Sazuna/UAT_keywords huggingface dataset:
A Wide and Deep Exploration of Radio Galaxies with Subaru HSC (WERGS). VII. Redshift Evolution of Radio Galaxy Environments at z = 0.3-1.4. We examine the redshift evolution of density environments around 2163 radio galaxies with the stellar masses of ~109-1012 M ⊙ between redshifts of z = 0.3-1.4, based on the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) and Faint Images of the Radio Sky at Twenty cm. We use the k-nearest neighbor method to measure the local galaxy number density around our radio galaxy sample. We find that the overdensities of the radio galaxies are weakly but significantly anticorrelated with redshift. This is consistent with the known result that the relative abundance of less-massive radio galaxies increases with redshift, because less-massive radio galaxies reside in relatively low-density regions. Massive radio galaxies with stellar masses of M * &gt; 1011 M ⊙ are found in high density environments compared with the control sample galaxies with radio nondetection and matched stellar mass. Less-massive radio galaxies with M * &lt; 1011 M ⊙ reside in average density environments. The fraction of the radio galaxies associated with the neighbors within a typical major merger scale, &lt;70 kpc, is higher than (comparable to) that of the control galaxies at M * &gt; 1011 M ⊙ (M * &lt; 1011 M ⊙). We also find that the local densities around the radio galaxies are anticorrelated with the radio luminosities and black hole mass accretion rates at a fixed stellar mass. These findings suggest that massive radio galaxies have matured through galaxy mergers in the past, and have supermassive black holes whose mass accretion almost ceased at z &gt; 1.4, while less-massive radio galaxies undergo active accretion just at this epoch, as they have avoided such merger events.

Keywords: Galaxy formation, Radio galaxies, Active galactic nuclei, Galaxy evolution
LARS XIII: High Angular Resolution 21 cm H I Observations of Lyα Emitting Galaxies. The Lyα emission line is one of the main observables of galaxies at high redshift, but its output depends strongly on the neutral gas distribution and kinematics around the star-forming regions where UV photons are produced. We present observations of Lyα and 21 cm H I emission at comparable scales with the goal to qualitatively investigate how the neutral interstellar medium (ISM) properties impact Lyα transfer in galaxies. We have observed 21 cm H I at the highest possible angular resolution (≍3″ beam) with the Very Large Array in two local galaxies from the Lyman Alpha Reference Sample. We compare these data with Hubble Space Telescope Lyα imaging and spectroscopy, and Multi Unit Spectroscopic Explorer and Potsdam MultiAperture Spectrophotometer ionized gas observations. In LARS08, high-intensity Lyα emission is cospatial with high column density H I where the dust content is the lowest. The Lyα line is strongly redshifted, consistent with a velocity redistribution that allows Lyα escape from a high column density neutral medium with a low dust content. In eLARS01, high-intensity Lyα emission is located in regions of low column density H I, below the H I data sensitivity limit ( &lt; 2 × 1020 cm-2). The perturbed ISM distribution with low column density gas in front of the Lyα emission region plays an important role in the escape. In both galaxies, the faint Lyα emission (~1×10-16 erg s-1cm-2 arcsec-2) traces intermediate Hα emission regions where H I is found, regardless of the dust content. Dust seems to modulate, but not prevent, the formation of a faint Lyα halo. This study suggests the existence of scaling relations between dust, Hα, H I, and Lyα emission in galaxies.

