Miracle-dz/UniFAR-FTUs huggingface dataset:
BROADBAND OBSERVATIONS OF THE GAMMA-RAY EMITTING NARROW LINE SEYFERT 1 GALAXY SBS 0846+513

We present the results of our broadband study of the γ-ray emitting narrow line Seyfert 1 (NLSy1) galaxy SBS 0846+513 (z = 0.585). This includes multiband flux variations, γ-ray spectral analysis, broadband spectral energy distribution (SED) modeling, and intranight optical variability (INOV) observations carried out over six nights between 2012 November and 2013 March using the 2 m Himalayan Chandra Telescope and the 1.3 m telescope at Devasthal, India. Multiple episodes of flaring activity are seen in the γ-ray light curve of the source which are also reflected in the observations at lower frequencies. A statistically significant curvature is noticed in the seven years averaged γ-ray spectrum, thus indicating its similarity with powerful flat spectrum radio quasars (FSRQs). Modeling the SEDs with a one-zone leptonic emission model hints that the optical UV spectrum is dominated by synchrotron radiation, whereas inverse Compton scattering of broad line region photons reproduces the γ-ray part of the SEDs. The source was found to be variable on all the six nights of optical observations with a variation of ∼0.3 mag within a single night, coinciding with a high γ-ray activity state. The observed large amplitude INOV clearly indicates the presence of a closely aligned beamed relativistic jet in SBS 0846+513. Our broadband study supports the recent claims in literature that γ-ray emitting NLSy1 galaxies are similar to blazars and constitute the low black hole mass counterparts to FSRQs.
Orbit and spin evolution of synchronous binary stars on the main sequence

A set of synchronous equations are derived from a set of non-synchronous equations. The analytical solutions are given by solving the set of differential equations. The results of the evolutionary trend of the spin-orbit interaction are that the semi-major axis gradually shrinks with time; the orbital eccentricity gradually decreases with time until orbital circularization occurs; the orbital period gradually shortens with time and the rotational angular velocity of the primary component gradually speeds up with time before the orbit achieves circularization. The theoretical results are applied to evolution of the orbit and spin of synchronous binary stars Algol A and B that are on the main sequence. The circularization time, lifetime and the evolutionary numerical solutions of orbit and spin when circularization time occurs are estimated for Algol A and B.
DUST AROUND R CORONAE BOREALIS STARS. I. SPITZER/INFRARED SPECTROGRAPH OBSERVATIONS

Spitzer/infrared spectrograph (IRS) spectra from 5 to 37 μm for a complete sample of 31 R Coronae Borealis stars (RCBs) are presented. These spectra are combined with optical and near-infrared photometry of each RCB at maximum light to compile a spectral energy distribution (SED). The SEDs are fitted with blackbody flux distributions and estimates are made of the ratio of the infrared flux from circumstellar dust to the flux emitted by the star. Comparisons for 29 of the 31 stars are made with the Infrared Astronomical Satellite (IRAS) fluxes from three decades earlier: Spitzer and IRAS fluxes at 12 μm and 25 μm are essentially equal for all but a minority of the sample. For this minority, the IRAS to Spitzer flux ratio exceeds a factor of three. The outliers are suggested to be stars where formation of a dust cloud or dust puff is a rare event. A single puff ejected prior to the IRAS observations may have been reobserved by Spitzer as a cooler puff at a greater distance from the RCB. RCBs which experience more frequent optical declines have, in general, a circumstellar environment containing puffs subtending a larger solid angle at the star and a quasi-constant infrared flux. Yet, the estimated subtended solid angles and the blackbody temperatures of the dust show a systematic evolution to lower solid angles and cooler temperatures in the interval between IRAS and Spitzer. Dust emission by these RCBs and those in the LMC is similar in terms of total 24 μm luminosity and [8.0]−[24.0] color index.
Higher-Order Total Directional Variation. Part II: Analysis

