Sazuna/UAT_keywords huggingface dataset:
The Behavior of HgMn Stars in the Far UV-Paper 11: HD 53929 and HD 172044. The analysis of low and high resolution spectra of the chemically peculiar stars HD 53929 and HD 172044 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far-ultraviolet fluxes of these stars. The far-ultraviolet Ga II and Ga III resonance lines are strong absorbers in the spectrum of HD 172044. The TESS lightcurve of HD 172044 suggests a period close to 4.347 ± 0.135 days which could be the rotational period. On SWP 34118 the resonance lines of Si II and Ga II are blueshifted compared to SWP 34110 probably reflecting the orbital motion of HD 172044.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Evolutionary Status of Selected Post-AGB Single and Binary Stars in Gaia DR3. Gaia data is helping to further understand the evolutionary status of post-AGB and related stars. In this paper we present an analysis of Gaia DR3 data of post-AGB stars and post-AGB binaries with accurate parallaxes. Gaia DR3 data of 44 post-AGB candidates are analyzed, including 16 post-AGB binary candidates. Of these, 19 stars have RUWE values &gt;1.4. For several stars, the calculated absolute luminosities confirm that they are indeed in post-AGB evolutionary stage. We find that 12 stars have relatively lower luminosities; some of them may be post-RGB stars and some may be post-HB stars. We find that IRAS 01427+4633 (BD+46 442), IRAS 16230-3410, and IRAS 19199+3950 (HP Lyr) are evolved high velocity stars.

Keywords: Stellar distance, Post-asymptotic giant branch stars, Binary stars, Stellar evolution
Photometric Masses of Eclipsing Binary Components. Eclipsing binaries allow the study of physical stellar parameters in a model-independent way, when photometric and spectroscopic data are combined. However, when spectroscopic data are not available, purely photometric methods can be adopted to first estimate stellar properties, especially for large samples. Cruz et al. have then characterized components of detached EB systems from photometric colors and light curves from the literature, with the purpose of estimating trends from statistical values. An inflation trend of around 20% was estimated, which is in agreement with several results from the literature. As a response to MacDonald &amp; Mullan, the obtained values for individual systems should not be analyzed separately, since they could mislead the results. We encourage further spectroscopic measurements to verify the values estimated from the photometric method.

Keywords: Eclipsing binary stars, Photometry
Orb_It: A Validation Package for Orbit Integrators. We present a testing platform and package that can validate the accuracy of an orbit integrator. Orb_It is written in Python and is capable of validating the most heavily used orbital integrators such as Find_Orb, OpenOrb, and OrbFit. Orb_It performs an "end-to-end" test of each integrator to check for internal consistency of the integrators functions. For a given objects state vector and epoch, Orb_It uses a user-specified integrator to generate the objects ephemeris for a specified time range and observer, uses those ephemerides as observations to fit an orbit, and then compares that fitted orbit to the original input state vector propagated to the fitted orbits epoch. This allows users to understand the internal accuracy of each integrator. This testing suite and package can be found on GitHub with a demo on Binder (https://github.com/B612-Asteroid-Institute/orb_it).

Keywords: Ephemerides, Small Solar System bodies, Asteroids, Astronomy software, Orbit determination
Plaskett's Star and Its Environment. Astrometric information from GAIA DR3 is used to examine the environment around the massive binary system Plaskett's Star (PS). PS is found to be embedded in a stellar grouping that has distinct kinematic and spatial distributions. Based on the characteristics of these neighboring stars, it is suggested that PS may have formed during the earliest phases of star formation in the neighboring cluster NGC 2244-if so, then PS likely has an age in excess of ~5 million years.

Keywords: Binary stars, Oe stars
Hydrostatic Equilibrium Does Not Solve the C<SUP>18</SUP>O Flux Problem in Protoplanetary Disks. ALMA observations have shown that there is discrepancy between the disk mass estimate from CO emission and disk masses estimated from other tracers. This discrepancy has been interpreted as lower than expected CO abundance in the warm, surface layers of the disk. Recent work by Ruaud et al. claims that the low observed C18O fluxes can be explained with a ISM abundance of CO, that is 10-4 w.r.t. H2 by including hydrostatic equilbrium in the model density setup. We show that the Ruaud et al. low CO fluxes are due to an unrealistic temperature structure in the outer disk, due to an interaction of their dust model and hydrostatic equilibrium at their inner model edge. Furthermore, we show with our own modeling that a parametric model does a better job at matching the measured outer disk temperature structure.

