Sazuna/UAT_keywords huggingface dataset:
What Does the Geometry of the Hβ BLR Depend On?. We combine our dynamical modeling black-hole mass measurements from the Lick AGN Monitoring Project 2016 sample with measured cross-correlation time lags and line widths to recover individual scale factors, f, used in traditional reverberation-mapping analyses. We extend our sample by including prior results from Code for AGN Reverberation and Modeling of Emission Lines (CARAMEL) studies that have utilized our methods. Aiming to improve the precision of black-hole mass estimates, as well as uncover any regularities in the behavior of the broad-line region (BLR), we search for correlations between f and other AGN/BLR parameters. We find (i) evidence for a correlation between the virial coefficient ${\mathrm{log}}_{10}({f}_{\mathrm{mean},\sigma })$ and black-hole mass, (ii) marginal evidence for a similar correlation between ${\mathrm{log}}_{10}({f}_{\mathrm{rms},\sigma })$ and black-hole mass, (iii) marginal evidence for an anticorrelation of BLR disk thickness with ${\mathrm{log}}_{10}({f}_{\mathrm{mean},\mathrm{FWHM}})$ and ${\mathrm{log}}_{10}({f}_{\mathrm{rms},\mathrm{FWHM}})$ , and (iv) marginal evidence for an anticorrelation of inclination angle with ${\mathrm{log}}_{10}({f}_{\mathrm{mean},\mathrm{FWHM}})$ , ${\mathrm{log}}_{10}({f}_{\mathrm{rms},\sigma })$ , and ${\mathrm{log}}_{10}({f}_{\mathrm{mean},\sigma })$ . Last, we find marginal evidence for a correlation between line-profile shape, when using the root-mean-square spectrum, ${\mathrm{log}}_{10}{(\mathrm{FWHM}/\sigma )}_{\mathrm{rms}}$ , and the virial coefficient, ${\mathrm{log}}_{10}({f}_{\mathrm{rms},\sigma })$ , and investigate how BLR properties might be related to line-profile shape using CARAMEL models.

Keywords: Supermassive black holes, Reverberation mapping, Active galaxies, Seyfert galaxies, Active galactic nuclei
Understanding the Chemical Evolution of Blue Edge-on Low Surface Brightness Galaxies. We present a sample of 330 blue edge-on low surface brightness galaxies (ELSBGs). To understand the chemical evolution of ELSBGs, we derived the gas-phase abundance and the [α/Fe] ratio. Compared with star-forming galaxies, ELSBGs show a flatter trend in the mass-metallicity (M *-Z) relation, which suggests that the oxygen abundance enhancement is inefficient. We focused on 77 ELSBGs with H I data and found that the closed-box model cannot explain their gas fraction and metallicity relation, which implies that infall and/or outflow is needed. We derived the [α/Fe] ratio of normal ELSBG (&lt;109.5 M ⊙) and massive ELSBG (&gt; = 109.5 M ⊙) using single stellar population grids from the MILES stellar library. The mean [α/Fe] ratios are 0.18 and 0.4 for normal ELSBG and massive ELSBG, respectively. We suggest that the long timescales of star formation and/or metal-rich gas outflow events caused by SNe Ia winds are likely to be responsible for the α-enhancement of massive ELSBGs.

