Miracle-dz/UniFAR-FTUs huggingface dataset:
VEGAS: A VST Early-type GAlaxy Survey. IV. NGC 1533, IC 2038, and IC 2039: An Interacting Triplet in the Dorado Group

This paper focuses on NGC 1533 and the pair IC 2038 and IC 2039 in Dorado a nearby, clumpy, still un-virialized group. We obtained their surface photometry from deep OmegaCAM@ESO-VST images in g and r bands. For NGC 1533, we map the surface brightness down to μg ≃ 30.11 mag arcsec−2 and μr ≃ 28.87 mag arcsec−2 and out to about 4 Re. At such faint levels, the structure of NGC 1533 appears amazingly disturbed with clear structural asymmetry between inner and outer isophotes in the northeast direction. We detect new spiral arm-like tails in the outskirts, which might likely be the signature of a past interaction/merging event. Similarly, IC 2038 and IC 2039 show tails and distortions indicative of their ongoing interaction. Taking advantage of deep images, we are able to detect the optical counterpart to the H i gas. The analysis of the new deep data suggests that NGC 1533 had a complex history made of several interactions with low-mass satellites that generated the star-forming spiral-like structure in the inner regions and are shaping the stellar envelope. In addition, the VST observations also show that the two less luminous galaxies, IC 2038 and IC 2039, are probably interacting each other and IC 2038 could have also interacted with NGC 1533 in the past, which stripped away gas and stars from its outskirts. The new picture emerging from this study is that of an interacting triplet, where the brightest galaxy, NGC 1533, has ongoing mass assembly in the outskirts.
RADIAL STELLAR PULSATION AND THREE-DIMENSIONAL CONVECTION. III. COMPARISON OF TWO-DIMENSIONAL AND THREE-DIMENSIONAL CONVECTION EFFECTS ON RADIAL PULSATION

We have developed a multi-dimensional radiation hydrodynamics code to simulate the interaction of radial stellar pulsation and convection for full-amplitude pulsating models. Convection is computed using large eddy simulations. Here, we perform three-dimensional (3D) simulations of RR Lyrae stars for comparison with previously reported 2D simulations. We find that the time-dependent behavior of the peak convective flux on pulsation phase is very similar in both the 2D and 3D calculations. The growth rates of the pulsation in the 2D calculations are about 0.1% higher than in the 3D calculations. The amplitude of the light curve for a 6500 K RR Lyrae model is essentially the same for our 2D and 3D calculations, as is the rising light curve. There are differences in the slope at various times during falling light.
The impact of magnetic geometry on wave modes in cylindrical plasmas

Both space and laboratory plasmas can be associated with static magnetic field, and the field geometry varies from uniform to non-uniform. This thesis investigates the impact of magnetic geometry on wave modes in cylindrical plasmas. The cylindrical configuration is chosen so as to explore this impact in a tractable but experimentally realisable configuration. Three magnetic geometries are considered: uniform, focused and rippled. These studies suggest suppressing drift waves in a uniformly magnetised plasma by increasing the field strength, enhancing the efficiency of helicon wave production of plasma by using a focused magnetic field, and forming a gap eigenmode on a linear plasma device by introducing a local defect to the system's periodicity, which is useful for understanding the gap-mode formation and interaction with energetic particles in fusion plasmas.
Does wave function collapse cause gravity

We give a twist to the assumption – discussed in various earlier works – that gravity plays a role in the collapse of the wave function. This time we discuss the contrary assumption that the collapse of the wave function plays a role in the emergence of the gravitational field. We start from the mathematical framework of a particular Newtonian gravitational collapse theory proposed by the author longtime ago, and we reconciliate it with the classical equivalence principle.
Suppression of x-rays during an optical outburst of the helium dwarf nova kl dra

