Miracle-dz/UniFAR-FTUs huggingface dataset:
325 and 610 MHz radio counterparts of SNR G353.6−0.7 also known as HESS J1731−347

PC acknowledges support from the Department of Science and Technology via SwaranaJayanti Fellowship award (file no. DST/SJF/PSA-01/2014-15). We thank the staff of the GMRT that made these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research.
RX J1301.9+2747: A HIGHLY VARIABLE SEYFERT GALAXY WITH EXTREMELY SOFT X-RAY EMISSION

In this paper we present a temporal and spectral analysis of X-ray data from XMM-Newton and Chandra observations of the ultrasoft and variable Seyfert galaxy RX J1301.9+2747. In both observations the source clearly displays two distinct states in the X-ray band: a long quiescent state and a short flare (or eruptive) state which differs in count rates by a factor of 5–7. The transition from the quiescent to the flare state occurs in 1–2 ks. We have observed that the quiescent state spectrum is unprecedentedly steep with a photon index Γ ∼ 7.1, and the spectrum of the flare state is flatter with Γ ∼ 4.4. X-rays above 2 keV were not significantly detected in either state. In the quiescent state, the spectrum appears to be dominated by a blackbody component of temperature about ∼30–40 eV, which is comparable to the expected maximum effective temperature from the inner accretion disk. The quiescent state, however, requires an additional steep power law, presumably arising from Comptonization by transient heated electrons. The optical spectrum from the Sloan Digital Sky Survey shows Seyfert-like narrow lines for RX J1301.9+2747, while Hubble Space Telescope imaging reveals a central point source for the object. In order to precisely determine the hard X-ray component, future longer X-ray observations are required. This will help constrain the accretion disk model for RX J1301.9+2747, and shed new light on the characteristics of the corona and accretion flows around black holes.
Influence of eye movements on academic performance: A bibliometric and citation network analysis

Background: For many years it has been studied how eye movements influence reading and learning ability. The objective of this study is to determine the relationships between the different publications and authors. As well as to identify the different areas of research ocular movement. ; Methods: Web of Science was the database for the search of publications for the period 1900 to May 2021, using the terms: “Eye movement" AND “Academic achiev*”. The analysis of the publication was performed using the CitNetExplorer, VOSviewer and CiteSpace software. ; Results: 4391 publications and 11033 citation networks were found. The year with the most publications is 2018, a total of 318 publications and 10 citation networks. The most cited publication was "Saccade target selection and object recognition: evidence for a common attentional mechanism. " published by Deubel et al. in 1999, with a citation index of 214. Using the Clustering function, nine groups were found that cover the main research areas in this field: neurological, age, perceptual attention, visual disturbances, sports, driving, sleep, vision therapy and academic performance. ; Conclusion: Even being a multidisciplinary field of study, the topic with the most publications to date is the visual search procedure at the neurological level.
X-Ray Flares in Orion Young Stars. I. Flare Characteristics

Pre-main-sequence (PMS) stars are known to produce powerful X-ray flares, which resemble magnetic reconnection solar flares scaled by factors up to 104. However, there are numerous puzzles, including the structure of X-ray-emitting coronae and magnetospheres, the effects of protoplanetary disks, and the effects of stellar rotation. To investigate these issues in detail, we examine 216 of the brightest flares from 161 PMS stars observed in the Chandra Orion Ultradeep Project (COUP). These constitute the largest homogeneous data set of PMS, or indeed stellar flares at any stellar age, ever acquired. Our effort is based on a new flare spectral analysis technique that avoids nonlinear parametric modeling. We provide a catalog of derived properties and an electronic atlas for this unique collection of flares. The current study (Paper I) examines the flare morphologies, and provides a general comparison of COUP flare characteristics with those of other active X-ray stars and the Sun. Paper II will concentrate on relationships between flare behavior, protoplanetary disks, and other stellar properties. Several results are obtained. First, COUP flares are among the most powerful, longest, and hottest, corresponding to the largest known coronal structures. Second, no significant statistical differences in peak flare luminosity or temperature distributions are found among different morphological flare classes, suggesting a common underlying mechanism for all flares. Third, comparison with the general solar scaling laws indicates that COUP flares may not adequately fit proposed power-temperature and duration-temperature solar-stellar fits. Fourth, COUP superhot flares are found to be brighter but shorter than cooler COUP flares. Finally, the majority of bright COUP flares can be viewed as enhanced analogs of the rare solar ``long-duration events. ''
Spectroscopic Comparison of Metal-rich RRab Stars of the Galactic Field with their Metal-poor Counterparts

