Miracle-dz/UniFAR-FTUs huggingface dataset:
NEUTRINO PAIR ANNIHILATION IN COLLAPSARS: A RAY-TRACING METHOD IN SPECIAL RELATIVITY

We develop a numerical scheme and code for estimating the energy and momentum transfer via neutrino pair annihilation , bearing in mind the application to the collapsar models of gamma-ray bursts (GRBs). To calculate the neutrino flux illuminated from the accretion disk, we perform a ray-tracing calculation in the framework of special relativity. The numerical accuracy of the developed code is certified by several tests, in which we show comparisons with the corresponding analytical solutions. Using hydrodynamical data in our collapsar simulation, we estimate the annihilation rates in a post-processing manner. We show that the neutrino energy deposition and momentum transfers are strongest near the inner edge of the accretion disk. The beaming effects of special relativity are found to change the annihilation rates by several factors in the polar funnel region. After the accretion disk settles into a stationary state (typically later than ∼9 s from the onset of gravitational collapse), we find that the neutrino-heating timescale in the vicinity of the polar funnel (≲80 km) can become shorter than the hydrodynamical timescale, indicating that the neutrino-heated outflows can be launched there. We point out that the momentum transfer can play an important role as the energy deposition for the efficient acceleration of neutrino-driven outflows. Our results suggest that the neutrino pair annihilation has a potential importance equal to the conventional magnetohydrodynamic mechanism for igniting the GRB fireballs.
The evolution of the mass-size relation for early type galaxies from z 1 to the present: dependence on environment, mass-range and detailed morphology

We study the dependence of the galaxy size evolution on morphology, stellar mass and large-scale environment for a sample of 298 group and 384 field quiescent early-type galaxies from the COSMOS survey, selected from z similar to 1 to the present, and with masses log(M/M-circle dot) \textgreater 10.5. From a detailed morphological analysis we infer that similar to 80 per cent of passive galaxies with mass log(M/M-circle dot) \textgreater 10.5 have an early-type morphology and that this fraction does not evolve over the last 6 Gyr. However, the relative abundance of lenticular and elliptical galaxies depends on stellar mass. Elliptical galaxies dominate only at the very high mass end -log(M/M-circle dot) \textgreater 11 - while S0 galaxies dominate at lower stellar masses -10.5 \textless log(M/M-circle dot) \textless 11. The galaxy size growth depends on galaxy mass range and early-type galaxy morphology, e.g. elliptical galaxies evolve differently than lenticular galaxies. At the low-mass end -10.5 \textless log(M/M-circle dot) \textless 11 - ellipticals do not show strong size growth from z similar to 1 to the present (10 to 30 per cent depending on the morphological classification). On the other end, massive ellipticals -log(M/M-circle dot) \textgreater 11.2 - approximately doubled their size. Interestingly, lenticular galaxies display different behaviour: they appear more compact on average and they do show a size growth of similar to 60 per cent since z = 1 independent of stellar mass range. We compare our results with state-of-the art semi-analytic models. While major and minor mergers can account for most of the galaxy size growth, we find that with present data and the theoretical uncertainties in the modelling we cannot state clear evidence favouring either merger or mass-loss via quasar and/or stellar winds as the primary mechanism driving the evolution. The galaxy mass-size relation and size growth do not depend on environment in the halo mass range explored in this work (field to group mass log(M-h/M-circle dot) \textless 14), i.e. group and field galaxies follow the same trends. At low redshift, where we examine both Sloan Digital Sky Survey and COSMOS groups, this result is at variance with predictions from some current hierarchical models that show a clear dependence of size growth on halo mass for massive ellipticals (log(M-*/M-circle dot) \textgreater 11.2). In future work, we will analyse in detail if this result is specific of the observations and model used in this work. Brightest Cluster Galaxies (BCG) and satellite galaxies lie on the same mass-size relation, at variance with predictions from hierarchical models, which predict that BCGs should have larger sizes than satellites because they experience more mergers in groups over the halo mass range probed.
Evaluation of Immunogenicity to Three Doses of the SARS-CoV-2 BNT162b2 mRNA Vaccine in Lung Transplant Patients