KL Dra is a helium-accreting AM CVn binary system with an orbital period close to 25 min. Approximately every 60 d there is a 4-mag optical outburst lasting ∼10 d. We present the most sensitive X-ray observations made of an AM CVn system during an outburst cycle. A series of eight observations were made using XMM–Newton which started shortly after the onset of an optical outburst. We find that X-rays are suppressed during the optical outburst. There is some evidence for a spectral evolution of the X-ray spectrum during the course of the outburst. A periodic modulation is seen in the ultraviolet data at three epochs – this is a signature of the binary orbital or the superhump period. The temperature of the X-ray-emitting plasma is cooler compared to dwarf novae, which may suggest that a wind is the origin of a significant fraction of the X-ray flux.
Landau quantization and mass-radius relation of magnetized White Dwarfs in general relativity

Recently, several white dwarfs have been proposed with masses significantly above the Chandrasekhar limit, known as Super-Chandrasekhar White Dwarfs, to account for the overluminous Type Ia supernovae. In the present work, Equation of State of a completely degenerate relativistic electron gas in magnetic field based on Landau quantization of charged particles in a magnetic field is developed. The mass-radius relations for magnetized White Dwarfs are obtained by solving the Tolman-Oppenheimer-Volkoff equations. The effects of the magnetic energy density and pressure contributed by a density-dependent magnetic field are treated properly to find the stability configurations of realistic magnetic White Dwarf stars.
Association between Short-Term Exposure to Air Pollution and COVID-19 Mortality: A Population-Based Case-Crossover Study Using Individual-Level Mortality Registry Confirmed by Medical Examiners

Background: Studies have suggested links between ambient air pollution and coronavirus 2019 (COVID-19) mortality, yet confirmation by well-designed epidemiological studies with individual data is needed. Objectives: We aimed to examine whether short-term exposure to air pollution is associated with risk of mortality from COVID-19 for those infected with COVID-19. Methods: The Cook County Medical Examiner’s Office reports individual-level data for deaths from COVID-19 that occur in its jurisdiction, which includes all confirmed COVID-19 deaths in Cook County, Illinois. Case-crossover analysis was conducted to estimate the associations of estimated short-term exposures to particulate matter (PM) with aerodynamic diameter ≤2. 5μm (PM2.5) and ozone (O3) on the day of death and up to 21 d before death at location of death with COVID-19. A total of 7,462 deaths from COVID-19 that occurred up to 28 February 2021 were included in the final analysis. We adjusted for potential confounders by time-stratified case-crossover design and by covariate adjustments (i.e., time-invariant factors, meteorological factors, viral transmission, seasonality, and time trend). Results: Of the 7,462 case and 25,457 self-control days, almost all were days with exposure levels below the PM2.5 24-h National Ambient Air Quality Standard (NAAQS) (35 μg/m3); 98.9% had O3 levels below the maximum 8-h NAAQS (35.7 μg/m3 or 70 parts per billion). An interquartile range (IQR) increase (5.2 μg/m3) in cumulative 3-wk PM2.5 exposure was associated with a 69.6% [95% confidence interval (CI): 34.6, 113.8] increase in risk of COVID-19 mortality. An IQR increase (8.2 μg/m3) in 3-d O3 exposure was associated with a 29.0% (95% CI: 9.9, 51.5) increase in risk of COVID-19 mortality. The associations differed by demographics or race/ethnicity. There was indication of modification of the associations by some comorbid conditions. Discussion: Short-term exposure to air pollution below the NAAQS may increase the mortality burden from COVID-19. https://doi.org/10.1289/EHP10836
Spectral energy distribution variations of nearby Seyfert galaxies during AGN watch monitoring programs

FREJA Fellowship - Faculty of Natural Sciences at the University of Copenhagen; Marie Curie International Incoming Fellowship [REA FP7-PEOPLE-2009-IIF, 255190]; Danish Council for Independent Research [DFF 4002-00275]; Dark Cosmology Centre; Danish National Research Foundation; NASA [NAS5-26555]; NASA Office of Space Science [NNX09AF08G]
On non-local energy transfer via zonal flow in the Dimits shift

