Sazuna/UAT_keywords huggingface dataset:
The Coevolution of Galaxies and the Cool Circumgalactic Medium Probed with the SDSS and DESI Legacy Imaging Surveys. We study the evolution of galaxies and the circumgalactic medium (CGM) through cosmic time by correlating ∼50,000 Mg II absorbers, tracers of cool gas (∼104 K), detected in the Sloan Digital Sky Survey quasar spectra with galaxies detected in the DESI Legacy Imaging Surveys. By doing so, we extract the properties of galaxies associated with absorbers from redshift 0.4 to 1.3 with effectively ∼15,000 pairs and explore the covering fraction of Mg II absorbers as a function of galaxy type, stellar mass, impact parameter, and redshift. We find that the gas covering fraction increases with stellar mass of galaxies by $\sim {M}_{* }^{0.4}$ . However, after we normalize the impact parameter by the virial radius of dark matter halos, the gas profiles around galaxies with masses ranging from 109 to ${10}^{11}\,{M}_{\odot }$ become weakly dependent on stellar mass. In addition, the gas distribution depends on galaxy type: the covering fraction within $0.3\,{r}_{\mathrm{vir}}$ around star-forming galaxies is 2-4 times higher than that around passive galaxies at all redshifts. We find that the covering fraction of strong absorbers ( ${W}_{\lambda 2796}\gt 1\,\mathring{\rm A} $ ) around both types of galaxies evolves significantly with redshift, similarly to the evolution of star formation rate (SFR) of galaxies, while such an evolution is not detected for weak absorbers ( ${W}_{\lambda 2796}\lt 1\,\mathring{\rm A} $ ). We quantify the H I mass traced by strong absorbers and find that the gas mass around galaxies evolves consistently with the SFR of galaxies. This result suggests that the properties of galaxies and their CGM coevolve through cosmic time. Finally, we discuss the origins of strong absorbers around passive galaxies and argue that its redshift evolution may trace the star formation activity of satellite galaxies.

Keywords: Galaxy evolution, Quasar absorption line spectroscopy, Circumgalactic medium
HST Grism-derived Forecasts for Future Galaxy Redshift Surveys. The mutually complementary Euclid and Roman galaxy redshift surveys will use Hα- and [O III]-selected emission-line galaxies (ELGs) as tracers of the large-scale structure at 0.9 ≲ z ≲ 1.9 (Hα) and 1.5 ≲ z ≲ 2.7 ([O III]). It is essential to have a reliable and sufficiently precise knowledge of the expected numbers of Hα-emitting galaxies in the survey volume in order to optimize these redshift surveys for the study of dark energy. Additionally, these future samples of ELGs will, like all slitless spectroscopy surveys, be affected by a complex selection function that depends on galaxy size and luminosity, line equivalent width (EW), and redshift errors arising from the misidentification of single ELGs. Focusing on the specifics of the Euclid survey, we combine two slitless spectroscopic WFC3-IR data sets—3D-HST+AGHAST and the WFC3 Infrared Spectroscopic Parallel survey—to construct a Euclid-like sample that covers an area of 0.56 deg2 and includes 1277 ELGs. We detect 1091 (∼3270 deg-2) Hα+[N II]-emitting galaxies in the range 0.9 ≤ z ≤ 1.6 and 162 (∼440 deg-2) [O III] λ5007 emitters over 1.5 ≤ z ≤ 2.3 with line fluxes ≥2 × 10-16 erg s-1 cm-2. The median of the Hα+[N II] EW distribution is ∼250 Å, and the effective radii of the continuum and Hα+[N II] emission are correlated with a median of ∼0"38 and significant scatter (σ ∼ 0"2-0"35). Finally, we explore the prevalence of redshift misidentification in future Euclid samples, finding potential contamination rates of ∼14%-20% and ∼6% down to 2 × 10-16 erg s-1 cm-2 and 6 × 10-17 erg s-1 cm-2, respectively, although with increased wavelength coverage these percentages drop to nearly zero.

Keywords: Redshift surveys, Emission line galaxies, Spectroscopy
Effect of Electromagnetic Interaction on Galactic Center Flare Components. Recently, near-infrared GRAVITY@ESO observations at 2.2 μm announced the detection of three bright "flares" in the vicinity of the Galactic center supermassive black hole (SMBH) that exhibited orbital motion at a distance of about 6-11 gravitational radii from an ∼4 × 106 M⊙ black hole. There are indications of the presence of a large-scale, organized component of the magnetic field at the Galactic center. Electromagnetic effects on the flare dynamics were previously not taken into account despite the relativistic motion of a plasma in magnetic field leading to the charge separation and nonnegligible net charge density in the plasma. Applying various approaches, we find the net charge number density of the flare components of the order of 10-3-10-4 cm-3, while the particles' total number density is of the order of 106-108 cm-3. However, even such a tiny excess of charged particles in the quasi-neutral plasma can significantly affect the dynamics of flare components, which can then lead to the degeneracy in the measurements of spin of the SMBH. Analyzing the dynamics of recent flares in the case of the rapidly rotating black hole, we also constrain the inclination angle between the magnetic field and spin axis to α &lt; 50°, as for larger angles, the motion of the hot spot is strongly chaotic.

