A FDR-preserving field theory for interacting Brownian particles: one-loop theory and MCT

We develop a field theoretical treatment of a model of interacting Brownian particles. We pay particular attention to the requirement of the time reversal invariance and the fluctuation-dissipation relationship (FDR). The method used is a modified version of the auxiliary field method due originally to Andreanov, Biroli and Lefevre [J. Stat. Mech. P07008 (2006)]. We recover the correct diffusion law when the interaction is dropped as well as the standard mode coupling equation in the one-loop order calculation for interacting Brownian particle systems.Comment: 66 pages, 8 figures, submitted to J. Stat. Mec

Inclusion and Equity Committee Diverse Recruitment Task Force 1 “Literature Review”

Engage in a literature review of current recruitment of underrepresented groups and from the literature review, recommend a series of policies that encapsulate best practices for use at the UNLV Libraries

Elemental Abundances in the X-Ray Gas of Early-Type Galaxies with XMM and Chandra Observations

The source of hot gas in elliptical galaxies is thought to be due to stellar mass loss, with contributions from supernova events and possibly from infall from a surrounding environment. This picture predicts supersolar values for the metallicity of the gas toward the inner part of the galaxy, which can be tested by measuring the gas phase abundances. We use high-quality data for 10 nearby early-type galaxy from XMM-Newton, featuring both the EPIC and the Reflection Grating Spectrometer, where the strongest emission lines are detected with little blending; some Chandra data are also used. We find excellent consistency in the elemental abundances between the different XMM instruments and good consistency with Chandra. Differences in abundances with aperture size and model complexity are examined, but large differences rarely occur. For a two-temperature thermal model plus a point source contribution, the median Fe and O abundances are 0.86 and 0.44 of the Solar value, while Si and Mg abundances are similar to that for Fe. This is similar to stellar abundances for these galaxies but supernovae were expected to enhance the gas phase abundances considerably, which is not observed.Comment: 35 pages, 10 figures, accepted for publication in Astrophysical Journa

Learning from Las Vegas: Adapting Workflows for Managing Born-Digital Design Records

Architecture collections have been a mainstay for Special Collections and Archives at the University of Nevada, Las Vegas (UNLV SCA), since the late 1970s. Until 2017, most architecture collections in Special Collections and Archives have consisted of physical records. In recent years, curators began acquiring architecture collections with significant born-digital content, which present unique challenges different from other types of born-digital materials. This case study discusses how staff adapted existing workflows for born-digital materials to process and describe two collections comprised of born-digital architecture and design records. The authors also describe how UNLV SCA provides access to proprietary design files through the creation of access surrogates. Lessons learned from adapting workflows and processing these collections are detailed, as well as future steps for continuing the development of workflows and policies for managing born-digital architecture and design records

Draft Genome Sequence of the Lignocellulose Decomposer Thermobifida fusca Strain TM51.

Here, we present the complete genome sequence of Thermobifida fusca strain TM51, which was isolated from the hot upper layer of a compost pile in Hungary. T. fusca TM51 is a thermotolerant, aerobic actinomycete with outstanding lignocellulose-decomposing activity

Metallicity Effect on LMXB Formation in Globular Clusters

We present comprehensive observational results of the metallicity effect on the fraction of globular clusters (GC) that contain low-mass X-ray binaries (LMXB), by utilizing all available data obtained with Chandra for LMXBs and HST ACS for GCs. Our primary sample consists of old elliptical galaxies selected from the ACS Virgo and Fornax surveys. To improve statistics at both the lowest and highest X-ray luminosity, we also use previously reported results from other galaxies. It is well known that the LMXB fraction is considerably higher in red, metal-rich, than in blue, metal-poor GCs. In this paper, we test whether this metallicity effect is X-ray luminosity-dependent, and find that the effect holds uniformly in a wide luminosity range. This result is statistically significant (at >= 3 sigma) in LMXBs with luminosities in the range LX = 2 x 10^37 - 5 x 10^38 erg s-1, where the ratio of LMXB fractions in metal-rich to metal-poor GCs is R = 3.4 +- 0.5. A similar ratio is also found at lower (down to 10^36 erg s-1) and higher luminosities (up to the ULX regime), but with less significance (~2 sigma confidence). Because different types of LMXBs dominate in different luminosities, our finding requires a new explanation for the metallicity effect in dynamically formed LMXBs. We confirm that the metallicity effect is not affected by other factors such as stellar age, GC mass, stellar encounter rate, and galacto-centric distance.Comment: 21 pages, 5 figures, accepted in Ap

