Sazuna/UAT_keywords huggingface dataset:
Encounters between M33 and Present-day M31 Satellites Hint at a Previous Group Accretion. This work investigates whether two known Andromeda (M31) satellites, Pisces (LGS 3) and Andromeda XVI (And XVI), have interacted with M33, M31's most massive satellite. ΛCDM predictions imply a handful of satellite galaxies around M33, yet few M33 satellites have been found and confirmed despite its high mass. We use proper motions combined with backward orbit integration in a semianalytic potential to constrain plausible interaction scenarios for Pisces and And XVI. Both dwarfs are currently M31 satellites, defined as being inside its virial radius. However, our results show that, in our fiducial mass models, 42% (And XVI) and 60% (Pisces) of dwarf orbits support that they were previously satellites of M33 (i.e., once inside its virial radius). Both dwarfs had flyby encounters with M33 at relative velocities greater than M33's escape speed within the past 1─2 Gyr. In over 70% of orbits, Pisces and And XVI also had a close approach with each other post-M33 interaction and share an orbital plane, suggesting possible past group accretion. We explore a range of mass combinations for M31 and M33, finding that these primarily regulate the likelihood that the dwarfs were satellites of M33 in the past, while upholding conclusions of recent flybys about M33. These close interactions provide new evidence for past satellite exchange and/or group infall scenarios between M31 and M33. Such interactions also affect comparisons to observational surveys that define satellites primarily by their distance relative to host galaxies.

Keywords: Local Group, Galaxy dynamics, Dwarf galaxies
Glimmers in the Cosmic Dawn. III. On the Photometrically Determined Black Hole Mass to Stellar Mass Relation across Cosmic Time. We present the results from performing spectral energy distribution (SED) fitting on 121 variable active galactic nuclei (AGN) candidates in the Hubble Ultra Deep Field using photometry from both the Hubble Space Telescope and the James Webb Space Telescope (JWST) covering 0.2─4.8 μm. We designed a bespoke SED fitting code, which decomposes the total SED into its stellar and AGN contributions. Our SED fitting retrieves a significant contribution to the total SED from an AGN template for 26 of our variable sources with 0 &lt; z &lt; 7. We leverage the model AGN spectrum to estimate black hole masses (MBH) using the measured luminosity at 5100 Å and local empirical calibrations. Common with recently discovered JWST broad-line AGN, we observe a trend in the MBH─M* plane where low-redshift sources have MBH that agrees with local relations while high-redshift sources have increasingly overmassive black holes with respect to the stellar mass (M*) of their host galaxies. Within our sample, we identify two IMBH candidates hosted by dwarf galaxies at z &lt; 1 featuring overmassive black holes in the MBH─M* plane, similarly to our high-redshift sources. Finally, our SED fitter successfully retrieves the AGN nature of one source at z &gt; 6. This object has zphot = 6.74, and we estimate a lower limit on its black hole mass of  log10(MBH/M⊙)&gt;7.36 . *This research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with GO programs 1563, 12498, 17073. This work is also based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with GTO programs 1180, 1181, 1210, 1286 and GO programs 1895, 1963, 3215.

Keywords: Active galactic nuclei, High-redshift galaxies, Galaxy evolution
SN 2021aaev: A Hydrogen-rich Superluminous Supernova with Early Flash and Long-lived Circumstellar Interaction in an Unusual Host Environment. We present photometric and spectroscopic observations of SN 2021aaev, a hydrogen-rich, superluminous supernova with persistent (at least ∼100 days) narrow Balmer lines (SLSN-IIn) at redshift z = 0.1557. SN 2021aaev rose over 28.1 ± 1.0 rest-frame days after explosion, reaching a peak absolute magnitude of −21.46 ± 0.01 in the ATLAS o band. The prepeak spectra resemble those of typical Type IIn SNe with flash-ionization features arising from the interaction with a dense, confined circumstellar medium (CSM), albeit the flash timescale is longer than usual (&gt;20 days). Postpeak, the narrow emission lines evolve slowly, and the absence of ejecta features indicates strong deceleration by the CSM. The total radiated energy (about 1.41 × 1051 erg) is possibly explained by a low-mass (1─2 M⊙) ejecta ploughing into a massive (9─19 M⊙), extended (outer radius &gt;1 × 1016 cm) H-rich CSM, or alternatively by magnetar-powered models. Interestingly, the host environment consists of a spiral galaxy with a red substructure in the southeastern part, and the SN's exact location coincides with this quiescent red region (star formation rate  =0.02−0.02+0.13M⊙  yr−1). Given the atypical environment and the obscuring effect of the massive CSM, a thermonuclear (Type Ia-CSM) origin cannot be ruled out. Altogether, SN 2021aaev is a compelling case to study the diversity of SLSN-IIn features and their host environments.

