Sazuna/UAT_keywords huggingface dataset:
Pulsating and Nonpulsating Components of Detached Eclipsing Binaries in the δ Scuti Instability Strip. Pulsating detached eclipsing binary systems are crucial for studying the internal structure of oscillating stars. These systems are advantageous because binary effects on pulsations are minimal, allowing for more accurate determinations of fundamental stellar parameters such as mass and radius. They serve as unique laboratories for detailed investigations of pulsating stars. In this study, we focused on four detached eclipsing binaries exhibiting δ Scuti−type oscillations: HD 117476, 205 Dra, HY Vir, and V1031 Ori. Our preliminary investigation showed that all binary components of these targets lie within the δ Scuti instability strip. Therefore, we aimed to determine which components are pulsating and which are not and to explore the differences between them. To achieve this, we analyzed TESS photometric data and high-resolution spectra of the targets. Radial velocity (RV) variations were measured, and atmospheric parameters for each component were derived using spectral disentangling or synthetic composite spectra. We also modeled the binary light and RV curves to determine the fundamental physical parameters of the components. Furthermore, we examined pulsation properties using three different approaches to identify the pulsating components. The evolutionary status of the targets was also assessed. Our analysis revealed that, in each system, only one component exhibits δ Scuti−type pulsations, while the others are nonpulsating. Interestingly, we found that the key difference between pulsating and nonpulsating components within the same binary is metallicity: the metal-rich components were found to be nonpulsators, supporting theoretical studies on the effect of metallicity on δ Scuti−type pulsations.

Keywords: Eclipsing binary stars, Delta Scuti variable stars, Stellar pulsations
Physical Properties of Gas Departing from Circular Rotation at 50 pc Scales Using the PHANGS-MUSE Galaxies. Noncircular (NC) motions have been observed across various spatial scales in disk galaxies, yet the physical properties of the gas involved in these motions remain poorly constrained. Using data from 19 galaxies from the PHANGS-MUSE sample, we investigated the prevalence of NC flows at spatial resolutions of tens of parsecs. We developed a new tool for 3D kinematic modeling of data cubes and applied to the PHANGS-MUSE Hα spectral lines to recover the underlying circular, NC motions, as well as the intrinsic velocity dispersion in these objects. The PHANGS-MUSE galaxies exhibit rotation-supported disks with Vrot/σintrin ratios ≳5. Our analysis revealed ionized gas exhibiting NC motions at different amplitudes, with low velocity amplitudes of about 5 km s−1 associated with the axisymmetric rotation component, deviations of ∼10 km s−1 primarily linked to interarm regions and spiral arms, and larger deviations (&gt;20 km s−1), found in the central and bar regions. We found that the velocity dispersion and the strength of ionization correlate with the amplitude of NC motions, suggesting that the underlying dynamics of the warm gas are closely tied to its physical properties.

Keywords: Publicly available software, Spiral galaxies, Disk galaxies, Galaxy kinematics, Interstellar medium, Barred spiral galaxies
Apache Point Rapid Response Characterization of Primitive Imminent Impactor 2024 RW<SUB>1</SUB>. Imminent impactors may be detected only a few hours before their impact with Earth, providing a brief opportunity to characterize them before impact. We describe the characterization of imminent impactor 2024 RW1, which was discovered by the Catalina Sky Survey on 2024 September 4 at 05:43 UTC, before it entered the atmosphere near the northern Philippines at 16:39 UTC. We observed 2024 RW1 with the Astrophysical Research Consortium Telescope Imaging Camera on the Apache Point Astrophysical Research Consortium's 3.5 m telescope on 2024 September 4 at 10:16 UTC. We obtained g, r, i, and z photometry of 2024 RW1, yielding color indices of g–r = 0.47 ± 0.04, r–i = 0.13 ± 0.04, i–z = –0.11 ± 0.07, and g–i = 0.60 ± 0.04, corresponding to a spectral slope of 0.67 ± 0.40 %/100 nm. The closest match to an asteroid spectral type is with B-type asteroids from the C complex. We detect variations in the time-series photometry of the asteroid with an amplitude of ∼0.75, and a double-peaked rotation period of ∼1900 s. Assuming a visible albedo of 0.07 ± 0.03, a density of ∼1500 kg m‑3, and a calculated absolute magnitude of 30.92 ± 0.05, we estimate that the asteroid has a diameter of 3.3 ± 0.7 m and a total mass of ∼28,000 kg. Comparing our astrometric orbital solutions to NEOMOD3, the most likely source of 2024 RW1 is the 3:1 main-belt mean-motion resonance (77% probability) followed by the ν6 resonance (13% probability), consistent with its organic B-type nature.

