{"total":46,"items":[{"citing_arxiv_id":"2606.27586","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Detached Post-Algol Eclipsing Binaries Caught Between Case A and Case AB Mass Transfer","primary_cat":"astro-ph.SR","submitted_at":"2026-06-25T22:35:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Discovery of detached post-Algol eclipsing binaries in the LMC with measured subgiant Roche-lobe fill factors of 73-89% that match the predicted TAMS contraction phase between Case A and Case AB mass transfer.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.26098","ref_index":32,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Population of Little Red Dot-like Quasars in SDSS","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Defines a sample of ~1300 SDSS quasars as Local Red Dots matching LRD photometric colors at z~0.4-0.8, with a V-shaped subset showing Balmer absorption and [NeV] emission, and SEDs modeled as reddened AGN plus host galaxy that match LRD stacks.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24159","ref_index":20,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A First Measurement of Circumgalactic Dust Reddening from Only 4.6 deg$^2$ of the Rubin Observatory's DP1","primary_cat":"astro-ph.GA","submitted_at":"2026-06-23T05:27:38+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The first circumgalactic dust reddening measurement from Rubin DP1 data finds A_V proportional to r_perp to the -1.8 power within 120 kpc, consistent with prior SDSS/KiDS/DES results despite 1000x smaller area and fainter foreground sample.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18971","ref_index":10,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Candidate Low-mass Disk-eclipsing Binary in the ~316 Myr Open Cluster UPK 13","primary_cat":"astro-ph.SR","submitted_at":"2026-06-17T11:54:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Photometric reanalysis identifies UPK 13-c2 as a candidate late-K/early-M binary with circumbinary disk in the ~316 Myr cluster UPK 13, potentially the oldest main-sequence disk-eclipsing binary known.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17563","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A MUSE View of the Optical Torus within the Supernova Remnant 1E 0102.2-7219","primary_cat":"astro-ph.HE","submitted_at":"2026-06-16T06:09:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Higher-resolution MUSE data shows the optical torus in SNR E0102 as a multiphase cavity whose line ratios require coexisting shock and ionization conditions rather than any single-component model.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12862","ref_index":47,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Ultraviolet Imaging of SR 12 c with HST/WFC3: Accretion and Variability of a Giant Planet at the End Stages of Growth","primary_cat":"astro-ph.EP","submitted_at":"2026-06-11T03:46:28+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"HST/WFC3 UV imaging of SR 12 c measures accretion luminosity of 1.65 ± 0.19 × 10^{-5} L_⊙ and rate of 8 ± 2 × 10^{-12} M_⊙ yr^{-1}, placing it at the end stages of giant planet assembly with a full UV-to-sub-mm SED.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12249","ref_index":136,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spatially Resolved Nebular-Stellar Reddening with JWST/NIRISS","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T15:52:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST observations of high-redshift galaxies show no evolution in dust geometry to z~2.4 and yield an empirical calibration linking resolved differential reddening to SFR surface density.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05321","ref_index":41,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Hot Degenerate Components in Blue Stragglers: A Multi-Wavelength SED Analysis of Nine Open Clusters with Swift/UVOT","primary_cat":"astro-ph.SR","submitted_at":"2026-06-03T18:08:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SED analysis of blue stragglers in open clusters finds UV excesses indicating hot degenerate companions in 15 of 35 candidates, supporting binary evolution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04624","ref_index":240,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Blue Straggler Stars in Berkeley 18: A Multiwavelength Study of Their Physical Properties and Dynamical Evolution","primary_cat":"astro-ph.SR","submitted_at":"2026-06-03T08:59:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Multiwavelength study identifies 24 BSS candidates in Berkeley 18, derives their properties via SEDs, and infers binary evolution as the dominant channel from low dynamical interaction indicators.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04208","ref_index":183,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"HETDEX Public Data Release 1: Source Catalog 2 and Data Cubes from ~90 sq deg of Integral-Field Optical Spectroscopy","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T20:52:21+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":5.0,"formal_verification":"none","one_line_summary":"HETDEX PDR1 releases an expanded public catalog of 426,654 LAEs, 491,411 [O II] emitters and additional sources from 86.67 sq deg of integral-field spectroscopy with improved classifiers.