Keywords: Protoplanetary disks, Astrochemistry
New Close Binary Central Stars of Planetary Nebulae from Gaia DR3 Epoch Photometry. Close binary interactions perform a key role in the formation and shaping of planetary nebulae (PNe). However only a small fraction of Galactic PNe are known to host close binary systems. Many such systems are detectable through photometric variability. We searched recently published epoch photometry data from Gaia DR3 for planetary nebula central stars with periodic photometric variability indicative of binarity, uncovering four previously unknown close binaries.

Keywords: Planetary nebulae nuclei, Planetary nebulae, Gaia, Common envelope binary stars
Infrared Coronal Line Emission during the 2010 Outburst of the Recurrent Nova U Scorpii. Infrared spectroscopy of the recurrent nova U Scorpii from 14.2 days after its 2010 outburst reveals two very strong infrared coronal lines: [Si X] at 1.4305 μm and [Al IX] at 2.0400 μm. Taken together with the detection of coronal lines in the 2022 outburst, this suggests that coronal line emission from U Sco may be a regular, if previously under-observed, occurrence. The strength of the two coronal lines relative the H I emission, and the surprising absence of several commonly seen coronal lines, including some that form under similar conditions as the [Si X] and [Al IX] features, are discussed.

Keywords: Recurrent novae
Smallest Scale Clumpy Star Formation in Stephan's Quintet Revealed from UV and IR Imaging. The spatial distribution and physical sizes of star-forming clumps at the smallest scales provide valuable information on hierarchical star formation (SF). In this context, we report the sites of ongoing SF at ~120 pc along the interacting galaxies in Stephan's Quintet compact group using AstroSat-UVIT and JWST data. Since ultraviolet radiation is a direct tracer of recent SF, we identified star-forming clumps in this compact group from the FUV imaging which we used to guide us to detect star-forming regions on JWST IR images. The FUV imaging reveals star-forming regions within which we detect smaller clumps from the higher spatial resolution images of JWST, likely produced by PAH molecules and dust ionized by FUV emission from young massive stars. This analysis reveals the importance of FUV imaging data in identifying star-forming regions in the highest spatial resolution IR imaging available.

Keywords: Ultraviolet astronomy, Star formation
Polar Upwelling at Three Sunspot Minima. We summarize the analysis methods used to derive differential rotation leading to the Torsional Oscillations (TO) and a new method for determining Meridional Circulation (MC). The new MC results show a reversal of the flow direction at near-polar latitudes with the time of reversal corresponding closely to the time of sunspot Minima.

Keywords: Solar rotation, Solar meridional circulation, Sunspot cycle
Revisiting the Mass-excitation (MEx) Diagram using the MaNGA Data Set. The diagram comparing the flux ratio of the [O III] and Hβ emission lines with the total stellar mass of galaxies (also known as the mass-excitation diagram, MEx) has been widely used to classify the ionization mechanism in high redshift galaxies, dividing star-forming galaxies from those where active galactic nuclei are important. This diagram was mainly derived using single-fiber spectroscopy from the SDSS-DR7 survey. In this study, we revise this diagram using the central and integrated spectral measurement from the entire Integral Field Spectroscopic MaNGA sample. Our results suggest that along with these physical parameters, the equivalent width of the Hα emission line is also required to constrain the ionization mechanism of a high-redshifted galaxy. Furthermore, the location of a galaxy in the excitation-mass diagram varies depending on the use of central or integrated properties.

Keywords: Surveys, Astronomical techniques, Active galactic nuclei, Spectroscopy, High-redshift galaxies
The Exoplanet Modeling and Analysis Center at NASA Goddard. The Exoplanet Modeling and Analysis Center (EMAC) at NASA Goddard Space Flight Center is a web-based catalog, repository, and integration platform for modeling and analysis resources focused on the study of exoplanet characteristics and environments. EMAC hosts user-submitted resources ranging in category from planetary interior models to data visualization tools. Other features of EMAC include integrated web tools developed by the EMAC team in collaboration with the tools' original author(s) and video demonstrations of a growing number of hosted tools. EMAC aims to be a comprehensive repository for researchers to access a variety of exoplanet resources that can assist them in their work, and currently hosts a growing number of code bases, models, and tools. EMAC is a key project of the NASA GSFC Sellers Exoplanet Environments Collaboration and can be accessed at https://emac.gsfc.nasa.gov.

