid before such 7th day. (C) Payments of property transportation tax within controlled group.--In the case of the tax imposed by section 4271 of the Internal Revenue Code of 1986, subparagraph (B) shall not apply to any amount paid by 1 member of a controlled group for transportation furnished by another member of such group. For purposes of the preceding sentence, all persons treated as a single employer under subsection (a) or (b) of section 52 of the Internal Revenue Code of 1986 shall be treated as members of a controlled group. (f) Application of Look-Back Safe Harbor for Deposits.--Nothing in the look-back safe harbor prescribed in Treasury Regulation section 40.6302(c)-1(c)(2) shall be construed to permit such safe harbor to be used with respect to any tax.


If we do, we then enact democratic legislation that will ensure there is transparency and accountability in the appointment process and execution of duty, which conduct must be guided by the Constitution. “For many years the Censorship Board has assumed the notorious character of a morality police as well as an unchecked gatekeeper who decides what content is right or wrong for Zimbabweans. “They have banned some plays with political satire and films that reflect badly on the ruling elite all on flimsy grounds that they were not suitable for the majority of the people. “And now that Chombo says the new board will extend its control tentacles to the social media, it’s clear it’s not about the contested moral righteousness but policing citizens’ artistic freedoms, freedom of expression, generation and access to information online and offline,” said Ngwenya. He added that Zimbabwe does not need another body or layer of repression under the guise of promoting morality; it needs democratic laws and institutions that will ensure constitutionalism goes beyond simply flaunting the Constitution. Playwright and actor Slyvanos Mudzvova said this board has actually been put to silence mainly artists dealing with human rights-related artistic products. “The board consists of people who have no experience in dealing with artistic products at all. Their agenda is so simple — ban anything that is critical to President Robert Mugabe and his regime. “Serious artists will not submit anything to this board as a way of protest for its composition,” said Mudzvova. Social commentator Rejoice Ngwenya said: “With the drastic modernisation of the creative industry (e-ntertainment, e-reading, the drone and virtual creations), it’s surprising that Mugabe can appoint dinosaurs, drunken with conservative stupour, to preside over 21st Century creativity. “It shows Mugabe views everything through the partisan prism, with an eye on 2018. What these human fossils do not know is that the IOT (internet of things) no longer allows political hoodlums clad in statutory censorship clothes to poison creativity.” Theatre producer Mthabisi Phili believes any sinking man will catch at a straw. “They are catching at straws now; I think Zanu PF is strengthening its censorship and control muscle ahead of the upcoming elections. “It’s more of a political move than just the employment of people. The true colours that we are under a dictatorship are really coming out through the rampant nepotism and focus


We present observations of the O VI system at z_abs = 0.495096 toward PKS 0405-123 (z_em = 0.5726) obtained with FUSE and STIS. In addition to strong O VI, with log N(O VI) = 14.47+/-0.02, and moderate H I this absorber shows C III, N IV, O IV, and O V, with upper limits for another seven ions. The large number of available ions allows us to test ionization models usually adopted with far less contraints. We find the ionic column densities cannot be matched by collisional ionization models, in or out of equilibrium. Photoionization models can match the observed column densities, including O VI. If one assumes photoionization by a UV background dominated by QSOs, the metallicity of the gas is [O/H] = -0.15, while a model for the UV background with contributions from ionizing photons escaping from galaxies gives [O/H] = -0.62. Both give [N/O] ~ -0.6 and [C/H] ~ -0.2 to -0.1. The choice of ionizing spectrum is poorly constrained. Multiphase models with a contribution from both photoionized gas (at T~10^4 K) and collisionally ionized gas (at T~(1-3)x10^5 K) can also match the observations giving very similar metallicities. The O VI in this system is not necessarily a reliable tracer of WHIM matter. We do not detect Ne VIII or Mg X absorption. The limit on Ne VIII/O VI < 0.21 (3 sigma), the lowest yet observed. Thus this absorber shows no firm evidence of the "warm-hot intergalactic medium" at T~(0.5-3)x10^6 K thought to contain a significant fraction of the baryons at low redshift. We present limits on the total column of warm-hot gas in this absorber as a function of temperature. This system would be unlikely to provide detectable X-ray absorption in the ions O VII or O VIII even.


We examine the Lagrangian divergence of the displacement field, arguably a more natural object than the density in a Lagrangian description of cosmological large-scale structure. This quantity, which we denote \psi, quantifies the stretching and distortion of the initially homogeneous lattice of dark-matter particles in the universe. \psi\ encodes similar information as the density, but the correspondence has subtleties. It corresponds better to the log-density A than the overdensity \delta. A Gaussian distribution in \psi\ produces a distribution in A with slight skewness; in \delta, we find that in many cases the skewness is further increased by 3. A local spherical-collapse-based (SC) fit found by Bernardeau gives a formula for \psi's particle-by-particle behavior that works quite well, better than applying Lagrangian perturbation theory (LPT) at first or second (2LPT) order. In 2LPT, there is a roughly parabolic relation between initial and final \psi\ that can give overdensities in deep voids, so low-redshift, high-resolution 2LPT realizations should be used with caution. The SC fit excels at predicting \psi\ until streams cross; then, for particles forming haloes, \psi\ plummets as in a waterfall to -3. This gives a new method for producing N-particle realizations. Compared to LPT realizations, such SC realizations give reduced stream-crossing, and better visual and 1-point-PDF correspondence to the results of full gravity. LPT, on the other hand, predicts large-scale flows and the large-scale power-spectrum amplitude better.


We consider a Hamiltonian action of n-dimensional torus, T^n, on a compact symplectic manifold (M,\omega) with d isolated fixed points. For every fixed point p there exists (though not unique) a class a_p in H^*_{T}(M; Q) such that the collection {a_p}, over all fixed points, forms a basis for H^*_{T}(M; Q) as an H^*(BT; Q) module. The map induced by the inclusion, \iota^*:H^*_{T}(M; Q) \rightarrow H^*_{T}(M^{T}; Q)= \oplus_{j=1}^{d}Q[x_1, ..., x_n] is injective. We use such classes {a_p} to give necessary and sufficient conditions for f=(f_1, ...,f_d) in \oplus_{j=1}^{d}Q[x_1, ..., x_n] to be in the image of \iota^*, i.e. to represent an equiviariant cohomology class on M. In the case when T is a circle and present these conditions explicitly. We explain how to combine this 1-dimensional solution with Chang-Skjelbred Lemma in order to obtain the result for a torus T of any dimension. Moreover, for a GKM T-manifold M our techniques give combinatorial description of H^*_{K}(M; Q), for a generic subgroup K \hookrightarrow T, even.