Keywords: Galaxy abundances, Metallicity, Chemical abundances
Third Epoch HST Imaging of a Nonradiative Shock in the Cygnus Loop Supernova Remnant. We present new HST/WFC3 optical images of a region in the northeastern part of the Cygnus Loop supernova remnant, which includes a well-studied Balmer-line filament. These data represent the third epoch of HST Hα imaging and a second epoch of [O III] λ5007 imaging of that particular filament. The Hα images were used to measure the proper motions at various locations along the shock front, and the values ranged from 55 to 85 mas yr-1 with a median value of 70 mas yr-1, which corresponds to a shock velocity of 240 km s-1. The proper motions between epochs 1 and 2 were the same as between epochs 2 and 3, implying that there has been no measurable deceleration of the shock in the 22 yr period between the first and third epochs. The range of proper motions (and therefore shock velocities) along the filament indicate variations of over a factor of two in the preshock density. The [O III] emission is prominent toward one end of the filament where the shock has transitioned from nonradiative to radiative. The proper motion is smaller than for the Hα filaments, and it corresponds to a shock velocity of about 155 km s-1. The images obtained about 18 yr apart show that the [O III] morphology has not changed, which places limits on any short-timescale variations due to catastrophic cooling or thermal instabilities. We find that the effective shock age is less than the eddy turnover timescale, which implies that turbulence has not yet influenced the dynamics of the shock.

Keywords: Supernova remnants, Shocks, Filamentary nebulae
Planetesimal Growth in Evolving Protoplanetary Disks: Constraints from the Pebble Supply. In the core accretion model, planetesimals grow by mutual collisions and engulfing millimeter-to-centimeter particles, i.e., pebbles. Pebble accretion can significantly increase the accretion efficiency and help explain the presence of planets on wide orbits. However, the pebble supply is typically parameterized as a coherent pebble mass flux, sometimes being constant in space and time. Here we solve the dust advection and diffusion within viciously evolving protoplanetary disks to determine the pebble supply self-consistently. The pebbles are then accreted by planetesimals interacting with the gas disk via gas drag and gravitational torque. The pebble supply is variable with space and decays with time quickly, with a pebble flux below 10 M ⊕ Myr-1 after 1 Myr in our models. As a result, only when massive planetesimals (&gt;0.01 M ⊕) are luckily produced by the streaming instability or the disk has low viscosity (α ~ 0.0001) can the herd of planetesimals grow over a Mars mass within 2 Myr. By then, planetesimals only capture pebbles about 50 times their mass and as little as 10 times beyond 20 au due to limited pebble supply. Further studies considering multiple dust species in various disk conditions are warranted to fully assess the realistic pebble supply and its influence on planetesimal growth.

Keywords: Circumstellar dust, Protoplanetary disks, Planet formation, Planetesimals
The Aemulus Project. V. Cosmological Constraint from Small-scale Clustering of BOSS Galaxies. We analyze clustering measurements of BOSS galaxies using a simulation-based emulator of two-point statistics. We focus on the monopole and quadrupole of the redshift-space correlation function, and the projected correlation function, at scales of 0.1 ~ 60 h -1 Mpc. Although our simulations are based on wCDM with general relativity (GR), we include a scaling parameter of the halo velocity field, γ  f , defined as the amplitude of the halo velocity field relative to the GR prediction. We divide the BOSS data into three redshift bins. After marginalizing over other cosmological parameters, galaxy bias parameters, and the velocity scaling parameter, we find f σ 8(z = 0.25) = 0.413 ± 0.031, f σ 8(z = 0.4) = 0.470 ± 0.026, and f σ 8(z = 0.55) = 0.396 ± 0.022. Compared with Planck observations using a flat Lambda cold dark matter model, our results are lower by 1.9σ, 0.3σ, and 3.4σ, respectively. These results are consistent with other recent simulation-based results at nonlinear scales, including weak lensing measurements of BOSS LOWZ galaxies, two-point clustering of eBOSS LRGs, and an independent clustering analysis of BOSS LOWZ. All these results are generally consistent with a combination of ${\gamma }_{f}^{1/2}{\sigma }_{8}\approx 0.75$ . We note, however, that the BOSS data is well fit assuming GR, i.e., γ  f  = 1. We cannot rule out an unknown systematic error in the galaxy bias model at nonlinear scales, but near-future data and modeling will enhance our understanding of the galaxy-halo connection, and provide a strong test of new physics beyond the standard model.

