Miracle-dz/UniFAR-FTUs huggingface dataset:
THE ASSEMBLY HISTORIES OF QUIESCENT GALAXIES SINCE z = 0.7 FROM ABSORPTION LINE SPECTROSCOPY

We present results from modeling the optical spectra of a large sample of quiescent galaxies between 0.1 < z < 0.7 from the Sloan Digital Sky Survey (SDSS) and the AGN and Galaxy Evolution Survey (AGES). We examine how the stellar ages and abundance patterns of galaxies evolve over time as a function of stellar mass from 109.6–1011.8 M☉. Galaxy spectra are stacked in bins of mass and redshift and modeled over a wavelength range from 4000 Å to 5500 Å. Full spectrum stellar population synthesis modeling provides estimates of the age and the abundances of the elements Fe, Mg, C, N, and Ca. We find negligible evolution in elemental abundances at fixed stellar mass over roughly 7 Gyr of cosmic time. In addition, the increase in stellar ages with time for massive galaxies is consistent with passive evolution since z = 0.7. Taken together, these results favor a scenario in which the inner ∼0.3–3 Re of massive quiescent galaxies have been passively evolving over the last half of cosmic time. Interestingly, the derived stellar ages are considerably younger than the age of the universe at all epochs, consistent with an equivalent single-burst star formation epoch of z ≲ 1.5. These young stellar population ages coupled with the existence of massive quiescent galaxies at z > 1 indicate the inhomogeneous nature of the z ≲ 0.7 quiescent population. The data also permit the addition of newly quenched galaxies at masses below ∼1010.5 M☉ at z < 0.7. Additionally, we analyze very deep Keck DEIMOS spectra of the two brightest quiescent galaxies in a cluster at z = 0.83. There is tentative evidence that these galaxies are older than their counterparts in low-density environments. In the Appendix, we demonstrate that our full spectrum modeling technique allows for accurate and reliable modeling of galaxy spectra to low S/N (∼20 Å−1) and/or low spectral resolution (R ∼ 500).
Cosmic ray acceleration in young supernova remnants

We investigate the appearance of magnetic field amplification resulting from a cosmic ray escape current in the context of supernova remnant shock waves. The current is inversely proportional to the maximum energy of cosmic rays, and is a strong function of the shock velocity. Depending on the evolution of the shock wave, which is drastically different for different circumstellar environments, the maximum energy of cosmic rays as required to generate enough current to trigger the non-resonant hybrid instability that confines the cosmic rays follows a different evolution and reaches different values. We find that the best candidates to accelerate cosmic rays to ~few PeV energies are young remnants in a dense environment, such as a red supergiant wind, as may be applicable to Cassiopeia A. We also find that for a typical background magnetic field strength of 5 microG the instability is quenched in about 1000 years, making SN1006 just at the border of candidates for cosmic ray acceleration to high energies.
Prospective Association of Circulating Adipokines with Cardiometabolic Risk Profile Among Women: The Rape Impact Cohort Evaluation Study

Background: Sexual violence is associated with poor cardiometabolic outcomes, yet the etiopathogenic pathways remain unclear. Adipokines may contribute to pathways in the development of cardiometabolic disease (CMD), including in vulnerable populations. Further investigation of adipokines among sexually traumatized individuals may inform cardiometabolic screening. This study aimed to investigate the association between circulating adipokines, metabolic syndrome (MetS), and longitudinal change in MetS components (namely abdominal obesity, blood pressure, lipid profile, and glycemic status) over a 1-year period in a cohort of rape exposed (RE) and rape unexposed (RUE) females. Materials and Methods: Seven hundred seventy-eight RE and 617 RUE black South African women aged 18–40 years were recruited for the Rape Impact Cohort Evaluation study. Nonfasting blood samples were analyzed for cardiometabolic variables and adipokine levels using enzyme-linked immunosorbent assay. Serum adiponectin was measured in both RE and RUE and resistin, leptin, and leptin/adiponectin (L/A) ratio in RE only. Associations between baseline serum adipokines, MetS, and its components were assessed at baseline and follow-up using adjusted linear and logistic regressions. Results: In the RE group, adiponectin, leptin, and L/A ratio were significantly associated with MetS prevalence cross-sectionally (all p ≤ 0.001). No adipokine marker was related to incident MetS at 12-month follow-up. In the RE group, significant longitudinal associations with high-density lipoprotein cholesterol were shown for adiponectin (β = 0.146 [0.064], p = 0.022) and leptin (β = 0.001 [0.002], p = 0.012). Conclusions: Findings suggest that adipokines may have a potential role as biomarkers to identify RE individuals at high risk for CMD.
SIMULATIONS ON A MOVING MESH: THE CLUSTERED FORMATION OF POPULATION III PROTOSTARS