The aim of the study was to explore the humoral and T-cell response in lung transplant (LuT) patients. Two-time points were considered, before (T0) and after (Tpost) the third dose of the BNT162b2 mRNA vaccine, comparing LuT with healthy donors (HD). LuT patients showed a lower serologic response against SARS-CoV-2 compared with HD at both time-points (p = 0.0001 and p = 0.0011, respectively). A lower percentage of IFNγ+orIL2+orTNFα+CD4+ and CD8+ T-cells LuT patients was observed in LuT patients compared with HD at T0 (CD4+: p = 0.0001; CD8+: p = 0.0005) and Tpost (CD4+: p = 0.0028; CD8+: p = 0.0114), as well as in the percentage of IFNγ+IL2+TNFα+CD4+ T-cells (T0: p = 0.0247; Tpost: p = 0.0367). Finally, at Tpost, a lower percentage of IFNγ+IL2+TNFα+ CD8+ T-cells in LuT patients compared with HD was found (p = 0.0147). LuT patients were stratified according to the lowest cut-off value for the detection of a humoral response (4.81 BAU/mL) at T0, into responder (R) and non-responder (NR) groups. In the R group, no differences in the percentage of IFNγ+or IL2+orTNFα+ and IFNγ+IL2+TNFα+CD4+ and CD8+ T-cells compared with HD at both time-points were observed. Otherwise, in the NR group, lower percentages of IFNγ+IL2+TNFα+CD4+ T-cells compared with the R group (T0: p = 0.0159; Tpost: p = 0.0159), as well as compared with the HD, at both time-points, were observed (T0: p = 0.0064; Tpost: p = 0.0064). These data seem to confirm that some LuT patients can mount cellular responses even in the absence of a positive humoral response (>33.8 BAU/mL), although this cellular response is dysfunctional and partially detrimental.
Center of Mass and spin for isolated sources of gravitational radiation

We define the center of mass and spin of an isolated system in General Relativity. The resulting relationships between these variables and the total linear and angular momentum of the gravitational system are remarkably similar to their Newtonian counterparts, though only variables at the null boundary of an asymptotically flat spacetime are used for their definition. We also derive equations of motion linking their time evolution to the emitted gravitational radiation. The results are then compared to other approaches. In particular one obtains unexpected similarities as well as some differences with results obtained in the Post Newtonian literature . These equations of motion should be useful when describing the radiation emitted by compact sources such as coalescing binaries capable of producing gravitational kicks, supernovas, or scattering of compact objects.
An X-ray detected group of quiescent early-type galaxies at z = 1.6 in the Chandra Deep Field South

We report the discovery of an X-ray group of galaxies located at a high redshift of z = 1.61 in the Chandra Deep Field South. Based on 4 Ms Chandra data, the group is ﬁrst identiﬁed as an extended X-ray source. We have used a wealth of deep multi-wavelength data to identify the optical counterpart—our red sequence ﬁnder detects a signiﬁcant over-density of galaxies at z (cid:3) 1.6. The brightest group galaxy is spectroscopically conﬁrmed at z = 1.61, based on published spectroscopic redshifts. Using this as a central redshift of the group, we measure an X-ray luminosity of L 0:1 – 2:4 keV = (1.8 ˙ 0.6) (cid:4) 10 43 erg s (cid:5) 1 , which then translates into a group mass of (3.2 ˙ 0.8) (cid:4) 10 13 M ˇ . This is the lowest-mass group ever conﬁrmed at z > 1.5. Deep optical–nearIR images from CANDELS reveal that the group exhibits a surprisingly prominent red sequence, and most of the galaxies are consistent with a formation redshift of z f = 3. A detailed analysis of the spectral energy distributions of the group member candidates conﬁrms that most of them are indeed passive galaxies. Furthermore, their structural parameters measured from near-IR CANDELS images show that they are morphologically early-type. The newly identiﬁed group at z = 1.61 is dominated by quiescent early-type galaxies, and the group appears to be similar to those in the local Universe. One possible difference is the high fraction of AGN—38 + 23 (cid:5) 20 % of the bright group member candidates are AGN, which might indicate a role for AGN in the quenching of star formation. However, a statistical sample of high- z groups is needed to draw a general picture of groups at this redshift. Such a sample will hopefully be available in near-future surveys.
THE WIRED SURVEY. III. AN INFRARED EXCESS AROUND THE ECLIPSING POST-COMMON ENVELOPE BINARY SDSS J030308.35+005443.7

