Miracle-dz/UniFAR-FTUs huggingface dataset:
Outbreak of toxoplasmosis associated with muscular lesions in finishing pigs caused by an atypical Toxoplasma gondii genotype

Abstract Toxoplasma gondii infections are usually asymptomatic in pigs, and an acute clinical disease is rare in this host. This study aimed to determine the pathological and molecular aspects of an outbreak of fatal systemic toxoplasmosis in finishing pigs in Brazil. The outbreak occurred on a commercial finishing pig farm in the state of Santa Catarina in southern Brazil. The farm had 1500 pigs and 3.8% of mortality rate during the outbreak. The pigs had fever, anorexia, apathy, and locomotor deficits. Seven pigs were necropsied. Gross findings included multifocal to coalescent pale areas in skeletal muscles, lymphadenomegaly, hepatosplenomegaly, and non-colapsed lungs. The histological findings included granulomatous lymphadenitis, hepatitis and splenitis, necrotizing myositis, and lymphoplasmacytic interstitial pneumonia. Lung and liver lesions were occasionally accompanied by T. gondii parasitic structures. Positive immunolabeling for T. gondii tachyzoites and encysted bradyzoites was detected in all examined pigs. PCR-RFLP (11 markers) and microsatellite analysis (15 markers) identified the non-archetypal genotype #278 in pigs. This is the first report of systemic toxoplasmosis in pigs with muscle lesions and additionally shows the diversity of disease-causing T. gondii genotypes circulating in animals in Brazil.
Magnetic bimerons as skyrmion analogues in in-plane magnets

A magnetic bimeron is a pair of two merons and can be understood as the in-plane magnetized version of a skyrmion. Here we theoretically predict the existence of single magnetic bimerons as well as bimeron crystals, and compare the emergent electrodynamics of bimerons with their skyrmion analogues. We show that bimeron crystals can be stabilized in frustrated magnets and analyze what crystal structure can stabilize bimerons or bimeron crystals via the Dzyaloshinskii-Moriya interaction. We point out that bimeron crystals, in contrast to skyrmion crystals, allow for the detection of a pure topological Hall effect. By means of micromagnetic simulations, we show that bimerons can be used as bits of information in in-plane magnetized racetrack devices, where they allow for current-driven motion for torque orientations that leave skyrmions in out-of-plane magnets stationary.
Evaluation of the Role of BIOCHIP Mosaic Based Indirect Immunofluorescence and ELISA BP 180 and BP 230 Autoantibodies in the Diagnosis of Bullous Pemphigoid Patients

Background: Bullous pemphigoid (BP) is characterized by tissue-bound and circulating Immunoglobulin G (IgG) autoantibodies against BP 180 and BP 230. Diagnosis of BP is a multi-step procedure. Enzyme-linked immunosorbent assay (ELISA) is a quantitative analysis of target antigens, whereas BIOCHIP mosaic-based indirect immunofluorescence (IIF) has a combination of screening and target antigen-specific substrates in a single miniature incubation field. This study is done to compare BIOCHIP mosaic based IIF and ELISA for the diagnosis of BP. Materials and Methods: A total of 42 biopsy and/or direct immunofluorescence (DIF) proven BP patients were included in the study. Serum was subjected to BIOCHIP mosaic-based IIF and ELISA. The results were then compared. Results: Using ELISA, the sensitivity of BP 180 and BP 230 was 92.3% and 54.5%, respectively. The sensitivity of BP 180 and BP 230 by BIOCHIP was 77.4% and 60%, respectively. The association between ELISA and BIOCHIP was analyzed using the Chi-square test and was found to be statistically significant with a P value ≤ 0.05. Conclusion: Our study concluded that both BIOCHIP and ELISA showed comparable sensitivity in diagnosing BP. Both are non-invasive, less time-consuming, and provide fast results. However, BIOCHIP can delineate bullous pemphigoid from other sub-epidermal bullous diseases.
Water Absorption from Line-of-Sight Clouds toward W49A

