Miracle-dz/UniFAR-FTUs huggingface dataset:
Bayesian Meta-analysis of Direct Oral Anticoagulation Versus Vitamin K Antagonists With or Without Concomitant Antiplatelet After Transcatheter Aortic Valve Implantation in Patients With Anticoagulation Indication

Patients undergoing transcatheter aortic valve implantation (TAVI) commonly have co-morbidities requiring anticoagulation. However, the optimal post-procedural anticoagulation regimen is not well-established. This meta-analysis investigates safety and efficacy outcomes of direct oral anticoagulants (DOACs) and Vitamin K Antagonist (VKA), with or without concomitant antiplatelet therapy. We searched EMBASE and MEDLINE for appropriate studies. Subgroup analyses were performed for anticoagulant monotherapy and combined therapy with antiplatelet agents. Eleven studies (6359 patients) were included. Overall, there were no differences between DOACs and VKA for all-cause mortality (Odds Ratio [OR]: .69; Credible Interval [CrI]: .40–1.06), cardiovascular-related mortality (OR: .76; Crl: .13–3.47), bleeding (OR: .95; CrI: .75–1.17), stroke (OR: 1.04; CrI: .65–1.63), myocardial infarction (OR: 1.51; CrI: .55–3.84), and valve thrombosis (OR: .29; CrI: .01–3.54). For DOACs vs VKA monotherapy subgroup, there were no differences in outcomes. For the combined therapy subgroup, there was decreased odds of all-cause mortality in the DOACs group compared with the VKA group (OR: .13; CrI: .02–.65), but no differences for bleeding and stroke. DOACs and VKA have similar safety and efficacy profiles for post-TAVI patients with anticoagulation indication. However, if concomitant antiplatelet therapy is required, DOACs were more favorable than VKA for all-cause mortality.
HUBBLE SPACE TELESCOPE OBSERVATIONS OF FIELD ULTRACOOL DWARFS AT HIGH GALACTIC LATITUDE

We present a sample of 17 newly discovered ultracool dwarf candidates later than ∼M8, drawn from 231.90 arcmin2 of Hubble Space Telescope Wide Field Camera 3 infrared imaging. By comparing the observed number counts for 17.5 ⩽ J125 ⩽ 25.5 AB mag to an exponential disk model, we estimate a vertical scale height of zscl = 290 ± 25 (random) ± 31 (systematic) pc for a binarity fraction of fb = 0. While our estimate is roughly consistent with published results, we suggest that the differences can be attributed to sample properties, with the present sample containing far more substellar objects than previous work. We predict the object counts should peak at J125 ∼ 24 AB mag due to the exponentially declining number density at the edge of the disk. We conclude by arguing that trend in scale height with spectral type may breakdown for brown dwarfs since they do not settle onto the main sequence.
The impact of numerical oversteepening on the fragmentation boundary in self-gravitating disks

Context. It is still an open issue whether a self-gravitating accretion disk fragments. There are many different physical and numerical explanations for fragmentation, but simulations often show a non-convergent behavior for ever better resolution. Aims. We investigate the influence of different numerical limiters in Godunov type schemes on the fragmentation boundary in self- gravitating disks. Methods. We compare the linear and non-linear outcome in two-dimensional shearingsheet simulations using the VANLEER and the SUPERBEE limiter. Results. We show that choosing inappropriate limiting functions to handle shock-capturing in Godunov type schemes can lead to an overestimation of the surface density in regions with shallow density gradients. The effect amplifies itself on timescales comparable to the dynamical timescale even at high resolutions. This is exactly the environment, where clumps are expected to form. The effect is present without, but scaled up by, self-gravity and also does not depend on cooling. Moreover it can be backtracked to a well known effect called oversteepening. If the effect is also observed in the linear case, the fragmentation limit is shifted to larger values of the critical cooling timescale.
Similar Slow Component of Oxygen Uptake and Ventilatory Efficiency between an Aerobic Dance Session on an Air Dissipation Platform and a Constant-Load Treadmill Test in Healthy Women