Keywords: Cosmology, Observational cosmology, Large-scale structure of the universe
Toward Accurate Modeling of Galaxy Clustering on Small Scales: Halo Model Extensions and Lingering Tension. This paper represents an effort to provide robust constraints on the galaxy-halo connection and simultaneously test the Planck ΛCDM cosmology using a fully numerical model of small-scale galaxy clustering. We explore two extensions to the standard Halo Occupation Distribution model: assembly bias, whereby halo occupation depends on both halo mass and the larger environment, and velocity bias, whereby galaxy velocities do not perfectly trace the velocity of the dark matter within the halo. Moreover, we incorporate halo mass corrections to account for the impact of baryonic physics on the halo population. We identify an optimal set of clustering measurements to constrain this "decorated" HOD model for both low- and high-luminosity galaxies in SDSS DR7. We find that, for low-luminosity galaxies, a model with both assembly bias and velocity bias provides the best fit to the clustering measurements, with no tension remaining in the fit. In this model, we find evidence for both central and satellite galaxy assembly bias at the 99% and 95% confidence levels, respectively. In addition, we find evidence for satellite galaxy velocity bias at the 99.9% confidence level. For high-luminosity galaxies, we find no evidence for either assembly bias or velocity bias, but our model exhibits significant tension with SDSS measurements. We find that all of these conclusions still stand when we include the effects of baryonic physics on the halo mass function, suggesting that the tension we find for high-luminosity galaxies may be due to a problem with our assumed cosmological model.

Keywords: Galaxy dark matter halos, Large-scale structure of the universe, Clustering, Galaxy groups, Redshift surveys
Feedback in the Extremely Violent Group Merger NGC 6338. The galaxy group NGC 6338 is one of the most violent group-group mergers known to date. While the central dominant galaxies rush at each other at 1400 km s-1 along the line of sight, with dramatic gas heating and shock fronts detected, the central gas in the BCGs remains cool. There are also indications of feedback from active galactic nuclei, and neither subcluster core has been disrupted. With our deep radio uGMRT data at 383 and 650 MHz, we clearly detect a set of large, old lobes in the southern BCG coinciding with the X-ray cavities, while the northern and smaller BCG appears slightly extended in the radio. The southern BCG also hosts a smaller younger set of lobes perpendicular to the larger lobes, but also coinciding with the inner X-ray cavities and matching the jet direction in the parsec-resolution VLBA image. Our spectral analysis confirms the history of two feedback cycles. The high radio frequency analysis classifies the compact source in the southern BCG with a power law, while ruling out a significant contribution from accretion. The radio lightcurve over three decades shows a change about 10 yr ago, which might be related to ongoing feedback in the core. The southern BCG in the NGC 6338 merger remains another prominent case where the direction of jet-mode feedback between two cycles changed dramatically.

Keywords: Radio continuum emission, Active galactic nuclei, Spectral energy distribution, Galaxy groups
Giant Impacts and Debris Disk Morphology. Certain debris disks have nonaxisymmetric shapes in scattered light which are unexplained. The appearance of a disk depends on how its constituent Keplerian ellipses are arranged. The more the ellipses align apsidally, the more nonaxisymmetric the disk. Apsidal alignment is automatic for fragments released from a catastrophic collision between solid bodies. We synthesize scattered light images, and thermal emission images, of such giant impact debris. Depending on the viewing geometry, and if and how the initial apsidal alignment is perturbed, the remains of a giant impact can appear in scattered light as a one-sided or two-sided "fork," a lopsided "needle," or a set of "double wings." The last shape is difficult to reproduce in other scenarios involving gravitational forcing or gas drag, which do not align orbits as well. We compare our images with observations and offer a scorecard assessing whether the scattered light asymmetries in HD 15115, HD 32297, HD 61005, HD 111520, HD 106906, β Pic, and AU Mic are best explained by giant impacts, gravitational perturbations, or sculpting by the interstellar medium.