The two-dimensional Terry–Horton equation is shown to exhibit the Dimits shift when suitably modified to capture both the nonlinear enhancement of zonal/drift-wave interactions and the existence of residual Rosenbluth–Hinton states. This phenomenon persists through numerous simplifications of the equation, including a quasilinear approximation as well as a four-mode truncation. It is shown that the use of an appropriate adiabatic electron response, for which the electrons are not affected by the flux-averaged potential, results in an $\boldsymbol{E}\times \boldsymbol{B}$ nonlinearity that can efficiently transfer energy non-locally to length scales of the order of the sound radius. The size of the shift for the nonlinear system is heuristically calculated and found to be in excellent agreement with numerical solutions. The existence of the Dimits shift for this system is then understood as an ability of the unstable primary modes to efficiently couple to stable modes at smaller scales, and the shift ends when these stable modes eventually destabilize as the density gradient is increased. This non-local mechanism of energy transfer is argued to be generically important even for more physically complete systems.
The H i content of dark matter haloes at z ≈ 0 from ALFALFA

AO is supported by the INFN grant PD 51 INDARK. DA acknowledges support from the Beecroft trust and from the Science and Technology Facilities Council (STFC) through an Ernest Rutherford Fellowship, grant reference ST/P004474/1. The work of FVN is supported by the Simons Foundation. MGJ is supported by a Juan de la Cierva formacion fellowship and also acknowledges support from the grant AYA2015-65973-C3-1-R (MINECO/FEDER, UE) and the >Centro de Excelencia Severo Ochoa> program of the Spanish Science Ministry under grant SEV-2017-0709.
Diagnostic accuracy for self‐reported methamphetamine use versus oral fluid test as the reference standard in a methamphetamine‐dependent intervention trial population

Abstract Aims Treatment of methamphetamine dependence requires monitoring of recent use or abstinence. Self‐report is commonly used for routine monitoring, but the accuracy of self‐report is not established. For the treating clinician, the key accuracy statistic is the negative predictive value (NPV). The study aim was to estimate the NPV of self‐reported non‐use of methamphetamine compared with an oral fluid reference standard. Design, Setting and Participants This study was a secondary (subgroup) analysis from a randomized controlled pharmacotherapy trial. Three Australian outpatient addiction services took part. Particpants were 139 people dependent on methamphetamine. Measurements Weekly oral fluid samples over 12 weeks to determine methamphetamine (and amphetamine) concentrations were used as the reference standard. Self‐report of any methamphetamine use in the previous 7 days by the time‐line follow‐back method was the index test. Standard diagnostic accuracy statistics were calculated for all available paired episodes (n = 1134). Three NPV values were calculated: unadjusted NPV and NPV adjusted for clustering of observations through logistic regression and generalized estimating equation (GEE). We also calculated the NPVs for a range of prevalence rates of methamphetamine use, for the calculated levels of sensitivity and specificity. Findings Sensitivity was 96.4% [95% confidence interval (CI) = 95–97.5], specificity was 63.7% (95% CI = 57.3–69.8) and positive predictive value (PPV) was 90.8% (95% CI = 88.8–92.6). The unadjusted NPV was 82.7% (95% CI = 76.5–87.9), adjusted NPV by logistic regression 82.7% (95% CI = 73.9–91.5) and GEE 76.8% (95% CI = 66.8–86.8). At a methamphetamine use prevalence of 5%, the estimated NPV would be 99.7% (95% CI = 99.6–99.9) and at 95% prevalence, 48.2% (95% CI = 39.6–57.0). Conclusions Self‐report of no recent methamphetamine use appears to be sufficiently accurate to be clinically useful at the expected prevalence rates of methamphetamine use in clinical treatment settings. If generalizable to clinical settings, where these tests are routinely conducted, this may permit a reduction in the frequency and cost of oral fluid assays.
A spectroscopic analysis of the chemically peculiar star HD 207561