The cosmic dark ages ended a few hundred million years after the big bang, when the first stars began to fill the universe with new light. It has generally been argued that these stars formed in isolation and were extremely massive—perhaps 100 times as massive as the Sun. In a recent study, Clark and collaborators showed that this picture requires revision. They demonstrated that the accretion disks that build up around Population III stars are strongly susceptible to fragmentation and that the first stars should therefore form in clusters rather than in isolation. We here use a series of high-resolution hydrodynamical simulations performed with the moving mesh code AREPO to follow up on this proposal and to study the influence of environmental parameters on the level of fragmentation. We model the collapse of five independent minihalos from cosmological initial conditions, through the runaway condensation of their central gas clouds, to the formation of the first protostar, and beyond for a further 1000 years. During this latter accretion phase, we represent the optically thick regions of protostars by sink particles. Gas accumulates rapidly in the circumstellar disk around the first protostar, fragmenting vigorously to produce a small group of protostars. After an initial burst, gravitational instability recurs periodically, forming additional protostars with masses ranging from ∼0.1 to 10 M☉. Although the shape, multiplicity, and normalization of the protostellar mass function depend on the details of the sink-particle algorithm, fragmentation into protostars with diverse masses occurs in all cases, confirming earlier reports of Population III stars forming in clusters. Depending on the efficiency of later accretion and merging, Population III stars may enter the main sequence in clusters and with much more diverse masses than are commonly assumed.
On the origin of a model ENSO in the western Pacific

The origin of an air-sea coupled disturbance in the Anderson-McCreary model (Anderson and McCreary, 1985) with external land heating west of the Pacific is investigated in detail. It is demonstrated that nonlinearities in the Anderson-McCreary model dramatically change the state predicted by the linear theory. The repetitious generation of the coupled disturbance has nothing to do with the linear U1 mode of Hirst (1988) as well as off-equatorial Rossby waves. It is perfectly determined by the amplitude of the external heating. The mass budget analysis demonstrates that the change of zonal wind direction in the western Pacific, which is due to relative importance between the external land heating and the heating associated with the previous coupled disturbance, modulates the oceanic heat content relevant to the origin of the following coupled disturbance. This mechanism gives the oscillation between two stable equilibria (La Nina and El Nino), which is very different from those described in Battisti (1988), Schopf and Suarez (1987) and Zebiak and Cane (1987). Despite lots of model limitations the present results seem to be compatible with the recent analyses of the air-sea-land system in the western Pacific.
Depth dependence of the ionization energy of shallow hydrogen states in ZnO and CdS

The characteristics of shallow hydrogen-like muonium (Mu) states in nominally undoped ZnO and CdS (0001) crystals have been studied close to the surface at depths in the range of 10 nm - 180 nm by using low-energy muons, and in the bulk using conventional muSR. The muon implantation depths are adjusted by tuning the energy of the low-energy muons between 2.5 keV and 30 keV. We find that the bulk ionization energy of the shallow donor-like Mu state is lowered by about 10 meV at a depth of 100 nm, and continuously decreasing on approaching the surface. At a depth of about 10 nm the ionization energy is further reduced by 25-30 meV compared to its bulk value. We attribute this change to the presence of electric fields due to band bending close to the surface, and we determine the depth profile of the electric field within a simple one-dimensional model.
Hematopoietic Stem Cell Transplantation for Acute Myeloid Leukemia: An Overview of Systematic Reviews

