Corporation shall keep, at its principal office, a record of the names of all members having the right to vote in any proceeding of the corporation. (c) Right To Inspect Books and Records.--All books and records of the corporation may be inspected by any member having the right to vote, or by any agent or attorney of such member, for any proper purpose, at any reasonable time. (d) Application of State Law.--No provision of this section may be construed to contravene any applicable State law. SEC. 11. AUDIT OF FINANCIAL TRANSACTIONS. The first section of the Act entitled ``An Act to provide for audit of accounts of private corporations established under the Federal law'', approved August 30, 1964 (36 U.S.C. 1101), is amended by adding at the end of the following: ``Ukrainian American Veterans, Incorporated.''. SEC. 12. ANNUAL REPORT. The corporation shall annually submit to the Congress a report concerning the activities of the corporation during the preceding fiscal year. The annual report shall be submitted at the same time as is the report of the audit required by section 11. The report shall not be printed as a public document. SEC. 13. RESERVATION OF RIGHT TO AMEND OR REPEAL CHAPTER. The right to amend or repeal this Act is expressly reserved to the Congress. SEC. 14. DEFINITIONS. For purposes of this Act-- (1) the term ``corporation'' means the Ukrainian American Veterans, Incorporated; and (2) the term ``State'' means any of the several States, the District of Columbia, the Commonwealth of Puerto Rico, the Commonwealth of the Northern Mariana Islands, the Virgin Islands, Guam, American Samoa, the Trust Territories of the Pacific Islands, or any other territory or possessions of the United States. SEC. 15. TAX EXEMPT STATUS. The corporation shall maintain its status as an organization exempt from taxation as provided in the Internal Revenue Code of 1986. SEC. 16. TERMINATION. The charter granted in this Act shall expire.


Compact binary mergers are prime sources of gravitational waves, targeted by current and next generation detectors. The question "what is the observable electromagnetic (EM) signature of a compact binary merger?" is an intriguing one with crucial consequences to the quest for gravitational waves. We present a large set of numerical simulations that focus on the electromagnetic signals that emerge from the dynamically ejected sub-relativistic material. These outflows produce on a time scale of a day macronovae - short-lived IR to UV signals powered by radioactive decay. The interaction of this outflow with the surrounding matter inevitably leads to a long-lasting remnant. The expected radio signals of these remnants last longer than a year, when the sub-relativistic ejecta dominate the emission. We discuss their detectability in 1.4 GHz and 150 MHz and compare it with the detectability of short GRBs' orphan afterglows (which are produced by a different component of this outflow). Mergers with characteristics similar to those of the Galactic neutron star binary population (similar masses and typical circum-merger Galactic disk density of ~1cm^-3) taking place at the detection horizon of advanced GW detectors (300 Mpc) yield 1.4 GHz [150 MHz] signals of ~50 [300] microJy. The signal on time scales of weeks, is dominated by the mildly and/or ultra-relativistic outflow, which is not accounted for by our simulations, and is expected to be even brighter. Upcoming all sky surveys are expected to detect a few dozen, and possibly more, merger remnants at any given time thereby providing robust lower limits to the mergers rate even before the advanced GW detectorsbecome operational. Macronovae from the same distance peak in the IR to UV range at an observed magnitude that may be as bright as 22-23 about 10 hours after the merger but dimmer, redder and longer.


Can change things, that bit of jealousy seeing your rivals raising trophies aloft. In the early 90s, Down (twice), Donegal and Derry won All-Ireland titles. Every other county in the north was supporting them. It's something unique to the northern counties and it’s something you don’t get in the other three provinces. Through the tough times of the troubles, our identity was even more important. To those looking on from over the border, we were often viewed as outcasts. My own club is on the border with Armagh, but when Derry won the All-Ireland in '93 the village was packed out for the Derry team on their way home. Tyrone looked on hoping some day it would be them. That day, thankfully did come. I mentioned earlier life skills and it’s well documented the many advantages that you can take from the various battles on the field of play. There are huge benefits for people as individuals in terms of what they can learn from playing team sports. The attributes that make you a good footballer or hurler - hard work and discipline - are things that stand to you in your work life. I would like to think that football has taught me a fair bit in how to deal with situations. You play games of football and you are faced with a lot of adversity at times. You have to learn to overcome such adversity. I know players at inter-county level have put their careers on hold because of their dedication to the game. I would counterbalance that by saying that performing at a unique level teaches you a lot about the work-related environment. Teams will sit down and set goals for the year and that's something people at work will do on a regular basis. It's not surprising that businesses bring in sports people to provide insights into how you build a successful team. So much of what they have to say is about maintaining discipline and the commitment to excel in whatever you do. After winning my All-Irelands, I was on cloud nine. Life was great. Confidence was oozing out of every pore and dealing with the likes of the media was no problem. My aim was always to try and reach my potential. You think you will never get to your potential, but you will always try to get as close as you can. My motto was to aim for perfection and.


Spitzer spectroscopy has revealed that ~80% of submm galaxies (SMGs) are starburst (SB) dominated in the mid-infrared. Here we focus on the remaining ~20% that show signs of harboring powerful active galactic nuclei (AGN). We have obtained Spitzer-IRS spectroscopy of a sample of eight SMGs which are candidates for harboring powerful AGN on the basis of IRAC color-selection (S8/S4.5>2; i.e. likely power-law mid-infrared SEDs). SMGs with an AGN dominating (>50%) their mid-infrared emission could represent `missing link' sources in an evolutionary sequence involving a major merger. First of all, we detect PAH features in all of the SMGs, indicating redshifts from 2.5-3.4, demonstrating the power of the mid-infrared to determine redshifts for these optically faint dusty galaxies. Secondly, we see signs of both star-formation (from the PAH features) and AGN activity (from continuum emission) in our sample: 62% of the sample are AGN-dominated in the mid-infrared with a median AGN content of 56%, compared with <30% on average for typical SMGs, revealing that our IRAC color selection has successfully singled out sources with proportionately more AGN emission than typical SB-dominated SMGs. However, we find that only about 10% of these AGN dominate the bolometric emission of the SMG when the results are extrapolated to longer infrared wavelengths, implying that AGN are not a significant power source to the SMG population overall, even when there is evidence in the mid-infrared for substantial AGN activity. When existing samples of mid-infrared AGN-dominated SMGs are considered, we find that S8/S4.5>1.65 works well at selecting mid-infrared energetically dominant AGN in SMGs, implying a duty cycle of ~15%.


We use the Mars Regional Atmospheric Modeling System (MRAMS) to simulate lake storms on Mars, finding that intense localized precipitation will occur for lake size >=10^3 km^2. Mars has a low-density atmosphere, so deep convection can be triggered by small amounts of latent heat release. In our reference simulation, the buoyant plume lifts vapor above condensation level, forming a 20km-high optically-thick cloud. Ice grains grow to 200 microns radius and fall near (or in) the lake at mean rates up to 1.5 mm/hr water equivalent (maximum rates up to 6 mm/hr water equivalent). Because atmospheric temperatures outside the surface layer are always well below 273K, supersaturation and condensation begin at low altitudes above lakes on Mars. In contrast to Earth lake-effect storms, lake storms on Mars involve continuous precipitation, and their vertical velocities and plume heights exceed those of tropical thunderstorms on Earth. Convection does not reach above the planetary boundary layer for lakes <<10^3 km^2 or for atmospheric pressure >O(10^2) mbar. Instead, vapor is advected downwind with little cloud formation. Precipitation occurs as snow, and the daytime radiative forcing at the land surface due to plume vapor and storm clouds is too small to melt snow directly (<+10 W/m^2). However, if orbital conditions are favorable, then the snow may be seasonally unstable to melting and produce runoff to form channels. We calculate the probability of melting by running thermal models over all possible orbital conditions and weighting their outcomes by probabilities given by Laskar et al., 2004. We determine that for an equatorial vapor source, sunlight 15% fainter than at present, and snowpack with albedo 0.28 (0.35), melting may occur with 4%(0.1%) probability. This rises to 56%(12%).


