Miracle-dz/UniFAR-FTUs huggingface dataset:
A CORRECTION TO THE STANDARD GALACTIC REDDENING MAP: PASSIVE GALAXIES AS STANDARD CRAYONS

We present corrections to the Schlegel et al. (SFD98) reddening maps over the Sloan Digital Sky Survey (SDSS) northern Galactic cap area. To find these corrections, we employ what we call the “standard crayon” method, in which we use passively evolving galaxies as color standards to measure deviations from the reddening map. We select these passively evolving galaxies spectroscopically, using limits on the Hα and [O ii] equivalent widths to remove all star-forming galaxies from the SDSS main galaxy catalog. We find that by correcting for known reddening, redshift, color–magnitude relation, and variation of color with environmental density, we can reduce the scatter in color to below 3% in the bulk of the 151,637 galaxies that we select. Using these galaxies, we construct maps of the deviation from the SFD98 reddening map at 4. °5 resolution, with 1σ error of ∼1.5 mmag E(B − V). We find that the SFD98 maps are largely accurate with most of the map having deviations below 3 mmag E(B − V), though some regions do deviate from SFD98 by as much as 50%. The maximum deviation found is 45 mmag in E(B − V), and spatial structure of the deviation is strongly correlated with the observed dust temperature, such that SFD98 underpredict reddening in regions of low dust temperature. Our maps of these deviations, as well as their errors, are made available to the scientific community on the Web as a supplemental correction to SFD98.
ATCA detections of massive molecular gas reservoirs in dusty, high-z radio galaxies

This is an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. © 2016 The Authors. First published online October 27, 2016, available online at doi: 10.1093/mnras/stw2774. Published by Oxford University Press on behalf of the Royal Astronomical Society.
The AGN content of deep radio surveys and radio emission in radio-quiet AGN. Why every astronomer should care about deep radio fields

Abstract We present our very recent results on the sub-mJy radio source populations at 1.4 GHz based on the Extended Chandra Deep Field South VLA survey, which reaches ~ 30 μJy, with details on their number counts, evolution, and luminosity functions. The sub-mJy radio sky turns out to be a complex mix of star-forming galaxies and radio-quiet AGN evolving at a similar, strong rate and declining radio-loud AGN. While the well-known flattening of the radio number counts below 1 mJy is mostly due to star-forming galaxies, these sources and AGN make up an approximately equal fraction of the sub-mJy sky. Our results shed also light on a fifty-year-old issue, namely radio emission from radio-quiet AGN, and suggest that it is closely related to star formation, at least at z ~ 1.5 − 2. The implications of our findings for future, deeper radio surveys, including those with the Square Kilometre Array, are also discussed. One of the main messages, especially to non-radio astronomers, is that radio surveys are reaching such faint limits that, while previously they were mainly useful for radio quasars and radio galaxies, they are now detecting mostly star-forming galaxies and radio-quiet AGN, i.e., the bulk of the extragalactic sources studied in the infrared, optical, and X-ray bands.
Phonon and crystal field excitations in geometrically frustrated rare earth titanates

The phonon and crystal field excitations in several rare earth titanate pyrochlores are investigated. Magnetic measurements on single crystals of Gd(2)Ti(2)O(7), Tb(2)Ti(2)O(7), Dy(2)Ti(2)O(7), and Ho(2)Ti(2)O(7) are used for characterization, while Raman spectroscopy and terahertz time domain spectroscopy are employed to probe the excitations in the materials. The lattice excitations are found to be analogous across the compounds over the whole temperature range investigated (295-4 K). The resulting full phononic characterization of the R(2)Ti(2)O(7) pyrochlore structure is then used to identify crystal field excitations observed in the materials. Several crystal field excitations have been observed in Tb(2)Ti(2)O(7) in Raman spectroscopy, among which all of the previously reported excitations. The presence of additional crystal field excitations, however, suggests the presence of two inequivalent Tb(3+) sites in the low-temperature structure. Furthermore, the crystal field level at approximately 13 cm(-1) is found to be both Raman and dipole active, indicating broken inversion symmetry in the system and thus undermining its current symmetry interpretation. In addition, evidence is found for a significant crystal field-phonon coupling in Tb(2)Ti(2)O(7). The additional crystal field information on Tb(2)Ti(2)O(7) adds to the recent discussion on the low temperature symmetry of this system and may serve to improve its theoretical understanding.
Electronic structure and thermoelectric properties of n - and p -type SnSe from first-principles calculations