Background Hematopoietic stem cell transplantation (HSCT) has become the main treatment for acute myeloid leukemia (AML) and has been studied in many systematic reviews (SRs), but strong conclusions have not been drawn yet. Objective This study aimed to summarize and critically evaluate the methodological and evidence quality of SRs and meta-analysis on this topic. Methods PubMed, Embase, the Cochrane Library, and Web of Science were searched for SRs/meta-analyses regarding HSCT for AML. Two reviewers assessed the quality of SRs/meta-analyses in line with AMSTAR-2 and evaluated the strength of evidence quality with the grading of the evaluation system (GRADE) for concerned outcomes independently. Results 12 SR/Meta articles were included, and the AMSTAR-2 scale showed that the quality grade of all articles was low or very low. GRADE results showed 29 outcomes, 2 of which were high, 12 were moderate, and 15 were low. Limitations and inconsistency were the most important factors leading to degradation, followed by imprecision and publication bias. Allo-SCT had better OS and DFS benefits than auto-SCT and significantly reduced the relapse in intermediate-risk AML/CR1 patients. Auto-SCT was associated with lower TRM than allo-SCT but generally had higher relapse. The results should be confirmed further for the low or moderate evidence quality. Conclusion Current SRs show that allo-SCT in the treatment of AML might improve the OS, RFS, and DFS. Auto-SCT has significantly lower TRM but higher RR. Whether bone marrow transplantation is superior to nonmyeloablative chemotherapy remains to be evaluated. Meanwhile, the quality of methodology needs to be further improved. The intensity of evidence was uneven, and the high-quality evidence of outcomes was lacking. Considering the limitations of our overview, more rigorous and scientific studies are needed to fully explore the efficacy of different interventions of HSCT in AML, and clinicians should be more cautious in the treatment.
Evidence for Two-Component Jet in Sw J1644+57

The continued observations of Sw J1644+57 in X-ray and radio bands accumulated a rich data set to study the relativistic jet launched in this tidal disruption event. We find that the re-brightening feature in the radio light curve can be naturally explained by the two-component jet model. The possible origin of this structured jet are the Blandford-Znajek and Blandford-Payne mechanisms. We also show that this two-component jet model can interpret the two kinds of quasi-periodic variations in the X-ray light curve: a 200 second quasi-periodic oscillation (QPO) and a 2.7-day quasi-periodic variation. The latter is interpreted by a precessing outer jet launched near the Bardeen-Petterson radius of a warped disk. The $\sim$ 200s QPO could be associated with a second, narrower jet sweeping the observer line-of-sight periodically, which is launched from a spinning black hole in the misaligned direction with respect to the black hole's angular momentum.
Quantitative description of the azimuthal dependence of the exchange bias effect

While the principal features of the exchange bias between a ferromagnet and an antiferromagnet are believed to be understood, a quantitative description is still lacking. We show that interface spin disorder is the main reason for the discrepancy of model calculations versus experimental results. Taking into account spin disorder at the interface between the ferromagnet and the antiferromagnet by modifying the well known Meiklejohn and Bean model, an almost perfect agreement can be reached. As an example this is demonstrated for the CoFe/IrMn exchange biased bilayer by analysing the azimuthal dependence of magnetic hysteresis loops from MOKE measurements. Both exchange bias and coercive fields for the complete 360° angular range are reproduced by our model.
Spectral Energy Distributions of Be and Other Massive Stars

