It should also affect the orbital motions of the solar system's bodies moving in the space regions in which the PA manifested itself in its presently known form, i.e. as a constant and uniform acceleration approximately directed towards the Sun with a non-zero magnitude APio = (8.74 +/- 1.33) x 10^-10 m s^-2 after 20 au from the Sun. In this paper we preliminarily investigate its effects on the orbital motions of the Neptunian satellites Triton, Nereid and Proteus, located at about 30 au from the Sun, both analytically and numerically. Extensive observational records covering sev- eral orbital revolutions have recently been analyzed for them, notably improving the knowledge of their orbits. Both analytical and numerical calculations, limited to the direct, Neptune-satellite interaction, show that the peak-to-peak amplitudes of the PA-induced radial, transverse and out-of-plane perturbations over one century are up to 300 km, 600 km, 8 m for Triton, 17,500 km, 35,000 km, 800 km for Nereid, and 60 km, 120 km, 30 m for Proteus. The corresponding orbital uncertainties ob- tained from a recent analysis of all the data available for the satellites considered are, in general, smaller by one-two orders of magnitude, although obtained without modeling a Pioneer-like extra-force. Further investigations based on a re-processing of the satellites' real or simulated data with modified equations of motions including an additional Pioneer-type force as well are worth being implemented and may shed further light on this important issue.


Receive from the Secretary a grant for each fiscal year in an amount equal to the total amount expended by the State during the immediately preceding fiscal year under the State program funded under this part for assistance to any exempt family or exempt adult for any month for which the family or the adult, in the absence of section 408(a)(7)(E), would not be eligible for such assistance. ``(B) Appropriation.--Out of any money in the Treasury of the United States not otherwise appropriated, there are appropriated for grants under this paragraph such sums as may be necessary for each fiscal year.''. SEC. 5. DEFINITIONS. Section 419 of the Social Security Act (42 U.S.C. 607(b)), as added by section 103(a) of the Personal Responsibility and Work Opportunity Reconciliation Act of 1996, is amended by redesignating paragraphs (2) through (5) as paragraphs (4) through (7), respectively, and by inserting after paragraph (1) the following: ``(2) Exempt adult.--The term `exempt adult' means an adult who is-- ``(A) living with and caring for a minor child who is related to (but not a biological child of) the adult; and ``(B) the head of a family that-- ``(i) does not include a parent of any such minor child; and ``(ii) does not include a biological child of the adult. ``(3) Exempt family.--The term `exempt family' means a family which-- ``(A) is headed by an adult who is living with and caring for a minor child who is related to (but not a biological child of) the adult; ``(B) does not include a parent of any such minor child; and ``(C) does not include a biological child of the adult.''. SEC. 6. EFFECTIVE DATE. The amendments made by this Act shall take effect as.


The beginning of questions all Manitoba employers will face. Overt smoking of cannabis at the workplace can be neatly banned under the tobacco-smoking restrictions that already exist. But what about cannabis edibles? While it will be illegal for cannabis stores to sell edibles in Manitoba, cannabis cookies are easily made by anyone with access to an oven: can employees bring cannabis cookies to work or to “pot luck” workplace functions? What about executives who have expense accounts on which they “wine and dine” important clients? If the client prefers weed to wine, can the company representative vape with the VIP and write off the reefer? If the Manitoba government finds itself confounded by workplace policies around cannabis, it’s not alone. The Canadian Human Resources Professionals Association surveyed more than 700 of its members in January and found a full 71 per cent of employers were not prepared for the legalization of cannabis. A report titled Clearing the Haze: The Impacts of Marijuana in the Workplace recommends government sets a clear legal definition of “impairment” and the grounds under which an employee can be drug-tested. This remains a serious debate for employers, as cannabis chemicals remain in the bloodstream and employees who use the drug only after clocking out could fail a drug test even if they’re not under the influence at work. The report also says provincial governments should co-ordinate recreational marijuana regulations as much as possible, so employers with a national workforce can easily adhere to the policies. It’s incumbent on both employees and employers to be responsible about cannabis. For employers, this includes giving workers a clear cannabis-use policy before the drug becomes legal. Workers have a right to know specifically what is, and isn’t, allowed at their office, plant and job site. If workplaces don’t yet have clear policies, the employers should get to work, and put in the overtime.


High-resolution submm imaging of the HzRG, 4C60.07, at z=3.8, has revealed two dusty components. Spitzer imaging shows that one of these components (B) is coincident with an extremely red AGN, offset by ~4" (~30 kpc) from the HzRG core. The other submm component (A) - resolved by our beam and devoid of emission at 3.6-8.0um - lies between B and the HzRG core. Since the HzRG was discovered via its young, steep-spectrum lobes and their creation was likely triggered by the interaction, we argue that we are witnessing an early-stage merger, prior to its eventual equilibrium state. The interaction is between the host galaxy of an actively-fueled BH, and a gas-rich starburst/AGN (B) marked by the compact submm component and coincident with broad CO emission. `A' is a plume of cold, dusty gas, associated with a narrow (~150 km/s) CO feature, and may represent a short-lived tidal structure. It has been claimed that HzRGs and SMGs differ only in the activity of their AGNs, but such complex submm morphologies are seen only rarely amongst SMGs. Our study has important implications: where a galaxy's gas is not aligned with its central BH, CO may be an unreliable probe of dynamical mass, affecting work on the co-assembly of BHs and spheroids. Our data support the picture wherein close binary AGN are induced by mergers. They also raise the possibility that some supposedly jet-induced starbursts may have formed co-evally with (yet independently of) the radio jets, both triggered by the same interaction. We note that the HzRG host would have gone unnoticed without its jets/companion, so there may be many other unseen BHs at high redshift, lost in the sea of ~5 x 10^8 similarly bright IRAC sources - sufficiently massive to drive a >10^27-W radio source, yet practically invisible.


Why it matters to you If you're sitting on a trove of Bitcoin now might be a good time to sell. Or it might not be. It's very hard to predict what Bitcoin will do. Bitcoin has once again beaten all of its own records for the value of a single unit of cryptocurrency by breaching the $4,000 mark. This latest surge follows a month-long climb back to new heights after it dropped to a quarterly low of around $1,900 as a new-generation of graphics card miners began dumping their newly acquired number-crunching hardware. The price of Bitcoin has a history of rising to new highs, crashing in the aftermath of reduced confidence, and then slowly building up to even greater highs. That pattern is evident if you look at multiple year graphs of the cryptocurrency’s value, and was highlighted in our recent chat with a few experts about Bitcoin’s past and future. This latest peak is astronomically high, though. It’s more than twice the value the currency held in mid-May and at the time of writing sits at $4,308. It’s rising so quickly in fact, that we’ve updated that total twice just while writing this story. That rise has pushed Bitcoin’s market cap to $70.6 billion, which is tens of billions more than it was a mere few months ago. This is perhaps more impressive since there was some consideration earlier this month that Bitcoin could become the lesser of two currencies, after a “hard fork,” saw the creation of “Bitcoin Cash.” Although essentially merely an alternative, or “altcoin” much like many other cryptocurrencies, Bitcoin Cash was the first to attempt to use the recognizable name of Bitcoin for its nomenclature. Despite its promises to deliver a more consumer friendly experience than its parent though, Bitcoin Cash has fallen from its $640 peak to $300 per unit at the time of writing. Although it’s possible that Bitcoin Cash will gather more steam in the future, for now it’s Bitcoin, not its young upstart, that is seeing monumental growth, more than eight years on from its debut. One other cryptocurrency that is in vogue, Ether, has also recovered from its valuation tumble in late July. It’s now reached close to $300 again itself, following a similar trend to Bitcoin in rises and falls that gradually trend upward. The trend could end up skyrocketing once again.


We are all ready to take the plunge into fall food trends. Luckily a lot of them are a whole lot healthier than the sugar-loaded calorie bomb that has a special place in every sweater-lovers’ heart. To the contrary, fall produce is chock full of healthy nutrients. We all know that in-season foods tend to be a little easier on your wallet, plus they introduce a whole new array of ingredients to get creative with in the kitchen. (Admit it, you're a little tired of the chopped salads.) What's on the menu? Root vegetables like turnips and sweet potatoes, winter squash and a new lineup of fruit to fill the bowl on your kitchen counter. Whether you’re cooking up a weeknight dinner for one, meal prepping lunch or serving a hungry crowd of football fans, use the super foods of the season as inspiration to infuse autumn flavor and nutrients into your meals. Brussels Sprouts “Brussels sprouts are cruciferous vegetables, which means they're loaded with cancer-fighting compounds,” says Lainey Younkin, MS, RD, LDN, founder of Lainey Younkin Nutrition in Boston, MA. “They are also high in vitamin K, which helps your blood clot. Shred them in a food processor and use as a base for your next salad or simply roast them on a baking sheet in the oven — add a little maple syrup for a sweet-savory punch.” Recipe box: Serve Maple-Balsamic Roasted Brussels Sprouts as a side dish, or toss with onions, cranberries and toasted pecans and serve over farro for a heartier main course. (We are starring this one for the Thanksgiving spread!) Whole Wheat Pumpkin Pancakes Pinch of Yum Pumpkin Canned pumpkin may just be the best kept secret on the grocery store shelves. While it’s available all year long, we feel a re-invigorated love for the ingredient when fall rolls around. “A cup of sliced pumpkin has almost 200 percent of your daily value of vitamin A and is shock-full of vitamin C and potassium,” says Younkin. “As long as you aren't drinking it in syrup form in your latte, pumpkin is a healthy addition to any fall meal. A 1/2 cup of canned pumpkin delivers 3 grams of fiber and has just 5 grams of sugar and 50 calories. There isn't much


42 U.S.C. 300gg-13(a)(4)) is amended by inserting ``(including oral contraceptives for routine, daily use approved by the Food and Drug Administration for use without a prescription, even if the individual does not have a prescription for such contraceptive)'' after ``additional preventive care''. SEC. 6. RULES OF CONSTRUCTION. (a) Non-Interference With FDA Regulation.--Nothing in this Act (or the amendment made by this Act) shall be construed to modify or interfere with Food and Drug Administration processes to review or approve, or otherwise determine the safety and efficacy of, and make available, non-prescription drugs or devices, modify or interfere with the scientific and medical considerations of the Food and Drug Administration, or alter any other authority of the Food and Drug Administration. (b) Non-Preemption.--Nothing in this Act (or the amendment made by this Act) preempts any provision of Federal or State law to the extent that such Federal or State law provides protections for consumers that are greater than the protections provided for in this Act. SEC. 7. DUTIES OF RETAILERS TO ENSURE ACCESS TO ORAL BIRTH CONTROL FOR USE WITHOUT A PRESCRIPTION. (a) In General.--Any retailer that stocks oral birth control for routine, daily use that is approved by, or otherwise legally marketed under regulation by, the Food and Drug Administration for use without a prescription may not interfere with an individual's access to or purchase of such birth control or access to medically accurate, comprehensive information about such birth control. (b) Limitation.--Nothing in this section shall prohibit a retailer that stocks oral birth control for routine, daily use from refusing to provide an individual with such oral birth control that is approved by, or otherwise legally marketed under regulation by, the Food and Drug Administration.