We investigate atmospheric properties of 35 stable RRab stars that possess the full ranges of period, light amplitude, and metal abundance found in Galactic RR Lyrae stars. Our results are derived from several thousand echelle spectra obtained over several years with the du Pont telescope of Las Campanas Observatory. Radial velocities of metal lines and the Hα line were used to construct curves of radial velocity versus pulsation phase. From these we estimated radial velocity amplitudes for metal lines (formed near the photosphere) and Hα Doppler cores (formed at small optical depths). We also measured Hα emission fluxes when they appear during primary light rises. Spectra shifted to rest wavelengths, binned into small phase intervals, and co-added were used to perform model atmospheric and abundance analyses. The derived metallicities and those of some previous spectroscopic surveys were combined to produce a new calibration of the Layden abundance scale. We then divided our RRab sample into metal-rich (disk) and metal-poor (halo) groups at [Fe/H] = −1.0; the atmospheres of RRab families, so defined, differ with respect to (a) peak strength of Hα emission flux, (b) Hα radial velocity amplitude, (c) dynamical gravity, (d) stellar radius variation, (e) secondary acceleration during the photometric bump that precedes minimum light, and (f) duration of Hα line-doubling. We also detected Hα line-doubling during the “bump” in the metal-poor family, but not in the metal-rich one. Although all RRab probably are core helium-burning horizontal branch stars, the metal-rich group appears to be a species sui generis.
Sex- and Neuropsychiatric-Dependent Circadian Alterations in Daily Voluntary Physical Activity Engagement and Patterns in Aged 3xTg-AD Mice

Alzheimer’s disease (AD) patients suffer from circadian rhythm alterations affecting their daily physical activity patterns with less willingness to perform a voluntary exercise. In preclinical studies, there is no clarity on whether animal models of AD can replicate these impairments. Here, we provide a proof of concept of the performance and behavioral effects of four weeks of voluntary wheel running (VWR) in a group of 14-month-old male and female 3xTg-AD mice at advanced stages of AD and the daily variance (behavioral circadian rhythmicity) of VWR associated with sex and their neuropsychiatric-like phenotype. Higher levels of horizontal exploration in the open field (OF) test were found in mice submitted to exercise. A linear mixed effect model showed significant sex-dependent differences in the VWR activity performed on the first night of follow-up, with high-NIBI males running less than high-NIBI females. Thus, an influence of NPS-like symptoms on the circadian patterns of VWR may account for such differences. In addition, males remained more active than females during diurnal periods. We hypothesize that this increment in energy expenditure during resting periods may be related to hyperactive behavior, similar to that observed in humans’ exacerbated agitation or sundowning behavior. These findings support the usage of the 3xTg-AD mouse as a reliable model for studying circadian rhythm alterations in AD and, at the translational level, the importance of tailored and individualized physical activity programs in clinical settings.
BRIGHT 22 μm EXCESS CANDIDATES FROM THE WISE ALL-SKY CATALOG AND THE HIPPARCOS MAIN CATALOG

