Sazuna/UAT_keywords huggingface dataset:
No Turnover Found in Giant-Planet Occurrence Within 3 au Around Low-mass Stars. Understanding how giant planet occurrence rates vary with stellar mass and orbital distance provides key insights into planet formation and evolution. However, most surveys are limited in sample size and stellar mass coverage, inhibiting demographic studies. Using an integrated demographics approach, we combine transit (Kepler, K2) and radial-velocity (CLS) surveys to measure the occurrence of 0.1─10 MJ planets around M-K (0.4─0.8 M⊙) stars and compare with population-synthesis models. We find no evidence for a turnover inside 3 au, unlike observations around Sun-like stars. We interpret the implications of this result and use our forward model to predict exoplanet occurrence at semimajor axes relevant for Gaia and direct imaging, which will provide critical constraints at wide separations and test the existence of a turnover.

Keywords: M dwarf stars, Extrasolar gaseous giant planets, Exoplanets
The NEAR Infrared Spectrometer (NIS) Instrument Bundle V1.0. This bundle contains all the data collected from the NIS instrument during the NEAR mission.

Keywords: Space probes, Orbiters, Asteroids, Eros, Infrared astronomy, Spectrophotometry, Solar system astronomy
Rivkin Three Micron Asteroid Data Bundle V1.0. This data set includes 3-micron spectra of asteroids and other small bodies taken by Andy Rivkin and collaborators.

Keywords: Martian satellites, Asteroids, Spectroscopy, Infrared spectroscopy
Rhea SPC Shape Model and Assessment Products Bundle. This bundle contains the first shape model for the Saturnian moon Rhea submitted to the PDS, along with quality assessment data. The data is provided in multiple formats.

Keywords: Saturnian satellites
Dione SPC Shape Model and Assessment Products Bundle. This bundle contains global and regional topography of Saturn's moon Dione, as well as photometric data for each of the regional models. Data products were generated using the Gaskell Stereophotoclinometry (SPC) software suite with images from the Cassini mission to Saturn. The global model is an update to the archived "Gaskell Dione Shape Model", and is generated with more images. In addition to the topographic models, we also provide assessment data to understand the uncertainty of the models.

Keywords: Saturnian satellites
Tethys SPC Shape Model and Assessment Products Bundle. This bundle contains global and regional topography of Saturn's moon Tethys, as well as photometric data for each of the regional models. Data products were generated using the Gaskell Stereophotoclinometry (SPC) software suite with images from the Cassini mission to Saturn. The global model is an update to the archived "Gaskell Tethys Shape Model", and is generated with more images and has higher resolution topography in some locations. In addition to the topographic models, we also provide assessment data to understand the uncertainty of the models.

Keywords: Saturnian satellites
Mimas SPC Shape Model and Assessment Products Bundle. This bundle contains a shape model for the Saturnian moon Mimas, along with quality assessment data. The global model is an update to the archived "Gaskell Mimas Shape Model", and is generated with more images and has higher resolution topography in some locations. The data is provided in multiple formats.

Keywords: Saturnian satellites
Galileo NIMS Radiance Point Spectra of Gaspra. This bundle contains radiometrically corrected point spectra of asteroid 951 Gaspra as acquired by the Galileo spacecraft Near Infrared Mapping Spectrometer (NIMS) on October 29, 1991. They record the spectra collected as the Galileo spacecraft approached the target asteroid. These data are products of the calibration of the raw data number files gap015tn.qub, gap035tn.qub, gap036qtn.qub, gap037tn.qub, and gap038tn.qub (DATA SET ID ='GO-A-NIMS-3 TUBE-V1.0') with calibration factors acquired during the first Earth/Moon encounter of the Galileo mission. These raw data .qub files are archived in the Imaging Node of the NASA Planetary Data System (PDS). The calibrated spectra consist of radiance measurements for wavelengths between 0.7 - 5.2 micrometers.

Keywords: Flyby missions, Asteroids, Infrared spectroscopy
Stooke small bodies maps. This bundle contains maps of small solar system bodies which have been prepared by Philip Stooke of the University of Western Ontario. It includes 270 map sheets of six asteroids, five planetary satellites, and three comets, all prepared from spacecraft images.