Keywords: Exoplanet dynamics, Asteroids, Circumstellar disks, Debris disks, Hirayama families
The Stellar Mass-Black Hole Mass Relation at z 2 down to {{M }}_{\mathrm{BH}}∼ {10}(7} {M) _{☉ } Determined by HETDEX. We investigate the stellar mass-black hole mass ( ${{ \mathcal M }}_{* }\mbox{--}{{ \mathcal M }}_{\mathrm{BH}}$ ) relation with type 1 active galactic nuclei (AGNs) down to ${{ \mathcal M }}_{\mathrm{BH}}={10}^{7\,}{M}_{\odot }$ , corresponding to a ≃ -21 absolute magnitude in rest-frame ultraviolet, at z = 2-2.5. Exploiting the deep and large-area spectroscopic survey of the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX), we identify 66 type 1 AGNs with ${{ \mathcal M }}_{\mathrm{BH}}$ ranging from 107-1010 M ☉ that are measured with single-epoch virial method using C IV emission lines detected in the HETDEX spectra. ${{ \mathcal M }}_{* }$ of the host galaxies are estimated from optical to near-infrared photometric data taken with Spitzer, the Wide-field Infrared Survey Explorer, and ground-based 4-8 m class telescopes by CIGALE spectral energy distribution (SED) fitting. We further assess the validity of SED fitting in two cases by host-nuclear decomposition performed through surface brightness profile fitting on spatially resolved host galaxies with the James Webb Space Telescope/NIRCam CEERS data. We obtain the ${{ \mathcal M }}_{* }\mbox{--}{{ \mathcal M }}_{\mathrm{BH}}$ relation covering the unexplored low-mass ranges of ${{ \mathcal M }}_{\mathrm{BH}}\,\sim \,{10}^{7}\mbox{--}{10}^{8}\,{M}_{\odot }$ , and conduct forward modeling to fully account for the selection biases and observational uncertainties. The intrinsic ${{ \mathcal M }}_{* }\mbox{--}{{ \mathcal M }}_{\mathrm{BH}}$ relation at z ~ 2 has a moderate positive offset of 0.52 ± 0.14 dex from the local relation, suggestive of more efficient black hole growth at higher redshift even in the low-mass regime of ${{ \mathcal M }}_{\mathrm{BH}}\,\sim \,{10}^{7}\mbox{--}{10}^{8}\,{M}_{\odot }$ . Our ${{ \mathcal M }}_{* }\mbox{--}{{ \mathcal M }}_{\mathrm{BH}}$ relation is inconsistent with the ${{ \mathcal M }}_{\mathrm{BH}}$ suppression at the low- ${{ \mathcal M }}_{* }$ regime predicted by recent hydrodynamic simulations at a 98% confidence level, suggesting that feedback in the low-mass systems may be weaker than those produced in hydrodynamic simulations.

Keywords: AGN host galaxies, Supermassive black holes, Active galactic nuclei, Galaxy evolution
Evidence for a Massive Andromeda Galaxy Using Satellite Galaxy Proper Motions. We present new mass estimates for Andromeda (M31) using the orbital angular momenta of four satellite galaxies (M33, NGC 185, NGC 147, and IC 10) derived from existing proper motions, distances, and line-of-sight velocities. We infer two masses for M31: ${M}_{\mathrm{vir}}={2.85}_{-0.77}^{+1.47}\times {10}^{12}\,{M}_{\odot }$ using satellite galaxy phase-space information derived with Hubble Space Telescope (HST)-based M31 proper motions and ${M}_{\mathrm{vir}}\,={3.02}_{-0.69}^{+1.30}\times {10}^{12}\,{M}_{\odot }$ using phase-space information derived with the weighted average of HST+Gaia-based M31 proper motions. The precision of our new M31 mass estimates (23%-50%) improves by a factor of two compared to previous mass estimates using a similar methodology with just one satellite galaxy, and places our results among the highest-precision M31 estimates in recent literature. Furthermore, our results are consistent with recently revised estimates for the total mass of the Local Group (LG), with the stellar mass-halo mass relation, and with observed kinematic data for both M31 and its entire population of satellites. An M31 mass &gt;2.5 × 1012 M ⊙ could have major implications for our understanding of LG dynamics, M31's merger and accretion history, and our understanding of LG galaxies in a cosmological context.