We present the discovery with WISE of a significant infrared excess associated with the eclipsing post-common envelope binary SDSS J030308.35+005443.7, the first excess discovered around a non-interacting white dwarf+main-sequence M dwarf binary. The spectral energy distribution of the white dwarf+M dwarf companion shows significant excess longward of 3 μm. A Teff of 8940 K for the white dwarf is consistent with a cooling age >2 Gyr, implying that the excess may be due to a recently formed circumbinary dust disk of material that extends from the tidal truncation radius of the binary at 1.96 R☉ out to <0.8 AU, with a total mass of ∼1020 g. We also construct WISE and follow-up ground-based near-infrared light curves of the system and find variability in the K band that appears to be in phase with ellipsoidal variations observed in the visible. The presence of dust might be due to (1) material being generated by the destruction of small rocky bodies that are being perturbed by an unseen planetary system or (2) dust condensing from the companion's wind. The high inclination of this system and the presence of dust make it an attractive target for M dwarf transit surveys and long-term photometric monitoring.
HIGH-RESOLUTION X-RAY SPECTRA OF THE SYMBIOTIC STAR SS73 17

SS73 17 was an innocuous Mira-type symbiotic star until the International Gamma-Ray Astrophysics Laboratory and Swift discovered its bright hard X-ray emission, adding it to the small class of “hard X-ray emitting symbiotics. ” Suzaku observations in 2006 then showed it emits three bright iron lines as well, with little to no emission in the 0.3–2.0 keV bandpass. We present here follow-up observations with the Chandra High Energy Transmission Grating and Suzaku that confirm the earlier detection of strong emission lines of Fe Kα fluorescence, Fe xxv and Fe xxvi but also show significantly more soft X-ray emission. The high-resolution spectrum also shows emission lines of other highly ionized ions as Si xiv and possibly S xvi. In addition, a re-analysis of the 2006 Suzaku data using the latest calibration shows that the hard (15–50 keV) X-ray emission is brighter than previously thought and remains constant in both the 2006 and 2008 data. The G ratio calculated from the Fe xxv lines shows that these lines are thermal, not photoionized, in origin. With the exception of the hard X-ray emission, the spectra from both epochs can be fit using thermal radiation assuming a differential emission measure based on a cooling-flow model combined with a full and partial absorber. We show that acceptable fits can be obtained for all the data in the 1–10 keV band varying only the partial absorber. Based on the temperature and accretion rate, the thermal emission appears to be arising from the boundary layer between the accreting white dwarf and the accretion disk.
THE DISTANCE TO M101 HOSTING TYPE Ia SUPERNOVA 2011fe BASED ON THE TIP OF THE RED GIANT BRANCH

We present a new determination of the distance to M101, host of the Type Ia supernova (SN Ia) 2011fe, based on the tip of the red giant branch (TRGB) method. Our determination is based on Hubble Space Telescope archival F555W and F814W images of nine fields within the galaxy. Color–magnitude diagrams of arm-free regions in all fields show a prominent red giant branch. We measure the I-band magnitudes of the TRGB, obtaining a mean value of ITRGB = 25.28 ± 0.01 (where the error is a standard error), using an edge-detection method. We derive a weighted mean value of distance modulus (m − M)0 = 29.30 ± 0.01(random) ± 0.12(systematic), corresponding to a linear distance of 7.24 ± 0.03 ± 0.40 Mpc. While previous estimates for M101 show a large range (TRGB distances of (m − M)0 = 29.05–29.42 and Cepheid distances of (m − M)0 = 29.04–29.71), our measurements of the TRGB distances for nine fields show a small dispersion of only 0.02. We combine our distance estimate and photometry in the literature to derive absolute peak magnitudes in optical and near-infrared bands of SN 2011fe. Absolute maximum magnitudes of SN 2011fe are ∼0.2 mag brighter in the optical band and much more in the NIR than the current calibrations of SNe Ia in the literature. From the optical maximum magnitudes of SN 2011fe we obtain a value of the Hubble constant, H0 = 65.0 ± 0.5(random) ± 5.7(systematic) km s−1 Mpc−1, slightly smaller than other recent determinations of H0.
Pathological studies and ORF 103 gene based molecular characterization of sheep pox virus from outbreaks in Maharashtra, India