In this paper, we present a catalog that includes 141 bright candidates (⩽10.27 mag, V band) showing an excess of infrared (IR) at 22 μm. Of these 141 candidates, 38 stars are known IR-excess stars or disks, 23 stars are double or multiple stars, and 4 are Be stars while the remaining more than 70 stars are identified as 22 μm excess candidates in our work. The criterion for selecting candidates is Ks − [22]μm. All these candidates are selected from the Wide-field Infrared Survey Explorer all-sky data cross-correlated with the Hipparcos main catalog and the likelihood-ratio technique is employed. Considering the effect of background, we introduce the IRAS 100 μm level to exclude the high background. We also estimate the coincidence probability of these sources. In addition, we present the optical to mid-IR spectral energy distributions and optical images for all the candidates, and give the observed optical spectra of six stars with the National Astronomical Observatories, Chinese Academy of Sciences' 2.16 m telescope. To measure for the amount of dust around each star, the fractional luminosity is also provided. We also test whether our method of selecting IR-excess stars can be used to search for extra-solar planets; we cross-match our catalog with known IR-excess stars with planets but found no matches. Finally, we give the fraction of stars showing excess IR for different spectral types of main-sequence stars.
Interacting viscous dark energy in a Bianchi type-III universe

We study the evolution of the equation of state of viscous dark energy in the scope of Bianchi type III space-time. We consider a case where the dark energy is minimally coupled to the perfect fluid, as well as in direct interaction with it. The viscosity and the interaction between the two fluids are parameterized by constants ζ0 and σ, respectively. We have made a detailed investigation of the cosmological implications of this parametrization. To differentiate between different dark energy models, we have performed a geometrical diagnostic by using the statefinder pair {s, r}.
Regular black holes from semi-classical down to Planckian size

In this paper, we review various models of curvature singularity free black holes (BHs). In the first part of the review, we describe semi-classical solutions of the Einstein equations which, however, contains a “quantum” input through the matter source. We start by reviewing the early model by Bardeen where the metric is regularized by-hand through a short-distance cutoff, which is justified in terms of nonlinear electro-dynamical effects. This toy-model is useful to point-out the common features shared by all regular semi-classical black holes. Then, we solve Einstein equations with a Gaussian source encoding the quantum spread of an elementary particle. We identify, the a priori arbitrary, Gaussian width with the Compton wavelength of the quantum particle. This Compton–Gauss model leads to the estimate of a terminal density that a gravitationally collapsed object can achieve. We identify this density to be the Planck density, and reformulate the Gaussian model assuming this as its peak density. All these models, are physically reliable as long as the BH mass is big enough with respect to the Planck mass. In the truly Planckian regime, the semi-classical approximation breaks down. In this case, a fully quantum BH description is needed. In the last part of this paper, we propose a nongeometrical quantum model of Planckian BHs implementing the Holographic Principle and realizing the “classicalization” scenario recently introduced by Dvali and collaborators. The classical relation between the mass and radius of the BH emerges only in the classical limit, far away from the Planck scale.
Farmers’ perceptions of the degradation of natural resources in lowlands in the Sudano-Sahelian zone: The case of the Nakanbé-Dem sub-watershed in Burkina Faso

The Burkinabe Sahel is characterized by a strong degradation of natural resources. This regression is attributable to natural and anthropogenic factors. The present study concerns the lowlands of the Nakanbé-Dem sub-watershed located in the southern limit of the Sahel. In this area dominated by rain-fed agriculture and extensive livestock farming, wetlands are of paramount importance. In the face of their continued degradation, community participation is necessary for the sustainable management of the lowlands. This study analyzes endogenous indicators of inland valley degradation in the Sudano-Sahelian zone. Semi-structured survey data were collected from 325 farmers in six lowlands. Descriptive statistics and correspondence factor analysis (CFA) was applied. The results show that farmers clearly perceive the degradation of the islands. Farmers use meteorological, floristic, and physical elements to characterize the state of degradation of the islands. The disappearance of several species and the appearance of ubiquitous species allow them to assess the degradation of inland valley lands. These endogenous indicators vary according to gender and education level. The study highlighted the importance of endogenous knowledge in the analysis of inland valley degradation. It suggests the need to take it into account in the implementation of restoration techniques for degraded inland valleys.
DARK MATTER HEATING AND EARLY CORE FORMATION IN DWARF GALAXIES