We present a model-independent investigation of the WMAP data with respect to scale- dependent non-Gaussianities (NGs) by employing the method of constrained randomization. For generating so-called surrogate maps a shuffling scheme is applied to the Fourier phases of the original data, which allows to test for the presence of higher order correlations (HOCs) on well-defined scales. Using scaling indices as test statistics we find highly significant signatures for non-Gaussianities when considering all scales. We test for NGs in the bands l = [2,20], l = [20,60], l = [60,120] and l = [120,300]. We find highly significant signatures for non-Gaussianities and ecliptic hemispherical asymmetries for l = [2, 20]. We also obtain highly significant deviations from Gaussianity for the band l = [120,300]. The result for the full l-range can be interpreted as a superposition of the signatures found in the bands l = [2, 20] and l = [120, 300]. We find remarkably similar results when analyzing different ILC-like maps. We perform a set of tests to investigate if the detected anomalies can be explained by systematics. While no test can convincingly rule out the intrinsic nature of the anomalies for the low l case, the ILC map making procedure and/or residual noise in the maps can also lead to NGs at small scales. Our investigations prove that there are phase correlations in the WMAP data of the CMB. In the absence of an explanation in terms of Galactic foregrounds or known systematic artefacts, the signatures at low l must so far be taken to be cosmological at high significance. These findings strongly disagree with predictions of isotropic cosmologies with single field slow roll inflation. The task is now to elucidate the origin of the phase correlations and to understand the physical processes leading to these scale-dependent non-Gaussianities -.


Chances are you’re going to enroll in Medicare. While it’s common knowledge that Medicare is the United States’ health insurance program for retirees, many people don’t fully understand certain things about Medicare, such as when to enroll, how much it costs, what all the “parts” of Medicare are, and more. Continue Reading Below Image source: Getty Images. With that in mind, here’s a quick guide that could answer some of your Medicare questions before you have them. Is Medicare enrollment automatic? For many people, Medicare enrollment happens automatically. Specifically, if any of these three criteria apply to you, there’s nothing you need to do — you’ll be automatically enrolled in Medicare Parts A and B (more on the “parts” in the next section). In these cases, expect to receive your Medicare card in the mail about three months before you’ll be eligible for benefits. You already get Social Security benefits or retirement benefits from the Railroad Retirement Board (RRB). In this case, you’ll automatically get Medicare Parts A and B on the first day of the month you’ll turn 65. You’ve gotten SS or RRB disability benefits for 24 months. You have ALS (Lou Gehrig’s disease). In this case, you’ll get Parts A and B the month your disability benefits begin. Continue Reading Below ADVERTISEMENT If none of these applies to you, you’ll need to sign up for Medicare. For those who are eligible based on age, the initial seven-month enrollment period begins three months before the month in which you’ll turn 65 and includes the three months after your birth month. You don’t have to sign up during the initial enrollment period, but not doing so can result in permanently higher premiums when you do. The Medicare general enrollment period runs from Jan.1 through March 31 each year. The easiest way to sign up for Medicare is online at the Social Security Administration’s website. Doing so takes about 10 minutes, and there are no forms to sign and no additional documentation requirements. If you already have Part A and just need to sign up for Part B, there is a separate application for this purpose. Of course, you can always choose to apply in person at a Social Security office, or over the phone, but these options can be much more time-consuming. What are the “parts” of Medicare? You may have heard about the “parts” of Medicare — for example, maybe you heard someone refer


I hesitated for a long time before giving shape to these notes, originally intended for preliminary reading by the attendees to the Summer School "New paths towards quantum gravity" (Holbaek Bay, Denmark, May 2008). At the end, I decide against just selling my mathematical wares, and for a survey, necessarily very selective, but taking a global phenomenological approach to its subject matter. After all, non-commutative geometry does not purport yet to solve the riddle of quantum gravity; it is more of an insurance policy against the probable failure of the other approaches. The plan is as follows: the introduction invites students to the fruitful doubts and conundrums besetting the application of even classical gravity. Next, the first experiments detecting quantum gravitational states inoculate us a healthy dose of skepticism on some of the current ideologies. In Section 3 we look at the action for general relativity as a consequence of gauge theory for quantum tensor fields. Section 4 briefly deals with the unimodular variants. Section 5 arrives at non-commutative geometry. I am convinced that, if this is to play a role in quantum gravity, commutative and non-commutative manifolds must be treated on the same footing; which justifies the place granted to the reconstruction theorem. Together with Section 3, this part constitutes the main body of the notes. Only very summarily at the end of this section we point to some approaches to gravity within the non-commutative realm. The last section delivers a last dose of skepticism. My efforts will have been rewarded.


We report recent studies on structure functions of the nucleon and nuclei. First, clustering effects are investigated in the structure function F_2 of Be-9 for explaining an unusual nuclear correction found in a JLab experiment. We propose that high densities created by formation of clustering structure like 2*alpha+neutron in Be-9 is the origin of the unexpected JLab result by using the antisymmetrized molecular dynamics (AMD). There is an approved proposal at JLab to investigate the structure functions of light nuclei including the cluster structure, so that much details will become clear in a few years. Second, tensor-polarized quark and antiquark distributions are obtained by analyzing HERMES measurements on the structure function b_1 for the deuteron. The result suggests a finite tensor polarization for antiquark distributions, which is an interesting topic for further theoretical and experimental investigations. An experimental proposal exists at JLab for measuring b_1 of the deuteron as a new tensor-structure study in 2010's. Furthermore, the antiquark tensor polarization could be measured by polarized deuteron Drell-Yan processes at hadron facilities such as J-PARC and GSI-FAIR. Third, the recent CDF dijet anomaly is investigated within the standard model by considering possible modifications of the strange-quark distribution. We find that the shape of a dijet-mass spectrum changes depending on the strange-quark distribution. It indicates that the CDF excess could be partially explained as a PDF effect, particularly by the strangeness in the nucleon, within the standard model.


A seemingly contrived hierarchy in the squark mass spectrum appears to be required. We show that composite supersymmetric theories at the bottom of the conformal window can automatically yield the spectrum that is suggested by experimental data and naturalness. With a non-tuned choice of parameters, the only superpartners below one TeV will be the partners of the Higgs, the electroweak gauge bosons, the left-handed top and bottom, and the right-handed top, which are precisely the particles needed to make weak scale supersymmetry breaking natural. In the model considered here, these correspond to composite (or partially composite) degrees of freedom via Seiberg duality, while the other MSSM fields, with their heavier superpartners, are elementary. The key observation is that at or near the edge of the conformal window, soft supersymmetry breaking scalar and gaugino masses are transmitted only to fundamental particles at leading order. With the potential that arises from the duality, a Higgs with a 125 GeV mass, with nearly SM production rates, is naturally accommodated without tuning. The lightest ordinary superpartner is either the lightest stop or the lightest neutralino. If it is the stop, it is natural for it to be almost degenerate with the top, in which case it decays to top by emitting a very soft gravitino, making it quite difficult to find this mode at the LHC and more challenging to find SUSY in general, yielding a simple realization of the stealth supersymmetry idea. We analyze four benchmark spectra in detail.


We analyze the behavior of an itinerant Fermi system near a charge nematic(n=2) Pomeranchuk instability in terms of the Landau Fermi liquid (FL) theory. The main object of our study is the fully renormalized vertex function $\Gamma\Omega$, related to the Landau interaction function. We derive $\Gamma^\Omega$ for a model case of the long-range interaction in the nematic channel. Already within the Random Phase Approximation (RPA), the vertex is singular near the instability. The full vertex, obtained by resumming the ladder series composed of the RPA vertices, differs from the RPA result by a multiplicative renormalization factor $Z_\Gamma$, related to the single-particle residue $Z$ and effective mass renormalization $m^*/m$. We employ the Pitaevski-Landau identities, which express the derivatives of the self-energy in terms of $\Gamma^\Omega$, to obtain and solve a set of coupled non-linear equations for $Z_\Gamma$, $Z$, and $m^*/m$. We show that near the transition the system enters a critical FL regime, where $Z_\Gamma \sim Z \propto (1 + g_{c,2})^{1/2}$ and $m^*/m \approx 1/Z$, where $g_{c,2}$ is the $n=2$ charge Landau component which approaches -1 at the instability. We construct the Landau function of the critical FL and show that all but $g_{c,2}$ Landau components diverge at the critical point. We also show that in the critical regime the one-loop result for the self-energy $\Sigma (K) \propto \int dP G(P) D (K-P)$ is asymptotically exact.


We consider some generalizations of the Asymmetric Traveling Salesman Path problem. Suppose we have an asymmetric metric G = (V,A) with two distinguished nodes s,t. We are also given a positive integer k. The goal is to find k paths of minimum total cost from s to t whose union spans all nodes. We call this the k-Person Asymmetric Traveling Salesmen Path problem (k-ATSPP). Our main result for k-ATSPP is a bicriteria approximation that, for some parameter b >= 1 we may choose, finds between k and k + k/b paths of total length O(b log |V|) times the optimum value of an LP relaxation based on the Held-Karp relaxation for the Traveling Salesman problem. On one extreme this is an O(log |V|)-approximation that uses up to 2k paths and on the other it is an O(k log |V|)-approximation that uses exactly k paths. Next, we consider the case where we have k pairs of nodes (s_1,t_1), ..., (s_k,t_k). The goal is to find an s_i-t_i path for every pair such that each node of G lies on at least one of these paths. Simple approximation algorithms are presented for the special cases where the metric is symmetric or where s_i = t_i for each i. We also show that the problem can be approximated within a factor O(log n) when k=2. On the other hand, we demonstrate that the general problem cannot be approximated within any bounded ratio.


