Sazuna/UAT_keywords huggingface dataset:
Characterization of the Visual Binary TOI-6883AB and its Dynamical Implications for the Planetary Companion TOI-6883Ab. We demonstrate that TOI-6883 is a physically bound visual binary system composed of two solar-type stars, TOI-6883A (TIC 393818343) and TOI-6883B (TIC 393818340), initially regarded as a single star hosting the exoplanet TOI-6883b. Gaia DR3 astrometry shows that both stars have nearly identical parallaxes (∼10.6 mas), consistent proper motions, and a projected separation of ∼616 au, confirming their binary nature. Using astrometric and photometric data, we estimate the stellar masses, physical separation, and an orbital period of ∼15,000 yr. The system is energetically bound. We revise the planet's designation to TOI-6883Ab to reflect stellar multiplicity. We evaluate the impact of the binary companion on planetary stability and find the planet's orbit to be long-term stable, although Kozai–Lidov perturbations remain possible. Further astrometric and photometric follow-up will be essential to better constrain the binary orbit and assess potential dynamical influences on the planetary architecture.

Keywords: Binary stars, Timing variation methods, Transit photometry, Astrometry, Proper motions, Exoplanet detection methods, Visual binary stars
Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXI. HD 53588. The weak line of Hg II located at 5677.10 Å is detected in SOPHIE spectra of the HgMn star HD 53588 as a feature absorbing about 2% of the continuum. The synthesis of this line yields a mercury abundance which agrees well with previous determinations. Abundances of helium, magnesium, silicon, phosphorus, titanium, chromium, manganese, iron and gallium are also measured from the synthesis of the several spectral intervals. The Transiting Exoplanet Survey Satellite lightcurves of HD 53588 show a periodic variability. The Lomb Scargle algorithm provided on-line by MAST yields a main period of 2.325 days which could be the rotational period. Two other periods at 2.030 and 2.700 days, which have less power, may exist too.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Hidden Companions to Intermediate-mass Stars. XXVIII. Uncovering a 0.62 M<SUB>⊙</SUB>, 0.18 au Companion to Lambda Aquilae. Lambda Aquilae (λ Aql) is a nearby late B-type star with somewhat contradictory evidence of being a binary system. Here we report on a VLTI/GRAVITY interferometric observation in which we directly detected a close companion with a K band flux ratio of 2.206% at projected separation ρ = 4.72 mas ↔ 0.18 au. Isochrone fitting implies masses MA ≃ 3.0 M⊙ and MB ≃ 0.62M⊙ and an age of 90 Myr. The secondary can explain the X-ray emission of λ Aql. The primary should easily fill its Roche lobe in the red giant branch and trigger a common envelope event, which will most likely result in a merger. *Based on observations collected at the European Southern Observatory, Chile, Program ID 113.26GM.001.

Keywords: Optical interferometry, Multiple stars, B stars
Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XXII. HD 144206 (υ Her). The weak line of Hg II located at 5677.10 Å is detected in ELODIE spectra of the HgMn star HD 144206 as a feature absorbing about 2% of the continuum. The synthesis of this line yields a mercury abundance which is slightly larger than previous determinations. Line synthesis is used to measure the abundances of several elements. The following excesses/deficiencies are found: helium (‑1.00 dex), magnesium (‑0.47 dex), titanium (+0.91) , chromium (+0.54), manganese (+1.92), iron (‑0.71) , yttrium (+2.50), mercury (+4.97). A conservative uncertainty on the excesses/deficiencies is estimated to be ±0.10 dex. The recent Transiting Exoplanet Survey Satellite lightcurves of HD 144206 acquired in 2022 and 2024 show a complex pattern of variability but no clear periodicity.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Ending the Hubble Tension. If primordial black holes of mass 10‑19M⊙ formed in the early universe, their Hawking radiation would have delayed recombination and increased the cosmic microwave background Hubble Constant by 10%. The hypothesis that the ionization history of the universe is locked to the thermal history is too precarious an assumption to hang the expansion rate on. It is better to measure H0 at z &lt; 1.

