Miracle-dz/UniFAR-FTUs huggingface dataset:
METALLICITY DISTRIBUTION FUNCTIONS, RADIAL VELOCITIES, AND ALPHA ELEMENT ABUNDANCES IN THREE OFF-AXIS BULGE FIELDS

We present radial velocities and chemical abundance ratios of [Fe/H], [O/Fe], [Si/Fe], and [Ca/Fe] for 264 red giant branch stars in three Galactic bulge off-axis fields located near (l, b) = (−5.5, −7), (−4, −9), and (+8.5, +9). The results are based on equivalent width and spectrum synthesis analyses of moderate resolution (R ≈ 18,000), high signal-to-noise ratio (S/N ∼ 75–300 pixel-1) spectra obtained with the Hydra spectrographs on the Blanco 4 m and WIYN 3.5 m telescopes. The targets were selected from the blue side of the giant branch to avoid cool stars that would be strongly affected by CN and TiO; however, a comparison of the color–metallicity distribution in literature samples suggests that our selection of bluer targets should not present a significant bias against metal-rich stars. We find a full range in metallicity that spans [Fe/H] ≈−1.5 to +0.5, and that, in accordance with the previously observed minor-axis vertical metallicity gradient, the median [Fe/H] also declines with increasing Galactic latitude in off-axis fields. The off-axis vertical [Fe/H] gradient in the southern bulge is estimated to be ∼0.4 dex kpc-1; however, comparison with the minor-axis data suggests that a strong radial gradient does not exist. The (+8.5, +9) field exhibits a higher than expected metallicity, with a median [Fe/H] = −0.23, that might be related to a stronger presence of the X-shaped bulge structure along that line-of-sight. This could also be the cause of an anomalous increase in the median radial velocity for intermediate metallicity stars in the (+8.5, +9) field. However, the overall radial velocity and dispersion for each field are in good agreement with recent surveys and bulge models. All fields exhibit an identical, strong decrease in velocity dispersion with increasing metallicity that is consistent with observations in similar minor-axis outer bulge fields. Additionally, the [O/Fe], [Si/Fe], and [Ca/Fe] versus [Fe/H] trends are identical among our three fields, and are in good agreement with past bulge studies. We find that stars with [Fe/H] ≲ −0.5 are α-enhanced, and that the [α/Fe] ratios decline at higher metallicity. At [Fe/H] ≲ 0, the α-element trends are indistinguishable from the halo and thick disk, and the variations in the behavior of individual α-elements are consistent with production in massive stars and a rapid bulge formation timescale.
THE FRACTION OF GLOBULAR CLUSTER SECOND-GENERATION STARS IN THE GALACTIC HALO

Many observational studies have revealed the presence of multiple stellar generations in Galactic globular clusters. These studies suggest that second-generation stars make up a significant fraction of the current mass of globular clusters, with the second-generation mass fraction ranging from ∼50% to 80% in individual clusters. In this Letter, we carry out hydrodynamical simulations to explore the dependence of the mass of second-generation stars on the initial mass and structural parameters and stellar initial mass function (IMF) of the parent cluster. We then use the results of these simulations to estimate the fraction fSG,H of the mass of the Galactic stellar halo composed of second-generation stars that originated in globular clusters. We study the dependence of fSG,H on the parameters of the IMF of the Galactic globular cluster system. For a broad range of initial conditions, we find that the fraction of mass of the Galactic stellar halo in second-generation stars is always small, fSG,H < 4%–6% for a Kroupa-1993 IMF and fSG,H < 7%–9% for a Kroupa-2001 IMF.
Estimation of Genetic Parameters a nd Non Genetic Factors for Milk Yield and Litter Size at Birth of Awassi Sheep in Drylands

SUMMARY The present study utilized 1195 records from 702 ewes of Awassi sheep progenies of 111 sires and 451 dams bred in the drylands at Al-Fjaj station, Jordan. The aim of this study was to estimate genetic parameters as well as to investigate non-genetic factors affecting milk yield (MK) and litter size at birth (LZB) using SAS and MTDFREML programs. Average of MK and LZB were 92.84 (kg) and 1.16, respectively. MK was high significantly (P<0.01) affected by parity, age of ewe, year of lambing, and lactation period, while only the year of lambing had a significant (P<0.05) effect on LZB. The heritability and repeatability were 0.07 and 0.10 for MK, while they were 0.05 and 0.25 for LZB. Genetic and phenotypic correlations between MK and LZB were 0.17 and 0.02, respectively. The research concluded that the herd is genetically homozygous and therefore there are a need to increase genetic variance by introducing improved rams and selected females.
Imprints of white dwarf recoil in the separation distribution of Gaia wide binaries