. Pulaski County Circuit Judge Wendell Griffen placed a temporary restraining order on the state's ability to use the second drug in its lethal injection protocol — vecuronium bromide. Pharmaceutical company McKesson Medical-Surgical claimed the Department of Corrections essentially duped them in acquiring the drug, stating that they sold the vecuronium bromide under the pretense that it would be used for health reasons — not an execution. The state's director of the department of corrections, Wendy Kelly, disputed the charge in testimony on Thursday. But it was the judge in the pharmaceutical company's case who developed intrigue Friday evening. Soon after Griffen scheduled a hearing for Tuesday morning, he joined a protest of the executions outside the governor's mansion. To depict the inmate's experience on the Arkansas death house gurney, he strapped himself to a cot on the sidewalk outside Hutchinson's home. Judge Wendell Griffen portrays a prisoner on a gurney during a protest against executions in front of the governor's mansion in Little Rock, Ark. on April 14, 2017. Mitchell McCoy / KARK The state attorney general's office is now seeking to have him removed from the case and Republican lawmakers want him to leave the bench altogether, stating that he did not act impartially. "As a public opponent of capital punishment, Judge Griffen should have recused himself from this case," said the state attorney general's spokesman, Judd Deere. Man on cot is judge who just blocked execution of seven brutal murderers. Who thinks he's impartial & fair in death-penalty cases? https://t.co/VrUOSvCcdz — Tom Cotton (@TomCottonAR) April 15, 2017 But for now, that case floats in a new state of legal limbo. McKesson, the pharmaceutical company, is seeking to drop its lawsuit and vacate the temporary restraining order against its drug after Baker's temporary injunction, but it plans to bring its lawsuit up again.


Os, undefeated? YM; Towards the end. We care about the game, like I said we wanted to win the game, but it was not about what the results showed, it was about what we did for our people in Puerto Rico. We were down (in the championship game) by seven, eight runs and you see the people in the stands chanting, screaming, dancing and having fun. That’s the point, when you play for your country and you see the people enjoying the game, being Puerto Rican that is the reason. LS: Yadier, you have been lucky playing in the biggest of games in baseball (World Series) and you have been in the World Classic games. What is the difference? YM: I have not been lucky, I have been blessed. I work hard for that and both are amazing. I play for St. Louis, but when you play in the World Classic your playing for your parents, for your cousins, for your uncles. It’s about your grandma; it’s about your grandpa, its different. Obviously you care about wining, but the classic is about your country. LS: All of you guys did so much more than many even politicians, or other leaders were able to do by bringing an entire country and people together. Congratulations. Also what do you think of Latino Sports having an award for the Latino players? YM: That’s the goal no matter where you are at to represent your country. You can be Dominican, Mexican from Venezuela wherever you come from your going to put your best and when you see the support that our people bring to us every night here in the states that is amazing. It makes you work harder, it makes you want to do the best that you can do for them. It’s an amazing feeling. LS: So hopefully, before this season ends we in Latino Sports want to make sure that you have something to take with you that your grandchildren will remember, a museum piece (both laugh. A LatinoMVP award painting by famed artist, James Fiorentino). YM: Thank you, thank you. It’s a great honor for me to be able to receive that. Hopefully, I can be there for that day, I’m going to do by best to be there, but.


In a further development of a deterministic planet-formation model (Ida & Lin 2004), we consider the effect of type-I migration of protoplanetary embryos due to their tidal interaction with their nascent disks. During the early embedded phase of protostellar disks, although embryos rapidly emerge in regions interior to the ice line, uninhibited type-I migration leads to their efficient self-clearing. But, embryos continue to form from residual planetesimals at increasingly large radii, repeatedly migrate inward, and provide a main channel of heavy element accretion onto their host stars. During the advanced stages of disk evolution (a few Myr), the gas surface density declines to values comparable to or smaller than that of the minimum mass nebula model and type-I migration is no longer an effective disruption mechanism for mars-mass embryos. Over wide ranges of initial disk surface densities and type-I migration efficiency, the surviving population of embryos interior to the ice line has a total mass several times that of the Earth. With this reservoir, there is an adequate inventory of residual embryos to subsequently assemble into rocky planets similar to those around the Sun. But, the onset of efficient gas accretion requires the emergence and retention of cores, more massive than a few M_earth, prior to the severe depletion of the disk gas. The formation probability of gas giant planets and hence the predicted mass and semimajor axis distributions of extrasolar gas giants are sensitively determined by the strength of type-I migration. We suggest that the observed fraction of solar-type stars with gas giant planets can be reproduced only.


A wind energy development company is ‘disappointed’ at a decision by planners to reject its scheme for a 10-turbine wind farm on Fulbeck Airfield. South Kesteven District Council officers have refused the application for the 110m-high wind turbines under delegated powers. Should the applicant, Energiekontor, want to appeal the decision to the Planning Inspectorate it has six months to do so. Michael Briggs from Energiekontor UK, said: “We are obviously very disappointed with the council’s decision to refuse the planning application, as will be the hundreds of people who have written in to express their support for the project. “The wind farm would have delivered many benefits to the local and wider area which are now in doubt, particularly in relation to the economy, as numerous local construction companies were hoping the project would come forward. “At the same time, we fully understand the reasons why many have expressed their objections to the project and have always tried to do our best to address those concerns. “But the council was of the view that concerns in relation to landscape and cultural heritage issues were not outweighed by the benefits from the wind farm. We will need to look at the council’s reasons closely with our team before deciding what next for Fulbeck Airfield.” Planning officers said they refused the wind farm on the former wartime airfield on a number of grounds, including its potentially adverse visual and physical impact on the landscape and on the settings of numerous ‘high grade’ heritage assets. Concerns were also raised over an adverse impact on air safety through interference with aircraft radar and conflict with government policy. They further pointed to a Written Ministerial Statement from June 18, 2015, in which it states wind energy development should be in areas specified in local plans as being suitable for such development, and that wind farms should have the backing of local people. Local campaigning residents are delighted and relieved having seen a smaller project two miles away at Temple Hill rejected two years ago. Paul Miley of local anti-wind farm group reVOLT/VETO said: “Now the community asks that the developer respects local democracy and does not seek to appeal this decision.” He said: “An appeal would be an expensive and time consuming process both for the council and the community.” However, he did say ‘local people are ready to continue the fight.


Except for the fact that it is not a trust, constitute an individual investment account described in subsection (b). For purposes of this title, in the case of a custodial account treated as a trust by reason of the preceding sentence, the custodian of such account shall be treated as the trustee thereof. ``(g) Reports.--The trustee of an individual investment account shall make such reports regarding such account to the Secretary and to the individual for whose benefit the account is maintained with respect to contributions, distributions, and such other matters as the Secretary may require under regulations. The reports required by this subsection shall be filed at such time and in such manner and furnished to such individuals at such time and in such manner as may be required by those regulations.''. (b) Deduction Allowed in Arriving at Adjusted Gross Income.-- Subsection (a) of section 62 of such Code (defining adjusted gross income) is amended by inserting after paragraph (17) the following new paragraph: ``(18) Individual investment account contributions.--The deduction allowed by section 222 (relating to individual investment accounts).'' (c) Individual Investment Accounts Exempt From Estate Tax.--Part III of subchapter A of chapter 11 of such Code is amended by redesignating section 2046 as section 2047 and by inserting after section 2045 the following new section: ``SEC. 2046. INDIVIDUAL INVESTMENT ACCOUNTS. ``Notwithstanding any other provision of law, there shall be excluded from the value of the gross estate of the value of any individual investment account (as defined in section 222(b)). Section 1014 shall not apply to such accounts.'' (d) Tax on Prohibited Transactions.--Section 4975 of such Code (relating to prohibited transactions) is amended-- (1) by adding at the end of subsection (c) the following new paragraph: ``(6) Special rule for individual investment accounts.--An individual for whose benefit an individual investment account is established shall be exempt from the tax imposed by this section with respect to any transaction concerning such account (which would otherwise be taxable under this section) if, with respect to such transaction, the account ceases to be an individual investment account by reason of the application of section 222(d)(2)(A) to such account.''; and (2) in subsection (e)(1), by striking ``or'' at the end of subparagraph (E


Given a group G, the model \mathcal{G}(G,p) denotes the probability space of all Cayley graphs of G where each element of the generating set is chosen independently at random with probability p. Given a family of groups (G_k) and a c \in \mathbb{R}_+ we say that c is the threshold for diameter 2 for (G_k) if for any \varepsilon > 0 with high probability \Gamma \in \mathcal{G}(G_k,p) has diameter greater than 2 if p \leqslant \sqrt{(c - \eps)\frac{\log{n}}{n}} and diameter at most 2 if p \geqslant \sqrt{(c + \eps)\frac{\log{n}}{n}}. In [5] we proved that if c is a threshold for diameter 2 for a family of groups (G_k) then c \in [1/4,2] and provided two families of groups with thresholds 1/4 and 2 respectively. In this paper we study the question of whether every c \in [1/4,2] is the threshold for diameter 2 for some family of groups. Rather surprisingly it turns out that the answer to this question is negative. We show that every c \in [1/4,4/3] is a threshold but a c \in (4/3,2] is a threshold.