Keywords: Near-Earth objects, CCD photometry, Martian satellites, Asteroids, Short period comets, Saturnian satellites, Jovian satellites
Galileo NIMS Radiance Point Spectra of Ida and Dactyl. This bundle contains radiometrically corrected point spectra of asteroid 243 Ida and a spectrum of the asteroid satellite Dactyl (Ida I) as acquired by the Galileo spacecraft Near Infrared Mapping Spectrometer (NIMS) on August 28, 1993. They record the spectra collected as the Galileo spacecraft approached the 243 Ida system. These data are products of the calibration of the raw data number files idu002tn.qub, idu005tn.qub, idu006tn.qub, idu007tn.qub, idu019tn.qub, idu020tn.qub, idu022tn.qub, idu028tn.qub, idu032tn.qub, idu033tn.qub, and idu035tn.qub (DATA SET ID ='GO-A-NIMS-3-TUBE-V1.0') with calibration factors acquired during the Jovian tour of the Galileo mission. These raw data .qub files are archived in the Imaging Node of the NASA Planetary Data System (PDS). The calibrated spectra consist of radiance and incidence/flux measurements for wavelengths between 0.7 - 5.2 micrometers.

Keywords: Asteroid satellites, Flyby missions, Asteroids, Infrared spectroscopy
Stooke small bodies shape models. This data set contains Philip Stooke shape models for 243 Ida, 253 Mathilde, 951 Gaspra, comet Halley, J5 Amalthea, J14 Thebe, N7 Larissa, N8 Proteus, S10 Janus, S11 Epimetheus, S16 Prometheus, and S17 Pandora, based on optical data from the NEAR, Galileo, Giotto, Vega 1, Vega 2, and Voyager missions.

Keywords: CCD photometry, Asteroids, Neptunian satellites, Comet Halley, Saturnian satellites, Jovian satellites
The NEAR Multi-spectral Imager (MSI) Instrument Bundle. This bundle contains all the calibrated and raw data collected from the MSI instrument during the NEAR mission, as well as a documentation collection, a calibration collection, and a browse product collection.

Keywords: Near-Earth objects, Flyby missions, Asteroids, Eros
Interferometric Detection and Orbit Modeling of the Subcomponent in the Hot-dust System κ Tuc A: A Low-mass Star on an Eccentric Orbit in a Hierarchical-quintuple System. The system κ Tuc A is part of a hierarchical-quintuple system and is a prime target for studies of hot-exozodiacal dust, because a time-variable near-infrared excess has been detected. We observed the system with the Multi Aperture mid-Infrared Spectroscopic Experiment (MATISSE) and GRAVITY at the Very Large Telescope Interferometer, and detected the stellar companion to the primary κ Tuc Aa that was previously inferred by astrometry, κ Tuc Ab. Its L-band flux ratio to the primary is 1.32% and its signature in the MATISSE closure phases is mostly smaller than ±2°, which makes κ Tuc Ab the highest-contrast companion ever detected with MATISSE closure phases. We verified with GRAVITY that relative astrometry with milliarcsecond precision can be retrieved from MATISSE closure phases. Using multiple epochs of observations, we obtain a full orbital solution for κ Tuc Ab. Its orbit has an eccentricity of 0.94 and a semimajor axis of 4.8 au. The orbit of κ Tuc Ab and the orbit of the wider separation companion κ Tuc B are mutually inclined. Based on the measured flux ratio of κ Tuc Ab to Aa and their dynamical mass, we estimate the spectral type of κ Tuc Ab to be M3.5 V to M4.5 V. While the then unknown star κ Tuc Ab might have caused the putative detection of hot-exozodiacal dust around κ Tuc Aa in 2012 and 2014, this cannot be for the detection in 2019, giving rise to an intriguing system architecture. This motivates studies investigating the interplay of the low-mass star on an eccentric orbit, the hot-exozodiacal dust, and a possible planetesimal reservoir.

Keywords: M dwarf stars, Multiple stars, Elliptical orbits, Exozodiacal dust, Long baseline interferometry
A Comparative Study of Time on Mars with Lunar and Terrestrial Clocks. As space exploration extends into cislunar space and further toward Mars, understanding the relativistic effects on clocks on Mars—particularly in relation to multibody gravitational influences—becomes increasingly important for accurate clock synchronization. This study estimates clock rates on Mars and compares them to those on the Moon and Earth. We find that, on average, clocks on Mars tick faster than those on the Earth's geoid by 477 μs day−1, with a variation of 226 μs day−1 over a Martian year. Additionally, there is an amplitude modulation of approximately 40 μs day−1 over seven synodic cycles. We also introduce a formalism that includes the effects of solar tides on the Earth─Moon system for predicting clock rates on the Moon and Mars more accurately when compared to using only Keplerian orbit approximations. Our analysis quantifies the relativistic proper-time offsets among Martian, lunar, and terrestrial clocks, highlighting important implications for mission planning and the implementation of timekeeping systems on Mars.

