Sazuna/UAT_keywords huggingface dataset:
False Alarms Revealed in a Planet Search of TESS Light Curves. In this paper, we investigate the impact of false alarms on planet searches of TESS data by performing a search of a large number of stars. We examine the period distribution of transit-like signatures uncovered in a Box-Least Squares transit search of TESS light curves, and show significant pileups at periods related to instrumental and astrophysical noise sources. Signatures uncovered in a search of inverted light curves feature similar structures in the period distribution. Automated vetting methods will need to remove these excess detections, and light curve inversion appears to be a suitable method for simulating false alarms and designing new vetting metrics. Automated vetting will be a significant step toward making TESS data useful for demographic studies.

Keywords: Transit photometry, Exoplanets
Research, Experiment and Validation of Adaptive Optics with a Legacy Telescope (REVOLT): First On-sky Results. The first on-sky results of the Research, Experiment and Validation of Adaptive Optics with a Legacy Telescope (REVOLT) project are presented, along with a description of the project and its purpose. The REVOLT project has so far demonstrated successful closed loop, single conjugate adaptive optics using a natural guide star at the 1.22 m McKellar telescope at the Dominion Astrophysical Observatory in Victoria, BC, Canada. In so doing, we have made the first on-sky demonstration of the Herzberg Extensible Adaptive Realtime Toolkit-based Real Time Controller, and First Light Imaging's C-Blue One camera.

Keywords: Astronomical detectors, Astronomical instrumentation, Adaptive optics
On the Spatial Distribution of Polarization and Color of a Distant Comet C/2017 K2 (PanSTARRS). Comet C/2017 K2 (PanSTARRS) was observed at two wavelengths using two different-sized apertures in two measurement campaigns. We find that all the observations can be interpreted using a two-component mixture of dust composed of Mg-rich silicates and amorphous carbon. The modeling suggests a slight increase in the absorption of the refractory component at shorter wavelengths, which is consistent with the optical properties of Mg-rich silicates, and a change in the size distribution as a function of distance from the cometary nucleus, a result of smaller particles accelerating more rapidly from the expanding-gas and radiative-pressure forces.

Keywords: Long period comets, Comets, Comae, Coma dust
The Abundances of Carbon, Sulfur, Scandium, Titanium, Manganese, Iron, Gallium and Strontium in the Atmosphere of HD144844. Abundances of manganese and gallium are derived in LTE for the B9 Mn P Ga star HD 144844 using the Mn II lines at 4206.37 and 4259.19 Å and the Ga II line at 6334.07 Å including hyperfine spliting and nuclear shifts. Both elements are found to be overabundant, about 7-10 times the manganese abundance, depending on the line of Mn II used, and about 1800 times the solar gallium abundance. The synthesis of three Fe II lines at 4258.15, 4273.33 and 4296.57 Å yields an abundance of iron marginally above the solar iron abundance. The synthesis of other lines in the range 4200 up to 4300 Å yields information on the abundances of carbon and sulfur (0.05 times the solar abundances), of scandium (5 solar), titanium (1.5 solar), strontium (4.5 solar) and samarium (consistent with a 1.0 solar upper limit).

Keywords: Helium-weak stars, Chemically peculiar stars
The Behavior of HgMn Stars in the Far UV-Paper 25: HD 77350. The analysis of five spectra of the Hg Mn spectroscopic binary star HD 77350 recorded by the SWP camera on board the International Ultraviolet Explorer reveals one instance of variation of the far-ultraviolet flux of this star shortwards of 1800 Å. The analysis of the coadded SWP spectrum built from the high resolution SWP spectra obtained through the small aperture shows the importance of low excitation and resonance Si II lines shortwards of 1540 Å, of the Ga II and Ga III resonance lines at 1414 and 1495 Å and of the Al II resonance line at 1670 Å. A very rough estimate of a period from the currently available Transiting Exoplanet Survey Satellite lightcurves yields a value of 9.63 ± 0.18 days which could be the rotation period but this needs confirmation.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Non-confirmation of the Astrometric Binary Candidate HD 113283 Using FEROS Radial Velocities. We present fifteen radial velocity (RV) measurements taken with FEROS for the astrometric binary candidate HD 113283 analyzed with the "exoplanet pipeline" and published in the nss_two_body_orbit table of Gaia Data Release 3. We have performed a periodogram analysis on the RVs and found no evidence of the stellar companion of mass m 2 &gt; 0.15M ⊙. We discuss indications for the likely spurious astrometric two-body solution based on the Gaia products, including the comparably low significance, the small reduction of the astrometric excess noise after applying the two-body solution, inconsistent with the provided orbital solution, and the proximity of the orbital period to periods of known spurious solutions caused by Gaia's scanning law. We aim to contribute toward a refined solution filtering of the Gaia two-body solutions.