Keywords: Dwarf galaxies, Andromeda Galaxy, Astrometry, Astrostatistics
The Locations of Features in the Mass Distribution of Merging Binary Black Holes Are Robust against Uncertainties in the Metallicity-dependent Cosmic Star Formation History. New observational facilities are probing astrophysical transients such as stellar explosions and gravitational-wave sources at ever-increasing redshifts, while also revealing new features in source property distributions. To interpret these observations, we need to compare them to predictions from stellar population models. Such models require the metallicity-dependent cosmic star formation history ( ${ \mathcal S }(Z,z)$ ) as an input. Large uncertainties remain in the shape and evolution of this function. In this work, we propose a simple analytical function for ${ \mathcal S }(Z,z)$ . Variations of this function can be easily interpreted because the parameters link to its shape in an intuitive way. We fit our analytical function to the star-forming gas of the cosmological TNG100 simulation and find that it is able to capture the main behavior well. As an example application, we investigate the effect of systematic variations in the ${ \mathcal S }(Z,z)$ parameters on the predicted mass distribution of locally merging binary black holes. Our main findings are that (i) the locations of features are remarkably robust against variations in the metallicity-dependent cosmic star formation history, and (ii) the low-mass end is least affected by these variations. This is promising as it increases our chances of constraining the physics that govern the formation of these objects (https://github.com/LiekeVanSon/SFRD_fit/tree/7348a1ad0d2ed6b78c70d5100fb3cd2515493f02/).

Keywords: Gravitational wave astronomy, Star formation, Stellar mass black holes, Astrophysical black holes
Measuring the Vortex-Nucleus Pinning Force from Pulsar Glitch Rates. Superfluid vortex avalanches are one plausible cause of pulsar glitch activity. If they occur according to a state-dependent Poisson process, the measured long-term glitch rate is determined by the spin-down rate of the stellar crust, ${\dot{{\rm{\Omega }}}}_{c}$ , and two phenomenological parameters quantifying the vortex-nucleus pinning force: a crust-superfluid angular velocity lag threshold, X cr, and a reference unpinning rate, λ 0. A Bayesian analysis of 541 glitches in 177 pulsars, with N g ≥ 1 events per pulsar, yields ${X}_{\mathrm{cr}}={0.15}_{-0.04}^{+0.09}\,\mathrm{rad}\,{{\rm{s}}}^{-1}$ , ${\lambda }_{\mathrm{ref}}={7.6}_{-2.6}^{+3.7}\times {10}^{-8}\,{{\rm{s}}}^{-1}$ , and $a=-{0.27}_{-0.03}^{+0.04}$ assuming the phenomenological rate law λ 0 = λ ref[τ/(1 yr)] a , where τ denotes the characteristic spin-down age. The results are broadly similar, whether one includes or excludes quasiperiodic glitch activity, giant glitches, or pulsars with N g = 0, up to uncertainties about the completeness of the sample and the total observation time per pulsar. The X cr and λ 0 estimates are consistent with first-principles calculations based on nuclear theory, e.g., in the semiclassical local density approximation.

