Miracle-dz/UniFAR-FTUs huggingface dataset:
He II optical depth and ultraviolet escape fraction of galaxies

We study the effect of H I ionizing photons escaping from high-redshift (high-z) galaxies have on the He II ionizing ultraviolet background (UVB) radiation. While these photons do not directly interact with He II ions, we show that they play an important role, through radiative transport, in modifying the shape of He II ionizing part of UVB spectrum. Within the observed range of UV escape from galaxies, we show that the rapid increase in He II Lyman alpha effective optical depth at z~2.7 can naturally be explained by radiative transport effects. Therefore, the relationship between a well measured He II Lyman alpha effective optical depth and the redshift in the post-He II reionization era can be used to place additional constraints on the redshift evolution of UV escape from high-z galaxies. Our study also suggests that the escape fraction of H I ionizing photons from galaxies has an important role in the fluctuations of the He II ionizing UVB.
Micrococcus porci sp. nov., Isolated from Feces of Black Pig (Sus scrofa)

An aerobic bacterium, designated as strain KD337-16T, was isolated from the fecal samples of a black pig. It exhibited spherical, non-motile and non–spore-forming, Gram-positive cells. KD337-16T was identified as a member of the genus Micrococcus through 16S rRNA gene sequencing, and its closest relatives were found to be Micrococcus endophyticus YIM 56238T (99.5% similarity), Micrococcus luteus NCTC 2665T (99.1%), Micrococcus yunnanensis YIM 65004T (99.1%), Micrococcus aloeverae AE-6T (99.1%), Micrococcus antarcticus T2T (98.9%), and Micrococcus flavus LW4T (98.7%). Phylogenomic trees were constructed, and strain KD337-16T was found to form its own cluster as an independent lineage of M. flavus LW4T. Between KD337-16T and its close relatives, the average nucleotide identity, average amino acid identity, and digital DNA–DNA hybridization were below the respective species delineation thresholds at 82.1–86.6%, 78.1–86.1%, and 24.4–34.9%. The major cellular fatty acids and polar lipids were anteiso-C15:0 and iso-C15:0, and DPG and PG, respectively. The predominant menaquinone was MK-8(H2). Taken together, the results indicate that strain KD337-16T is a novel species of the genus Micrococcus, for which the name Micrococcus porci sp. nov. is proposed. The type strain is KD337-16T (=BCRC 81318T = NBRC 115578T).
THE UBIQUITOUS RADIO CONTINUUM EMISSION FROM THE MOST MASSIVE EARLY-TYPE GALAXIES

We have measured the radio continuum emission of 396 early-type galaxies brighter than K = 9, using 1.4 GHz imagery from the NRAO Very Large Array Sky Survey, Green Bank 300 ft Telescope, and 64 m Parkes Radio Telescope. For MK < −24 early-type galaxies, the distribution of radio powers at fixed absolute magnitude spans four orders of magnitude and the median radio power is proportional to K-band luminosity to the power 2.78 ± 0.16. The measured flux densities of MK < −25.5 early-type galaxies are greater than zero in all cases. It is thus highly likely that the most massive galaxies always host an active galactic nucleus or have recently undergone star formation.
ROTATION PERIODS AND AGES OF SOLAR ANALOGS AND SOLAR TWINS REVEALED BY THE KEPLER MISSION

A new sample of solar analogs and twin candidates has been constructed and studied, paying particular attention to their light curves from NASA's Kepler mission. This Letter aims to assess their evolutionary status, derive their rotation and ages, and identify those which are solar analogs or solar twin candidates. We separate out the subgiants that compose a large fraction of the asteroseismic sample, and which show an increase in the average rotation period as the stars ascend the subgiant branch. The rotation periods of the dwarfs, ranging from 6 to 30 days and averaging 19 days, allow us to assess their individual evolutionary states on the main sequence and to derive their ages using gyrochronology. These ages are found to be in agreement with a correlation coefficient of r = 0.79 with independent asteroseismic ages, where available. As a result of this investigation, we are able to identify 34 stars as solar analogs and 22 of them as solar twin candidates.
AN INTERACTING GALAXY SYSTEM ALONG A FILAMENT IN A VOID