The impact of a random disorder potential on the dynamical properties of Bose Einstein condensates is a very wide research field. In microcavities, these studies are even more crucial than in the condensates of cold atoms, since random disorder is naturally present in the semiconductor structures. In this chapter, we consider a stable condensate, defined by a chemical potential, propagating in a random disorder potential, like a liquid flowing through a capillary. We analyze the interplay between the kinetic energy, the localization energy, and the interaction between particles in 1D and 2D polariton condensates. The finite life time of polaritons is taken into account as well. In the first part, we remind the results of [G. Malpuech et al. Phys. Rev. Lett. 98, 206402 (2007).] where we considered the case of a static condensate. In that case, the condensate forms either a glassy insulating phase at low polariton density (strong localization), or a superfluid phase above the percolation threshold. We also show the calculation of the first order spatial coherence of the condensate versus the condensate density. In the second part, we consider the case of a propagating non-interacting condensate which is always localized because of Anderson localization. The localization length is calculated in the Born approximation. The impact of the finite polariton life time is taken into account as well. In the last section we consider the case of a propagating interacting condensate where the three regimes of strong localization, Anderson localization, and superfluid behavior are accessible. The localization length is calculated versus the system parameters. The localization length is strongly modified with respect to the non-interacting case. It is infinite in the superfluid regime whereas it is strongly reduced.


Suggested by Leggett, indicates supersolid behavior, we make a number of remarks about both theory and experiment. (1) The long-wavelength, low-frequency ("hydrodynamic") part of the theory of Andreev and Lifshitz has nine variables, and thus must have nine modes. We find a new mode associated with lattice point diffusion (and thus vacancy diffusion); it may explain the absence of supersolid behavior in low-frequency pressure-driven flow. (2) The observed upper limit for the NCRI fraction (NCRIf) of about 20%, in disordered samples, is more-or-less the same as the already predicted upper limit for the superfluid fraction of a well-ordered crystal; we argue that this may not be a coincidence. (3) The negative experimental evidence for a second propagating hydrodynamic mode (expected to be fourth sound-like) may be due to the long relaxation times $\tau$ at low temperature $T$; only for frequencies satisfying $\omega\tau\ll1$ does the hydrodynamic theory apply. (4) The fundamental principles of quantum mechanics imply that Bose-Einstein condensation is not necessary to define a quantum-mechanical phase; therefore the absence of a finite condensate fraction $f_{0}$ does not necessarily imply the absence of superfluidity. (5) Just as vortices should avoid occupied lattice sites to provide a vortex-lattice interaction, the lattice should interact with the vortices to provide a lattice-vortex interaction; thus dislocations should interact with vortices, whose motion is affected by rotation. We discuss some experimental implications for the vortex liquid model, shear response, hysteresis, and relaxation.


By using a string-inspired modular invariant supergravity, which was proved well to explain WMAP observations appropriately, a mechanism of supersymmetry breaking (SSB) and Gravitino Production just after the end of inflation are investigated. Supersymmetry is broken mainly by F-term of the inflaton superfield and the Goldstino is identified to be inflatino in this model, which fact is shown numerically. By using the canonically normalized and diagonalized scalars, the decay rates of these fields are calculated, for both the $T$ and $Y$ into gravitinos. Non-thermal production of gravitinos is not generated from the inflaton (dilaton), since the inflaton mass is lighter than gravitino, but they are produced by the decay of modular field $T$ and scalar field $Y$. Because the reheating temperature $T_R$ is about order $\sim O(10^{10})$ GeV and the mass of gravitino is $3.16 \times 10^{12}$ GeV, it is not reproduced after the reheating of the universe. The gravitinos are produced almost instantly just after the end of inflation through $Y$ and $T$, not from inflaton. Because the decay time appears very rapid, gravitinos disappear before the BBN stage of the universe. The effects of the lightest supersymmetric particles (LSP) produced by gravitinos may be important to investigate more carefully.


We study spontaneous symmetry breaking in a system of two parallel quasi-one-dimensional traps, equipped with optical lattices (OLs) and filled with a Bose-Einstein condensate (BEC). The cores are linearly coupled by tunneling. Analysis of the corresponding system of linearly coupled Gross-Pitaevskii equations (GPEs) reveals that spectral bandgaps of the single GPE split into subgaps. Symmetry breaking in two-component BEC solitons is studied in cases of the attractive (AA) and repulsive (RR) nonlinearity in both traps; the mixed situation, with repulsion in one trap and attraction in the other (RA), is considered too. In all the cases, stable asymmetric solitons are found, bifurcating from symmetric or antisymmetric ones (and destabilizing them), in the AA and RR systems, respectively. In either case, bi-stability is predicted, with a nonbifurcating stable branch, either antisymmetric or symmetric, coexisting with asymmetric ones. Solitons destabilized by the bifurcation tend to rearrange themselves into their stable asymmetric counterparts. The impact of a phase mismatch, between the OLs in the two cores is also studied. Also considered is a related model, for a binary BEC in a single-core trap with the OL, assuming that the two species (representing different spin states of the same atom) are coupled by linear interconversion. In that case, the symmetry-breaking bifurcations in the AA and RR models switch their character.


One of those bald cap masks with the Bozo hair and glasses and nose and then she walked me around the back lot. Related: Critic's Notebook: Carrie Fisher, Child of Hollywood and Droll Observer of Celebrity The lengths I would go to hear her laugh - there were no limits. I loved her and loved making her laugh. She would do these crazy things and make me do these crazy things, but I really don't think they were crazy after all. In a way, it was a defense mechanism for her. She was so off the wall, she could use it as protection. Part of what was so poignant about her was that she was vulnerable, that there was this glimmer of a little girl that was so appealing and it roused the protective nature in my personality. I'm grateful that we stayed friends and got to have this second act with the new movies. I think it was reassuring to her that I was there, the same person, that she could trust me, as critical as we could sometimes be with each other. We ran the gamut over the years, where we were in love with each other, where we hated each other's guts. "I'm not speaking to you, you're such a judgmental, royal brat!" We went through it all. It's like we were a family. When you were in her good graces, you couldn't have more fun with any person on the planet. She was able to make you feel like you were the most important thing in her life. I think that's a really rare quality. And then you could go 180 degrees opposite, where you were furious with one another and wouldn't speak for weeks and weeks. But that's all part of what makes a relationship complete. It's not all one sided. Like I say, she was a handful. She was high maintenance. But my life would have been so much drabber and less interesting.


We re-visit the role of their annihilation on the temperature of diffuse gas in the high redshift universe. We consider neutralinos of particle mass 36 GeV and 100 GeV, respectively. The former is able to produce ~7 electron/positron particles per annihilation through the fremionic channel, and the latter ~53 particles assuming a purely bosonic channel. High energy electron/positron particles up-scatter the Cosmic Microwave Background (CMB) photons into higher energies via the inverse-Compton scattering. The process produces a power-law electron/positron energy spectrum of index -1 in the energy range of interest, independent of the initial energy distribution. The corresponding energy spectrum of the up-scattered photons is a power-law of index -1/2, if absorption by the gas is not included. The scattered photons photo-heat the gas by releasing electrons which deposit a fraction (14%)of their energy as heat into the ambient medium. For uniformly distributed neutralinos the heating is insignificant. The effect is greatly enhanced by the clumping of neutralinos into dense haloes. We use a time-dependent clumping model which takes into account the damping of density fluctuations on mass scales smaller than ~10^{-6}M_sol. With this clumping model, the heating mechanism boosts the gas temperature above that of the CMB after a redshift of z 30. By z\approx 10 the gas temperature is nearly 100 times its temperature when no heating is invoked. Similar increase is obtained for the two neutralino masses considered.


The growth of the supermassive black holes (BHs) that reside at the centres of most galaxies is intertwined with the physical processes that drive the formation of the galaxies themselves. The evolution of the relations between the mass of the BH, m_BH, and the properties of its host therefore represent crucial aspects of the galaxy formation process. We use a cosmological simulation, as well as an analytical model, to investigate how and why the scaling relations for BHs evolve with cosmic time. We find that a simulation that reproduces the observed redshift zero relations between m_BH and the properties of its host galaxy, as well as the thermodynamic profiles of the intragroup medium, also reproduces the observed evolution in the ratio m_BH/m_s for massive galaxies, although the evolution of the m_BH/sigma relation is in apparent conflict with observations. The simulation predicts that the relations between m_BH and the binding energies of both the galaxy and its dark matter halo do not evolve, while the ratio m_BH/m_halo increases with redshift. The simple, analytic model of Booth & Schaye (2010), in which the mass of the BH is controlled by the gravitational binding energy of its host halo, quantitatively reproduces the latter two results. Finally, we can explain the evolution in the relations between m_BH and the mass and binding energy of the stellar component of its host galaxy for massive galaxies (m_s~10^11 M_sun) at low redshift (z<1).


