Sazuna/UAT_keywords huggingface dataset:
The Jets and the Neutron Star Kick Velocity of the Supernova Remnant CTB 1. We identify jet-shaped morphology in the core-collapse supernova remnant (SNR) CTB 1 that includes two opposite structural features. We identify these as the imprints of a pair of jets that were among the last jets to explode the massive stellar progenitor of CTB 1. We find the projected angle between the jets' axis and the direction of the pulsar velocity, which is the neutron star natal kick, to be α = 78°. We tentatively identify possible signatures of a second pair of opposite jets along a different direction. If this identification holds, SNR CTB 1 has a point-symmetric structure. The morphology and large angle of the jets' axis to kick velocity are expected in the jittering jets explosion mechanism of core-collapse supernovae.

Keywords: Supernova remnants, Neutron stars, Stellar jets, Core-collapse supernovae
Fifteen Hypervelocity Stars Whose Gaia G Magnitudes are Less Than 16.0 and Radial Velocities Less Than-600 km per second. From Gaia DR3 data using a simple search criteria fifteen hypervelocity stars (HVS) are detected. These stars have radial velocities less than -600 km s-1, Gaia G magnitudes less than 16.0 and Renormalized Unit Weight Error values less than 1.4. The U, V, W velocities also indicate that these stars are HVS. The effective temperatures of these stars indicate that they are F and G type stars. Gaia DR3 409420157955913856 and Gaia DR3 2198292118993038464 seems to be metal-poor HVS. High resolution spectroscopy of these stars is needed to derive the atmospheric parameters, chemical composition and to understand their evolutionary status and origin. The progenitors of these stars may be close binary systems with white dwarf companions. When the white dwarf companions became Type Ia supernovae and their F-G companion stars have become HVS. Or they may be the result of other unknown processes.

Keywords: Hypervelocity stars
Gnuastro: Estimating the Zero-point Magnitude in Astronomical Imaging. Calibration of pixel values is a fundamental step for accurate measurements in astronomical imaging. In astronomical jargon this is known as estimating zero-point magnitude. Here, we introduce a newly added script in GNU Astronomy Utilities (Gnuastro) version 0.20 for the zero-point magnitude estimation, named: astscript-zero-point. The script offers numerous features, such as the flexibility to use either image(s) or a catalog as the reference data set. Additionally, steps are parallelized to enhance efficiency for big data. Thanks to Gnuastro's minimal dependencies, the script is both flexible and portable. The figures of this research note are reproducible with Maneage, on the Git commit e31dd15.

Keywords: Astronomical techniques, Open source software, Astronomy software, Flux calibration
Cometary Activity Discovered on Vacationing Centaur 2019 OE31. We have detected cometary activity on minor planet 2019 OE31 through both the Active Asteroids Citizen Science program and an independent archival search. Before 2013, 2019 OE31 was on a Centaur orbit, between the orbits of Jupiter and Neptune. Centaurs are objects in transition from the outer solar system to the inner solar system. They play a vital role in the understanding of the Kuiper Belt and comets. In 2013 October, following a close encounter with Jupiter, 2019 OE31 moved to an orbit entirely interior to that of Jupiter. This reduced orbital distance and, hence, increased temperature is likely the cause of the observed activity. Through a suite of orbital dynamics simulations, we find that 2019 OE31 will experience many more similar encounters and is statistically likely to return to a Centaur orbit, potentially within the next 80 yr, from its current "vacation."

Keywords: Comet tails, Centaur group, Comet dynamics, Asteroids
WRAP: A Tool for Efficient Cross-Identification of Proper Motion Objects Spanning Multiple Surveys. We introduce the Wide-field Retrieval of Astrodata Program (WRAP), a tool created to aid astronomers in gathering photometric and astrometric data for point sources that may confuse simple cross-matching algorithms because of their faintness or motion. WRAP allows astronomers to correctly cross-identify objects with proper motion across multiple surveys by wedding the catalog data with its underlying images, thus providing visual confirmation of cross-associations in real time. Developed within the Backyard Worlds: Planet 9 citizen science project, WRAP aims to aid in the characterization of faint, high motion sources by this collaboration (and others).