Keywords: Cosmology, Primordial black holes, Recombination (cosmology)
Spurious Oscillatory Signal in Kepler Eclipsing Binary Light Curves. In our study of the O'Connell effect in Kepler eclipsing binaries, we found that some systems display a spurious oscillatory signal in their long-cadence light curves. This signal occurred in 12% of our sample of 258 systems. The cause of this signal is a resonance between the binary's orbital period and Kepler's integration time. We found that binaries that have an orbital period that is close to (within ∼1%) an integer multiple or a simple fraction of the effective long-cadence integration time of 1765.5 s displayed an oscillatory signal. In this note, we highlight this phenomenon due to its potential impact on research using Kepler data, especially the study of pulsating variable stars.

Keywords: Eclipsing binary stars, Light curves, Astronomy data analysis, Pulsating variable stars
Variability Census of Legacy Catalogs. V. 11,820+ New δ Scuti and γ Doradus Stars. This study identifies over 3335 new δ Scuti and 8496 new γ Doradus stars. These discoveries result from the fifth phase of a variability census of A-F stars selected from the legacy catalogs: PPM, HD, SAO, Bonner Durchmusterung, Córdoba Durchmusterung, and Southern Durchmusterung. Across all the five project phases, this comprehensive survey has analyzed TESS light curves for 193,940 A-F stars and identified over 14,510 δ Scuti, 18,382 γ Doradus, and 2354 eclipsing binaries (EBs), along with thousands of rotational variables. Notably, over 3900 of these variables exhibit hybrid δ Sct-γ Dor pulsations, and more than 360 EBs contain pulsating (δ Sct or γ Dor) primary components. Using TESS data, this work has revealed a significant population of previously undetected variable stars, essential for stellar and asteroseismic studies due to their relatively bright nature.

Keywords: Eclipsing binary stars, Gamma Doradus variable stars, Delta Scuti variable stars, Pulsating variable stars
Equivalent Width of the Interstellar Na I D<SUB>1</SUB> and D<SUB>2</SUB> Absorption Lines for Stars with E(B ‑ V) &lt; 0.15. New measurements of the equivalent width of the interstellar Na I D1 and D2 absorption lines for 62 bright B-type stars with E(B ‑ V) &lt; 0.15 are used to recalibrate the relation between these quantities in this low-reddening regime, and to quantify the scatter around this relation. Stars showing multiple components in their interstellar Na I lines clearly show a larger total equivalent width at the same E(B ‑ V) than stars with a single interstellar Na I absorption lines. Semi-empirical relations are derived that allow for the reddening toward stars showing single interstellar Na I absorption lines to be estimated. Previous calibrations of this relation are typically found to underestimate E(B ‑ V) for these stars.

Keywords: Interstellar line absorption, Interstellar reddening, Interstellar extinction
Temporal Changes in High-velocity Gas Associated with the Monoceros Loop SNR. We present observations of interstellar Na I and Ca II absorption lines toward HD 47240, which probes shocked gas in the Monoceros Loop supernova remnant. The observations were obtained at five different epochs spanning the time period from 2017 January to 2024 September. Time variable Na I and Ca II absorption is observed in two high-velocity components at +63 and +73 km s‑1. These are the same high-velocity features discussed by C. Dirks &amp; D. M. Meyer, who found significant variations in Na I column densities between 2006 January and 2014 January. We discuss our new observations of temporal variability in the context of these and other previous observations of the high-velocity gas toward HD 47240. We speculate that the column density variations are a result of small-scale structure in the post-shock flow passing in front of the background star.

Keywords: Interstellar dynamics, Interstellar atomic gas, Interstellar line absorption, Supernova remnants, Interstellar medium
Identification of a Possible Supernova Remnant in Pegasus. The census of galactic supernova remnants (SNRs) is largely incomplete due to the intrinsic short duration of these structures and to the low luminosity of the oldest ones. We investigated by ultra-deep narrow-band imaging a particular nebular filament easily detectable in wide-field photos. The presence of weak emission in [O III] and the presence of two pulsars nearby, suggests that it could be an ancient SNR at the galactic coordinates G82.9–29.2, to be confirmed with new follow-up observations.

Keywords: Supernova remnants
Limits to Star Formation in Post Starburst Galaxies from Type II Supernovae. We establish significant upper limits to the current star formation rate in two samples of post starburst galaxies by measuring the rate of Type II supernovae from the Zwicky Transient Factory Bright Transient Survey. No Type II supernovae are observed within the Petrosian radii of z &lt; 0.05 post starburst galaxies during this supernova search survey. We calculate that at 95% confidence level the star formation rate in these galaxies is &lt;0.8 M⊙ yr‑1.