1994.''. (2) Expenditure limits on exceptions.--The aggregate amount of additional payments or payment adjustments made under section 1861(v)(1)(L)(ii)(II), as added by paragraph (1), with respect to a fiscal year may not exceed 5 percent of the aggregate payments projected or estimated by the Secretary to be made under section 1861(v)(1)(L) for such fiscal year. (b) Additional Payments for Outliers.--Section 1861(v)(1)(L) of such Act (42 U.S.C. 1395x(v)(1)(L)), as amended by section 3(a), is further amended by adding at the end the following new clause: ``(xi) Notwithstanding clauses (v) through (ix), the Secretary shall provide for an additional payment amount to a provider equal to the difference between the reasonable cost incurred by the provider and the limit under such clauses applicable to the provider if the provider demonstrates to the Secretary that-- ``(I) the provider incurred costs in excess of the limits applicable under such clauses with respect to an individual described in subclause (II); ``(II) with respect to an individual to whom the provider furnished home health services under this title, the individual requires the most expensive home health services (case outliers) or requires such services for a far longer than average period of time (case and duration outliers), such outliers determined by the Secretary; and ``(III) such incurred costs are reasonable. No payment shall be made under this clause to a provider that, as of October 1, 1999, has ceased furnishing home health services for which payment may be made under this title.''. (c) Effective Date.--The amendments made by this section shall apply as.


Proceed with caution, light spoilers ahead. In The Crown, Prince Philip's close relative Lord Mountbatten is portrayed by English actor Greg Wise. Here's the true story of the man who mentored the Duke of Edinburgh. The Mountbatten connection to the Royal Family Advertisement - Continue Reading Below As with many royal relatives, Louis Mountbatten was related to both Prince Philip and Queen Elizabeth. A great-grandson of Queen Victoria, he was both a distant cousin of the Queen's and Prince Philip's uncle. Philip's mother, Princess Alice of Battenberg, was Louis's sister. Philip also lived with the Mountbattens for several years following his mother's institutionalization. A Complicated Marriage Lord Louis Mountbatten and his wife Lady Edwina in London, 1941. Getty In a particularly tender scene in the first episode of season two of The Crown, Elizabeth II speaks candidly with Uncle Dickie about her marital woes. “You married a wild spirit—we both did," he says, referring to his wife Lady Edwina Ashley Mountbatten, whom he married on July 18, 1922. "Trying to tame them is no use." Advertisement - Continue Reading Below "Of course I considered ending it," he continues. "Then I imagined how thin, how poor life would be. I realized, when you really adore someone, as fully and as hopelessly as I think you and I do, you put up with anything." This season of The Crown centers around infidelity—rumors followed many of the couples featured on the show—but in reality Louis and Edwina Mountbatten had a rather unorthodox marriage. Certainly, Edwina could not be tamed, to use the language of the show, but by 1931 the couple had reportedly "cut a deal," according to the Washington Post: "They would stay together with separate beds and, to some extent, separate lives. But they would remain loving, mutually supportive chums. Above all, they would be discreet." Both Mountbattens had affairs; Louis wasn't just sitting at home sulking. He once reportedly said, "Edwina and I spent all our married lives getting into other people's beds." The couple did have two daughters together: Patricia Knatchbull, who later became the 2nd Countess Mountbatten of Burma, and Lady Pamela Hicks, mother of


We consider the question: can the isotropy representation of an irreducible pseudo-Riemannian symmetric space be realized as a conformal holonomy group? Using recent results of Cap, Gover and Hammerl, we study the representations of SO(2,1), PSU(2,1) and PSp(2,1) as isotropy groups of irreducible symmetric spaces of signature (3,2), (4,4) and (6,8), respectively, describing the geometry induced by a conformal holonomy reduction to the corresponding subgroups. In the case of SO(2,1) we show that conformal manifolds with such a holonomy reduction are always locally conformally flat and hence this group cannot be a conformal holonomy group. This result completes the classification of irreducible conformal holonomy groups in Lorentzian signature. In the case of PSU(2,1), we show that conformal manifolds of signature (3,3) with this holonomy reduction carry, on an open dense subset, a canonical nearly para-Kaehler metric with positive Einstein constant. For PSp(2,1) we also show that there is an open dense subset endowed with a canonical Einstein metric in the conformal class. As a result, after restricting to an open dense subset the conformal holonomy must be a proper subgroup of PSU(2,1) or of PSp(2,1), respectively. Finally, using a recent result of Graham and Willse we prove the following general non-existence result: for a real-analytic, odd-dimensional conformal manifold, the conformal holonomy group can never be given by the isotropy representation of an irreducible pseudo-Riemannian symmetric space.


The proportionate amount of interest on such loan which accrues for such year shall be repaid by the Secretary. (c) Repayment to Eligible Lenders.--The Secretary shall pay to each eligible lender or holder for each fiscal year an amount equal to the aggregate amount of loans which are subject to repayment pursuant to this section for such year. (d) Application for Repayment.-- (1) In general.--Each eligible individual desiring loan repayment under this section shall submit a complete and accurate application to the Secretary at such time, in such manner, and containing such information as the Secretary may require. (2) Conditions.-- (A) Years of service.--An eligible individual may apply for loan repayment under this section after completing the required number of years of qualifying employment. (B) Fully qualified teachers in public elementary or secondary schools.--An application for loan repayment under this section shall include such information as is necessary to demonstrate that the applicant-- (i) if teaching in a public elementary, middle, or secondary school (other than as a teacher in a public charter school), has obtained State certification as a teacher (including certification obtained through alternative routes to certification) or passed the State teacher licensing exam and holds a license to teach in such State; and (ii) if teaching in-- (I) a public elementary school, holds a bachelor's degree and demonstrates knowledge and teaching skills in reading, writing, mathematics, science, and other areas of the elementary school curriculum; or (II) a public middle or secondary school, holds a bachelor's degree and demonstrates a high level of competency in all subject areas in which he or she teaches through-- (aa) a high level of performance on a rigorous State or local academic subject areas test; or (bb) completion of an academic major in each of the subject areas in which he or she provides instruction. (C) Teachers in nonprofit private elementary or secondary schools or charter schools.--In the case of an applicant who is teaching in a nonprofit private elementary or secondary school, or in a charter school, an application for loan repayment under this section shall include such information as is necessary to demonstrate that the applicant has knowledge and teaching skills in reading, writing, and mathematics, as certified by the chief administrative officer of the school. (e) Treatment of Consolidation Loans.--A loan amount for a consolidation loan made under section 428C of the Higher


A family child care provider, or an adult permitted to reside in such a family child care provider's private residence reveals an adult felony conviction for-- ``(A) child abuse or neglect; ``(B) spousal abuse; ``(C) a crime against children (including child pornography); ``(D) a violent crime, including-- ``(i) physical assault or battery; ``(ii) rape; ``(iii) sexual assault; or ``(iv) homicide; or ``(E) distribution of, possession with intent to distribute, or importation of a controlled substance committed within 5 years prior to submission to a criminal background check. ``(3) Submittal of requests.--Subject to paragraph (4), a child care provider or a family child care provider shall submit a request for a State and national criminal background check to the appropriate State agency designated by the State-- ``(A) with respect to an individual who became a child care staff member or family child care provider, or an adult who began to reside in the private residence of such a provider, before the date of the enactment of the Child Care Accountability and Responsibility Act of 2012-- ``(i) not later than the date under subsection (b) in which a State implements the requirements of this section; and ``(ii) during each 5-year period following the first submission date under this subparagraph for such staff member, family provider, or adult; and ``(B) with respect to an individual who is a prospective child care staff member or family child care provider, or an adult who begins to reside in the private residence of such a provider, on or after the date of the enactment of such Act-- ``(i) prior to the date the individual becomes a child care staff member, a family child care provider, or such adult begins to reside in such residence; and ``(ii) during each 5-year period following the first submission date under this subparagraph for such staff member, family provider, or adult. ``(4) Limitation on requests.--Not more than 1 request for a State and national criminal background check under paragraph (3) is required for any child care staff member, family child care provider, or adult who resides in the private residence of such provider, for each 5-year period described in such paragraph. ``(5) Results.-- ``(A) In general.--Not later than 10 business days after the date on which a request under this section is made for


Spin foam models are an attempt for a covariant, or path integral formulation of canonical loop quantum gravity. The construction of such models usually rely on the Plebanski formulation of general relativity as a constrained BF theory and is based on the discretization of the action on a simplicial triangulation, which may be viewed as an ultraviolet regulator. The triangulation dependence can be removed by means of group field theory techniques, which allows one to sum over all triangulations. The main tasks for these models are the correct quantum implementation of the Plebanski constraints, the existence of a semiclassical sector implementing additional "Regge-like" constraints arising from simplicial triangulations, and the definition of the physical inner product of loop quantum gravity via group field theory. Here we propose a new approach to tackle these issues stemming directly from the Holst action for general relativity, which is also a proper starting point for canonical loop quantum gravity. The discretization is performed by means of a "cubulation" of the manifold rather than a triangulation. We give a direct interpretation of the resulting spin foam model as a generating functional for the n-point functions on the physical Hilbert space at finite regulator. This paper focuses on ideas and tasks to be performed before the model can be taken seriously. However, our analysis reveals some interesting features of this model: first, the structure of its amplitudes differs from the standard spin foam models. Second, the tetrad n-point functions admit a "Wick-like" structure. Third, the restriction to simple representations does not automatically occur --.