Cosmological voids provide a unique environment for the study of galaxy formation and evolution. The galaxy population in their interiors has properties significantly different from average field galaxies. As part of our Void Galaxy Survey (VGS), we have found a system of three interacting galaxies (VGS_31) inside a large void. VGS_31 is a small elongated group whose members are embedded in a common H i envelope. The H i picture suggests a filamentary structure with accretion of intergalactic cold gas from the filament onto the galaxies. We present deep optical and narrowband Hα data, optical spectroscopy, near-UV, and far-UV Galaxy Evolution Explorer and CO(1–0) data. We find that one of the galaxies, a Markarian object, has a ring-like structure and a tail evident both in optical and H i. While all three galaxies form stars in their central parts, the tail and the ring of the Markarian object are devoid of star formation. We discuss these findings in terms of a gravitational interaction and ongoing growth of galaxies out of a filament. VGS_31 is one of the first observed examples of a filamentary structure in a void. It is an important prototype for understanding the formation of substructure in a void. This system also shows that the galaxy evolution in voids can be as dynamic as in high-density environments.
Determinants of left ventricular diastolic dysfunction in hemodialysis patients

Introduction: Chronic kidney disease (CKD) induces changes in the myocardium known to influence morbidity and mortality, most severe in patients with end stage renal disease. Objectives: The working hypothesis was that in patients on chronic hemodialysis the prevalence of left ventricular diastolic dysfunction is correlated with the inflammatory, oxidative, metabolic, nutritional, and atherosclerotic status. Patients and Methods: An observational study was performed on 51 patients (age 59.76 ± 13.24 years) on hemodialysis treatment. Transthoracic cardiac ultrasound was conducted to evaluate LVDD. The burden of cardiac and arterial atherosclerosis was evaluated by cardiac ultrasound (aortic and mitral valve calcifications), vascular ultrasound (carotid and femoral atheroma plaques, common carotid intima-media thickness), and by abdominal radiography (aortic calcification score). Demographic and anthropometric parameters were determined. Blood samples were used to determine laboratory parameters reflecting the inflammatory, oxidative, and metabolic/nutrition status. Results: LVDD is positively correlated with the serum level of C-reactive protein (CRP) (P=0.04), the total antioxidant capacity of the serum (P=0.04), the presence (P=0.022) and number (P=0.04) of femoral plaques, the aortic calcification score (P=0.02), aortic valve stenosis (P=0.037), aortic annulus calcifications (P=0.02) and mitral valve calcifications (P=0.041). After the removal of the main confounder, degenerative aortic stenosis, only the associations with serum total antioxidant capacity (P=0.04) and aortic calcification score (P= 0.02) maintain their statistical significance. Conclusion: LVDD is positively correlated with inflammation and oxidative stress markers and with the severity of aortic calcification.
Physical conditions in star-forming regions around S235

Gas density and temperature in star forming regions around Sh2-235 are derived from ammonia line observations. This information is used to evaluate formation scenarios and to determine evolutionary stages of the young embedded clusters S235 East1, S235 East2, and S235 Central. We also estimate the gas mass in the embedded clusters and its ratio to the stellar mass. S235 East1 appears to be less evolved than S235 East2 and S235 Central. In S235 East1 the molecular gas mass exceeds that in the other clusters. Also, this cluster is more embedded in the parent gas cloud than the other two. Comparison with a theoretical model shows that the formation of these three clusters could have been stimulated by the expansion of the Sh2-235 HII region (hereafter S235) via a collect-and-collapse process, provided the density in the surrounding gas exceeds $3\cdot10^3$ cm$^{-3}$, or via collapse of pre-existing clumps. The expansion of S235 cannot be responsible for star formation in the southern S235 A-B region. However, formation of the massive stars in this region might have been triggered by a large-scale supernova shock. Thus, triggered star formation in the studied region may come in three varieties, namely collect-and-collapse and collapse of pre-existing clumps, both initiated by expansion of the local HII regions, and triggering by an external large-scale shock. We argue that the C235 A HII region expands into a highly non-uniform medium with increasing density. It is too young to trigger star formation in its vicinity by a collect-and-collapse process. There is an age spread inside the S235 A-B region. Massive stars in the S235 A-B region are considerably younger than lower mass stars in the same area. This follows from the estimates of their ages and the ages of associated HII regions.
Complex molecules in the W51 North region