Keywords: Type II supernovae, Post-starburst galaxies
Discovery of 12 New Orbital Periods for Classical Novae. I report newly discovered orbital periods for 12 classical novae, based on recent light curves from the TESS satellite. These are 0.61975 for V679 Car, 0.17317 for BC Cas, 0.14812 for V842 Cen, 1.66971 for DE Cir, 0.10180 for V476 Cyg, 0.10665 for V2468 Cyg, 0.11570 for DM Gem, 0.56498 for V2944 Oph, 0.61378 for BS Sgr, 0.17978 for V732 Sgr, 0.17016 for V4092 Sgr, and 0.15616 for V5668 Sgr, all in units of days. The folded light curves for V679 Car, DE Cir, DM Gem, BS Sgr, and V732 Sgr show eclipses. V679 Car and V842 Cen both show a handful of intermittent periodic signals, but only the given orbital periodicities are coherent and steady throughout the 4–6 yr of data. This brings my total to 66 nova orbital periods that I have discovered.

Keywords: Classical novae
Carbon Monoxide Emission from the 1998 Outburst of the Recurrent Nova V2487 Ophiuchi. Infrared spectral observations from 2.3 to 2.48 μm from the 1998 outburst of V2487 Ophiuchi (Nova Oph 1998) show the presence of carbon monoxide emission from both 12CO and 13CO four days after discovery and five days after peak brightness. This makes V2487 Oph only the second recurrent novae to have detected CO emission (after V745 Sco) and the first without a giant as the secondary component. The CO emission was short-lived, disappearing from the spectrum three days after detection.

Keywords: Recurrent novae
Crossmatching the TESS Eclipsing Binary Catalog with Kepler. The Transiting Exoplanet Survey Satellite (TESS) is at the forefront of the eclipsing binary (EB) cataloging effort, with a list of TESS observed EBs exceeding 4500 entries. We cross-match Villanova's TESS EB catalog with the Kepler EB catalog. By matching Kepler IDs to TESS IDs, we determine if they were observed in 2 minutes cadence by TESS and if they exist in the TESS EB catalog. We found 21 missing EBs observed within the first 2 yr of observation (Sectors 1–26). We then run diagnostic validation tests on the missing targets, matching threshold crossing event data to confirm their EB designation. The targets are also manually vetted to assess the likelihood of false positives. This process enables the increased completeness of the TESS catalog and the process can be applied to other EB catalogs, such as Optical Gravity Lensing Experiment and All Sky Automated Survey.

Keywords: Eclipsing binary stars, Cross-validation , Catalogs
Measurements of Jupiter's Gravitational Deflections Using Galilean Moons. General Relativity predicts that light from a star is deflected by 0 ″. 0163 during a close conjunction with Jupiter. Using the Galilean moons as targets presents a similar observing opportunity. Data was recently collected over different nights by different observers, recording images over several hours. Small telescopes used with a methane filter allowed target measurements close to Jupiter's limb. The data analysis extracted the moon positions from thousands of images followed by averaging the values in 30 minutes intervals. The final result had too much noise to confirm a gravitational deflection.

Keywords: General relativity
Stereo-imaging of Martian Dust Plumes by Multiple Coordinated Spacecraft. Atmospheric dust plumes on Mars can rise to very high altitudes, and the resulting injection of dust into the atmosphere has a variety of impacts, including on water loss rates. Observing the time evolution of such plumes would therefore bear on key processes on Mars. As shown here, repeat imaging by coordinated spacecraft even with modest resolution could reveal that time evolution.

Keywords: Mars, Atmospheric dynamics
Seeing-correlated Variability in ZTF Light Curves. We report on spurious quasi-periodic variability detected in high-cadence Zwicky Transient Facility (ZTF) Data Release 23 light curves from Field 840, observed on the night of 2024 January 9. The apparent flux variations correlate strongly with the seeing full width at half maximum. This effect can occur even in galaxies that appear point-like at ZTF resolution, making them difficult to distinguish from true astrophysical variability. This highlights the importance of careful inspection of image metadata when interpreting short-term variability in time-domain surveys.