Keywords: Neutron stars, Stellar rotation, Nuclear astrophysics, Pulsars
Gas Accretion Can Drive Turbulence in Galaxies. The driving of turbulence in galaxies is deeply connected with the physics of feedback, star formation, outflows, accretion, and radial transport in disks. The velocity dispersion of gas in galaxies therefore offers a promising observational window into these processes. However, the relative importance of each of these mechanisms remains controversial. In this work we revisit the possibility that turbulence on galactic scales is driven by the direct impact of accreting gaseous material on the disk. We measure this effect in a disk-like star-forming galaxy in IllustrisTNG, using the high-resolution cosmological magnetohydrodynamical simulation TNG50. We employ Lagrangian tracer particles with a high time cadence of only a few million years to identify accretion and other events. The energies of particles are measured by stacking the events in bins of time around the event. The average effect of each event is measured by fitting explicit models for the kinetic and turbulent energies as a function of time. These measurements are corroborated by cross-correlating the turbulent energy with other time series and searching for signals of causality, i.e., asymmetries across zero time lag. We find that accretion contributes to the large-scale turbulent kinetic energy even if it does not dominate in this ~5 × 109 M ⊙ stellar mass galaxy. Extrapolating this finding to a range of galaxy masses, we find that there are regimes where energy from direct accretion may dominate the turbulent energy budget, particularly in disk outskirts, galaxies less massive than the Milky Way, and at redshift ~2.

Keywords: Galaxy formation, Disk galaxies, Galaxy dynamics, Galaxy physics, Star formation, High-redshift galaxies, Galaxy processes
The Direct-method Oxygen Abundance of Typical Dwarf Galaxies at Cosmic High Noon. We present a Keck/MOSFIRE rest-optical composite spectrum of 16 typical gravitationally lensed star-forming dwarf galaxies at 1.7 ≲ z ≲ 2.6 (z mean = 2.30), all chosen independent of emission-line strength. These galaxies have a median stellar mass of $\mathrm{log}{({M}_{* }/{M}_{\odot })}_{\mathrm{med}}={8.29}_{-0.43}^{+0.51}$ and a median star formation rate of ${{\rm{S}}{\rm{F}}{\rm{R}}}_{{\rm{H}}\alpha }^{{\rm{m}}{\rm{e}}{\rm{d}}}={2.25}_{-1.26}^{+2.15}\,{M}_{\odot }\,{{\rm{y}}{\rm{r}}}^{-1}$ . We measure the faint electron-temperature-sensitive [O III] λ4363 emission line at 2.5σ (4.1σ) significance when considering a bootstrapped (statistical-only) uncertainty spectrum. This yields a direct-method oxygen abundance of $12+\mathrm{log}{({\rm{O}}/{\rm{H}})}_{\mathrm{direct}}={7.88}_{-0.22}^{+0.25}$ ( ${0.15}_{-0.06}^{+0.12}\ {Z}_{\odot }$ ). We investigate the applicability at high z of locally calibrated oxygen-based strong-line metallicity relations, finding that the local reference calibrations of Bian et al. best reproduce (≲0.12 dex) our composite metallicity at fixed strong-line ratio. At fixed M *, our composite is well represented by the z ~ 2.3 direct-method stellar mass-gas-phase metallicity relation (MZR) of Sanders et al. When comparing to predicted MZRs from the IllustrisTNG and FIRE simulations, having recalculated our stellar masses with more realistic nonparametric star formation histories $(\mathrm{log}{({M}_{* }/{M}_{\odot })}_{\mathrm{med}}={8.92}_{-0.22}^{+0.31})$ , we find excellent agreement with the FIRE MZR. Our composite is consistent with no metallicity evolution, at fixed M * and SFR, of the locally defined fundamental metallicity relation. We measure the doublet ratio [O II] λ3729/[O II] λ3726 = 1.56 ± 0.32 (1.51 ± 0.12) and a corresponding electron density of ${n}_{e}={1}_{-0}^{+215}\ {\mathrm{cm}}^{-3}$ ( ${n}_{e}={1}_{-0}^{+74}\ {\mathrm{cm}}^{-3}$ ) when considering the bootstrapped (statistical-only) error spectrum. This result suggests that lower-mass galaxies have lower densities than higher-mass galaxies at z ~ 2. ∗ The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with programs #9289, #11710, #11802, #12201, #12931, #13389, #13498, #13504.

Keywords: Dwarf galaxies, Scaling relations, Galaxy abundances, Galaxy evolution, Interstellar medium, High-redshift galaxies