Sazuna/UAT_keywords huggingface dataset:
DRAGONS-A Quick Overview. Data Reduction for Astronomy from Gemini Observatory North and South (DRAGONS) is a platform for the reduction and processing of astronomical data. The Python-based, open-source package includes infrastructure for automation and algorithms for the processing of imaging and spectroscopic data, up to the analysis-ready stage. DRAGONS currently focuses on the reduction of Gemini data, although it allows for support of data from other instruments and telescopes through third-party extensions. Its latest release (v3.1) enables automated reduction of all currently active Gemini imaging facility instruments, as well as optical longslit spectroscopic data, acquired with GMOS.

Keywords: Astronomy data reduction, Astronomy software
Dataset of Classified Chandra Sources in Globular Clusters. We present a collection of classified X-ray sources in Globular Clusters (GCs) observed by the Chandra X-ray Observatory, including active binaries, cataclysmic variables, millisecond pulsars, and low-mass X-ray binaries. We cross-match the most accurate published positions from multiwavelength observations of these sources to the Chandra Source Catalog Release 2.1, and the HST UV Globular Cluster Survey to extract their multiwavelength properties. The data set can be accessed via an interactive website (https://home.gwu.edu/~kargaltsev/XCLASS_GC) and used as a training data set for machine-learning classification of unidentified X-ray sources in GCs.

Keywords: X-ray astronomy, Globular star clusters, Classification, HST photometry, Astronomy data visualization
A Pipeline for Modeling Rapidly Rotating Stars. Recent stellar intensity interferometry observations of stars at 416 nm complement Michelson interferometry observations in the near-infrared where stellar surface intensity gradients (e.g., limb darkening) are weaker. Intensity gradients due to gravity darkening in rapidly rotating stars are also expected to show higher contrast at 416 nm relative to the near-infrared. We have created a software pipeline to model stellar photospheres of rapidly rotating stars to compare predictions at these wavelength regions. The pipeline can produce model images, visibility predictions, and synthetic spectra. Here we show examples for the Be star β CMi, which has not been interferometrically imaged. We see higher contrast from gravity darkening at 416 nm in model images for rapid rotators, but only for those stars that are not viewed equator-on.

Keywords: Astronomy data modeling, Stellar photospheres, Long baseline interferometry, Stellar rotation, Gravity darkening
Using cGANs for Anomaly Detection: Identifying Astronomical Anomalies in JWST Imaging. We present a proof of concept for mining JWST imaging data for anomalous galaxy populations using a conditional Generative Adversarial Network (cGAN). We train our model to predict long wavelength NIRcam fluxes (LW: F277W, F356W, F444W between 2.4 and 5.0 μm) from short wavelength fluxes (SW: F115W, F150W, F200W between 0.6 and 2.3 μm) in ~2000 galaxies. We test the cGAN on a population of 37 Extremely Red Objects (EROs) discovered by the CEERS JWST Team. Despite their red long wavelength colors, the EROs have blue short wavelength colors (F150W - F200W ~ 0 mag) indicative of bimodal SEDs. Surprisingly, given their unusual SEDs, we find that the cGAN accurately predicts the LW NIRcam fluxes of the EROs. However, it fails to predict LW fluxes for other rare astronomical objects, such as a merger between two galaxies, suggesting that the cGAN can be used to detect some anomalies. (The source code and trained model (Pearce-Casey 2023) are available at https://github.com/RubyPC/Anomaly_Detection_with_cGANs.)

Keywords: Eros, Galaxy photometry, Galaxy mergers, Spectral energy distribution, Galaxies
Abundances of Heavy Elements in the B8 Mn Star HD 110073. The synthesis of several spectral intervals in the optical range allows the determination of LTE abundances of strontium, yttrium, zirconium, barium, praseodymium, neodymium, platinum and mercury for this B8 Mn star. Compared to the solar abundances, strontium, yttrium, barium, praseodymium and mercury are found to be overabundant by factors of 2.5, 130, 10, 150 and 60,000. Only upper limits could be determined for zirconium and platinum. The lines of Nd III are blended with lines of more abundant elements which precludes the determination of the abundance of neodymium. The abundance of manganese, derived from the Mn II line at 3986.59 Å is about 100 times larger than in the Sun.