Keywords: Near-Earth objects, Asteroids, Meteoroids, Bolides, Apollo group
An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b. Ground-based high-resolution spectroscopy enables precise molecular detections and velocity-resolved atmospheric dynamics, offering a distinct advantage over low-resolution methods for exoplanetary atmospheric studies. Immersion GRating INfrared Spectrograph 2 (IGRINS-2), the successor to IGRINS, features improved throughput and enhanced sensitivity to carbon monoxide by shifting its K-band coverage by 36 nm to longer wavelengths. IGRINS is a near-infrared high-resolution spectrograph mounted at McDonald, Lowell, and Gemini-South observatories. Our order-drop test shows this added range improves the CO cross-correlation signal-to-noise ratio (SNR) by ∼2%─3%, confirming a measurable but modest sensitivity gain. To evaluate its performance, we attempt to investigate the atmospheric characteristics of WASP-33 b. Observations were conducted on 2024 January 7 for a total of 2.43 hr; This includes 1.46 hr in the pre-eclipse phase to capture the planet's thermal emission spectrum. We successfully detect clear cross-correlation signals from molecular species in the dayside atmosphere of WASP-33 b with a combined SNR of 7.4. More specifically, we capture CO, H2O, and OH with SNRs of 6.3, 4.7, and 4.2, respectively. These results are consistent with previous studies and demonstrate that IGRINS-2 is well suited for detailed investigation of exoplanetary atmospheres. We anticipate that future observations with IGRINS-2 will further advance our understanding of exoplanetary atmospheres.

Keywords: High resolution spectroscopy, Exoplanet atmospheric composition , Infrared spectroscopy, Hot Jupiters, Spectrometers, Astronomical instrumentation, Exoplanet atmospheres
Molecular Gas Distribution Toward the Inner and Outer Galaxy Revealed by MWISP—The Galactic Longitude 45°–60° and 120°–130°. Molecular clouds (MCs) are cradles of star and planet formation, thereby playing an important role in the evolution of galaxies. Based on the unbiased Milky Way Imaging Scroll Painting survey data of 12CO, 13CO, and C18O (J = 1–0) line emission in two regions toward the inner and outer Galaxy, i.e., the G50 (44 .° 75 ≤ l ≤ 60 .° 25) and G120 (119 .° 75 ≤ l ≤ 130 .° 25) regions, the distribution of molecular gas is studied. Both regions have Galactic latitudes of ∣b∣≤ 5 .° 25. A catalog containing 24,724 MCs is constructed from the data. In our proximity, several molecular structures with large angular scales and small velocity dispersions are discovered, resembling curtains of mist. Beyond the nearby molecular gas, a clear aggregation of MCs along coherent structures in the Galactic plane is visible, sketching spiral arm structures. Nevertheless, the aggregation of MCs is also detected in the inter-arm region between the Perseus and Outer arms in the G50 region. The Galactic molecular disk in this inter-arm region is found to be thinner than that in the adjacent spiral arm region. In addition, the thickness of the Galactic molecular disk examined here is found to be correlated with the warp of it, indicating their homologous origins. The molecular disk has a typical thickness of ∼220 pc in the inner Galaxy. Moreover, the dispersion of the MC systemic velocity decreases with increasing galactocentric radius, resulting in lower kinematic distance uncertainties at larger radii. However, the Perseus arm segment in the G120 region exhibits a relatively large cloud-to-cloud velocity dispersion and split components in its MC velocity distribution.

Keywords: Galaxy structure, Radio astronomy, Molecular clouds, Interstellar medium
Hot Rocks Survey. IV. Emission from LTT 3780 b Is Consistent with a Bare Rock. It is an open question whether small planets around M dwarfs are able to maintain atmospheres. The Hot Rocks Survey aims to address this question by observing nine rocky exoplanets orbiting M dwarfs with MIRI emission photometry to constrain the onset of atmospheres. In this paper, we present two MIRI F1500W (15 μm) eclipses of LTT 3780 b, an ultrashort-period super-Earth (P = 0.768 days, R = 1.325 R⊕, M = 2.46 M⊕) that receives 111× Earth's instellation, the highest in the survey. We find a combined eclipse depth of 312 ± 38 ppm, which is consistent between different data reduction and analysis assumptions, bolstering our confidence in the eclipse detection. This eclipse depth is consistent with the thermal emission from a bare rock surface, with a dayside temperature of  Tday=1143‑99+104  K, 98% ± 9% of the maximum temperature predicted for a zero-albedo, zero heat redistribution blackbody. We are able to confidently rule out CO2-based atmospheres down to a 0.01 bar surface pressure to greater than 3σ (ruling out an approximately Mars-like atmosphere). We are unable to rule out a pure H2O 1 bar atmosphere, though we argue that this composition is unlikely on such a highly irradiated planet, nor O2 atmospheres due to the lack of features in the bandpass, though we can put constraints on CO2-mixture atmospheres. As a potential bare rock, we consider a variety of surface composition models, but are unable to distinguish between them. However, LTT 3780 b is an excellent target for follow-up JWST observations to determine its surface composition and rule out additional atmospheric compositions.