, IMF, and World Bank. The Georgian Government has only applied this new law, which gives the Government the right to seize loan collateral before the banks that issued the loan, to Bank Cartu and no other banks. As a result, the Saakashvili regime continues to seize Bank Cartu assets in an effort to force the bank out of business and remove a source of Ivanishvili's financial support. (20) United States national security interests are best served by a democratic Georgia no matter what individuals and which parties are in control of the country. An undemocratic Georgia will breed instability in a volatile region and increase the likelihood of violent conflict. As such, it is incumbent on the United States Government to clearly communicate to President Saakashvili that if he continues down his current path and does not allow free, fair, and competitive elections, the special relationship between the United States and Georgia will be at risk and Georgia will face the loss of both United States political support and financial assistance. SEC. 3. LIMITATION ON ASSISTANCE TO THE REPUBLIC OF GEORGIA. (a) Limitation.--No funds available to any United States department or agency for fiscal year 2013 may be used to provide assistance to the Republic of Georgia until the Secretary of State certifies and reports to the Committee on Foreign Affairs of the House of Representatives and the Committee on Foreign Relations of the Senate that the parliamentary elections held in October 2012 or such other date if rescheduled were carried out in a free, fair, and competitive manner consistent with international standards. (b) Matters To Be Included.--The report required under subsection (a) shall include information on-- (1) the presence and findings of election observers; (2) the ability of opposition parties to campaign effectively; and (3) whether Bidzina Ivanishvili and the Georgian Dream Party participated in the election, and.


Applicable life insurance account'' after ``health benefits account'' each place it appears, and (B) in paragraph (1), by inserting ``or applicable life insurance benefit liabilities'' after ``health benefits liabilities''. (f) Technical Correction.--Clause (iii) of section 420(f)(6)(B) is amended by striking ``416(I)(1)'' and inserting ``416(i)(1)''. (g) Repeal of Deadwood.-- (1) Subparagraph (A) of section 420(b)(1) of the Internal Revenue Code of 1986 is amended by striking ``in a taxable year beginning after December 31, 1990''. (2) Subsection (b) of section 420 of such Code is amended by striking paragraph (4) and by redesignating paragraph (5), as amended by this Act, as paragraph (4). (3) Paragraph (2) of section 420(b) of such Code, as amended by this section, is amended-- (A) by striking subparagraph (B), and (B) by striking ``per year.--'' and all that follows through ``No more than'' and inserting ``per year.--No more than''. (4) Paragraph (2) of section 420(c) of such Code is amended-- (A) by striking subparagraph (B), (B) by moving subparagraph (A) two ems to the left, and (C) by striking ``before transfer.--'' and all that follows through ``The requirements of this paragraph'' and inserting the following: ``before transfer.--The requirements of this paragraph''. (5) Paragraph (2) of section 420(d) of such Code is amended by striking ``after December 31, 1990''. (h) Effective Date.-- (1) In general.--The amendments made by this section shall apply to transfers made after the date of the enactment of this Act. (2) Conforming amendments relating to pension protection act.--The amendments made by subsections (b)(3)(B) and (f) shall take effect as.


Let (g,K)(k) be a CMC (vacuum) Einstein flow over a compact three-manifold M with non-positive Yamabe invariant (Y(M)). As noted by Fischer and Moncrief, the reduced volume V(k)=(-k/3)^{3}Vol_{g(k)}(M) is monotonically decreasing in the expanding direction and bounded below by V_{\inf}=(-1/6)Y(M))^{3/2}. Inspired by this fact we define the ground state of the manifold M as "the limit" of any sequence of CMC states {(g_{i},K_{i})} satisfying: i. k_{i}=-3, ii. V_{i} --> V_{inf}, iii. Q_{0}((g_{i},K_{i}))< L where Q_{0} is the Bel-Robinson energy and L is any arbitrary positive constant. We prove that (as a geometric state) the ground state is equivalent to the Thurston geometrization of M. Ground states classify naturally into three types. We provide examples for each class, including a new ground state (the Double Cusp) that we analyze in detail. Finally consider a long time and cosmologically normalized flow (\g,\K)(s)=((-k/3)^{2}g,(-k/3))K) where s=-ln(-k) is in [a,\infty). We prove that if E_{1}=E_{1}((\g,\K))< L (where E_{1}=Q_{0}+Q_{1}, is the sum of the zero and first order Bel-Robinson energies) the flow (\g,\K)(s) persistently geometrizes the three-manifold M and the geometrization is the ground state.


The author gives the full list of his conjectures on series for powers of $\pi$ and other important constants scattered in some of his public papers or his private diaries. The list contains 234 reasonable conjectural series. On the list there are 178 reasonable series for $\pi^{-1}$, four series for $\pi^2$, two series for $\pi^{-2}$, four series for $\pi^4$, two series for $\pi^5$, three series for $\pi^6$, seven series for $\zeta(3)$, one series for $\pi\zeta(3)$, two series for $\pi^2\zeta(3)$, one series for $\zeta(3)^2$, three series involving both $\zeta(3)^2$ and $\pi^6$, one series for $\zeta(5)$, three series involving both $\zeta(5)$ and $\zeta(2)\zeta(3)$, two series involving both $\pi\zeta(5)$ and $\pi^3\zeta(3)$, three series involving $\zeta(7)$, three series for $K=L(2,(\frac{\cdot}{3}))$, one series for the Catalan constant $G$, two series for $\pi G$, one series involving both $\pi^3G$ and $\pi^2\zeta(3)$, two series for $\pi K$, two series involving $L=L(4,(\frac{\cdot}3))$, three series involving $\beta(4)=L(4,(\frac{-4}{\cdot}))$, and four series for $\pi^2\log a$ with $a=2,3,(\sqrt5+1)/2$. The code of a conjectural series is underlined.


, 2019-- (1) the pause or moratorium on the issuance of new Federal coal leases under the Secretarial order referred to in subsection (a)(1) is terminated; and (2) that Secretarial order shall have no force or effect. SEC. 5. GRANDFATHERING OF COAL LEASES ON APPLICATION AND COAL LEASE MODIFICATIONS. Nothing in the order of the Secretary of the Interior entitled ``Discretionary Programmatic Environmental Impact Statement to Modernize the Federal Coal Program'', numbered 3338 and dated January 15, 2016, shall be considered to prohibit or restrict any issuance of a coal lease on application or coal lease modification, pursuant to section 3432 of title 43, Code of Federal Regulations, for which the Bureau of Land Management has begun its review under section 102 of the National Environmental Policy Act of 1969 (42 U.S.C. 4332) as of January 15, 2016. SEC. 6. DEADLINE FOR COAL LEASE SALES AND MODIFICATIONS. Not later than 1 year after the date on which the Secretary completes the analysis required under section 102 of the National Environmental Policy Act of 1969 (42 U.S.C. 4332) for an application for a coal lease, or an application for a modification to a coal lease pursuant to subpart 3432 of part 3430 of title 43, Code of Federal Regulations (or successor regulations), accepted by the Secretary, the Secretary shall conduct the lease sale and issue the lease, or approve the modification.


Let $E_d(n)$ be the maximum number of pairs that can be selected from a set of $n$ points in $R^d$ such that the midpoints of these pairs are convexly independent. We show that $E_2(n)\geq \Omega(n\sqrt{\log n})$, which answers a question of Eisenbrand, Pach, Rothvo\ss, and Sopher (2008) on large convexly independent subsets in Minkowski sums of finite planar sets, as well as a question of Halman, Onn, and Rothblum (2007). We also show that $\lfloor\frac{1}{3}n^2\rfloor\leq E_3(n)\leq \frac{3}{8}n^2+O(n^{3/2})$. Let $W_d(n)$ be the maximum number of pairwise nonparallel unit distance pairs in a set of $n$ points in some $d$-dimensional strictly convex normed space. We show that $W_2(n)=\Theta(E_2(n))$ and for $d\geq 3$ that $W_d(n)\sim\frac12\left(1-\frac{1}{a(d)}\right)n^2$, where $a(d)\in N$ is related to strictly antipodal families. In fact we show that the same asymptotics hold without the requirement that the unit distance pairs form pairwise nonparallel segments, and also.


Right in line with the GTX 1080, and beats it by a more comfortable margin than the RX Vega 56. Nvidia’s champion, the GTX 1080 Ti, remains far ahead of the RX Vega 64 – yet at pricing just below $700 for the most affordable variants, it’s not in the same league. How long will it last? With solid 1080p and 1440p performance, the Radeon RX Vega 56 and RX Vega 64 should have no problem keeping up for several years. The openness of FreeSync also gives AMD an edge here, since it should be easier and more affordable to upgrade to a FreeSync monitor in the future, if you don’t have on already. Should you buy it? Yes, for both models – with the RX Vega 56 taking an edge in terms of value. At $400, it’s still expensive by the standards of most gamers (you could buy a PS4 Pro for as much), but it delivers top-tier performance at 1080p and 1440p resolution. It delivers GTX 1080-level performance for $100 less, and that’s awesome. The RX Vega 64 is also recommended, but we’re surprised by the small improvement it offers over the RX Vega 56. That blunts its value. Will you notice that the RX Vega 64 is, on average, three frames per second quicker than the RX Vega 56 in Battlefield 1? We doubt it. Yet the RX Vega 64 does generally beat the GTX 1080, and it’s priced the same. That makes it the card to buy if you have $500 to spend. Vega is a not the landslide AMD needs, but it is a victory. Nvidia’s alternatives have been around for some time, and the green team could blunt much of AMD’s momentum by dropping prices. Still, a win is a win. RX Vega is the way to go.


The classical Lojasiewicz inequality and its extensions for partial differential equation problems (Simon) and to o-minimal structures (Kurdyka) have a considerable impact on the analysis of gradient-like methods and related problems: minimization methods, complexity theory, asymptotic analysis of dissipative partial differential equations, tame geometry. This paper provides alternative characterizations of this type of inequalities for nonsmooth lower semicontinuous functions defined on a metric or a real Hilbert space. In a metric context, we show that a generalized form of the Lojasiewicz inequality (hereby called the Kurdyka-Lojasiewicz inequality) relates to metric regularity and to the Lipschitz continuity of the sublevel mapping, yielding applications to discrete methods (strong convergence of the proximal algorithm). In a Hilbert setting we further establish that asymptotic properties of the semiflow generated by $-\partial f$ are strongly linked to this inequality. This is done by introducing the notion of a piecewise subgradient curve: such curves have uniformly bounded lengths if and only if the Kurdyka-Lojasiewicz inequality is satisfied. Further characterizations in terms of talweg lines -a concept linked to the location of the less steepest points at the level sets of $f$- and integrability conditions are given. In the convex case these results are significantly reinforced, allowing in particular to establish the asymptotic equivalence of discrete gradient methods and continuous gradient curves. On the other hand, a counterexample of a convex C^2 function in in the plane is constructed to illustrate the fact that, contrary to our intuition, and.