Keywords: High resolution spectroscopy, Binary stars, Spectroscopic binary stars, Astrometric binary stars, Astrometry, Radial velocity, Gaia
Identifying Ultracool Binary Systems using Machine Learning Methods. Ultracool spectral binaries are unresolved pairs of low-mass stars and brown dwarfs revealed by peculiarities in their combined light spectra. Methods to identify these systems have relied on spectral indices, which have known selection biases. We report on a pilot study examining the application of machine learning methods to identify ultracool spectral binaries. Using a sample of single and binary templates constructed from low-resolution, near-infrared spectra, we trained a random forest model to identify binaries composed of M7-L7 primaries and T1-T8 secondaries. We find that uniform data preparation and balancing of the training sample are critical to building an effective model. Our model achieves precisions of ≥95%, confirms known spectral binaries, and identifies new spectral features sensitive to multiplicity, illustrating the utility of machine learning methods to identify these rare systems.

Keywords: M dwarf stars, Brown dwarfs, Close binary stars, L dwarfs, T dwarfs
The Behavior of HgMn Stars in the Far-UV-Paper 26: HD 207857. The analysis of two spectra of the Mn P Ga spectroscopic binary HD 207857 recorded by the SWP camera on board the International Ultraviolet Explorer reveals one instance of variation of the far-ultraviolet flux of this star over a time interval of about 10 months. The orbital period of this spectroscopic binary being 338.2 days, the observed increases of flux below 1800 Å could be due to the presence of a hot companion.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Photometric Observations of Nine High Mass X-Ray Binaries and Analysis of Potential Periodicities and Variations. Beginning with American Association of Variable Star Observers Alert Notice 348 (2007 April 6) and being continually extended and updated through 2020 April 17 with Alert Notice 377, Dr. Gordon Sarty requested continuing assistance with his ongoing radial velocity observations of High Mass X-Ray Binaries. As of Alert Notice 377, nine targets were identified. These are: 1H 1936+541, RX J2030.5+4751, V2175 Cyg, V1008 Cep, V831 Cas, RX J0440.9+4431/LS V+44 17, V420 Aur, HD 249179, and SAX J0635+0533. While these Alert Notices prioritized radial velocity observations with the objective of determining orbital periods of these binary systems, optical photometry can also reveal other periods and variations due to mass transfer, pulsations, rotations, spin rates, and other effects. This Research Note will address in more detail the observation and analysis of one of these nine High Mass X-Ray Binaries, specifically 1H 1936+541.

Keywords: High mass x-ray binary stars
The Behavior of HgMn Stars in the Far UV-Paper 27: HD 1909. The analysis of two spectra of the spectroscopic binary B9 Hg star HD 1909 recorded by the SWP camera on board the International Ultraviolet Explorer reveals one instance of variations of the far-ultraviolet flux of this star from 1300 up to 2000 Å. The first TESS lightcurve of HD 1909 on the MAST website is periodic with a period close to 7 days which is very close to an earlier period found for the variations of the Strömgren index u. The FUV variations, which occur over about 5 yr, could be caused by the motion of the lower mass companion.

Keywords: Mercury-manganese stars, Chemically peculiar stars
FluxCT: A Web Tool for Identifying Contaminating Flux in Kepler and TESS Target Pixel Files. We announce FluxCT, a web tool for identifying contaminating flux in Kepler and TESS target pixel files due to secondary visual sources. We demonstrate the usage of this tool and discuss the benefits of this tool over a simple Gaia radius search. FluxCT focuses on clarity and simplicity, where the only input needed from the user is a KIC or TIC ID. By more appropriately accounting for the actual shape of the photometric pixel apertures, FluxCT can produce much more accurate estimates of contaminating flux than simple radial cone searches.

