Miracle-dz/UniFAR-FTUs huggingface dataset:
HIFLUGCS: X-ray luminosity -- dynamical mass relation and its implications for mass calibrations with the SPIDERS and 4MOST surveys

We present the X-ray luminosity (L) versus dynamical mass (M) relation for 63 nearby clusters in the HIFLUGCS. The luminosity measurements are obtained based on ~1.3 Ms of clean XMM data and ROSAT pointed observations. The masses are estimated using optical spectroscopic redshifts of 13647 cluster galaxies in total. Given sufficient numbers of member galaxies in computing the dynamical masses, the L-M relations agree between the disturbed and undisturbed clusters. The cool-core clusters still dominate the scatter in the L-M relation even when a core corrected X-ray luminosity is used, which indicates that the scatter mainly reflects the structure formation history of the clusters. As shown by the clusters with a small number of redshifts, the dynamical masses can be underestimated leading to a biased scaling relation. To investigate the potential of spectroscopic surveys to follow up high-redshift galaxy clusters/groups observed in X-ray surveys for the identifications and mass calibrations, we carried out Monte-Carlo re-sampling of the cluster galaxy redshifts and calibrated the uncertainties of the redshift and dynamical mass estimates when only reduced numbers of galaxy redshifts per cluster are available. The re-sampling considers the SPIDERS and 4MOST configurations, designed for the follow-up of the eROSITA clusters, and was carried out for each cluster at the actual cluster redshift as well as at z=0.2, 0.4, 0.6, and 0.8. For following up very distant cluster/groups, we carried out the mass calibration based on the re-sampling with only 10zs/cluster, and redshift calibration based on the re-sampling with only 5zs/cluster and 10zs/cluster, respectively. Our results demonstrate the power of combining upcoming X-ray and optical spectroscopic surveys for mass calibration. The scatter in the dynamical mass estimates for the clusters with at least ten members is within 50%.
XMM-Newton observations of the Lockman hole: X-ray source catalogue and number counts

Context. The Lockman Hole field represents the sky area of lowest Galac tic line-of-sight column density NH=5.7×10 19 cm −2 . It was observed by the XMM-Newton X-ray observatory in 18 pointings for a total of 1.16 Msec (raw EPIC pn observing time) constituting the deepest XMM-Newton exposure so far. After the removal of time intervals with high particle background, the final e ffective exposure was 637 ks. Aims. We present a catalogue of the X-ray sources detected in the central 0.196 deg 2 of the field and discuss the derived number counts and X-ray colours. Methods. The analysis was performed using the XMM-SAS data analysis package version 6.0. The detection sensitivity and fraction of spurious detections was calibrated using Monte Carlo simulations. Results. In the 0.5‐2.0 keV band, a sensitivity limit (defined as the fa intest detectable source) of 1.9×10 −16 erg cm −2 s −1 was reached. The 2.0‐10.0 keV band and 5.0‐10.0 keV band sensitivity limits were 9×10 −16 erg cm −2 s −1 and 1.8×10 −15 erg cm −2 s −1 , respectively. A total of 409 sources above a detection likelihood of 10 (3.9 sigma) were found within a radius of 15 ′ off the field centre, of which 340, 266, and 98 sources were detected in the soft, hard, and very hard bands, respectively. The number counts in each energy band are in close agreement with results from previous surveys and with the synthesis models of the X-ray background. A 6% of Comptonthick source candidates have been selected from the X-ray colour-colour diagram. This fraction is consistent with the most recent predictions of X-ray background population synthesis models at our flux limits. We also estimated, for the first time, the logN-logS relation for Compton-thick AGN.
Positive Influence of Cooperative Learning and Emotion Regulation on EFL Learners’ Foreign Language Enjoyment