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"However, we note that large varia- tions of this re-calibration are seen in the Milky Way interstellar medium (Zhang & Green 2025; Lee et al. 2025).A V values range from 0.01 to 1.44 with a median value of 0.04. Extinction corrections of line fluxes are ap- plied at the central wavelength of each catalogued emis- sion line according to theR V = 3.1 extinction curve of Fitzpatrick (1999), implemented using the open source Python softwareextinction 9. 3.7.ML/AI Assisted Classification 9 https://github.com/kbarbary/extinction 23 Machine Learning (ML) and Artificial Intelligence (AI) tools provide efficient methods for data classifica- tion, and the HETDEX collaboration has explored sev- eral such approaches. Unsupervised learning has proven"},{"citing_arxiv_id":"2605.20887","ref_index":23,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Difference Between Half-mass Radius and Half-light Radius of Galaxies at 0.2 $< z <$ 2.5 Revealed by JWST/NIRCam Data","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T08:26:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST data shows half-light radii larger than half-mass radii in galaxies at 0.2<z<2.5, with mass-dependent differences, steeper size-mass slopes for light, and faster mass-size growth for star-forming galaxies at high redshift.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20153","ref_index":25,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The exceptional 2017 gamma-ray flare of the radio galaxy NGC 1275: VERITAS and Multiwavelength Observations","primary_cat":"astro-ph.HE","submitted_at":"2026-05-19T17:42:24+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18161","ref_index":202,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SDSS-V: Revealing a weak accretion state in X-ray selected red quasars","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T10:05:20+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Red quasars are intrinsically X-ray weak with low alpha_OX values, tracing a distinct evolutionary stage of suppressed black hole accretion relative to stellar mass growth.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.12503","ref_index":22,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Unveiling Hidden Lyman Alpha Emitters in the DESI DR1 Data","primary_cat":"astro-ph.GA","submitted_at":"2026-05-12T17:59:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A CNN detects 19,685 LAEs at z=2-3.5 in DESI DR1 spectra with 95% purity and completeness.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"chitecture, training procedure and the performance and Section 4 presents the LAE catalog and the basic prop- erties. Finally, Section 5 summarizes the results. We adopt a flat ΛCDM cosmology withh= 0.6766 and Ωm = 0.30966 (Plank18; Planck Collaboration et al. 2020). Galactic extinction corrections are applied to the spectra and magnitudes using Schlegel et al. (1998) dust map and Fitzpatrick (1999) extinction law. Magnitudes are in AB system. 2.DATA Constructing a supervised machine leaning model for identifying LAEs requires a training dataset to train model, a validation dataset to optimize hyper- parameters, and a test dataset to quantify the perfor- mance of the model (See Bishop & Nasrabadi 2006; Goodfellow 2016, for a review). Therefore, we first need"},{"citing_arxiv_id":"2605.11486","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Hybrid Origin for the Multiple Ring-Gap Structures in the Large Protoplanetary Disk V1094 Sco: A Low-Mass Planet and Secular Gravitational Instability","primary_cat":"astro-ph.EP","submitted_at":"2026-05-12T04:03:32+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"This design re- duces the degeneracy between g and R⋆ in broadband SED fitting while directly incorporating external physi- cal information into the inference. During each grid fit, SHIDARE linearly interpolates synthetic spectra in Teff-log g-[Fe/H] space, scales the model fluxes by ( R⋆/d)2, and evaluates wavelength dependent extinction using the E. Fitzpatrick (1999) 29 100 101 102 103 104 Wavelength ( m) 10 13 10 12 10 11 10 10 10 9 F (erg s 1 cm 2) Photosphere model Spitzer IRS Johnson:B Gaia2:GBP Johnson:V Gaia2:G Gaia2:GRP 2MASS:J 2MASS:H 2MASS:Ks WISE:W1 WISE:W2 AKARI:S9W AKARI:N60 AKARI:WIDE-S AKARI:N160 Herschel:F250 Herschel:F350 Herschel:F500 ALMA:Band6 Figure D1. Spectral energy distribution (SED) of V1094"},{"citing_arxiv_id":"2605.11074","ref_index":178,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)","primary_cat":"astro-ph.SR","submitted_at":"2026-05-11T18:00:02+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11067","ref_index":52,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Spectroscopic Bolometric