We have observed six clouds along the line of sight toward W49A using the Submillimeter Wave Astronomy Satellite and several ground-based observatories. The ortho-H2O 110 → 101 and OH (1665 and 1667 MHz) transitions are observed in absorption, whereas the low-J CO, 13CO, and C18O lines, as well as the [C I] 3P1-3P0 transition, are seen in emission. The emission lines allow us to determine the gas density (n ~ 1500-3000 cm-3) and CO column densities [N(CO) ~ 7.9 × 1015-2.8 × 1017 cm-2] using a standard large velocity gradient analysis. By using both the o-H218O and o-H2O absorption lines, we are able to constrain the column-averaged o-H2O abundances in each line-of-sight cloud to within about an order of magnitude. Assuming the standard N(H2)/N(CO) ratio of 104, we find N(o-H2O)/N(H2) = 8.1 × 10-8 to 4 × 10-7 for three clouds with optically thin water lines. In three additional clouds, the H2O lines are saturated, so we have used observations of the H218O ground-state transition to find upper limits to the water abundance of 8.2 × 10-8 to 1.5 × 10-6. We measure the OH abundance from the average of the 1665 and 1667 MHz observations and find N(OH)/N(H2) = 2.3 × 10-7 to 1.1 × 10-6. The o-H2O and OH abundances are similar to those determined for line-of-sight water absorption features toward W51 and Sgr B2 but are higher than those seen from water emission lines in molecular clouds. However, the clouds toward W49 have lower ratios of OH relative to H2O column densities than are predicted by simple models, which assume that dissociative recombination is the primary formation pathway for OH and H2O. Building on the 2002 work of Neufeld and coworkers, we present photochemistry models including additional chemical effects, which can also explain the observed OH and H2O column densities, as well as the observed H2O/CO abundance ratios.
Representations of functions, celestial mechanics and KAM theory, 1957-1965

On the representation of functions of two variables in the form ? [? (x) + ? (y)]. - On functions of three variables. - The mathematics workshop for schools at Moscow State University. - The school mathematics circle at Moscow State University: harmonic functions. - On the representation of functions of several variables as a superposition of functions of a smaller number of variables. - Representation of continuous functions of three variables by the superposition of continuous functions of two variables. - Some questions of approximation and representation of functions. - Kolmogorov seminar on selected questions of analysis. - On analytic maps of the circle onto itself. - Small denominators. I. Mapping of the circumference onto itself. - The stability of the equilibrium position of a Hamiltonian system of ordinary differential equations in the general elliptic case. - Generation of almost periodic motion from a family of periodic motions. - Some remarks on flows of line elements and frames. - A test for nomographic representability using Decartes' rectilinear abacus. - Remarks on winding numbers. - On the behavior of an adiabatic invariant under slow periodic variation of the Hamiltonian. - Small perturbations of the automorphisms of the torus. - The classical theory of perturbations and the problem of stability of planetary systems. - Letter to the editor. - Dynamical systems and group representations at the Stockholm Mathematics Congress. - Proof of a theorem of A. N. Kolmogorov on the invariance of quasi-periodic motions under small perturbations of the Hamiltonian. - Small denominators and stability problems in classical and celestial mechanics. - Small denominators and problems of stability of motion in classical and celestial mechanics. - Uniform distribution of points on a sphere and some ergodic properties of solutions of linear ordinary differential equations in a complex region. - On a theorem of Liouville concerning integrable problems of dynamics. - Instability of dynamical systems with several degrees of freedom. - On the instability of dynamical systems with several degrees of freedom. - Errata to V.I. Arnol'd's paper: "Small denominators. I. ". - Small denominators and the problem of stability in classical and celestial mechanics. - Stability and instability in classical mechanics. - Conditions for the applicability, and estimate of the error, of an averaging method for systems which pass through states of resonance in the course of their evolution. - On a topological property of globally canonical maps in classical mechanics.
The Ultraviolet Upturn in Elliptical Galaxies as an Age Indicator

