Miracle-dz/UniFAR-FTUs huggingface dataset:
SDSS J074511.56+194926.5: DISCOVERY OF A METAL-RICH AND TIDALLY DISTORTED EXTREMELY LOW MASS WHITE DWARF

We present the discovery of an unusual, tidally distorted extremely low mass white dwarf (WD) with nearly solar metallicity. Radial velocity measurements confirm that this is a compact binary with an orbital period of 2.6975 hr and a velocity semi-amplitude of K = 108.7 km s−1. Analysis of the hydrogen Balmer lines yields an effective temperature of Teff = 8380 K and a surface gravity of log g = 6.21 that in turn indicate a mass of M = 0.16 M☉ and a cooling age of 4.2 Gyr. In addition, a detailed analysis of the observed metal lines yields abundances of log (Mg/H) = −3.90, log (Ca/H) = −5.80, log (Ti/H) = −6.10, log (Cr/H) = −5.60, and log (Fe/H) = −4.50, similar to the sun. We see no evidence of a debris disk from which these metals would be accreted, though the possibility cannot entirely be ruled out. Other potential mechanisms to explain the presence of heavy elements are discussed. Finally, we expect this system to ultimately undergo unstable mass transfer and merge to form a ∼0.3–0.6 M☉ WD in a few Gyr.
A Novel Method to Identify AGNs Based on Emission Line Excess and the Nature of Low-luminosity AGNs in the Sloan Digital Sky Survey: II - Nature of Low-luminosity AGNs

We develop a novel method to identify active galactic nuclei (AGNs) and study the nature of low-luminosity AGNs in the Sloan Digital Sky Survey. This is the second part of a series of papers and we study the correlations between the AGN activities and host galaxy properties. Based on a sample of AGNs identified with the new method developed in Paper-I, we find that AGNs typically show extinction of tau_V=1.2 and they exhibit a wide range of ionization levels. The latter finding motivates us to use [OII]+[OIII] luminosity as an indicator of AGN power. We find that AGNs are preferentially located in massive, red, early-type galaxies. By carefully taking into account a selection bias of the Oxygen-excess method, we show that strong AGNs are located in actively star forming galaxies and rapidly growing super-massive black holes are located in rapidly growing galaxies, which clearly shows the co-evolution of super-massive black holes and the host galaxies. This is a surprising phenomenon given that the growths of black holes and host galaxies occur at very different physical scales. Interestingly, the AGN power does not strongly correlate with the host galaxy mass. It seems that mass works like a 'switch' to activate AGNs. The absence of AGNs in low-mass galaxies might be due the absence of super-massive black holes in those galaxies, but a dedicated observation of nuclear region of nearby low-mass galaxies would be necessarily to obtain deeper insights into it.
THE DISSECTION OF ABELL 2744: A RICH CLUSTER GROWING THROUGH MAJOR AND MINOR MERGERS

New Chandra X-ray data and extensive optical spectroscopy, obtained with AAOmega on the 3.9 m Anglo-Australian Telescope, are used to study the complex merger taking place in the galaxy cluster Abell 2744. Combining our spectra with data from the literature provides a catalog of 1237 redshifts for extragalactic objects lying within 15′ of the cluster center. From these, we confirm 343 cluster members projected within 3 Mpc of the cluster center. Combining positions and velocities, we identify two major substructures, corresponding to the remnants of two major subclusters. The new data are consistent with a post-core-passage, major merger taking place along an axis that is tilted well out of the plane of the sky, together with an interloping minor merger. Supporting this interpretation, the new X-ray data reveal enriched, low entropy gas from the core of the approaching, major subcluster, lying ∼2′ north of the cluster center, and a shock front to the southeast of the previously known bright, compact core associated with the receding subcluster. The X-ray morphology of the compact core is consistent with a Bullet-like cluster viewed from within ∼45° of the merger axis. An X-ray peak ∼3′ northwest of the cluster center, with an associated cold front to the northeast and a trail of low entropy gas to the south, is interpreted as the remnant of an interloping minor merger taking place roughly in the plane of the sky. We infer approximate paths for the three merging components.
Enhancing vitamin B 12 content in co-fermented soy-milk via a Lotka Volterra model

: Soybean products are popular because of its taste, digestibility, and health benefits. However, soybean lacks vitamin, mainly the low water-soluble vitamin B 12 . This study investigated the effects of fermentation conditions on the synthesis of vitamin B 12 , production of metabolites, and growth of Lactobacillus reuteri and Propionibacterium shermainii in fermented soy-milk. A Lotka Volterra model was successfully employed to describe the competition relationship between the two microorganisms under various fermentation conditions. A quadratic function between the ratio of interaction coefficients and vitamin B 12 content was found. Higher vitamin B 12 in soy-milk can be produced when the ratio of interaction coefficients approach to one. Compared with other fermented soybean products, fermented soy-milk contains more acetate, ethanol, and propionic acid. This study successfully demonstrated a mathematical model to enhance soy-milk vitamin B 12 production.
The Blue Straggler Population of the Globular Cluster M5