We construct from Gaia DR2 an extensive and very pure ($\lesssim 0.2\%$ contamination) catalog of wide binaries containing main-sequence (MS) and white dwarf (WD) components within 200 pc of the Sun. The public catalog contains, after removal of clusters and resolved higher-order multiples, $>$50,000 MS/MS, $>$3,000 WD/MS, and nearly 400 WD/WD binaries with projected separations of $50 \lesssim s/{\rm AU} 10,000$ AU. In contrast, the separation distributions of WD/MS and WD/WD binaries show distinct breaks at $\sim$ 3,000 AU and $\sim$1,500 AU, respectively: they are flatter than the MS/MS distribution at small separations and steeper at large separations. Using binary population synthesis models, we show that these breaks are unlikely to be caused by external factors but can be explained if the WDs incur a kick of $\sim$ 0.75 km s$^{-1}$ during their formation, presumably due to asymmetric mass loss. The data rule out typical kick velocities above 2km s$^{-1}$. Our results imply that most wide binaries with separations exceeding a few thousand AU become unbound during post-MS evolution.
Multiwavelength diagnostics of accretion in an X-ray selected sample of CTTSs

Context. High resolution X-ray spectroscopy has revealed soft X-rays from high density plasma in classical T Tauri stars (CTTSs), probably arising from the accretion shock region. However, the mass accretion rates derived from the X-ray observations are consistently lower than those derived from UV/optical/NIR studies. Aims. We aim to test the hypothesis that the high density soft X-ray emission originates from accretion by analysing, in a homogeneous manner, optical accretion indicators for an X-ray selected sample of CTTSs. Methods. We analyse optical spectra of the X-ray selected sample of CTTSs and calculate the accretion rates based on measuring the Hα ,H β ,H γ ,H eii 4686 A, He i 5016 A, He i 5876 A, O i 6300 A, and He i 6678 A equivalent widths. In addition, we also calculate the accretion rates based on the full width at 10% maximum of the Hα line. The different optical tracers of accretion are compared and discussed. The derived accretion rates are then compared to the accretion rates derived from the X-ray spectroscopy. Results. We find that, for each CTTS in our sample, the different optical tracers predict mass-accretion rates that agree within the errors, albeit with a spread of ≈1 order of magnitude. Typically, mass-accretion rates derived from Hα and He i 5876 A are larger than those derived from Hβ ,H γ ,a nd Oi. In addition, the Hα full width at 10%, whilst a good indicator of accretion, may not accurately measure the mass-accretion rate. When the optical mass-accretion rates are compared to the X-ray derived mass-accretion rates, we
REVISITING THE LIGHT CURVES OF GAMMA-RAY BURSTS IN THE RELATIVISTIC TURBULENCE MODEL

Rapid temporal variability has been widely observed in the light curves of gamma-ray bursts (GRBs). One possible mechanism for such variability is related to the relativistic eddies in the jet. In this paper, we include the contribution of the inter-eddy medium together with the eddies to the gamma-ray emission. We show that the gamma-ray emission can either lead or lag behind the observed synchrotron emission, where the latter originates in the inter-eddy medium and provides most of the seed photons for producing gamma-ray emission through inverse Compton scattering. As a consequence, we argue that the lead/lag found in non-stationary short-lived light curves may not reveal the intrinsic lead/lag of different emission components. In addition, our results may explain the lead of gamma-ray emission with respect to optical emission observed in GRB 080319B.
M2K: I. A Jupiter-Mass Planet Orbiting the M3V Star HIP 79431

Doppler observations from Keck Observatory reveal the presence of a planet with M sin i of 2.1 MJup orbiting the M3V star HIP 79431. This is the sixth giant planet to be detected in Doppler surveys of M dwarfs and it is one of the most massive planets discovered around an M dwarf star. The planet has an orbital period of 111.7 days and an orbital eccentricity of 0.29. The host star is metal rich, with an estimated [Fe/H] = +0.4. This is the first planet to emerge from our new survey of 1600 M-to-K dwarf stars.
DOES SIZE MATTER? THE UNDERLYING INTRINSIC SIZE DISTRIBUTION OF RADIO SOURCES AND IMPLICATIONS FOR UNIFICATION BY ORIENTATION