Keywords: Stellar astronomy, Educational software, Astronomy software
Are Brightest Cluster Galaxies Special?. A longstanding question when studying Brightest Cluster Galaxies (BCGs) and their evolution is whether their luminosities are statistical extremes of the luminosity distribution of other cluster member galaxies, or whether their luminosities follow a different,"special" distribution. To explore this question, we use the two Tremaine-Richstone (TR) statistics that sometimes lead to different conclusions about BCG specialness. We run Monte Carlo simulations of galaxy clusters with varying galaxy luminosity functions and BCG properties, and explore the sensitivity of the TR statistics to the adjusted BCG properties. We identify cases where the two statistics lead to different conclusions. The first of the TR statistics, which relies on the spread of BCG luminosities, is more reliable for determining specialness than the second, which utilizes the spread in the luminosity gap between the BCG and second ranked galaxy.

Keywords: Brightest cluster galaxies
Early Galaxy Formation and the Hubble Constant Tension. Tension between local determinations of the Hubble constant and the value found in fits to the cosmic microwave background (CMB) acoustic power spectrum have emerged as finer angular scales (higher multipoles ℓ) have been measured in the latter. Independent observations indicate that massive galaxies emerged at higher redshift than anticipated in the standard ΛCDM structure formation paradigm. If genuine, these early galaxies would cause excess gravitational lensing of the CMB, adding an anomalous source of power at high ℓ. I suggest that accommodating this anomalous source of power in multiparameter fits might be the root cause of the Hubble tension rather than systematics in local measurements.

Keywords: Hubble constant, Galaxy formation, Cosmic microwave background radiation
Identifying Habitable-zone Planet Systems Susceptible to Nearby Supernovae. We investigate whether any known candidate habitable-zone exoplanet systems could be imperiled by being sufficiently close to a future supernova. Using existing exoplanet databases, we identify 24 stars possessing at least one planet in the star's habitable zone. We search the Gaia EDR3 catalog for possible core-collapse supernova progenitors within 150 lt-yr of each of these systems, using Pan-STARRS and Gaia EDR3/DR2 colors to identify neighboring stars that are likely to have masses ≥8M ⊙ (i.e., potential supernova Type II progenitors). Within, our sample, we find one instance of a habitable-zone planetary system within 150 lt-yr of a possible Type II supernova progenitor.

Keywords: Habitable zone, Supernovae, Core-collapse supernovae
Discovery of Dust Emission Activity Emanating from Main-belt Asteroid 2015 FW412. We present the discovery of activity emanating from main-belt asteroid 2015 FW412, a finding stemming from the Citizen Science project Active Asteroids, a NASA Partner program. We identified a pronounced tail originating from 2015 FW412 and oriented in the anti-motion direction in archival Blanco 4 m (Cerro Tololo Inter-American Observatory, Chile) Dark Energy Camera images from UT 2015 April 13, 18, 19, 21 and 22. Activity occurred near perihelion, consistent with the main-belt comets (MBCs), an active asteroid subset known for sublimation-driven activity in the main asteroid belt; thus 2015 FW412 is a candidate MBC. We did not detect activity on UT 2021 December 12 using the Inamori-Magellan Areal Camera and Spectrograph on the 6.5 m Baade telescope, when 2015 FW412 was near aphelion.

Keywords: Comet tails, Asteroid belt, Asteroids, Comae
The JWST Resolved Stellar Populations Early Release Science Program. III. Photometric Star-Galaxy Separations for NIRCam. We present criteria for separately classifying stars and unresolved background galaxies in photometric catalogs generated with the point-spread function fitting photometry software DOLPHOT from images taken of Draco II, WLM, and M92 with the Near Infrared Camera (NIRCam) on JWST. Photometric quality metrics from DOLPHOT in one or two filters can recover a pure sample of stars. Conversely, colors formed between short-wavelength and long-wavelength filters can be used to effectively identify pure samples of galaxies. Our results highlight that the existing DOLPHOT output parameters can be used to reliably classify stars in our NIRCam data without the need to resort to external tools or more complex heuristics.

Keywords: Multi-color photometry, Classification, Stellar populations, Two-color diagrams, James Webb Space Telescope, Photometry
The Far-ultraviolet Variability of the Early A-type Star HD 1280 (θ And). The analysis of two spectra of the early A-type star HD 1280, recorded by the SWP camera on board the International Ultraviolet Explorer, reveals large variations of the far-ultraviolet flux shortwards of 1850 Å. The amplitude of these variations increases toward shorter wavelengths. In contrast, the mid-ultraviolet flux from 2200 up to 3000 Å is constant in the available spectra collected with the LWP camera. These variations could be due to large horizontal chemical or thermal gradients over the stellar surface, or stellar pulsation, or the presence of a companion.