We present spectrophotometric data from 0.4 μm to 4.2 μm for bright, northern sky, Be stars and several other types of massive stars. Our goal is to use these data with ongoing high–angular-resolution interferometric observations to model the density structure and sky orientation of the gas surrounding these stars. We also present a montage of the Hα and near-infrared emission lines that form in Be star disks. We find that a simplified measurement of the IR excess flux appears to be correlated with the strength of emission lines from high level transitions of hydrogen. This suggests that the near-IR continuum and upper level line fluxes both form in the inner part of the disk, close to the star.
THE COLDEST BROWN DWARF (OR FREE-FLOATING PLANET)?: THE Y DWARF WISE 1828+2650

We have monitored the position of the cool Y dwarf WISEPA J182831.08+265037.8 using a combination of ground- and space-based telescopes and have determined its distance to be 11.2+1.3−1.0 pc. Its absolute H magnitude, MH = 22.21+0.25−0.22 mag, suggests a mass in the range 0.5–20 MJup for ages of 0.1–10 Gyr with an effective temperature in the range 250–400 K. The broad range in mass is due primarily to the unknown age of the object. Since the high tangential velocity of the object, 51 ± 5 km s−1, is characteristic of an old disk population, a plausible age range of 2–4 Gyr leads to a mass range of 3–6 MJup based on fits to the (highly uncertain) COND evolutionary models. The range in temperature is due to the fact that no single model adequately represents the 1–5 μm spectral energy distribution (SED) of the source, failing by factors of up to five at either the short or long wavelength portions of the SED. The appearance of this very cold object may be affected by non-equilibrium chemistry or low temperature condensates forming clouds, two atmospheric processes that are known to be important in brown dwarf atmospheres but have proven difficult to model. Finally, we argue that there would have to be a very steep upturn in the number density of late-type Y-dwarfs to account for the putative population of objects suggested by recent microlensing observations. Whether WISE 1828+2650 sits at the low-mass end of the brown dwarf population or is the first example of a large number of “free-floating” planets is not yet known.
ON THE IMPOSSIBILITY TO EXTEND TRIPLES OF MUTUALLY UNBIASED PRODUCT BASES IN DIMENSION SIX

An analytic proof is given which shows that it is impossible to extend any triple of mutually unbiased (MU) product bases in dimension six by a single MU vector. Furthermore, the 16 states obtained by removing two orthogonal states from any MU product triple cannot figure in a (hypothetical) complete set of seven MU bases. These results follow from exploiting the structure of MU product bases in a novel fashion, and they are among the strongest ones obtained for MU bases in dimension six without recourse to computer algebra.
Regulatory space in local government audit: An international comparative study of 20 countries

IMPACT Auditing fulfils a public interest role for public spending, which is important to underpin the state and democracy. However, public sector auditing is under increasing public scrutiny and political pressure, especially following crises that challenge public finances including at state and local level. This article provides a comparative analysis of the development of auditing practices in governments internationally at both local and state level. To do so it analyses themes of ‘organization and fragmentation’, ‘independence and competition’, ‘audit scope’, and ‘inspection/performance assessment’. This will help inform academics, policy-makers and practitioners of contemporary practice to improve their own regulatory space.
Repairing relationship conflict in community sport work: “Offender” perspectives

ABSTRACT Through our investigation of relationship conflict and repair in community sport coaching this article makes a novel contribution to the sociology of sport work. Such inquiry is necessary as interpersonal conflict has the potential to erode worker commitment, engagement, performance, satisfaction, and mental health. To date, the study of interpersonal conflict in coaching has been framed psychologically. It is our position that sociologically inspired inquiry is not only necessary but can valuably contribute to academic debate in this area. To redress this situation we conducted in-depth, semi-structured, interviews with 18 community sport coaches to produce rich insights into the participants’ (transgressors) understandings of fractured workplace relations, remedial work used to repair and restore relationships, as well as desirable and undesirable consequences emanating from these restorative efforts. Through our application of Ren and Gray’s and Goffman’s theorization addressing restoration mechanismsthe present study extends existing understanding by detailing how a) relationship conflict was triggered by the participants having violated the identity and control of significant working others, b) participants attempted to repair relations by offering accounts, apologies, and demonstrations of concern, and c) the success of these restorative efforts was variable and dependent on their being accepted by the offended parties. It is our hope that these original empirical and theoretical insights not only advance understanding about relationship conflict and repair but prompt further sociologically inspired research into this important interpersonal aspect of sport work.
Modified anterior transarticular C1/2 fixation for odontoid fractures: An approach with high complication rate in geriatric population