Keywords: Core-collapse supernovae, Type II supernovae, Massive stars, Stellar mass loss, Circumstellar matter, Supernovae
Lyα Intensity Mapping in HETDEX: Galaxy-Lyα Intensity Cross-power Spectrum. We present a measurement of the Lyα intensity mapping power spectrum from the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). We measure the cross-power spectrum of the Lyα intensity and Lyα-emitting galaxies (LAEs) in a redshift range of 1.9 ≤ z ≤ 3.5. We calculate the intensity from HETDEX spectra that do not contain any detected LAEs above a signal-to-noise ratio of 5.5. To produce a power spectrum model and its covariance matrix, we simulate the data using lognormal mocks for the LAE catalog and Lyα intensity in redshift space. The simulations include the HETDEX sensitivity, selection function, and mask. The measurements yield the product of the LAE bias, the intensity bias, the mean intensity of undetected sources, and the ratio of the actual and fiducial redshift-space distortion parameters,  bgbI&lt;I&gt;F̄RSD/F̄RSDfid= (6.7 ± 3.1), (11.7 ± 1.4), and (8.3 ± 1.5) × 10−22 erg s−1 cm−2 arcsec−2 Å−1 in three redshift bins centered at  z̄=2.1 , 2.6, and 3.2, respectively. The results are reasonably consistent with cosmological hydrodynamical simulations that include Lyα radiative transfer. They are, however, significantly smaller than previous results from cross-correlations of quasars with Lyα intensity. These results demonstrate the statistical power of HETDEX for Lyα intensity mapping and pave the way for a more comprehensive analysis. They will also be useful for constraining models of Lyα emission from galaxies used in modern cosmological simulations of galaxy formation and evolution.

Keywords: Lyman-alpha galaxies, Observational cosmology, Large-scale structure of the universe
The Effects of Non-ideal Mixing in Planetary Magma Oceans and Atmospheres. Sub-Neptunes with hydrogen-rich envelopes are expected to sustain long-lived magma oceans that continuously exchange volatiles with their overlying atmospheres. Capturing these interactions is key to understanding the chemical evolution and present-day diversity of sub-Neptunes, super-Earths, and terrestrial planets, particularly in light of new JWST observations and upcoming missions. Recent advances in both geochemistry and astrophysics now allow for the integration of experimental constraints and thermodynamic models across melt, metal, and gas phases. Here we extend a global chemical equilibrium model to include non-ideal behavior in all three phases. Our framework combines fugacity corrections for gas species with activity coefficients for silicate and metal species, enabling a fully coupled description of volatile partitioning. We show that for planetary embryos (0.5 M⊕ at 2350 K), non-ideality introduces only modest corrections to atmosphere─magma ocean interface (AMOI) pressures, volatile inventories, and interior compositions. In contrast, for sub-Neptunes with higher temperatures (≍3000 K) and pressures, non-ideal effects are more pronounced, though still modest in absolute terms—typically within 20% and at most a factor of 2. Including activity and fugacity coefficients simultaneously increases the AMOI pressure, and enhances water retention in the mantle and the envelope. Our results demonstrate that non-ideality must be treated globally: applying corrections to only one phase leads to incomplete or even misleading trends. These findings highlight the importance of self-consistent global thermodynamic treatments for interpreting atmospheric spectra and interior structures of sub-Neptunes and super-Earths.