Keywords: Direct imaging, Catalogs
The Importance of Neural Network Hyperparameters in Determining Age Inference Quality. To estimate precise ages for large samples across the galaxy, it has become common to train machine learning models on smaller, well-characterized samples of stars and then apply them to larger samples. As part of an undergraduate course, we used this technique to train a simple neural network with varying nodes and layers using ~11,800 ages from the upcoming APOGEE-Kepler-3 sample of stars. We find that the fraction of stars in the testing sample whose ages are recovered to better than 30% is only weakly correlated with these hyperparameters so long as the network is well fit. However, we note that it is sensitive to the chosen training sample, and that the network is susceptible to overfitting, which tends to lead to less accurate ages, particularly for the youngest and oldest stars in the sample. We provide the Jupyter notebook for this project for others wishing to do similar exercises.

Keywords: Galactic archaeology, Red giant stars, Neural networks
Discovery of an Emission Nebula in Direction of γ Aql. An emission nebula has been discovered in close apparent proximity to γ Aql (aka Tarazed). The diameter of the nebula is about $27\buildrel{\,\prime}\over{.} 4$ and its center is about $7^{\prime} $ away from γ Aql, which is known to be an X-ray source. However, γ Aql is most likely not the ionization source of the nebula. To my knowledge, this emission nebula has not been previously reported in the literature or on the Internet.

Keywords: Emission nebulae, H II regions, Interstellar medium, Nebulae
The Global 2:1 Mean-motion Resonance in HD 110067 is Not Vacant!. Extensive modeling of observations obtained by two space telescopes and 14 ground-based observatories revealed the presence of at least six closely packed planets orbiting HD 110067. Their orbital periods form a nearly perfect resonant chain, in which adjacent periods are in a geometric sequence with a ratio of r = 3/2 (planets b to e) that switches to r = 4/3 (planets e to g). The latter part of the sequence is based on single transits of planets f and g and their periods are model-dependent, as only first-order mean-motion resonances (MMRs) were so far investigated; and there is no physical justification for this assumption besides the simplicity imprinted on to the resonant chain itself. Furthermore, the global 2:1 MMR is apparently occupied, whereas this orbit is vacant in all other multibody (extra) solar systems. We summarize the physical arguments for/against the above r = 4/3 period ratios in anticipation of future observations to resolve the issue.

Keywords: Exoplanet dynamics, Tidal interaction, Orbital resonances, Exoplanets
Synthesis of the 4400-4600 Å Spectral Range for the A2.5V star HD 176687 (ζ Sagitarii A). The synthesis of a high resolution high signal-to-noise spectrum of HD 176687 from 4400 to 4600 Å allows the determination of LTE abundances for magnesium, calcium, scandium, titanium, chromium, iron, nickel and barium. This A2.5V star has recently been found to be the most massive star in a triple system. Magnesium and calcium are found to have a solar abundance. Scandium and titanium are depleted by a factor of 0.50, chromium, nickel by a factor of 0.70 and iron by 0.60 compared to their respective solar abundances. Barium is overabundant by a factor of 7.50. The found abundances fit well within the abundance pattern previously found for a few normal A stars. There is no sign of the recently discovered companion to HD 176687 in the spectrum analyzed.

Keywords: A stars
The Late-Epoch, Matter-Bounded Spectrum of the Nova V1405 Cassiopeiae. Optical and near-infrared spectra of the classical nova V1405 Cassiopeiae (V1405 Cas) from more than two years after outburst show a still bright nova of intermediate excitation with coronal lines, some high-ionization but non-coronal forbidden lines, and very strong emission features of He II. However, the common nebular lines of [N II], [O II], and [O III] are absent and the lines of He I are very weak. Analysis with the photoionization code CLOUDY indicates a emission line region that is sharply matter-bounded, truncating before the gas excitation drops sufficiently to support the parent ions of lower excitation lines.

Keywords: Classical novae
Baked before Breaking into Bits: Evidence for Atira-type Asteroid Splits. Current near-Earth asteroid orbital models cannot reproduce the observed populations close to the Sun. Supercatastrophic and tidal disruptions may explain the differences between theoretical models and observational data. Here, we explore the distributions of mutual nodal distances and the angular separation of perihelia of the known Atiras looking for evidence of past splittings. We find a number of pairs, trios, and one quartet of Atiras with mutual nodal distances as short as 0.001 au at the orbits of Mercury and Venus. The smallest of these highly correlated objects is 2023 WK3. Fragmentation or binary disruption may have triggered the recent formation of the unusual pair made of 594913 'Ayló'chaxnim (2020 AV2) and 2012 VE46 with both mutual nodal distance and angular separation of perihelia in the first percentile of the distribution, making 2012 VE46 a robust candidate to being a former moon or piece of 'Ayló'chaxnim.

