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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


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


The Secretary shall issue an order requiring implementation of such plan by the covered air carriers who submitted such plan and any other covered air carriers. If there are any covered air carriers who did not participate in development of a plan approved under this section, such carriers shall be treated under such order and plan in the same manner as carriers who did participate in development of such plan. ``(d) Regulations.--If a plan described in subsection (a) is not submitted within 180 days after the date of the enactment of this section, or if the Secretary disapproves a plan submitted in accordance with subsection (a), or if the Secretary determines that a plan approved under this section is not being implemented in a manner which provides satisfactory protection for all persons who hold airline tickets described in subsection (a), the Secretary shall issue regulations requiring all covered air carriers to provide air transportation for persons who hold such tickets. Such regulations must be issued within 90 days after the expiration of such 180-day period, the date of disapproval of such plan, or the date of such determination, as the case may be. ``(e) Definitions.--For purposes of this section-- ``(1) Airline ticket.--The term `airline ticket' means any written instrument that embodies a contract of carriage between a covered air carrier and a passenger thereof for interstate or overseas air transportation. ``(2) Covered air carrier.--The term `covered air carrier' means-- ``(A) an air carrier which provides interstate or overseas air transportation primarily with aircraft having seating for more than 60 passengers and which in the 12-month period preceding the date of the enactment of this section, enplaned more than.2 percent of the total number of passengers enplaned on all aircraft used to provide interstate and overseas air transportation in such period; and ``(B) an air carrier not described in subparagraph (A) who enters into an agreement with an air carrier who is described in subparagraph (A) to operate under or use a single air carrier designator code to provide interstate or overseas air transportation, but only with respect to those operations of the carrier not described in subparagraph (A) which are carried out under such code. ``(3) Secretary.--The term `Secretary' means the Secretary of Transportation.''. (b) Conforming Amendment to Table of Contents.--The table of contents in the first section of the Federal Aviation Act of 1958 is amended by adding at the end of the


In the United States. ``(5) Carryback and carryforward allowed.-- ``(A) In general.--If the credit allowable under subsection (a) for a taxable year exceeds the amount of the limitation under subsection (f)(1) for such taxable year (in this paragraph referred to as the `unused credit year'), such excess shall be a credit carryback to each of the 3 taxable years preceding the unused credit year and a credit carryforward to each of the 20 taxable years following the unused credit year. ``(B) Rules.--Rules similar to the rules of section 39 shall apply with respect to the credit carryback and credit carryforward under subparagraph (A). ``(6) Certain rules to apply.--Rules similar to the rules of subsections (c), (d), and (e) of section 52 shall apply.''. (b) Conforming Amendment.--Section 55(c)(2) of the Internal Revenue Code of 1986 is amended by inserting ``30B(f)(1),'' after ``30(b)(3),''. (c) Clerical Amendment.--The table of sections for subpart B of part IV of subchapter A of chapter 1 of the Internal Revenue Code of 1986 is amended by adding at the end of 30A the following new item: ``Sec. 30B. Employer wage credit for activated military reservists''. (d) Effective Date; Special Rule.-- (1) Effective date.--The amendments made by this section shall apply to amounts paid after September 11, 2001, in taxable years ending after such date. (2) Waiver of limitations.--If refund or credit of any overpayment of tax resulting from the amendments made by this section is prevented at any time before the close of the 1-year period beginning on the date of the enactment of this Act by the operation of any law or rule of law (including res judicata), such refund or credit may nevertheless be made or allowed.


(Abridged) Recent results from the Pierre Auger Observatory (PAO) indicate that the composition of ultra-high-energy cosmic rays (UHECRs) with energies above $10^{19}$ eV may be dominated by heavy nuclei. An important question is whether the distribution of arrival directions for such UHECR nuclei can exhibit observable anisotropy or positional correlations with their astrophysical source objects despite the expected strong deflections by intervening magnetic fields. For this purpose, we have simulated the propagation of UHECR nuclei including models for both the extragalactic magnetic field and the Galactic magnetic field. Assuming that only iron nuclei are injected steadily from sources with equal luminosity and spatially distributed according to the observed large scale structure in the local Universe, at the number of events published by the PAO so far, the arrival distribution of UHECRs would be consistent with no auto-correlation at 95% confidence if the mean number density of UHECR sources $n_s >~ 10^{-6}$ Mpc$^{-3}$, and consistent with no cross-correlation with sources within 95% errors for $n_s >~ 10^{-5}$ Mpc$^{-3}$. On the other hand, with 1000 events above $5.5 \times 10^{19}$ eV in the whole sky, next generation experiments can reveal auto-correlation with more than 99% probability even for $n_s <~ 10^{-3}$ Mpc$^{-3}$, and cross-correlation with sources with more than 99% probability for $n_s <~ 10^{-4}$ Mpc$^{-3}$. In addition, we find that the contribution of Centaurus A is required to reproduce the currently observed UHECR excess in the Centaurus region. Secondary protons generated by photodisintegration of primary heavy nuclei during propagation play a crucial role in all cases, and the resulting anisotropy at small angular scales should provide a strong hint of the source location.