Keywords: Mercury-manganese stars, Chemically peculiar stars
The Distribution of High-excitation OCS Emission Around the Cep A-East Protostellar Cluster. The Cepheus A East high-mass star-forming region has been mapped at 1.4 mm using the OCS(17-16) and (18-17) lines observed with the IRAM 30 m antenna. Contour maps and high-resolution line profiles reveal the association of OCS with both (i) the hot-core region, and (ii) with the NE, SE, and S outflows driven by the young stellar objects. This confirms that OCS is among the main S-molecules observed in the gas-phase after thermal evaporation due to protostellar heating or shocks due to propagation of protostellar jets. Adopting Local Thermodynamic Equilibrium conditions, optically thin emission, and a temperature of 100 K, the total OCS column density (after correction for beam dilution) of the hot-core component is ~1016 cm-2. For the outflow component, assuming a temperature range of 20-100 K, and extended emission, the OCS column density is ≤ 5 ×1014 cm-2 for a temperature ≥ 20 K.

Keywords: Interstellar molecules, Star forming regions, Astrochemistry
Anthropogenic Coal Ash as a Contaminant in a Micro-meteoritic Underwater Search. Chemical composition for spherules recovered from the search area of CNEOS 2014-01-08 in the Pacific Ocean has been recently released. A three-order of magnitude difference from CI-chondrites has been identified for elements beryllium, lanthanum and uranium in five samples. The lack of consensus regarding atmospheric survival and precision of path estimates motivate an examination of possible contaminants. Contents of nickel, beryllium, lanthanum and uranium are examined in the context of a known anthropogenic source of contamination, and found to be consistent with coal ash as suggested from a publicly available coal chemical composition database (COALQUAL). The meteoritic origin is disfavored.

Keywords: Interdisciplinary astronomy, Micrometeorites, Meteorite composition
Results of Polarimetric Observations of Near-Earth Asteroid 433 Eros. Near-Earth asteroids are of great importance for science. We present the results of polarimetric observations of near-Earth asteroid 433 Eros. Previous polarimetric observations of this asteroid did not cover a range of phase angles less than 9°. We were able to measure the degree of linear polarization of asteroid 433 Eros at a phase angle ≈4.°8. The data obtained made it possible to determine the parameters of the negative branch of the degree of linear polarization of this asteroid, such as the magnitude and position of the polarization minimum in four spectral ranges.

Keywords: Polarimetry, Asteroids
The Behavior of Bp HgMn Stars in the Far UV-Paper 28: HD 110073. The analysis of three spectra of the B8 Mn star HD 110073 recorded by the SWP camera on board the International Ultraviolet Explorer does not reveal any variations of the far ultraviolet spectral energy distribution shortwards of 1800 Å in spectra collected over 8 yr with identical exposure times. The Ga II line at 1414.40 Å is a prominent feature in the mean FUV spectrum of this star. The modeling of the optical line of Ga II at 6334.07 Å yields an overabundance of 1600 times the solar abundance, much lower than previous determinations. The projected rotational velocity ${v}_{{\rm{e}}}\sin \,i$ is close to 15 km s-1. The silicon abundance derived from the Si II line at 6347.10 Å is solar.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Custom JWST NIRSpec/IFU and MIRI/MRS Data Reduction Pipelines for Solar System Targets. We present custom JWST data reduction pipelines for JWST NIRSpec/IFU and MIRI/MRS observations of solar system objects. The pipelines simplify the process of reducing the JWST observations, and include custom steps to significantly improve the data quality. Our custom processing routines include a "desaturation" routine to reduce the effect of saturation while still maintaining high signal-to-noise ratio, and custom flat field correction code to remove the significant artifacts found in MIRI/MRS observations. The pipelines also automatically generate a series of quick look plots and animations to simplify exploration of a dataset. These custom JWST pipelines can be downloaded from https://github.com/JWSTGiantPlanets/pipelines.

Keywords: Astronomy image processing, Astronomy software, Astronomy data visualization, Astronomy data reduction
Spectral Background-subtracted Activity Maps. High-resolution solar spectroscopy provides a wealth of information from photospheric and chromospheric spectral lines. However, the volume of data easily exceeds hundreds of millions of spectra on a single observation day. Therefore, methods are needed to identify spectral signatures of interest in multidimensional data sets. Background-subtracted activity maps (BaSAMs) have previously been used to locate features of solar activity in time series of images and filtergrams. This research note shows how this method can be extended and adapted to spectral data.

