Sazuna/UAT_keywords huggingface dataset:
The Cosmic Infrared Background Experiment-2: An Intensity-mapping Optimized Sounding-rocket Payload to Understand the Near-IR Extragalactic Background Light. The background light produced by emission from all sources over cosmic history is a powerful diagnostic of structure formation and evolution. At near-infrared wavelengths, this extragalactic background light (EBL) is comprised of emission from galaxies stretching all the way back to the first-light objects present during the Epoch of Reionization. The Cosmic Infrared Background Experiment 2 (CIBER-2) is a sounding-rocket experiment designed to measure both the absolute photometric brightness of the EBL over 0.5─2.0 μm and perform an intensity-mapping measurement of EBL spatial fluctuations in six broad bands over the same wavelength range. CIBER-2 comprises a 28.5 cm, 80 K telescope that images several square degrees to three separate cameras. Each camera is equipped with an HAWAII-2RG detector covered by an assembly that combines two broadband filters and a linear-variable filter, which perform the intensity mapping and absolute photometric measurements, respectively. CIBER-2 has flown three times: an engineering flight in 2021, a terminated launch in 2023, and a successful science flight in 2024. In this paper, we review the science case for the experiment; describe the factors motivating the instrument design; review the optical, mechanical, and electronic implementation of the instrument; present preflight laboratory characterization measurements; and finally assess the instrument's performance in flight.

Keywords: Rockets, Cosmic background radiation, Astronomical instrumentation, Infrared telescopes
COSINE (Cometary Object Study Investigating Their Nature and Evolution). I. Project Overview and General Characteristics of Detected Comets. We present the first results from the Cometary Object Study Investigating their Nature and Evolution (COSINE) project, based on a uniformly processed data set of 484 comets observed over the full 15 yr duration of the Wide-field Infrared Survey Explorer (WISE)/NEOWISE mission. This compilation includes 1633 coadded images spanning 966 epochs with signal-to-noise ratios greater than 4, representing the largest consistently analyzed infrared comet data set obtained from a single instrument. Dynamical classification identifies 234 long-period comets (LPCs) and 250 short-period comets (SPCs), spanning heliocentric distances of 0.996–10.804 au. LPCs are statistically brighter than SPCs in the W1 (3.4 μm) and W2 (4.6 μm) bands at comparable heliocentric distances. Cometary activity peaks near perihelion, with SPCs exhibiting a pronounced postperihelion asymmetry. Multiepoch photometry reveals that SPCs show steeper brightening and fading slopes than LPCs. The observing geometry of WISE/NEOWISE—constrained to a fixed ∼90° solar elongation from low-Earth orbit—introduces systematic biases in the sampling of orientation angles for extended features. Collectively, the results reveal a continuous evolutionary gradient across comet populations, likely driven by accumulated solar heating and surface processing. This study establishes a foundation for subsequent COSINE analyses, which will separate nucleus and coma contributions and model dust dynamics to further probe cometary activity and evolution.

Keywords: Long period comets, Comets, Short period comets
Subaru High-z Exploration of Low-luminosity Quasars (SHELLQs). XXIV. 54 New Quasars and Candidate Obscured Quasars at 5.71 ≤ z ≤ 7.02. We present spectroscopic identification of 43 quasars and 11 candidate obscured quasars in the epoch of reionization (EoR) at 5.71 ≤ z ≤ 7.02, along with 29 galaxies at similar redshifts. This is the 24th publication from the Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs) project, which exploits the Hyper Suprime-Cam (HSC) Subaru Strategic Program (SSP) imaging survey to search for EoR quasars. The HSC-SSP survey has finished, and this paper is likely the final installment of major (unobscured) quasar discoveries from the SHELLQs project. In addition to the EoR objects, we identified five strong [O III] line emitters at z &lt; 1, 30 Galactic brown dwarfs, and 14 passive galaxies at z ∼ 2, which contaminated our sample of photometric quasar candidates. The present paper focuses on describing the immediate outcome of the spectroscopic observations, while a statistical analysis of the full SHELLQs sample will be presented in our next publication.