Unification by orientation is a ubiquitous concept in the study of active galactic nuclei. A gold standard of the orientation paradigm is the hypothesis that radio galaxies and radio-loud quasars are intrinsically the same, but are observed over different ranges of viewing angles. Historically, strong support for this model was provided by the projected sizes of radio structure in luminous radio galaxies, which were found to be significantly larger than those of quasars, as predicted due to simple geometric projection. Recently, this test of the simplest prediction of orientation-based models has been revisited with larger samples that cover wider ranges of fundamental properties—and no clear difference in projected sizes of radio structure is found. Cast solely in terms of viewing angle effects, these results provide convincing evidence that unification of these objects solely through orientation fails. However, it is possible that conflicting results regarding the role orientation plays in our view of radio sources simply result from insufficient sampling of their intrinsic size distribution. We test this possibility using Monte Carlo simulations constrained by real sample sizes and properties. We develop models for the real intrinsic size distribution of radio sources, simulate observations by randomly sampling intrinsic sizes and viewing angles, and analyze how likely each sample is to support or dispute unification by orientation. We find that, while it is possible to reconcile conflicting results purely within a simple, orientation-based framework, it is very unlikely. We analyze the effects that sample size, relative numbers of radio galaxies and quasars, the critical angle that separates the two subclasses, and the shape of the intrinsic size distribution have on this type of test.
Electromagnetic properties of spin-3/2 Majorana particles

The structure of the electromagnetic vertex function of spin-3/2 particles is analyzed in a general way, for the diagonal and off-diagonal couplings, of charged as well as neutral particles including the case of self-conjugate (Majorana) particles. The restrictions imposed by common principles such as electromagnetic gauge invariance and hermiticity are studied, and the implications due to the discrete space-time symmetries or the Majorana condition are deduced when they are applicable. In some cases certain features of the vertex function are analogous to the known ones for the spin-1/2 or spin-1 particles, but we find and discuss other particular properties which are related to the spin-3/2 Rarita-Schwinger representation. For example, in the diagonal Majorana case, the vertex function can contain a term of the form $\gamma_\mu\gamma_5$, which resembles the axial charge radius term for Majorana neutrinos, plus another one that resembles the vertex function for self-conjugate spin-1 particles, but with the particularity that the two terms may not appear independently of each other, but instead with a specific relative coefficient. In essence this is due to the requirement that the vertex function does not mix the genuine spin-3/2 degrees of freedom with the spurious spin-1/2 components of the Rarita-Schwinger representation. The analogous results for the other cases (off-diagonal and charged couplings) are discussed as well.
MOKA: a new tool for Strong Lensing Studies

Strong gravitational lensing is a powerful tool that can be used to probe the matter distribution in the cores of massive dark matter haloes. Recent and ongoing analyses of galaxy cluster surveys – such as the Massive Cluster Survey (MACS), the Canada–France–Hawaii Telescope Legacy Survey (CFHTLS), the Sloan Digital Sky Survey (SDSS), the Sloan Giant Arcs Survey (SGAS), the Cluster Lensing and Supernova Survey with Hubble (CLASH) and the Local Cluster Substructure Survey (LoCuSS) – have addressed the question of the nature of the dark matter distribution in clusters. Using N-body simulations of cold dark matter haloes, it is consistently found that haloes should be characterized by a concentration–mass relation, which decreases monotonically with halo mass, and that they should be populated by a large amount of substructures, representing the cores of accreted progenitor halos. It is important for our understanding of dark matter that we test these predictions. We present moka, a new algorithm for simulating the gravitational lensing signal from cluster-sized haloes. It implements the most recent results from numerical simulations to create realistic cluster-scale lenses with properties independent of numerical resolution. We perform systematic studies of the strong lensing cross-section as a function of halo structures. We find that the strong lensing cross-sections depend most strongly on the concentration and on the inner slope of the density profile of a halo, followed in order of importance by halo triaxiality and the presence of a bright central galaxy.
X-RAY BINARY EVOLUTION ACROSS COSMIC TIME