This study approaches foreign language enjoyment (FLE) through the lenses of positive psychology, and in particular, examines how enjoyment is affected by emotion regulation (ER) and two factors concerning cooperative learning (CL) in a classroom climate, namely positive goal interdependence (PGI) and peer personal support (PPS). To achieve this goal, 115 Chinese university freshmen (male 47; female 68) aged between 18 to 20 (M = 18.69; SD = 0.65) were invited to complete a questionnaire. Regression analyses revealed a clear three-factor structure determining the FLE of students learning English as a foreign language (EFL), which are ER, PGI that highlights cooperation, and PPS that emphasizes the interpersonal relationship between peers. It also showed that PGI and PPS significantly influence each other while positively and jointly shaping FLE. The findings suggest that university EFL students with higher ER abilities are more likely to obtain enjoyment in the learning process and that positive interdependence and interpersonal support during CL also play an effective role in deciding students’ FLE. The study not only confirms the importance of ER and CL which may lead to high-level learning enjoyment, but also provides practical implications for the realization of an enjoyable second language acquisition (SLA) experience.
An Individualized Approach to Managing Testosterone Therapy in the Primary Care Setting

Abstract The incidence of testosterone deficiency and the use of testosterone therapy have increased in recent years, and currently the majority of testosterone prescriptions in the United States and Canada are written by primary care physicians. Meanwhile, the range of available testosterone therapy formulations has widened to include buccal tablets, intramuscular injections, transdermal gels, intranasal gel, subcutaneous injections, oral capsules, and subdermal pellets, each with unique pharmacokinetic and clinical characteristics. Despite the growing use of testosterone therapy and its overall efficacy and safety as demonstrated in clinical trials, concerns exist about the potential impact of testosterone therapy on spermatogenesis and fertility, development of prostate cancer, and risk of polycythemia and cardiovascular events. In addition, ongoing research aims to better characterize the effects of testosterone therapy in specific populations, such as patients aged 65 years and older, patients with obesity and type 2 diabetes, and transgender patients. The range of treatment options and the diversity of patients’ goals, preferences, comorbidities, and risk factors necessitate an individualized approach to testosterone therapy that considers each patient’s clinical needs alongside the distinct features of different testosterone formulations.
H i in HO: Hoag's Object revisited

We present new HI observations of Hoag's Object (HO) obtained with the Westerbork Synthesis Radio Telescope. The data show that the luminous optical ring around the elliptical body has a bright HI counterpart that shares the kinematical properties of the optical ring. The entire HI structure is twice as large as the optical ring and shows a mild warp in its outer regions relative to the inner ring. We detect two additional HI sources close in redshift to that of HO, and report on a newly identified SDSS optical companion galaxy. The HI sources are similar to 0.3 and similar to 1 Mpc away in projected distance, and the companion galaxy is also similar to 1 Mpc away. Our main conclusion is that the HI detected in HO shows no indication that this galaxy has experienced a recent (less than similar to 1 Gyr ago) accretion event. At least one of the two additional HI detected objects does not have an optical counterpart. One possibility is that this object is an HI filament left over from an interaction shaping HO, in which case this interaction must also have occurred at least 1-2 Gyr ago.
Performance degradation of Geiger-mode APDs at cryogenic temperatures

Two-phase Cryogenic Avalanche Detectors (CRADs) with THGEM multipliers, optically read out with Geiger-mode APDs (GAPDs), were proposed as potential technique for charge recording in rare-event experiments. In this work we report on the degradation of the GAPD performance at cryogenic temperatures revealed in the course of the study of two-phase CRAD in Ar, with combined THGEM/GAPD-matrix multiplier; the GAPDs recorded secondary scintillation photons from the THGEM holes in the Near Infrared. The degradation effect, namely the loss of the GAPD pulse amplitude, depended on the incident X-ray photon flux. The critical counting rate of photoelectrons produced at the 4.4 mm2 GAPD, degrading its performance at 87 K, was estimated as ∼ 104 s−1. This effect was shown to result from the considerable increase of the pixel quenching resistor of this CPTA-made GAPD type. Though not affecting low-rate rare-event experiments, the observed effect may impose some limitations on the performance of CRADs with GAPD-based optical readout at higher-rate applications.
NEW YOUNG STAR CANDIDATES IN CG4 AND Sa101