The UV upturn phenomenon in elliptical galaxies, although challenging because of its complexity, is attractive for its potential value as an age indicator of old stellar systems. This work represents the combined efforts of two population synthesis groups with substantially different views to work together to minimize uncertainties in modeling and analysis. Unfortunately, this study, using the currently available data, cannot determine the metallicity of the dominant UV sources, one of the most outstanding problems related to the UV upturn phenomenon, as some input parameters need to be constrained better. We have found, however, that it is feasible to select a more likely model empirically because different models predict substantially different UV-to-V flux ratios as functions of redshift: metal-rich solutions predict a much steeper decline in the UV-to-V flux ratio than metal-poor solutions. We show that such differences in model predictions are quite independent of cosmology and are detectable using current and upcoming space UV facilities. The various alternatives suggest significantly different ages for the present-epoch giant ellipticals: the metal-rich solutions suggest 30%-50% smaller ages than the metal-poor solutions. Thus, an empirical fitting would not only reveal the origin of the UV upturn but yield independent age estimations for ellipticals. We show that this may effectively constrain some of the cosmological parameters that predict a unique age for the present-epoch galaxies. If we use the most recent estimations of H0 and Ω0, the younger, metal-rich models would have no conflict with a cosmology of a negligibly small Λ0, whereas the older, metal-poor models unavoidably suggest a substantially large value of Λ0 (i.e., Λ0≳0.63 for zfor=∞) in the context of an inflationary universe.
M101: Spectral Observations of H ii Regions and Their Physical Properties

By using the Hectospec 6.5 m Multiple Mirror Telescope and the 2.16 m telescope of the National Astronomical Observatories, of the Chinese Academy of Sciences, we obtained 188 high signal-to-noise ratio spectra of regions in the nearby galaxy M101, which is the largest spectroscopic sample of regions for this galaxy so far. These spectra cover a wide range of regions on M101, which enables us to analyze two-dimensional distributions of its physical properties. The physical parameters are derived from emission lines or stellar continua, including stellar population age, electron temperature, oxygen abundance, etc. The oxygen abundances are derived using two empirical methods based on O3N2 and R23 indicators, as well as the direct method when is available. By applying the harmonic decomposition analysis to the velocity field, we obtained a line-of-sight rotation velocity of 71 and a position angle of 36°. The stellar age profile shows an old stellar population in the galaxy center and a relatively young stellar population in outer regions, suggesting an old bulge and a young disk. The oxygen abundance profile exhibits a clear break at ∼18 kpc, with a gradient of −0.0364 dex kpc−1 in the inner region and −0.00686 dex kpc−1 in the outer region. Our results agree with the “inside-out” disk growth scenario of M101.
Galaxy Mergers up to Z < 2.5. I. The Star Formation Properties of Merging Galaxies at Separations of 3–15 kpc

We present a study of the influence of galaxy mergers on star formation at 0.3 < z < 2.5. Major mergers are selected from the CANDELS/3D-HST catalog using a peak-finding algorithm. Mergers have projected galaxy nucleus separation of their members between 3 and 15 kpc. We compare the star formation activity in merging and nonmerging galaxies and find no significant differences. We find that only 12% of the galaxies in major mergers (in which both galaxies have ) are starbursting (i.e., with star formation rate (SFR) above the main sequence of star-forming galaxies by >0.5 dex). Merging galaxies, which include galaxies with lower masses, show a higher fraction of starbursting galaxies (20%). The low fraction of starbursting merging galaxies in this sample suggests that at galaxy nucleus separations of 3–15 kpc merging galaxies are still in an early stage and are yet to reach the maximum level of star formation activity. Furthermore, the level of star formation enhancement and its duration could be arguably reduced compared to local mergers, as shown by simulations of high-z mergers, and might also depend on the physical properties (such as stellar mass and gas fraction) of the merging galaxies. Finally, we compare the specific SFR between merging galaxies. Our results suggest that, as the mass of the merging galaxies increases, the star formation activity in the less massive member in the merger suffers a more dramatic impact than its companion galaxy.
Spots, Flares, Accretion, and Obscuration in the Pre-main-sequence Binary DQ Tau