Keywords: Reionization, High-redshift galaxies, Sky surveys, Quasars
Identifying Dust-lane Spheroidal Galaxies in DESI Legacy Imaging Surveys Using Semisupervised Methods. Dust-lane spheroidal galaxies (DLSGs) are unique astrophysical systems that exhibit the morphology of early-type galaxies (ETGs) but are distinguished by prominent dust lanes. Recent studies propose that they form through minor mergers between ETGs and gas-rich dwarf galaxies, offering a window into the interstellar medium (ISM) of ETGs and star formation triggered by small-scale interactions. However, their rarity poses a challenge for assembling large, statistically robust samples via manual selection. To overcome this limitation, we employ GC-SWGAN, a semisupervised learning method developed by Z. Luo et al., to systematically identify DLSGs within the DESI Legacy Imaging Surveys (DESI-LS). The methodology involves training a generative adversarial network on unlabeled galaxy images to extract morphological features, followed by fine-tuning the model using a small data set of labeled DLSGs. In our experiments, despite DLSGs constituting only ∼3.7% of the test set, GC-SWGAN achieves remarkable performance, with an 87% recall rate, 84% accuracy, and an F1 score of 86%, underscoring its efficacy for DLSG detection. By applying this model to ∼310,000 DESI-LS galaxies that meet the criteria mr &lt; 17.0 and 0.01 &lt; z &lt; 0.07 we compile the largest catalog of DLSG candidates to date, identifying 9482 dust-lane ETGs. A preliminary analysis reveals that these DLSGs exhibit significantly redder g ‑ r colors and higher specific star formation rates compared to non-DLSGs. This catalog enables future studies of ISM properties in ETGs and the role of minor mergers in driving star formation in the nearby Universe.

Keywords: Galaxies, Computational astronomy, Convolutional neural networks, Astronomy data analysis, Ground-based astronomy, Astronomy image processing
Statistical Analyses of Solar Active Regions in SDO/HMI Magnetograms Detected by the Unsupervised Machine Learning Method DSARD. Solar active regions (ARs) host the majority of solar eruptions. Studying the evolution and morphological features of ARs is significant for understanding the physical mechanisms of solar eruptions and beneficial for forecasting hazardous space weather. This work presents an automated DBSCAN-based solar active region detection (DSARD) method for ARs observed in magnetograms. DSARD is based on an unsupervised machine learning algorithm called density-based spatial clustering of applications with noise (DBSCAN). This method is employed to identify ARs in magnetograms observed by the Helioseismic and Magnetic Imager on board the Solar Dynamics Observatory from 2010 to 2023. To avoid duplicate detections and minimize projection effects, we focus on a longitudinal range of ±6° from the central meridian of the solar disk. Within this range, we obtain the distributions of the number, area, magnetic flux, tilt angle, and butterfly diagram of bipolar ARs in latitudes and time intervals during solar cycle 24, as well as their drift velocities. Most of these statistical results align with previous studies, which validates our method. The asymmetry indices of the number of ARs, cumulative area, and total unsigned magnetic flux indicate that the northern hemisphere dominated in terms of AR activity during most of solar cycle 24, except near solar maximum. Additionally, we analyze the dipole tilt angles of ARs in solar cycle 24 and the rising phase of solar cycle 25, revealing that 13% and 16% of ARs, respectively, violate Hale's law.

Keywords: Solar cycle, Astronomical techniques, Solar active regions, Solar magnetic fields
Radio Afterglow Detection and AI-driven Response (RADAR): A Federated Framework for Gravitational-wave Event Follow-up. The landmark detection of both gravitational waves (GWs) and electromagnetic (EM) radiation from the binary neutron star merger GW170817 has spurred efforts to streamline the follow-up of GW alerts in current and future observing runs of ground-based GW detectors. Within this context, the radio band of the EM spectrum presents unique challenges. Sensitive radio facilities capable of detecting the faint radio afterglow seen in GW170817, and with sufficient angular resolution, have small fields of view compared to typical GW localization areas. Additionally, theoretical models predict that the radio emission from binary neutron star mergers can evolve over weeks to years, necessitating long-term monitoring to probe the physics of the various postmerger ejecta components. These constraints, combined with limited radio observing resources, make the development of more coordinated follow-up strategies essential—especially as the next generation of GW detectors promises a dramatic increase in detection rates. Here, we present RADAR, a framework designed to address these challenges by promoting community-driven information sharing, federated data analysis, and system resilience, while integrating AI methods for both GW signal identification and radio data aggregation. We show that it is possible to preserve data rights while sharing models that can help design and/or update follow-up strategies. We demonstrate our approach through a case study of GW170817, and discuss future directions for refinement and broader application.