Keywords: Near-Earth objects
Mars-Crossing Minor Planet 2018 VL10: a Jupiter-family Comet Discovery via Citizen Science. We announce the discovery of cometary activity emitting from minor planet 2018 VL10 in Dark Energy Camera images spanning from UT 2018 December 31 to UT 2019 March 3. The activity was identified by volunteers of our NASA Partner program Active Asteroids, a Zooniverse-hosted Citizen Science project designed to find previously unknown activity in known minor planets. Notably, 2018 VL10 crosses the orbits of Mars and Jupiter, and experiences close approaches of less than 0.5 au with both Earth and Jupiter. We classify 2018 VL10 as a member of the Jupiter-family comets, a group of objects especially important to understand because they hold important clues about the solar system volatile distribution, past and present.

Keywords: Comet tails, Short period comets, Comet dynamics, Asteroids
Distance to Leo A Based on a Post-asymptotic-giant-branch Star. A yellow post-asymptotic-giant-branch (PAGB) star was recently identified in the dwarf galaxy Leo A. Using this yellow PAGB star, I derived a distance of 794.3 ± 10.0 kpc to Leo A, illustrating the yellow PAGB star can be used as a distance indicator.

Keywords: Dwarf galaxies, Post-asymptotic giant branch stars, Stellar distance, Distance indicators
Comparison between Analytical and Numerical Results for Twisted Magnetosphere of Magnetars. The analytical calculations for twisted magnetosphere of magnetars are compared with recent numerical simulations. A larger polar cap, a smaller magnetospheric opening radius in previous analytical modelings are confirmed by the numerical simulations. In the case of magnetars, the particle outflow luminosity in the open field line regions may be powered by the magnetic energy.

Keywords: Magnetars
A Fully Explicit Integrator for Modeling Astrophysical Reactive Flows. Simulating complex astrophysical reacting flows is computationally expensive-reactions are stiff and typically require implicit integration methods. The reaction update is often the most expensive part of a simulation, which motivates the exploration of more economical methods. In this research note, we investigate how the explicit Runge-Kutta-Chebyshev (RKC) method performs compared to an implicit method when applied to astrophysical reactive flows. These integrators are applied to simulations of X-ray bursts arising from unstable thermonuclear burning of accreted fuel on the surface of neutron stars. We show that the RKC method performs with similar accuracy to our traditional implicit integrator, but is more computationally efficient when run on CPUs.

Keywords: Hydrodynamical simulations, Open source software, Hydrodynamics, Computational methods, GPU computing, X-ray bursts
CO and Atomic Line Emission from the Young Stellar Object V1331 Cygni. The infrared spectrum of the young disk star V1331 Cygni shows rare atomic emission lines from several species including C I, O I, Na I, Mg I, Al I, Si I, Ca I, Fe I, and probably S I. The presence of H I emission but the absence of N I recombination lines indicates excitation by a comparatively cool source unable to ionize nitrogen. Measurements of both the fundamental and first overtone emission of carbon monoxide indicate a hot (T ≈ 3000 K), optically thick (optical depth ≈100 in the strongest transitions of the fundamental) for the molecular gas.

Keywords: Young stellar objects
Solar Cycle Observations. We describe the defining observations of the solar cycle that provide constraints for the dynamo processes operating within the Sun. Specifically, we report on the following topics: historical sunspot numbers and revisions; active region (AR) flux ranges and lifetimes; bipolar magnetic region tilt angles; Hale and Joy's law; the impact of rogue ARs on cycle progression and the amplitude of the following cycle; the spatio-temporal emergence of ARs that creates the butterfly diagram; polar fields; large-scale flows including zonal, meridional, and AR in-flows; short-term cycle variability; and helioseismic results including mode parameter changes.

Keywords: Solar cycle, Sunspots, Helioseismology, Solar dynamo
OSIRIS-REx Derived Thermal Data Products Bundle V1.0. This bundle collects the derived thermal data products produced by the OSIRIS-REx Thermal Working Group (TAWG). Derived prodcuts include (101955) Bennu global and sample site specific thermal inertia maps, and global predicted temperature maps.