We analyse a new class of higher-order anisotropic total variation which is defined for possibly inhomogeneous, smooth elliptic anisotropies. We prove some properties of the associated tensor space, the existence of solutions to a canonically related regularity-fidelity optimization problem, and we prove a decomposition formula for this new criterion which appears to be helpful for the design of numerical schemes as shown in a companion paper.
Validation Parameters of the Magnetic Stirrer Method for Pooled Sample Digestion for Trichinella spp. in Horse Meat Based on Proficiency Tests Results

Meat of horses may be infested with nematodes of the genus Trichinella spp. and can cause serious disease in humans. Rules for the carcasses sampling of species susceptible to Trichinella spp. infection and examination are laid down in Commission Regulation 1375/2015, where the magnetic stirrer method for pooled-sample digestion is recommended (Commission Regulation 1478/2020). All personnel involved in the examination should be properly trained and participate in quality control programs. Proficiency tests (PTs) play a key role in the quality verification process. This paper presents the results of PTs organized for 68 Polish laboratories in 2014–2019. Results were assessed qualitatively at three levels of sample contamination (0, 3, 5 larvae) and quantitatively at one level (5 larvae). The laboratories have achieved the average correct qualitative results 100%, 96.2% and 96.8% for the samples contaminated with 0, 3 and 5 larvae, respectively. In the quantitative evaluation, an average 94.1% of the reported results were correct. The data from PTs enabled us to define, for the first time, validation parameters of the digestion method for the horse meat matrix in a large-scale experiment including: specificity (100%), sensitivity (95.6%), accuracy (97.1%), the limit of detection (LOD) (1.14 ≈ 1) and the limit of quantification (LOQ) (3.42 ≈ 3).
Online assessment in two consequent semesters during COVID-19 pandemic: K-means clustering using data mining approach

BACKGROUND: Education and assessment have changed during the COVID-19 pandemic so that online courses replaced face-to-face classes to observe the social distance. The quality of online assessments conducted during the pandemic is an important subject to be addressed. In this study, the quality of online assessments held in two consecutive semesters was investigated. MATERIALS AND METHODS: One thousand two hundred and sixty-nine multiple-choice online examinations held in the first (n = 535) and second (n = 734) semesters in Birjand University of Medical Sciences during 2020–2021 were examined. Mean, standard deviation, number of questions, skewness, kurtosis, difficulty, and discrimination index of tests were calculated. Data mining was applied using the k-means clustering approach to classify the tests. RESULTS: The mean percentage of answers to all tests was 69.97 ± 19.16, and the number of questions was 34.48 ± 18.75. In two semesters, there was no significant difference between the difficulty of examinations (P = 0.84). However, there was a significant difference in the discrimination index, skewness, and kurtosis of tests (P < 0.001). Moreover, according to the results of the clustering analysis in the first semester, 43% of the tests were very hard, 16% hard, and 7% moderate. In the second semester, 43% were hard, 16% moderate, and 41% easy. CONCLUSION: To evaluate the tests’ quality, calculating difficulty and discrimination indices is not sufficient; many factors can affect the quality of tests. Furthermore, the experience of the first semester had changed characteristics of the second-semester examinations. To enhance the quality of online tests, establishing appropriate rules to hold the examinations and using questions with higher taxonomy are recommended.
CutTools: a program implementing the OPP reduction method to compute one-loop amplitudes

We present a program that implements the OPP reduction method to extract the coefficients of the one-loop scalar integrals from a user defined (sub)-amplitude or Feynman Diagram, as well as the rational terms coming from the 4-dimensional part of the numerator. The rational pieces coming from the -dimensional part of the numerator are treated as an external input, and can be computed with the help of dedicated tree-level like Feynman rules. Possible numerical instabilities are dealt with the help of arbitrary precision routines, that activate only when needed.
The impact of AGN feedback and baryonic cooling on galaxy clusters as gravitational lenses