Keywords: Exoplanet structure, Exoplanet atmospheric composition , Exoplanet atmospheric structure
Dynamics of the Coronal Magnetic Field in the 2022 October 2 X-class Flare. Solar flares are driven by the release of free magnetic energy and are often associated with the restructurization of the magnetic field topology. Yet, observations of the evolving magnetic field in the flaring volume are limited to very few cases, including the 2017 September 10 X8.2 limb flare; thus, a verification of whether a similar evolution takes place in other solar flares is needed. Here, we report one more: the 2022 October 2 X1.1-class solar flare, seen on the disk, whose microwave data permit mapping the magnetic field over the flaring source and tracking the magnetic field evolution over the course of the flare. We find that the coronal magnetic field shows a prominent decay with a rate up to 10 G s−1 in several (above the) looptop locations. The magnetic field is also confidently measured at the loop legs and the bottom part of the erupting filament. Prominent acceleration of electrons is detected where the magnetic field decays. We develop 3D models of the flare, whose magnetic field shows resemblance to and also deviation from the magnetic field inferred from the microwave data. This study confirms that the coronal magnetic field decays during the rise phase of the solar flare. The amount of released magnetic energy is sufficient to support other components of the flare energy.

Keywords: Non-thermal radiation sources, Solar radio emission, Solar flares, Solar magnetic fields
ATOMS-QUARKS Survey: Inflow and Infall in Massive Protocluster G318.049+00.086— Evidence of Competitive Accretion. We present a gas kinematic study of the massive protocluster G318.049+00.086. The protocluster is reported to contain 12 prestellar core candidates and four protostellar cores. Filamentary structures are identified using the 1.3 mm dust continuum map, with four of them converging into a dense central region, forming a hub-filament system. High velocity gradients (10─20 km s−1 pc−1) derived from position─velocity analysis of H13CO+ emission along three of those filaments are suggestive of mass inflow onto the central hub. A mass inflow rate higher than 103 M⊙ Myr−1 along the filaments indicates that the central hub is capable of forming massive star(s). Investigation of H13CO+ and CCH spectral profiles revealed the majority of the cores having the characteristic blue asymmetric line profiles, a typical signature of gravitational collapse. The remaining few cores showed red asymmetric profiles, indicative of gas expansion. Also, the derived mass infall rates for the protostellar cores in the hub region are significantly higher in comparison to those located along the filaments. The mass─radius relation of the cores revealed that the cores with red profiles reside in the massive star formation regime. However, the global velocity gradient along the filaments suggests that these particular cores are losing material to the hub. Our results support a competitive accretion scenario of massive star formation where gas is expected to be funnelled from less gravitationally dominant cores to the cores located at the gravitationally favorable position.

Keywords: Interstellar filaments, Stellar kinematics, Protoclusters, Star forming regions, Molecular clouds, Interstellar medium, Radio astronomy
TTC: Transformer-based TDE Classifier for the Wide Field Survey Telescope (WFST). We propose the Transformer-based Tidal disruption events (TDE) Classifier (TTC), specifically designed to operate effectively with both real-time alert streams and archival data of the Wide Field Survey Telescope (WFST). It aims to minimize the reliance on external catalogs and find TDE candidates from pure light curves, which is more suitable for finding TDEs in faint and distant galaxies. TTC consists of two key modules that can work independently: (1) A light-curve parametric fitting module and (2) a Transformer (Mgformer) based classification network. The training of the latter module and the evaluations for each of the modules utilize a light-curve dataset of 7413 spectroscopically classified transients from the Zwicky Transient Facility (ZTF). The Mgformer-based module is superior in performance and flexibility. Its representative recall and precision values are 0.79 and 0.76, respectively, and can be modified by adjusting the threshold. It can also efficiently find TDE candidates within 30 days from the first detection. For comparison, the parametric fitting module yields values of 0.72 and 0.40, respectively, while it is &gt;10 times faster in average speed. Hence, the setup of modules allows a trade-off between performance and time, as well as precision and recall. TTC has successfully picked out all spectroscopically identified TDEs among ZTF transients in a real-time classification test, and selected ∼20 TDE candidates in the deep field survey data of WFST. The discovery rate will greatly increase once the differential database for the wide-field survey is ready.