Keywords: Lyman-alpha galaxies, Starburst galaxies, Interacting galaxies, Interstellar atomic gas
Chemical and Physical Characterization of the Isolated Protostellar Source CB68: FAUST IV. The chemical diversity of low-mass protostellar sources has so far been recognized, and environmental effects are invoked as its origin. In this context, observations of isolated protostellar sources without the influence of nearby objects are of particular importance. Here, we report the chemical and physical structures of the low-mass Class 0 protostellar source IRAS 16544-1604 in the Bok globule CB 68, based on 1.3 mm Atacama Large Millimeter/submillimeter Array observations at a spatial resolution of ~70 au that were conducted as part of the large program FAUST. Three interstellar saturated complex organic molecules (iCOMs), CH3OH, HCOOCH3, and CH3OCH3, are detected toward the protostar. The rotation temperature and the emitting region size for CH3OH are derived to be 131 ± 11 K and ~10 au, respectively. The detection of iCOMs in close proximity to the protostar indicates that CB 68 harbors a hot corino. The kinematic structure of the C18O, CH3OH, and OCS lines is explained by an infalling-rotating envelope model, and the protostellar mass and the radius of the centrifugal barrier are estimated to be 0.08-0.30 M ⊙ and &lt;30 au, respectively. The small radius of the centrifugal barrier seems to be related to the small emitting region of iCOMs. In addition, we detect emission lines of c-C3H2 and CCH associated with the protostar, revealing a warm carbon-chain chemistry on a 1000 au scale. We therefore find that the chemical structure of CB 68 is described by a hybrid chemistry. The molecular abundances are discussed in comparison with those in other hot corino sources and reported chemical models.

Keywords: Interstellar molecules, Star formation, Circumstellar disks
Radio Scattering Horizons for Galactic and Extragalactic Transients. Radio wave scattering can cause severe reductions in detection sensitivity for surveys of Galactic and extragalactic fast (~ms duration) transients. While Galactic sources like pulsars undergo scattering in the Milky Way interstellar medium (ISM), extragalactic fast radio bursts (FRBs) can also experience scattering in their host galaxies and other galaxies intervening in their lines of sight. We assess Galactic and extragalactic scattering horizons for fast radio transients using a combination of NE2001 to model the dispersion measure and scattering time (τ) contributed by the Galactic disk, and independently constructed electron density models for the Galactic halo and other galaxies' ISMs and halos that account for different galaxy morphologies, masses, densities, and strengths of turbulence. For source redshifts 0.5 ≤ z s ≤ 1, an all-sky, isotropic FRB population has simulated values of τ (1 GHz) ranging from ~1 μs to ~2 ms (90% confidence, observer frame) that are dominated by host galaxies, although τ can be ≫2 ms at low Galactic latitudes. A population at z s = 5 has 0.01 ≲ τ ≲ 300 ms at 1 GHz (90% confidence), dominated by intervening galaxies. About 20% of these high-redshift FRBs are predicted to have τ &gt; 5 ms at 1 GHz (observer frame), and ≳40% of FRBs between z s ~ 0.5-5 have τ ≳ 1 ms for ν ≤ 800 MHz. Our scattering predictions may be conservative if scattering from circumsource environments is significant, which is possible under specific conditions. The percentage of FRBs selected against from scattering could also be substantially larger than we predict if circumgalactic turbulence causes more small-scale (≪1 au) density fluctuations than observed from nearby halos.

Keywords: Intergalactic medium, Extragalactic radio sources, Radio pulsars, Radio bursts, Interstellar medium, Circumgalactic medium, Interstellar scattering, Radio transient sources
Vetting the "Lobster" Diagram: Searching for Unseen Companions in Wide Binaries Using NASA Space Exoplanet Missions. Over the past decade, the number of known wide-binary systems has expanded exponentially, thanks to the release of data from the Gaia Mission. Some of these wide-binary systems are actually higher-order multiples, where one of the components is an unresolved binary itself. One way to search for these systems is by identifying the overluminous components in the systems. In this study, we examine 4947 K+K wide-binary pairs from the SUPERWIDE catalog, and quantify the relative colors and luminosities of the components to find evidence for additional unresolved companions. The method is best illustrated in a graph that we call the "Lobster" diagram. To confirm that the identified overluminous components are close binary systems, we cross-match our wide binaries with the TESS, K2, and Kepler archives, and search for signs of eclipses and fast stellar rotation modulation in the light curves. We find that 78.9% ± 20.7% of the wide binaries that contain an eclipsing system are identified as overluminous in the "Lobster" diagram, and that 73.5% ± 12.4% of the wide binaries that contain a component showing fast rotation (P &lt; 5 days) also show an overluminous component. From these results, we calculate a revised lower limit on the higher-order multiplicity fraction for K+K wide binaries of 40.0% ± 1.6%. We also examine the higher-order multiplicity fraction as a function of projected physical separation and metallicity. The fraction is unusually constant as a function of projected physical separation, while we see no statistically significant evidence that the fraction varies with metallicity.