We investigate the impact of AGN feedback on the gravitational lensing properties of a sample of galaxy clusters with masses in the range 10 14 - 10 15 M , using state-ofthe-art simulations. Adopting a ray-tracing algorithm, we compute the cross-section of giant arcs from clusters simulated with dark-matter only physics (DM), dark matter plus gas with cooling and star formation (CSF), and dark matter plus gas with cooling, star formation and AGN feedback (CSFBH). Once AGN feedback is included, baryonic physics boosts the strong lensing cross-section by much less than previously estimated using clusters simulated with only cooling and star formation. For a cluster with a virial mass of 7:4 10 14 M , inclusion of baryonic physics without feedback can boost the cross-section by as much as a factor of 3, in agreement with previous studies, whereas once AGN feedback is included this maximal gure falls to a factor of 2 at most. Typically, clusters simulated with DM and CSFBH physics have similar crosssections for the production of giant arcs. We also investigate how baryonic physics aects the weak lensing properties of the simulated clusters by tting NFW proles to synthetic weak lensing data sets using a Markov Chain Monte Carlo approach, and by performing non-parametric mass reconstructions. Without the inclusion of AGN feedback, measured concentration parameters can be much larger than those obtained with AGN feedback, which are similar to the dark-matter only case.
Remnants of massive metal-poor stars: Viable engines for ultra-luminous X-ray sources

Massive metal-poor stars might end their life by directly collapsing into massive (≈25–80 M⊙) black holes (BHs). We derive the number of massive BHs (N BH) that are expected to form per galaxy via this mechanism. We select a sample of 66 galaxies with X-ray coverage, measurements of the star formation rate (SFR) and of the metallicity. We find that NBH correlates with the number of observed ultra-luminous X-ray sources (ULXs) per galaxy in this sample. We discuss the dependence of NULX and of NBH on the SFR and on the metallicity (© 2011 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
LIGHT-BENDING SCENARIO FOR ACCRETING BLACK HOLES IN X-RAY POLARIMETRY

We discuss a model of an X-ray illuminating source above an accretion disk of a rotating black hole. Within the so-called lamp-post scheme we compute the expected (observed) polarization properties of the radiation reaching an observer. We explore the dependences on model parameters, employing Monte Carlo radiation transfer computations of the X-ray reflection on the accretion disk and taking general relativity effects into account. In particular, we discuss the role of the black hole spin, of the observer viewing angle, and of the primary X-ray source distance from the black hole. We give several examples of the resulting polarization degree for two types of exemplary objects—active galactic nuclei and Galactic black holes. In order to assess potential observability of the polarization features, we assume the sensitivity of the proposed New Hard X-ray Mission (NHXM). We examine the energy range from several keV to ∼50 keV, so the iron line complex and the Compton hump are included in our model spectra. We find the resultant polarization degree to increase at the higher end of the studied energy band, i.e., at ≳20 keV. Thus, the best results for polarimetry of reflection spectra should be achieved at the Compton hump energy region. We also obtain a higher polarization degree for large spin values of the black hole, small heights of the primary source, and low inclination angles of the observer.
SLOW EVOLUTION OF THE SPECIFIC STAR FORMATION RATE AT z > 2: THE IMPACT OF DUST, EMISSION LINES, AND A RISING STAR FORMATION HISTORY

We measure the evolution of the specific star formation rate (sSFR = SFR/Mstellar) between redshift 4 and 6 to assess the reported “constant” sSFR at z > 2. We derive stellar masses and star formation rates (SFRs) for a large sample of 750 z ∼ 4–6 galaxies in the GOODS-S field by fitting stellar population models to their spectral energy distributions. Dust extinction is derived from the observed UV colors. We evaluate different star formation histories (SFHs, constant and rising with time) and the impact of optical emission lines. The SFR and Mstellar values are insensitive to whether the SFH is constant or rising. The derived sSFR is very similar (within 0.1 dex) in two Mstellar bins centered at 1 and 5 × 109 M☉. The effect of emission lines was, however, quite pronounced. Assuming no contribution from emission lines, the sSFR for galaxies at 5 × 109 M☉ evolves weakly at z > 2 (sSFR(z)∝(1 + z)0.6 ± 0.1), consistent with previous results. When emission lines are included in the rest-frame optical bands, consistent with the observed Infrared Array Camera [3.6] and [4.5] fluxes, the sSFR shows higher values at high redshift following sSFR(z)∝(1 + z)1.0 ± 0.1, i.e., the best-fit evolution shows a sSFR ∼2.3 × higher at z ∼ 6 than at z ∼ 2. This is, however, a substantially weaker trend than that found at z < 2 and even than that expected from current models for z > 2 (sSFR(z)∝(1 + z)2.5). Even accounting for emission lines, the observed sSFR(z) trends at z > 2 are still in tension with theoretical expectations.
Clinico-Biochemical Parameters, Treatment, and Prognostic Indicators of Peritonitis in Buffaloes