Keywords: Astronomy software, Extragalactic radio sources, Astronomy data analysis, Gravitational wave astronomy, Gravitational waves, Radio astronomy
Statistical Properties of Solar Wind and Interplanetary Magnetic Field Upstream of Planets at 1 au and Beyond: A Comprehensive Analysis. The solar wind and the interplanetary magnetic field (IMF) are of significant importance, as they affect the plasma environment and dynamic processes in the planetary magnetosphere. This study statistically analyzes the solar wind parameters upstream of Earth (ACE), Mars (MAVEN), Jupiter (Ulysses, Galileo, Juno), and Saturn (Cassini) and their solar activity phase (solar maximum, descending, minimum, and ascending phases) dependence. The heliolatitude variations are validated using Ulysses observations. Results show that the radial magnetic field decays more gradually than expected (r‑2), and the IMF intensity (B) decreases more rapidly at higher heliolatitudes. The solar wind proton density (Np) near Mars is significantly higher than expected, while the solar wind speed (V) is lower. The IMF spiral angle (SA) aligns well with the Parker SA upstream of planets and at high heliolatitudes, except for Mars. Martian anomalies may stem from mass loading by pickup ions (contributing to the increased Np and lower V) and the IMF bending effect caused by Martian current systems. The B and solar wind dynamic pressure are higher during solar maximum compared to solar minimum. Additionally, the V, plasma beta, and Alfvén Mach number exhibit larger values during the solar descending phase compared to the solar ascending phase. The higher V results in a smaller IMF SA, and this effect is more pronounced near Earth and Mars but less noticeable near Jupiter and Saturn. Our statistical survey provides a reference for the upstream solar wind conditions at these planets, benefiting solar wind studies and planetary space environment research.

Keywords: Solar cycle, Solar wind, Interplanetary magnetic fields, Solar activity
AllBRICQS: The Discovery of Luminous Quasars in the Northern Hemisphere. We present the second catalog of bright quasars from the All-sky BRIght, Complete Quasar Survey (AllBRICQS), focusing on spectroscopically observed quasars in the Northern Hemisphere with Galactic latitude ∣b∣ &gt; 10°. This catalog includes their spectral data, redshifts, and luminosities. AllBRICQS aims to identify the last remaining optically bright quasars using data from the Wide-field Infrared Survey Explorer and Gaia all-sky survey Data Release 3 (DR3). AllBRICQS searches for quasars that are brighter than BP = 16.5 or RP = 16 mag in Gaia DR3, based on simple selection criteria. Here, we report 62 new AllBRICQS quasars spanning various types, which include typical broad emission line quasars and the most luminous iron low-ionization broad absorption line quasars discovered to date. Spectroscopic observations were conducted using the Long-Slit Spectrograph on the 1.8 m telescope at Bohyunsan Optical Astronomy Observatory, the Yunnan Faint Object Spectrograph and Camera on the 2.4 m telescope at Lijiang Observatory, and the Beijing Faint Object Spectrograph and Camera on the 2.16 m telescope at Xinglong Observatory. We applied flux calibration using Zwicky Transient Facility broadband photometry to correct for attenuation due to intermittent thin clouds during the observations. Redshifts were determined using inverse-variance weighted cross-correlation methods. Our targets span the bolometric luminosity range of  44.9&lt;logLbol/ergs−1&lt;48.0  at redshifts between 0.09 and 2.48. These confirmed AllBRICQS quasars provide a valuable resource for future research into quasar evolution, black holes, their environments, and their host galaxies across multiple wavelengths.