By combining high-resolution HST and wide-field ground-based observations, in ultraviolet and optical bands, we study the blue straggler star (BSS) population of the galactic globular cluster M5 (NGC 5904) from its very central regions up to its periphery. The BSS distribution is highly peaked in the cluster center, decreases at intermediate radii and rises again outward. Such a bimodal distribution is similar to those previously observed in other globular clusters (M3, 47 Tucanae, NGC 6752). As for these clusters, dynamical simulations suggest that, while the majority of BSSs in M5 could be originated by stellar collisions, a significant fraction (20%-40%) of BSSs generated by mass transfer processes in primordial binaries is required to reproduce the observed radial distribution. A candidate BSS has been detected beyond the cluster tidal radius. If confirmed, this could represent an interesting case of an "evaporating" BSS.
Spatial correlations in nonequilibrium reaction-diffusion problems by the Gillespie algorithm

We present a study of the spatial correlation functions of a one-dimensional reaction-diffusion system in both equilibrium and out of equilibrium. For the numerical simulations we have employed the Gillespie algorithm dividing the system into cells to treat diffusion as a chemical process between adjacent cells. We find that the spatial correlations are spatially short ranged in equilibrium but become long ranged in nonequilibrium. These results are in good agreement with theoretical predictions from fluctuating hydrodynamics for a one-dimensional system and periodic boundary conditions.
Hodge numbers and Hodge structures for Calabi-Yau categories of dimension three

Let $\mathcal{A}$ be a smooth proper $\mathbb{C}$-linear triangulated category Calabi-Yau of dimension 3 endowed with a (non-trivial) rank function. Using the homological unit of A with respect to the given rank function, we define Hodge numbers for $\mathcal{A}$. If the classes of unitary objects generate the complexified numerical $\mathrm{K}$-theory of $\mathcal{A}$ (hypothesis satisfied for many examples of smooth proper Calabi-Yau categories of dimension 3), it is proved that these numbers are independent of the chosen rank function : they are intrinsic invariants of the triangulated category $\mathcal{A}$. In the special case where $\mathcal{A}$ is a semi-orthogonal component of the derived category of a smooth complex projective variety and the homological unit of $\mathcal{A}$ is $\mathbb{C} ⊕ \mathbb{C}[3]$ (that is $\mathcal{A}$ is strict Calabi-Yau with respect to the rank function), we define a Hodge structure on the Hochschild homology of $\mathcal{A}$. The dimensions of the Hodge spaces of this structure are the Hodge numbers aforementioned. Finally, we give some numerical applications toward the Homological Mirror Symmetry conjecture for cubic sevenfolds and double quartic fivefolds.
The structure of the jet in Cyg X-1 inferred from orbital modulation of the radio emission

We study free–free absorption of radio emission by winds of massive stars. We derive formulae for the optical depth through the wind measured from a point of emission along a jet, taking into account Compton and photoionization heating and Compton, recombination, line and advection cooling. We apply the developed formalism to radio monitoring data for Cyg X-1, which allows us to obtain strong constraints on the structure of its inner jet. With the data at 15 GHz, and taking into account an anisotropy of the stellar wind in Cyg X-1, we estimate the location of the peak of that emission along the jet at about one orbital separation, i.e. ∼3 × 1012 cm. Given a previous determination of the turnover frequency in Cyg X-1, this implies the location of the base of the jet at ∼103 gravitational radii. We also obtain corresponding results at 8.3 and 2.25 GHz, which roughly follow the standard conical partially self-absorbed jet model. Furthermore, we find that the level of the orbital modulation depends on the radio flux, with the modulation being substantially stronger when the radio flux is lower. This is explained by the height of the radio emission along the jet decreasing with the decreasing radio flux, as predicted by jet models. Based on the finding of the flux-dependent orbital modulation, we are able to estimate a range of the possible changes of the form of the radio/X-ray correlation in Cyg X-1 due to free–free absorption. We also derive predictions for the orbital modulation and flux attenuation at frequencies beyond the 2.25–15 GHz range.
Effects of Caffeine on Human Body