DQ Tau is a young low-mass spectroscopic binary, consisting of two almost equal-mass stars on a 15.8 day period surrounded by a circumbinary disk. Here, we analyze DQ Tau’s light curves obtained by Kepler K2, the Spitzer Space Telescope, and ground-based facilities. We observed variability phenomena, including rotational modulation by stellar spots, brief brightening events due to stellar flares, long brightening events around periastron due to increased accretion, and short dips due to brief circumstellar obscuration. The rotational modulation appears as a sinusoidal variation with a period of 3.017 days. In our model, this is caused by extended stellar spots 400 K colder than the stellar effective temperature. During our 80 day long monitoring, we detected 40 stellar flares with energies up to 1.2 × 1035 erg and duration of a few hours. The flare profiles closely resemble those in older late-type stars, and their occurrence does not correlate with either the rotational or the orbital period. We observe elevated accretion rates of up to 5 × 10−8 M⊙ yr−1 around each periastron. Our Spitzer data suggest that the increased accretion luminosity temporarily heats up the inner part of the circumbinary disk by about 100 K. We found an inner disk radius of 0.13 au, significantly smaller than expected from dynamical modeling of circumbinary disks. Interestingly, the inner edge of the disk corotates with the binary’s orbit. DQ Tau also shows short dips of <0.1 mag in its light curve, reminiscent of the well-known “dipper phenomenon” observed in many low-mass young stars.
Local estimation of parametric point spread functions in thermal images via convolutional neural networks

Thermal image formation can be modeled as the convolution of an ideal image with a point spread function (PSF) that characterizes the optical degradations. Although simple space-invariant models are sufficient to model diffraction-limited optical systems, they cannot capture local variations that arise because of nonuniform blur. Such degradations are common when the depth of field is limited or when the scene involves motion. Although space-variant deconvolution methods exist, they often require knowledge of the local PSF. In this paper, we adapt a local PSF estimation method (based on a learning approach and initially designed for visible light microscopy) to thermal images. The architecture of our model uses a ResNet-34 convolutional neural network (CNN) that we trained on a large thermal image dataset (CVC-14) that we split in training, tuning, and evaluation subsets. We annotated the sets by synthetically blurring sharp patches in the images with PSFs whose parameters covered a range of values, thereby producing pairs of sharp and blurred images, which could be used for supervised training and ground truth evaluation. We observe that our method is efficient at recovering PSFs when their width is larger than the size of a pixel. The estimation accuracy depends on the careful selection of training images that contain a wide range of spatial frequencies. In conclusion, while local PSF parameter estimation via a trained CNN can be efficient and versatile, it requires selecting a large and varied training dataset. Local deconvolution methods for thermal images could benefit from our proposed PSF estimation method.
Assessment of Stabilities of Two Local Plant Dyes as Colorants for Petroleum Products (Petrol, Kerosene, and Diesel)

Dyes from Pterocarpusosun Craib and Lawsoniainermis Linn. were extracted by cold maceration using ethanol and methanol, respectively. The extracted dyes were subsequently purified using chromatographic methods and characterized using ultra-violet (UV) visible and Fourier Transform Infrared Spectrophotometer (FTIR). The UV spectra of the dyes in petrol, kerosene, and diesel indicated presence of chromophores. The FTIR spectra of the dyes showed presence of phenolic O-H and C=C stretching of aromatic functional groups. The color intensity of the dye from Lawsoniainermis measured with Lovibond Tintometer was remarkably stable in coloring petrol for a period of at least twenty-eight days but not kerosene or diesel while the color intensity of the dye from Pterocarpusosun was not stable. Thus, dye from Lawsoniainermis can be used as alternative colorants to synthetic dyes for petrol but not for kerosene or diesel. The dyes from Pterocarpusosun cannot be so used for any of the petroleum products because of their instability.
Performance of Low Dissipative High Order Shock-Capturing Schemes for Shock-Turbulence Interactions