Non-gaussianity in the initial conditions of the universe is one of the most powerful mechanisms to discriminate among the competing theories of the early universe. Measurements using bispectrum of cosmic microwave background anisotropies are limited by the cosmic variance, i.e. available number of modes. Recent work has emphasized the possibility to probe non-gaussianity of local type using the scale dependence of large scale bias from highly biased tracers of large scale structure. However, this power spectrum method is also limited by cosmic variance, finite number of structures on the largest scales, and by the partial degeneracy with other cosmological parameters that can mimic the same effect. Here we propose an alternative method that solves both of these problems. It is based on the idea that on large scales halos are biased, but not stochastic, tracers of dark matter: by correlating a highly biased tracer of large scale structure against an unbiased tracer one eliminates the cosmic variance error, which can lead to a high signal to noise even from the structures comparable to the size of the survey. The square of error improvement on non-gaussianity parameter f_nl relative to the power spectrum method scales as Pn/2, where P and n is the power spectrum and the number density of the biased tracer, respectively. For an ideal survey out to z=2 the error reduction can be as large as a factor of seven, which should guarantee a detection of non-gaussianity from an all sky survey of this type. The improvements could be even larger.


Your menstrual cycle is regular Marcos Mesa Sam Wordley/Shutterstock"Regular menstrual cycles (intervals of 27 to 35 days) are a sign of reproductive health. Regular cycles suggest normal ovulation, and that reflects balanced hormone levels from the brain down to the ovaries. Women who are unhealthy because they're overweight or underweight tend to have more erratic or even absent periods; the brain shuts down ovarian function and ovulation doesn't happen or happens unpredictably." —Janet Choi, MD, reproductive endocrinologist, CCRM-New York. These are the period problems you shouldn't ignore. You have thick hair and strong nails Focus and Blur/Shutterstock"Thick abundant hair and firm, fast growing nails tend to be a sign of good health. The opposite, thinning hair, brittle or cracked nails are often a sign of marked nutritional deficiencies such as lack of iron, Vitamin D and other key vitamins." —Arielle Levitan MD, founder of Vous Vitamin, LLC. If you're looking to get more luster in your hair and nails, check out these quick tips. You tend to have a lot of energy A. and I. Kruk/Shutterstock"If you spring out of bed each morning, ready to hit the gym and face the day, you are likely doing pretty well. Many illnesses and vitamin deficiencies can leave you sluggish, lacking energy and fatigued." —Arielle Levitan MD, founder, Vous Vitamin, LLC Content continues below ad You can deal with your emotions and others' emotions. fizkes/Shutterstock"We've all got needs—for connection, nurturing, respect, autonomy, to name just a few—and being able to recognize, express, and pursue these creates better relationships and a happier life. Healthy people also try to understand and meet the emotional needs of others. They're curious and attentive to how others feel. When they do something that's hurtful, they make amends and they make changes." —Holly Brown, marriage and family therapist. These are the five things you need for emotional intelligence. You don't get many headaches, and they don't last long Syda Productions/Shutterstock"Headaches—we all get them. They are the result of stress, or tense musculature, and are normal. In a healthy person, they pass in time and do not linger. An occasional migraine or other headache is not uncommon, but if medications no longer work, and other medical causes have


Given two genomes with duplicate genes, \textsc{Zero Exemplar Distance} is the problem of deciding whether the two genomes can be reduced to the same genome without duplicate genes by deleting all but one copy of each gene in each genome. Blin, Fertin, Sikora, and Vialette recently proved that \textsc{Zero Exemplar Distance} for monochromosomal genomes is NP-hard even if each gene appears at most two times in each genome, thereby settling an important open question on genome rearrangement in the exemplar model. In this paper, we give a very simple alternative proof of this result. We also study the problem \textsc{Zero Exemplar Distance} for multichromosomal genomes without gene order, and prove the analogous result that it is also NP-hard even if each gene appears at most two times in each genome. For the positive direction, we show that both variants of \textsc{Zero Exemplar Distance} admit polynomial-time algorithms if each gene appears exactly once in one genome and at least once in the other genome. In addition, we present a polynomial-time algorithm for the related problem \textsc{Exemplar Longest Common Subsequence} in the special case that each mandatory symbol appears exactly once in one input sequence and at least once in the other input sequence. This answers an open question of Bonizzoni et al. We also show that \textsc{Zero Exemplar Distance} for multichromosomal genomes without gene order is fixed-parameter tractable.


Blast away from traffic lights (thanks to a 48-horsepower motor that pushes 53 pounds of torque). There are two other modes available: Road gives you all the power with a little regenerative braking while Sail removes all regenerative braking. I stuck with Eco Pro and Dynamic modes for 95 percent of my rides, since they offered the best combination of riding and regenerative energy creation. Regardless of how you ride, there is the usual electric-vehicle caveat that if you spend any time at high speeds on the freeway, you're going to burn through your charge. During an 11-mile jaunt on the highway at a steady 65MPH, I drained 20 percent of the battery. That's something to consider if you're interested in any EV for a daily commute that involves a lot of time on the freeway. Recharging the bike after flying down the highway via the level 2 port took about 4 to 4.5 hours. It can also be charged with the 110-volt outlet you have at home, but expect it to take about twice as long. In a city like Los Angeles where malls, Whole Foods Markets and other businesses have chargers in their parking lot, pushing past the century mark during a single day wasn't a problem -- that is, if you're cool shopping or eating while you charge. That might not be so healthy for the bank account. That's the rub with electric motorcycles and scooters. Unlike their four-wheeled counterparts, it's tough to see a financial incentive. The gas-powered BMW counterparts to the C evolution both get 51 miles per gallon, so the monthly outlay of cash isn't that high to begin with. There are the maintenance cost savings, but with a price tag that's about $3,000 more than comparable with BMW gas-powered scooters, it's tough to see the financial upside of the C evolution. That said, as I rode through LA and saw a constant brown haze on the horizon, both over land and water, it was a reminder that petrol-powered vehicles contribute to that smog. In the grand scheme of things, it's important to see the C evolution and other EVs as vehicles that will reduce that brown sky. Sure, on a spreadsheet buying one doesn't add up, but when you take into account the impact vehicles have on our air.


We present the first metallicity distribution functions of the old field populations in the Magellanic Clouds. Our metallicities are based on the Fourier decomposition of Type ab RR Lyrae light curves from the Optical Gravitational Lensing Experiment (OGLE-III). On the metallicity scale of Zinn & West; we find a mean metallicity of [Fe/H] = -1.50 +/- 0.24 dex based on 16776 RR Lyrae stars in the Large Magellanic Cloud (LMC). For the Small Magellanic Cloud (SMC) we obtain -1.70 +/- 0.27 dex based on 1831 RR Lyrae stars. These uncertainties represent the intrinsic spread in the population rather than the standard deviation of the mean. Our results are in good agreement with the few existing spectroscopic metallicity determinations for LMC RR Lyrae stars from the literature. For both the LMC and the SMC the metallicity spread exceeds 1 dex in [Fe/H]. The distribution of metallicities in both Clouds is very uniform, and no significant metallicity gradient is detectable. We also do not find any pronounced populations of extremely metal-poor RR Lyrae candidates with metallicities well below -2 dex, although we need to caution that the photometric method used may overestimate the metallicities of metal-deficient stars. Moreover, because of stellar evolutionary effects one does not expect to observe many RR Lyrae stars among very metal-poor horizontal branch stars. We suggest that the Magellanic Clouds experienced fairly rapid and efficient early enrichment involving pre-enriched gas as well as possibly gas infall, while metal loss through outflows does not seem to have played a significant role. Moreover we suggest that the differences in the metallicities of the old population of LMC and SMC make an origin from a single, common progenitor unlikely.


The Secretary shall advise the management entity in writing of the reasons for the disapproval and shall make recommendations for revisions to the management plan. (B) Deadline for approval of revision.--The Secretary shall approve or disapprove a proposed revision within 90 days after the date on which the revision is submitted to the Secretary. (c) Approval of Amendments.-- (1) Review.--The Secretary shall review substantial amendments (as determined under section 6(c)(8)) to the management plan for the Heritage Area. (2) Requirement of approval.--Funds made available under this Act shall not be expended to implement the amendments described in paragraph (1) until the Secretary approves the amendments. SEC. 8. SUNSET PROVISION. The Secretary shall not provide any grant or other assistance under this Act after September 30, 2012. SEC. 9. AUTHORIZATION OF APPROPRIATIONS. (a) In General.--There is authorized to be appropriated to carry out this Act $10,000,000, except that not more than $1,000,000 may be appropriated to carry out this Act for any fiscal year. (b) 50 Percent Match.--The Federal share of the cost of activities carried out using any assistance or grant under this Act shall not exceed 50 percent. Passed the Senate November 19, 1999. Attest: Secretary. 106th CONGRESS 1st Session S. 905 _______________________________________________________________________ AN ACT To establish the Lackawanna Valley National Heritage Area and for other purposes.


Be prepared for traffic. "They definitely need to leave earlier and that is anytime for any school zone, particularly for this one but leave yourself enough time so that when traffic does back that you are not rushed, the kids aren't going to be late for school, they aren't going to be late for work and nobody is trying to short cut," said Officer Jamie Hamrick, a prevention resource officer at schools in Bridgeport and member of the Bridgeport Police Department. Drop off will be different this year at Johnson Elementary because of construction for the new school. A few things have changed to the drop off routine and parents and commuters need to be aware when traveling in front of the schools. "Johnson Avenue does not have the entrance that they had last year for Johnson Elementary School. This year all Johnson traffic will have to come down City Park Drive and then come behind the school, let their kids out or go into the parking lot and then proceed out because there is only one way in and one way out this year," explained Hamrick. Parents must enter the City Park entrance and travel around the back of the school. The parking lot next to the school's entrance has been repaved and is just for parent parking. "I will be out in the back actually this year trying to keep things moving along because the high school students will actually be coming down the same way and then parking behind the high school so I will be directing traffic back there but yes we will be having an increased police presence out along Johnson Avenue, making sure everyone is going the way they should be," added Hamrick. The best advice Bridgeport Police can give the community? Avoid Johnson Avenue if you are not part of school traffic and remember, Johnson Avenue is 15 m.p.h during school times.