Keywords: Supernovae, Transient detection, Time domain astronomy, Time series analysis
Avoiding (photo-z) Catastrophe. Spectral modeling codes that estimate photometric redshifts (photo-z) are a powerful and often reliable method for determining redshifts of galaxies. However, there are notable instances where degeneracies in spectral energy distribution (SED) colors lead to "catastrophic" failures. We highlight the case of COSBO-7, a dusty, intermediate-z galaxy that masqueraded as a high-z source, because it demonstrates a unique scenario where photo-z codes run into issues despite extensive multi-wavelength photometry. We advocate that photo-z fitting should aim to: (1) use the entire available SED (UV–radio) whenever possible to help break color degeneracies, (2) allow flexible dust attenuation prescriptions, both in terms of the attenuation curve slope and a varying 2175 Å absorption feature, and (3) implement uncertainty floors to account for limitations in spectral models and also on the photometry itself.

Keywords: Astronomy data analysis, Interstellar dust extinction, Spectral energy distribution, High-redshift galaxies, Galaxies
The Effect of Photometric Errors on the Measured Width of the Main Sequence in Star Clusters. This note deals with the effect of errors in the B and V magnitudes, or measurements in any other color system, on the width of the main sequence (MS) in a color–magnitude (Hertzsprung–Russell) diagram. The width is defined as the dispersion in apparent (or absolute) magnitude at a fixed, measured photometric color. I find that the dispersion is larger than might be thought a priori. A statistical analysis is presented which demonstrates that the error in the magnitude residual from a linear approximation to the MS is Gaussian, but with a standard deviation which is much larger, in general, than the errors in the individual B and V magnitudes. This result is confirmed by a Monte Carlo simulation of a MS population with specified errors in B and V magnitudes.

Keywords: Open star clusters, Solar analogs
Spectroscopic Observations of Eleven Cataclysmic Variable Candidates Using the Liverpool Telescope. This paper presents spectroscopic observations of eleven candidate cataclysmic variables (CVs). Observations of the candidates were performed using the Liverpool Telescope and the SPRAT spectrograph, following initial identification from the Gaia Alerts Index. Through line identification, with supporting evidence from Gaia light curves, nine out of the eleven targets show emission features consistent with that of CVs, leading to their classifications as CVs. No obvious emission features are identified in the remaining two, meaning further observations are required for classification.

Keywords: Binary stars, Interacting binary stars, Dwarf novae, Semi-detached binary stars, Stellar accretion disks, Cataclysmic variable stars
Roche-lobe Overflow Ejecta Cannot Explain Carbon Enhancement of GDR3-0928. Carbon Enhanced Metal-Poor (CEMP) stars offer critical insights into the chemical processes of the early universe. Their formation has been attributed to either global enrichment events, like explosions of Population III stars, or local enrichment processes involving close binary interactions. A recently discovered CEMP-r star, GDR3-0928, has a highly carbon-enhanced composition in a dwarf galaxy where other stars are largely unaffected by carbon pollution, likely requiring a local carbon enrichment event. Here we investigate a new local mechanism in which Roche-lobe overflow (RLOF) ejecta from a massive star pollutes a distant third star. We find that reasonable wind velocities, densities, and accretion durations produce accreted masses that are several orders of magnitudes too low to form a CEMP star. These results show that RLOF ejecta alone cannot explain the carbon enhancement observed in GDR3-0928.

Keywords: CEMP stars, Dwarf galaxies, Roche lobe overflow
An Outer-disk SX Phe Variable Star in Rubin Data Preview 1. We report the discovery of an SX Phoenicis-type pulsating variable star via 217 epochs of time-series photometry from the Vera C. Rubin Observatory's Data Preview 1. The star, designated LSST-DP1-O-614435753623041404 (or LSST-C25_var1 for short), has mean magnitudes of (&lt;g&gt;, &lt;r&gt;) = (18.65, 18.63), with pulsation amplitudes of (0.60, 0.38) mag in these bands. Its period is 0.0767day (1.841 hr), typical of SX Phe pulsators. We derive a distance to the star of 16.6 kpc based on an SX Phe period–luminosity relation. Its position ∼5 kpc from the Galactic plane, in the outer Milky Way disk at a Galactocentric distance of ∼22 kpc, and its proper motion suggest that LSST-C25_var1 is part of the Monoceros Ring structure. This star is presented as a small taste of the many thousands of variable stars expected in Rubin/Legacy Survey of Space and Time data.