Simple Summary The evaluation of the kinetics of oxygen uptake is considered an essential practice to analyze the effect of exercise intensity, mainly in endurance exercise. This study aimed to compare the slow component of oxygen uptake, ventilatory efficiency, blood lactate concentration, and the rating of perceived exertion between an aerobic dance session on an air dissipation platform and a constant-load treadmill test. Seventeen young adult and healthy women (aged 23.5 ± 2.2 years) completed three evaluation sessions. In session 1, an incremental test to exhaustion was completed. In sessions 2 and 3, the participants were randomly assigned to the aerobic dance session on an air dissipation platform or to a treadmill test at a constant-load corresponding to the first ventilatory threshold. No significant differences were found between the constant-load treadmill test and aerobic dance session on an air dissipation platform regarding the slow component of oxygen uptake, ventilatory efficiency, and the rating of perceived exertion. Higher blood lactate concentrations were observed in the aerobic dance session on an air dissipation platform than in the constant-load treadmill test. In conclusion, two different exercise modalities elicited similar slow components of oxygen uptake, ventilatory efficiency, and ratings of perceived exertion, even though the blood lactate concentrations were different. Abstract There is a lack of evidence about the slow component of oxygen consumption (V.O2sc) and ventilatory efficiency (slope VE·VCO2−1) during an aerobic dance (AD) session on an air dissipation platform (ADP) despite the key role played in endurance exercises. This research was designed to assess V.O2sc, ventilatory efficiency, and blood lactate concentration by comparing two exercise modes: AD session on an ADP versus treadmill test at a constant-load intensity of the first ventilatory threshold (VT1). In the first session, an incremental treadmill test was completed. In sessions 2 and 3, the participants were randomly assigned to the AD session on an ADP or to a treadmill constant-load test at VT1 intensity to determine their cardioventilatory responses. In addition, their blood lactate levels and ratings of perceived exertion (RPE, CR-10) were evaluated. No significant differences were found between the constant-load treadmill test and AD session on an ADP with respect to V.O2sc, VE VCO2−1 slope, and RPE (p > 0.05). Higher blood lactate concentrations were observed in an AD session on an ADP than in a constant-load treadmill test at 10 min (p = 0.003) and 20 min (p < 0.001). The two different exercise modalities showed similar V.O2sc and VE·VCO2−1 slope, even though the blood lactate concentrations were different.
The remarkable outburst of the highly evolved post- period- minimum dwarf nova SSS J122221.7-311525

We report extensive 3-yr multiwavelength observations of the WZ Sge-type dwarf nova SSS J122221.7−311525 during its unusual double superoutburst, the following decline and in quiescence. The second segment of the superoutburst had a long duration of 33 d and a very gentle decline with a rate of 0.02 mag d−1, and it displayed an extended post-outburst decline lasting at least 500 d. Simultaneously with the start of the rapid fading from the superoutburst plateau, the system showed the appearance of a strong near-infrared excess resulting in very red colours, which reached extreme values (B − I ≃ 1.4) about 20 d later. The colours then became bluer again, but it took at least 250 d to acquire a stable level. Superhumps were clearly visible in the light curve from our very first time-resolved observations until at least 420 d after the rapid fading from the superoutburst. The spectroscopic and photometric data revealed an orbital period of 109.80 min and a fractional superhump period excess ≲0.8 per cent, indicating a very low mass ratio q ≲ 0.045. With such a small mass ratio the donor mass should be below the hydrogen-burning minimum mass limit. The observed infrared flux in quiescence is indeed much lower than is expected from a cataclysmic variable with a near-main-sequence donor star. This strongly suggests a brown-dwarf-like nature for the donor and that SSS J122221.7−311525 has already evolved away from the period minimum towards longer periods, with the donor now extremely dim.
Asteroseismology of 1523 misclassified red giants using Kepler data

We analysed solar-like oscillations in 1523 $\textit{Kepler}$ red giants which have previously been misclassified as subgiants, with predicted $\nu_{\rm max}$ values (based on the Kepler Input Catalogue) between 280$\mu$Hz to 700$\mu$Hz. We report the discovery of 626 new oscillating red giants in our sample, in addition to 897 oscillators that were previously characterized by Hekker et al. (2011) from one quarter of $\textit{Kepler}$ data. Our sample increases the known number of oscillating low-luminosity red giants by $26\%$ (up to $\sim$ 1900 stars). About three quarters of our sample are classified as ascending red-giant-branch stars, while the remainder are red-clump stars. A novel scheme was applied to determine $\Delta \nu$ for 108 stars with $\nu_{\rm max}$ close to the Nyquist frequency (240$\mu$Hz < $\nu_{\rm max}$ < 320$\mu$Hz). Additionally, we identified 47 stars oscillating in the super-Nyquist frequency regime, up to 387$\mu$Hz, using long-cadence light curves. We show that the misclassifications are most likely due to large uncertainties in KIC surface gravities, and do not result from the absence of broadband colors or from different physical properties such as reddening, spatial distribution, mass or metallicity. The sample will be valuable to study oscillations in low-luminosity red giants and to characterize planet candidates around those stars.
Dark halo response and the stellar initial mass function in early-type and late-type galaxies