The CG4 and Sa101 regions together cover a region of ∼0.5 deg2 in the vicinity of a “cometary globule” that is part of the Gum Nebula. There are seven previously identified young stars in this region; we have searched for new young stars using mid- and far-infrared data (3.6–70 μm) from the Spitzer Space Telescope, combined with ground-based optical data and near-infrared data from the Two Micron All Sky Survey. We find infrared excesses in all six of the previously identified young stars in our maps and identify 16 more candidate young stars based on apparent infrared excesses. Most (73%) of the new young stars are Class II objects. There is a tighter grouping of young stars and young star candidates in the Sa101 region, in contrast to the CG4 region, where there are fewer young stars and young star candidates, and they are more dispersed. Few likely young objects are found in the “fingers” of the dust being disturbed by the ionization front from the heart of the Gum Nebula.
Regular orthogonal basis on Heisenberg group and application to function spaces

In this paper, we construct some compactly supported orthogonal regular wavelet basis on Heisenberg group Hd . Because of the regularity of wavelets, we could use such wavelets to characterize function spaces on Hd , such as bounded mean oscillation space (BMO) space, Hardy space, Besov spaces and Besov–Morrey spaces. Copyright © 2014 John Wiley & Sons, Ltd.
Optimal Sparse Output Feedback Control Design: a Rank Constrained Optimization Approach

We consider the problem of optimal sparse output feedback controller synthesis for continuous linear time invariant systems when the feedback gain is static and subject to specified structural constraints. Introducing an additional term penalizing the number of non-zero entries of the feedback gain into the optimization cost function, we show that this inherently non-convex problem can be equivalently cast as a rank constrained optimization, hence, it is an NP-hard problem. We further exploit our rank constrained approach to define a structured output feedback control feasibility test with global convergence property, then, obtain upper/lower bounds for the optimal cost of the sparse output feedback control problem. Moreover, we show that our problem reformulation allows us to incorporate additional implementation constraints, such as norm bounds on the control inputs or system output, by assimilating them into the rank constraint. We propose to utilize a version of the Alternating Direction Method of Multipliers (ADMM) as an efficient method to sub-optimally solve the equivalent rank constrained problem. As a special case, we study the problem of designing the sparsest stabilizing output feedback controller, and show that it is, in fact, a structured matrix recovery problem where the matrix of interest is simultaneously sparse and low rank. Furthermore, we show that this matrix recovery problem can be equivalently cast in the form of a canonical and well-studied rank minimization problem. We finally illustrate performance of our proposed methodology using numerical examples.
A PERIODICALLY VARYING LUMINOUS QUASAR AT z = 2 FROM THE PAN-STARRS1 MEDIUM DEEP SURVEY: A CANDIDATE SUPERMASSIVE BLACK HOLE BINARY IN THE GRAVITATIONAL WAVE-DRIVEN REGIME

Supermassive black hole binaries (SMBHBs) should be an inevitable consequence of the hierarchical growth of massive galaxies through mergers and the strongest sirens of gravitational waves (GWs) in the cosmos. Yet, their direct detection has remained elusive due to the compact (sub-parsec) orbital separations of gravitationally bound SMBHBs. Here, we exploit a theoretically predicted signature of an SMBHB in the time domain: periodic variability caused by a mass accretion rate that is modulated by the binary’s orbital motion. We report our first significant periodically varying quasar detection from the systematic search in the Pan-STARRS1 (PS1) Medium Deep Survey. Our SMBHB candidate, PSO J334.2028+01.4075, is a luminous radio-loud quasar at z = 2.060, with extended baseline photometry from the Catalina Real-Time Transient Survey, as well as archival spectroscopy from the FIRST Bright Quasar Survey. The observed period (542 ± 15 days) and estimated black hole mass ( log ( M BH / M ⊙ ) = 9.97 ± 0.50 ? > ) correspond to an orbital separation of 7 − 4 + 8 ? > Schwarzschild radii ( ∼ 0.006 − 0.003 + 0.007 ? > pc), assuming the rest-frame period of the quasar variability traces the orbital period of the binary. This SMBHB candidate, discovered at the peak redshift for SMBH mergers, is in a physically stable configuration for a circumbinary accretion disk and within the regime of GW-driven orbital decay. Our search with PS1 is a benchmark study for the exciting capabilities of LSST, which will have orders of magnitude larger survey power and will potentially pinpoint the locations of thousands of SMBHBs in the variable night sky.
Plasma jet generation by flyer disk collision with massive target