Keywords: M dwarf stars, Exoplanet astronomy, Exoplanet atmospheres, Extrasolar rocky planets
The DELVE Quadruple Quasar Search. I. A Lensed Low-luminosity Active Galactic Nucleus. A quadruply lensed source, J125856.3–031944, has been discovered using the DELVE survey and Wide-field Infrared Survey Explorer W1–W2 colors. Follow-up direct imaging carried out with the Magellan Baade 6.5 m telescope is analyzed, as is spectroscopy from the 2.5 m Nordic Optical Telescope. The lensed image configuration is kite-like, with the major axis of the lensing galaxy along the symmetry axis of the kite, and with the faintest image at its tail. Redward of 6000 Å, the tail image is strongly blended with the lensing galaxy. The Sloan g direct imaging carried out with Magellan permits deblending. As the lensed image configuration is nearly circular, simple models give high predicted magnifications for all four images. The source's narrow emission lines at redshift z = 2.225 and low intrinsic luminosity qualify it as a type 2 active galactic nucleus. The Magellan image shows a substantial residual that suggests a second lensing galaxy.

Keywords: Strong gravitational lensing, Low-luminosity active galactic nuclei, Quasars
V659 Cen: System Members Updated. V659 Cen is a classical Cepheid which is part of a multiple system. Previous observations have shown that a hot companion dominates an ultraviolet spectrum and a cooler main-sequence star dominates an XMM-Newton spectrum. The Hubble Space Telescope Space Telescope Imaging Spectrograph spectra discussed here spatially resolve the components and show that the secondary in the spectroscopic binary with the Cepheid is the low-mass star, and the hottest star in the system is the outer companion. In addition a fourth star is a likely member of the system based on Gaia data. A new orbit is derived, which includes new radial velocities.

Keywords: Multiple stars, Massive stars, Delta Cepheid variable stars
Revealing the Bifurcations of the Milky Way Spiral Arms Based on Hi-GAL and ATLASGAL Clumps. The spiral structure of the Milky Way remains under debate. Y. Xu et al. proposed, for the first time, a multiple-arm morphology for our Galaxy, with two spiral arms in the inner disk bifurcating outward alongside additional independent arms in the outer disk. This model aligns with the statistical properties of spiral arms seen in many extragalactic spiral galaxies and differs from the traditional standard model primarily in the presence of bifurcation points. This study aims to search for observational evidence of spiral arm bifurcations in the Milky Way and constrain its structure. Using the Herschel Infrared Galactic Plane Survey and the APEX Telescope Large Area Survey of the Galaxy clump catalogs, we first reassess the spiral arm tangent points, then analyze the statistical distributions of Galactic longitude, latitude, and velocity to identify signatures of bifurcations and constrain their potential locations. Our results suggest that the Perseus and Sagittarius arms may merge near Galactic longitude ℓ ∼ 15° in the first quadrant. Symmetrically, in the fourth quadrant, the sources are distributed along the Galactic longitude with a concentration at ℓ ∼ 333°, where the Norma and Centaurus arms are likely to converge.

Keywords: Interstellar dust, Galaxy structure, Galaxy kinematics, Molecular clouds
JWST/MIRI Imaging of the Warm Dust Component of the ϵ Eridani Debris Disk. We present JWST/MIRI observations of the debris disk surrounding the nearby solar analog ϵ Eridani obtained as part of the Archetypal Debris Disk Guaranteed Time Observation program. Multiwavelength images from 15, 18, 21, and 25.5 μm show a smooth dust distribution with no evidence of sculpting by massive planets outside of 5 au. Maps of the color temperature and opacity constrain the dust properties, while radiative transfer modeling of a warm dust component traces the interaction between the debris disk and ϵ Eridani b (∼3.5 au). Dynamical and collisional modeling further shows that the disk morphology is dominated by dust produced in the outer planetesimal belt (∼70 au) moving inward via stellar wind drag. We confirm the presence of a disk interior to the ϵ Eri b orbit first detected from mid-IR interferometry. Drag-dominated inner disk regions have also been observed around Vega and Fomalhaut, hinting at the diversity of asteroid belt analogs.