We investigate the origin of the relations between stellar mass and optical circular velocity for early-type galaxies (ETGs) and late-type galaxies (LTGs) – the Faber–Jackson (FJ) and Tully–Fisher (TF) relations. We combine measurements of dark halo masses (from satellite kinematics and weak lensing), and the distribution of baryons in galaxies (from a new compilation of galaxy scaling relations), with constraints on dark halo structure from cosmological simulations. The principal unknowns are the halo response to galaxy formation and the stellar initial mass function (IMF). The slopes of the TF and FJ relations are naturally reproduced for a wide range of halo response and IMFs. However, models with a universal IMF and universal halo response cannot simultaneously reproduce the zero-points of both the TF and FJ relations. For a model with a universal Chabrier IMF, LTGs require halo expansion, while ETGs require halo contraction. A Salpeter IMF is permitted for high-mass (σ≳ 180 km s−1) ETGs, but is inconsistent for intermediate masses, unless Vcirc(Re)/σe≳ 1.6. If the IMF is universal and close to Chabrier, we speculate that the presence of a major merger may be responsible for the contraction in ETGs while clumpy accreting streams and/or feedback leads to expansion in LTGs. Alternatively, a recently proposed variation in the IMF disfavours halo contraction in both types of galaxies. Finally we show that our models naturally reproduce flat and featureless circular velocity profiles within the optical regions of galaxies without fine-tuning.
Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

Context. A complex of Hα emitting blobs with strong FUV excess is associated to the dIrr galaxy VCC 1217/IC 3418 (Hester et al. 2010, ApJ, 716, L14), and extends up to 17 Kpc in the southeast direction. These outstanding features can be morphologically divided into diffuse filaments and compact knots, where most of the star formation activity traced by Hα takes place. Aims. We investigate the properties of the galaxy and the blobs using a multiwavelength approach to constrain their origin. Methods. We collected publicly available data in UV and Hα and observed the scene in the optical U ,g ,r,i bands with LBT. The photometric data allows evaluation of the star formation rate and performance of a SED fitting separately for the galaxy and the blobs in order to constrain their stellar population age. Moreover we analyzed the color and luminosity profile of the galaxy and its spectrum to investigate its recent interaction with the Virgo cluster. Results. Our analysis confirms that the most plausible mechanism for the formation of the blobs is ram pressure stripping by the Virgo cluster IGM. The galaxy colors, luminosity profile and SED are consistent with a sudden gas depletion in the last few hundred Myr. The SED fitting of the blobs constrains their ages in <400 Myr.
MICROWAVE OBSERVATIONS OF EDGE-ON PROTOPLANETARY DISKS: PROGRAM OVERVIEW AND FIRST RESULTS

We are undertaking a multi-frequency Expanded Very Large Array (EVLA) survey of edge-on protoplanetary disks to probe the growth of solids in each disk, sedimentation of such material into the disk midplane, and the connection of these phenomena to the planet formation process. The projection of edge-on disk systems along our line of sight enables a study of the vertical stratification of large grains with fewer model dependencies than would be required for disks that are more face-on. Robust studies of the spatial distribution of grains up to ≈1 cm in size are possible with the wavelength range and sensitivity of the EVLA. In this contribution, we describe target selection and observational strategies. First results concerning the Class 0 source IRAS 04368+2557 (L1527 IRS) are presented, including a study of this source's 8.46 GHz continuum variability over short and long time baselines and an indication that its protoplanetary disk may have a dearth of pebble-sized grains.
The scaling relation between the mass of supermassive black holes and the kinetic energy of random motions of the host galaxies