In this paper, results from experiments with Al flyer targets (disks with a diameter of 300 µm and a thickness of 6 µm) accelerated at first to high velocities by PALS iodine laser pulses (with an energy of 130 J, pulse duration of 400 ps, a wavelength of 1.315 µm, and laser spot diameter of 250 µm), subsequently creating craters after their collisions with massive Al targets (placed at a distance of the order of 200 µm) are presented. To measure the plasma density evolution a three frame interferometric system was employed. The experimental results demonstrate that the flyer disk–massive target collision generates an axial plasma jet corresponding to a flat shock wave propagating in a massive target. This form of the shock wave was deduced from a crater trapezoidal shape which was reconstructed by means of crater replica technique.
Examining shortened versions of the Social Responsiveness Scale for use in autism spectrum disorder prediction and as a quantitative trait measure: Results from a validation study of 3–5 year old children

Abstract Background The Social Responsiveness Scale (SRS) is a 65‐item measure yielding a continuous score capturing autism‐related traits. Scores based on SRS item subsets have been analytically examined but administration of shortened versions has not been evaluated prospectively. Objective The goal of this study was to compare psychometric properties of two shortened versions of the SRS to the full 65‐item SRS, in young children from both a clinical and general population setting. Methods Study participants (aged 3–5 years) were drawn from the AJ Drexel Autism Institute clinic (n = 154) and Kaiser Permanente Northern California (n = 201) and block randomized to receive either the 16‐item short SRS, a newly developed computer adaptive testing‐SRS, or the published full‐length SRS. Total scores across the three SRS administration methods were scaled to facilitate comparisons. Scores were plotted to assess distributional properties, while Receiver Operating Characteristic analysis was used to estimate Area Under the Curve (AUC) and address predictive ability. Results Overall, distributional properties of the three administration methods were highly comparable, with shortened measures demonstrating similar ability to capture the range of the distribution and case non‐case separation as the full SRS. In addition, AUC values were high (0.91–0.97) and comparable across the administration methods, though there was evidence of difference in predictive ability across measures for females (AUC for full SRS = 0.99 vs. 0.84 for short). Within individual comparisons of short versus full scores (available only for participants at the general population site) suggested underestimation of actual full SRS scores with the CAT‐SRS. Conclusions Our findings broadly support the construct validity and performance of shortened SRS versions examined here, though the full measure may be needed to more accurately assess traits consistent with ASD diagnosis in females. This work suggests opportunities for collection of ASD‐related phenotype in settings where participant burden or feasibility considerations may have otherwise prohibited such measurement.
Structural and T c inhomogeneities inherent to doping in La 2 − x Sr x CuO 4 superconductors and their effects on the precursor diamagnetism

The inhomogeneities inherent to the random distribution of Sr dopants in ${\text{La}}_{2\ensuremath{-}x}{\text{Sr}}_{x}{\text{CuO}}_{4}$ superconductors are probed by measuring the x-ray diffraction linewidths and the Meissner transition widths, and then consistently explained on the grounds of a simple model in which the local Sr content is calculated by averaging over distances close to the in-plane electronic mean free path. By taking into account these intrinsic bulk inhomogeneities with long characteristic lengths (much larger than the superconducting coherence length amplitudes), the precursor diamagnetism measured above ${T}_{c}$, a fingerprint of the superconducting transition own nature, is then explained for all doping levels in terms of the conventional Gaussian-Ginzburg-Landau approach for layered superconductors. These results also suggest that the electronic inhomogeneities observed in the normal state by using surface probes overestimate the ones in the bulk.
Physical Activity and Well-being Status among Employees of University of Medical Sciences

