Sazuna/UAT_keywords huggingface dataset:
OGLE-2014-BLG-1760: A Jupiter─Sun Analogue Residing in the Galactic Bulge. We present the analysis of OGLE-2014-BLG-1760, a planetary system in the galactic bulge. We combine Keck Adaptive Optics follow-up observations in K-band with re-reduced light-curve data to confirm the source and lens star identifications and stellar types. The re-reduced Microlensing Observations in Astrophysics data set had an important impact on the light-curve model. We find the Einstein ring crossing time of the event to be ∼2.5 days shorter than previous fits, which increases the planetary mass-ratio and decreases the source angular size by a factor of 0.25. Our OSIRIS images obtained 6 yr after the peak of the event show a source-lens separation of 54.20 ± 0.23 mas, which leads to a relative proper motion of μrel = 9.14 ± 0.05 mas yr−1 and is larger than the previous light-curve-only models. Our analysis shows that the event consists of a Jupiter-mass planet of Mp = 0.931 ± 0.117 MJup orbiting a K-dwarf star of M* = 0.803 ± 0.097 M⊙ with a K-magnitude of KL = 18.30 ± 0.05, located in the galactic bulge or bar. We also attempt to constrain the source properties using the source angular size θ* and K-magnitude. Our results favor the scenario of the source being a younger star in the galactic disk, behind the galactic bulge, but future multicolor observations are needed to constrain the source and thus the lens properties.

Keywords: Gravitational microlensing, Galactic bulge, Exoplanets, Adaptive optics
Tools for High-precision Photometry from Wide-field Color Images. We present AstroWISP: a collection of image processing tools for source extraction, background determination, point-spread function/pixel-response function fitting, and aperture photometry. AstroWISP is particularly well suited for working with detectors featuring a Bayer mask (an array of microfilters applied to each detector pixel to allow color photography), such as consumer digital single-lens reflex (DSLR) cameras. Such detectors pose significant challenges for existing tools while offering a much cheaper alternative to specialized devices. As a result, consumer DSLR cameras with Bayer masks are often underutilized for precision photometry. AstroWISP addresses this limitation in an effort to democratize precision photometry and support broader community participation in research. We demonstrate that our tools produce high-precision photometry from such images, enabling the use of such devices for detecting exoplanet transits. We package our tools for all major operating systems to ensure accessibility for amateur astronomers.

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
Delayed and Displaced: The Impact of Binary Interactions on Core-collapse SN Feedback. Core-collapse supernova feedback models in hydrodynamical simulations typically assume that all stars evolve as single stars. However, the majority of massive stars are formed in binaries and multiple systems, where interactions with a companion can affect stars' subsequent evolution and kinematics. We assess the impact of binary interactions on the timing and spatial distribution of core-collapse supernovae, using cogsworth simulations to evolve binary star populations, and their subsequent galactic orbits, within state-of-the-art hydrodynamical zoom-in galaxy simulations. We show that binary interactions: (a) displace supernovae, with ∼13% of all supernovae occurring more than 0.1 kpc from their parent cluster; and (b) produce delayed supernovae, such that ∼25% of all supernovae occur after the final supernova from a single star population. Delays are largest for low-mass merger products, which can explode more than 200 Myr after a star formation event. We characterize our results as a function of: (1) initial binary population distributions, (2) binary physics parameters and evolutionary pathways, (3) birth cluster dissolution assumptions, and (4) galaxy models (which vary metallicity, star formation history, gravitational potential, and simulation codes), and show that the overall timing and spatial distributions of supernovae are surprisingly insensitive to most of these variations. We provide metallicity-dependent analytic fits that can be substituted for single-star subgrid feedback prescriptions in hydrodynamical simulations, and discuss some of the possible implications for binary-driven feedback in galaxies, which may become particularly important at high redshift.