We present Submillimeter Array (SMA) molecular line observations in two 2 GHz-wide bands centered at 217.5 and 227.5 GHz, toward the massive star forming region W51 North. We identified 84 molecular line transitions from 17 species and their isotopologues. The molecular gas distribution of these lines mainly peaks in the continuum position of W51 North, and has a small tail extending to the west, probably associated with W51 d2. In addition to the commonly detected nitrogen and oxygen-bearing species, we detected a large amount of transitions of the Acetone (CH$_3$COCH$_3$) and Methyl Formate (CH$_3$OCHO), which may suggest that these molecules are present in an early evolutionary stage of the massive stars. We also found that W51 North is an ethanol-rich source. There is no obvious difference in the molecular gas distributions between the oxygen-bearing and nitrogen-bearing molecules. Under the assumption of Local Thermodynamic Equilibrium (LTE), with the XCLASS tool, the molecular column densities, and rotation temperatures are estimated. We found that the oxygen-bearing molecules have considerable higher column densities and fractional abundances than the nitrogen-bearing molecules. The rotation temperatures range from 100 to 200 K, suggesting that the molecular emission could be originated from a warm environment. Finally, based on the gas distributions, fractional abundances and the rotation temperatures, we conclude that CH$_3$OH, C$_2$H$_5$OH, CH$_3$COCH$_3$ and CH$_3$CH$_2$CN might be synthesized on the grain surface, while gas phase chemistry is responsible for the production of CH$_3$OCH$_3$, CH$_3$OCHO and CH$_2$CHCN.
Understanding pan-Asian identity: how and when threat affects Asian and national origin identity attachment

Asians in the United States have traditionally been treated as a monolithic group, both in public discourse as well as in political science research. Despite the political origins of the Asian label, how unifying is it in practice? Using experimental design, I explicitly measure changes in the importance of one's Asian and national origin identities. Results show that individuals' national origin identity becomes more salient in the face of identity threat, whereas their Asian identity does not. Additionally, whether one's national origin identity becomes more salient depends on the type of identity threat. These results suggest that Asians' sense of pan-ethnic identity is not conditional on their national origin identity, with implications for the expected effects of identity primes in electoral and political contexts, as well as for research designs relying on such identity primes.
Who Controls the Immigration Bureaucracy? The Relative Influence of the Three Branches Over Asylum Policy Implementation

At the center of contentious debates concerning U.S. asylum policy are immigration judges, bureaucrats who decide life and death cases on a daily basis. Congress, the executive and the courts compete for influence over these key actors — administrative judges distinct from those examined in much of the bureaucratic control literature. They are hired, fired, promoted or demoted by executive officials; face congressional oversight; and must follow circuit law. We argue that, because of the fear of reversal, immigration judges will look most to the courts in the decision-making process. Our results support our theory. Examining over 900,000 immigration judges’ decisions, we find that, although IJs are influenced by a fear of pushback from the elected branches, the impact is conditional on circuit preferences. Our findings inform scholarly understanding of judicial behavior and bureaucratic accountability, and support the pursuit of judicial independence and due process in immigration courts.
Detection of Coherent Emission from the Bp Star HD 142990 at uGMRT Frequencies

HD 142990 is a Bp-type star with a nearly dipolar surface magnetic field of kilogauss strength. Recently, Lenc et al. reported the tentative discovery of Electron Cyclotron Maser Emission (ECME) from this star at 200 MHz. This type of emission has been observed from only three other hot magnetic stars. In this paper, we present our observations of HD 142990 with the upgraded Giant Metrewave Radio telescope at 550–804 MHz and with the legacy GMRT at 1420 MHz near the rotational phases of the nulls of the longitudinal magnetic field. We found strong enhancements in flux density in both circular polarizations, suggesting an ECME bandwith of at least 1.2 GHz (200–1420 MHz). In one of the observation sessions, we observed enhancements with opposite circular polarizations from the same magnetic pole. This has not been reported in any other hot magnetic star known to exhibit ECME. In order to explain this unusual finding, we suggest a scenario that involves a transition of the dominant mode of ECME between the magneto-ionic modes.
Quantization, holography, and the universal coefficient theorem