Keywords: Solar physics, Spectroscopy, Solar chromosphere, Astronomical methods, Astronomy image processing
Hidden Companions to Intermediate-mass Stars. XI. Uncovering a 0.7 M <SUB>⊙</SUB>, 2.3 au Companion in the Astrometric Binary HIP 111200 = 58 Aquarii. We report on the direct VLTI/GRAVITY interferometric detection of a close companion in the nearby Hipparcos astrometric binary 58 Aquarii with a K band flux ratio of 5.0% at a projected separation 32 mas ↔ 2.3 au. Through isochrone fitting we find that the primary is a 1.4 Gyr old, 1.68 M ⊙ late A-type star and the companion is a 0.72 M ⊙ K-type star. The estimated cooling age of 900 Myr for the wide (9940 au), 0.70 M ⊙ white dwarf (WD) companion to the system is consistent with a progenitor star of 2.9 M ⊙ assuming single star evolution. The survival of the triple system at such large separation suggests a low kick in the formation of the WD or alternatively that it has since migrated outwards through three-body interaction. *Based on observations collected at the European Southern Observatory, Chile, Program ID 111.24UP.001.

Keywords: Optical interferometry, Multiple stars, A stars, White dwarf stars, Astrometric binary stars
Gaia Astrometry and MIKE+PFS Doppler Data Joint Analysis Reveals that HD 175167b is a Massive Cold Jupiter. HD 175167b is a cold (P  b  ~ 1200 days) Jupiter with a minimum mass of ${M}_{p}\,\sin \,i=7.8\pm 3.5\ {M}_{J}$ orbiting a Sun-like star, first discovered by the Magellan Planet Search Program based on MIKE observations. Through a joint analysis of the MIKE data and the Gaia two-body orbital solution, Winn found a companion mass of M  p  = 14.8 ± 1.8 M  J  and suggested that it might be better designated as a brown dwarf. Additional publicly available radial velocity data from Magellan/PFS better constrains the model, and reveals that the companion is a massive cold Jupiter with a mass of M  p  = 10.2 ± 0.4 M  J  and a period of P  b  = 1275.8 ± 0.4 days. The planet orbit is inclined by i = 38.°6 ± 1.°7 with an eccentricity of 0.529 ± 0.002.

Keywords: Radial velocity, Extrasolar gaseous giant planets, Astrometry
Identifying SuperWASP Detected Candidate Variables with TESS. Using Transiting Exoplanet Survey Satellite light curves, I have identified more than 1200 new pulsating variable stars from the SuperWASP-detected but unclassified candidate variables. These include a variety of types of pulsating variable stars, including 125 δ Scuti stars, 235 γ Doradus stars, 302 RR Lyrae stars, and 450+ Mira/SR/IR/LPV variables. I also identified 1300+ rotating variable stars. Additionally, I revealed that 16 of 91 newly identified eclipsing binary systems have pulsating components. These findings will help us to better understand the properties and evolution of pulsating variable stars. *Dedicated to my wife Jingyun Zhang.

Keywords: Delta Scuti variable stars, Pulsating variable stars, RR Lyrae variable stars, Mira variable stars, Eclipsing binary stars, Gamma Doradus variable stars
Constraints to Efficiently Find Interstellar Object Generated Craters on the Moon. Recent observations of interstellar objects (ISO) crossing the solar system suggest the possible existence of ISO-generated craters on the Moon. We explore how different crater properties such as age, size, melt, and position can be used to search for ISO-generated craters on the lunar surface. We find that selecting young, small craters with a high volume of melt located away from the lunar poles increases the likelihood of association with a high-speed ISO by 100 fold as compared to selecting randomly, assuming high-speed ISO impacts generate melt. We note that craters from other sources however still massively outnumber ISO-generated craters.

Keywords: Lunar craters, Interstellar objects
Optical Observations of the Type Ia Supernova 2022hrs. We present optical photometry and spectra of supernova (SN) 2022hrs (distance ~ 19 Mpc). It was classified as a Type Ia SN (SN Ia) based on its optical spectra, which exhibited high velocities in both Si II and Ca II absorption lines. The light curve of SN 2022hrs was typical of an SN Ia, with a peak magnitude of 13.01 ± 0.30 in B and a time interval of 14.5 days between detection and peak; its optical spectra are also normal. It is a standard SN Ia with no evidence of circumstellar material.