Equivocation rate has been widely used as an information-theoretic measure of security after Shannon[10]. It simplifies problems by removing the effect of atypical behavior from the system. In [9], however, Merhav and Arikan considered the alternative of using guessing exponent to analyze the Shannon's cipher system. Because guessing exponent captures the atypical behavior, the strongest expressible notion of secrecy requires the more stringent condition that the size of the key, instead of its entropy rate, to be equal to the size of the message. The relationship between equivocation and guessing exponent are also investigated in [6][7] but it is unclear which is a better measure, and whether there is a unifying measure of security. Instead of using equivocation rate or guessing exponent, we study the wiretap channel in [2] using the success exponent, defined as the exponent of a wiretapper successfully learn the secret after making an exponential number of guesses to a sequential verifier that gives yes/no answer to each guess. By extending the coding scheme in [2][5] and the converse proof in [4] with the new Overlap Lemma 5.2, we obtain a tradeoff between secrecy and reliability expressed in terms of lower bounds on the error and success exponents of authorized and respectively unauthorized decoding of the transmitted messages. From this, we obtain an inner bound to the region of strongly achievable public, private and guessing rate triples for which the exponents are strictly positive. The closure of this region is equivalent to the closure of the region in Theorem 1 of [2] when we treat equivocation rate as the guessing rate. However, it is unclear.


Purpose of including such information in the timely reports required under this paragraph; and ``(III) ensure that when a crime of violence (as defined in section 16 of title 18, United States Code) is reported to a campus security authority, the authority reports the crime to local law police agencies; ``(ii) establish policies or procedures for training campus security authorities and the campus security authority coordinator; and ``(iii) employ or designate an individual or other entity to conduct such training using the policies or procedures established under clause (ii), upon receiving approval from the Secretary for such individual or other entity to conduct such training.''; (4) in paragraph (13)-- (A) by striking ``Upon'' and inserting ``(A) Upon''; (B) by inserting ``which distinguishes between institutional neglect and intentional misrepresentation or withholding of information,'' after ``this subsection,''; (C) by inserting ``, except that the Secretary shall impose a larger civil penalty in the case of an institution of higher education determined to have intentionally violated this subsection, as compared to an institution of higher education that violated this subsection as a result of institutional neglect. An intentional violation of this subsection by an institution of higher education shall be subject to criminal prosecution'' after ``under section 487(c)(3)(B)''; and (D) by adding at the end the following: ``(B) Prior to making a determination described in subparagraph (A) with respect to an institution of higher education, the Secretary shall-- ``(i) conduct an investigation with respect to the institution; and ``(ii) provide the institution with a timeline of the investigation and a preliminary report that includes the reasons for conducting such investigation.''; and (5) in paragraph (17), before the period insert the following: ``or any individual because such individual provided information or made a complaint to a law enforcement agency relating to the implementation of any provision of this subsection.


We study the quantum phase transition from a super solid phase to a solid phase of rho = 1/2 for the extended Bose-Hubbard model on the honeycomb lattice using first principles Monte Carlo calculations. The motivation of our study is to quantitatively understand the impact of theoretical input, in particular the dynamical critical exponent z, in calculating the critical exponent nu. Hence we have carried out four sets of simulations with beta = 2N^{1/2}, beta = 8N^{1/2}, beta = N/2, and beta = N/4, respectively. Here beta is the inverse temperature and N is the numbers of lattice sites used in the simulations. By applying data collapse to the observable superfluid density rho_{s2} in the second spatial direction, we confirm that the transition is indeed governed by the superfluid-insulator universality class. However we find it is subtle to determine the precise location of the critical point. For example, while the critical chemical potential (mu/V)_c occurs at (mu/V)_c = 2.3239(3) for the data obtained using beta = 2N^{1/2}, the (mu/V)_c determined from the data simulated with beta = N/2 is found to be (mu/V)_c = 2.3186(2). Further, while a good data collapse for rho_{s2}N can be obtained with the data determined using beta = N/4 in the simulations, a reasonable quality of data collapse for the same observable calculated from another set of simulations with beta = 8N^{1/2} can hardly be reached. Surprisingly, assuming z for this phase transition is determined to be 2 first in a Monte Carlo calculation, then a high quality data collapse for rho_{s2}N can be achieved for (mu/V)_c ~ 2.3184 and nu ~ 0.7 using the data obtained with beta = 8N^{1/2}. Our results imply that one might need to reconsider the established phase diagrams of some models.


We have detected narrow HI 21cm and CI absorption at $z \sim 1.4 - 1.6$ towards Q0458$-$020 and Q2337$-$011, and use these lines to test for possible changes in the fine structure constant $\alpha$, the proton-electron mass ratio $\mu$, and the proton gyromagnetic ratio $g_p$. A comparison between the HI 21cm and CI line redshifts yields $\Delta X/X = [+6.8 \pm 1.0] \times 10^{-6}$ over $0 < <z> \le 1.46$, where $X = g_p \alpha^2/\mu$, and the errors are purely statistical, from the gaussian fits. The simple line profiles and the high sensitivity of the spectra imply that statistical errors in this comparison are an order of magnitude lower than in previous studies. Further, the CI lines arise in cold neutral gas that also gives rise to HI 21cm absorption, and both background quasars are core-dominated, reducing the likelihood of systematic errors due to local velocity offsets between the hyperfine and resonance lines. The dominant source of systematic error lies in the absolute wavelength calibration of the optical spectra, which appears uncertain to $\sim 2$ km/s, yielding a maximum error in $\Delta X/X$ of $\sim 6.7 \times 10^{-6}$. Including this, we obtain $\Delta X/X = [+6.8 \pm 1.0 (statistical) \pm 6.7 (max. systematic)] \times 10^{-6}$ over $0 < <z> \le 1.46$. Using literature constraints on $\Delta \mu/\mu$, this is inconsistent with claims of a smaller value of $\alpha$ from the many-multiplet method.


.''. (b) Effective Date.--The amendment made by this section shall apply to taxable years beginning after December 31, 2013. SEC. 105. LIMITATION ON DEDUCTION FOR TERTIARY INJECTANTS. (a) In General.--Section 193 of the Internal Revenue Code of 1986 is amended by adding at the end the following new subsection: ``(d) Application With Respect to Major Integrated Oil Companies.-- This section shall not apply to amounts paid or incurred by a taxpayer in any taxable year in which such taxpayer is a major integrated oil company (as defined in section 167(h)(5)(B)).''. (b) Effective Date.--The amendment made by this section shall apply to amounts paid or incurred in taxable years beginning after December 31, 2013. Subtitle B--Outer Continental Shelf Oil and Natural Gas SEC. 111. REPEAL OF OUTER CONTINENTAL SHELF DEEP WATER AND DEEP GAS ROYALTY RELIEF. (a) In General.--Sections 344 and 345 of the Energy Policy Act of 2005 (42 U.S.C. 15904, 15905) are repealed. (b) Limitation on Application.--The repeal under subsection (a) shall not affect the application of the repealed sections with respect to any lease sale for which a notice of sale is published before the date of enactment of this Act. TITLE II--BUDGETARY EFFECTS SEC. 201. DEFICIT REDUCTION. The net amount of any savings realized as a result of the enactment of this Act and the amendments made by this Act (after any expenditures authorized by this Act and the amendments made by this Act) shall be deposited in the Treasury and used for Federal budget deficit reduction or.


Using Chebyshev polynomials combined with some mild combinatorics, we provide a new formula for the analytical planar limit of a random matrix model with a one-cut potential $V$. For potentials $V(x)=x^{2}/2-\sum_{n\ge1}a_{n}x^{n}/n$, as a power series in all $a_{n}$, the formal Taylor expansion of the analytic planar limit is exactly the formal planar limit. In the case $V$ is analytic in infinitely many variables $\{a_{n}\}_{n\ge1}$ (on the appropriate spaces), the planar limit is also an analytic function in infinitely many variables and we give quantitative versions of where this is defined. Particularly useful in enumerative combinatorics are the gradings of $V$, $V_{t}(x)=x^{2}/2-\sum_{n\ge1}a_{n}t^{n/2}x^{n}/n$ and $V_{t}(x)=x^{2}/2-\sum_{n\ge3}a_{n}t^{n/2 -1}x^{n}/n$. The associated planar limits $F(t)$ as functions of $t$ count planar diagram sorted by the number of edges respectively faces. We point out a method of computing the asymptotic of the coefficients of $F(t)$ using the combination of the \emph{wzb} method and the resolution of singularies. This is illustrated in several computations revolving around the important extreme potential $V_{t}(x)=x^{2}/2+\log(1-\sqrt{t}x)$ and its variants. This particular example gives a quantitive and sharp answer to a conjecture of t'Hoofts which states that.