What time will their next match be? And where can you watch it? England are now just one game away from reaching a World Cup semi-final and having their best tournament since Italia 1990. But if they beat Sweden in their quarter-final (Saturday 7th July, 3pm, BBC1), when will they play next? And against who? Advertisement Here’s everything you need to know… When will England play in the World Cup 2018 semi-finals? If they reach this stage, England will play at Luzhniki on Wednesday 11 July. What time is kick off? The match begins at 7pm BST What channel is the game on? If England get through, the match is extremely likely to air on ITV, with the broadcaster having first dibs of the semi-final games. Who could England play against in the World Cup semi-finals? The Three Lions could face a match between Croatia or hosts Russia. Those two sides play Saturday 7th July at 7pm, ITV – a few hours after England’s game with Sweden. Check the full World Cup 2018 schedule here. Advertisement Who could the winner face in the final? The victor of this semi-final will go on to face either Uruguay, France, Brazil or Belgium, with those four sides currently contending in the quarter-finals. The final will be held at the Luzhniki Stadium in Moscow at 4pm BST on Sunday 15th July, with the game airing both on ITV and BBC1.


The requirements of such title solely on the basis of its failure to meet these additional requirements before the first day of the first calendar quarter beginning after the close of the first regular session of the State legislature that begins after the date of enactment of this Act. For purposes of the previous sentence, in the case of a State that has a 2-year legislative session, each year of the session is considered to be a separate regular session of the State legislature. SEC. 4. INCREASING AWARENESS OF THE IMPORTANCE OF END-OF-LIFE PLANNING. Title III of the Public Health Service Act (42 U.S.C. 241 et seq.) is amended by adding at the end the following new part: ``PART R--PROGRAMS TO INCREASE AWARENESS OF ADVANCE DIRECTIVE PLANNING ISSUES ``SEC. 399Z-1. ADVANCE DIRECTIVE EDUCATION CAMPAIGNS AND INFORMATION CLEARINGHOUSES. ``The Secretary shall provide for the establishment of a national, toll-free, information clearinghouse as well as clearinghouses that the public may access to find out about State-specific information regarding advance directive and end-of-life decisions.''. SEC. 5. GAO STUDY AND REPORT ON ESTABLISHMENT OF NATIONAL ADVANCE DIRECTIVE REGISTRY. (a) Study.--The Comptroller General of the United States shall conduct a study on the feasibility of a national registry for advance directives, taking into consideration the constraints created by the privacy provisions enacted as a result of the Health Insurance Portability and Accountability Act. (b) Report.--Not later than 18 months after the date of enactment of this Act, the Comptroller General of the United States shall submit to Congress a report on the study conducted under subsection (a) together with recommendations for such legislation and administrative action as the Comptroller General of the United States determines to be appropriate. SEC. 6. ADVANCE DIRECTIVES AT STATE DEPARTMENT OF MOTOR VEHICLES. Each State shall establish a program of providing information on the advance directives clearinghouse established pursuant to section 399Z-1 of the Public Health Service Act to individuals who are residents of the State at such State's department of motor vehicles. Such program shall be modeled after the program of providing information regarding organ donation established at the State's department of motor vehicles.


We present the burst ages for young stellar populations in a sample of six nearby (< 10 Mpc) spiral galaxies using a differential pixel-based analysis of the ionized gas emission. We explore this as an alternative approach for connecting large-scale dynamical mechanisms with star formation processes in disk galaxies, based on burst ages derived from the Ha to far UV (FUV) flux ratio. Images of each galaxy in Ha were taken with Taurus Tunable Filter (TTF) and matched to FUV imaging from GALEX. The resulting flux ratio provides a robust measure of relative age across the disk which we discuss in terms of the large-scale dynamical motions. Systematic effects, such as a variable initial mass function (IMF), non-solar metallicities, variable star-formation history (SFHs), and dust attenuation, have been used to derive estimates of the systematic uncertainty. The resulting age maps show a wide range of patterns outside of those galaxies with the strongest spiral structure, confirming the idea that star formation is driven one by several processes, largely determined by the individual circumstances of the galaxy. Generally, grand design spirals such as M74, M100, and M51 exhibit age gradients across the main spiral arms, with the youngest star formation regions along the central and inner edges. In M63 and M74 galaxy-wide trends emerge, suggesting that although most star formation is located along spiral arms, spiral density waves are not the only driver in these cases. We argue that despite appearances, galaxy morphology is not an absolute discriminator of the star formation history of an individual galaxy, nor of the processes triggering it. We conclude that Ha-to-FUV flux ratios are a relatively direct way to probe burst ages across galaxies and infer something of their dynamical histories.


Government data that focuses specifically on that population. For that reason, many assertions about the effects of family immigration tend to be based on assumptions about the skills and education held by family-sponsored immigrants. “Do I think the poor labor market for situation for these folks is a serious and profound social problem? You bet,” Camarota said. “Do I think immigration is contributing to that problem? I do.” But others say a policy that reduces legal immigration would probably hurt Americans more than it would help. “If we want our economy to be dynamic, we need immigrants,” said Jim Russell, a research consultant with the Center for Population Dynamics at Cleveland State University. Cities like Cleveland are struggling to attract residents, he said. At the same time, immigrants are helping to fill gaps in the region’s labor market, not just in low-skill jobs in the service and agriculture sectors, but also in high-skill professions like engineering and medicine. If those folks can’t someday bring their parents or siblings, Russell said, they may be deterred from moving here. “The signal you're sending to the rest of the world is one that will reach highly skilled people as well,” he said. “And they will see the United States as intolerant and instead of going to Cleveland, they'll go to Toronto, or they'll go to Sydney.” Or professionals, like attorney Su He, may decide to leave. Ms. He moved here from China about a decade ago to attend law school at Case Western Reserve University. Along the way, she met her husband, a scientist. And last year she hung up a shingle, her own immigration law practice. She said, she and her husband have plans to put down roots in Cleveland, become citizens, and one day, sponsor their aging parents to come live here. “When I get older, my parents get older,” she said, “and because me and my husband, we’re both the only child in the family, if we don’t care of them, no one will take care of them.” But those plans could change if President Trump were to get his way. Ms. He said.


We use a non-equilibrium chemical network to revisit and study the effect of H_{2}, HD and LiH molecular cooling on a primordial element of gas. We solve both the thermal and chemical equations for a gas element with an initial temperature T\approx 1000K and a gas number density in the range n_{tot}=1-10^{4} cm^{-3}. At low densities, n_{tot}<10^{2} cm^{-3}, the gas reaches temperatures \sim 100K and the main coolant is H_{2}, but at higher densities, n_{tot}>10^{2} cm^{-3}, the HD molecule dominates the gas temperature evolution. The effect of LiH is negligible in all cases. We studied the effect of D abundance on the gas cooling. The D abundance was set initially to be in the range n_{D}/n_{H}=10^{-7}-10^{-4.5}, with n_{HD}/n_{H}={D^{+}}/n_{H}=10^{-10}. The simulations show that at n_{tot}>10^{2} cm^{-3} the HD cooling dominates the temperature evolution for D abundances greater than 10^{-5}n_{H}. This number decrease at higher densities. Furthermore, we studied the effect of electrons and ionized particules on the gas temperature. We followed the gas temperature evolution with n_{H_{+}}/n_{H}=10^{-4}-10^{-1} and n_{D^{+}}/n_{H^{+}}=10^{-5}. The gas temperature reached lower values at high ionization degree because electrons, H^{+} and D^{+} are catalizers in the formation paths of the H_{2} and HD molecules, which are the main coolers at low temperatures. Finaly, we studied the effect of an OB star, with T_{eff}=4\times 10^{4}K, would have on gas cooling. It is very difficult for a gas with n_{tot} in the range between 1-100 cm^{-3} to drop its temperature.


Observations are revealing the ubiquity of filamentary structures in molecular clouds. As cores are often embedded in filaments, it is important to understand how line profiles from such systems differ from those of isolated cores. We perform radiative transfer calculations on a hydrodynamic simulation of a molecular cloud in order to model line emission from collapsing cores embedded in filaments. We model two optically thick lines, CS(2-1) and HCN(1-0), and one optically thin line, N2H+(1-0), from three embedded cores. In the hydrodynamic simulation, gas self-gravity, turbulence, and bulk flows create filamentary regions within which cores form. Though the filaments have large dispersions, the N2H+(1-0) lines indicate subsonic velocities within the cores. We find that the observed optically thick line profiles of CS(2-1) and HCN(1-0) vary drastically with viewing angle. In over 50% of viewing angles, there is no sign of a blue asymmetry, an idealised signature of infall motions in an isolated spherical collapsing core. Profiles which primarily trace the cores, with little contribution from the surrounding filament, are characterised by a systematically higher HCN(1-0) peak intensity. The N2H+(1-0) lines do not follow this trend. We demonstrate that red asymmetric profiles are also feasible in the optically thick lines, due to emission from the filament or one-sided accretion flows onto the core. We conclude that embedded cores may frequently undergo collapse without showing a blue asymmetric profile, and that observational surveys including filamentary regions may underestimate the number of collapsing cores.


We present Chandra ACIS-I and ACIS-S observations (~200ks in total) of the X-ray luminous elliptical galaxy NGC4636, located in the outskirts of the Virgo cluster. A soft band (0.5-2 keV) image shows the presence of a bright core in the center surrounded by an extended X-ray corona and two pronounced quasi-symmetric, 8 kpc long, arm-like features. Each of this features defines the rim of an ellipsoidal bubble. An additional bubble-like feature, whose northern rim is located ~2 kpc south of the north-eastern arm, is detected as well. We present surface brightness and temperature profiles across the rims of the bubbles, showing that their edges are sharp and characterized by temperature jumps of about 20-25%. Through a comparison of the observed profiles with theoretical shock models, we demonstrate that a scenario where the bubbles were produced by shocks, probably driven by energy deposited off-center by jets, is the most viable explanation to the X-ray morphology observed in the central part of NGC4636. As a confirmation to this scenario, radio jets extending towards the bubbles and a central weak X-ray and radio source are detected and are most likely the signs of AGN activity which was more intense in the past. A bright dense core of ~1 kpc radius is observed at the center of NGC4636. A sharp decline in surface brightness from the core to the ambient gas is observed and is not accompanied by a variation in the temperature and thus could not be in thermal pressure equilibrium. However the bright core could be a long lived feature.