Corrections and Empirical Zero-point Constants of \\textit{Gaia} Magnitudes, $G$, $G_{\\rm BP}$, and $G_{\\rm RP}$, from \\textit{Gaia} XP Spectra","primary_cat":"astro-ph.SR","submitted_at":"2026-05-11T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Empirical zero-point constants for Gaia bolometric corrections are derived as weighted averages 0.8677, 1.0449, and 2.0510 mag for G, GBP, and GRP from 88 stars, yielding corresponding magnitude zero-points via IAU definitions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.10940","ref_index":117,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Electromagnetic Follow-up of the Sub-Solar Mass Gravitational Wave Candidate S251112cm: Kilonova Constraints and a Coincident IIb Supernova","primary_cat":"astro-ph.HE","submitted_at":"2026-05-11T17:59:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"No kilonova detected from sub-solar GW candidate S251112cm, but coincident IIb supernova SN 2025adtq yields suggestive evidence for the superkilonova channel, though inconclusive after accounting for chance coincidence.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.07965","ref_index":45,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Changing-Look Seyfert Discovered by eROSITA Reveals a Two-Component Broad-Line Region","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T16:28:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"HE 1237-2252 exhibits a changing-look event driven by intrinsic accretion-rate variations, revealing a two-component broad-line region consisting of virialized gas at ~27 light-days and disk emission at larger radii.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.06925","ref_index":33,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Scylla VI: Parsec-Scale Dust Extinction Maps in the SMC and LMC","primary_cat":"astro-ph.GA","submitted_at":"2026-05-07T20:36:42+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Kriging and Gaussian mixture modeling applied to HST data yield 1-pc resolution dust extinction maps in the SMC and LMC, showing log-normal column density distributions and systematic differences from FIR-derived dust masses.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Draine 2003) - ultimately providing a more complete estimate of the total ISM mass budget of galaxies. One way to observe dust is through its extinction of light. Due to the distribution of dust grain sizes, extinction from dust is minimal in the near-IR but increases towards optical and ultraviolet (UV) wave- lengths (e.g., J. A. Cardelli et al. 1989; E. L. Fitzpatrick 1999; B. T. Draine 2003; K. D. Gordon et al. 2023). This wavelength-dependent characteristic means that the col- umn density of dust extinction can be constrained with multi-wavelength data (e.g., spectra or multi-band pho- tometry) as long as the background source of light can be modeled adequately. For nearby galaxies with resolved stellar populations,"},{"citing_arxiv_id":"2605.06799","ref_index":185,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"On the origin of the environmental step: A BayeSN view of the ZTF SN Ia DR2","primary_cat":"astro-ph.CO","submitted_at":"2026-05-07T18:01:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"BayeSN analysis of ZTF Type Ia supernovae confirms a ~0.1 mag intrinsic environmental step in standardized brightness that is not explained by differences in dust extinction properties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.04869","ref_index":206,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Exploration of the inner region of the system HD 142527","primary_cat":"astro-ph.EP","submitted_at":"2026-05-06T13:01:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"High-contrast imaging with PACO and REXPACO reveals a new candidate companion at ~14 au and a tightly wound H-alpha spiral in the inner disk of HD 142527, suggesting ongoing companion-disk interactions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03124","ref_index":136,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Nowhere Left to Hide: Uncovering All of the Massive Young Embedded Star Clusters in the Antennae with JWST","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T20:04:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST observations identify all massive young embedded star clusters in the Antennae, revealing they are extremely young, heavily obscured, and account for ~60% of the ionizing luminosity.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02999","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Peering down the barrel with DESI DR2: 10 000+ inflows at $z$ < 0.6 reveal how galaxies accrete cold gas","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T18:00:00+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20480","ref_index":62,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The January 2010 flare of Mrk421: Insights from a stochastic acceleration model","primary_cat":"astro-ph.HE","submitted_at":"2026-04-22T12:09:40+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The January 2010 flare of Mrk421 shows spectral variability consistent with stochastic acceleration, including development of a Maxwellian pile-up component in the particle distribution on three nights.