Background: Workplace physical activity plays an important role in employees’ health. As university employees are a population at risk for a sedentary working pattern, this study aimed to investigate the physical activity status of employees of Iran University of Medical Sciences (IUMS) and its subsequent effects on their well-being. Methods: This cross-sectional study included 472 employees from different units of IUMS in Tehran. The participants were selected by a multistage sampling method. Interviews were conducted by using an international physical activity questionnaire, a questionnaire for stages of behavioral change, the World Health Organization Well-being Questionnaire, and a demographic checklist from July to October 2019. Analysis of variance, t test, and logistic regression analysis were used. Data were analyzed using IBM SPSS (Version 21.0). Results: Total physical activity in the study population was 6216.58 ± 5886.09 MET-minutes/week. The mean score of the well-being index was 54.72 ± 22.4; there was an association between sex and location of work with physical activity in domains (p<0.05). The highest prevalence rates for change of stage of physical activity were found in the maintenance stage for men and the contemplation stage for women. There was a significant difference between men and women's well-being index—men reported being more active and energetic than women (p<0.001). Results also revealed that having vigorous physical activity compared with a moderate level could increase the well-being index. Conclusion: Physical activity behavior at the workplace was associated with well-being level. It could, therefore, be postulated that enhancing physical activity may be beneficial to improving well-being in an academic environment.
The Tropical Diurnal Cycle Under Varying States of the Monsoonal Background Wind

The impact of the environmental background wind on the diurnal cycle near tropical islands is examined in observations and an idealized model. Luzon Island in the northern Philippines is used as an observational test case. Composite diurnal cycles of CMORPH precipitation are constructed based on an index derived from the first empirical orthogonal function (EOF) of ERA5 zonal wind profiles. A strong precipitation diurnal cycle and pronounced offshore propagation in the leeward direction tends to occur on days with a weak, offshore prevailing wind. Strong background winds, particularly in the onshore direction, are associated with a suppressed diurnal cycle. Idealized high resolution 2-D Cloud Model 1 (CM1) simulations test the dependence of the diurnal cycle on environmental wind speed and direction by nudging the model base-state toward composite profiles derived from the reanalysis zonal wind index. These simulations can qualitatively replicate the observed development, strength, and offshore propagation of diurnally generated convection under varying wind regimes. Under strong background winds, the land-sea contrast is reduced, which leads to a substantial reduction in the strength of the sea-breeze circulation and precipitation diurnal cycle. Weak offshore prevailing winds favor a strong diurnal cycle and offshore leeward propagation, with the direction of propagation highly sensitive to the background wind in the lower free troposphere. Offshore propagation speed appears consistent with density current theory rather than a direct coupling to a single gravity wave mode, though gravity waves may contribute to a destabilization of the offshore environment.
A UNIFIED MODEL OF THE MAGNETAR AND RADIO PULSAR BURSTING PHENOMENOLOGY

Anomalous X-ray pulsars (AXPs) and soft gamma-ray repeaters (SGRs) are young neutron stars (NSs) characterized by high X-ray quiescent luminosities, outbursts, and, in the case of SGRs, sporadic giant flares. They are believed to be powered by ultra-strong magnetic fields (hence dubbed magnetars). The diversity of their observed behaviors is however not understood and made even more puzzling by the discovery of magnetar-like bursts from “low-field” pulsars. Here, we perform long-term two-dimensional simulations that follow the evolution of magnetic stresses in the crust; these, together with recent calculations of the breaking stress of the NS crust, allow us to establish when starquakes occur. For the first time, we provide a quantitative estimate of the burst energetics, event rate, and location on the NS surface, which bear a direct relevance for the interpretation of the overall magnetar phenomenology. Typically, an “SGR-like” object tends to be more active than an “AXP-like” object or a “high-B radio pulsar,” but there is no fundamental separation among what constitutes the apparent different classes. Among the key elements that create the variety of observed phenomena, age is more important than a small variation in magnetic field strength. We find that outbursts can also be produced in old, lower-field pulsars (B∼ a few ×1012 G), but those events are much less frequent than in young, high-field magnetars.