We present more results from a fully cosmological ΛCDM simulation of a group of isolated dwarf galaxies that has been shown to reproduce the observed stellar mass and cold gas content, resolved star formation histories, and metallicities of dwarfs in the Local Volume. Here we investigate the energetics and timetable of the cusp–core transformation. As suggested by previous work, supernova-driven gas outflows remove dark matter (DM) cusps and create kiloparsec-size cores in all systems having a stellar mass M* > 106 M☉. The “DM core mass removal efficiency”—dark mass ejected per unit stellar mass—ranges today from a few to a dozen, and increases with decreasing host mass. Because dwarfs form the bulk of their stars prior to redshift 1 and the amount of work required for DM heating and core formation scales approximately as , the unbinding of the DM cusp starts early and the formation of cored profiles is not as energetically onerous as previously claimed. DM particles in the cusp typically migrate to 2–3 core radii after absorbing a few percent of the energy released by supernovae. The present-day slopes of the inner DM mass profiles, Γ ≡ dlog M/dlog R ≃ 2.5–3, of the simulated “Bashful” and “Doc” dwarfs are similar to those measured in the luminous Fornax and Sculptor dwarf spheroidals. None of the simulated galaxies has a circular velocity profile exceeding 20 km s−1 in the inner 1 kpc, implying that supernova feedback is key to solve the “too-big-to-fail” problem for Milky Way subhalos.
Regarding how Tycho Brahe noted the absurdity of the Copernican Theory regarding the Bigness of Stars, while the Copernicans appealed to God to answer that absurdity

Tycho Brahe, the most prominent and accomplished astronomer of his era, made measurements of the apparent sizes of the Sun, Moon, stars, and planets. From these he showed that within a geocentric cosmos these bodies were of comparable sizes, with the Sun being the largest body and the Moon the smallest. He further showed that within a heliocentric cosmos, the stars had to be absurdly large - with the smallest star dwarfing even the Sun. (The results of Tycho's calculations are illustrated in this paper.) Various Copernicans responded to this issue of observation and geometry by appealing to the power of God: They argued that giant stars were not absurd because even such giant objects were nothing compared to an infinite God, and that in fact the Copernican stars pointed out the power of God to humankind. Tycho rejected this argument.
The Carbon Holdings of Northern Ecuador's Mangrove Forests

Within a geographic information systems environment, we combine field measures of mangrove tree diameter, mangrove species distribution, and mangrove tree density with remotely sensed measures of mangrove location and mangrove canopy cover to estimate the mangrove carbon holdings of northern Ecuador. We find that the four northern estuaries of Ecuador contain approximately 7,742,999 t (±15.47 percent) of standing carbon. Of particularly high carbon holdings are the Rhizophora mangle–dominated mangrove stands found in and around the Cayapas-Mataje Ecological Reserve in northern Esmeraldas Province, Ecuador, and certain stands of Rhizophora mangle in and around the Isla Corazón y Fragata Wildlife Refuge in central Manabí Province, Ecuador. Our field-driven mangrove carbon estimate is higher than all but one of the comparison models evaluated. We find that basic latitudinal mangrove carbon models performed at least as well, if not better, than the more complex species-based allometric models in predicting standing carbon levels. In addition, we find that improved results occur when multiple models are combined as opposed to relying on any one single model for mangrove carbon estimates. The high level of carbon contained in these mangrove forests, combined with the future atmospheric carbon sequestration potential they offer, makes it a necessity that they are included in any future payment for ecosystem services strategy aimed at using forest systems to offset CO2 emissions and mitigate predicted CO2-driven temperature increases.
Holographic Non-Gaussianity