In this paper we present a high-resolution spectroscopic analysis of the chemically peculiar star HD 207561. During a survey programme to search for new rapidly oscillating Ap (roAp) stars in the Northern hemisphere, Joshi et al. observed significant photometric variability on two consecutive nights in the year 2000. The amplitude spectra of the light curves obtained on these two nights showed oscillations with a frequency of 2.79 mHz (P ∼ 6 min). However, subsequent follow-up observations could not confirm any rapid variability. In order to determine the spectroscopic nature of HD 207561, high-resolution spectroscopic and spectropolarimetric observations were carried out. A reasonable fit of the calculated Hβ line profile to the observed one yields an effective temperature (T eff) and surface gravity (logg) of 7300 K and 3.7 dex, respectively. The derived projected rotational velocity (v sini) for HD 207561 is 74 km s −1 , indicative of a relatively fast rotator. The position of HD 207561 in the Hertzsprung–Russell diagram implies that this is slightly evolved from the main-sequence and located well within the δ-Scuti instability strip. The abundance analysis indicates the star has slight underabundances of Ca and Sc and mild overabundances of iron-peak elements. The spectropolarimetric study of HD 207561 shows that the effective magnetic field is within the observational error of 100 G. The spectroscopic analysis revealed that the star has most of the characteristics similar to an Am star, rather than an Ap star, and that it lies in the δ-Scuti instability strip; hence roAp pulsations are not expected in HD 207561, but low-overtone modes might be excited.
Measurement of the $e^+e^- \to \omega\eta$ cross section below $\sqrt{s}=2$ GeV

The cross section for the process $e^+e^- \to \omega\eta$ is measured in the center-of-mass energy range 1.34--2.00 GeV. The analysis is based on data collected with the SND detector at the VEPP-2000 $e^+e^-$ collider. The measured $e^+e^- \to \omega\eta$ cross section is the most accurate to date. A significant discrepancy is observed between our data and previous BABAR measurement.
Breathing-like excited state of the Hoyle state in C 12

The existence of the ${0}_{3}^{+}$ and ${0}_{4}^{+}$ states around 10 MeV excitation energy in $^{12}\mathrm{C}$ is confirmed by a fully microscopic $3\ensuremath{\alpha}$ cluster model. Firstly, a generator coordinate method (GCM) calculation is performed by superposing optimized $2\ensuremath{\alpha}+\ensuremath{\alpha}$ Tohsaki-Horiuchi-Schuck-R\"opke (THSR) wave functions with the radius-constraint method. The obtained two excited ${0}^{+}$ states above the Hoyle state are consistent with the recently observed states by experiment. Secondly, a variational calculation using the single $2\ensuremath{\alpha}+\ensuremath{\alpha}$ THSR wave function orthogonalized to the ground and Hoyle states is made and it also supports the existence of the ${0}_{3}^{+}$ state obtained by the GCM calculation. The analysis of the obtained ${0}_{3}^{+}$ state is made by studying its $2\ensuremath{\alpha}\ensuremath{-}\ensuremath{\alpha}$ reduced width amplitude, its $2\ensuremath{\alpha}$ correlation function, and the large monopole matrix element between this state and the Hoyle state, which shows that this ${0}_{3}^{+}$ state is a breathing-like excited state of the Hoyle state. This character of the ${0}_{3}^{+}$ state is very different from the ${0}_{4}^{+}$ state which seems to have a bent-arm $3\ensuremath{\alpha}$ structure.
Crossover from weak to strong pairing in unconventional superconductors

Superconductors are classified by their pairing mechanism and the coupling strength, measured as the ratio of the energy gap, $2\ensuremath{\Delta}$, to the critical temperature, ${T}_{\mathrm{c}}$. We present an extensive comparison of the $2\ensuremath{\Delta}/{k}_{\mathrm{B}}{T}_{\mathrm{c}}$ ratios among many single- and multiband superconductors from simple metals to high-${T}_{\mathrm{c}}$ cuprates and iron pnictides. Contrary to the recently suggested universality of this ratio in Fe-based superconductors, we find that the coupling in pnictides ranges from weak, near the BCS limit, to strong, as in cuprates, bridging the gap between these two extremes. Moreover, for Fe- and Cu-based materials, our analysis reveals a universal correlation between the gap ratio and ${T}_{\mathrm{c}}$, which is not found in conventional superconductors and therefore supports a common unconventional pairing mechanism in both families. An important consequence of this result for ferropnictides is that the separation in energy between the excitonic spin-resonance mode and the particle-hole continuum, which determines the resonance damping, no longer appears independent of ${T}_{\mathrm{c}}$.
Rating Dyspnea and Pain: “No” is Not Always “Zero”