Keywords: Near-Earth objects, Asteroids
A Blind Search for Transit Depth Variability with TESS. The phenomenon of transit depth variability offers a pathway through which processes such as exoplanet atmospheric activity and orbital dynamics can be studied. In this work we conduct a blind search for transit depth variations among 330 known planets observed by the Transiting Exoplanet Survey Satellite within its first four years of operation. Through an automated periodogram analysis, we identify four targets (KELT-8b, HAT-P-7b, HIP 65 Ab, and TrES-3b) that appear to show significant transit depth variability. We find that KELT-8b's transit depth variability likely comes from contaminating flux from a nearby star, while the apparent variabilities of HIP 65 Ab and TrES-3b are probable artifacts due to their grazing orbits. HAT-P-7b indicates signs of variability that possibly originate from the planet or its host star. A population-level analysis does not reveal any significant correlation between transit depth variability and the effective temperature and mass of the host star; such correlation could arise if stellar activity was the cause of depth variations via the transit light source effect. Extrapolating our ~1% detection rate to the upcoming Roman mission, predicted to yield of order 100,000 transiting planets, we expect that ~1000 of these targets will be found to exhibit significant transit depth variability.

Keywords: Catalogs, Transit photometry, Exoplanets
Low-frequency Radio Recombination Lines Away from the Inner Galactic Plane. Diffuse radio recombination lines (RRLs) in the Galaxy are possible foregrounds for redshifted 21 cm experiments. We use EDGES drift scans centered at -26.°7 decl. to characterize diffuse RRLs across the southern sky. We find that RRLs averaged over the large antenna beam (72° × 110°) reach minimum amplitudes of R.A. = 2-6 hr. In this region, the Cα absorption amplitude is 33 ± 11 mK (1σ) averaged over 50-87 MHz (27 ≳ z ≳ 15 for the 21 cm line) and increases strongly as frequency decreases. Cβ and Hα lines are consistent with no detection with amplitudes of 13 ± 14 and 12 ± 10 mK (1σ), respectively. At 108-124.5 MHz (z ≈ 11) in the same region, we find no evidence for carbon or hydrogen lines at the noise level of 3.4 mK (1σ). Conservatively assuming that observed lines come broadly from the diffuse interstellar medium, as opposed to a few compact regions, these amplitudes provide upper limits on the intrinsic diffuse lines. The observations support expectations that Galactic RRLs can be neglected as significant foregrounds for a large region of sky until redshifted 21 cm experiments, particularly those targeting cosmic dawn, move beyond the detection phase. We fit models of the spectral dependence of the lines averaged over the large beam of EDGES, which may contain multiple line sources with possible line blending, and find that including degrees of freedom for expected smooth, frequency-dependent deviations from local thermodynamic equilibrium (LTE) is preferred over simple LTE assumptions for Cα and Hα lines. For Cα we estimate departure coefficients 0.79 &lt; b  n  β  n  &lt; 4.5 along the inner Galactic plane and 0 &lt; b  n  β  n  &lt; 2.3 away from the inner Galactic plane.

Keywords: Radio spectroscopy, Reionization, Milky Way Galaxy, Interstellar medium
Chemical Homogeneity of Wide Binary Systems: An Approach from Near-Infrared Spectroscopy. Wide binaries, with separations between the two stars from a few au to more than several thousand au, are valuable objects for various research topics in Galactic astronomy. As the number of newly reported wide binaries continues to increase, studying the chemical abundances of their component stars becomes more important. We conducted high-resolution near-infrared (NIR) spectroscopy for six pairs of wide binary candidates using the Immersion Grating Infrared Spectrometer at the Gemini-South telescope. One pair was excluded from the sample due to a significant difference in radial velocity between its component stars, while the remaining five pairs exhibited homogeneous properties in 3D motion and chemical composition among the pair stars. The differences in [Fe/H] ranged from 0.00 to 0.07 dex for these wide binary pairs. The abundance differences between components are comparable to the previous results from optical spectroscopy for other samples. In addition, when combining our data with literature data, it appears that the variation of abundance differences increases in wide binaries with larger separations. However, SVO 2324 and SVO 3206 showed minimal differences in most elements despite their large separation, supporting the concept of multiple formation mechanisms depending on each wide binary. This study is the first approach to the chemical properties of wide binaries based on NIR spectroscopy. Our results further highlight that NIR spectroscopy is an effective tool for stellar chemical studies based on equivalent measurements of chemical abundances from the two stars in each wide binary system.