Keywords: Accretion, Black hole physics, Galactic center, Milky Way magnetic fields, Galaxy accretion disks, Magnetic fields
Polluting the Pair-instability Mass Gap for Binary Black Holes through Super-Eddington Accretion in Isolated Binaries. The theory for single stellar evolution predicts a gap in the mass distribution of black holes (BHs) between approximately 45 and 130 $\,{M}_{\odot }$ , the so-called "pair-instability mass gap." We examine whether BHs can pollute the gap after accreting from a stellar companion. To this end, we simulate the evolution of isolated binaries using a population synthesis code, where we allow for super-Eddington accretion. Under our most extreme assumptions, we find that at most about 2% of all merging binary BH systems contains a BH with a mass in the pair-instability mass gap, and we find that less than 0.5% of the merging systems has a total mass larger than 90 $\,{M}_{\odot }$ . We find no merging binary BH systems with a total mass exceeding 100 $\,{M}_{\odot }$ . We compare our results to predictions from several dynamical pathways to pair-instability mass gap events and discuss the distinguishable features. We conclude that the classical isolated binary formation scenario will not significantly contribute to the pollution of the pair-instability mass gap. The robustness of the predicted mass gap for the isolated binary channel is promising for the prospective of placing constraints on (I) the relative contribution of different formation channels, (II) the physics of the progenitors including nuclear reaction rates, and, tentatively, (III) the Hubble parameter.

Keywords: Accretion, Binary stars, Black holes, High energy astrophysics, Compact binary stars, Gravitational wave sources
The Space Environment and Atmospheric Joule Heating of the Habitable Zone Exoplanet TOI 700 d. We investigate the space environment conditions near the Earth-size planet TOI 700 d using a set of numerical models for the stellar corona and wind, the planetary magnetosphere, and the planetary ionosphere. We drive our simulations using a scaled-down stellar input and a scaled-up solar input in order to obtain two independent solutions. We find that for the particular parameters used in our study, the stellar wind conditions near the planet are not very extreme—slightly stronger than that near the Earth in terms of the stellar wind ram pressure and the intensity of the interplanetary magnetic field. Thus, the space environment near TOI 700 d may not be extremely harmful to the planetary atmosphere, assuming the planet resembles the Earth. Nevertheless, we stress that the stellar input parameters and the actual planetary parameters are unconstrained, and different parameters may result in a much greater effect on the atmosphere of TOI 700 d. Finally, we compare our results to solar wind measurements in the solar system and stress that modest stellar wind conditions may not guarantee atmospheric retention of exoplanets.

Keywords: Geomagnetic fields, Exoplanet atmospheric variability, Solar wind, Stellar winds, Stellar coronae
Quenching as a Contest between Galaxy Halos and Their Central Black Holes. Existing models of galaxy formation have not yet explained striking correlations between structure and star formation activity in galaxies, notably the sloped and moving boundaries that divide star-forming from quenched galaxies in key structural diagrams. This paper uses these and other relations to "reverse engineer" the quenching process for central galaxies. The basic idea is that star-forming galaxies with larger radii (at a given stellar mass) have lower black hole (BH) masses due to lower central densities. Galaxies cross into the green valley when the cumulative effective energy radiated by their BH equals ∼4× their halo gas-binding energy. Because larger-radii galaxies have smaller BHs, one finds that they must evolve to higher stellar masses in order to meet this halo energy criterion, which explains the sloping boundaries. A possible cause of radii differences among star-forming galaxies is halo concentration. The evolutionary tracks of star-forming galaxies are nearly parallel to the green-valley boundaries, and it is mainly the sideways motions of these boundaries with cosmic time that cause galaxies to quench. BH scaling laws for star-forming, quenched, and green-valley galaxies are different, and most BH mass growth takes place in the green valley. Implications include the radii of star-forming galaxies are an important second parameter in shaping their BHs; BHs are connected to their halos but in different ways for star-forming, quenched, and green-valley galaxies; and the same BH-halo quenching mechanism has been in place since z ∼ 3. We conclude with a discussion of BH-galaxy coevolution and the origin and interpretation of BH scaling laws.