Nurses routinely assess pain in hospitalized patients; similar assessment of dyspnea is increasing. Most nurses start with a yes–no question when assessing pain or dyspnea; many record “no” as a zero rating, skipping the rating scale. We tested the hypothesis that recording “no” answers as “zero” fails to detect the symptoms that would have been detected with a rating scale. Nurses asked 60 patients yes–no questions about the presence of dyspnea and pain, then asked patients to rate the symptoms using a 0–10 scale. All “yes” answers were followed by a concordant rating (i.e., greater than zero). More than 25% of “no” answers were followed by a discordant rating (> zero). Documenting “no” as “zero” missed information potentially useful in care planning; patients who rate dyspnea above zero are at greater risk of adverse outcomes. This information can also provide opportunity to start a discussion with patients who may benefit from symptom management.
Mst1 silencing alleviates hypertensive myocardial injury associated with the augmentation of microvascular endothelial cell autophagy

The activation of mammalian ste20-like kinase1 (Mst1) is a crucial event in cardiac disease development. The inhibition of Mst1 has been recently suggested as a potential therapeutic strategy for the treatment of diabetic cardiomyopathy. However, whether silencing Mst1 also protects against hypertensive (HP) myocardial injury, or the mechanisms through which this protection is conferred are not yet fully understood. The present study aimed to explore the role of Mst1 in HP myocardial injury using in vivo and in vitro hypertension (HP) models. Angiotensin II (Ang II) was used to establish HP mouse and cardiac microvascular endothelial cell (CMEC) models. CRISPR/adenovirus vector transfection was used to silence Mst1 in these models. Using echocardiography, hematoxylin and eosin staining, Masson's trichrome staining, the enzyme-linked immunosorbent assay detection of inflammatory factors, the enzyme immunoassay detection of oxidative stress markers, terminal deoxynucleotidyl transferase dUTP nick-end labeling staining, scanning electron microscopy, transmission electron microscopy, as well as immunofluorescence and western blot analysis of the autophagy markers, p62, microtubule-associated proteins 1A/1B light chain 3B and Beclin-1, it was found that Ang II induced HP myocardial injury with impaired cardiac function, increased the expression of inflammatory factors, and elevated oxidative stress in mice. In addition, it was found that Ang II reduced autophagy, enhanced apoptosis, and disrupted endothelial integrity and mitochondrial membrane potential in cultured CMECs. The silencing of Mst1 in both in vivo and in vitro HP models attenuated the HP myocardial injury. On the whole, these findings suggest that Mst1 is a key contributor to HP myocardial injury through the regulation of cardiomyocyte autophagy.
SCATTERING POLARIZATION IN THE Ca ii INFRARED TRIPLET WITH VELOCITY GRADIENTS

Magnetic field topology, thermal structure, and plasma motions are the three main factors affecting the polarization signals used to understand our star. In this theoretical investigation, we focus on the effect that gradients in the macroscopic vertical velocity field have on the non-magnetic scattering polarization signals, establishing the basis for general cases. We demonstrate that the solar plasma velocity gradients may have a significant effect on the linear polarization produced by scattering in chromospheric spectral lines. In particular, we show the impact of velocity gradients on the anisotropy of the radiation field and on the ensuing fractional alignment of the Ca ii levels, and how they can lead to an enhancement of the zero-field linear polarization signals. This investigation remarks on the importance of knowing the dynamical state of the solar atmosphere in order to correctly interpret spectropolarimetric measurements, which is important, among other things, for establishing a suitable zero-field reference case to infer magnetic fields via the Hanle effect.
From deep-inelastic structure functions to two-photon dilepton production in proton-proton collisions

We compare two different approaches used for calculating cross sections for the two-photon $p p \to l^+ l^- X$ process. In one of the approaches photon is treated as a collinear parton in the proton. In the second approach a recently proposed $k_T$-factorization method is used. In this presentation we discuss sensitivity of the results to the choice of structure function parametrization and experimental cuts in the $k_T$-factorization approach. We compare results of our calculations with recent experimental data for dilepton production and find that in most cases the contribution of the photon-photon mechanism is rather small. We discuss how to enhance the photon-photon contribution. We also compare our results to those of recent measurements of exclusive and semi-exclusive $e^+ e^-$ pair production with certain experimental data by the CMS collaboration.