Keywords: Am stars, A stars
The Effect of Multiple Low-mass Flybys Can Preserve the Orbit of Neptune-like Objects in Slightly Perturbed Orbits in Star Formation Clusters. The objective of this work is focused on solving the problem in the regular theory where the strong effects of single impacts on proplanetary particles in the early stages of the Solar system can noticeably perturb the orbit of inner planets such as Neptune. As a first-approach solution, I propose that multiple low-mass flybys can produce the observed orbit of a Neptune-like particle. I calculated the effects of four subsequent flybys to know the difference between their effects and the effect of a massive encounter. The effects of multiple low-mass impacts deliver lower eccentricities and inclinations of the planetary particle compared to the result produced by the single encounter.

Keywords: Orbits, Debris disks, Protoplanetary disks, Stellar dynamics
Early Infrared and Visible Spectra from the 2022 Outburst of the Recurrent Novae U Scorpii. Spectroscopy from 0.46-2.5 μm is presented for the 2022 outburst of the recurrent nova U Scorpii from 2.54, 3.60, and 8.59 days after maximum light. During this period the spectra evolved from comparatively low excitation to the verge of displaying coronal lines. Between days 2.54 and 3.60, the nova showed a marked decrease in the low excitation lines of N I, O I, and Mg II , an increase in He I, the emergence of N III, and changes to the very broad line profiles. By day 8.59, the He I lines had been largely replaced by He II emission and most broad component were weak or undetectable. No optical coronal lines were observed during or immediately following the detection of infrared coronal lines by Banerjee et al.

Keywords: Recurrent novae
New Active Asteroid 2015 VA108: A Citizen Science Discovery. We announce the discovery of activity, in the form of a distinct cometary tail, emerging from main-belt asteroid 2015 VA108. Activity was first identified by volunteers of the Citizen Science project Active Asteroids (a NASA Partner). We uncovered one additional image from the same observing run which also unambiguously shows 2015 VA108 with a tail oriented between the anti-solar and anti-motion vectors that are often correlated with activity orientation on sky. Both publicly available archival images were originally acquired UT 2015 October 11 with the Dark Energy Camera (DECam) on the Blanco 4 m telescope at the Cerro Tololo Inter-American Observatory (Chile) as part of the Dark Energy Camera Legacy Survey. Activity occurred near perihelion and, combined with its residence in the main asteroid belt, 2015 VA108 is a candidate main-belt comet, an active asteroid subset known for volatile sublimation.

Keywords: Comet tails, Asteroid belt, Asteroids
QLP Data Release Notes 003: GPU-based Transit Search. The Quick-Look Pipeline (QLP; Huang et al. 2020; Kunimoto et al. 2021, and references therein) searches for transit signals in the multi-sector light curves of several hundreds of thousand stars observed by TESS every 27.4 day sector. The computational expense of the planet search has grown considerably over time, especially as the TESS observing baseline continues to increase in the second Extended Mission. Starting in Sector 59, QLP has switched to a significantly faster GPU-based transit search capable of searching an entire sector in only ~1 day. We describe its implementation and performance.

Keywords: Exoplanet detection methods, Transit photometry, Exoplanets, Time series analysis
Revised Radiative Response Coefficients for the Curiosity Rover Mastcam from Direct Solar Images and Analog Tests. We have used solar images taken by the Curiosity rover's Mastcam to derive new radiometric response coefficients. In addition, we used calibration data from the Perseverance rover's Mastcam-Z instrument, which used the same detector, to estimate temperature sensitivity of the radiative response. The new coefficients allow calibration of raw data to radiance using the illuminant (the Sun) as the calibration source. Compared to the original pre-flight and early in-flight calibration, the revised calibration is expected to be more consistent across instrument temperature and allow for a self-consistent conversion to radiance factor values when contemporaneous calibration target images are not available or not appropriate. The revised coefficients were incorporated in a recalibration of Mastcam radiance products.