Keywords: High resolution spectroscopy, Stellar abundances, Chemical abundances, Wide binary stars, Near infrared astronomy
TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf. We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0-dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6 m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet (ρ = 0.80 ${}_{-0.15}^{+0.17}$ g cm-3) with a planetary radius of 9.7 ± 0.5 R ⊕ (0.87 ± 0.04 R Jup) and a planetary mass of ${135}_{-18}^{+17}\ {M}_{\oplus }$ (0.42 ${}_{-0.06}^{+0.05}\ {M}_{\mathrm{Jup}}$ ). It has an orbital period of ${3.792622}_{-0.000010}^{+0.000010}$ days and an orbital eccentricity of ${0.06}_{-0.04}^{+0.07}$ . We measure a high metallicity for TOI-5344 of [Fe/H] = 0.48 ± 0.12, where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of nongiants (≲8 R ⊕). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats.

Keywords: M dwarf stars, Extrasolar gaseous giant planets, Exoplanet systems
JWST/NIRSpec Observations of the Coldest Known Brown Dwarf. We present 1-5 μm spectroscopy of the coldest known brown dwarf, WISE J085510.83-071442.5 (WISE 0855), performed with the Near-Infrared Spectrograph (NIRSpec) on board the James Webb Space Telescope (JWST). NIRSpec has dramatically improved the measurement of the spectral energy distribution (SED) of WISE 0855 in terms of wavelength coverage, signal-to-noise ratios, and spectral resolution. We have performed preliminary modeling of the NIRSpec data using the ATMO 2020 models of cloudless atmospheres, arriving at a best-fitting model that has T eff = 285 K. That temperature is ~20 K higher than the value derived by combining our luminosity estimate with evolutionary models (i.e., the radius in the model fit to the SED is somewhat smaller than expected from evolutionary models). Through comparisons to the model spectra, we detect absorption in the fundamental band of CO, which is consistent with an earlier detection in a ground-based spectrum and indicates the presence of vertical mixing. Although PH3 is expected in Y dwarfs that experience vertical mixing, it is not detected in WISE 0855. Previous ground-based M-band spectroscopy of WISE 0855 has been cited for evidence of H2O ice clouds, but we find that the NIRSpec data in that wavelength range are matched well by our cloudless model. Thus, clear evidence of H2O ice clouds in WISE 0855 has not been identified yet, but it may still be present in the NIRSpec data. The physical properties of WISE 0855, including the presence of H2O clouds, can be better constrained by more detailed fitting with both cloudless and cloudy models and the incorporation of unpublished 5-28 μm data from the Mid-infrared Instrument on JWST. *Based on observations made with the NASA/ESA/CSA James Webb Space Telescope.

Keywords: Brown dwarfs, Y dwarfs, Exoplanet atmospheres
Alpha Element Populations Among Local Halo Stars. Previous studies have shown that the halo of the Milky Way galaxy is made up of two distinct stellar populations, one from dissipative collapse and the other accreted. Elemental abundances with small relative uncertainties along with kinematics are determined for 20 local halo stars in the metallicity range -2.2 ≤ [Fe/H] ≤-1.2. Stars with metallicities [Fe/H] &gt; -1.75 show clear separation into high-α and low-α groups. New results extend the work of Nissen &amp; Schuster to the elements Co and K and to lower metallicities. The five program stars with [Fe/H] &lt; -1.75 appear to follow the low-α sequence and may be distinguishable by lower [Ba/Fe] abundances. The results for potassium help to clarify its behavior for -2.2 ≤ [Fe/H] ≤ -1.2 with [K/Fe] ~ 0.25 and approximately constant with [Fe/H]. Evidence is discussed regarding the cause of the low [α/Fe] abundances, i.e., whether a lower star-formation rate resulted in slower chemical evolution or if the initial mass function was deficient in high-mass stars. The low-α stars show larger dispersions in U and W velocities, as expected for an accreted population, but unlike Nissen &amp; Schuster we find that the high-α and low-α stars do not have significantly different net orbital rotation (V).

Keywords: Stellar abundances, Milky Way stellar halo, Population II stars