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.20010","ref_index":151,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The First Infrared Portrait of A Solar-Like Host Star with Debris Disk: Pioneering High-Resolution H- and K-Band Spectroscopy of HD115617 with Comparative Optical Spectrum Analysis","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T21:39:21+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The first NIR high-resolution spectroscopy of solar analog HD115617 shows a 250 K temperature discrepancy with optical data but confirms solar composition, main-sequence status, and no chemical signature of planetary formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19975","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The FUor Mass Distribution Matches the Solar Neighborhood IMF: Evidence for a Universal Eruptive Phase","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T20:34:17+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FUor masses inferred from Keplerian line broadening in H-band spectra match the solar neighborhood IMF, indicating a universal eruptive phase during star formation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.19942","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Prevailing thermally-pulsing-asymptotic-giant branch stars in the near-infrared rest-frame spectra of distant quiescent galaxies: towards robust galaxy ages and masses","primary_cat":"astro-ph.GA","submitted_at":"2026-04-21T19:44:35+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Models with prominent TP-AGB phases best fit the near-IR spectra of high-redshift quiescent galaxies, yielding younger ages and lower stellar masses than models with weaker TP-AGB contributions.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"The input spectral resolution for the stacks was determined during the stacking process (Section 4.2.1). The best-fit results fort >0.4Gyr stacks remain robust when adopting alternative SFHs (e.g., exponentially declining SFH or non-parametric SFH) and different dust attenuation laws (e.g., Milky Way or Large Magellanic Cloud, LMC, extinction curves; E. L. Fitzpatrick 1999). Because only three galaxies fall in thet≤0.4 Gyr bin, masking emission lines and shifting to the rest frame prior to stacking results in limited NIR coverage with numerous absorption features (see Figure F1). A larger sample is required to confirm these results and to identify the NIR features robustly in future work. Here, we present only the best-fitting models to the stacked spectrum in this younger bin, after masking the∼2000 ˚A unidentified features,"},{"citing_arxiv_id":"2604.19919","ref_index":8,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Neural Simulation-based Inference with Hierarchical Priors for Detached Eclipsing Binaries","primary_cat":"astro-ph.SR","submitted_at":"2026-04-21T18:59:57+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A multimodal amortized neural posterior estimator trained on realistic simulations recovers DEB parameters accurately with calibrated uncertainties on held-out tests.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"A small number of samples lie outside the plotted ranges and are omitted for clarity. Distance Scaling.-The PHOEBE bundle is evaluated at the sampled system distance, and absolute passband lumi- nosities are converted to band-integrated fluxes at Earth assuming isotropic emission. Interstellar Extinction.-Interstellar reddening is applied after computing intrinsic band-integrated fluxes. For each passband, we convolve the Fitzpatrick (1999) extinction curve with the PHOEBE passband transmission function to compute an effective attenuation factor, Aband = R T(λ) 10−0.4Aλ dλR T(λ)dλ , whereT(λ) is the filter transmission curve andA λ is the extinction at wavelengthλfor a givenE(B−V) and fixed RV = 3.1. This produces a band-specific multiplicative attenuation applied to the intrinsic flux."},{"citing_arxiv_id":"2604.18859","ref_index":44,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Testing $\\Lambda$CDM versus dynamical dark energy in one year: A DESI spectroscopic follow-up program for Rubin supernovae","primary_cat":"astro-ph.CO","submitted_at":"2026-04-20T21:33:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A coordinated Rubin-DESI supernova survey could distinguish dynamical dark energy from Lambda CDM at over 5 sigma in one year using 2300 spectroscopically confirmed SNe Ia at low redshift.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.16601","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SDSS-V LVM: Verifying what, and where, the 'Galactic Center' Lobe is","primary_cat":"astro-ph.GA","submitted_at":"2026-04-17T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"The Galactic Center Lobe is a foreground HII region at ~2 kpc, photoionized and forming a closed outer loop, not a Galactic center feature.