Keywords: Light curve classification , Tidal disruption, Transient sources, Wide-field telescopes
First Detection of γ-Ray Emission from the Compact Symmetric Object JVAS J1311+1658. We report the first detection of γ-ray emission from the young radio galaxy JVAS J1311+1658, classified as a compact symmetric object (CSO). This detection is characterized by a recent GeV γ-ray flare identified in Fermi-Large Area Telescope data during MJD 60032.6─60132.6, with a γ-ray source detected at a significance level of ∼6.2σ. The average 0.1─300 GeV flux is measured to be (1.6 ± 0.6) × 10−8 ph cm−2 s−1, with a photon spectral index of Γ = 2.15 ± 0.185. We find that a radiative model of the radio lobes significantly underestimates the observed γ-ray emission. The strong flux and short-term variability over ∼100 days suggest that the emission likely originates from newly launched subkiloparsec-scale jets at the core. This detection provides a unique window into the extreme environments and early-stage jet activity of young radio galaxies, offering insights into their initial evolution and the formation of relativistic jets in the earliest phases of galaxy growth.

Keywords: Gamma-ray sources, Relativistic jets, Active galactic nuclei, Radio galaxies
A Black Hole Envelope Interpretation for Cosmological Demographics of Little Red Dots. Little Red Dots (LRDs) newly discovered with JWST are active galactic nuclei (AGNs) that may represent black hole (BH) growth at the earliest cosmic epochs. These sources show puzzling features unlike typical AGNs, including red optical continua, weak hot-dust emission, and a lack of detectable X-rays. Previously, LRDs have often been interpreted as dust-reddened AGNs, leading to severe inconsistencies with the luminosity and BH mass densities inferred for previously known AGNs over 0 &lt; z &lt; 5. The BH envelope (BHE) model has been proposed to explain these characteristics, in which an accreting BH is enshrouded by a dense, optically thick gaseous envelope. In this article, we reanalyze the spectral energy distributions of ∼400 photometric LRDs in the COSMOS-Web survey using the BHE model and reassess their implications for cosmological BH evolution. We find that the optical─near-IR spectra of LRDs are well reproduced by blackbody emission with an effective temperature of 4000─6000 K. Within the BHE framework, the inferred bolometric luminosities decrease by ≳1─2 orders of magnitude compared to assumptions for dust-reddened AGNs. As a result, the revised luminosity function, BH accretion density, and BH mass function become consistent with those of AGNs at z &lt; 5. The stellar masses of LRD hosts are estimated by attributing the UV excesses to star formation. Although the resulting MBH/M⋆ ratio remains higher than the local empirical value, the excess is modest. Overall, the BHE model not only resolves the spectral features of LRDs but also brings their statistical properties into agreement with the broader cosmological BH population.

Keywords: Supermassive black holes, Galaxy formation, Active galactic nuclei
The Effect of Planetary Rotation Period on Clouds in a Global Climate Model with a Bin Microphysics Scheme. Clouds are the largest source of uncertainty in climate simulations. For exoplanets, cloud simulation is particularly challenging because of the lack of observational data to tune parameterized cloud models. Here we apply Community Aerosol and Radiation Model for Atmospheres (CARMA), a size-resolved bin cloud microphysics model, to the atmospheric global climate model Community Atmosphere Model (CAM6) and simulate exoplanets with a range of planetary rotation rates. CARMA produces fewer liquid clouds than the native CAM6 parameterized cloud microphysics scheme (Morrison─Gettelman two-moment microphysics, MG), more ice clouds, and a significantly different ice cloud size distribution. Overall, this leads to a decrease in the magnitude of the net CRE by 4─10 W m−2, which is unlikely to change the determination of habitability from a climate perspective in most cases. The difference in ice cloud size distribution is likely to strongly affect transmission spectral retrievals. Our work confirms that the MG parameterized cloud microphysics scheme can produce reasonable climate simulation when extrapolated to some exoplanet contexts and highlights the value of resolved cloud microphysics for evaluating parameterized schemes and for interpreting observations.