Keywords: Circumstellar dust, Debris disks, Exoplanet systems, Direct imaging
Investigating Phosphorus Abundances in a Sample of APOGEE-2 Bulge Globular Clusters. Phosphorus-enhanced (P-rich; [P/Fe] ≳ +0.8) giants have been found among mildly metal-poor field stars, but in only one star in a globular cluster (GC), M4 (NGC 6121). Also, in a sample of bulge spheroid stars, some of them showed a moderate P enhancement in the range +0.5 &lt; [P/Fe] &lt; +1.0. In this paper we derive the P abundance of moderately metal-poor ([Fe/H] ≳ ‑1) GC stars, aiming to check if the phenomenon could be related to the unusual multiple stellar populations found in most GCs. Here we present the detection of moderately P-enhanced stars among two out of seven bulge GCs (Tonantzintla 1 and NGC 6316), with metallicities similar to those of the bulge-field P-rich stars. Using H-band high-resolution (R ∼ 22,500) spectra from the APOGEE-2 survey, we present the first high-resolution abundance analysis of [P/Fe] from the P I 16482.932 Å line in a sample of selected bulge GCs. We find that all P-rich stars tend to also be N-rich, which hints at the origin of P-rich stars as second-generation stars in GCs. However no other correlations of P and other elements are found, which are usually indicators of second-generation stars. Further studies with larger samples and comparisons with field stars will be needed before any firm conclusions are drawn.

Keywords: Globular star clusters, Stellar abundances, Galactic bulge
An Algorithm Architecture for Radio Interferometric Data Processing. We present a foundational, scalable algorithm architecture for processing data from aperture synthesis radio telescopes. The analysis leading to the architecture is rooted in the theory of aperture synthesis, signal processing, and numerical optimization, keeping it scalable for variations in computing load, algorithmic complexity, and accommodate the continuing evolution of algorithms. It also adheres to scientific software design principles and use of modern performance engineering techniques providing a stable foundation for long-term scalability, performance, and development cost. We first show that algorithms for both calibration and imaging share a common mathematical foundation and can be expressed as numerical optimization problems. We then decompose the resulting mathematical framework into fundamental conceptual architectural components, and assemble calibration and imaging algorithms from these foundational components. For a physical architectural view, we used a library of algorithms implemented in the LibRA software for the various architectural components, and used the Kokkos framework in the compute-intensive components for performance portable implementation. This was deployed on hardware ranging from desktop-class computers to multiple supercomputer class high-performance computing and high-throughput computing (HTC) platforms with a variety of CPU and GPU architectures, and job schedulers (HTCondor and Slurm). As a test, we imaged archival data from the Very Large Array telescope in the A-array configuration for the Hubble Ultra Deep Field. Using over 100 GPUs, we achieve a processing rate of ∼2 TB hr−1 to make one of the deepest images in the 2─4 GHz band with an rms noise of ∼1 μJy beam−1.

Keywords: Radio interferometry, Astronomy software, Astronomy data reduction
Stringent Upper Bounds on Atmospheric Mass Loss from Three Neptune-sized Planets in the TOI-4010 System. Photoevaporative models predict that the lower edge of the Neptune desert is sculpted by atmospheric mass loss. However, the stellar high-energy fluxes that power hydrodynamic escape and set predicted mass loss rates can be uncertain by multiple orders of magnitude. These uncertainties can be bypassed by studying mass loss for planets within the same system, as they have effectively undergone scaled versions of the same irradiation history. The TOI-4010 system is an ideal test case for mass loss models, as it contains three Neptune-sized planets with planet b located in the "Neptune desert," planet c in the "Neptune ridge," and planet d in the "Neptune savanna." Using Keck/NIRSPEC, we measured the metastable helium transit depths of all three planets in order to search for evidence of atmospheric escape. We place upper bounds on the excess helium absorption of 1.23%, 0.81%, and 0.87% at 95% confidence for TOI-4010 b, c, and d respectively. We fit our transmission spectra with Parker wind models and find that this corresponds to 95th-percentile upper limits of 1010.17 g s‑1, 1010.53 g s‑1, and 1010.50 g s‑1 on the mass loss rates of TOI-4010 b, c, and d respectively. Our non-detections are inconsistent with expectations from one-dimensional hydrodynamic models for solar composition atmospheres. We consider potential reductions in signal from a decreased host star extreme ultra-violet and X-ray luminosity, planetary magnetic fields, enhanced atmospheric metallicities, and fractionation, and explore the implications of our measurements for the past evaporation histories of all three planets.