We investigate the non-Gaussianity of primordial cosmological perturbations within our recently proposed holographic description of inflationary universes. We derive a holographic formula that determines the bispectrum of cosmological curvature perturbations in terms of correlation functions of a holographically dual three-dimensional non-gravitational quantum field theory (QFT). This allows us to compute the primordial bispectrum for a universe which started in a non-geometric holographic phase, using perturbative QFT calculations. Strikingly, for a class of models specified by a three-dimensional super-renormalisable QFT, the primordial bispectrum is of exactly the factorisable equilateral form with f_nl^eq=5/36, irrespective of the details of the dual QFT. A by-product of this investigation is a holographic formula for the three-point function of the trace of the stress-energy tensor along general holographic RG flows, which should have applications outside the remit of this work.
Exploring the association between sleep insufficiency and self-reported cardiovascular disease among northeastern Greeks

Objective To explore the association of sleep characteristics with cardiovascular disease (CVD) using self-reported questionnaires. Material and Methods 957 adults between 19 and 86 years old were enrolled in this cross-sectional study. The participants were classified into three groups [short (<6h), normal (6-8h), and long (>8h) sleepers] by using multistage stratified cluster sampling. CVD was defined by a positive response to the questions: “Have you been told by a doctor that you have had a heart attack or angina or stroke or have you undergone bypass surgery? ”. Sleep quality, utilizing Epworth sleepiness scale, Athens insomnia scale, Pittsburgh sleep quality index and Berlin questionnaire, was also examined. Results Prevalence of CVD was 9.5%. Individuals with CVD exhibited reduced sleep duration by 33 min ( p <0.001) and sleep efficiency by 10% ( p <0.001). In multivariable logistic regression analysis, adjusting for subjects’ sociodemographic, lifestyle habits and health related characteristics, short sleep duration was almost three times more frequent in patients with CVD (aOR=2.86, p <0.001 in the entire sample; aOR=2.68, p =0.019 in women and aOR=2.57, p =0.009 in men). Furthermore, CVD was significantly associated with excessive daytime sleepiness (aOR=2.02, p =0.026), insomnia (aOR=1.93, p =0.010), poor sleep quality (aOR=1.90, p =0.006) and increased risk of obstructive sleep apnea (aOR=2.08, p =0.003). Conclusion Our study highlights a strong correlation of sleep insufficiency with CVD and promotes early pharmacological or cognitive behavioral interventions in order to protect cardiovascular health.
Some new results for 'jet' stopping in AdS/CFT

We give a simple overview and perspective on our recent results (Arnold and Vaman 2010 J. High Energy Phys. JHEP10(2010)099, Arnold and Vaman 2011 J. High Energy Phys. JHEP04(2011)027) on jet stopping in strongly coupled plasmas using gauge-gravity duality. There is an important distinction between typical and maximum stopping distances, and we find that the typical stopping distance scales with energy as E1/4.
Sensitivity of {gamma}-ray telescopes for detection of magnetic fields in the intergalactic medium

We explore potential of current and next-generation {gamma}-ray telescopes for the detection of weak magnetic fields in the intergalactic medium. We demonstrate that using two complementary techniques, observation of extended emission around point sources and observation of time delays in {gamma}-ray flares, one would be able to probe most of the cosmologically and astrophysically interesting part of the 'magnetic field strength' vs 'correlation length' parameter space. This implies that {gamma}-ray observations with Fermi and ground-based Cherenkov telescopes will allow to (a) strongly constrain theories of the origin of magnetic fields in galaxies and galaxy clusters and (b) discover, constrain or rule out the existence of weak primordial magnetic field generated at different stages of evolution of the Early Universe.
Research on The Influence of Social Network Information Quality On Tourism Willingness

Social networks have become an important way for people to obtain information, socialize and show their lifestyles. They have also become an important platform for cloud tourism and cloud exhibitions against the backdrop of COVID-19. Will photos or videos on social networks have an impact on individual travel intentions? Based on these questions, this study explores the measurement of information quality of social networks and its impact on individual travel decisions. Based on the social impact theory, this study constructed THE SOR theoretical model from the perspective of informational social impact. Through questionnaires, 696 sample data were obtained, and AMOS was used to analyze the Structural equation model. It is found that the quality of social network information can be composed of five dimensions. The tourism information published by others in social network has a significant positive influence on tourism decision making. The higher the information quality is, the stronger the individual will be to travel.