High-redshift galaxies permit the study of the formation and evolution of X-ray binary (XRB) populations on cosmological timescales, probing a wide range of metallicities and star formation rates (SFRs). In this paper, we present results from a large-scale population synthesis study that models the XRB populations from the first galaxies of the universe until today. We use as input to our modeling the Millennium II cosmological simulation and the updated semi-analytic galaxy catalog by Guo et al. to self-consistently account for the star formation history and metallicity evolution of the universe. Our modeling, which is constrained by the observed X-ray properties of local galaxies, gives predictions about the global scaling of emission from XRB populations with properties such as SFR and stellar mass, and the evolution of these relations with redshift. Our simulations show that the X-ray luminosity density (X-ray luminosity per unit volume) from XRBs in our universe today is dominated by low-mass XRBs, and it is only at z ≳ 2.5 that high-mass XRBs become dominant. We also find that there is a delay of ∼1.1 Gyr between the peak of X-ray emissivity from low-mass XRBs (at z ∼ 2.1) and the peak of SFR density (at z ∼ 3.1). The peak of the X-ray luminosity from high-mass XRBs (at z ∼ 3.9) happens ∼0.8 Gyr before the peak of the SFR density, which is due to the metallicity evolution of the universe.
Cool Gas in High-Redshift Galaxies

Over the past decade, observations of the cool interstellar medium (ISM) in distant galaxies via molecular and atomic fine structure line (FSL) emission have gone from a curious look into a few extreme, rare objects to a mainstream tool for studying galaxy formation out to the highest redshifts. Molecular gas has been observed in close to 200 galaxies at z > 1, including numerous AGN host-galaxies out to z ∼ 7, highly star-forming submillimeter galaxies, and increasing samples of main-sequence color-selected star-forming galaxies at z ∼ 1.5 to 2.5. Studies have moved well beyond simple detections to dynamical imaging at kiloparsec-scale resolution and multiline, multispecies studies that determine the physical conditions in the ISM in early galaxies. Observations of the cool gas are the required complement to studies of the stellar density and star-formation history of the Universe as they reveal the phase of the ISM that immediately precedes star formation in galaxies. Current observations suggest that t.
POPULATION I WOLF-RAYET RUNAWAY STARS: THE CASE OF WR124 AND ITS EXPANDING NEBULA M1–67

In 1997 and 2008 we used the WFPC2 camera on board the Hubble Space Telescope to obtain two sets of narrow-band Hα images of the runaway Wolf-Rayet (WR) star WR 124 surrounded by its nebula M1–67. This two-epoch imaging provides an expansion parallax and thus a practically assumption-free geometric distance to the nebula, d = 3.35 ± 0.67 kpc. Combined with the global velocity distribution in the ejected nebula, this confirms the extreme runaway status of WR 124. WR stars embedded within such ejection nebulae at the point of core collapse would produce different supernova characteristics from those expected for stars surrounded by wind-filled cavities. In galaxies with extremely low ambient metallicity, Z ⩽ 10−3Z☉, γ-ray bursts originating from fast-moving runaway WR stars may produce afterglows which appear to be coming from regions with a relatively homogeneous circumburst medium.
The X-ray spectrum of the newly discovered accreting millisecond pulsar IGR J17511−3057

We report on a 70 ks XMM–Newton Target of Opportunity (ToO) observation of the newly discovered accreting millisecond pulsar, IGR J17511−3057. Pulsations at 244.833 9512(1) Hz are observed throughout the outburst with an rms-pulsed fraction of 14.4(3) per cent. Pulsations have been used to derive a precise solution for the Porb= 12 487.51(2) s binary system. The measured mass function indicates a main-sequence companion star with a mass between 0.15 and 0.44 M⊙. The XMM–Newton 0.5–11 keV spectrum of IGR J17511−3057 can be modelled by at least three components, which we interpret, from the softest to the hardest, as multi-coloured disc emission, thermal emission from the neutron star surface and thermal Comptonization emission. Spectral fit of the XMM–Newton data and of the Rossi X-ray Timing Explorer (RXTE) data, taken in a simultaneous temporal window, well constrain the Comptonization parameters: the electron temperature, kTe= 51+6−4 keV, is rather high, while the optical depth (τ= 1.34+0.03−0.06) is moderate. The energy dependence of the pulsed fraction supports the interpretation of the cooler thermal component as coming from the accretion disc, and indicates that the Comptonizing plasma surrounds the hot spots on the neutron star surface, which in turn provides the seed photons. Signatures of reflection, such as a broadened iron Kα emission line and a Compton hump at ∼30 keV, are also detected. We derive from the smearing of the reflection component an inner disc radius of ≳40 km for a 1.4 M⊙ neutron star, and an inclination between 38° and 68°. XMM–Newton also observed two type I X-ray bursts, whose fluence and recurrence time suggest that the bursts are ignited in a nearly pure helium environment. No photospheric radius expansion is observed, thus leading to an upper limit on the distance to the source of 10 kpc. A lower limit of 6.5 kpc can be also set if it is assumed that emission during the decaying part of the burst involves the whole neutron star surface. Pulsations are observed during the burst decay with an amplitude similar to the persistent emission. They are also compatible with being phase locked to pre-burst pulsations, suggesting that the location on the neutron star surface where they are formed does not change much during bursts.
X-RAY BINARIES AND STAR CLUSTERS IN THE ANTENNAE: OPTICAL CLUSTER COUNTERPARTS