That team would be wearing green and white. “I think he’d be a fantastic fit with the Jets,” said Mora, the former UCLA coach who has served as an analyst for the NFL Network on its “Path to the Draft” program. “Josh is kind of ready to go. You give him the keys to the offense, teach it to him, and then he’s going to master it pretty quickly. He’s that type of kid. I think he’d be a tremendous fit with that coaching staff, with that city. I think it would be a great spot for him.” Mora will be tuning in to NFL Network on Thursday to see where Rosen winds up. Rosen is considered one of the top quarterbacks in this draft, but has not really been linked to the Browns or Giants (who own the top two picks) in any of the recent mock drafts. The Jets are a different story. There are people inside the Jets’ organization who like Rosen a lot. Some people around the NFL believe the Jets are debating whether to take Rosen or Oklahoma’s Baker Mayfield with the No. 3 pick. Rosen blew away members of the Jets’ coaching staff with his intelligence. He is viewed by many experts as the most ready quarterback to play immediately. “I’m hoping that’s where he ends up,” Mora said. “I’m hoping he ends up with the Giants or the Jets. I want to see him go as high as possible, but I think the Jets would be a great place for him.” Mora said he believes Rosen is cut out for being a quarterback in New York. When he said this a month ago and said Sam Darnold was a better fit for Cleveland, it caused a stir. But Mora said he did not mean that as a negative. He just believes New York fits Rosen. “He’s incredibly smart,” Mora said. “He can handle a lot of volume. He can handle being the quarterback of an NFL team in New York City with that type of scrutiny. He can handle the workload that comes with being a quarterback in the NFL. He’s been here in Los Angeles. I don’t know which one is the larger media market, but they’re both certainly very big and very prominent. He’s been under the microscope for a long time. He’s been highly scrutinized since high school


This paper reports Very Large Array observations at 325 and 1425 MHz (90cm and 20cm) during and near the periastron passage of HD 80606b on 2007 November 20. We obtain flux density limits (3-sigma) of 1.7 mJy and 48 microJy at 325 and 1425 MHz, respectively, equivalent to planetary luminosity limits of 2.3 x 10^{24} erg/s and 2.7 x 10^{23} erg/s. These are well above the Jovian value (at 40 MHz) of 2 x 10^{18} erg/s. The motivation for these observations was that the planetary magnetospheric emission is driven by a stellar wind-planetary magnetosphere interaction so that the planetary luminosity would be elevated. Near periastron, HD 80606b might be as much as 3000 times more luminous than Jupiter. Recent transit observations of HD 80606b provide stringent constraints on the planetary mass and radius, and, because of the planet's highly eccentric orbit, its rotation period is likely to be "pseudo-synchronized" to its orbital period, allowing a robust estimate of the former. We are able to make robust estimates of the emission frequency of the planetary magnetospheric emission and find it to be around 60--90 MHz. We compare HD 80606b to other high-eccentricity systems and assess the detection possibilities for both near-term and more distant future systems. Of the known high eccentricity planets, only HD 80606b is likely to be detectable, as HD 20782B b and HD 4113b are both likely to have weaker magnetic field strengths. Both the forthcoming "EVLA low band" system and the Low Frequency Array may be able to improve upon our limits for HD 80606b, and do so at a more optimum frequency. If the low-frequency component of the Square Kilometre Array (SKA-lo) and a future lunar radio array are able to approach their thermal noise limits, they should be able to detect an HD 80606b-like planet.