Keywords: Supermassive black holes, Galaxy physics, Galaxy structure, Star formation, Galaxy evolution, Galaxy quenching
Black Hole Growth and Feedback in Isolated ROMULUS25 Dwarf Galaxies. We investigate the effects of massive black hole growth on the structural evolution of dwarf galaxies within the ROMULUS25 cosmological hydrodynamical simulation. We study a sample of 205 central, isolated dwarf galaxies with stellar masses ${M}_{\mathrm{star}}\lt {10}^{10}{M}_{\odot }$ and a central BH. We find that the local MBH-Mstar relation exhibits a high degree of scatter below Mstar &lt; 1010M⊙, which we use to classify BHs as overmassive or undermassive relative to their host Mstar. Within isolated dwarf galaxies, only 8% of undermassive BHs ever undergo a BH merger, while 95% of overmassive BHs grow through a mixture of BH mergers and accretion. We find that isolated dwarf galaxies that host overmassive BHs also follow different evolutionary tracks relative to their undermassive BH counterparts, building up their stars and dark matter earlier and experiencing star formation suppression starting around z = 2. By z = 0.05, overmassive BH hosts above Mstar &gt; 109M⊙ are more likely to exhibit lower central stellar mass density, lower H I gas content, and lower star formation rates than their undermassive BH counterparts. Our results suggest that overmassive BHs in isolated galaxies above Mstar &gt; 109M⊙ are capable of driving feedback, in many cases suppressing and even quenching star formation by late times.

Keywords: Black hole physics, Supermassive black holes, Dwarf galaxies, N-body simulations
CO Emission and CO Hot Spots in Diffuse Molecular Gas. We observed λ3 mm ${}^{12}\mathrm{CO}$ , ${}^{13}\mathrm{CO}$ , ${{\rm{C}}}^{18}{\rm{O}}$ , ${\mathrm{HCO}}^{+}$ , HCN, and CS emission from diffuse molecular gas along sight lines with ${E}_{B-V}$ ≈ 0.1-1 mag. Directions were mostly chosen for their proximity to sight lines toward background millimeter-wave continuum sources studied in ${\mathrm{HCO}}^{+}$ absorption at positions where maps of ${}^{12}\mathrm{CO}$ at 1' resolution showed surprisingly bright integrated CO J = 1-0 emission, ${W}_{\mathrm{CO}}$ = 5-12 K km s-1, but we also observed in L121 near ζ Oph. Coherence emerges when the data are considered over a broad range of ${}^{12}\mathrm{CO}$ and ${}^{13}\mathrm{CO}$ brightness. In this work ${W}_{\mathrm{CO}}$ / ${W}_{13}$ and N( ${}^{12}\mathrm{CO}$ )/N( ${}^{13}\mathrm{CO}$ ) are 20-40 for ${W}_{\mathrm{CO}}$ ≲ 5 K km s-1 and N(CO) $\lesssim \ 5\times {10}^{15}\,{\mathrm{cm}}^{-2}$ , increasing with much scatter for larger ${W}_{\mathrm{CO}}$ or N(CO). Here N( ${}^{13}\mathrm{CO}$ )/N( ${{\rm{C}}}^{18}{\rm{O}}$ ) &gt; 20-40 (3σ) versus an intrinsic ratio 13C/18O = 8.4 from a combination of selective photodissociation and enhancement of ${}^{13}\mathrm{CO}$ . The observations are understandable if ${}^{12}\mathrm{CO}$ forms from the thermal recombination of ${\mathrm{HCO}}^{+}$ with electrons, after which the observed ${}^{13}\mathrm{CO}$ forms via endothermic carbon isotope exchange with 13C+. ${W}_{\mathrm{CS}}$ / ${W}_{\mathrm{CO}}$ increases abruptly for ${W}_{\mathrm{CO}}$ ≳ 10 K km s-1, and ${W}_{\mathrm{CS}}$ / ${W}_{{\mathrm{HCO}}^{+}}$ is bimodal, showing two branches having N(CS)/N( ${\mathrm{HCO}}^{+}$ ) ≈5 and 1.25. Because CO formation and ${\mathrm{HCO}}^{+}$ excitation both involve collisions between ${\mathrm{HCO}}^{+}$ and ambient electrons, comparison of the CO and ${\mathrm{HCO}}^{+}$ emission shows that the CO hot spots are small regions of enhanced N(CO) occupying only a small fraction of the column density of the medium in which they are embedded. The ${\mathrm{HCO}}^{+}$ /CO and HCN/CO brightness ratios are 1%-2%, with obvious implications for determinations of the true dense gas fraction.