000 as Royal Mail begins its search for the UK’s most festive home. Whether you live in a bungalow or a flat, the Stop, Look, Glisten campaign is encouraging homeowners to transform their properties into magical award-winning grottos that even Santa Claus would be proud of. Stop, Look, Glisten. David Gold, Royal Mail spokesperson, said: “When it comes to an award-winning house, we’re looking for originality, personality and festivity. “Royal Mail has a footprint in communities across the UK and we enjoy all the brilliant and magical ways people celebrate Christmas.” He added: “Light decorations are a particular favourite. That’s why we decided to launch our Stop, Look, Glisten competition, to encourage people across the UK to take pride in their decorations and share them far and wide.” The lucky winner will win £1,000 whilst the runners up will receive a set of 50 Christmas stamps and a framed personalised image. Do you live in the UK's most festive home? But whilst the decorations go up, Royal Mail are reminding contestants not to blind their local postie with festive lights, and to stay safe. “Whilst Christmas lights are a beautiful addition to our communities, it’s important to remember to stay safe when decorating your house and take the appropriate precautions,” said Gold. “Also, keep in mind how your decorations might impact those visiting you – especially your postman or postwoman!” To be in with a chance of winning, send an image or video of your house to glisten@jpress.co.uk, upload your image/video on Twitter or Instagram including #ChristmasLights, @RoyalMail and @sunderlandecho, or visit www.facebook.com/RoyalMail. The Stop, Look, Glisten competition closes midnight on Sunday, December 17, and the winner and runners-up will be announced week commencing December 18. The usual terms and conditions apply to this competition. This Competition Notice should be read together with, and is in addition to, Johnston Press Plc’s Competition/Prize Draw Terms and Conditions at: www.johnstonpress.co.uk/terms-conditions


We study near a Feshbach resonance, as a function of the mass ratio, the fermion-dimer scattering amplitude in fermionic mixtures of two fermion species. When masses are equal the physical situation is known to be quite simple. We show that, when the mass ratio is increased, the situation becomes much more complex. For the s-wave contribution we obtain an analytical solution in the asymptotic limit of very large mass ratio. In this regime the s-wave scattering amplitude displays a large number of zeros, essentially linked to the known large value of the fermion-dimer scattering length in this regime. We find by an exact numerical calculation that a zero is still present for a mass ratio of 15. For the p-wave contribution we make our study below the mass ratio of 8.17, where a fermion-dimer bound state appears. We find that a strong p-wave resonance is present at low energy, due to a virtual bound state, in the fermion-dimer system, which is a forerunner of the real bound state. This resonance becomes prominent in the mass ratio range around the one corresponding to the $^{40}$K - $^6$Li mixtures, much studied experimentally. This resonance should affect a number of physical properties. These include the equation of state of unbalanced mixtures at very low temperature but also the equation of state of balanced mixtures at moderate or high temperature. The frequency and the damping of collective modes should also provide a convenient way to evidence this resonance. Finally it should be possible to modify the effective mass of one of the fermionic species by making use of an optical lattice. This would allow to study the strong dependence of the resonance as a function of the mass ratio of the two fermionic elements. In particular one could check.


Say this for Mayor de Blasio: He’s an equal-opportunity enabler. Fat cats, lobbyists, unions — they all get to wield their influence at City Hall, once they pledge their loyalty (and their wallets) to the mayor. That de Blasio is a union advocate is no secret. But now PoliticoNY reports that some unions seem to be more equal than others. Hundreds of pages of newly disclosed e-mails show that 32BJ SEIU, which represents building-service workers, pretty much ran the process of coming up with new laws to “protect” non-unionized fast-food workers. That included drafting, editing and dictating last-minute changes to a set of bills even before it was introduced in the City Council. Yes, it’s normal for elected officials to routinely solicit input from advocates for and against proposed legislation, and that’s what the mayor’s minions claim is all that happened here. But Politico New York says the e-mails (released under the Freedom of Information laws) show that here it was the union, not City Hall, driving the bill-drafting process. And with good reason: Besides setting scheduling rules for fast-food workers, one bill required employers to deduct fees for a nonprofit if employees request it. That nonprofit, Fast Food Justice, claims 1,200 members. Critics call it an alternative union not subject to the disclosure rules that govern actual unions. But (as Politico notes) if Fast Food Justice evolves into a real union, as is its goal, then it will logically become part of 32BJ, the first union to back de Blasio’s re-election. Whether 32BJ or BerlinRosen or Jona Rechnitz or Harendra Singh, everyone has long known they can gain something from Team de Blasio.


It is well known that the differential operators $X=Q(x)$, $Y=Q(\partial)$, and $H=E+\frac{n}{2}$, where $E$ is the Euler operator, generate a Lie algebra isomorphic to ${\go sl}_{2}$. Therefore the associative algebra they generate is a quotient of the universal enveloping algebra ${\cal U}({\go sl}_{2})$. This fact is in some sense the foundation of the metaplectic representation. The present paper is devoted to the study of the case where $Q(x)$ is replaced by $\Delta_{0}(x)$, where $\Delta_{0}(x)$ is the relative invariant of a prehomogeneous vector space of commutative parabolic type ($ {\go g},V $), or equivalently where $\Delta_{0}$ is the "determinant" function of a simple Jordan algebra $V$ over ${\bb C}$. In this Part I we show several structure results for the associative algebra generated by $X=\Delta_{0}(x)$, $Y=\Delta_{0}(\partial)$. Our main result shows that if we consider this algebra as an algebra over a certain commutative ring ${\bf A}$ of invariant differential operators it is isomorphic to the quotient of what we call a generalized Smith algebra $S(f, {\bf A}, n)$ where $f\in {\bf A}[t]$. The Smith algebras (over ${\bb C}$) were introduced by P. Smith as "natural" generalizations of ${\cal U}({\go sl}_{2})$.


Action and a copy of the complaint to the Federal Trade Commission immediately upon the filing of the action. (3) Authority of federal trade commission.-- (A) In general.--On receiving notice under paragraph (2) of an action under this subsection, the Federal Trade Commission shall have the right-- (i) to intervene in the action; (ii) upon so intervening, to be heard on all matters arising therein; and (iii) to file petitions for appeal. (B) Limitation on state action while federal action is pending.--If the Federal Trade Commission or the Attorney General of the United States has instituted a civil action for violation of a rule promulgated under subsection (a) (referred to in this subparagraph as the ``Federal action''), no State attorney general, official, or agency may bring an action under this subsection during the pendency of the Federal action against any defendant named in the complaint in the Federal action for any violation of such rule alleged in such complaint. (4) Rule of construction.--For purposes of bringing a civil action under this subsection, nothing in this Act shall be construed to prevent an attorney general, official, or agency of a State from exercising the powers conferred on the attorney general, official, or agency by the laws of such State to conduct investigations, administer oaths and affirmations, or compel the attendance of witnesses or the production of documentary and other evidence. (d) Definitions.--In this section: (1) Child.--The term ``child'' means an individual that is less than 18 years of age. (2) Firearm.--The term ``firearm'' has the meaning.


High resolution X-ray spectroscopy has revealed soft X-rays from high density plasma in Classical T-Tauri stars (CTTSs), probably arising from the accretion shock region. However, the mass accretion rates derived from the X-ray observations are consistently lower than those derived from UV/optical/NIR studies. We aim to test the hypothesis that the high density soft X-ray emission is from accretion by analysing optical accretion tracers from an X-ray selected sample of CTTSs in a homogeneous manner. We analyse optical spectra of a sample of CTTSs and calculate the accretion rates based on measuring optical emission lines. These are then compared to the accretion rates derived from the X-ray spectroscopy. We find that, for each CTTS in our sample, the different optical tracers predict mass accretion rates that agree within the errors, albeit with a spread of ~1 order of magnitude. Typically, mass accretion rates derived from Halpha and HeI 5876 Ang are larger than those derived from Hbeta, Hgamma and OI. When comparisons of the optical mass accretion rates are made to the X-ray derived mass accretion rates, we find that: a) the latter are always lower (but by varying amounts); b) the latter range within a factor of ~2 around 2x10^{-10} M_odot yr^{-1}, despite the fact that the former span a range of ~3 orders of magnitude. We suggest that the systematic underestimation of the X-ray derived mass accretion rates could depend on the density distribution inside the accretion streams, where the densest part of the stream is not visible in the X-ray band because of the absorption by the stellar atmosphere. We also suggest that a non-negligible optical depth of X-ray emission lines produced by post-shock accreting plasma may explain the almost constant mass accretion rates derived in X-rays.


The government would assess the “direct and upstream greenhouse gas emissions linked to projects.” This requires regulators to engage in an extraordinary amount of guesswork. It ignores the fact that other countries will supply fossil fuels if we choose not to. And it makes an already fraught regulatory climate that much more uncertain. Energy East should not have been subject to criteria not in place when the company filed its application Energy East filed its application with the NEB before these new rules were in effect, so the project shouldn’t have been subject to the new criteria in the first place. But it was. It leaves one to wonder whether the Liberals intended to orchestrate a cancellation of Energy East to avoid the political fallout of approving or rejecting it later on. This is the same government, after all, that used an oil-tanker traffic ban to undermine the Northern Gateway project (which had previously been approved by the Harper government), to curry political favour in some parts of the country, while hurting others. Whether the Liberals knowingly sabotaged Energy East, or are merely oblivious to the importance of maintaining a stable business climate, there is no silver lining here. The damage is not easily undone, and our economy will continue to lose investment, even as Alberta’s oil ships anyway, at greater risk, by rail, and is sold at a discount. Eastern Canadians will continue to import energy from often abhorrent regimes abroad, thousands of potential jobs have been lost, and a grim signal has been sent to global investors about our willingness and ability to get business done. All of this was avoidable. And yet, sadly, none of it is surprising.


Context: The chemical composition of a molecular cloud changes dramatically as it collapses to form a low-mass protostar and circumstellar disk. Two-dimensional (2D) chemodynamical models are required to properly study this process. Aims: The goal of this work is to follow, for the first time, the chemical evolution in two dimensions all the way from a pre-stellar core into a circumstellar disk. Of special interest is the question whether the chemical composition of the disk is a result of chemical processing during the collapse phase, or whether it is determined by in situ processing after the disk has formed. Methods: Our model combines a semi-analytical method to get 2D axisymmetric density and velocity structures with detailed radiative transfer calculations to get temperature profiles and UV fluxes. Material is followed in from the core to the disk and a full gas-phase chemistry network -- including freeze-out onto and evaporation from cold dust grains -- is evolved along these trajectories. The abundances thus obtained are compared to the results from a static disk model and to observations of comets. Results: The chemistry during the collapse phase is dominated by a few key processes, such as the evaporation of CO or the photodissociation of H2O. At the end of the collapse phase, the disk can be divided into zones with different chemical histories. The disk is not in chemical equilibrium at the end of the collapse, so care must be taken when choosing the initial abundances for stand-alone disk chemistry models. Our model results imply that comets must be formed from material with different chemical histories: some of it is strongly processed, some of it remains pristine. Variations between individual comets are possible.