Context. Thanks to the improved angular resolution of modern telescopes and kinematic models, the existence of supermassive black holes (SMBHs) in the inner part of galaxies, regardless their morphology and nuclear activity, has been established on quite solid grounds. A possible correlation between the mass of SMBHs (M•) and the evolutionary state of their host galaxies is expected and is currently under a heated debate. Aims. Based on the recent 2D decomposition of 3.6 µm Spiter/IRAC images of local late- and early-type galaxies with Mmeasurements, we investigated various scaling laws, studying what the best predictor of the mass of the central black holes is. In particular, we focused on the MMG� 2 law, that is the relation between the mass of SMBHs and the kinetic energy of random motions of the corresponding host galaxies, MG is the mass andthe velocity dispersion of the host galaxy (bulge). Methods. In order to find the best fit for each of the scaling laws examined, we performed a least-squares regression of Mon x for the considered sample of galaxies, x being a whatever known parameter of the galaxy bulge. For this purpose, we made use of both the linear regression LINMIX ERR and FITEXY methods. Results. Our analysis shows that MMG� 2 law fits the examined experimental data successfully as much as the other known scaling laws (all correlations have similar intrinsic scatters within the errors) and shows a value of � 2 (estimated by FITEXY) better than the others, a result which is consistent with previous determinations at shorter wavelengths. This means that a combination ofand MG (or Re) could be necessary to drive the correlations between Mand other bulge properties. This issue has been investigated by a careful, although not fully conclusive, analysis of the residuals of the various relations. Conclusions. In order to avoid rushed conclusions on galaxy activity and evolution, the indirect inferring of the masses of the supermassive black holes from the kinetic energy of random motions via the MMG� 2 relation should be considered, especially when applied to higher redshift galaxies (z > 0.01). This statement is suggested by a reanalysis of the Sloan Digital Sky Survey (SDSS) data used to study the black hole growth in the nearby Universe. By adopting the MMG� 2 relation instead of the M• � relation, a radio-quiet/radio-loud dichotomy appears in the SMBH mass distribution of the corresponding SDSS early-type AGN galaxies.
Trends of re-operative coronary artery bypass grafting: A two-decade experience

Background The prevalence of redo coronary artery bypass grafting has markedly changed over the last two decades. We aim to assess the trends of redo coronary artery bypass grafting and clinical outcomes of redo coronary artery bypass grafting over two different periods. Methods This is a retrospective, metachronous, observational study of patients who underwent redo coronary artery bypass grafting between January 1998 through December 2004 and January 2005 through September 2021 who were categorized into group 1 and group 2, respectively. The trends in the prevalence of redo coronary artery bypass grafting, and 30-day outcomes were analyzed. Results A total of 261 patients underwent a redo coronary artery bypass grafting. Group 1 and group 2 included 114 and 147 patients, respectively. 62.59% of group 2 patients underwent off-pump coronary artery bypass grafting compared to 6.14% in group 1 (p < 0.01). The patients undergoing redo coronary artery bypass grafting in group 2 were significantly older (60.65 ± 7.78 years vs. 50.99 ± 7.66 years, p < 0.001) and were more likely to be hypertensive (49.66% vs. 29.82%, p < 0.001). There was no significant difference in the proportion of diabetes (p = 0.82), smoking (p = 0.24), dyslipidemia (p = 0.64), and preoperative myocardial infarction (p = 0.14). The proportion of patients who presented post-PCI was significantly higher in group 2 (27.89% vs. 10.53%, p < 0.001). There was also a shift in the usage of grafts from the left internal thoracic artery to the saphenous vein graft (p < 0.001). Conclusion The annual rate of redo coronary artery bypass grafting was declining but has now reached a plateau. The current outcomes of patients undergoing redo coronary artery bypass grafting are comparable to that of the earlier times despite a higher co-morbidity burden in patients of recent times.
ANGULAR MOMENTUM OF DWARF GALAXIES