We present results of electronic band structure, Fermi surface and electron transport properties calculations in orthorhombic $n$- and $p$-type SnSe, applying Korringa-Kohn-Rostoker method and Boltzmann transport approach. The analysis accounted for temperature effect on crystallographic parameters in $Pnma$ structure as well as the phase transition to $CmCm$ structure at $T_c\sim 807 $K. Remarkable modifications of conduction and valence bands were notified upon varying crystallographic parameters within the structure before $T_c$, while the phase transition mostly leads to jump in the band gap value. The diagonal components of kinetic parameter tensors (velocity, effective mass) and resulting transport quantity tensors (electrical conductivity $\sigma$, thermopower $S$ and power factor PF) were computed in wide range of temperature ($15-900 $K) and, hole ($p-$type) and electron ($n-$type) concentration ($10^{17}-10^{21}$ cm$^{-3}$). SnSe is shown to have strong anisotropy of the electron transport properties for both types of charge conductivity, as expected for the layered structure. In general, $p$-type effective masses are larger than $n$-type ones. Interestingly, $p$-type SnSe has strongly non-parabolic dispersion relations, with the 'pudding-mold'-like shape of the highest valence band. The analysis of $\sigma$, $S$ and PF tensors indicates, that the inter-layer electron transport is beneficial for thermoelectric performance in $n$-type SnSe, while this direction is blocked in $p$-type SnSe, where in-plane transport is preferred. Our results predict, that $n$-type SnSe is potentially even better thermoelectric material than $p$-type one. Theoretical results are compared with single crystal $p$-SnSe measurements, and good agreement is found.
A Correlational Study on Teachers' Occupational Stress, Job Anxiety, Personality Dimensions and Performance

This study determined the correlations between occupational stress, job anxiety, personality dimensions and instructional competence of elementary teachers. The study employed the descriptive-correlational research design. There were 161 respondents composed of different teachers from small and big schools in the District of Los Banos, Laguna. The study utilized standardized questionnaires to assess the Occupational Stress, Job Anxiety, Personality Dimensions, and Instructional Competence of Elementary Teachers. The data gathered were treated using Mean, Standard Deviation, and ANOVA. The findings revealed that occupational stress has a significant relationship with the teacher's competence in terms of communicative competence. However, occupational stress has no significant relationship between the teacher's competence in terms of instructional competence and social skills. The result also shows that there is a significant relationship between job anxiety in terms of recognition and teacher's competence in terms of instructional competence. However, there is no significant relationship between job anxiety in terms of recognition and teacher's performance in terms of communicative competence and social skills. Similarly, there is a significant relationship between job anxiety in terms of self-esteem and teacher's competence in terms of instructional and communicative competence. However, there is no significant relationship between job anxiety in terms of self-esteem and teacher's competence in terms of social skills. Lastly, the result shows that there is no significant relationship between job anxiety in terms of security, human relations at work, rewards and punishment, future prospects and capacity for work, and teacher's performance in terms of instructional competence, communicative competence, and social skills.
LITHIUM IN OPEN CLUSTER RED GIANTS HOSTING SUBSTELLAR COMPANIONS