Keywords: Relativity
Methanol Emission Tracing Ice Chemistry and Dust Evolution in the TW Hya Protoplanetary Disk. Methanol (CH3OH) ice is abundant in space and is a key feedstock for seeding chemical complexity in interstellar and circumstellar environments. Despite its ubiquity, gas-phase methanol has only been detected in one disk around a solar-type star to date, TW Hya. Here, we present new high-sensitivity (∼1 mJy beam−1) observations of TW Hya with the Atacama Large Millimeter/submillimeter Array that detect four individual transitions of gas-phase methanol spanning upper level energies from 17 to 38 K. We confirm the presence of gas-phase methanol in the lukewarm molecular layer of the disk ( 35.9−10.6+25.9  K) and with a disk-integrated column density of  1.8−0.5+1.3×1012 cm−2. A radially resolved analysis suggests that the gas-phase methanol is centrally compact, peaking within the spatial extent of the mm-sized dust grains (≲80 au). Static gas-grain chemical disk models confirm photodesorption as an important mechanism releasing methanol into the gas phase, with the column density further boosted by the inclusion of grain-surface chemistry, reactive desorption, and an increase in dust-grain surface area assuming fractal grains. However, no model can fully reproduce the observed column density nor the radial distribution, and we suggest that the inclusion of dynamic processes such as vertical mixing and radial drift would be required to do so. Our results demonstrate that the abundance and distribution of the precursors for complex chemistry in the planet-forming regions around solar-type stars is ultimately controlled by the interplay of grain surface chemistry coupled with the evolution of dust in their disks.

Keywords: Interstellar molecules, Protoplanetary disks, Planet formation, Astrochemistry
Evolution of the Accretion Rate of Young Intermediate-mass Stars: Implications for Disk Evolution and Planet Formation. This work presents a study of the evolution of the stellar accretion rates of pre-main-sequence intermediate-mass stars. We compare the accretion rate of the younger intermediate-mass T Tauri stars (IMTTSs) with the older Herbig stars into which they evolve. We find that the median accretion rate of IMTTSs (1.2 × 10−8 M⊙ yr−1) is significantly lower than that of Herbig stars (1.9 × 10−7 M⊙ yr−1). This increase stands in stark contrast with canonical models of disk evolution that predict that the stellar accretion rate declines with age. We put forward a physically plausible scenario that accounts for the systematic increase of stellar accretion based on the increase of the effective temperature of the stars as they evolve towards the zero-age main sequence. For example, the temperature of a 2M⊙ star will increase from 4900 K in the IMTTS phase to 9100 K during the Herbig phase. Thus, the luminosity of the far-ultraviolet (FUV) radiation will increase by orders of magnitude. We propose that this increase drives a higher stellar accretion rate. The scenario we propose to account for the increase in the stellar accretion rate solves the lifetime problem for Herbig disks because the increasing stellar accretion rates require lower initial disk masses to account for present-day disk masses. This work highlights the importance of the role FUV radiation has in driving the accretion rate, predicts a large population of pre-main-sequence nonaccreting A stars, and has implications for interpreting disk morphologies that may serve as signposts of embedded gas giant planets in Herbig disks.

Keywords: Herbig Ae/Be stars, Intermediate-type stars, T Tauri stars, Protoplanetary disks, Circumstellar disks, Stellar accretion disks
SCExAO/CHARIS and Gaia Direct Imaging and Astrometric Discovery of a Superjovian Planet 3─4 λ/D from the Accelerating Star HIP 54515. We present the discovery of a superjovian planet around the young A5 star HIP 54515, detected using precision astrometry from the Hipparcos Gaia Catalogue of Accelerations and high-contrast imaging with SCExAO/CHARIS from the recently commenced OASIS program. SCExAO/CHARIS detects HIP 54515 b in five epochs 0 .″ 145─0 .″ 192 from the star (∼3─4 λ/D at 1.65 μm), exhibiting clockwise orbital motion. HIP 54515 b lies near the M/L transition with a luminosity of log(L/L⊙) ∼−3.52 ± 0.03. Dynamical modeling constrains its mass and mass ratio to be  17.7−4.9+7.6  MJup and  0.0090−0.0024+0.0036  and favors a ∼25 au semimajor axis. HIP 54515 b adds to a growing list of superjovian planets with moderate eccentricities (e ≍ 0.4). Now, the third planet discovered from surveys combining high-contrast extreme adaptive optics imaging with precision astrometry, HIP 54515 b, should help improve empirical constraints on the luminosity evolution and eccentricity distribution of the most massive planets. It may also provide a key technical test of the Roman Space Telescope Coronagraph Instrument's performance in the low stellar flux, small angular separation limit, and a demonstration of its ability to yield constrainable planet spectral properties. *Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.