Throughout the beyond a decade, Food Rule Experts have deduced that caffeine usage isn't risky at whatever point consumed at levels of 200 mg at a time (around 2½ cups of coffee) or 400 mg everyday (around 5 cups of coffee). Moreover, caffeine has various positive exercises on the frontal cortex. It can augment availability and success, help obsession, further foster perspective likewise, limit distress. Caffeine could disturb rest, regardless, simply in fragile individuals. It could raise anxiety in a little subset of particularly fragile people. Caffeine does not seem to provoke dependence, yet a minority of people experience withdrawal secondary effects. Caffeine can potentiate the effect of standard torment alleviating drugs in cerebral agony and migraine. Well established coffee/caffeine usage has been connected with expectation of mental disintegration, and diminished risk of making stroke, Parkinson's ailment and Alzheimer's ailment. Its usage does not seem to influence seizure occasion. Thusly, everyday coffee and caffeine confirmation can be significant for a strong changed diet; its use does not ought to be ended in elderly people.
The effect of internal control quality on real and accrual‑based earnings management: evidence

This paper examines the effect of internal control (IC) quality, measured by IC weakness disclosures, on the quality of financial statements’ information, measured by real and accrual-based earnings management. The sample consists of 686 firm-year observations of French non-financial companies listed in the SBF 120 index during the period between 2012 and 2018. Using ordinary least squares (OLS) and generalized method of moments (GMM) regression, our empirical results indicate that IC weakness disclosures are positively and significantly related to real activities manipulation and negatively associated with discretionary accruals. This provides empirical evidence that a good system of IC reduces accrual-based earnings management activities and improves the reliability of financial statements; however, it cannot control real earnings management (REM). The research findings are of practical interest not only to financial analysts, auditors, and investors—guiding them to pay attention to REM activities in case of disclosures of IC weaknesses—but also to regulators, who may consider additional disclosure requirements when reporting material IC weaknesses and designing policies that could help in reducing REM practices.
Persistent homology and Floer-Novikov theory

We construct "barcodes" for the chain complexes over Novikov rings that arise in Novikov's Morse theory for closed one-forms and in Floer theory on not-necessarily-monotone symplectic manifolds. In the case of classical Morse theory these coincide with the barcodes familiar from persistent homology. Our barcodes completely characterize the filtered chain homotopy type of the chain complex; in particular they subsume in a natural way previous filtered Floer-theoretic invariants such as boundary depth and torsion exponents, and also reflect information about spectral invariants. We moreover prove a continuity result which is a natural analogue both of the classical bottleneck stability theorem in persistent homology and of standard continuity results for spectral invariants, and we use this to prove a C^0-robustness result for the fixed points of Hamiltonian diffeomorphisms. Our approach, which is rather different from the standard methods of persistent homology, is based on a non-Archimedean singular value decomposition for the boundary operator of the chain complex.
Weak Poincaré inequalities for convergence rate of degenerate diffusion processes

For a contraction $C_0$-semigroup on a separable Hilbert space, the decay rate is estimated by using the weak Poincar\'e inequalities for the symmetric and anti-symmetric part of the generator. As applications, non-exponential convergence rate is characterized for a class of degenerate diffusion processes, so that the study of hypocoercivity is extended. Concrete examples are presented.
TOWARD A DETERMINISTIC MODEL OF PLANETARY FORMATION. VI. DYNAMICAL INTERACTION AND COAGULATION OF MULTIPLE ROCKY EMBRYOS AND SUPER-EARTH SYSTEMS AROUND SOLAR-TYPE STARS

Radial velocity and transit surveys indicate that solar-type stars bear super-Earths, with masses up to ∼20 M⊕ and periods up to a few months, that are more common than those with Jupiter-mass gas giants. In many cases, these super-Earths are members of multiple-planet systems in which their mutual dynamical interaction has influenced their formation and evolution. In this paper, we modify an existing numerical population synthesis scheme to take into account protoplanetary embryos’ interaction with their evolving natal gaseous disks, as well as their close scatterings and resonant interaction with each other. We show that it is possible for a group of compact embryos to emerge interior to the ice line, grow, migrate, and congregate into closely packed convoys which stall in the proximity of their host stars. After the disk–gas depletion, they undergo orbit crossing, close scattering, and giant impacts to form multiple rocky Earths or super-Earths in non-resonant orbits around ∼0.1 AU with moderate eccentricities of ∼0.01–0.1. We suggest that most refractory super-Earths with periods in the range of a few days to weeks may have formed through this process. These super-Earths differ from Neptune-like ice giants by their compact sizes and lack of a substantial gaseous envelope.
QED spectra in the path integral formalism

Relativistic Hamiltonians, derived from the path integrals, are known to provide a simple and useful formalism for hadrons spectroscopy in QCD. The accuracy of this approach is tested using the QED systems, and the calculated spectrum is shown to reproduce exactly that of the Dirac hydrogen atom, while the Breit-Fermi nonrelativistic expansion is obtained using Foldy-Wouthuizen transformation. Calculated positronium spectrum, including spin-dependent terms, coincides with the standard QED perturbation theory to the considered order O(alpha^s).
The influence of United States monetary policy on the South African economy