We have measured stellar parameters, [Fe/H], lithium abundances, rotation, and 12C/13C in a small sample of red giants (RGs) in three open clusters that are each home to a RG star that hosts a substellar companion (SSC) (NGC 2423 3, NGC 4349 127, and BD+12 1917 in M67). Our goal is to explore whether the presence of SSCs influences the Li content. Both 12C/13C and stellar rotation are measured as additional tracers of stellar mixing. One of the companion hosts, NGC 2423 3, is found to be Li-rich with A(Li) NLTE = ? > 1.56 dex, and this abundance is significantly higher than the A(Li) of the two comparison stars in NGC 2423. All three SSC hosts have the highest A(Li) and 12C/13C when compared to the control RGs in their respective clusters; however, except for NGC 2423 3, at least one control star has similarly high abundances within the uncertainties. Higher A(Li) could suggest that the formation or presence of planets plays a role in the degree of internal mixing on or before the RG branch. However, a multitude of factors affect A(Li) during the RG phase, and when the abundances of our sample are compared with the abundances of RGs in other open clusters available in the literature, we find that they all fall well within a much larger distribution of A(Li) and 12C/13C. Thus, even the high Li in NGC 2423 3 cannot be concretely tied to the presence of the SSC.
Optical absorption of twisted bilayer graphene with interlayer potential asymmetry

We investigate the band structure and the optical absorption spectrum of twisted bilayer graphenes with changing interlayer bias and Fermi energy simultaneously. We show that the interlayer bias lifts the degeneracy of the superlattice Dirac point, while the amount of the Dirac point shift is significantly suppressed in small rotation angles, and even becomes opposite to the applied bias. We calculate the optical absorption spectrum in various asymmetric potentials and Fermi energies, and associate the characteristic spectral features with the band structure. The spectroscopic features are highly sensitive to the interlayer bias and the Fermi energy, and widely tunable by the external field effect.
On Spectral Evolution and Temporal Binning in Gamma-Ray Bursts

ABSTRACT The understanding of the prompt γ-ray spectra of gamma-ray bursts (GRBs) is ofgreat importance to correctly interpreting the physical mechanisms that produce theunderlying event as well as the structure of the relativistic jet from which the emissionemanates. Time-resolved analysis of these spectra is the main method of extractinginformation from the data. In this work, several techniques for temporal binning ofGRB spectra are examined to understand the systematics associated with each withthe goal of ﬁnding the best method(s) to bin lightcurves for analysis. The followingbinning methods are examined: constant cadence (CC), Bayesian blocks (BB), signal-to-noise (S/N) and Knuth bins (KB). I ﬁnd that both the KB and BB methodsreconstruct the intrinsic spectral evolution accurately while the S/N method failsin most cases. The CC method is accurate when the cadence is not too coarse butdoes not necessarily bin the data based on the true source variability. Additionally,the integrated pulse properties are investigated and compared to the time-resolvedproperties. If intrinsic spectral evolution is present then the integrated propertiesare not useful in identifying physical and cosmological properties of GRBs withoutknowing the physical emission mechanism and its evolution.Key words: (stars:) gamma ray bursts – methods: data analysis
Gender Bias in Urology: How Do Patients Really Choose Their Urologist?

Purpose The present study aimed to investigate the influence of patients’ and urologists’ gender when choosing a urologist. With rising population diversity through immigration and generational differences, patient-centered healthcare has recently moved to the focus of European healthcare systems. As healthcare in urology often concentrates on sensitive topics, and often involves gender-specific diseases, research on the influence of gender on decision-making processes is of high importance. Understanding influence of gender on patients’ choices in real life would provide patients, and physicians alike, with the means to provide better resources to achieve greater satisfaction from visits to a urologist. Patients and Methods A questionnaire was prepared, and patients at our tertiary referral center were given the opportunity to voluntarily participate in our survey. We collected questionnaires from 1012 patients during their visits from June 2021 to October 2021. Results Patients were divided into groups according to their gender: male (n=763), female (n=246), and non-binary (n=3). Our patient cohort consisted of more men than women (75% vs 24%), with only three patients identifying as non-binary. Irrespective of the patients’ own gender, patients preferred a male urologist when problems were considered embarrassing, limiting daily activities, or when worrisome. When problems were considered painful, all patients preferred a female urologist. When patients had had a previous positive experience with a female or male urologist, they preferred to be treated by a female or male urologist, respectively. Overall, 65% of patients stated a gender preference for at least one given situation, or consultation scenario. Conclusion As the majority of our patients stated a gender preference, urological departments should be considerate of potential patients’ preferences for urologist gender that may be based on the individual patient’s history, taking a comprehensive approach to fulfill the patients’ need for same gender urologists in educational hospitals and health care services.
DISCOVERY OF X-RAY PULSATIONS FROM THE NEXT GEMINGA, PSR J1836+5925