A new determination of the sound horizon scale in angular coordinates is presented. It makes use of ~ 0.6 x 10^6 Luminous Red Galaxies, selected from the Sloan Digital Sky Survey imaging data, with photometric redshifts. The analysis covers a redshift interval that goes from z=0.5 to z=0.6. We find evidence of the Baryon Acoustic Oscillations (BAO) signal at the ~ 2.3 sigma confidence level, with a value of theta_{BAO} (z=0.55) = (3.90 \pm 0.38) degrees, including systematic errors. To our understanding, this is the first direct measurement of the angular BAO scale in the galaxy distribution, and it is in agreement with previous BAO measurements. We also show how radial determinations of the BAO scale can break the degeneracy in the measurement of cosmological parameters when they are combined with BAO angular measurements. The result is also in good agreement with the WMAP7 best-fit cosmology. We obtain a value of w_0 = -1.03 \pm 0.16 for the equation of state parameter of the dark energy, Omega_M = 0.26 \pm 0.04 for the matter density, when the other parameters are fixed. We have also tested the sensitivity of current BAO measurements to a time varying dark energy equation of state, finding w_a = 0.06 \pm 0.22.


From warehouse for consumption, on or after December 1, 2007. (f) Reliquidation of Entries.-- (1) In general.--Notwithstanding section 514 of the Tariff Act of 1930 (19 U.S.C. 1514) or any other provision of law and subject to the provisions of paragraph (2), the U.S. Customs and Border Protection shall, not later than 90 days after the receipt of a request described in paragraph (2), liquidate or reliquidate as applicable any entry described in paragraph (4) at the applicable rate under subchapter II of chapter 99 of the Harmonized Tariff Schedule of the United States, as amended by subsection (d). (2) Requests.--Liquidation or reliquidation may be made under paragraph (1) with respect to an entry described in paragraph (4) only if-- (A) a request therefore is filed with U.S. Customs and Border Protection not later than 90 days after the date of the enactment of this Act; and (B) the request contains sufficient information to enable U.S. Customs and Border Protection to locate the entry or reconciliation entry if it cannot be located. (3) Payment of amounts owed.--Any amounts owed by the United States pursuant to the liquidation or reliquidation of any entry under paragraph (1) shall be paid, with interest, not later than 180 days after the date of such liquidation or reliquidation. (4) Entries described.--The entries referred to in paragraph (1) are the entries, or withdrawals from warehouse for consumption, of goods to which duty-free treatment is provided by subsections (d) and (e)-- (A) that was made on or after December 1, 2007; and (B) with respect to which there would have been no duty.


With high resolution (0.46kpc/h), adaptive mesh-refinement Eulerian cosmological hydrodynamic simulations we compute properties of O VI and O VII absorbers from the warm-hot intergalactic medium (WHIM). Our new simulations are in broad agreement with previous simulations, with ~40% of the intergalactic medium being in the WHIM at z=0. It is found (1) The amount of gas in the WHIM at temperature below and above 10^6K is about equal within uncertainties. (1) Our simulations are in excellent agreement with observed properties of O VI absorbers, with respect to the line incidence rate and Doppler width-column density relation. (2) Velocity structures within absorbing regions are a significant, and for large Doppler width clouds, a dominant contributor to the Doppler widths of both O VI and O VII absorbers. A non-negligible fraction (in number and mass) of O VI and O VII clouds can arise from gas of temperature lower than 10^5, until the Doppler width is well in excess of 100km/s. (3) Strong O VI absorbers are predominantly collisionally ionized. About (61%, 57%, 39%) of O VI absorbers in the column density ranges of log N(OVI) cm^2=(12.5-13,13-14,>14) have temperature lower than 10^5K. (4) Quantitative prediction is made for the presence of broad and shallow O VI lines, which current observations may have largely missed. Upcoming observations by COS may be able to provide a test. (5) The reported 3 sigma upper limit on the mean column density of coincidental O VII lines at the location of detected O VI lines by Yao et al is above the predicted value by a factor of 2.5-4. (6) The claimed observational detection of O VII lines by Nicastro et al.


This act or any compact may be construed to limit the applicability of any Federal law or to diminish or to otherwise impair the jurisdiction of any action taken pursuant to any compact. ``(C) State authority preserved.--Except as expressly provided in this Act, nothing contained in this Act expands, diminishes, or otherwise affects State law. ``(3) Restricted Use of Regional Solid Waste Disposal Facilities.-- Any authority in a compact to restrict the use of regional solid waste disposal facilities under the compact to the disposal of solid waste generated within the compact region shall not take effect before each of the following occurrs: ``(1) January 1, 1995; and ``(2) the Congress by law consents to the compact. ``(4) Congressional Review.--Each compact shall: Provide, That every 5 years after the compact has taken effect the Congress may by law withdraw its consent. ``(c) Alternative Solid Waste Disposal Methods.-- ``(1) Not later than 12 months after the date of enactment of the Solid Waste Compact Act of 1993, the Environmental Protection Agency shall, in consultation with the States and other interested persons, identify potential alternative management programs for the control of solid waste, and establish and publish technical guidance regarding the implementation of such programs. ``(2) Not later than 24 months after the date of the enactment of the Solid Waste Compact Act of 1993, the Environmental Protection Agency shall, in consultation with the States and other interested persons, identify and publish all relevant technical information regarding the technologies pursuant to subsection (1) that a State or compact must provide to the Agency in order to pursue such programs, together with the requirements that such facilities must meet, in the judgment of the Agency.


Who've recently resigned after allegations of sexual misconduct. Humphreys has not responded to requests from The Associated Press for comment. ___ 12:15 p.m. The president of the University of Oklahoma is distancing himself from comments made by a Board of Regents member who compared gay people to pedophiles. University President David Boren said in a statement Monday that board member and former Oklahoma City Mayor Kirk Humphreys wasn't speaking on behalf of the university. Boren also says he doesn't share Humphreys' views and that the university is a diverse and inclusive family. Humphreys made the comments during a local TV public affairs show that aired over weekend on KFOR-TV. He also compared gay people to politicians who've recently resigned after allegations of sexual misconduct. A staffer at Humphreys' office says he was out of town Monday and unavailable to comment. Humphreys also didn't immediately reply to an email seeking comment from The Associated Press. ___ 10:55 a.m. A former Oklahoma City mayor and member of the University of Oklahoma Board of Regents is being criticized for comparing gay people to pedophiles. Kirk Humphreys made the comments over the weekend on KFOR-TV's public affairs show. He also compared gay people to politicians who've recently resigned after allegations of sexual misconduct. LGBTQ advocacy group Freedom Oklahoma has called for his removal from the board if he doesn't apologize. Executive Director Troy Stevenson says Humphreys' comments were disheartening and dangerous for LGBTQ youth who are already harassed and bullied. A staffer at Humphreys' office said he was out of town Monday and unavailable to comment. Stevenson said Monday his group will protest an Oklahoma City real estate project that belongs to Humphreys' family business.


Angela Eagle and Imran Ahmed’s new book “The New Serfdom“, a 400-page hatchet job on the great liberal thinker Friedrich Hayek, is being lauded with praise in Labour circles, most effusively from Nick Cohen. Guido must come to Hayek’s defence in the face of their rewriting of history. The New Serfdom is a reminder that, even as the relatively moderate challenger to Corbyn, Eagle is still a liberty-hating socialist who opposes free markets and fundamentally values the state over the freedom of the individual. Even Ed Miliband’s office warned that Ahmed was “dangerously left-wing” when he became a Shadow Cabinet adviser. Their book condemns the “veneration of markets”, the “infiltration of marketisation” into the public sector, capitalism’s promotion of competition, the “toxic culture” of admiring those who succeed, and calls for a Labour government to create an “empowered state… pursuing a reinvigorated democratic socialism”. It wants to sweep back Thatcher’s trade union reforms, regulate the food and drink industry to the hilt and put taxes through the roof. It offers a depressing view of Britain today, talking the country down as “divided and resentful”, dismisses capitalist liberal democracy as a “con”, calls Hayek a “liar” with “extreme views” who inspired Thatcher and her “successor” Trump, and claims Brexit is evidence of “the extreme right on the march”. According to the respected academic Chris Hanretty, Eagle’s Wallasley seat voted 53% to Leave… The history of the last century comprehensively proved correct Hayek’s central assertion that socialism morphs into totalitarianism. He was proved right when the Keynesian post-war consensus collapsed and Thatcher used his ideas – “this is what we believe” – to turn the economy around. The New Serfdom is an unashamedly socialist critique of the last forty years of British political life, and so is as dangerous and wrong as you would expect. The key question for Eagle and Ahmed:?