Background: The present study aimed to describe clinical findings, hemato-biochemical changes, response to medical treatment, and outcomes for buffaloes suffering from peritonitis. Another objective of this study was to determine the prognosis of the disease. Methods: The study was conducted on 25 buffaloes suffering from peritonitis and presented to the Large Animal Hospital of Guru Angad Dev Veterinary and Animal Science University, Ludhiana, Punjab, India. The buffaloes were subjected to detailed clinical examination. Hematological, biochemical, and peritoneal fluid analysis was carried out along with treatment. Results: Peritonitis was more prevalent in pregnant buffaloes, being septic peritonitis in 60% of cases. The important clinical findings were depression, anorexia, reduced water intake, scanty feces, dehydration, and absence of rumen motility. The hematological findings were hemoconcentration, left shift, and toxic changes in neutrophils. Biochemical analysis revealed increased total bilirubin, AST, ALP, GGT, glucose, triglycerides, BUN, creatinine, lactate, fibrinogen, and rumen chloride, whereas albumin, fibrinogen ratio, potassium, chloride, calcium, and phosphorus were decreased. Abnormal peritoneal fluid changes were altered physical parameters and the presence of degenerated neutrophils, bacteria, and gut contents. Nucleated cell count and total peritoneal fluid protein were not reliable indicators of peritonitis. The absence of rumen motility, marked left shift, toxic changes in neutrophils, higher BUN, lower potassium (≤3.6 mmol/L), and unfavorable peritoneal fluid changes were the negative prognostic signs. Treatment with broad-spectrum antibiotics and supportive therapy led to a recovery in about 50 percent of cases, with diffuse peritonitis cases being unresponsive. Long time survival rate was good, and there was no recurrence. Conclusion: The prognosis of peritonitis in buffaloes has to be precisely assessed on the basis of clinical, hemato-biochemical, and peritoneal fluid alterations. Standard classification of transudate and exudate did not apply in the majority of buffaloes with peritonitis.
Herpetological Assemblages in Tropical Forests of the Taguibo Watershed, Butuan City, Eastern Mindanao, Philippines

Tropical watershed ecosystems support heterogeneous habitats and diverse non-human species assemblages, together providing ecosystem services to humans. Amphibians and reptiles are recognized as sensitive indicators of ecosystem “health,” related to beneficial services (provisional, regulating, cultural, structural, functional) human societies receive from terrestrial watersheds. The Taguibo Watershed supplies fresh drinking water to Butuan City in the Caraga Region of northeast Mindanao Island. However, very little is known about the herpetofauna of the area. Here, we synthesize biodiversity data from historical (1971, 1979) and recent (2013, 2017) herpetological surveys from the region. We utilize specimen-associated occurrence records and natural history information to produce a species inventory, analyze their habitat utilization, and characterize diversity metrics to describe herpetological communities of the watershed – resulting in 44 species (27 new records). A number of historically-documented species persist, having partitioned riparian and terrestrial habitat types in dipterocarp and secondary-growth forests of Taguibo. Reptiles exhibit little overlap in the use of microhabitats – in contrast to amphibians, which exhibit either unique or frequently shared microhabitat substrates. In terrestrial microhabitats (not immediately associated with water), many newly-recorded reptiles and amphibians (particularly, of the genus Platymantis) partition space predictably – either occupying a single microhabitat or, in one species (a pit viper, Tropidolaemus subannulatus), two microhabitats. We anticipate that our initial characterization of Taguibo’s herpetofauna may serve as a baseline to promote further research and facilitate conservation initiatives. We emphasize the importance of primary sources – field-based surveys and re-surveys – and open-access biodiversity data served via online platforms that provide live, transparent access to original, unaltered data. Anthropogenic threats involving economic-driven activities present a need for field-based research in support of watershed management. Periodic, survey, and re-survey studies – continuously updating earlier work – are the most reliable, repeatable, and publicly-transparent use of biodiversity survey data in support of societal benefits and ecosystem services.
The effect of inhomogeneities on the distance to the last scattering surface and the accuracy of the CMB analysis