Sheep and goat pox are endemic in India and causes considerable losses to the animal husbandry sector every year. There are multiple reports of this disease from different states of India; however, information on the occurrence of this disease in Maharashtra state is very scanty. In this context, the present investigation reports the outbreaks of sheep pox in Satara and Solapur districts of Maharashtra state, India, from August 2019 to February 2020 based on clinical signs, gross and histopathological lesions, and molecular detection. Additionally, the ORF 103 gene sequence analysis from field samples revealed 100 to 99% identity with SPPV from Egypt, China, Pune, Ahmedabad, and Makhdoom. In phylogeny, sequences of the present study grouped into SPPVs clade. The finding of this study adds to the knowledge of the epidemiology of sheep pox in Maharashtra state and may help in planning effective prevention and control strategies.
Localization and characterization of SSCs from pre-pubertal bovine testes

Self renewal and proliferation ability of spermatogonial stem cells (SSCs) support spermatogenesis during adult life. Theoretically, these stem cells can be utilized for transmission of genetic information to descendants via testicular transplantation. However, lack of knowledge in methodologies for identification of SSCs limits the application of SSCs transplantation in domestic animals. Accumulated studies have shown that SSCs specific markers (DBA, UCHL1) and stem cell marker (Sox2, Oct4) are useful to screen SSCs that able to be used for transplantation. However, in cattle, less information is available on the expression status of these markers till date. Therefore, a study was carried out in 2019 at Tsukuba University, Japan where testes from 3, 5 and 7 months old calves were utilized to examine testicular localization and in vitro propogation of stem cell markers. SSCs were isolated by enzymatic digestion combined with centrifugal separation on discontinuous Percoll density gradient. Cell propagation and SSCs marker expression were determined at 5, 10 and 15 days post-culture. Immunostaining in conjunction with Western Blot analysis of cultured cells showed that stem cell markers (UCHL1, Oct4 and Sox2) were expressed in SSCs suggesting that differentiation of gonocyte started by 3 months and SSCs differentiation begins after 5 months of age. Taken together, these results demonstrated marker expression and localization of bull SSCs and showed that in vitro culturing of bull SSCs is implementable.
Minor Salivary Gland Surgery and Histopathological Scoring System: A Systematic Review

Sjögren’s syndrome is a systemic autoimmune disease characterized by chronic inflammation of the exocrine glands with an associated functional deficit. The clinical picture is characterized by symptoms such as dry eyes (xerophthalmia) and dry mouth (xerostomia). The disease is defined as primary if no other autoimmune diseases are associated, otherwise, it is defined as secondary. A systematic review was made using the databases PubMed (MEDLINE), Scopus, and keywords “biopsy,” “classification,” “clinical pathology,” “salivary glands,” and “Sjogren’s syndrome. ” The diagnosis of Sjögren’s syndrome is based on a combination of clinical, serologic, instrumental, and histological features. In addition to ocular tests, a biopsy of the minor salivary glands represents one of the most relevant examinations for the diagnosis. In fact, the evaluation of specific histopathological features represents one of the most important criteria proposed in the last international consensus of 2016, which developed the most recent classification criteria for Sjögren’s syndrome. Knowledge of classification criteria, minor salivary gland biopsy techniques, and histopathological features are essential for the clinician to evaluate the pathology report and make a diagnosis of Sjögren’s syndrome. The aim of this review is to describe the classification criteria of the disease proposed to date, the main biopsy techniques used to analyze the minor salivary glands, and finally, the histopathological diagnostic scoring systems currently applied.
New Lagrangian and Hamiltonian Methods in Field Theory

This work incorporates three modern aspects of mathematical physics: the jet methods in differntial geometry, the Lagrangian formalism on jet manifolds and the multimomentum approach to the Hamiltonian formalism. Several contemporary field models are investigated in detail. This is not a book on differential geometry, although modern concepts of differential geometry are used throughout the book. Quadratic Lagrangians and Hamiltonians are studied on the general level including the treatment of Hamiltonian formalism on composite fibre manifolds. The book presents new geometric methods and results in field theory.
Complete four-loop four-point amplitude in N=4 super-Yang-Mills theory