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Due to the faintness of this line, we find it is primarily detected within a few individual fibers that contain the brightest regions of the GCL, and within the high surface brightness GCL-1 re- gion. In Figure 6 we compare Pa9/Hαto Hα/Hβfor all individ- ual fibers with S/N>5 (grey) and S/N>10 (red). As most extinc- tion laws are very similar in shape in the optical, we adopt the Fitzpatrick (1999) extinction curve and overplot lines for fiducial values of RV=3.1 (dashed, typical of diffuse conditions; Cardelli et al. 1989) and R V=4.05 (dotted, typical of denser conditions; Calzetti et al. 2000). We find our high confidence detections and the GCL-1 region fall between these two regimes, consistent with RV=3.6, and adopt this value for the remainder of our anal-"},{"citing_arxiv_id":"2604.13983","ref_index":11,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Radial Velocity Evidence for a Post-Mass-Transfer Massive Binary System: NaSt1","primary_cat":"astro-ph.SR","submitted_at":"2026-04-15T15:28:03+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Radial velocity data reveal a 310-day orbital period in NaSt1 with opposing phases in two groups of emission lines, supporting its nature as a post-mass-transfer massive binary system.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"180◦ out of phase from all other lines, as shown in Fig- ures 3 and 4. We will discuss the implications of these RV behaviors in Section 4. 3.2.Dust Parameter Estimation in the mid-IR Using the 1-5µm spectrum, we corrected the ob- served fluxes for interstellar extinction, assumingA V = 6.5 mag andR V = 3.1 (P. A. Crowther & L. J. Smith 1999; E. L. Fitzpatrick 1999). For wavelengths corre- sponding to 0.3≤1/λ≤3.3µm −1, we adopt the ex- tinction law of E. L. Fitzpatrick (1999). At longer wave- lengths (λ >3.3µm), we apply the near- and mid-IR extinction relations from R. Indebetouw et al. (2005), scaled to the adopted visual extinction. The extinction- corrected fluxes were computed asFdered =F obs 100.4Aλ, and uncertainties were propagated accordingly."},{"citing_arxiv_id":"2604.12494","ref_index":35,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Multiwavelength Study of Blue Straggler Stars in Tombaugh 2: Evidence for Binary Mass Transfer and Constraints on Cluster Dynamical State","primary_cat":"astro-ph.SR","submitted_at":"2026-04-14T09:19:08+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"In Tombaugh 2, 32% of blue straggler stars show ultraviolet excess from hot companions consistent with recent binary mass transfer, supporting this channel over mergers in a low-density cluster.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"Each field was visually inspected using Al- adin11 to identify possible contamination from nearby stars within the retrieval radius; no significant blend- ing was found. Interstellar extinction corrections were 10 https://svo2.cab.inta-csic.es/theory/vosa 11 https://aladin.u-strasbg.fr/ 8 applied by VOSA using the extinction prescriptions of (E. L. Fitzpatrick 1999; R. Indebetouw et al. 2005), as- suming a standard total-to-selective ratio ofR V = 3.1. The extinction-corrected SEDs were initially fitted with single-star atmosphere models from the Kurucz ODFNEW/NOVER grid (F. Castelli et al. 1997; F. Castelli & R. L. Kurucz 2003). The parameter space coveredT eff = 5000-15000 K. The best-fitting model was determined by minimizing the reduced chi-square"},{"citing_arxiv_id":"2604.07134","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"LightCurveLynx: Forward Modeling of Time-Domain Surveys with Application to ZTF SN Ia DR2","primary_cat":"astro-ph.IM","submitted_at":"2026-04-08T14:28:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LightCurveLynx is a flexible forward-modeling tool that produces supernova light-curve simulations matching ZTF observations with low KL divergence and consistent completeness limits.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We obtain the extinction parameter E(B-V) from D. J. Schlegel et al. (1998); E. F. Schlafly & D. P. Finkbeiner (2011) using the sfdmap2 package (K. Barbary & AmpelAstro 2023) wrapped by LightCurveLynx, and apply extinction to the observer-frame SN SED, before integrating over the passbands to generate 6 broadband photometry. We use the extinction curve from E. L. Fitzpatrick (1999) as provided in thedust extinction package (K. D. Gordon 2024). 3.5. Filter Transmission Curves The ZTFSNDR2 data include three passbands, g, r, and i. We obtain the filter transmission curves from SNCosmo9. LightCurveLynx provide a variety of ways to obtain transmission curves from different sources. 