Keywords: Ejecta, Astronomical techniques, Type Ia supernovae, Astrometry, Photometry, Spectroscopy, Supernovae
Abundances of Light Elements in the B8 Mn Star HD 110073. The synthesis of spectral intervals in the optical range allows the determination of LTE abundances of several chemical elements lighter than titanium for HD 110073. Compared to the solar abundances, helium, magnesium, oxygen, aluminum, silicon and calcium are underabundant by factors of 0.4, 0.25, 0.90, 0.20, 0.85, 0.5 times the respective solar abundances. Carbon and sulfur have solar abundances. Phosphorus and scandium are overabundant by factors of 10 and 30 times their solar abundances. These new determinations differ from previous determinations partly because the atomic data have changed. A non-uniform distribution of the elements over the surface of HD 110073 could also account for the differences.

Keywords: Mercury-manganese stars, Chemically peculiar stars
Hidden Companions to Intermediate-mass Stars. XII. Discovery of a 1.8 M <SUB>⊙</SUB>, 1.3 au Companion to Delta Serpentis A. Delta Serpentis is a nearby 4″ visual binary (A+B) that has accrued a number of astrometric anomalies. Here we show that the primary component is actually a close binary based on a VLTI/GRAVITY archival interferometric observation. The newly discovered companion has a K band flux ratio of 33% at a projected separation ρ = 23.9 mas ↔ 1.3 au. Through isochrone fitting we find somewhat evolved 1.2 Gyr old M Aa = 1.98 M ⊙, M Ab = 1.80 M ⊙ and M B = 1.88 M ⊙ stars. Delta Ser joins a growing list of intermediate mass hierarchical multiples and may be a progenitor of a rather rare system of three white dwarfs. *Based on observations collected at the European Southern Observatory, Chile, Program ID 60.A-9801(U).

Keywords: Optical interferometry, Multiple stars, Delta Scuti variable stars, A stars
Merger Interactions Enhance Star Formation Rates in Galaxy Group Housing QSO PKS0405-123 and Gaseous Nebulae. The star formation rate (SFR) of galaxies can change due to interactions between galaxies, stellar feedback ejection of gas into the circumgalactic medium, and energy injection from accretion onto black holes. However, it is not clear which of these processes dominantly alters the formation of stars within galaxies. Johnson et al. reported the discovery of large gaseous nebulae in the intragroup medium of a galaxy group housing QSO PKS0405-123 and hypothesized they were created by galaxy interactions. We identify a sample of 30 group member galaxies at z ~ 0.57 from the Very Large Telescope/Multi Unit Spectroscopic Explorer observations of the field and calculate their [O II]λλ3727,3729 SFRs in order to investigate whether the QSO and nebulae have affected the SFRs of the surrounding galaxies. We find that star formation is more prevalent in galaxies within the nebulae, signifying galaxy interactions are fueling higher SFRs.

Keywords: Galaxy interactions, Star formation, Quasars
Hycean Exoplanets as Targets for Technosignature Detection: A Case Study of K2-18 b in the 3-10 GHz Band. Recently the James Webb Space Telescope performed near-infrared spectroscopic observations of the atmosphere of a potential Hycean exoplanet, K2-18 b. These spectra provided evidence of methane and carbon dioxide in its atmosphere, along with a possible line attributed to biomarker dimethyl sulfide. In this work, we present triggered narrow-band radio observations of K2-18 b conducted using the Allen Telescope Array over 3-10 GHz, in search of signs of artificially produced radio emissions (technosignatures). We do not find any spatially isolated signals in the direction of K2-18 b, establishing lower and upper limits on the equivalent isotropic radiated power (~1013-1016 W) of potential extraterrestrial transmitters between 3 and 10 GHz. This study emphasizes the importance of ongoing observations to further explore K2-18 b's potential as a candidate for the detection of technosignatures.

Keywords: Observational astronomy, Exoplanets, Exoplanet astronomy, Astronomical techniques, Astrobiology, Radio observatories, Radio interferometry, Radio astronomy, Astronomical methods, Doppler shift
Hidden Companions to Intermediate-mass Stars. XIII. Discovery of a 0.80 M <SUB>⊙</SUB>, 4.3 au Companion to HIP 7298. Proper motion changes between astrometric surveys provide a hint for unresolved companions and near-infrared interferometry is arguably the most efficient way to reveal or constrain their nature. Here we report on the VLTI/GRAVITY. detection of a companion to the nearby star HIP 7298 with a K band flux ratio of 11.9% at a projected separation ρ = 57.1 mas ↔ 4.3 au. Through isochrone fitting we find that the primary is a 1 Gyr old M  A  = 1.56M ⊙ star while the newly discovered secondary is a M  B  = 0.80M ⊙ K dwarf. The stars will most likely avoid common envelope evolution and will become a system similar to Gliese 86 in about 1.5 Gyr. *Based on observations collected at the European Southern Observatory, Chile, Program ID 111.24UP.001.