Keywords: Interstellar molecules, Interstellar medium
The Copula of the Cosmological Matter Density Field is Non-Gaussian. Non-Gaussianity of the cosmological matter density field can be largely reduced by a local Gaussianization transformation (and its approximations, such as the logarithmic transformation). Such behavior can be recast as the Gaussian copula hypothesis (GCH), and has been verified to very high accuracy at a two-point level. On the other hand, statistically significant non-Gaussianities in the Gaussianized field have been detected in simulations. We point out that this apparent inconsistency is caused by the very limited degrees of freedom in the copula function, which make it misleading as a diagnosis of residual non-Gaussianity in the Gaussianized field. Using the copula density and at the two-point level, we highlight the departure from Gaussianity. We further quantify its impact in the predicted nth (n ≥ 2) order correlation functions. We explore a remedy of the GCH, which alleviates but does not completely solve the above problems.

Keywords: Non-Gaussianity, Dark matter distribution, N-body simulations, Large-scale structure of the universe
A New Metal-poor Globular Cluster and Resolved Stars in the Outer Disk of the Black Eye Galaxy M64: Implication for the Origin of the Type III Disk Break. M64 is a nearby spiral galaxy with a Type III antitruncation component. To trace the origin of the Type III component, we present Hubble Space Telescope/Advanced Camera for Surveys (ACS) F606W/F814W photometry of resolved stars in a field located in the outer disk ( $2\buildrel{\,\prime}\over{.} 5\lesssim r\lesssim 6\buildrel{\,\prime}\over{.} 5$ ) of M64. At $r\approx 5\buildrel{\,\prime}\over{.} 5$ (7 kpc) to the east, we discover a new metal-poor globular cluster ( ${R}_{\mathrm{eff}}=5.73\pm 0.02$ pc and MV = -9.54 ± 0.09 mag), M64-GC1. This is the first globular cluster found in M64. The color-magnitude diagram (CMD) of the resolved stars in M64-GC1 is well matched by 12 Gyr isochrones with [Fe/H] = -1.5 ± 0.2, showing that this cluster belongs to a halo. The CMD of the resolved stars in the entire ACS field shows two distinguishable red giant branches (RGBs): a curved metal-rich RGB and a vertical metal-poor RGB. The metal-rich RGB represents an old metal-rich ([Fe/H] ≈ -0.4) disk population. In contrast, the CMD of the metal-poor RGB stars is very similar to the CMD of M64-GC1, showing that the metal-poor RGB represents a halo population. The radial number-density profile of the metal-rich RGB stars is described by an exponential disk law, while the profile of the metal-poor RGB stars is described by a de Vaucouleurs's law. From these, we conclude that the origin of the Type III component in M64 is a halo that has a much lower metallicity than the disk or bulge population.

Keywords: Globular star clusters, Galaxy distances, Spiral galaxies, Galaxy stellar content, Galaxy stellar halos, Galaxy disks
Nature of Compton-thick Active Galactic Nuclei in "Nonmerging" Luminous Infrared Galaxies UGC 2608 and NGC 5135 Revealed with Broadband X-Ray Spectroscopy. We have analyzed the broadband X-ray spectra of active galactic nuclei (AGNs) in two "nonmerging" luminous infrared galaxies (LIRGs), UGC 2608 and NGC 5135, utilizing the data of Nuclear Spectroscopic Telescope Array, Suzaku, XMM-Newton, and Chandra. Applying the X-ray clumpy-torus model (XCLUMPY), we find that both sources have similar spectra characterized by Compton-thick (CT) absorption ( ${N}_{{\rm{H}}}$ ∼ 5-7 × 1024 cm-2) and small torus angular width (σ &lt; 20°). The intrinsic 2-10 keV luminosities are ${3.9}_{-1.7}^{+2.2}$ × 1043 erg s-1 (UGC 2608) and ${2.0}_{-0.9}^{+3.3}$ × 1043 erg s-1 (NGC 5135). The [O IV]-to-nuclear-12 μm luminosity ratios are larger than those of typical Seyferts, which are consistent with the torus covering factors ( ${C}_{{\rm{T}}}\,\lesssim $ 0.7) estimated from the torus angular widths and column densities by X-ray spectroscopy. The torus covering factors and Eddington ratios ( ${\lambda }_{\mathrm{Edd}}$ ∼ 0.1) follow the relation found by Ricci et al. for local AGNs, implying that their tori become geometrically thin, due to significant radiation pressure of the AGN that blows out some part of the tori. These results indicate that the CT AGNs in these "nonmerger" LIRGs are just a normal AGN population seen edge-on through a large line-of-sight column density. They are in contrast to the buried CT AGNs in late-stage mergers that have large torus covering factors even at large Eddington ratios.