Keywords: Orbits, Adaptive optics, Extrasolar gaseous planets, Exoplanet detection methods, Exoplanet atmospheres
On the Interpretation of Velocity Residuals in Protoplanetary Disks. We present a first-order analytical model for line-of-sight velocity residuals, defined as the difference between observed velocities and those predicted by a fiducial model, assuming a flared, nearly axisymmetric disk with the perturbations in disk surface height δh(r), inclination δi(r), and position angle δPA(r). Introducing projection─deprojection mapping between sky-plane and disk-frame coordinates, we demonstrate that the normalized velocity residuals exhibit Fourier components up to the third harmonic ( sin3ϕ  and  cos3ϕ ). Moreover, we show that the radial profiles of δh(r), δi(r), and δPA(r) can be uniquely recovered from the data by solving a linear inverse problem. For comparison, we highlight factors that are not considered in previous models. We also outline how our framework can be extended beyond the first-order residuals and applied to additional observables, such as line intensities and widths.

Keywords: Protoplanetary disks
Accounting for Transit Timing Detectability: Biases in Planetary Radius and Orbital Period. Transit Timing Variations (TTVs) are deviations from the time an observer would expect to see an exoplanet transit its host star. In multiplanetary systems, significant TTVs may indicate the presence of another body in the system gravitationally interacting with the transiting exoplanet. T. Holczer et al. catalog 2599 Kepler Objects of Interest (KOIs) and provide a statistical analysis of their TTVs for candidates that have transited at least seven times. However, this conservative limit on the number of transits neglects long-period KOIs. Therefore, we extend the statistical analysis performed by T. Holczer et al. to the population of KOIs that have between three and six transits. We identify six KOIs, three of which have Kepler names (Kepler─103 c, Kepler─90 g, and Kepler─1662 c), with significant TTV signals that were originally overlooked by T. Holczer et al. Additionally, we search for trends regarding the planetary radius and orbital period of KOIs with significant TTVs. Through a survival analysis, we determine that planets with shorter orbital periods require larger TTV signals to be detected compared to longer period planets, regardless of planetary size. Uncovering trends in TTV statistics such as this one will provide targets for future forward modeling of planetary architectures.

Keywords: Exoplanet dynamics, Exoplanet detection methods, Transit timing variation method
A Combined Photometric and Polarimetric Study of L1578 and L1607: Dust Properties and Magnetic Field Structures. We present a combined photometric and R-band polarimetric study of the Lynds dark clouds L1578 and L1607 to investigate their physical properties—such as distance, column density, and dust temperature—and to examine the morphology of their magnetic fields in the optical regime. Based on stellar radial density profiles, we estimate distances of 1043 ± 36 pc (L1578) and 938 ± 49 pc (L1607), which are compared to the distances obtained from the 3D dust-reddening maps of the sky, and the results are found to be consistent. Extinction mapping using the PNICER method yields average visual extinctions of ∼1.7 and ∼1.4 mag, with corresponding hydrogen column densities of ∼1.6 × 1021 cm−2 and ∼1.3 × 1021 cm−2 for L1578 and L1607, respectively. From Herschel SPIRE observations, we derive mean dust temperatures of 13.5 K (L1578) and 14.0 K (L1607), and column densities consistent with extinction-based estimates. For L1578, an elliptical fit to the central clump yields a position angle of ∼−35° and a mass of ∼35 M⊙; the virial parameter is found to lie in the range 4.8─5.9, indicating a gravitationally unbound structure. Polarimetric observations show mean degrees of polarization of 3.36% ± 0.05% (L1578) and 2.84% ± 0.06% (L1607), with well-aligned polarization angles (∼149° and ∼155°, respectively). The polarization vector maps exhibit ordered magnetic fields in the cloud envelopes, closely aligned with the Galactic plane. L1578 shows no observational evidence of ongoing star formation, while further investigation is needed to assess the star-forming status of L1607.