Keywords: Exoplanet dynamics, Open source software, Astronomy databases, Astronomy software, Exoplanets, Exoplanet systems, Software tutorials, Planetary science, Star-planet interactions, Planetary interior, Astronomy data visualization, Exoplanet atmospheres
Expected Brightness of Ejecta Caused by the DART Impact. We estimate the volume of material that could be excavated from asteroid Dimorphos and expelled into the surrounding space by the DART impact on 2022 September 26. What emerges from our computations is that the total volume of ejected material could be as high as 5710 m3. Assuming that the fraction of fine-dust particles constitutes 5% of this volume, we estimate the apparent brightness of the ejecta to be (6.5 ± 1.5) mag in the V filter. This makes ground-based astronomical observations of the DART impact on asteroid Dimorphos with small telescopes feasible.

Keywords: Impact phenomena, Near-Earth objects, Ejecta, Asteroids, Broad band photometry, Astronomical simulations
Noise2Astro: Astronomical Image Denoising with Self-supervised Neural Networks. In observational astronomy, noise obscures signals of interest. Large-scale astronomical surveys are growing in size and complexity, which will produce more data and increase the workload of data processing. Developing automated tools, such as convolutional neural networks (CNN), for denoising has become a promising area of research. We investigate the feasibility of CNN-based self-supervised learning algorithms (e.g., Noise2Noise) for denoising astronomical images. We experimented with Noise2Noise on simulated noisy astronomical data. We evaluate the results based on the accuracy of recovering flux and morphology. This algorithm can well recover the flux for Poisson noise (98.13 ${}_{-0.90}^{+0.77} \% $ ) and for Gaussian noise when image data has a smooth signal profile (96.45 ${}_{-0.96}^{+0.80} \% $ ).

Keywords: Astronomy image processing, Astronomy data reduction, Neural networks
9-yr Deep Sky unWISE Coadds. We present our most recent set of "full-depth" unWISE coadds, static sky stacks that combine nine years of Wide-field Infrared Survey Explorer (WISE) and NEOWISE exposures, resulting in the deepest ever 3-5 μm full-sky maps. Here, we publicly release these all-sky W1 (3.4 μm) and W2 (4.6 μm) coadded images.

Keywords: Infrared astronomy, Astronomy data analysis, Astronomy image processing
VVV J165507.19-421755.5: A Nearby T Dwarf Hidden in the Galactic Plane. We present the discovery of VVV J165507.19-421755.5, a mid-T dwarf found through ongoing unWISE-based proper motion searches. A near-infrared spectrum of this object obtained with the NIRES instrument on the Keck II telescope indicates a spectral classification of T5. Using data from the VISTA Variables in the Via Lactea (VVV) catalog with a 9 year baseline, we measure a proper motion of ( ${\mu }_{\alpha }\cos (\delta )$ , μ  δ ) = (-631.0 ± 1.3, -315.0 ± 1.4) mas yr-1 and a trigonometric parallax of π abs = 66.0 ± 4.8 mas, corresponding to a distance of 15.2 ± 1.1 pc. The trigonometric parallax agrees well with our photometric distance estimate (16.1 ${}_{-3.9}^{+5.1}$ pc) assuming that VVV J165507.19-421755.5 is a single T5 dwarf. VVV J165507.19-421755.5 is a new member of the 20 parsec census.

Keywords: Brown dwarfs, Infrared spectroscopy, Spectroscopy, T dwarfs
The Silicon Lines in the Far Ultraviolet Spectrum of HD 172883. The comparison of the mean high resolution spectrum of the chemically peculiar star HD 172883 recorded by the SWP camera on board the International Ultraviolet Explorer with the mean spectrum of HD 38899, a normal late B-type star having similar fundamental parameters, reveals the large flux deficiency of HD 172883 shortwards of 1700 Å. This flux deficiency is due to the strong lines, photoionization edges and autoionization transitions of Si II. The three strongest autoionization lines of Si II are present The strong resonance line of Al II conspicuous in HD 38899 is very ewak in HD 172883 highlighting a strong aluminum deficiency in HD 172883. Conversely, the Hg II resonance line at 1649.94 Å is much stronger in HD 172883, confirming the large overabundance of mercury in this star.