Keywords: Hydrodynamical simulations, Binary stars, Stellar feedback, Core-collapse supernovae, Galaxy dynamics, Stellar evolution
Consequences of Non-Gaussian Instrumental Noise in Perturbed Nulling Interferometers. With the astrophysics community working toward the first observations and characterizations of Earth-like exoplanets, interest in space-based nulling interferometry has been renewed. This technique promises unique scientific and technical advantages by enabling direct mid-infrared observations. However, concept studies of nulling interferometers often overlook the impact of systematic noise caused by instrument perturbations. Earlier research introduced analytical and numerical models to address instrumental noise; building on these results, we reproduce key simulations and report that the noise in the differential output of nulling interferometers follows a non-Gaussian distribution. The presence of non-Gaussian noise challenges the validity of classical hypothesis tests in detection performance estimates, as their reliance on Gaussian assumptions leads to overconfidence in detection thresholds. For the first time, we derive the true noise distribution of the differential output of a dual Bracewell nulling interferometer, demonstrating that it follows iterative convolutions of Bessel functions. Understanding this noise distribution enables a refined formulation of hypothesis testing in nulling interferometry, leading to a semianalytical prediction of detection performance. This computationally efficient instrument model, implemented in a publicly available codebase, is designed for integration into science yield predictions for nulling interferometry mission concepts. It will play a key role in refining key mission parameters for the Large Interferometer For Exoplanets.

Keywords: Direct detection interferometry, Analytical mathematics, Astronomical instrumentation, Space telescopes, Habitable planets
Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST. VV 191 is a nearby (z ∼ 0.05), overlapping (occulting) galaxy pair, where a multiple-armed spiral galaxy is backlit by an elliptical galaxy. The overlap is used to derive and map dust attenuation in two James Webb Space Telescope NIRCam filters (F090W and F150W) and one visible-band Hubble Space Telescope Wide Field Camera 3 filter (F606W). We present maps of the attenuation in each filter, the ratio of total to selective attenuation with a near-infrared (NIR) color excess,  RVI∼ , and the NIR attenuation curve power-law index, α, approximated via Monte Carlo resampling methods. The maps trace the optically thin outer disk of foreground galaxy VV 191b at ∼100 pc physical resolution. We find the distributions of attenuation and  RVI∼  to be close to log-normal, and the distribution of α to be close to Gaussian throughout the disk and in high signal-to-noise ratio areas of VV191b. We analyze three spatially resolved handpicked regions in the far outer disk that are well backlit by the background galaxy.

Keywords: Interstellar dust, Disk galaxies, Interstellar reddening, Interstellar medium, Interstellar extinction
When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST. We investigate the polycyclic aromatic hydrocarbon (PAH) emission features of T Cha, a G8-type T Tauri star that has exhibited "seesaw"-type mid-infrared continuum variability over nearly two decades due to the destruction of the disk's inner wall, using JWST/Mid-Infrared Instrument and Spitzer observations. We report the first detection of weak PAH emission at 6.2, 7.7, and 8.6 μm in the Spitzer/Infrared Spectrograph spectrum from 2005. The destruction of the inner wall in the 2022 JWST epoch allowed more ultraviolet photons to reach the outer disk, increasing the flux levels of PAH bands and allowing their detection well above the continuum. The 11.2 μm PAH flux increases by a factor of 3, yet its profile shape remains remarkably stable, and the 6.2/11.2 μm flux ratio has increased, but the charge state of the PAH population remains 75% neutral. The PAH features exhibit a "class C" spectral profile, with redshifted peaks and broadened wings consistent with emission from low-mass T Tauri disks, while the weak 12.7/11.2 ratio points to a lower abundance of duo and trio hydrogen modes, implying a predominantly zigzag carbon structure. A faint "class A" subcomponent in the 6.2 and 7.7 μm bands may indicate additional PAH processing by ultraviolet radiation from accretion hotspots. Placement on PAH charge─size grids locates T Cha in the low-ionization, small-size regime (NC ≤ 30), signifying a largely neutral PAH population in multiple epochs spanning 18 yr. Through multiepoch, high-resolution data from JWST and Spitzer, we identify T Cha as a benchmark source for probing disk evolution and PAH processing, emphasizing the potential of temporal monitoring with JWST.