We compare the locations of 82 X-ray binaries (XRBs) detected in the merging Antennae galaxies by Zezas et al., based on observations taken with the Chandra X-Ray Observatory, with a catalog of optically selected star clusters presented by Whitmore et al., based on observations taken with the Hubble Space Telescope. Within the 2σ positional uncertainty of ≈0. ″8, we find 22 XRBs are coincident with star clusters, where only two to three chance coincidences are expected. The ages of the clusters were estimated by comparing their UBVI, Hα colors with predictions from stellar evolutionary models. We find that 14 of the 22 coincident XRBs (64%) are hosted by star clusters with ages of ≈6 Myr or less. All of the very young host clusters are fairly massive and have M ≳ 3 × 104 M☉, with many having masses M ≈ 105 M☉. Five of the XRBs are hosted by young clusters with ages τ ≈ 10–100 Myr, while three are hosted by intermediate-age clusters with τ ≈ 100–300 Myr. Based on the results from recent N-body simulations, which suggest that black holes are far more likely to be retained within their parent clusters than neutron stars, we suggest that our sample consists primarily of black hole binaries with different ages.
Topical Treatment of Second-Degree Burn Wounds with Lactobacillus plantarum Supernatant: Phase I Trial

Background & Objective: A burn wound is sterile immediately after injury, but opportunistic bacteria colonize the wound within 48 to 72 hours after the burn, causing delayed or failed burn wound healing. In addition, the presence of multidrug-resistant (MDR) pathogens doubles the treatment problems. Lactobacillus plantarum (L. plantarum) is a well-known antibacterial and healing agent that could be used topically to treat burn wounds. Case Series Presentation: This clinical trial study (Case Series) was performed on 20 patients with deep second-degree burns. Patients had bilateral wounds; the wound on one side of the body was considered as control (treated with silver sulfadiazine) and the other side of the body as treatment (treated with bacteria-free supernatants (BFS) of L. plantarum). The wounds were evaluated by microbial assessments and assessments related to healing. Pseudomonas aeruginosa, Klebsiella pneumonia, and Staphylococcus aureus were isolated from 4 (22.2%), 0%, and 2 (11.1%) of wounds treated with L. plantarum on the fifth day of the treatment, respectively. Furthermore, 12 (66.7%) of wounds treated with L. plantarum were free from bacteria. The need for skin grafting was the same in both treatment and control groups, but graft rejection in the group treated with L. plantarum was (0%) (P=0.02). Conclusion: Regarding eliminating or reducing infection and wound healing, bacteria-free supernatants of L. plantarum can be considered a possible topical treatment option in the case of second-degree burn wounds.
Effects of foreign direct investment on trade-based money laundering: The case of Vietnam

Abstract This paper investigates the effect of foreign direct investment (FDI) flows on trade-based money laundering (TBML). Trade misinvoicing, including export under-invoicing and import over-invoicing, is a proxy of TBML. Using an extended gravity model in trade with data from Vietnam from 2000 to 2019, our empirical results show that FDI flows are positively associated with TBML, which supports the FDI-fueled capital flight hypothesis. Departing from the current literature, we show that this effect becomes pronounced for export under-invoicing when Vietnam trades with low-income and lower-middle-income countries. Moreover, this effect is negatively moderated by government effectiveness and economic freedom. Our findings are appealing because Vietnam is an export-oriented, FDI-dependent economy; however, trade misinvoicing may offset the contribution of FDI to Vietnam’s economic development. Hence, our findings suggest a number of policy implications for policymakers in attracting FDI.