Keywords: Quasars, Active galactic nuclei, Spectroscopy, Redshift surveys, Catalogs
Comprehensive Analysis of NGC 6134: Structure, Dynamics, and Blue Straggler Star Candidates. Open clusters play a critical role in the study of both stellar and Galactic evolution. We present a comprehensive analysis of the open cluster NGC 6134 using Gaia DR3 astrometric and photometric data, supplemented with multiwavelength observations from the Two Micron All Sky Survey, Wide-field Infrared Survey Explorer, NEOWISE, and Transiting Exoplanet Survey Satellite (TESS). A total of 714 high-probability members were identified using the Hierarchical Density-based Spatial Clustering of Applications with Noise algorithm. The cluster parameters were derived by Bayesian isochrone fitting with BASE-9, resulting in log (age/yr) = 9.1683 ± 0.019, [Fe/H] = 0.0911 ± 0.04, and AV = 1.2095 ± 0.015 mag. The cluster is dynamically relaxed (trh = 16.59 ± 0.25, ≪age) with significant mass segregation (ΛMSR = 1.71 ± 0.26). Galactic orbital integration using galpy indicates that the cluster resides in the thin disk on a slightly eccentric orbit. We identified three candidates of blue straggler stars (BSSs). The first candidate was modeled as an EA-type semidetached eclipsing binary using TESS photometry and Markov Chain Monte Carlo fitting, and Candidate 2 was fitted with a spectral energy distribution (SED) using the Virtual Observatory SED Analyzer tool, providing estimates of its temperature, surface gravity, and metallicity based on the SED-fitting results. However, the third candidate lacks sufficient observational data, which prevents further analysis. These results highlight binary mass transfer as a dominant channel of BSS candidates in NGC 6134, providing observational evidence for the formation mechanism of blue stragglers.

Keywords: Open star clusters, Blue straggler stars
Investigations of MWISP Clumps: <SUP>13</SUP>CO Clump Source Catalog and Physical Properties. We present the first comprehensive catalogs of 13CO clumps from the Milky Way Imaging Scroll Painting (MWISP) project. By developing an equivalent global detection scheme integrated with the FacetClumps algorithm, we successfully extract 71,661 molecular clumps across a high-resolution 13CO data cube spanning 2310 deg2 from the MWISP Phase I survey. To determine accurate distances, we design an automatic hierarchical distance decision method using signal regions as fundamental objects, effectively resolving the kinematic distance ambiguity problem and obtaining reliable measurements for 97.94% of the sample. Statistical analysis reveals that 65.3% of clumps are gravitationally bound, accounting for approximately 96.3% of the statistical total mass. Scaling relation analysis across multiple surveys reveals universal power-law behaviors in clump populations. Maser-associated clumps exhibit modified parameter distributions and scaling relations, revealing how active star formation alters clump dynamics and structure. These extensive catalogs establish a foundation for investigating molecular clump properties, star formation processes, and Galactic evolution.

Keywords: Stellar structures, Radio source catalogs, Astronomical techniques, Star formation, Radio sources
Exploring Warm Jupiter Migration Pathways with Eccentricities. I. Catalog of Uniform Keplerian Fits to Radial Velocities of 200 Warm Jupiters. Giant planets are expected to predominantly form beyond the water-ice line and occasionally undergo inward migration. Unlike hot Jupiters, which can result from high-eccentricity tidal migration, warm Jupiters between 0.1 and 1 au (≍10─365 days) are in many ways more challenging to explain because they reside outside the tidal influence of their host stars. Warm Jupiters should therefore preserve traces of their origins as their eccentricities are directly related to their past interactions. We analyze the eccentricities of 200 warm Jupiters orbiting 194 Sunlike host stars (with FGKM spectral types) using 18,587 radial velocity (RV) measurements across 40 high-resolution spectrographs. RVs are compiled from the literature and are supplemented with 540 new observations from MINERVA-Australis at Mount Kent Observatory and the Habitable-zone Planet Finder spectrograph at McDonald Observatory's Hobby-Eberly Telescope, which are timed to improve eccentricity constraints by sampling orbits near periastron passage. The overarching goal of this program is to establish the relative importance of giant planet migration channels through the largest homogeneous analysis of warm Jupiter orbital properties to date. In particular, we evaluate and compare the impact of different system architectures and host star characteristics on the population-level eccentricity distributions of warm Jupiters. Here, we present the target sample, observations, orbit-fitting procedure, and parameter summary statistics of our survey. All orbit fit solutions, parameter posterior chains, and merged RV tables for each system are made publicly available.