Keywords: Herbig Ae/Be stars, Polycyclic aromatic hydrocarbons, Astrochemistry, T Tauri stars, Young stellar objects, Protoplanetary disks
TrES-1 b: A Case Study in Detecting Secular Evolution of Exoplanet Orbits. We present a comprehensive analysis of transit, eclipse, and radial velocity data of the hot Jupiter TrES-1 b and confirm evidence of orbital variations on secular timescales. Apparent variations due to systemic motion and light travel time effects have been ruled out, indicating that the observed changes are dynamical in origin. Joint modeling of the TrES-1 b data favors an apsidal precession model, but the rapid precession rate of 4° yr−1 cannot be explained without invoking an undetected close-in planetary companion, which remains unseen in the data. While radial velocity measurements reveal a previously undetected companion candidate on a wide, eccentric orbit, it is unlikely to drive the observed evolution of TrES-1 b. However, an orbital decay model provides a plausible alternative if the loss of orbital energy is driven by planetary obliquity tides. We find that the best-fit orbital decay rate of  −7.1−1.6+1.5  ms yr−1 is aligned with theoretical predictions for modified tidal quality factors of hot Jupiters if TrES-1 b has a planetary obliquity ∊p &gt; 30°. We encourage follow-up observations of this system, particularly of eclipse timing and radial velocities, to further constrain the nature of the observed evolution. This paper provides a practical framework for studying secular variations and aims to accelerate future research on similar systems.

Keywords: Amateur astronomy, Hot Jupiters, Orbital evolution, Exoplanet astronomy, Exoplanet tides, Transit timing variation method
KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb: Mass Measurements for Two Super-Earth Microlensing Planets. KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb were the lowest mass-ratio microlensing planets at the time of discovery. For both events, microlensing parallax measurements from the Spitzer Space Telescope implied lens systems that were more distant and massive than those inferred from the ground-based parallax. Here, we report on the detection of excess flux aligned to the event locations using Keck Adaptive Optics imaging, which is consistent with the expected brightness of main-sequence hosts under the ground-based parallax, but inconsistent with that predicted by Spitzer. Based on the excess flux, ground-based parallax, and angular Einstein radius, we determine KMT-2018-BLG-0029Lb to be a 4.2 ± 0.5M⊕ planet orbiting a 0.70 ± 0.07M⊙ host at a projected separation of 3.1 ± 0.3 au, and OGLE-2019-BLG-0960Lb to be a 2.0 ± 0.2M⊕ planet orbiting a 0.40 ± 0.03M⊙ host at a projected separation of 1.7 ± 0.1 au. We report on additional light-curve models for KMT-2018-BLG-0029 under the generalized inner-outer (offset) degeneracy, which were not reported in the original analysis. We point out inconsistencies in the inner/outer labeling of the degenerate models in the lens and source planes, and advocate for the lens-plane convention, which refers to the planet being closer or further to the host star compared to the image it perturbs. Lastly, we discuss the possibility of breaking this degeneracy via ground concurrent observations with the Roman Space Telescope.

Keywords: Gravitational microlensing exoplanet detection, Exoplanets, Binary lens microlensing
A Search for Subdwarf B Binaries Using Pulsation Timing from TESS. Hot subdwarf B (sdB) stars are post-main-sequence stars of high temperature and gravity. Approximately 30% of sdBs exhibit stable pressure and/or gravity-mode pulsations, which can be used via the timing method to test for companion stars and determine their orbital solutions. We used short cadence data from the Transiting Exoplanet Survey Satellite (TESS) to search for previously undiscovered companions to sdBs. In this paper, we focus on searching for companions with orbital periods shorter than 13.5 days which are detectable within one sector of TESS data (about 27 days). The timing method requires that we derive pulsation frequencies in subsets of data significantly shorter than the periods we are searching for, which we set at 0.5–1.5 day. We investigated ten sdB stars with previously detected p-mode pulsations for which at least one p-mode pulsation remains detectable with a signal-to-noise ratio &gt; 4 within data subsets of duration 0.5–1.5 day. We find that two (TIC 202354658 and TIC 69298924) of these ten sdB stars likely have white-dwarf companions and set limits on companion masses for the other eight sdB stars.