The standard analysis of the CMB data assumes that the distance to the last scattering surface can be calculated using the distance-redshift relation as in the Friedmann model. However, in the inhomogeneous universe, even if δρ = 0, the distance relation is not the same as in the unperturbed universe. This can be of serious consequences as a change of distance affects the mapping of CMB temperature fluctuations into the angular power spectrum Cl. In addition, if the change of distance is relatively uniform no new temperature fluctuations are generated. It is therefore a different effect than the lensing or ISW effects which introduce additional CMB anisotropies. This paper shows that the accuracy of the CMB analysis can be impaired by the accuracy of calculation of the distance within the cosmological models. Since this effect has not been fully explored before, to test how the inhomogeneities affect the distance-redshift relation, several methods are examined: the Dyer-Roeder relation, lensing approximation, and non-linear Swiss-Cheese model. In all cases, the distance to the last scattering surface is different than when homogeneity is assumed. The difference can be as low as 1% and as high as 80%. An usual change of the distance is around 20–30%. Since the distance to the last scattering surface is set by the position of the CMB peaks, in order to have a good fit, the distance needs to be adjusted. After correcting the distance, the cosmological parameters change. Therefore, a not properly estimated distance to the last scattering surface can be a major source of systematics. This paper shows that if inhomogeneities are taken into account when calculating the distance then models with positive spatial curvature and with ΩΛ ~ 0.8−0.9 are preferred.
Isotopic fractionation of carbon, deuterium and nitrogen : a full chemical study

Context. The increased sensitivity and high spectral resolution of millimeter telescopes allow the detection of an increasing number of isotopically substituted molecules in the interstellar medium. The 14N/ 15N ratio is difficult to measure directly for carbon containing molecules. Aims. We want to check the underlying hypothesis that the 13C/ 12C ratio of nitriles and isonitriles is equal to the elemental value via a chemical time dependent gas phase chemical model. Methods. We have built a chemical network containing D, 13C and 15N molecular species after a careful check of the possible fractionation reactions at work in the gas phase. Results. Model results obtained for 2 different physical conditions corresponding respectively to a moderately dense cloud in an early evolutionary stage and a dense depleted pre-stellar core tend to show that ammonia and its singly deuterated form are somewhat enriched in 15N, in agreement with observations. The 14N/ 15N ratio in N2H+ is found to be close to the elemental value, in contrast to previous models which obtain a significant enrichment, as we found that the fractionation reaction between 15N and N2H+ has a barrier in the entrance channel. The large values of the N2H+/15NNH+ and N2H+/ N15NH+ ratios derived in L1544 cannot be reproduced in our model. Finally we find that nitriles and isonitriles are in fact significantly depleted in 13C, questioning previous interpretations of observed C15N, HC15N and H15NC abundances from 13C containing isotopologues.
Evaluation of the RIKEN Post-K Processor Simulator

For the purpose of developing applications for Post-K at an early stage, RIKEN has developed a post-K processor simulator. This simulator is based on the general-purpose processor simulator gem5. It does not simulate the actual hardware of a post-K processor. However, we believe that sufficient simulation accuracy can be obtained since it simulates the instruction pipeline of out-of-order execution with cycle-level accuracy along with performing detailed parameter tuning of out-of-order resources and function expansion of cache/memory hierarchy. In this simulator, we aim to estimate the execution cycles of one node application on a post-K processor with accuracy that enables relative evaluation and application tuning. In this paper, we show the details of the implementation of this simulator and verify its accuracy compared with that of a post-K test chip.