3.6. Noise Estimation The total noise standard deviation in electrons for a point source is calculated following standard photon noise"},{"citing_arxiv_id":"2604.06314","ref_index":25,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Dust and Grain Size Evolution in Galaxy Simulations: What Matters and What Does Not","primary_cat":"astro-ph.GA","submitted_at":"2026-04-07T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"Dust grain size distributions evolve from large-grain dominated at high redshift to MRN-like at low redshift, driven primarily by shattering and ISM accretion after stars supply initial large grains, reproducing z=0 dust masses and Milky Way extinction properties.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"suited to evaluating the cumulative effects of these pro- cesses in an evolved galaxy population. A summary of all simulation runs performed in this analysis is provided in Tab. 1. For each model (sub- script mod), we quantify its deviation from the fiducial run (subscript FID) for each of the three aforementioned relations by means of the metric ∆σ(x) = ymod(x)−y FID(x)p σ2 mod(x) +σ 2 FID(x) ,(25) wherey(x) is the median relation predicted by a given simulation, and σ(x) = yup(x)−y down(x) 2 (26) is the effective dispersion estimated from the upper and lower percentiles. In practice, the median relation and the corresponding percentiles ofyas a function ofxare the quantities shown in the figures. As a global summary statistic, we adopt the mean"},{"citing_arxiv_id":"2604.03385","ref_index":12,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Deep Adaptive Optics Imaging Rules Out a Helium Star Companion to PSR J1928+1815","primary_cat":"astro-ph.SR","submitted_at":"2026-04-03T18:28:26+00:00","verdict":null,"verdict_confidence":null,"novelty_score":null,"formal_verification":null,"one_line_summary":null,"context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"0 kpc, we conservatively cal- culate the extinction as a linear interpolation between the value given by G. M. Green et al. (2019) at 8.0 kpc 4 (E(B−V)≈2.735) and the total Galactic extinction given by the 2D dust map of E. F. Schlafly & D. P. Finkbeiner (2011) (E(B−V)≈4.380), which we take to apply at 12 kpc. We assume thatA Ks = 0.306E(B−V) based on the E. L. Fitzpatrick (1999) extinction law. We show the constraints on the distance to PSR 1928+1815 from the electron density maps of J. M. Cordes & T. J. W. Lazio (2002) and J. M. Yao et al. (2017) in Figure 3. Specifically, we plot the predicted dispersion measure (DM) as a function of distance along the sight line to the pulsar, with the observed DM and corresponding uncertainty marked with a dashed black"},{"citing_arxiv_id":"2602.12548","ref_index":29,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Structure and Evolution of LRDs: Insights from JWST NIRSpec Medium and High Resolution Spectroscopy at $z\\sim4$","primary_cat":"astro-ph.GA","submitted_at":"2026-02-13T02:56:31+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Spectroscopic study of 11 LRDs at z~4 finds AGN origin for optical emission via broad Hα correlations and introduces a clumpy envelope model with growth timescales of 10^5-10^7 years.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.05404","ref_index":16,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Double-Burst Nature and Early Afterglow Evolution of Long GRB 110801A","primary_cat":"astro-ph.HE","submitted_at":"2026-02-05T07:43:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"GRB 110801A shows double-burst gamma-ray emission with an early-rising optical afterglow from the first burst preceding the second prompt episode, modeled via reverse and forward shocks yielding Gamma_0 ~60, theta_j ~0.09, and E_k,iso ~10^54.8 erg.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2601.22490","ref_index":14,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SED and Galactic kinematic diagnostics for dormant BH/NS binary candidates","primary_cat":"astro-ph.SR","submitted_at":"2026-01-30T03:00:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"SED fitting plus kinematic diagnostics identify 182 top dormant BH/NS binary candidates from Gaia DR3, with 19 likely black hole systems having companion masses >=3 solar masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.23157","ref_index":31,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The GLASS-JWST Early Release Science Program. V. H$\\alpha$ luminosity functions at $z\\sim1.3$ and $z\\sim2.0$","primary_cat":"astro-ph.GA","submitted_at":"2025-12-29T02:40:50+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Hα luminosity functions at z~1.3 and z~2.0 yield faint-end slopes of -1.50 and -1.60, with integrated SFR densities of 0.097 and 0.129 M⊙ yr⁻¹ Mpc⁻³ from a sample of 99 emitters.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.19783","ref_index":24,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"SN 2025ogs: A Spectroscopically-Normal Type Ia Supernova at z = 2 as a Benchmark for Redshift Evolution","primary_cat":"astro-ph.CO","submitted_at":"2025-12-22T19:00:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"SN 2025ogs is a spectroscopically normal Type Ia supernova at z=2.05 whose luminosity distance and properties are consistent with low-z standards and current LambdaCDM constraints.