Keywords: Binary stars, Pulsating variable stars, B subdwarf stars, Pulsation frequency method, Timing variation methods
Spot-crossing Variations Confirm a Misaligned Orbit for a Planet Transiting an M Dwarf. TOI-3884 b is an unusual 6.4 R⊕ planet orbiting an M4 host, whose transits display large and persistent spot-crossing events. We used the Tierras Observatory to monitor both the long-term photometric variability of TOI-3884 and changes in the spot-crossing events across multiple transits of the planet. We show that the star rotates with a period of 11.020 ± 0.015 days. We simultaneously model the rotational modulation of the star and variations in transit shapes that arise due to rotation of the spot, allowing us to determine the true stellar obliquity, ψ⋆. The data are best described by a planet on a misaligned orbit around a highly inclined star (ψ⋆ =  77.°4‑2.°5+2.°3 ; i⋆ =  22.°3‑1.°6+1.°8 ) that hosts a large polar starspot (rspot =  31.2∘‑1.9∘+2.4∘ ; λspot = 80 .° 5 ± 1 .° 2). Archival photometry from the Zwicky Transient Facility suggests that this polar spot has persisted on TOI-3884 for at least seven years. The TOI-3884 system provides a benchmark for studying the evolution of a polar spot on an M dwarf.

Keywords: Starspots, Transits, Exoplanets, Planetary alignment, Stellar rotation, Infrared photometry
Classifying Compact Radio Emission in Nearby Galaxies: A 10 GHz Study of Active Galactic Nuclei, Supernovae, Anomalous Microwave Emission, and Star-forming Regions. We present 115 compact radio point sources in three galaxies, NGC 5474, NGC 4631, and M51, taken in the most extended (A-)configuration of the Karl G. Jansky Very Large Array at 10 GHz. Several of these compact radio point sources have diffuse counterparts identified in previous multiband studies of resolved radio continuum emission. We find compact counterparts to eight star forming regions, four anomalous microwave emission candidates, and one supernova remnant (SN 2011dh). Nine of the compact radio sources match X-ray counterparts, the majority of which are background galaxies. These AGN are all within the D25 (isophotal diameter) of the host galaxy and might act as contaminants for X-ray binary population studies, highlighting the need for high-resolution multiband imaging. This study showcases the broad number of science cases that require sensitive radio facilities, like the upcoming Square Kilometre Array and the planned next generation Very Large Array.

Keywords: Supernova remnants, X-ray binary stars, Active galactic nuclei
A Coronagraphic Pilot Study of the Circumstellar Environments around Red Supergiants: CD -31°4916's Dust Morphology. Many mechanisms have been proposed to contribute to massive-star mass loss, but in general little is known about the physics involved. Studies of circumstellar environments around massive stars might help to determine which mechanisms are the most common. With the recent advent of high-contrast, extreme adaptive optics, coronagraphic instruments, direct-imaging studies of massive-star circumstellar environments have become possible. With these instruments, one can directly observe regions closer to the star than ever before. We performed a pilot study to image red supergiant circumstellar environments using the Gemini Planet Imager on Gemini South. In this paper, we report on the first direct detection of circumstellar dust around CD -31°4916, an otherwise "normal" red supergiant. This dust appears in both the near-infrared and the optical, which we obtained with follow-up HST observations. The dust appears to be at least partially located in clumps within 1″ of the central star. Therefore, we believe that continued exploration of massive star circumstellar environments with these coronagraphic instruments is warranted, even for systems with no previously resolved circumstellar material, and may play a vital role in our understanding of their mass-loss physics.

Keywords: Coronagraphic imaging, Circumstellar matter, Red supergiant stars, Stellar mass loss
Searching for GEMS: TOI-7149 b, an Inflated Giant Planet Causing a 12% Transit of a Fully Convective M-dwarf. We describe the discovery and characterization of TOI-7149 b, a 0.705 ± 0.075 MJ, 1.18 ± 0.045 RJ gas giant on a ∼2.65 days period orbit transiting an M4V star with a mass of 0.344 ± 0.030 M⊙ and an effective temperature of 3363 ± 59 K. The planet was first discovered using NASA's TESS mission, which we confirmed using a combination of ground-based photometry, radial velocities, and speckle imaging. The planet has one of the deepest transits of all known main-sequence planet hosts at ∼12% (Rp/R⋆ ∼ 0.33). Pushing the bounds of previous discoveries of giant exoplanets around M-dwarf stars (GEMS), TOI-7149 is one of the lowest mass M-dwarfs to host a transiting giant planet. We compare the sample of transiting GEMS to stars within 200 pc with a Gaia color–magnitude diagram and find that the GEMS hosts are likely to be high metallicity stars. We also analyze the sample of transiting giant planets using the nonparametric MRExo framework to compare the bulk density of warm Jupiters across stellar masses. We confirm our previous result that transiting Jupiters around early M-dwarfs have similar masses and densities to warm Jupiters around FGK stars, and extend this to mid M-dwarfs, thereby suggesting a potential commonality in their formation mechanisms.