Keywords: Observational astronomy, Black hole physics, Supermassive black holes, X-ray active galactic nuclei, Infrared galaxies, Active galactic nuclei
The Dragonfly Edge-on Galaxies Survey: Shaping the Outer disk of NGC 4565 via Accretion. We present deep g- and r-band imaging of the well-known edge-on galaxy NGC 4565 (the "Needle Galaxy"), observed as part of the Dragonfly Edge-on Galaxies Survey. The 3σ local surface brightness contrast limit on 10″ scales is 28.616 ± 0.005 mag arcsec-2 for the r-band image and 28.936 ± 0.005 mag arcsec-2 for the g-band image. We trace the galaxy's starlight in narrow slice profiles spanning over 90 kpc along the major axis (with bin sizes ranging from 1.7 × 0.5 to 1.7 × 7.8 kpc) to surface brightnesses below 29 mag arcsec-2. We confirm the previously observed asymmetric disk truncation in NGC 4565. In addition, the sharp northwest truncation turns over to a shallower component that coincides with a fan-like feature seen to wrap around the northwest disk limb. We propose that the fan may be a tidal ribbon and qualitatively replicate the fan with simple simulations, although alternative explanations of the fan and the disk's asymmetry are shown to be possible. In any case, we conclude that there is strong evidence for accretion-based outer disk growth in NGC 4565.

Keywords: Spiral galaxies, Galaxy evolution, Disk galaxies
Suprathermal Proton Spectra at Interplanetary Shocks in 3D Hybrid Simulations. Interplanetary shocks are one of the proposed sources of suprathermal ion populations (I.e., ions with energies of a few times the solar-wind energy). Here we present results from a series of 3D hybrid simulations of collisionless shocks in the solar wind. We focus on the influence of the shock-normal angle, θBn, and the shock speed, Vs, on producing protons with energies a few to hundreds of times the thermal energy of the upstream plasma. The combined effects of θBn and Vs result in shocks with Alfvén Mach numbers in the range 3.0-6.0 and fast magnetosonic Mach numbers in the range 2.5-5.0, representing moderate to strong interplanetary shocks. We find that θBn largely organizes the shape of proton energy spectra, while shock speed controls acceleration efficiency. All shocks accelerate protons at the shock front, but the spectral evolution depends on θBn. Shocks with θBn ≥ 60° produce isolated bursts of suprathermal protons at the shock front, while shocks with θBn ≤ 45° create suprathermal beams upstream of the shock. Downstream proton energy spectra have exponential or smoothed broken power-law forms when θBn ≥ 45° and a single power-law form when θBn ≤ 30°. Protons downstream of the strongest shocks have energies at least 100 times the upstream thermal energy, with θBn ≤ 30° shocks producing the highest-energy protons and θBn ≥ 60° shocks producing the largest number of protons with energies at least a few times the thermal energy.

Keywords: Space plasmas, Interplanetary shocks, Solar energetic particles, Solar wind, Interplanetary particle acceleration
Chemical Variation among Protostellar Cores: Dependence on Prestellar Core Conditions. Hot corino chemistry and warm carbon chain chemistry (WCCC) are driven by gas-grain interactions in star-forming cores: radical-radical recombination reactions to form complex organic molecules (COMs) in the ice mantle, sublimation of CH4 and COMs, and their subsequent gas-phase reactions. These chemical features are expected to depend on the composition of the ice mantle, which is set in the prestellar phase. We calculated the gas-grain chemical reaction network considering a layered ice mantle structure in star-forming cores to investigate how the hot corino chemistry and WCCC depend on the physical condition of the static phase before the onset of gravitational collapse. We found that WCCC becomes more active if the temperature is lower, or the visual extinction is lower in the static phase, or the static phase is longer. The dependence of hot corino chemistry on the static-phase condition is more complex. While CH3OH is less abundant in the models with a warmer static phase, some COMs are formed efficiently in those warm models because there are various formation paths of COMs. If the visual extinction is lower, photolysis makes COMs less abundant in the static phase. Once the collapse starts and visual extinction increases, however, COMs can be formed efficiently. The duration of the static phase does not largely affect COM abundances. The chemical diversity between prototypical hot corinos and hybrid sources, in which both COMs and carbon chains are reasonably abundant, can be explained by the variation of prestellar conditions. Deficiency of gaseous COMs in prototypical WCCC sources is, however, hard to reproduce within our models.

Keywords: Star formation, Astrochemistry