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2512.01684","ref_index":36,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Transition from Outside-in to Inside-Out at $z\\sim 2$: Evidence from Radial Profiles of Specific Star Formation Rate based on JWST/HST","primary_cat":"astro-ph.GA","submitted_at":"2025-12-01T13:51:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Star-forming galaxies show a transition from negative to positive sSFR radial gradients around z~2, implying a change from outside-in to inside-out growth.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"We derive the integrated physical properties of the galax- ies in our sample usingCIGALEprogram (Boquien et al. 2019), based on 9-band photometry for the CEERS field and 10-band photometry for the remaining fields. The fit- ting setup ofCIGALEused in this work closely follows that of Shen et al. (2024). We first correct the photometric cat- alog for Milky Way extinction using the extinction curve of Fitzpatrick (1999) and the extinction map from Schlafly & Finkbeiner (2011). The SED fitting assumes a delayed- τstar formation history, Bruzual & Charlot (2003) stellar population with solar metallicity, the dust attenuation law of Calzetti et al. (2000), and the nebular emission models of In- oue (2011). Due to the lack of mid-infrared observations, we do not include a dust emission component in our modeling."},{"citing_arxiv_id":"2509.07810","ref_index":37,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The heart of NGC 5253 as seen with MUSE-NFM: nitrogen enrichment through stellar chemical feedback at parsec scales","primary_cat":"astro-ph.GA","submitted_at":"2025-09-09T14:48:47+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"High-resolution mapping reveals nitrogen enrichment around super star clusters in NGC 5253, attributed to Wolf-Rayet stars with material expelled to surrounding gas.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2503.12898","ref_index":17,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"A Sample of Active Galactic Nuclei with Intermediate-mass Black Holes Extended to $z \\approx$ 0.6","primary_cat":"astro-ph.GA","submitted_at":"2025-03-17T07:59:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A new sample of 930 IMBH AGNs at z up to 0.57 is compiled from SDSS, with preliminary evidence of declining maximum accretion rates and Hα luminosities toward lower redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2311.12098","ref_index":78,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Union Through UNITY: Cosmology with 2,000 SNe Using a Unified Bayesian Framework","primary_cat":"astro-ph.CO","submitted_at":"2023-11-20T19:00:01+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Union3 compilation of 2087 SNe Ia with UNITY1.5 framework shows 1.7-2.6 sigma tension with LambdaCDM and possible thawing dark energy.","context_count":1,"top_context_role":"method","top_context_polarity":"unclear","context_text":"However, future cos- mology analyses should explicitly marginalize over the true redshift of each SN to properly treat these effects.17 4.4.6. Milky Way Extinction We use the Schlafly & Finkbeiner (2011) recalibration of the Schlegel et al. (1998) Milky-Way extinction map for our MW extinctions (that is, we scale the SFD98 map by 0.86). We use the Fitzpatrick (1999) extinction curve with RV = 3.1. We assume each MW extinction has 16% statistical uncertainty and a correlated 10% systematic uncertainty in the normalization of the full map. Furthermore, we assume an additive zeropoint un- certainty of the map of 5 mmags in E(B − V ) motivated by a comparison between HI and reddening at low col- umn density (Lenz et al."},{"citing_arxiv_id":"2202.04077","ref_index":278,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"The Pantheon+ Analysis: Cosmological Constraints","primary_cat":"astro-ph.CO","submitted_at":"2022-02-08T19:00:00+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Pantheon+ delivers tighter SN Ia constraints on Ω_M, w0, wa, and H0 from 1550 events, consistent with a cosmological constant, with SN systematics contributing less than one third to H0 uncertainty.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"model spectra during both the model training process and during the data light-curve fitting process. The \"extinction curve\" describes the relation between the amount of reddening and extinction as a function of wavelength. Baseline: We account for MW extinction using maps from Schlegel et al. (1998), with a scale of 0.86 following Schlafly et al. (2010). We assume the MW extinction curve from Fitzpatrick (1999) with RV = 3.1. Systematics: Similarly to Pantheon, we adopt a global 5% uncertainty scaling of E(B− V )MW based on the fact that Schlafly & Finkbeiner (2011a), in a reanalysis of Schlafly et al. (2010), derive smaller values of redden- ing by 4%, despite using a very similar SDSS footprint (σψ = 1). While Schlafly & Finkbeiner (2011b) found that their results prefer the Fitzpatrick (1999) extinction"}],"limit":50,"offset":0}