Keywords: Space vehicle instruments, Mars, Calibration
New Determinations of the Surface Abundances of HD 1909: Paper I: The Light Elements (from Helium to Sulfur). New abundances for the elements helium to sulfur are derived for the brightest member of the spectroscopic binary HD 1909 using updated atomic data and spectrum synthesis. The majority of these elements are underabundant, the depletion factors appear in parenthesis: helium (0.02 times the solar helium abundance), carbon and oxygen (0.40 ⊙), neon (0.15 ⊙), magnesium (0.45 ⊙), aluminum (0.02 ⊙). silicon (0.50 ⊙) and sulfur (0.35 ⊙). In contrast, phosphorus is overabundant by a factor of 12.5 ⊙ and the silicon-phosphorus-sulfur triad is inverted. The lines of the companion are redshifted by about +122.5 km s-1 with respect to the B9 Hg star in the spectrum analyzed here.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Exploring the Chemical Evolution of Nitrogen and Oxygen in Local Star-forming Galaxies. We utilize a sample of 45 local star-forming galaxies (z &lt; 0.18) from the COS Legacy Archive Spectroscopic SurveY (CLASSY) to analyze the N/O versus O/H relationship. Nitrogen and oxygen are ejected into the interstellar medium at different timescales by intermediate-mass and massive stars. Therefore, the N/O abundance ratio with respect to the gas-phase metallicity (O/H) is a powerful tool to improve our interpretation on galaxy formation and evolution. In order to analyze such a relation, we derive the the electron density and temperature for the whole sample, allowing for accurate determinations of N/O and the metallicity. We compare our results with an additional sample of dwarf star-forming galaxies and extragalactic H II regions. We also analyze the N/O ratio with the stellar mass and star formation rate.

Keywords: Galaxy spectroscopy, Dwarf galaxies, Emission line galaxies, Galaxy chemical evolution
The Behavior of He-weak in the Far-UV-Paper I: HD 5737. The analysis of 28 spectra of the bright B6 He-weak star HD 5737 recorded by the SWP camera on board the International Ultraviolet Explorer reveals one instance of marginal variation of the far-ultraviolet flux of this star from 1300 up to 1700 Å. All the other large aperture spectra show a remarkably constant spectral energy distribution. Over the 6 yr of the IUE mission, HD 5737 has experienced at least two episodes of very strong absorption in the C IV resonance lines at 1548.19 and 1550.77 Å,

Keywords: Helium-weak stars, Chemically peculiar stars
Multi-band Tractor Forced Photometry and Redshifts in the CDFS and XMM-LSS Fields. We present a catalog of multi-band forced photometry in the CDFS and XMM-LSS fields. We used The Tractor image-modeling software to produce de-blended photometry across 13 to 15 optical/infrared bands and determine photometric redshifts. Our catalog, which is publicly available on IRSA, contains ~1.5 million sources and covers a total area of ~9 deg2.

Keywords: Surveys, Extragalactic astronomy, Multi-color photometry
Re-evaluation of Cosmogenic <SUP>10</SUP>Be Dating of the Ferromanganese Crust VA13/2 Archiving Interstellar Radionuclides on Earth. Interstellar radionuclides, such as 60Fe, are produced in massive stars, ejected by supernovae and can be recovered in geological archives on Earth. Ferromanganese encrustations on the bottom of Earth's major oceans represent one important geological archive with a time-record of interstellar radionuclides. The paper of Segl et al. provided the first cosmogenic 10Be dating of the ferromanganese crust VA13/2 in which interstellar 60Fe was discovered. After re-evaluation and comparison with other published and recently acquired data of the same crust, we conclude that the calculated 10Be/9Be data set is wrong by a factor of 9 due to a mathematical lapse. In addition, the ordinate of the corresponding 10Be/9Be graph is in discrepancy with the given data. The updated data set is now in agreement with recently published and acquired data.

Keywords: Cosmic ray nucleosynthesis
Mass and Color Dependence of the Hubble Spiral Sequence. In the classic Hubble spiral sequence, arm windiness correlates with bulge size; Sa type spiral galaxies with larger bulges also have the most tightly wound spirals. Exceptions to this have long been known, and in recent work using Galaxy Zoo morphologies no strong correlation was seen in a volume limited sample. In this Research Note, we explore the impact of galaxy mass and integrated color upon this correlation in the Galaxy Zoo sample, finding that bluer and lower mass spirals show the "expected" correlation; however, it becomes slightly negative for redder and/or more massive spiral galaxies.

Keywords: Spiral galaxies, Hubble classification scheme, Galaxy classification systems, Spiral arms, Spiral pitch angle