Then the manufacturer, distributor, or retailer shall elect to take one of those actions.''. (b) Hazardous Substances Amendment.--Section 15(b) of the Federal Hazardous Substances Act (15 U.S.C. 1274(b)) is amended-- (1) by striking ``Refund.--If'' and inserting ``Refund.-- Except as provided in paragraph (3), if''; (2) by striking ``(1) If'' and inserting ``(A) Repair.-- If''; (3) by striking ``(2)'' and inserting ``(B) Replacment.-- ''; (4) by striking ``(3)'' and inserting ``(C) Refund.--''; (5) by redesignating subparagraphs (A) and (B) of paragraph (3) as clauses (i) and (ii), respectively; (6) by striking ``An order'' the first place it appears and inserting ``(2) An order''; (7) by striking ``paragraph (3).'' and inserting ``paragraph (1)(C)''; and (8) by adding at the end thereof the following: ``(3) If the Commission determines, after affording opportunity for an informal hearing, that the action elected by a manufacturer, distributor, or retailer under paragraph (1)(A), (B), or (C) is not in the public interest, the Commission shall order the manufacturer, distributor, or retailer to take any other action described in paragraph that the Commission determines to be in the public interest. If the Commission determines that both of the remaining actions for election under paragraph (1) are in the public interest, then the manufacturer, distributor, or retailer shall elect to take one of those actions.''. (c) Discretionary Remedial Action Under the FHSA.--Section 1274(c) of the Federal Hazardous Substances Act (15 U.S.C. 1274(c) is amended-- (1) by striking ``(2) If'' and inserting ``(2) Except as provided in paragraph (3), if''; and (2) adding at the end thereof the following: ``(3) If the Commission determines, after affording opportunity for an informal hearing, that the action elected by a manufacturer, distributor, or retailer under paragraph (2)(A), (B), or (C) is not in


With a comprehensive understanding of gender, consent, and the critical issues at the center of the movement. Please read through their answers and jump into the comments with your thoughtful, balanced reactions. We think this is a discussion that is important and ongoing. Unsplash Lucia When I ask my guy friends, I haven’t found anyone who understands that they have a “gender.” They all think that the only thing that makes them a man is their junk, but I’m trying to understand the idea of gender outside of genitalia. Any chance you can help me with that — in straightforward terms? Dr. Casey Brienza, sociologist and author: Sex is determined by biology, whereas gender is determined by society and culture. Does a man have to show you his “junk” to assert his gender identity? Probably not. Other cues, such as dress, hairstyle, body language, speech patterns, etc. are usually sufficient, and the very fact that these may differ in different parts the world tells us that they are not inherent. Or, for that matter, immutable. Dr. Chauntelle Tibbals, sociologist and author: In sociology and social-psychology circles, this is often discussed as a (problematic, obvs) dimension of the “default person.” The default person is male, heterosexual, able-bodied, white, etc. As a society, we spent a lot of time using that default person/experience as the neutral guide for structuring society. So, to your question, we are talking “males don’t have a gender because they are conceptualized as the social default/generic”-type of thing. A gender is something that’s added in as an extra to move a human away from the “default” experience – and within this system and process, the penis has become a sort of symbolic embodiment of that default entity. It’s interesting to me too how this taps into interlocking systems of privileges and oppression. Like, a man may have none of those other “default” characteristics, but.


As is generally presumed, then one would not expect to observe indicators of activity in stars with T_eff > 8300 K. Any X-ray or ultraviolet line emission from hotter stars must be due either to a different mechanism or to an unresolved, active, binary companion. Due to their poor spatial resolution, X-ray instruments have been especially susceptible to source confusion. At wavelengths longward of 1216 Angstroms, the near ultraviolet spectra of stars hotter than this putative dividing line are dominated by photospheric continuum. We have used FUSE to obtain spectra of the subcoronal O VI emission lines, which lie at a wavelength where the photospheric continuum of the mid- and early-A stars is relatively weak. We observed 14 stars spanning a range in T_eff from 7720 to 10,000 K. Eleven of the 14 stars showed O VI emission lines, including 6 of the 8 targets with T_eff > 8300 K. At face value, this suggests that activity does not fall off with increasing temperature. However, the emission lines are narrower than expected from the projected rotational velocities of these rapidly-rotating stars, suggesting that the emission could come from unresolved late-type companions. Furthermore, the strength of the O VI emission is consistent with that expected from an unseen active K or M dwarf binary companinon, and the high x-ray to far uv luminosity ratios observed indicate that this must be the case. Our results are therefore consistent with earlier studies that have shown a rapid drop-off in activity at the radiative/convective boundary expected at T_eff about 8300 K, in agreement with conventional stellar structure models.


Entire Community Of Muslims Are Rounded Up And Booted Out For Terrifying Reason Nearly 40,000 Pakastani workers were deported from Saudi Arabia since October 2016. The reasons? Visa violations and terror concerns. I’m sure that nobody will have a problem calling the Saudi Arabian government “Islamophobic” for this, right? Right? From Independent.co.uk: The Kingdom of Saudi Arabia has expelled almost 40,000 Pakistani migrant workers in the last four months, local media has reported. Over 39,000 people have been deported since October 2016 over visa violations and security concerns, the Saudi Gazette reported, citing unnamed interior ministry officials. As well as crimes including drug trafficking, forgery and theft, an unknown number of those removed from the country were suspected to have links to Isis and other extremist groups, the paper said. The alleged mass deportations come after a year of strikes and other unrest in the kingdom due to unpaid wages following the oil market’s decline and subsequent blow to the Saudi economy. Official Saudi statistics say that 243,000 Pakistanis were deported between 2012 – 2015. Mass deportations of migrant workers – which Human Rights Watch and other rights organisations say often involve illegal beatings and detainment in poor conditions – are fairly common. 2010 census figures show that 8.5 million of Saudi Arabia’s 27 million strong population, or around 30 per cent, are foreign nationals. According to a 2014 European University Institute report, there are approximately 900,000 people of Pakistani nationality currently employed in Saudi Arabia’s vast construction industry and other low-paid service jobs. I’m looking forward to hearing American liberals preach to Saudi Arabia about the need for “tolerance,” Maybe.


-time employees of the Federal Government created under such program. (2) Appropriate congressional committees defined.--In this subsection, the term ``appropriate congressional committees'' means the following: (A) In the House of Representatives: (i) The Committee on Foreign Affairs. (ii) The Committee on Homeland Security. (iii) The Committee on the Judiciary. (iv) The Committee on Appropriations. (B) In the Senate: (i) The Committee on Foreign Relations. (ii) The Committee on Homeland Security and Governmental Affairs. (iii) The Committee on the Judiciary. (iv) The Committee on Appropriations. SEC. 6. SERVICES UPON ARRIVAL. (a) In General.--Aliens provided special immigrant status and visas pursuant to section 4 shall be eligible for the same resettlement assistance, programs, and benefits as refugees admitted under section 207 of the Immigration and Naturalization Act (8 U.S.C. 1157). The Secretary of of Health and Human Services, in cooperation with the Secretary of State, shall work with nongovernmental organizations to provide such assistance, programs, and benefits and ensure that such aliens are referred to refugee resettlement agencies. (b) Computer Literacy and Vocational Training.--The Secretary of State shall utilize existing programs of the Department of State and contracts between the Department and nongovernmental organizations to make available computer literacy programs and vocational training programs to aliens provided special immigrant status pursuant to section 4. (c) Rule of Construction.--Nothing in this section shall be construed as requiring the cooperation of nongovernmental organizations. SEC. 7. TRAINING AT THE DEPARTMENT OF STATE. Not later than 180 days after the date of the enactment of this Act, the Secretary of State shall establish a program in the Department of State to provide instruction in English as a second language, vocational training, computer training, employment services, and certain counseling services for Iraqis admitted to the United States as special immigrants. SEC. 8. SENSE OF CONGRESS. It is the sense of Congress that the United States should provide an orientation into life in the United States for Iraqi special immigrants under this Act who are newly admitted to the United States and should make all reasonable efforts to provide temporary safe haven for aliens described in section 4 who are applying for special immigrant status and visas.