Keywords: Mercury-manganese stars, Chemically peculiar stars
The JWST Resolved Stellar Populations Early Release Science Program. I. NIRCam Flux Calibration. We use globular cluster data from the Resolved Stellar Populations Early Release Science (ERS) program to validate the flux calibration for the Near Infrared Camera (NIRCam) on the James Webb Space Telescope. We find a significant flux offset between the eight short wavelength detectors, ranging from 1% to 23% (~0.01-0.2 mag) that affects all NIRCam imaging observations. We deliver improved zero-points for the ERS filters and show that alternate zero-points derived by the community also improve the calibration significantly. We also find that the detector offsets appear to be time variable by up to at least 0.1 mag.

Keywords: Globular star clusters, James Webb Space Telescope, Flux calibration
A Visually Classified Spectroscopic Object Catalog for SDSS-IV MaNGA. We provide a catalog of visually classified objects in the MaNGA integral field spectroscopic survey. The MaNGA survey is designed to target a single galaxy with each of its integral field units; however, many of these fields will host ancillary objects. We identify these discrete objects by cleaning up SDSS photometric objects in MaNGA's fields-of-view. We then use the spectra from MaNGA's data cubes to spectrally classify the identified objects. The catalog contains the positions and classifications of 1385 stars, 11,439 galaxies, and 107 broad-line active galactic nucleus (BLAGN) from the 10,130 unique MaNGA fields. We also provide spectroscopically derived parameters for the galaxies including; stellar masses, gas and stellar kinematics, and emission-line fluxes and equivalent widths. This catalog effectively expands the size of the MaNGA catalog by ~50%, increasing the utility of the MaNGA project.

Keywords: Galaxies
The Behavior of HgMn stars in the far-UV -Paper 13: HD 182308 and HD 190229. The analysis of low and high resolution spectra of the chemically peculiar stars HD 182308 and HD 190229 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far-ultraviolet fluxes of these stars. The far-ultraviolet resonance lines of Ga II and Ga III are strong absorbers in the spectrum of HD 182308. A search for successive maxima in the TESS lightcurves of HD 182308 and HD 190229 suggests periods close to 19.11 ± 0.15 days and 9.50 ± 0.15 days respectively which could be the rotational periods.

Keywords: Chemically peculiar stars
VLT/CRIRES Science Verification Observations: A hint of C<SUP>18</SUP>O in the Young Brown Dwarf 2M0355. Chemical and isotopic composition provide insights into the formation and evolution history of planets and brown dwarfs. Recent measurements of 12CO/13CO abundance ratios in the atmosphere of the young super-Jupiter YSES-1b and the isolated brown dwarf 2MASS J03552337+1133437 may point to distinct formation pathways. Here we present our analysis of 0.5 hr of science verification observations using the recently upgraded CRIRES spectrograph at ESO's Very Large Telescope on the same brown dwarf, with the aim to detect C18O and determine the 16O/18O isotope ratio. Our free retrieval analyses confirm the previous measurement of the carbon isotope ratio, and the inclusion of the C18O molecule in our models enables an initial tentative constraint of 16O/18O = ${1489}_{-426}^{+1027}$ on the oxygen isotope ratio, but this requires more data to be confirmed. These short observations showcase the prospect of studying the isotope inventory in brown dwarfs and super-Jovian exoplanets with high-dispersion spectroscopy.

Keywords: Brown dwarfs, Exoplanet atmospheres
LOFAR Search for Radio Emission from Galaxies Hosting Tidal Disruption Events. Radio emission from 23 tidal disruption event host galaxies were searched in the 144 MHz LOFAR-LoTSS2 images. Three host galaxies are detected with diffuse radio emission, which can be interpreted as either galactic synchrotron radio emission or diffuse radio halo in dense galactic environments. Non-detection of (transient) radio emission in majority of galaxies could be due to self-absorption of radio emission associated with the tidal disruption event.

Keywords: Extragalactic radio sources, Tidal disruption, Galaxy interactions
Characterization of a Solar Mass Eclipsing Binary with TESS and IGRINS. Stellar radius measurements from eclipsing binaries are typically ~5% larger than standard stellar models predict. This disagreement means we are unable to derive reliable model-dependent radii, which impact stellar and exoplanet characterization. Using light curves from the TESS satellite and high-resolution, near-infrared spectra from IGRINS, we determine the masses and radii of a main sequence eclipsing binary, V1177 Cen (TIC 3099339). We detrend the light curve using a Gaussian process and derive radial velocities using spectral-line broadening functions, fitting both jointly in an MCMC framework. We find that both stars are near 1 M ⊙ with radii 6%-9% larger than the Sun. Based on the absence of Lithium in optical spectra, the inflation is potentially the effect of early post-main sequence evolution, or magnetic fields. We compare our measurement to model isochrones, finding the most consistent agreement with models that include magnetic fields, and correspond to an age of ~4 Gyr.