The term `off-highway business use' has the meaning given to such term by section 6421(e)(2); except that such term shall not, for purposes of subsection (a)(1), include use in a diesel-powered train.'' (2) Repeal of reduced rate on ethanol fuel produced from natural gas.-- (A) Paragraph (1) of section 4041(m) of such Code is amended by striking ``or ethanol'' in the material preceding subparagraph (A). (B) Clause (i) of section 4041(m)(1)(A) of such Code is amended by striking ``shall be--'' and all that follows and inserting ``shall be 9.15 cents per gallon, and''. (C) Clause (ii) of section 4041(m)(1)(A) of such Code is amended by striking ``shall be--'' and all that follows and inserting ``shall be 2.15 cents per gallon, and''. (D) Paragraph (2) of section 4041(m) of such Code is amended-- (i) by striking ``or ethanol'' each place it appears in the heading and text, (ii) by striking ``, ethanol,'' and (iii) by inserting ``(other than ethanol)'' after ``alcohol''. (c) Tax of Fuel Alcohol To Same Extent as Other Motor Fuels.-- (1) Treatment as taxable fuel.--Paragraph (1) of section 4083(a) of such Code (defining taxable fuel) is amended by striking ``and'' at the end of subparagraph (B), by striking the period at the end of subparagraph (C) and inserting ``, and'', and by adding at the end the following: ``(D) fuel alcohol.'' (2) Definition of fuel alcohol.--Subsection (a) of section 4083 of such Code is amended by adding at the end the following new paragraph: ``(4) Fuel alcohol.--The term `fuel alcohol' means any alcohol (including ethanol and methanol)-- ``(A) which is produced other than from petroleum, natural gas, or coal (including peat), and ``(B) which is withdrawn from the distillery where produced free of tax under chapter 51 by reason of section 5181 or so much of section 5214(a)(1) as relates to fuel use.'' (3) Rate of


Long linear polymers in strongly disordered media are well described by self-avoiding walks (SAWs) on percolation clusters. The length-distribution of these SAWs encompasses to distinct averages, viz. the averages over cluster- and SAW-conformations. For the latter average, there are two basic options, one being static and one being kinetic. It is well known for static averaging that if the disorder of the underlying medium is weak, differences to the ordered case appear merely in non-universal quantities. Using dynamical field theory, we show that the same holds true for kinetic averaging. For strong disorder, i.e., the medium being close to the percolation point, we employ a field theory for the nonlinear random resistor network in conjunction with a real-world interpretation of Feynman diagrams, and we calculate the scaling exponents for the shortest, the longest and the mean or average SAW to 2-loop order. In addition, we calculate to 2-loop order the entire family of multifractal exponents that governs the moments of the the statistical weights of the elementary constituents (bonds or sites of the underlying fractal cluster) contributing to the SAWs. Our RG analysis reveals that kinetic averaging leads to renormalizability whereas static averaging does not, and hence, we argue that the latter does not lead to a well-defined scaling limit. We discuss the possible implications of this finding for experiments and numerical simulations which have produced wide-spread results for the exponent of the average SAW. To corroborate our results, we also study the well-known Meir-Harris model for SAWs on percolation clusters. We demonstrate that this model leads back to 2-loop order to the renormalizable real world formulation with kinetic averaging.


Several authors have found a statistically significant excess of galaxies with higher redshifts relative to the group centre, so-called discordant redshifts, in particular in groups where the brightest galaxy, identified in apparent magnitudes, is a spiral. Our aim is to explain the observed redshift excess. We use a semi-analytical galaxy catalogue constructed from the Millennium Simulation to study redshift asymmetries in spiral-dominated groups in the Lambda cold dark matter (LambdaCDM) cosmology. We show that discordant redshifts in small galaxy groups arise when these groups are gravitationally unbound and the dominant galaxy of the group is misidentified. The redshift excess is especially significant when the apparently brightest galaxy can be identified as a spiral, in full agreement with observations. On the other hand, the groups that are gravitationally bound do not show a significant redshift asymmetry. When the dominant members of groups in mock catalogues are identified by using the absolute B-band magnitudes, our results show a small blueshift excess. This result is due to the magnitude limited observations that miss the faint background galaxies in groups. When the group centre is not correctly identified it may cause the major part of the observed redshift excess. If the group is also gravitationally unbound, the level of the redshift excess becomes as high as in observations. There is no need to introduce any "anomalous" redshift mechanism to explain the observed redshift excess. Further, as the Friends-of-Friends percolation algorithm picks out the expanding parts of groups, in addition to the gravitationally bound group cores, group catalogues constructed in this way cannot be used as.


An edge-coloring of a graph $G$ with colors $1,...,t$ is an interval $t$-coloring if all colors are used, and the colors of edges incident to each vertex of $G$ are distinct and form an interval of integers. A graph $G$ is interval colorable if $G$ has an interval $t$-coloring for some positive integer $t$. Let $\mathfrak{N}$ be the set of all interval colorable graphs. For a graph $G\in \mathfrak{N}$, the least and the greatest values of $t$ for which $G$ has an interval $t$-coloring are denoted by $w(G)$ and $W(G)$, respectively. In this paper we first show that if $G$ is an $r$-regular graph and $G\in \mathfrak{N}$, then $W(G\square P_{m})\geq W(G)+W(P_{m})+(m-1)r$ ($m\in \mathbb{N}$) and $W(G\square C_{2n})\geq W(G)+W(C_{2n})+nr$ ($n\geq 2$). Next, we investigate interval edge-colorings of grids, cylinders and tori. In particular, we prove that if $G\square H$ is planar and both factors have at least 3 vertices, then $G\square H\in \mathfrak{N}$ and $w(G\square H)\leq 6$. Finally, we confirm the first author's conjecture on the $n$-dimensional cube $Q_{n}$ and show that $Q_{n}$ has an interval $t$-coloring.


The effect of disorder on pinning and wetting models has attracted much attention in theoretical physics. In particular, it has been predicted on the basis of the Harris criterion that disorder is relevant (annealed and quenched model have different critical points and critical exponents) if the return probability exponent alpha, a positive number that characterizes the model, is larger than 1/2. Weak disorder has been predicted to be irrelevant (i.e. coinciding critical points and exponents) if alpha < 1/2. Recent mathematical work has put these predictions on firm grounds. In renormalization group terms, the case alpha = 1/2 is a 'marginal case' and there is no agreement in the literature as to whether one should expect disorder relevance or irrelevance at marginality. The question is particularly intriguing also because the case alpha = 1/2 includes the classical models of two-dimensional wetting of a rough substrate, of pinning of directed polymers on a defect line in dimension (3+1) or (1+1) and of pinning of an heteropolymer by a point potential in three-dimensional space. Here we prove disorder relevance both for the general alpha = 1/2 pinning model and for the hierarchical version of the model proposed by B. Derrida, V. Hakim and J. Vannimenus (JSP, 1992), in the sense that we prove a shift of the quenched critical point with respect to the annealed one. In both cases we work with Gaussian disorder and we show that the shift is at least of order exp(-1/\beta^4) for beta small.


Iii) as clauses (iii) and (iv); and (3) by inserting after clause (i) the following new clause: ``(ii) The amount determined under this clause is-- ``(I) for discharges occurring during the first 3 12-month cost reporting periods that begin on or after April 1, 1990, the amount by which the hospital's target amount for the cost reporting period (as defined in subsection (b)(3)(D)) exceeds the amount determined under paragraph (1)(A)(iii); and ``(II) for discharges occurring during any subsequent cost reporting period (or portion thereof), 50 percent of the amount by which the hospital's target amount for the cost reporting period (as defined in subsection (b)(3)(D)) exceeds the amount determined under paragraph (1)(A)(iii).''. (b) Permitting Hospitals to Decline Reclassification.--If any hospital fails to qualify as a medicare-dependent, small rural hospital under section 1886(d)(5)(G)(i) of the Social Security Act as a result of a decision by the Medicare Geographic Classification Review Board under section 1886(d)(10) of such Act to reclassify the hospital as being located in an urban area for fiscal year 1994, the Secretary of Health and Human Services shall-- (1) notify such hospital of such failure to qualify, (2) provide an opportunity for such hospital to decline such reclassification, and (3) if the hospital declines such reclassification, administer the Social Security Act (other than section 1886(d)(8)(D)) for fiscal year 1994 as.


Using Hubble Space Telescope (HST) photometry, we characterize the age of the stellar association in the vicinity of supernova (SN) 2011dh and use it to infer the zero-age main sequence mass (M_{ZAMS}) of the progenitor star. We find two distinct and significant star formation events with ages of <6 and 17^{+3}_{-4} Myrs, and the corresponding M_{ZAMS} are >29 and 13^{+2}_{-1} M_{Sun}, respectively. These two bursts represent 18^{+4}_{-9}% (young) and 64^{+10}_{-14}% (old) of the total star formation in the last 50 Myrs. Adopting these fractions as probabilities suggests that the most probable M_{ZAMS} is 13^{+2}_{-1} M_{Sun}. These results are most sensitive to the luminosity function along the well-understood main sequence and are less sensitive to uncertain late-stage stellar evolution. Therefore, they stand even if the progenitor suffered disruptive post-main-sequence evolution (e.g. eruptive mass loss or binary Roche-lobe overflow). Progenitor identification will help to further constrain the appropriate population. Even though pre-explosion images show a yellow supergiant (YSG) at the site of the SN, panchromatic SN light curves suggest a more compact star as the progenitor. In spite of this, our results suggest an association between the YSG and the SN. Not only was the star located at the SN site, but reinforcing an association, the star's bolometric luminosity is consistent with the final evolutionary stage of the 17 Myr old star burst. If the YSG disappears, then M_{ZAMS}=13^{+2}_{-1} M_{Sun}, but.