We present the complete four-loop four-point amplitude in N = 4 super-Yang-Mills theory, for a general gauge group and general D-dimensional covariant kinematics, and including all non-planar contributions. We use the method of maximal cuts - an efficient application of the unitarity method - to construct the result in terms of 50 four-loop integrals. We give graphical rules, valid in D-dimensions, for obtaining various non-planar contributions from previously-determined terms. We examine the ultraviolet behavior of the amplitude near D = 11/2. The non-planar terms are as well-behaved in the ultraviolet as the planar terms. However, in the color decomposition of the three- and four-loop amplitude for an SU(N{sub c}) gauge group, the coefficients of the double-trace terms are better behaved in the ultraviolet than are the single-trace terms. The results from this paper were an important step toward obtaining the corresponding amplitude in N = 8 supergravity, which confirmed the existence of cancellations beyond those needed for ultraviolet finiteness at four loops in four dimensions. Evaluation of the loop integrals near D = 4 would permit tests of recent conjectures and results concerning the infrared behavior of four-dimensional massless gauge theory.
Efficient Design of Majority-Logic-Based Approximate Arithmetic Circuits

Approximate computing (AC) offers benefits by reducing the requirement for full accuracy, thereby reducing power consumption and area. The majority logic (ML) gate functions as the fundamental logic block of many emerging nanotechnologies. In this article, ML-based arithmetic circuits, i.e., multibit adders and multipliers, are proposed. These adders are designed to prevent the propagation of inexact carry-out signals to higher order computing parts to enhance accuracy. We implemented the proposed multiplier by using a unique partial product reduction (PPR) circuitry, which was based on the parallel approximate 6:3 compressor. Several logic implementation costs, error metrics, and layouts implemented by quantum-dot cellular automata (QCA) are analyzed to evaluate the adder designs. A significant improvement is observed over previous ML-based designs based on the experimental results. The proposed designs are further evaluated using both a neural network (NN) accelerator and image processing. A structural similarity (SSIM) value of 1 and a peak signal-to-noise ratio (PSNR) value of infinity are achieved by the proposed adder design.
MicroRNA‐582‐5p targeting Creb1 modulates apoptosis in cardiomyocytes hypoxia/reperfusion‐induced injury

Myocardial ischemia–reperfusion injury (MIRI) caused by the reperfusion therapy of myocardial ischemic diseases is a kind of major disease that threatens human health and lives severely. There are lacking of effective therapeutic measures for MIRI. MicroRNAs (miRNAs) are abundant in mammalian species and play a critical role in the initiation, promotion, and progression of MIRI. However, the biological role and molecular mechanism of miRNAs in MIRI are not entirely clear.
First X-ray-based statistical tests for clumpy-torus models: eclipse events from 230 years of monitoring of Seyfert AGN

We present an analysis of multi-timescale variability in line-of-sight X-ray absorbing gas as a function of optical classification in a large sample of Seyfert AGN to derive the first X-ray statistical constraints for clumpy-torus models. We systematically search for discrete absorption events in the vast archive of RXTE monitoring of dozens of nearby type I and Compton-thin type II AGN. We are sensitive to discrete absorption events due to clouds of full-covering, neutral or mildly ionized gas with columns >~ 10^(22-25) cm^-2 transiting the line of sight. We detect 12 eclipse events in 8 objects, roughly tripling the number previously published from this archive. Peak column densities span ~ 4-26 x 10^22 cm^-2. Event durations span hours to months. The column density profile for an eclipsing cloud in NGC 3783 is doubly spiked, possibly indicating a cloud that is being tidally sheared. We infer the clouds' distances from the black hole to span ~0.3 -140 x 10^4 R_g. In seven objects, the clouds' distances are commensurate with the outer portions of Broad Line Regions (BLR), or the inner regions of infrared-emitting dusty tori. We discuss implications for cloud distributions in the context of clumpy-torus models. The probability of observing a source undergoing an absorption event, independent of constant absorption due to non-clumpy material, is 0.006(+0.160,-0.003) for type Is and 0.110(+0.461,-0.071) for type IIs.