Keywords: Exoplanet evolution, Exoplanet migration
A Neural-network Model for Quickly Solving Multiple-band Light Curves of Contact Binaries. The advent of large-scale photometric surveys has led to the discovery of over one million contact binary systems. Conventional light-curve analysis methods are no longer adequate for handling such massive data sets. To address this challenge, we developed a neural-network-based model capable of rapid analysis of multiple-band light curves of contact binaries. Our model can determine the fundamental physical parameters, including temperature and mass ratios, orbital inclination, potential, fillout factor, primary and secondary luminosities and radii, third-light contribution, and spot parameters. Notably, unlike previous works, our model can simultaneously process multiple-band light curves and the four parameters of a starspot. The model's reliability was verified through analysis of the synthetic light curves generated by PHOEBE and the light curves of eight targets from L.-H. Wang et al.'s work. The discrepancy distribution between the physical parameters determined by our model and true values for the synthetic light curves shows very good agreement. In addition, the physical parameters determined by our model and the corresponding light curve fits show remarkable consistency with L.-H. Wang et al.'s results. By applying our model to Optical Gravitational Lensing Experiment contact binaries, physical parameters of 3541 systems were obtained. We have packaged our model into an executable (CBLA.exe) file and archived it in the China-VO repository (doi:10.12149/101626). The software supports light-curve analysis of 19 standard filters and allows for processing the data, whether from large-scale sky surveys or individual telescope observations.

Keywords: Astronomy software, Fundamental parameters of stars, Astronomy data analysis, Eclipsing binary stars, Contact binary stars
Roles of Supernova and Active Galactic Nucleus Feedback in Shaping the Baryonic Content in a Wide Range of Dark Matter Halo Masses. We build upon FEGA25, a previously introduced semianalytic model (SAM) for galaxy formation and evolution, by focusing on its enhanced treatment of supernova (SN) and active galactic nucleus (AGN) feedback mechanisms. In addition to the traditional AGN feedback mode—negative (suppressing cooling) and the new positive mode (triggering star formation)—we introduce two distinct implementations of a third mode: the ejection of hot gas beyond the virial radius (AGNeject1 and AGNeject2). This component addresses a longstanding issue in SAMs and hydrodynamical simulations: the overestimation of hot gas fractions in low- and intermediate-mass halos. FEGA25 is calibrated via Markov Chain Monte Carlo using a suite of cosmological N-body simulations (YS50HR, YS200, YS300) and a comprehensive set of observed stellar mass functions across a wide redshift range. We find that SN feedback dominates gas ejection in halos with  logMhalo≲12 , while AGN feedback becomes increasingly important at higher halo masses. The AGNeject2 model, which activates primarily at late times (z &lt; 1), reproduces a characteristic, roughly U-shaped, "cavity" in the baryon fraction at z = 0, similar to trends observed in simulations like SIMBA and IllustrisTNG. Conversely, AGNeject1 yields a smoother, redshift-independent evolution. Both models preserve the stellar and cold-gas components and successfully reproduce the stellar-to-halo mass relation up to z = 3. Our results emphasize that a physically motivated AGN-driven mechanism capable of selectively removing hot gas is essential to model the baryon cycle accurately, particularly in the intermediate-halo-mass regime.

Keywords: Galaxy formation, Galaxy evolution
POSYDON Version 2: Population Synthesis with Detailed Binary-evolution Simulations across a Cosmological Range of Metallicities. Whether considering rare astrophysical events on cosmological scales or unresolved stellar populations, accurate models must account for the integrated contribution from the entire history of star formation upon which that population is built. Here, we describe the second version of POSYDON, an open-source binary population synthesis code based on extensive grids of detailed binary evolution models computed using the MESA code, which follows both stars' structures as a binary system evolves through its complete evolution from the zero-age main sequence, through multiple phases of mass transfer and supernovae, to their death as compact objects. To generate synthetic binary populations, POSYDON uses advanced methods to interpolate between our large, densely spaced grids of simulated binaries. In our updated version of POSYDON, we account for the evolution of stellar binaries across a cosmological range of metallicities, extending from 10−4 to 2 Z⊙, including grids specifically focused on the Small and Large Magellanic Clouds (0.2 and 0.45 Z⊙). In addition to describing our model grids and detailing our methodology, we outline several improvements to POSYDON. These include the incorporation of single stars in stellar populations, a treatment for stellar mergers, and a careful modeling of "reverse-mass transferring" binaries in which a once-accreting star later becomes a donor star. Our simulations are focused on binaries with at least one high-mass component, such as those that host neutron stars and black holes, and we provide postprocessing methods to account for the cosmological evolution of metallicity and star formation as well as rate calculations for transient events.

Keywords: Binary stars, Stellar populations, Massive stars, Stellar evolutionary models, High mass x-ray binary stars