We present measurements of baryonic mass and specific angular momentum (sAM) in 14 rotating dwarf Irregular (dIrr) galaxies from the LITTLE THINGS sample. These measurements, based on 21 cm kinematic data from the Very Large Array and stellar mass maps from the Spitzer Space Telescope, extend previous AM measurements by more than two orders of magnitude in . The dwarf galaxies show systematically higher values than expected from the scaling of spiral galaxies, representative of a scale-free galaxy formation scenario. This offset can be explained by decreasing baryon mass fractions (where is the dynamical mass) with decreasing (for ). We find that the sAM of neutral atomic hydrogen (H i) alone is about 2.5 times higher than that of the stars. The M–j relation of H i is significantly steeper than that of the stars, as a direct consequence of the systematic variation of the H i fraction with .
Enhancing Anti-G Antibody Induction by a Live Single-Cycle Prefusion F—Expressing RSV Vaccine Improves In Vitro and In Vivo Efficacy

The human respiratory syncytial virus (RSV) is a major cause of severe respiratory tract disease, and a vaccine is not available. We previously reported a novel live vaccine expressing prefusion-stabilized fusion protein (preF) in place of the native F protein (RSV-preFΔCT). As preF is non-functional, RSV-preFΔCT was amplified in a production line expressing a functional substitute, and exhibited a single-cycle replication phenotype, which holds several unique potential advantages. RSV-preFΔCT prevented shedding and lung pathology after viral challenge in mice, but induced low levels of anti-attachment protein (G) antibodies (Abs). Given the significant contributions of anti-G Abs toward disease prevention, we generated modifications to RSV-preFΔCT in an effort to induce higher anti-G Ab levels. The Ab levels were monitored after the prime-boost vaccination of mice with modified vaccines. The most successful modification for enhancing induced anti-G Abs was seen with the placement of G in the first genome position. This vaccine also reduced the pathology after challenge with a high dose of wt RSV, and outperformed the sera from wt RSV-vaccinated mice in in vitro neutralization. Thus, raising the anti-G Ab levels induced by RSV-preFΔCT enhanced efficacy in vitro and in vivo, and constitutes an important next step in developing a live, single-cycle, efficacious vaccine for the human population.
Lorentz-violation-induced arrival delays of cosmological particles

We point out that previous studies of possible Lorentz-violating effects in astronomical time-of-flight data did not take into account the entire implications of the universe’s cosmological expansion. We present the derivation of the accurate formulation of the problem and show that the resulting correction of the limits on Lorentz violation is significant.
Inside the Bondi radius of M87

Chandra X-ray observations of the nearby brightest cluster galaxy M87 resolve the hot gas structure across the Bondi accretion radius of the central s upermassive black hole, a measurement possible in only a handful of systems but complicated by the bright nucleus and jet emission. By stacking only short frame-time observations to limit pileup, and after subtracting the nuclear PSF, we analysed the X-ray gas properties within the Bondi radius at 0.12− 0.22 kpc (1.5− 2.8 arcsec), depending on the black hole mass. Within 2 kpc radius, we detect two significant temperature components, which are consistent with constant values of 2 keV and 0.9 keV down to 0.15 kpc radius. No evidence was found for the expected temperature increase within ∼ 0.25 kpc due to the influence of the SMBH. Within the Bondi radius, the density profile is consistent with ρ∝r −1 . The lack of a temperature increase inside the Bondi radius suggests that the hot gas structure is not di ctated by the SMBH’s potential and, together with the shallow density profile, shows that th e classical Bondi rate may not reflect the accretion rate onto the SMBH. If this density profi le extends in towards the SMBH, the mass accretion rate onto the SMBH could be at least two orders of magnitude less than the Bondi rate, which agrees with Faraday rotation measurements for M87. We discuss the evidence for outflow from the hot gas and the cold gas disk and f or cold feedback, where gas cooling rapidly from the hot atmosphere could feed the cirumnuclear disk and fuel the SMBH. At 0.2 kpc radius, the cooler X-ray temperature component represents ∼ 20% of the total Xray gas mass and, by losing angular momentum to the hot gas component, could provide a fuel source of cold clouds within the Bondi radius.
Curved Herbig-Haro Jets: Simulations and Experiments

Herbig-Haro jets often show some degree of curvature along their path, in many cases produced by the ram pressure of a side wind. We present simulations of both laboratory and astrophysical curved jets and results from laboratory experiments. We discuss the properties and similarities of the laboratory and astrophysical flows, which show the formation of internal shocks and working surfaces. In particular, the results illustrate how the breakup of the bow shock and clumps in the flow are produced without invoking jet variability; we also discuss how jet rotation reduces the growth of the Rayleigh-Taylor instability in curved jets.