We have seen that if \phi: M_n(\C) \rightarrow M_n(\C) is a unital q-positive map and \nu is a type II Powers weight, then the boundary weight double (\phi, \nu) induces a unique (up to conjugacy) type II_0 E_0-semigroup. Let \phi: M_n(\C) \rightarrow M_n(\C) and \psi: M_{n'}(\C) \rightarrow M_{n'}(\C) be unital rank one q-positive maps, so for some states \rho \in M_n(\C)^* and \rho' \in M_{n'}(\C)^*, we have \phi(A)=\rho(A)I_n and \psi(D) = \rho'(D)I_{n'} for all A \in M_n(\C) and D \in M_{n'}(\C). We find that if \nu and \eta are arbitrary type II Powers weights, then (\phi, \nu) and (\psi, \eta) induce non-cocycle conjugate E_0-semigroups if \rho and \rho' have different eigenvalue lists. We then completely classify the q-corners and hyper maximal q-corners from \phi to \psi, obtaining the following result: If \nu is a type II Powers weight of the form \nu(\sqrt{I - \Lambda(1)} B \sqrt{I - \Lambda(1)})=(f,Bf), then the E_0-semigroups induced by (\phi,\nu) and (\psi, \nu) are cocycle conjugate.


Now’s your chance. There are about 200 stone houses for sale in an Italian village for just $1.50. Ollolai, located on the island of Sardinia, is partaking in a project called “Case a 1 euro,” which is aimed at preserving the history and charm of Italian villages at risk of depopulation. “My crusade is to rescue our unique traditions from falling into oblivion,” Efisio Arbau, the mayor of Ollolai, told CNN. “Pride in our past is our strength. We’ve always been tough people and won’t allow our town to die.” Though the deal is enticing — Sardinia has nearly 2,000 kilometres of coastline and picturesque beaches — it comes with conditions. The homes are in need of major renovation. Anyone that purchases a house in Ollolai will need to refurbish it within three years, and according to CNN, renovations are likely to cost around $25,000. In the past 50 years, the town’s population has shrunk from 2,250 to 1,300 people. The Municipality of Ollolai hopes that these sales will help draw in new homeowners and preserve the village’s history. “The internet has lit up from joyous dreamers who want to pack it in and live the la dolce vita,” Canadian Jennifer Avventura wrote on her blog, My Sardinian Life. But as dreamy as it sounds to move there, the realities of living on an Italian island shouldn’t be overlooked. “You will need to have a basic understanding of the Italian language to get by with day-to-day activities,” she wrote. “Remember – you’re re-building a home and will need to contact builders, plumbers, electricians, the local town hall, possibly a lawyer, a notary to notarize the billions of documents that will need to be signed, stamped and stamped again. Can you do this in Italian?” Arbau said in a statement that the town has received more requests than they have homes, and due to the overwhelming number of applications, the deadline for applications was moved up to Feb. 7 at 2 p.m. “If you can get over those small hurdles and prepare yourself for a beautiful, simple life, deep within the folds of Sardinia’s glorious mountains – then do


), the person engaged in, or seeking to engage in, an activity described in such subsection shall-- ``(1) inform the individual of all the purposes for which the number will be utilized and the persons to whom the number will be known; and ``(2) obtain affirmatively expressed consent in writing. ``(d) Exceptions.--Nothing in this section shall be construed to prohibit any use of social security account numbers permitted or required under section 205(c)(2) of this Act, section 7(a)(2) of the Privacy Act of 1974 (5 U.S.C. 552a note; 88 Stat. 1909), or section 6109(d) of the Internal Revenue Code of 1986. ``(e) Civil Action in United States District Court; Damages; Attorneys Fees and Costs; Nonexclusive Nature of Remedy.-- ``(1) In general.--Any individual aggrieved by any act of any person in violation of this section may bring a civil action in a United States district court to recover-- ``(A) such preliminary and equitable relief as the court determines to be appropriate; and ``(B) the greater of-- ``(i) actual damages; and ``(ii) liquidated damages of $25,000 or, in the case of a violation that was willful and resulted in profit or monetary gain, $50,000. ``(2) Attorney's fees and costs.--In the case of a civil action brought under paragraph (1) in which the aggrieved individual has substantially prevailed, the court may assess against the respondent a reasonable attorney's fee and other litigation costs and expenses (including expert fees) reasonably incurred. ``(3) Statute of limitations.--No action may be commenced under this subsection more than 3 years after the date on which the violation was or should reasonably have been discovered by the aggrieved individual. ``(4) Nonexclusive remedy.--The remedy provided under this subsection shall be in addition to any other lawful remedy available to the individual. ``(f) Civil Money Penalties.-- ``(1) In general.--Any person who the Commissioner of Social Security determines has violated this section shall be subject, in addition to any other penalties that may be prescribed by law, to-- ``(A) a civil money penalty of not more than $25,000 for each such violation, and ``(B) a civil money penalty of not more than $500,000.


Share This Video Facebook Twitter EMAIL Every day it gets harder and harder to tell if Kanye West has gone off the deep end, if he’s 100 percent sincere, or if he’s just elaborately trolling us all for attention with a ridiculous spate of GOOD Music albums supposedly on the way, but one thing is for sure: His weirdness is consistently and bizarrely captivating, entertaining, and surprising — you never know what he’ll do next. I love the way Candace Owens thinks — KANYE WEST (@kanyewest) April 21, 2018 Case in point, his latest stunt involved an unexpected response to Hot 97’s Ebro Darden after the gruff radio personality lambasted West yesterday during his show. After West tweeted in support of conservative commentator Candace Owens, Ebro and his cohosts delivered a rollicking , 16-minute explainer for his seemingly Trump-supporting tweets and why they hurt, confused, or angered many of Kanye’s longtime fans and supporters. While they weren’t exactly kind to Kanye, they weren’t totally disrespectful either, surmising that ultimately, Kanye likes Trump because Trump was nice to him at a low point in his life. Yes Kanye just called the show while we were in the middle of a break and just kept repeating "I love you" to Ebro…eventually he said lets meet in person off air and then talk on the air — RosenbergTelevision (@Rosenbergradio) April 24, 2018 Today, though, Kanye called into Hot 97 to speak his piece, except what actually happened is he simply kept repeating “I love you” in response to Ebro’s questions, to the confusion of the hosts. He seemed to be in good spirits, but refused to talk about the music or his tweets, offering to speak with Ebro in person before giving a radio interview. If it’s a troll, it’s one of the most masterful mind games anyone’s ever played with the rambunctious Ebro In The Morning crew, and if it was just “New” Kanye’s pacifistic way of blowing off steam, it certainly seems more productive than his old approach to radio host provocation. In either case, Kanye’s certainly built even more anticipation for his new music —.


Netflix Even if you’re still in the middle of Lost in Space from Netflix’s April additions, the month of May is nearly upon us and the streaming giant already has a whole of new shows and films in store for its subscribers. From the fourth season of the hugely popular Unbreakable Kimmy Schmidt to a seemingly endless array of new comedy specials from Tig Notaro, John Mulaney, and more, the sheer amount of new content Netflix is putting out next month is insurmountable. Then again, to make room for it all the streamer will have to sacrifice a few expired licenses, like the Martin Scorsese classic Goodfellas. ARRIVING The fourth season of Unbreakable Kimmy Schmidt (5/30) Share This Video Facebook Twitter EMAIL We haven’t heard much from Kimmy Schmidt (Ellie Kemper) since season three dropped in May of last year. That’s all about to change at the end of May, when the popular comedy series will return to Netflix for its fourth season. Slated for a split debut on Wednesday, May 30th, the first half of season four (six episodes) will be available to watch in full. As for the second half of the new season, they will be available to watch sometime “later in 2018.” No particular reason was given by Netflix back in February, though it probably has something to do with show creator Tina Fey’s busy schedule. DEPARTING Goodfellas says goodbye (5/1) Martin Scorsese’s 1990 film Goodfellas is an all-time cinematic classic, Tommy DeVito’s (Joe Pesci) crazed outbursts notwithstanding. The film was adapted from Nicholas Pileggi’s 1986 book Wiseguy, which chronicled the rise and fall of Henry Hill (Ray Liotta), a mobster who became an informant for the FBI. Anyone with a love of Scorsese films, Robert De Niro being Robert De Niro, or crime movies will love Goodfellas. Hence why.


Then M-theory on AdS_4 x Y^7 possesses "topological" U(1)^{b_2} gauge symmetry. The corresponding Abelian gauge fields come from three-form fluctuations with one index in AdS_4 and the other two in Y^7. We find black membrane solutions carrying one of these U(1) charges. In the zero temperature limit, our solutions interpolate between AdS_4 x Y^7 in the UV and AdS_2 x R^2 x squashed Y^7 in the IR. In fact, the AdS_2 x R^2 x squashed Y^7 background is by itself a solution of the supergravity equations of motion. These solutions do not appear to preserve any supersymmetry. We search for their possible instabilities and do not find any. We also discuss the meaning of our charged membrane backgrounds in a dual quiver Chern-Simons gauge theory with a global U(1) charge density. Finally, we present a simple analytic solution which has the same IR but different UV behavior. We reduce this solution to type IIA string theory, and perform T-duality to type IIB. The type IIB metric turns out to be a product of the squashed Y^7 and the extremal BTZ black hole. We discuss an interpretation of this type IIB background in terms of the (1+1)-dimensional CFT on D3-branes partially wrapped over the squashed Y^7.