Keywords: Optical interferometry, Multiple stars, A stars
Three Scattered Sunspot Records in the Archive of the Royal Astronomical Observatory of the Spanish Navy (1789-1790). The recovery of records of past solar observations is crucial to understand the evolution of solar activity. In this context, three records of sunspot observations made at the Royal Observatory of the Spanish Navy in 1789 January and July, and 1790 June are shown in the present work. The aim of the observers who performed these sunspot observations was the discovery of intramercurial planets crossing the solar disk. For that reason, the observers only recorded round and dark spots and they may not have recorded all the sunspots that they observed. However, these records provide us with previously unknown information such as dates of active days (days with sunspots on the Sun) and position of sunspots.

Keywords: Sunspots
Abundances of Iron-peak Elements in the B8 Mn Star HD 110073. The synthesis of spectral intervals in the optical range allows the determination of LTE abundances of several iron-peak elements for the chemically peculiar B8 Mn star HD 110073. Titanium, chromium and manganese are found to be overabundant by factors of 19, 4 and 250 times their respective solar abundances. Iron and nickel are deficient by factors of 0.25 and 0.10. Weak lines of Cr II formed deep in the atmosphere yield lower chromium abundances than strong lines do by a factor of 2. This supports that chromium is probably stratified vertically in the atmosphere of HD 110073. Several weak flat-bottomed lines which could be caused by vertical stratification of the abundances are present throughout the spectra. The new abundance determinations differ from previous determinations partly because the atomic data have changed. A non-uniform distribution of the elements over the surface of HD 110073 could also account for variation of the lines with time.

Keywords: Mercury-manganese stars, Chemically peculiar stars
New Active Quasi-Hilda Asteroid 2004 CV50: A Citizen Science Discovery. We report that minor planet 2004 CV50 displayed cometary activity in the form of a short, diffuse tail, first identified by volunteers of the Citizen Science program Active Asteroids, a NASA Partner program hosted on the Zooniverse online platform. The activity is present in three images, from UT 2020 February 15 and UT 2020 March 14, that were acquired with the Dark Energy Camera on the Blanco 4 m telescope at the Cerro-Tololo Inter-American Observatory in Chile. We find that 2004 CV50 is most likely an active quasi-Hilda object rather than an active asteroid, despite 2004 CV50 having a Tisserand parameter with respect to Jupiter of 3.06.

Keywords: Comet tails, Asteroids, Comae
No Dispersed Single Radio Pulses Detected in Archival Parkes Pulsar Observations Targeting Supernova Remnants and Anomalous X-Ray Pulsars. Four supernova remnants and four anomalous X-ray pulsars were previously observed with the Parkes telescope in a campaign to detect pulsed radio emission from associated neutron stars. No signals were detected in the original searches of these data. I have reprocessed the data with the more recently developed HEIMDALL and FETCH software packages, which are optimized for single-pulse detection and classification. In this new analysis, no astrophysical pulses were detected having a signal-to-noise ratio above 7 from any of the targets at dispersion measures ranging from 0 to 104 pc cm-3. I include calculated fluence limits on single radio pulses from these targets.

Keywords: Transient sources, Pulsars
Kepler Problem under Repulsive Inverse-square Central Forces. In this article, I present important results of the Kepler problem under repulsive inverse-square central forces. While motions of this type have been discussed thoroughly in the classical scattering theory, I do not find available literature that treats the problem as an analog of the Kepler problem under an attractive central force. My results are applicable to motions of dust particles subject to solar radiation pressure accelerations exceeding the solar gravitational acceleration in the two-body problem.

Keywords: Orbital motion, Comets, Comet dust tails, Two-body problem
AT 2023prq: A Classical Nova in the Halo of the Andromeda Galaxy. The classical nova, AT 2023prq, was discovered on 2023 August 15 and is located at a distance of 46 kpc from the Andromeda galaxy (M31). Here we report photometry and spectroscopy of the nova. The "very fast" ( ${t}_{2,{r}^{{\prime} }}\sim 3.4$ days) and low luminosity ( ${M}_{{r}^{{\prime} }}\sim -7.6$ ) nature of the transient along with the helium in its spectra would indicate that AT 2023prq is a "faint-and-fast" He/N nova. Additionally, at such a large distance from the center of M31, AT 2023prq is a member of the halo nova population.

Keywords: Classical novae