This paper discusses the approximation by %semigroups of operators of class ($\mathscr{C}_0$) on the sphere and focuses on a class of so called exponential-type multiplier operators. It is proved that such operators form a strongly continuous semigroup of contraction operators of class ($\mathscr{C}_0$), from which the equivalence between approximation for these operators and $K$-functionals introduced by the operators is given. As examples, the constructed $r$-th Boolean of generalized spherical Abel-Poisson operator and $r$-th Boolean of generalized spherical Weierstrass operator denoted by $\oplus^r V_t^{\gamma}$ and $\oplus^r W_t^{\kappa}$ separately ($r$ is any positive integer, $0<\gamma,\kappa\leq1$ and $t>0$) satisfy that $\|\oplus^r V_t^{\gamma}f - f\|_{\mathcal{X}}\approx \omega^{r\gamma}(f,t^{1/\gamma})_{\mathcal{X}}$ and $\|\oplus^r W_t^{\kappa}f - f\|_{\mathcal{X}}\approx \omega^{2r\gamma}(f,t^{1/(2\kappa)})_{\mathcal{X}}$, for all $f\in \mathcal{X}$, where $\mathcal{X}$ is a Banach space of continuous functions or $\mathcal{L}^p$-integrable functions ($1\leq p<\infty$) and $\|\cdot\|_{\mathcal{X}}$ is the norm on $\mathcal{X}$ and $\omega^s(f,t)_{\mathcal{X}}$ is the moduli of smoothness of degree $s>0$ for $f\in \mathcal{X}$. The saturation order and saturation class of the regular exponential-type multiplier operators with positive kernels are also obtained. Moreover, it is proved that $\oplus^r V_t^{\gamma}$ and $\oplus^r W_t^{\kappa}$ have the same saturation class.


Symmetry-protected topological (SPT) phases are gapped short-range-entangled quantum phases with a symmetry $G$, which can all be smoothly connected to the trivial product states if we break the symmetry. It has been shown that a large class of interacting bosonic SPT phases can be systematically described by group cohomology theory. In this paper, we introduce a (special) group supercohomology theory which is a generalization of the standard group cohomology theory. We show that a large class of short-range interacting fermionic SPT phases can be described by the group supercohomology theory. Using the data of super cocycles, we can obtain the ideal ground state wave function for the corresponding fermionic SPT phase. We can also obtain the bulk Hamiltonian that realizes the SPT phase, as well as the anomalous (ie, non-on-site) symmetry for the boundary effective Hamiltonian. The anomalous symmetry on the boundary implies that the symmetric} boundary must be gapless for 1+1D boundary, and must be gapless or topologically ordered beyond 1+1D. As an application of this general result, we construct a new SPT phase in 3D, for interacting fermionic superconductors with coplanar spin order (which have $T^2=1$ time-reversal $Z_2^T$ and fermion-number parity $Z_2^f$ symmetries described by a full symmetry group $Z_2^T\times Z_2^f$). Such a fermionic SPT state can neither be realized by free fermions nor by interacting bosons (formed by fermion-pairs), and thus are not included in the K-theory classification for free fermions or group cohomology description for interacting bosons. We also construct three interacting fermionic SPT phases in 2D with a full symmetry group $Z_2\times Z_2^f$. Those 2D fermionic SPT phases all have central-charge $c=1$ gapless edge excitations.


We present the first results of a program to characterize the disk and envelope structure of typical Class 0 protostars in nearby low-mass star forming regions. We use Spitzer IRS mid-infrared spectra, high resolution CARMA 230 GHz continuum imaging, and 2-D radiative transfer models to constrain the envelope structure, as well as the size and mass of the circum-protostellar disk in Serpens FIRS 1. The primary envelope parameters (centrifugal radius, outer radius, outflow opening angle, and inclination) are well constrained by the spectral energy distribution (SED), including Spitzer IRAC and MIPS photometry, IRS spectra, and 1.1 mm Bolocam photometry. These together with the excellent uv-coverage (4.5-500 klam) of multiple antenna configurations with CARMA allow for a robust separation of the envelope and a resolved disk. The SED of Serpens FIRS 1 is best fit by an envelope with the density profile of a rotating, collapsing spheroid with an inner (centrifugal) radius of approximately 600 AU, and the millimeter data by a large resolved disk with Mdisk~1.0 Msun and Rdisk~300 AU. These results suggest that large, massive disks can be present early in the main accretion phase. Results for the larger, unbiased sample of Class~0 sources in the Perseus, Serpens, and Ophiuchus molecular clouds are needed to determine.


We present deep Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) optical observations obtained as part of the ACS Nearby Galaxy Survey Treasury (ANGST) as well as early release Wide Field Camera 3 (WFC3) ultra-violet and infrared observations of the nearby dwarf starbursting galaxy NGC 4214. Our data provide a detailed example of how covering such a broad range in wavelength provides a powerful tool for constraining the physical properties of stellar populations. The deepest data reach the ancient red clump at M_F814W -0.2. All of the optical data reach the main sequence turnoff for stars younger than ~300 Myr, and the blue He burning sequence for stars younger than 500 Myr. The full CMD-fitting analysis shows that all three fields in our data set are consistent with ~75% of the stellar mass being older than 8 Gyr, in spite of showing a wide range in star formation rates at the present day. Thus, our results suggest that the scale length of NGC 4214 has remained relatively constant for many Gyr. As previously noted by others, we also find the galaxy has recently ramped up production, consistent with its bright UV luminosity and its population of UV-bright massive stars. In the central field we find UV point sources with F336W magnitudes as bright as -9.9. These are as bright as stars with masses of at least 52-56 M_sun and ages near 4 Myr in stellar evolution models. Assuming a standard IMF, our CMD is well-fitted by an increase in star formation rate beginning 100 Myr ago. The stellar populations of this late-type dwarf are compared with those of NGC 404, an early-type dwarf that is also the most massive galaxy in its local environment. The late-type dwarf appears to have a similar high fraction of ancient stars, suggesting that these dominant galaxies may form at early epochs even.