Keywords: M dwarf stars, Radial velocity, Extrasolar gaseous giant planets, Astrostatistics
Multiband, Multiepoch Photometry of the Spot-crossing System TOI-3884: Refined System Geometry and Spot Properties. Spot-crossing transits offer a unique opportunity to probe spot properties such as temperature, size, and surface distribution. TOI-3884 is a rare system in which spot-crossing features are persistently observed during every transit. This is due to its unusual configuration: a nearly polar-orbit super-Neptune transits a pole-on mid-M dwarf, repeatedly crossing a polar spot. However, previous studies have reported discrepant values in key system parameters, such as stellar inclination and obliquity. To address this, we conducted multiband, multiepoch transit observations of TOI-3884 b using the MuSCAT instrument series, along with photometric monitoring with the Las Cumbres Observatory 1 m telescopes/Sinistro. We detected time-dependent variations in the spot-crossing signals, indicating that the spot is not exactly on the pole. From the monitoring data, we measured a stellar rotation period of  11.043‑0.053+0.054  days with a modulation amplitude of ∼5% in the r band, consistent with the time variability in the spot-crossing features. Our analysis reconciles previous discrepancies and improves the constraints on the parameters of the system geometry ( i⋆=139.9‑2.0+1.2  deg and  λ=41.0‑9.0+3.7  deg) and those of the spot properties (spot radius of  0.425‑0.011+0.018R⋆  and a spot–photosphere temperature difference of  200‑9+11  K). These results provide a critical context for interpreting upcoming transmission spectroscopy of TOI-3884 b, as well as yielding new insights into the magnetic activity and spin–orbit geometry of M dwarfs.

Keywords: M dwarf stars, Starspots, Multi-color photometry, Exoplanet systems, Transit photometry, Planet hosting stars, Stellar rotation
Additional JWST/NIRSpec Transits of the Rocky M Dwarf Exoplanet GJ 1132 b Reveal a Featureless Spectrum. As an archetypal M-dwarf rocky exoplanet, GJ 1132 b has a varied history of atmospheric measurements. At 1.13 R⊕, 1.66 M⊕, and 580 K, it orbits a bright, slowly rotating M dwarf in a 1.6 day period, making it a prime target for characterization. In this study, we combine two JWST NIRSpec/G395H transits previously reported by E. M. May et al. (2023) with two new NIRSpec/G395M transits to constrain the presence of an atmosphere. This marks the first time the G395H and G395M modes have been combined for a single target, and we report no difference in the quality of data between the two modes. For rocky M-dwarf studies, G395H may still be preferred if stacking transits to utilize the high-resolution flux-calibrated stellar spectra and assess evolving stellar heterogeneity. GJ 1132 b's coadded transmission spectrum is best fit with a flat line. A thin steam atmosphere is also consistent with the data, but this interpretation is driven almost entirely by the first transit, which suggests an increase in cool spot coverage-fraction derived from the flux-calibrated stellar spectra. This demonstrates the importance of always considering stellar heterogeneity evolution in multivisit transits, and also the importance of a "leave-one-transit-out" approach in modeling efforts of coadded transits. We combine these results with MIRI/LRS emission data to show that together, transmission and emission are consistent with only the thinnest of atmospheres. Given GJ 1132 b's age and distance from the star, a thin atmosphere is not likely stable. Therefore, the simplest explanation is that GJ 1132 b is indeed a bare rock.

Keywords: Extrasolar rocky planets, M dwarf stars, Exoplanet atmospheric composition , Transmission spectroscopy, Exoplanet astronomy, Exoplanet atmospheres