I present a method of quantization using cohomology groups extended via coefficient groups of different types. This is possible according to the universal coefficient theorem. I also show that by using this method new features of quantum field theory not visible in the previous treatments emerge. The main argument is that several constructions considered as absolute until now may appear as relative, depending on individual choices of group structures needed to probe a topology. The universal coefficient theorem also gives information about how these structures, as measured by different choices of groups, relate to one another. This may result in the formulation of new dualities and a deeper understanding of the relation between quantum field theories and gravity.
Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). VIII. A less biased view of the early co-evolution of black holes and host galaxies

We present ALMA [C ii] line and far-infrared (FIR) continuum observations of three $z \gt 6$ low-luminosity quasars ($M_{\rm 1450} \gt -25$ mag) discovered by our Subaru Hyper Suprime-Cam (HSC) survey. The [C ii] line was detected in all three targets with luminosities of $(2.4\mbox{--}9.5) \times 10^8\, L_{\odot }$, about one order of magnitude smaller than optically luminous ($M_{\rm 1450} \lesssim -25$ mag) quasars. The FIR continuum luminosities range from $\lt 9 \times 10^{10}\, L_{\odot }$ (3 $\sigma$ limit) to ${\sim } 2 \times 10^{12}\, L_{\odot }$, indicating a wide range in star formation rates in these galaxies. Most of the HSC quasars studied thus far show [C ii]/ FIR luminosity ratios similar to local star-forming galaxies. Using the [C ii]-based dynamical mass ($M_{\rm dyn}$) as a surrogate for bulge stellar mass ($M_{\rm\, bulge}$), we find that a significant fraction of low-luminosity quasars are located on or even below the local $M_{\rm\, BH}$–$M_{\rm\, bulge}$ relation, particularly at the massive end of the galaxy mass distribution. In contrast, previous studies of optically luminous quasars have found that black holes are overmassive relative to the local relation. Given the low luminosities of our targets, we are exploring the nature of the early co-evolution of supermassive black holes and their hosts in a less biased way. Almost all of the quasars presented in this work are growing their black hole mass at a much higher pace at $z \sim 6$ than the parallel growth model, in which supermassive black holes and their hosts grow simultaneously to match the local $M_{\rm\, BH}$–$M_{\rm\, bulge}$ relation at all redshifts. As the low-luminosity quasars appear to realize the local co-evolutionary relation even at $z \sim 6$, they should have experienced vigorous starbursts prior to the currently observed quasar phase to catch up with the relation.
THE FIVE YEAR FERMI/GBM MAGNETAR BURST CATALOG

Since launch in 2008, the Fermi Gamma-ray Burst Monitor (GBM) has detected many hundreds of bursts from magnetar sources. While the vast majority of these bursts have been attributed to several known magnetars, there is also a small sample of magnetar-like bursts of unknown origin. Here, we present the Fermi/GBM magnetar catalog, providing the results of the temporal and spectral analyses of 440 magnetar bursts with high temporal and spectral resolution. This catalog covers the first five years of GBM magnetar observations, from 2008 July to 2013 June. We provide durations, spectral parameters for various models, fluences, and peak fluxes for all the bursts, as well as a detailed temporal analysis for SGR J1550–5418 bursts. Finally, we suggest that some of the bursts of unknown origin are associated with the newly discovered magnetar 3XMM J185246.6+0033.7.
Ly α emission from galaxies in the Epoch of Reionization