Uzbuda niskoležećeg izomernog stanja u 229Th

Gamma-ray spectroscopy measurements have revealed the presence of an isomeric excited state in 229Th only (3.5 ± 1.0) eV above the ground state, and recent measurements with a high resolution detector have resulted in the value of (7.6 ± 0.5) eV. The state is of interest due to the unique atomic-nuclear interactions which should govern its decay. The state is also of interest as excitation of the level allows the study of processes important in the development of gamma-ray lasers. Although a small number of experiments have been done in an attempt to observe the de-excitation of the isomeric level populated following alpha decay of 233U, the results remain controversial and inconclusive, mainly due to ambiguities in samples used by various researchers. To date no attempts have been made to excite the lowlying level from the ground state of 229Th, nor has there been a systematic study of 233U in various sample forms with suitable uranium control isotopes to look for evidence of the decay of the low-lying level consistent with theoretical predictions. We present a comparison of some possible excitation techniques, including the resonant (M¨ossbauer effect) and non-resonant (broadband) methods, and propose some possible experiments.Spektroskopska mjerenja gama zračenja otkrila su izomerno uzbudno stanje u 229Th samo (3.5±1.0) eV povrh osnovnog stanja, a novija mjerenja s detektorom visokog razlučivanja dala su iznos od (7.6±0.5) eV. Zanimanje za ovo stanje je zbog mogućeg jedinstvenog međudjelovanja atom-jezgra koje upravlja njegovim raspadom. To je stanje zanimljivo i zbog mogućnosti proučavanja procesa koji su važni za razvoj lasera gama zračenja. Iako je načinjen malen broj pokušaja da se opazi raspad tog izomernog stanja koje se popunjava alfa raspadom 233U, ishodi su nesuglasni i nisu zaključni, najviše zbog neodređenosti u sastavu uzoraka koje su razni istraživači rabili. Do sada se nije pokušalo uzbuditi to niskoležeće stanje polazeći od osnovnog stanja 229Th, niti je načinjeno sustavno proučavanje s uzorcima 233U u različitim spojevima, i s odgovarajućim uranovim izotopima za provjere, da bi se dobili podaci o raspadu o tom niskoležećem stanju radi usporedbe s teorijskim predviđanjima. Opisujemo usporedbe nekih mogućih metoda za uzbudu, uključujući rezonantnu (Mössbauerov efekt) i nerezonantne (širokopojasne) metode, te predlažemo neke moguće eksperimente

Uzbuda niskoležećeg izomernog stanja u 229Th

Gamma-ray spectroscopy measurements have revealed the presence of an isomeric excited state in 229Th only (3.5 ± 1.0) eV above the ground state, and recent measurements with a high resolution detector have resulted in the value of (7.6 ± 0.5) eV. The state is of interest due to the unique atomic-nuclear interactions which should govern its decay. The state is also of interest as excitation of the level allows the study of processes important in the development of gamma-ray lasers. Although a small number of experiments have been done in an attempt to observe the de-excitation of the isomeric level populated following alpha decay of 233U, the results remain controversial and inconclusive, mainly due to ambiguities in samples used by various researchers. To date no attempts have been made to excite the lowlying level from the ground state of 229Th, nor has there been a systematic study of 233U in various sample forms with suitable uranium control isotopes to look for evidence of the decay of the low-lying level consistent with theoretical predictions. We present a comparison of some possible excitation techniques, including the resonant (M¨ossbauer effect) and non-resonant (broadband) methods, and propose some possible experiments.Spektroskopska mjerenja gama zračenja otkrila su izomerno uzbudno stanje u 229Th samo (3.5±1.0) eV povrh osnovnog stanja, a novija mjerenja s detektorom visokog razlučivanja dala su iznos od (7.6±0.5) eV. Zanimanje za ovo stanje je zbog mogućeg jedinstvenog međudjelovanja atom-jezgra koje upravlja njegovim raspadom. To je stanje zanimljivo i zbog mogućnosti proučavanja procesa koji su važni za razvoj lasera gama zračenja. Iako je načinjen malen broj pokušaja da se opazi raspad tog izomernog stanja koje se popunjava alfa raspadom 233U, ishodi su nesuglasni i nisu zaključni, najviše zbog neodređenosti u sastavu uzoraka koje su razni istraživači rabili. Do sada se nije pokušalo uzbuditi to niskoležeće stanje polazeći od osnovnog stanja 229Th, niti je načinjeno sustavno proučavanje s uzorcima 233U u različitim spojevima, i s odgovarajućim uranovim izotopima za provjere, da bi se dobili podaci o raspadu o tom niskoležećem stanju radi usporedbe s teorijskim predviđanjima. Opisujemo usporedbe nekih mogućih metoda za uzbudu, uključujući rezonantnu (Mössbauerov efekt) i nerezonantne (širokopojasne) metode, te predlažemo neke moguće eksperimente

X-ray Properties of Young Early Type Galaxies: II. Abundance Ratio in the Hot ISM

Using Chandra X-ray observations of young, post-merger elliptical galaxies, we present X-ray characteristics of age-related observational results, by comparing with typical old elliptical galaxies in terms of metal abundances in the hot interstellar matter (ISM). While the absolute element abundances may be uncertain because of unknown systematic errors and partly because of the smaller amount of hot gas in young ellipticals, the relative abundance ratios (e.g., the alpha-element to Fe ratio, most importantly Si/Fe ratio) can be relatively well constrained. We find that in two young elliptical galaxies (NGC 720 and NGC 3923) the Si to Fe abundance ratio is super-solar (at a 99% significance level), in contrast to typical old elliptical galaxies where the Si to Fe abundance ratio is close to solar. Also the O/Mg ratio is close to solar in the two young elliptical galaxies, as opposed to the sub-solar O/Mg ratio reported in old elliptical galaxies. Both features appear to be less significant outside the effective radius (roughly 30" for the galaxies under study), consistent with the observations that confine to the centermost regions the signatures of recent star formation in elliptical galaxies. Observed differences between young and old elliptical galaxies can be explained by the additional contribution from SNe II ejecta in the former. In young elliptical galaxies, the later star formation associated with recent mergers would have a dual effect, resulting both in galaxy scale winds - and therefore smaller observed amounts of hot ISM - because of the additional SNII heating, and in different metal abundances, because of the additional SNII yields.Comment: 21 pages, 4 color figures, ApJ in press, minor revisions for referee's comments, a new figure adde