Background: In patients over 75 years of age, we applied a modified anterior transarticular C1/2 fixation with reduced pharyngeal mobilization versus the standard anterior triple/quadruple osteosynthesis procedures. Methods: From 2010 to 2018, 29 patients underwent a modified anterior transarticular C1/2 fixation utilizing single odontoid screw fixation through a right-sided Smith-Robinson – (i.e., short and steep screw trajectory for the right and long trajectory for the left side) approach. All the patients were 75 years of age or older (mean age 82.6) and had sustained odontoid Type II fractures. In addition, a subset exhibited further ligamentous injuries and/or atlas fractures. Their Mean Age-adjusted Charlson Comorbidity Index was 5.3 points (range 3–12), while mean American Society of Anesthesiologists scores averaged 2.9 (range 2–4). Results: The mean operating time was 55.8 min, there were no intraoperative complications, and there was minimal blood loss in all cases. The most common medical complications included aspiration pneumonia (24.1%, n = 7), altered mental status (17.2%, n = 5), and cardiac decompensation (6.9%, n = 2). One patient with delayed dysphagia and an infected implant resulting in loosening/dislocation required implant removal and long-term antibiotic therapy. The 30-day mortality rate was 13.8% (four patients) and the 1-year mortality rate was 27.6% (eight patients). Conclusion: Anterior transarticular C1/2/odontoid fixation with reduced pharyngeal mobilization and shorter operative times was associated with high morbidity/mortality rates. Dysphagia/aspiration was the major postoperative complications leading to some deaths especially in patients with dementia/Parkinsonism.
Wavelet analysis of pulsating white dwarfs.

Parts of light curves of two variable white dwarfs, G191 16 and PG 1351+489, are investigated by means of a wavelet analysis. This time-frequency analysis decomposes the light curves into their different oscillating components whose temporal behaviors are then individually studied. In addition to an oscillation of large amplitude, small amplitude oscillations are thereby clearly emphasized for both stars. Amplitude variations are found for most detected oscillations with periods of modulation as long or greater than the time intervals of the corresponding runs. A wavelet analysis of a comparison star gives the quality of the night in localizing perturbative atmospherical events
An efficient Fokker–Planck solver and its application to stochastic particle acceleration in galaxy clusters

Particle acceleration by turbulence plays a role in many astrophysical environments. The non- linear evolution of the underlying cosmic-ray spectrum is complex and can be described by a Fokker-Planck equation, which in general has to be solved numerically. We present here an implementation to compute the evolution of a cosmic-ray spectrum coupled to turbulence considering isotropic particle pitch-angle distributions and taking into account the relevant particle energy gains and losses. Our code can be used in run time and post-processing to very large astrophysical fluid simulations. We also propose a novel method to compress cosmic- ray spectra by a factor of ten, to ease the memory demand in very large simulations. We show a number of code tests, which firmly establish the correctness of the code. In this paper we focus on relativistic electrons, but our code and methods can be easily extended to the case of hadrons. We apply our pipeline to the relevant problem of particle acceleration in galaxy clusters. We define a sub-grid model for compressible MHD-turbulence in the intra- cluster-medium and calculate the corresponding reacceleration timescale from first principles. We then use a magneto-hydrodynamic simulation of an isolated cluster merger to follow the evolution of relativistic electron spectra and radio emission generated from the system over several Gyrs.