The extreme UV emitted by a very hot source ionizes low pressure molecular hydrogen making a transparent bubble of H II (Protons and electrons). For an increase of radius, intensity of extreme UV and temperature decrease, so that the plasma contains more and more atoms. A spherical shell, mainly of neutral atoms (H I) appears. If this shell is optically thick at Lyman frequencies of H I, it is superradiant and a competition of modes selects modes tangent to a sphere for which many atoms are excited. Thus, a shell of plasma emits, into a given direction, tangential rays showing a ring in which selected modes are brighter. While at Lyman frequencies, absorption of rays emitted by the source excites the atoms able to amplify the superradiance, a more powerful amplification of superradiance results from an induced scattering of the radial beams, which extends to feet of lines and progressively to the whole spectrum. Thermodynamics says that the brightness of radial and tangential beams tends to be equal; if the solid angle of observation is much larger for the ring than for the source, almost the whole light emitted by the source is transferred to the rings, and the source becomes invisible. Paradoxically, a glow due to incoherent scattering and impurities around the source remains visible. As the scattering decreases with the decrease of the radial intensity, the brightness of the ring decreases with radius. These characteristics are found in supernova remnant 1987A.


BARNEGAT – If you see or smell smoke in Barnegat on Wednesday, it is most likely a prescribed burn performed by the New Jersey Forest Fire Service. Prescribed burns are intentional fires set to clear out easily flammable brush before a wildfire does it. The area around Cloverdale Farms, by Cloverdale Road, will be the focus of the burn. It should take place between 8 a.m. and 8 p.m. The New Jersey State Forest Fire Service conducts burns throughout the state at the end of winter every year. The burns destroy fallen trees, branches, leaves, pine needles and other debris on the forest floor. “By burning them away now, we can reduce the risk of these materials serving as tinder for wildfires later in the year,” said Bill Edwards, chief of the state fire service. “This practice also improves the overall ecological health of our forests and grasslands.” The fire service expects to burn between 10,000 and 20,000 acres of forests and grasslands this season, they said. Most burns are on state-owned property. Because of the make-up of vegetation, the Pinelands region is the focus of much of the prescribed burning activity. During burns, personnel use hand-held torches to burn away debris on the forest floor, taking into account wind, moisture and other conditions. Last year, the Forest Fire Service responded to 1,065 wildfires, but 75 percent of them were a quarter acre or smaller. The largest was a 464-acre fire in Bass River State Forest in Burlington County. Residents are advised that they might see large plumes of smoke and might smell smoke for miles around. The burns will continue through the end of March, depending on weather. For more information, go to facebook.com/newjerseyforests or call 609-292-2977. If you are unsure.


We investigate the effect of monopolar charge disorder on the classical fluctuation-induced interactions between randomly charged net-neutral dielectric slabs and discuss various generalizations of recent results (A. Naji et al., Phys. Rev. Lett. 104, 060601 (2010)) to highly inhomogeneous dielectric systems with and without statistical disorder correlations. We shall focus on the specific case of two generally dissimilar plane-parallel slabs, which interact across vacuum or an arbitrary intervening dielectric medium. Monopolar charge disorder is considered to be present on the bounding surfaces and/or in the bulk of the slabs, may be in general quenched or annealed and may possess a finite lateral correlation length reflecting possible `patchiness' of the random charge distribution. In the case of quenched disorder, the bulk disorder is shown to give rise to an additive long-range contribution to the total force, which decays as the inverse distance between the slabs and may be attractive or repulsive depending on the dielectric constants of the slabs. We show that in the case of two dissimilar slabs the net effect due to the interplay between the disorder-induced and the pure van der Waals interactions can lead to a variety of unusual non-monotonic interaction profiles between the dielectric slabs. In particular, when the intervening medium has a larger dielectric constant than the two slabs, we find that the net interaction can become repulsive and exhibit a potential barrier, while the underlying van der Waals force is attractive. On the contrary, when the intervening medium has a dielectric constant in between that of the two slabs, the net interaction can become attractive and exhibit a free energy minimum, while the pure van der Waals force is repulsive. Therefore, the charge disorder.


We present a test of different error estimators for 2-point clustering statistics, appropriate for present and future large galaxy redshift surveys. Using an ensemble of very large dark matter LambdaCDM N-body simulations, we compare internal error estimators (jackknife and bootstrap) to external ones (Monte-Carlo realizations). For 3-dimensional clustering statistics, we find that none of the internal error methods investigated are able to reproduce neither accurately nor robustly the errors of external estimators on 1 to 25 Mpc/h scales. The standard bootstrap overestimates the variance of xi(s) by ~40% on all scales probed, but recovers, in a robust fashion, the principal eigenvectors of the underlying covariance matrix. The jackknife returns the correct variance on large scales, but significantly overestimates it on smaller scales. This scale dependence in the jackknife affects the recovered eigenvectors, which tend to disagree on small scales with the external estimates. Our results have important implications for the use of galaxy clustering in placing constraints on cosmological parameters. For example, in a 2-parameter fit to the projected correlation function, we find that the standard bootstrap systematically overestimates the 95% confidence interval, while the jackknife method remains biased, but to a lesser extent. The scatter we find between realizations, for Gaussian statistics, implies that a 2-sigma confidence interval, as inferred from an internal estimator, could correspond in practice to anything from 1-sigma to 3-sigma. Finally, by an oversampling of sub-volumes, it is possible to obtain bootstrap variances and confidence intervals that agree with external error estimates, but it is not clear.


(1) or (2)'' in paragraph (1)(C) (as so redesignated) and inserting ``subparagraph (A) or (B)''; and (4) by adding at the end the following new paragraph: ``(2) Additional requirements with respect to grantor retained annuities.--For purposes of subsection (a), in the case of an interest described in paragraph (1)(A) (determined without regard to this paragraph) which is retained by the transferor, such interest shall be treated as described in such paragraph only if-- ``(A) the right to receive the fixed amounts referred to in such paragraph is for a term of not less than 10 years, ``(B) such fixed amounts, when determined on an annual basis, do not decrease relative to any prior year during the first 10 years of the term referred to in subparagraph (A), and ``(C) the remainder interest has a value greater than zero determined as of the time of the transfer.''. (b) Effective Date.--The amendments made by this section shall apply to transfers made after December 31, 2010. TITLE IV--BUDGETARY EFFECTS SEC. 401. COMPLIANCE WITH PAYGO. The budgetary effects of this Act, for the purpose of complying with the Statutory Pay-As-You-Go Act of 2010, shall be determined by reference to the latest statement titled ``Budgetary Effects of PAYGO Legislation'' for this Act, submitted for printing in the Congressional Record by the Chairman of the Senate Budget Committee.


The peculiar motion of the Earth causes a dipole anisotropy modulation in the distant galaxy distribution due to the aberration effect. However, the amplitude and angular direction of the effect is not necessarily the same as those of the cosmic microwave background (CMB) dipole anisotropy due to the growth of cosmic structures. In other words exploring the aberration effect may give us a clue to the horizon-scale physics perhaps related to the cosmic acceleration. In this paper we develop a method to explore the dipole angular modulation from the pixelized galaxy data on the sky properly taking into account the covariances due to the shot noise and the intrinsic galaxy clustering contamination as well as the partial sky coverage. We applied the method to the galaxy catalogs constructed from the Sloan Digital Sky Survey (SDSS) Data Release 6 data. After constructing the four galaxy catalogs that are different in the ranges of magnitudes and photometric redshifts to study possible systematics, we found that the most robust sample against systematics indicates no dipole anisotropy in the galaxy distribution. This finding is consistent with the expectation from the concordance Lambda-dominated cold dark matter model. Finally we argue that an almost full-sky galaxy survey such as LSST may allow for a significant detection of the aberration effect of the CMB dipole having the precision of constraining the angular direction to ~ 20 degrees in radius. Assuming a hypothetical LSST galaxy survey, we find that this method can confirm or reject the result implied from a stacked analysis of the kinetic Sunyaev-Zel'dovich effect of X-ray luminous clusters in Kashlinsky et al. (2008,2009).


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


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


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


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


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


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


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


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


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


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