Keywords: Exoplanets, Planetary atmospheres, Exoplanet astronomy, Exoplanet evolution, Extrasolar gaseous planets, Extrasolar gaseous giant planets, Exoplanet atmospheres
Dense-photometry Validation of Superfast-rotating Asteroid Candidates. Superfast rotators (SFRs; P &lt; 2.2 hr) are of great importance in asteroid studies; yet, many reported detections suffer from aliasing caused by an insufficient observation cadence. We present dense CCD photometry for 15 SFR candidates (14 after excluding 11219 Benbohn, whose published period already exceeds the spin barrier) observed from 2023 August 11 to 2024 August 11 with the 1.5 m Sierra Nevada and 1.4 m Astronomical Station of Vidojevica telescopes. Our data set comprises approximately 2400 calibrated data points, with per-measurement formal errors of 0.02–0.04 mag and total on-target coverage of 2–13 hr per object. We have reliably determined periods for nine targets. In terms of spin rate, we have confirmed four SFRs with periods of 1.06–1.84 hr and peak-to-peak amplitudes of 0.054–0.685 mag. Three candidates remain ambiguous, while the rest are reclassified, showing the best solutions with periods greater than 2.5 hr. Extrapolating from our confirmation rate (4/14) to the 3.9% occurrence rate found in the Light Curve Database yields a central SFR fraction of 1.1%, with a 1σ lower bound of 0.6% among kilometer-scale asteroids.

Keywords: CCD photometry, Asteroid rotation, Solar system, Asteroids
FUMES. IV. Optical and Far-ultraviolet Spectra of a Flare on the M Dwarf GJ 4334. On 2017 September 20, we observed GJ 4334, an M5V dwarf rotating with a period of 23.5 days, simultaneously with both the Space Telescope Imaging Spectrograph aboard Hubble (1160─1710 Å) and the Dual Imaging Spectrograph mounted on the 3.5 m telescope at Apache Point Observatory (3750─5050; 5800─6950 Å) as part of a larger survey of intermediately active M dwarfs. GJ 4334 flared during the observation, starting with a rise in the flux of optical chromospheric emission lines, followed by the rapid rise and decay of multiple far-ultraviolet emission lines formed in the transition region, followed by the slow decay of the optical lines. We find significant broadening and asymmetries in the optical emission lines that are potentially from bulk plasma motion, a postflare elevated flux in both the optical and far-ultraviolet, and trends in the rise and decay timescales of the Balmer series such that higher-order lines rise earlier and decay faster than lower-order lines. The equivalent durations of the flare in individual lines range from 800 to 3 × 104 s, mapping to flare energies of 1 × 1028─3 × 1029 erg for each line. To contextualize GJ 4334's flare behavior, we measure and compare its optical flare frequency distribution with TESS to EV Lacertae, a similar mass but faster rotating M dwarf, and find that GJ 4334 has an excess of large flares relative to the power law established by the majority of its smaller flares. This data set is a rare opportunity to characterize flares near a critical transition in stellar magnetic activity.

Keywords: M dwarf stars, Stellar chromospheres, Ultraviolet spectroscopy, Stellar activity, Stellar flares, Optical flares
AutoWISP: Automated Processing of Wide-field Color Images. We have developed a software pipeline, AutoWISP, for extracting high-precision photometry from citizen scientists' observations made with consumer-grade color digital cameras (digital single-lens reflex, or DSLR, cameras), based on our previously developed tool, AstroWISP. The new pipeline is designed to convert these observations, including color images, into high-precision light curves of stars. We outline the individual steps of the pipeline and present a case study using a Sony-α 7R II DSLR camera, demonstrating subpercent photometric precision, and highlighting the benefits of three-color photometry of stars. Project PANOPTES will adopt this photometric pipeline and, we hope, be used by citizen scientists worldwide. Our aim is for AutoWISP to pave the way for potentially transformative contributions from citizen scientists with access to observing equipment. * https://github.com/kpenev/AutoWISP

Keywords: Publicly available software, Stellar photometry, Amateur astronomy, Multi-color photometry, Sky surveys, Exoplanets, Light curves, Time domain astronomy, Photometry, Variable stars, Transit photometry, Astronomy image processing