We report recent XMM-Newton investigations of PSR J1836+5925, the “next Geminga,” which determined an X-ray pulsation of ∼173.3 ms. Its X-ray periodicity is consistent with the γ-ray ephemeris at the same epoch. The X-ray folded light curve has a sinusoidal structure that is different from the double-peaked γ-ray pulse profile. We have also analyzed the X-ray phase-averaged spectra which shows that the X-ray emission from PSR J1836+5925 is thermal dominant. This suggests that the X-ray pulsation mainly originates from the modulated hot spot on the stellar surface.
Neutrino-assisted fermion-boson transitions

We study fermion-boson transitions. Our approach is based on the $3\times 3$ subequations of Dirac and Duffin-Kemmer-Petiau equations, which link these equations. We demonstrate that free Dirac equation can be invertibly converted to spin-$0$ Duffin-Kemmer-Petiau equation in presence of a neutrino field. We also show that in special external fields, upon assuming again existence of a neutrino (Weyl) spinor, the Dirac equation can be transformed reversibly to spin-$0$ Duffin-Kemmer-Petiau equation. We argue that such boson-fermions transitions are consistent with the main channel of pion decay.
Numerical Boson Stars with a Single Killing Vector I. The $D\ge5$ Case

We numerically construct asymptotically anti-de Sitter boson star solutions using a minimally coupled $\frac{D-1}{2}$-tuplet complex scalar field in $D=5,7,9,11$ dimensions. The metric admits multiple Killing vector fields in general, however the scalar fields are only invariant under a particular combination, leading to such boson star solutions possessing just a single helical Killing symmetry. These boson stars form a one parameter family of solutions, which can be parametrized by the energy density at their center. As the central energy density tends to infinity, the angular velocity, mass, and angular momentum of the boson star exhibit damped harmonic oscillations about finite central values, while the Kretschmann invariant diverges, signaling the formation of a black hole in this limit.
New Estimation of the Spectral Index of High-Energy Cosmic Rays as Determined by the Compton-Getting Anisotropy

The amplitude of the Compton-Getting (CG) anisotropy contains the power-law index of the cosmic-ray energy spectrum. Based on this relation and using the Tibet air shower array data, we measure the cosmic-ray spectral index to be –3.03 ± 0.55stat ± <0.62syst between 6 and 40 TeV, consistent with –2.7 from direct energy spectrum measurements. Potentially, this CG anisotropy analysis can be utilized to confirm the astrophysical origin of the “knee” against models for nonstandard hadronic interactions in the atmosphere.
SUBARU WEAK LENSING MEASUREMENTS OF FOUR STRONG LENSING CLUSTERS: ARE LENSING CLUSTERS OVERCONCENTRATED?

We derive radial mass profiles of four strong lensing selected clusters which show prominent giant arcs (Abell 1703, SDSS J1446+3032, SDSS J1531+3414, and SDSS J2111−0115), by combining detailed strong lens modeling with weak lensing shear measured from deep Subaru Suprime-cam images. Weak lensing signals are detected at high significance for all four clusters, whose redshifts range from z = 0.28 to 0.64. We demonstrate that adding strong lensing information with known arc redshifts significantly improves constraints on the mass density profile, compared with those obtained from weak lensing alone. While the mass profiles are well fitted by the universal form predicted in N-body simulations of the Λ-dominated cold dark matter model, all four clusters appear to be slightly more centrally concentrated (the concentration parameters cvir ∼ 8) than theoretical predictions, even after accounting for the bias toward higher concentrations inherent in lensing-selected samples. Our results are consistent with previous studies which similarly detected a concentration excess, and increase the total number of clusters studied with the combined strong and weak lensing technique to 10. Combining our sample with previous work, we find that clusters with larger Einstein radii are more anomalously concentrated. We also present a detailed model of the lensing cluster Abell 1703 with constraints from multiple image families, and find the dark matter inner density profile to be cuspy with the slope consistent with −1, in agreement with expectations.
ROCHE-LOBE OVERFLOW SYSTEMS POWERED BY BLACK HOLES IN YOUNG STAR CLUSTERS: THE IMPORTANCE OF DYNAMICAL EXCHANGES