A new type of neutrino mixing named bi-pair neutrino mixing is proposed to describe the current neutrino mixing pattern with a vanishing reactor mixing angle and is determined by a mixing matrix with two pairs of identical magnitudes of matrix elements. As a result, we predict \sin^2\theta_{12}=1-1/\sqrt{2}(\approx 0.293) for the solar neutrino mixing and either \sin^2\theta_{23}=\tan^2\theta_{12} or \cos^2\theta_{23}=\tan^2\theta_{12} for the atmospheric neutrino mixing. We determine flavor structure of a mass matrix M, leading to diagonal masses of m_{1,2,3}, and find that |M_{\mu\mu}-M_{ee}/t^2_{12}|:|M_{\mu \tau}|:|M_{\tau \tau}-M_{ee}/t^2_{12}|=t^2_{23}:|t_{23}|:1 for the normal mass hierarchy if m_1=0, where t_{ij}=\tan\theta_{ij} (i,j=1,2,3) and M_{ij} (i,j=e,\mu,\tau) stand for flavor neutrino masses. For the inverted mass hierarchy, the bi-pair mixing scheme turns out to satisfy the strong scaling ansatz requiring that |M_{\mu\mu}|:|M_{\mu\tau}|:|M_{\tau\tau}|=1:|t_{23}|:t^2_{23}.


Motorcycle in front of the office and moved to the Olomowewe area in Adiyan, where they burnt three motorcycles parked by the roadside. There was confusion everywhere. “Through the intervention of the police, the situation was brought under control on Sunday evening. Policemen have been patrolling the community.” Another resident, who did not want his name in print, said there might have been a disagreement between Olatunbosun and the vigilantes prior to the incident. “Those that killed him must be brought to book. I don’t think they beat him because he stole the dryer or not. “They probably had a disagreement with him before now and they decided to deal with him. They beat him with charms and later took him to the station,” he said. PUNCH Metro learnt that the two vigilantes were later arrested by the Agbado division. A police source said the hairdryer purportedly recovered from Olatunbosun was taken to the station. “By the time the vigilantes brought him to the station with the dryer, he had been seriously injured. “He was released to go and treat himself, but he died in the hospital,” the source added. The Ogun State Police Public Relations Officer, ASP Abimbola Oyeyemi, said the suspects were being investigated for murder and would be charged to court afterwards. “The two vigilantes in question are in custody. The Commissioner of Police, Ahmed Iliyasu, has ordered that they should be transferred to the Homicide Section of the State Criminal Investigation and Intelligence Department for proper investigation. Even.


The ISM evolution of elliptical galaxies experiencing feedback from accretion onto a central black hole was studied recently with high-resolution 1D hydrodynamical simulations including radiative heating and pressure effects, a RIAF-like radiative efficiency, mechanical input from AGN winds, and accretion-driven starbursts. Here we focus on the observational properties of the models in the X-ray band (nuclear luminosity; hot ISM luminosity and temperature; temperature and brightness profiles during quiescence and during outbursts). The nuclear bursts last for ~10^7 yr, with a duty-cycle of a few X (10^-3-10^-2); the present epoch bolometric nuclear emission is very sub-Eddington. The ISM thermal luminosity \lx oscillates in phase with the nuclear one; this helps reproduce statistically the observed large \lx variation. In quiescence the temperature profile has a negative gradient; thanks to past outbursts, the brightness profile lacks the steep shape typical of inflowing models. Outbursts produce disturbances in these profiles. Most significantly, a hot bubble from shocked hot gas is inflated at the galaxy center; the bubble would be conical in shape, and show radio emission. The ISM resumes a smooth appearance on a time-scale of ~200 Myr; the duty-cycle of perturbances in the ISM is of the order of 5-10%. From the present analysis, additional input physics is important in the ISM-black hole coevolution, to fully account for the properties of real galaxies, as a confining external medium and a jet. The jet will reduce further the mass available for accretion (and then the Eddington ratio $l$), and may help, together with an external pressure, to produce flat or positive temperature gradient profiles (observed in high density environments). Alternatively, $l$ can be reduced.