Abstract Accurate and efficient direct numerical simulation of turbulence in the presence of shock waves represents a significant challenge for numerical methods. The objective of this paper is to evaluate the performance of high order compact and non-compact central spatial differencing employing total variation diminishing (TVD) shock-capturing dissipations as characteristic based filters for two model problems combining shock wave and shear layer phenomena. A vortex pairing model evaluates the ability of the schemes to cope with shear layer instability and eddy shock waves, while a shock wave impingement on a spatially-evolving mixing layer model studies the accuracy of computation of vortices passing through a sequence of shock and expansion waves. A drastic increase in accuracy is observed if a suitable artificial compression formulation is applied to the TVD dissipations. With this modification to the filter step the fourth-order non-compact scheme shows improved results in comparison to second-order methods, while retaining the good shock resolution of the basic TVD scheme. For this characteristic based filter approach, however, the benefits of compact schemes or schemes with higher than fourth order are not sufficient to justify the higher complexity near the boundary and/or the additional computational cost.
A Meteor of Apparent Interstellar Origin in the CNEOS Fireball Catalog

The earliest confirmed interstellar object, ‘Oumuamua, was discovered in the solar system by Pan-STARRS in 2017, allowing for a calibration of the abundance of interstellar objects of its size ∼100 m. This was followed by the discovery of Borisov, which allowed for a similar calibration of its size ∼0.4–1 km. One would expect a much higher abundance of significantly smaller interstellar objects, with some of them colliding with Earth frequently enough to be noticeable. Based on the CNEOS catalog of bolide events, we identify the ∼0.45 m meteor detected at 2014 January 8 17:05:34 UTC as originating from an unbound hyperbolic orbit. The U.S. Department of Defense has released an official letter stating that “the velocity estimate reported to NASA is sufficiently accurate to indicate an interstellar trajectory,” which we rely on here as confirmation of the object’s interstellar trajectory. Based on the data provided by CNEOS, we infer that the meteor had an asymptotic speed of v ∞ ∼ 42.1 ± 5.5 km s−1 outside of the solar system. Note that v ∞ here refers to the velocity of the meteor outside the solar system, not the velocity of the meteor outside the atmosphere. Its origin is approximately toward R.A. 49. °4 ± 4. °1 and decl. 11. °2 ± 1. °8, implying that its initial velocity vector was 58 ± 6 km s−1 away from the velocity of the local standard of rest (LSR).
Erratum: “The Ultraviolet C ii Lines as a Diagnostic of κ-distributed Electrons in Planetary Nebulae” (2022, ApJ, 936, 143)

Zheng-Wei Yao and Yong Zhang 1 School of Physics and Astronomy, Sun Yat-sen University, Zhuhai, 519082, People’s Republic of China; zhangyong5@mail.sysu. edu.cn 2 CSST Science Center for the Guangdong-Hongkong-Macau Greater Bay Area, Sun Yat-Sen University, Guangdong Province, People’s Republic of China 3 Laboratory for Space Research, The University of Hong Kong, Hong Kong, People’s Republic of China Received 2022 October 13; published 2022 November 2
The formation of disc galaxies in a cosmological context: structure and kinematics

We present results concerning the internal structure and kinematics of disk galaxies formed in cosmologically motivated simulations. The calculations include dark matter, gas dynamics, radiative cooling, star formation, supernova feedback and metal enrichment. The initial model is a rigidly rotating overdense sphere with a mass of about 8 10^11 Msol which is perturbed by small scale fluctuations according to a biased CDM power spectrum. Converging, Jeans unstable and rapidly cooling regions are allowed to form stars. Via supernovae, metal enriched gas is returned to the interstellar medium. {}From these initial conditions a galaxy forms which shows the main properties of spiral galaxies: a rotationally supported exponential disk which consists of young stars with about solar metallicity, a slowly rotating halo of old metal poor stars, a bulge of old metal rich stars and a slowly rotating extended halo of dark matter. Bulge, stellar and dark halo are supported by an anisotropic velocity dispersion and have a de Vaucouleurs surface density profile. The flattening of the dark and stellar halo is too large to be explained by rotation only. Whether the flattening of the bulge is caused by an anisotropic velocity dispersion or by its rotation cannot be answered, because of the limited numerical resolution due to gravitational softening. The velocity dispersion and the thickness of the stellar disk increase with the age of the stars. Considering only the young stellar component, the disk is cold (sigma=20 km/sec) and thin (z <1 kpc). The dynamical formation process ends after about 4\,Gyr, when