Keywords: Multiple stars, Stellar rotation, Low mass stars, Eclipsing binary stars, Visual binary stars
Beyond the Local Volume. II. Population Scaleheights and Ages of Ultracool Dwarfs in Deep HST/WFC3 Parallel Fields. Ultracool dwarfs (UCDs) represent a significant proportion of stars in the Milky Way, and deep samples of these sources have the potential to constrain the formation history and evolution of low-mass objects in the Galaxy. Until recently, spectral samples have been limited to the local volume (d &lt; 100 pc). Here, we analyze a sample of 164 spectroscopically characterized UCDs identified by Aganze et al. in the Hubble Space Telescope (HST) WFC3 Infrared Spectroscopic Parallel Survey (WISPS) and 3D-HST. We model the observed luminosity function using population simulations to place constraints on scaleheights, vertical velocity dispersions, and population ages as a function of spectral type. Our star counts are consistent with a power-law mass function and constant star formation history for UCDs, with vertical scaleheights of 249 ${}_{-61}^{+48}$ pc for late-M dwarfs, 153 ${}_{-30}^{+56}$ pc for L dwarfs, and 175 ${}_{-56}^{+149}$ pc for T dwarfs. Using spatial and velocity dispersion relations, these scaleheights correspond to disk population ages of 3.6 ${}_{-1.0}^{+0.8}$ Gyr for late-M dwarfs, 2.1 ${}_{-0.5}^{+0.9}$ Gyr for L dwarfs, and 2.4 ${}_{-0.8}^{+2.4}$ Gyr for T dwarfs, which are consistent with prior simulations that predict that L-type dwarfs are on average a younger and less dispersed population. There is an additional 1-2 Gyr systematic uncertainty on these ages due to variances in age-velocity relations. We use our population simulations to predict the UCD yield in the James Webb Space Telescope PASSAGES survey, a similar and deeper survey to WISPS and 3D-HST, and find that it will produce a comparably sized UCD sample, albeit dominated by thick disk and halo sources.

Keywords: Brown dwarfs, Stellar ages, Hubble Space Telescope, Galactic archaeology, L dwarfs, Y dwarfs, T dwarfs
Interpreting the Atmospheric Composition of Exoplanets: Sensitivity to Planet Formation Assumptions. Constraining planet formation based on the atmospheric composition of exoplanets is a fundamental goal of the exoplanet community. Existing studies commonly try to constrain atmospheric abundances, or to analyze what abundance patterns a given description of planet formation predicts. However, there is also a pressing need to develop methodologies that investigate how to transform atmospheric compositions into planetary formation inferences. In this study we summarize the complexities and uncertainties of state-of-the-art planet formation models and how they influence planetary atmospheric compositions. We introduce a methodology that explores the effect of different formation model assumptions when interpreting atmospheric compositions. We apply this framework to the directly imaged planet HR 8799e. Based on its atmospheric composition, this planet may have migrated significantly during its formation. We show that including the chemical evolution of the protoplanetary disk leads to a reduced need for migration. Moreover, we find that pebble accretion can reproduce the planet's composition, but some of our tested setups lead to too low atmospheric metallicities, even when considering that evaporating pebbles may enrich the disk gas. We conclude that the definitive inversion from atmospheric abundances to planet formation for a given planet may be challenging, but a qualitative understanding of the effects of different formation models is possible, opening up pathways for new investigations.