Keywords: Stellar kinematics, Star forming regions, Molecular clouds, Interstellar dust extinction, Polarimetry, Extinction, Photometry, Magnetic fields
Unveiling Basalt Distribution of Lunar Cryptomaria from Gravity and Topography when Considering the Effect of Surface Cover-layer and Density Correction. The cryptomaria preserves critical evidence of early lunar volcanism and thermal evolution, offering key constraints on the Moon's internal heat flow and mantle melting processes. To better constrain the distribution of cryptomaria basalt, we present a three-layer density-structure model incorporating contributions from a surface cover-layer, basalt, and underlying anorthositic crust. First, we explicitly account for the effect of the surface cover-layer. Second, to realistically capture nonlinear variation within the anorthositic crust, we apply a Gaussian correction term to adjust the nonlinear component, thereby more accurately modeling density variation. Finally, by utilizing the effective density spectrum derived from Gravity Recovery and Interior Laboratory gravity and Lunar Reconnaissance Orbiter Laser Altimeter topographic data, we estimate the global average thickness of cryptomaria basalts to be approximately 0.54 km, which is notably greater than previous estimates (∼0.40 km) that did not account for the presence of a surface cover-layer and the Gaussian correction. Furthermore, based on the revised thickness distribution, we estimate the total volume of cryptomaria to be ∼4.7 × 106 km3, a value comparable to that of the visible mare, highlighting the significant contribution of buried basaltic deposits to the Moon's volcanic activity. Our findings suggest that the traditional model can lead to an underestimation of basalt thickness and volume. The result further indicates a modest negative correlation between basalt and crustal thickness, suggesting that variations in crust alone cannot fully account for the distribution. This finding implies that additional factors—such as mantle thermal heterogeneity and tectonic processes—may play a substantial role in controlling magma emplacement.

Keywords: Lunar maria, The Moon, Lunar composition
FALCO: Foundation Model of Astronomical Light Curves for Time Domain Astronomy. Implementation and Applications on Kepler Data. Time-domain surveys have advanced astronomical research by revealing diverse variable phenomena, from stellar flares to transient events. The scale and complexity of survey data, along with the demand for rapid classification, present significant challenges for analysis. While machine learning offers solutions, most existing models are tailored to single tasks, struggle to generalize, and depend heavily on large, accurately labeled datasets. This paper presents an initial implementation of FALCO, a foundation model trained on Kepler light curves via self-supervised learning using a Transformer-based architecture. The model has been evaluated on Kepler data across three distinct light-curve analysis tasks, and it demonstrates robust performance in all tasks, achieving an accuracy of 95% for stellar variability classification across eight classes, an overall RMSE of 0.1305 dex in surface gravity estimation (with significantly improved precision of RMSE &lt; 0.08 dex at the low-gravity end where log g &lt; 1, and 0.02 dex near log g ≍ 3), and a precision of 87% in flare identification. These results highlight the versatility of the foundation model in extracting generalizable representations from light curves, enabling easy adaptation to diverse tasks and making it a promising tool for time-domain analysis. Further analysis of model scaling and input light-curve sequence length reveals that larger models and longer input sequences improve performance. We have also applied the model to produce a comprehensive catalog of surface gravity (log g) measurements for 179,732 Kepler stellar targets, using their light curves.

Keywords: Light curve classification , Light curves, Surface gravity, Astronomy data analysis, Stellar flares, Optical flares, Time series analysis
Tidally Torn: Why the Most Common Stars May Lack Large, Habitable-zone Moons. Earth-like planets in the habitable zone (HZ) of M dwarfs have recently been targeted in the search for exomoons. We study the stability and lifetime of large (Luna-like) moons, accounting for the effects of three-body interactions and tidal forces using the N-body simulator rebound and its extension library reboundx. We find that those moons have a notably different likelihood of existence (and, by implication, observability). Large moons orbiting Earth-like planets in the HZs of M4 and M2 dwarfs become unstable well before 107 and 108 yr, respectively, and in most cases, those orbiting M0 dwarfs become unstable in much less than 109 yr. We conclude that HZ planets orbiting M dwarfs are unlikely to harbor large moons, thus affecting the total number of possible moons in our galaxy and the Universe at large. Since moons may help enhance the habitability of their host planet, besides being possibly habitable themselves, these results may have notable implications for exolife, and should also be considered when seeking solutions to the Drake equation and the Fermi paradox.

Keywords: Exoplanet dynamics, Exoplanet tides, Habitable zone