The intrinsic strength of the Ly$\alpha$ line in young, star-forming systems makes it a special tool for studying high-redshift galaxies. However, interpreting observations remains challenging due to the complex radiative transfer involved. Here, we combine state-of-the-art hydrodynamical simulations of 'Alth{\ae}a', a prototypical Lyman Break Galaxy (LBG, stellar mass $M_{\star}$$\simeq$ $10^{10}{\rm M}_{\odot})$ at $z=7.2$, with detailed radiative transfer computations of dust/continuum, C[II] 158 $\mu$m, and Ly$\alpha$ to clarify the relation between the galaxy properties and its Ly$\alpha$ emission. Alth{\ae}a exhibits low ($f_\alpha<1$\%) Ly$\alpha$ escape fractions and Equivalent Widths, EW $\lesssim 6$ Angstrom for the simulated lines of sight, with a large scatter. The correlation between escape fraction and inclination is weak, as a result of the rather chaotic structure of high-redshift galaxies. Low $f_\alpha$ values persist even if we artificially remove neutral gas around star forming regions to mimick the presence of HII regions. The high attenuation is primarily caused by dust clumps co-located with young stellar clusters. We can turn Alth{\ae}a into a Lyman Alpha Emitter (LAE) only if we artificially remove dust from the clumps, yielding EWs up to $22$ Angstrom. Our study suggests that the LBG-LAE duty-cycle required by recent clustering measurements poses the challenging problem of a dynamically changing dust attenuation. Finally, we find an anti-correlation between the magnitude of Ly$\alpha$-C[II] line velocity shift and Ly$\alpha$ luminosity.
Matching dust emission structures and magnetic field in high-latitude cloud L1642: comparing Herschel and Planck maps

The nearby cloud L1642 is one of only two known very high latitude (|b| > 30 deg) clouds actively forming stars. It is a rare example of star formation in isolated conditions, and can reveal important details of star formation in general, e.g., of the effect of magnetic fields. We compare Herschel dust emission structures and magnetic field orientation revealed by Planck polarization maps in L1642. The high-resolution ($\sim20"$) Herschel data reveal a complex structure including a dense, compressed central clump, and low density striations. The Planck polarization data (at 10$'$ resolution) reveal an ordered magnetic field pervading the cloud and aligned with the surrounding striations. There is a complex interplay between the cloud structure and large scale magnetic field. This suggests that the magnetic field is closely linked to the formation and evolution of the cloud. CO rotational emission confirms that the striations are connected with the main clumps and likely to contain material either falling into or flowing out of the clumps. There is a clear transition from aligned to perpendicular structures approximately at a column density of $N_{\rm{H}} = 1.6 \times 10^{21}\, {{\rm cm}}^{-2}$. Comparing the Herschel maps with the Planck polarization maps shows the close connection between the magnetic field and cloud structure even in the finest details of the cloud.
Impact of the symmetry energy on nuclear pasta phases and crust-core transition in neutron stars

We study the impact of the symmetry energy on properties of nuclear pasta phases and crust-core transition in neutron stars. We perform a self-consistent Thomas--Fermi calculation employing the relativistic mean-field model. The properties of pasta phases presented in the inner crust of neutron stars are investigated and the crust-core transition is examined. It is found that the slope of the symmetry energy plays an important role in determining the pasta phase structure and the crust-core transition. The correlation between the symmetry energy slope and the crust-core transition density obtained in the Thomas--Fermi approximation is consistent with that predicted by the liquid-drop model.
The weak Haagerup property

We introduce the weak Haagerup property for locally compact groups and prove several hereditary results for the class of groups with this approximation property. The class contains a priori all weakly amenable groups and groups with the (usual) Haagerup property, but examples are given of groups with the weak Haagerup property which are not weakly amenable and do not have the Haagerup property. In the second part of the paper we introduce the weak Haagerup property for finite von Neumann algebras, and we prove several hereditary results here as well. Also, a discrete group has the weak Haagerup property if and only if its group von Neumann algebra does. Finally, we give an example of two II_1 factors with different weak Haagerup constants.
Nonlinear Alfvén waves in extended magnetohydrodynamics

Large-amplitude Alfven waves are observed in various systems in space and laboratories, demonstrating an interesting property that the wave shapes are stable even in the nonlinear regime. The ideal magnetohydrodynamics (MHD) model predicts that an Alfven wave keeps an arbitrary shape constant when it propagates on a homogeneous ambient magnetic field. However, such arbitrariness is an artifact of the idealized model that omits the dispersive effects. Only special wave forms, consisting of two component sinusoidal functions, can maintain the shape; we derive fully nonlinear Alfven waves by an extended MHD model that includes both the Hall and electron inertia effects. Interestingly, these “small-scale effects” change the picture completely; the large-scale component of the wave cannot be independent of the small scale component, and the coexistence of them forbids the large scale component to have a free wave form. This is a manifestation of the nonlinearity-dispersion interplay, which is somewhat different from that of solitons.