We have run 600 N-body simulations of intermediate-mass (∼3500 M☉) young star clusters (SCs; with three different metallicities (Z = 0.01, 0.1, and 1 Z☉). The simulations include the dependence of stellar properties and stellar winds on metallicity. Massive stellar black holes (MSBHs) with mass >25 M☉ are allowed to form through direct collapse of very massive metal-poor stars (Z < 0.3 Z☉). We focus on the demographics of black hole (BH) binaries that undergo mass transfer via Roche lobe overflow (RLO). We find that 44% of all binaries that undergo an RLO phase (RLO binaries) formed through dynamical exchange. RLO binaries that formed via exchange (RLO-EBs) are powered by more massive BHs than RLO primordial binaries (RLO-PBs). Furthermore, the RLO-EBs tend to start the RLO phase later than the RLO-PBs. In metal-poor SCs (0.01–0.1 Z☉), >20% of all RLO binaries are powered by MSBHs. The vast majority of RLO binaries powered by MSBHs are RLO-EBs. We have produced optical color–magnitude diagrams of the simulated RLO binaries, accounting for the emission of both the donor star and the irradiated accretion disk. We find that RLO-PBs are generally associated with bluer counterparts than RLO-EBs. We compare the simulated counterparts with the observed counterparts of nine ultraluminous X-ray sources. We discuss the possibility that IC 342 X-1, Ho IX X-1, NGC 1313 X-2, and NGC 5204 X-1 are powered by an MSBH.
WHERE ARE THE FOSSILS OF THE FIRST GALAXIES? II. TRUE FOSSILS, GHOST HALOS, AND THE MISSING BRIGHT SATELLITES

We use a new set of cold dark matter simulations of the local universe to investigate the distribution of fossils of primordial dwarf galaxies within and around the Milky Way. Throughout, we build upon previous results showing agreement between the observed stellar properties of a subset of the ultra-faint dwarfs and our simulated fossils. Here, we show that fossils of the first galaxies have galactocentric distributions and cumulative luminosity functions consistent with observations. In our model, we predict ∼300 luminous satellites orbiting the Milky Way, 50%–70% of which are well-preserved fossils. Within the Milky Way virial radius, the majority of these fossils have luminosities LV < 106 L☉. Despite our multidimensional agreement with observations at low masses and luminosities, the primordial model produces an overabundance of bright dwarf satellites (LV > 104 L☉) with respect to observations where observations are nearly complete. The “bright satellite problem” is most evident in the outer parts of the Milky Way. We estimate that, although relatively bright, the primordial stellar populations are very diffuse, producing a population with surface brightnesses below surveys’ detection limits, and are easily stripped by tidal forces. Although we cannot yet present unmistakable evidence for the existence of the fossils of first galaxies in the Local Group, the results of our studies suggest observational strategies that may demonstrate their existence: (1) the detection of “ghost halos” of primordial stars around isolated dwarfs would prove that stars formed in minihalos (M < 108 M☉) before reionization and strongly suggest that at least a fraction of the ultra-faint dwarfs are fossils of the first galaxies; and (2) the existence of a yet unknown population of ∼150 Milky Way ultra-faints with half-light radii rhl ≈ 100–1000 pc and luminosities LV < 104 L☉, detectable by future deep surveys. These undetected dwarfs would have the mass-to-light ratios, stellar velocity dispersions, and metallicities predicted in this work.