Keywords: Habitable planets, Atmospheric clouds
ALMA [C I] Image of the Circumnuclear Disk of the Milky Way: Inflowing Low-density Molecular Gas. We present Atacama Large Millimeter/submillimeter Array [C I] 3P1─3P0 imaging of the central 6.6 × 4.2 pc2 region of the Galaxy encompassing the circumnuclear disk (CND). The data reveal low-density ( nH2∼103 cm−3) molecular gas with inward motion, widespread both inside and outside the CND. The normalized [C I] to CS 7─6 intensity difference decreases inwardly from R = 4 pc to 1.7 pc and azimuthally along the CND's rotation, likely tracing paths of low-density gas inflow. By projecting spaxels into orbital coordinates assuming a velocity field model, we identify four kinematic features: a pair of spiral outer streamers toward the CND, inner streamers extending to 0.5 pc from Sgr A*, an outer disk at R ∼ 3─6 pc, and the rotating ring at R = 2 pc. P─P─V correlation between the inner streamers and H42α indicates gas supply to the mini-spiral through the western arc (WA) and northern arm (NA). The total inflowing mass is 1.5 × 104 M⊙, 1.7 times the mass of the rotating ring. The identified flows can be organized into two main pathways connecting the CND exterior and interior: "WA flow" feeding the mini-spiral WA via the CND, and "NA flow" bypassing the purely rotating orbit. The inflow rate along the former is approximately constant (0.1─0.16 M⊙ yr−1), implying a CND dwelling time comparable to its orbital period and supporting the CND's transient nature. We also identify two [C I]-bright clumps (CBCs) lacking dense-gas counterparts near the contact point between the northern outer streamer and the CND. Apparently intact against tidal disruption despite subcritical densities, the CBCs may represent a chemically young phase shortly after formation in colliding flows.

Keywords: Galaxy circumnuclear disk, Galactic center, Molecular clouds
TransFit-CSM: A Fast, Physically Consistent Framework for Interaction-powered Transients. We introduce TransFit-CSM, a fast and physically consistent framework for modeling interaction-powered transients. The method self-consistently couples the ejecta─circumstellar medium (CSM) shock dynamics to radiative diffusion from a moving heating boundary that is tied to the shocks. In this way, both the photon escape path and the effective diffusion time evolve with radius and time. We numerically solve the mass─momentum equations for the forward and reverse shocks together with the diffusion equation in the unshocked CSM. As a result, TransFit-CSM reproduces the canonical sequence of an early dark phase, a diffusion-mediated rise and peak, and a post-interaction cooling tail, and it clarifies why Arnett-like peak rules break down in optically thick CSM. The framework is Bayesian-ready and constrains physical parameters of the ejecta and CSM from bolometric or joint multiband light curves. Applications to SN 2006gy and SN 2010jl demonstrate accurate fits and physically interpretable posteriors. These fits highlight the dominant role of pre-supernova mass loss in shaping the observables. Because it is both computationally efficient and physically grounded, TransFit-CSM bridges simple analytic prescriptions and radiation-hydrodynamic simulations. This capability enables population-level inference for current and upcoming time-domain surveys.

Keywords: Circumstellar matter, Supernovae, Core-collapse supernovae, Stellar mass loss
Constraining the Effects of Pre- and Post-accretionary Processes on Ryugu Insoluble Organic Matter. Asteroidal and cometary fragments have been indicated as possible sources of the building blocks of life for the early Earth. Samples returned from the asteroid Ryugu are uncontaminated and contain organic matter. Such samples enable an investigation of the processes that formed and altered extraterrestrial organic matter. Here, the FTIR and Raman responses of insoluble organic matter (IOM) isolated from Ryugu particles and carbonaceous chondrites are reported. Several relationships were observed: (1) a strong positive correlation of CH2/CH3 plotted against aliphatics/C=C; (2) a strong negative correlation of CH2/CH3 plotted against δ15N and δ13C; and (3) strong negative correlations of FTIR band ratios plotted against Raman band parameters and D/G values. The data are not consistent with even moderate heating of the IOM, as indicated by CH2/CH3 ratios that are consistent with unheated carbonaceous chondrites. The C and N isotope data previously collected for each Ryugu particle preclude aqueous alteration based on our understanding of its effects on carbonaceous chondrite IOM. Mixing of several IOM endmembers was considered, but due to the similarities of the particle with the lowest CH2/CH3 ratio to the other particles in terms of its other spectroscopic parameters, this scenario was considered unlikely. Finally, the effects of irradiation were considered, and UV irradiation, in particular, was hypothesised to be the best explanation for the trends observed. Overall, the data highlight the importance of comprehensive data sets for revealing extraterrestrial processes, which could define the nature of organic matter reaching habitable environments, such as those of the Early Earth.

Keywords: Near-Earth objects, Small Solar System bodies, Asteroids, Infrared spectroscopy, Carbonaceous chondrites, Planetesimals, Vibrational spectroscopy, Complex organic molecules