Keywords: Eclipsing binary stars
Breakthrough Listen Search for the WOW! Signal. Caballero identified the star 2MASS 19281982-2640123 as a potential Sun-like star from which the WOW! signal could have originated. We conducted a search for artificial narrowband (2.79 Hz/1.91 Hz), drifting (±4 Hz s-1) technosignatures from this source using the TURBOSETI pipeline, from 1-2 GHz, using simultaneous multi-telescope observations with both the Robert C. Byrd Green Bank Telescope and the newly refurbished Allen Telescope Array on 2022 May 21. Both telescope observations had an overlap of 580 s. While blind searches using radio telescopes have been conducted in the general field of view in which the WOW! signal was first detected, this is the first time a targeted search has been done. No technosignature candidates were detected. *Dedicated to the memory of Bart S. Wlodarczyk-Sroka.

Keywords: Biosignatures, Search for extraterrestrial intelligence, Technosignatures, Radio astronomy
[Eu/Ba]: Clock and r-process Indicator. The europium to barium ratio is both a clock and a measure of galactic chemical evolution of the r- and s-processes. We attribute much of the ratio's vertical scatter to real abundance differences attributable to streams and diffusion into and out of the solar neighborhood.

Keywords: F dwarf stars, K dwarf stars, G dwarf stars
The Behavior of HgMn Stars in the Far UV -Paper 14: HD 179761. The analysis of low and high resolution spectra of the late B-type star HD 179761 recorded by the SWP camera on board the International Ultraviolet Explorer reveals no variations of the far ultraviolet flux of this star in 1983 May and June. The far ultraviolet resonance lines of Si II are strong absorbers in the spectrum of HD 179761. The resonance lines of Ga II, Ga III and Hg II, characteristic of clasical HgMn stars, do not seem to be present in the mean SWP spectrum of HD 179761. The currently available TESS lightcurves of HD 179761 suffer from data dropouts and suggest low amplitude variations with periods runing from 4.86 to 5.44 days which need confirmation.

Keywords: Chemically peculiar stars
EPIC 219511354, A Binary Pair of Active K-stars: Modeling Activity-induced Radius Inflation by Magneto-convection. Magnetically active low-mass stars are observed to have their empirical radii R "inflated" and their empirical T eff reduced relative to standard predictions. Models which have been proposed to replicate these discrepancies include magneto-convection (M-C), and/or star-spots (S-S). Here we raise the question: is there any reason to prefer a dominant role for either M-C or S-S in order to replicate the data? In the binary EPIC 219511354, the empirical M and R values have remarkably high (1%-2%) precision. To replicate these data, the S-S model requires almost the entire (88%-94%) secondary surface to be spotted. Here, we report that our M-C model fits the empirical R and T eff values for both members of the binary within 1σ error bars without needing spots. If an areal spot coverage of 94% is regarded as physically implausible, the M-C model could be considered preferable over S-S in EPIC 219511354.

Keywords: K dwarf stars, Magnetic stars, Stellar evolutionary models, Stellar magnetic fields
A Pilot Survey of an M Dwarf Flare Star with Swift's UV Grism. The near-ultraviolet (NUV) spectral region is a useful diagnostic for stellar flare physics and assessing the energy environment of young exoplanets, especially as relates to prebiotic chemistry. We conducted a pilot NUV spectroscopic flare survey of the young M dwarf AU Mic with the Neil Gehrels Swift Observatory's UltraViolet and Optical Telescope. We detected four flares and three other epochs of significantly elevated count rates during the 9.6 hr of total exposure time, consistent with a NUV flare rate of ~0.5 hr-1. The largest flare we observed released a minimum energy of 6 × 1033 erg between 1730 and 5000 Å. All flares had durations longer than the ~14-17 minutes duration of each Swift visit, making measuring total flare energy and duration infeasible.

Keywords: M dwarf stars, Near ultraviolet astronomy, Pre-main sequence stars, Stellar flares, Pre-biotic astrochemistry