Keywords: Light curves, Sky surveys, SX Phoenicis variable stars, Pulsating variable stars
New Molecular Dynamics Methods for Simulating Neutron Star Crusts with Superfluid Vortices. Superfluid vortices in neutron star crusts are thought to be pinned to the lattice of nuclei in the crust. The unpinning of superfluid vortices in spin glitches therefore motivates us to study the vortex-crust interaction explicitly with molecular dynamics. In this work, we present a new molecular dynamics methods to characterize the response of the crust to a rigid vortex. When vortex pinning forces and nearest neighbor Coulomb forces are comparable, we observe a qualitatively new phenomena of lattice entrainment with implications for the elastic evolution of the crust.

Keywords: Neutron stars, Stellar interiors, Plasma physics, Computational methods, N-body simulations
2025 FP4: A New Transient Co-orbital Asteroid of Earth. We report the identification of 2025 FP4, a new co-orbital asteroid of Earth currently in a retrograde satellite orbit. It is expected to remain in this configuration for ∼500 yr and as a co-orbital for 6000 ± 1000 yr. Despite the potential for close planetary encounters, its small size suggests it poses minimal threat.

Keywords: Celestial mechanics, Asteroids, Earth (planet)
X-Ray versus Optical Line Emission: Searching for Highly Obscured AGN in the J1030 Field. In this research note, we consider a sample of 34 X-ray-selected active galactic nucleus (AGN) in the 500 ks Chandra/ACIS-I observation of the J1030+0524 field, which were identified through optical spectroscopy. The targets span a redshift range z ∼ 0.1─1.5 and feature detection of [O III]λ5007, [Ne V]λ3426, or both. We investigated the ratio between their absorption-corrected 2─10 keV luminosity, as derived from X-ray spectroscopy, versus [O III] and/or [Ne V] luminosity, and compared our measurements with literature results. Most targets align with the X-ray versus line luminosity relations in the literature, with a notable exception: the type 2 AGN XID 361 at z = 0.83 is significantly less luminous in the X-rays than what would be expected from its high-ionization lines, calling for heavy, Compton-thick absorption that was overlooked through X-ray spectroscopy.

Keywords: Active galaxies, X-ray active galactic nuclei, Galaxy evolution
A Catalog of Post-starburst Galaxies from DESI. Post-starburst galaxies are galaxies that are no longer producing stars and have entered or are entering quiescence. These galaxies can be identified with spectral features, for which the Dark Energy Spectroscopic Instrument (DESI) data provides an opportunity to do so at a higher redshift range compared to previous work with SDSS. Within the DESI field, we have selected 62,808 quiescent galaxies that meet our SNR cut and then measured the Lick HδA index to find 367 recently quiescent galaxies. We have observed a higher rate of post-starburst galaxies at 0.49 &lt; z &lt; 1.39 selected using [O II] than z &lt; 0.49 selected using Hα.

Keywords: Galaxies, Quenched galaxies, E+A galaxies, Galaxy spectroscopy, Post-starburst galaxies
Old and Metal-rich G Stars. Planetary systems of very old G stars could provide meaningful comparisons with the solar system. They may even have provided environments with the potential to harbor early exobiology within the Galaxy. It is within these contexts that attention is drawn to a selection of G stars for which there are indications of ages and metallicities significantly greater than solar. A significant fraction of these stars have been included in radial velocity exoplanet searches. Six are known to host orbiting gas giant planets. All warrant further investigation for exoplanets.

Keywords: Stellar ages, Chemical abundances, G stars
The Far Ultraviolet Spectrum of the Newly Discovered HgMn Star HD 145842 (θ Nor). The high resolution far ultraviolet spectrum of HD 145842, a newly discovered HgMn star, is compared to that of the normal star HD 152614, which has similar effective temperature, surface gravity and projected equatorial velocity. The spectrum of HD 145842 shows stronger lines of gallium, in particular the resonance line at 1414.40 Å, and a weaker resonance line of Al II at 1670.79 Å. The line synthesis of gallium , aluminium, carbon and iron lines yields the following excesses/deficiencies: +1.70 dex for gallium, ‑0.70 dex for aluminium, ‑0.52 dex for carbon and +0.00 dex for iron. These are the first measurements of the abundances of gallium and aluminium in HD 145842. They confirm the HgMn status for this star. The most recent TESS lightcurves yield a short rotational period of HD 145842, Prot = 1.144 days, in agreement with previously published values.

Keywords: Mercury-manganese stars, Chemically peculiar stars