Keywords: Exoplanet atmospheric composition , Exoplanet formation
A Theoretical Study of Infrared Spectra of Highly Positively Charged C<SUB>60</SUB> Fullerenes and Their Relevance to Observed UIE Features. By applying first principles quantum chemical calculations, we present a complete catalog of the theoretically expected mid-infrared signatures of cationic forms of fullerene with the general formula of ${{\rm{C}}}_{60}^{q+}$ (q = 1-26). The structural stability and bonding of these exotic species have been reported by us elsewhere. It is found that not only can some of these cations contribute significantly to the flux of the 17.4 and 18.9 μm bands of fullerene that are observed in some planetary nebulae but they also show strong bands that match the position of key astronomical unidentified infrared emission at 11.21, 16.40 and 20-21 μm, which makes them key species for identification. It is also found that the IR signatures of the group of these cations with q = 1-6 are well separated from the 6.2 μm band that is associated with free/isolated aromatic hydrocarbon molecules. This is particularly important in the discrimination and exploration of the coexistence of complex hydrocarbon organics and fullerenes in astronomical sources. To provide insight into the effect of ionization on the IR spectrum of fullerene, particularly at the long-wavelength range, the quantitative analysis of the origin of key bands of these cations is presented. Finally, the potential target(s) among these species, specifically aromatic ${{\rm{C}}}_{60}^{10+}$ , are discussed for further astrochemical observations.

Keywords: Interstellar molecules, Theoretical techniques, Astrochemistry, Infrared astronomy, Planetary nebulae
The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). II. The Spatially Resolved Recent Star Formation History of M33. We measure the spatially resolved recent star formation history (SFH) of M33 using optical images taken with the Hubble Space Telescope as part of the Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER) survey. The area covered by the observations used in this analysis covers a de-projected area of ~38 kpc2 and extends to ~3.5 and ~2 kpc from the center of M33 along the major and semimajor axes, respectively. We divide the PHATTER optical survey into 2005 regions that measure 24 arcsec, ~100 pc, on a side and fit color-magnitude diagrams for each region individually to measure the spatially resolved SFH of M33 within the PHATTER footprint. There are significant fluctuations in the SFH on small spatial scales and also galaxy-wide scales that we measure back to about 630 Myr ago. We observe a more flocculent spiral structure in stellar populations younger than about 80 Myr, while the structure of the older stellar populations is dominated by two spiral arms. We also observe a bar in the center of M33, which dominates at ages older than about 80 Myr. Finally, we find that the mean star formation rate (SFR) over the last 100 Myr within the PHATTER footprint is 0.32 ± 0.02 M⊙ yr-1. We measure a current SFR (over the last 10 Myr) of 0.20 ± 0.03 M⊙ yr-1. This SFR is slightly higher than previous measurements from broadband estimates, when scaled to account for the fraction of the D25 area covered by the PHATTER survey footprint.

Keywords: Stellar populations, Triangulum Galaxy, Star formation, Local Group
Continuous Wavelet Analysis of Matter Clustering Using the Gaussian-derived Wavelet. Continuous wavelet analysis has been increasingly employed in various fields of science and engineering due to its remarkable ability to maintain optimal resolution in both space and scale. Here, we introduce wavelet-based statistics, including the wavelet power spectrum, wavelet cross correlation, and wavelet bicoherence, to analyze the large-scale clustering of matter. For this purpose, we perform wavelet transforms on the density distribution obtained from the one-dimensional Zel'dovich approximation and then measure the wavelet power spectra and wavelet bicoherences of this density distribution. Our results suggest that the wavelet power spectrum and wavelet bicoherence can identify the effects of local environments on the clustering at different scales. Moreover, we apply the statistics based on the three-dimensional isotropic wavelet to the IllustrisTNG simulation at z = 0, and investigate the environmental dependence of the matter clustering. We find that the clustering strength of the total matter increases with increasing local density except on the largest scales. Besides, we notice that the gas traces dark matter better than stars on large scales in all environments. On small scales, the cross correlation between the dark matter and gas first decreases and then increases with increasing density. This is related to the impacts of the active galactic nucleus feedback on the matter distribution, which also varies with the density environment in a similar trend to the cross correlation between dark matter and gas. Our findings are qualitatively consistent with previous studies on matter clustering.