: This paper aims to analyse the influence of spillovers into South Africa ’ s economy from shifts in United States of America’s (US) monetary policy. Often changing, the US interest rate is regarded as an important driving force of economic growth in the world, since several developing economies are strongly dependent on the activity of the US dollar and monetary policy. To fulfil the aim of this study, the model specification examines the relationship and interaction between US interest rates and South Africa ’s gross domestic product (GDP), oil prices, all-share index, and bond index. The results from the non-linear autoregressive distributed lag technique employed show that US monetary policy has a negative effect on South Africa ’ s GDP in both the short and long run. The findings show that the impact of shocks caused by changes in US interest rates on South Africa’s GDP is strong but short-lived.
A DEEP SEARCH FOR FAINT GALAXIES ASSOCIATED WITH VERY LOW-REDSHIFT C iv ABSORBERS. II. PROGRAM DESIGN, ABSORPTION-LINE MEASUREMENTS, AND ABSORBER STATISTICS

To investigate the evolution of metal-enriched gas over recent cosmic epochs as well as to characterize the diffuse, ionized, metal-enriched circumgalactic medium, we have conducted a blind survey for C iv absorption systems in 89 QSO sightlines observed with the Hubble Space Telescope Cosmic Origins Spectrograph. We have identified 42 absorbers at z < 0.16, comprising the largest uniform blind sample size to date in this redshift range. Our measurements indicate an increasing C iv absorber number density per comoving path length ( d  / dX ? > = 7.5 ± 1.1) and modestly increasing mass density relative to the critical density of the universe (ΩC iv = 10.0 ± 1.5 × 10−8) from z ∼ 1.5 to the present epoch, consistent with predictions from cosmological hydrodynamical simulations. Furthermore, the data support a functional form for the column density distribution function that deviates from a single power law, also consistent with independent theoretical predictions. As the data also probe heavy element ions in addition to C iv at the same redshifts, we identify, measure, and search for correlations between column densities of these species where components appear to be aligned in velocity. Among these ion–ion correlations, we find evidence for tight correlations between C ii and Si ii, C ii and Si iii, and C iv and Si iv, suggesting that these pairs of species arise in similar ionization conditions. However, the evidence for correlations decreases as the difference in ionization potential increases. Finally, when controlling for observational bias, we find only marginal evidence for a correlation (86.8% likelihood) between the Doppler line width b(C iv) and column density N(C iv).
THE DYNAMICAL STATE OF BRIGHTEST CLUSTER GALAXIES AND THE FORMATION OF CLUSTERS

A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ∼92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz–Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.
Reconstruction of the primordial fluctuation spectrum from the five-year WMAP data by the cosmic inversion method with band-power decorrelation analysis

The primordial curvature fluctuation spectrum is reconstructed by the cosmic inversion method using the five-year Wilkinson Microwave Anisotropy Probe data of the cosmic microwave background temperature anisotropy. We apply the covariance matrix analysis and decompose the reconstructed spectrum into statistically independent band-powers. The statistically significant deviation from a simple power-law spectrum suggested by the analysis of the first-year data is not found in the five-year data except possibly at one point near the border of the wave number domain where accurate reconstruction is possible.
The sulfur depletion problem: upper limits on the H2S2, HS·2, and S2 gas-phase abundances toward the low-mass warm core IRAS 16293-2422

A fraction of the missing sulfur in dense clouds and circumstellar regions could be in the form of three species not yet de- tected in the interstellar medium: H2S2, HS2, and S2 according to experimental simulations performed under astrophysically relevant conditions. These S-S bonded molecules can be formed by the energetic processing of H2S-bearing ice mantles on dust grains, and subsequently desorb to the gas phase. The detection of these species could partially solve the sulfur depletion problem, and would help to improve our knowledge of the poorly known chemistry of sulfur in the interstellar medium. To this purpose we performed dedicated ground-based observations toward the low-mass warm core IRAS16293-2422. Observations in the submillimeter regime were obtained with the APEX 12 m telescope during 15 hours of observation, targeting a wide selection of the predicted rotational transitions of the three molecules. The 1{\sigma} noise rms values were extracted in the spectral regions where the targeted species should have been detected. These values were a factor of 2-7 lower than those reached by previous observations toward the same source, and allowed us to estimate a 1{\sigma} upper limit to their molecular abundances of 8.1E-9 , 1.1E-8 , and 2.9E-7 relative to H2, for H2S2, HS2, and S2, respectively. The upper limit abundances of the three molecules containing the S2 unit are up to two orders of magnitude lower than the H2S abundance in the source, and one order of magnitude lower than the expected abundances from the experimental simulations using ice analogs. Subsequent gas-phase chemistry after desorption could lower the abundances of the three species to undetectable levels in our observations.