Keywords: Large-scale structure of the universe, Dark matter, Wavelet analysis, Intergalactic medium
The Curious Case of the "Heartworm" Nebula. The curious Galactic features near G357.2-0.2 were observed with the MeerKAT radio interferometer array in the UHF and L bands (0.56-1.68 GHz). There are two possibly related features: a newly identified faint heart-shaped partial shell (the "heart"), and a series of previously known but now much better imaged narrow, curved features (the "worm") interior to the heart. Polarized emission suggests that much of the emission is nonthermal and is embedded in a dense plasma. The filaments of the worm appear to be magnetic structures powered by embedded knots that are sites of particle acceleration. The morphology of the worm broadly resembles some known pulsar wind nebulae (PWNe) but there is no known pulsar or PWN which could be powering this structure. We also present eROSITA observations of the field; no part of the nebula is detected in X-rays, but the current limits do not preclude the existence of a pulsar/PWN of intermediate spin-down luminosity.

Keywords: Neutron stars, Rotation powered pulsars, Galactic radio sources, Extended radiation sources, Supernova remnants
Patchy Nightside Clouds on Ultra-hot Jupiters: General Circulation Model Simulations with Radiatively Active Cloud Tracers. The atmospheres of ultra-hot Jupiters have been characterized in detail through recent phase curve and low- and high-resolution emission and transmission spectroscopic observations. Previous numerical studies have analyzed the effect of the localized recombination of hydrogen on the atmospheric dynamics and heat transport of ultra-hot Jupiters, finding that hydrogen dissociation and recombination lead to a reduction in the day-to-night contrasts of ultra-hot Jupiters relative to previous expectations. In this work, we add to previous efforts by also considering the localized condensation of clouds in the atmospheres of ultra-hot Jupiters, their resulting transport by the atmospheric circulation, and the radiative feedback of clouds on the atmospheric dynamics. To do so, we include radiatively active cloud tracers into the existing MITgcm framework for simulating the atmospheric dynamics of ultra-hot Jupiters. We take cloud condensate properties appropriate for the high-temperature condensate corundum from CARMA cloud microphysics models. We conduct a suite of general circulation model (GCM) simulations with varying cloud microphysical and radiative properties, and we find that partial cloud coverage is a ubiquitous outcome of our simulations. This patchy cloud distribution is inherently set by atmospheric dynamics in addition to equilibrium cloud condensation, and causes a cloud greenhouse effect that warms the atmosphere below the cloud deck. Nightside clouds are further sequestered at depth due to a dynamically induced high-altitude thermal inversion. We post-process our GCMs with the Monte Carlo radiative transfer code gCMCRT and find that the patchy clouds on ultra-hot Jupiters do not significantly impact transmission spectra but can affect their phase-dependent emission spectra.

Keywords: Atmospheric clouds, Hot Jupiters, Planetary atmospheres, Exoplanet atmospheres
Blueshifted Si IV 1402.77 Å Line Profiles in a Moving Flare Kernel Observed by IRIS. We analyze the spectra of a slipping flare kernel observed during the 2015 June 22 M6.5-class flare by the Interface Region Imaging Spectrograph (IRIS). During the impulsive and peak phases of the flare, loops exhibiting an apparent slipping motion along the ribbons were observed in the 131 Å channel of SDO/AIA. The IRIS spectrograph slit observed a portion of the ribbons, including a moving kernel corresponding to a flare loop footpoint in Si IV, C II, and Mg II at a very-high 1 s cadence. The spectra observed in the kernel were mostly redshifted and exhibited pronounced red wings, as typically observed in large flares. However, in a small region in one of the ribbons, the Si IV 1402.77 Å line was partially blueshifted, with the corresponding Doppler velocity ∣v D∣ exceeding 50 km s-1. In the same region, the C II 1334.53, 1335.66, and 1335.71 Å lines were weakly blueshifted (∣v D∣ &lt; 20 km s-1) and showed pronounced blue wings, which were also observed in the Mg II k 2796.35 Å as well as the Mg II triplet 2798.75 and 2798.82 Å lines. Using high-cadence AIA observations we found that the region where the blueshifts occurred corresponds to the accelerating kernel front as it moved through a weak field region. The IRIS observations with high resolution allowed us to capture the acceleration of the kernel under the slit for the first time. The unique observations of blueshifted chromospheric and TR lines provide new constraints for current models of flares.

Keywords: Solar flares, Solar ultraviolet emission, Solar magnetic reconnection, Solar transition region, Solar chromosphere