{"total":30,"items":[{"citing_arxiv_id":"2606.25856","ref_index":128,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"JWST resolves jet-driven H2 and ionized outflows in radio galaxy 3C305","primary_cat":"astro-ph.GA","submitted_at":"2026-06-24T14:03:23+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"JWST data on 3C305 shows the compact radio jet efficiently drives kiloparsec-scale multiphase outflows via shocks, with high coupling to the observed gas kinetic power and radiative losses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25654","ref_index":13,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A magnetically-supported disk-corona model for Changing-Look AGN transitions","primary_cat":"astro-ph.HE","submitted_at":"2026-06-24T10:08:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Magnetized disk models lower the thermal-viscous instability threshold to Eddington ratios of 0.01-0.03 and yield limit-cycle timescales of months to years, jointly matching observations in five CLAGN only when the inner disk is strongly magnetized.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.25517","ref_index":44,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Unveiling the nature of barium stars. 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Asteroseismic masses and the evolutionary link between Ba dwarfs and giants","primary_cat":"astro-ph.SR","submitted_at":"2026-06-24T07:50:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Asteroseismic masses average 1.29 Msun for Ba dwarfs versus 1.96 Msun for Ba giants, supporting main-sequence accretion evolution from dwarfs to giants, though models fail to match the observed [hs/ls] ratio.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.24458","ref_index":65,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"An Agnostic Machine Learning Model of Photosynthetic Habitability","primary_cat":"astro-ph.EP","submitted_at":"2026-06-23T11:45:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"An agnostic model using genetic algorithm optimization predicts photosynthetic viability declines linearly with orbital distance, expanding the photosynthetic habitable zone for M, K, and G stars beyond Earth-centric estimates.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23926","ref_index":74,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detection of relativistic orbital deformation from improved timing of PSR J1757$-$1854","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T20:44:51+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"First detection of relativistic angular deformation δ_θ in PSR J1757−1854 via MeerKAT-enhanced timing, ruling out two of four prior geometric solutions while confirming GR consistency for orbital decay.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21808","ref_index":22,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the stellar parameter dependence of the combined Fe I and Fe II chromospheric emission-line in the wings of the Ca II K line","primary_cat":"astro-ph.SR","submitted_at":"2026-06-20T00:05:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Observational analysis of 21 giant stars shows Fe I+Fe II blend emission proportional to Ca II K with matching Teff power-law exponent and a slope break in the flux ratio at log g ≈ 2.5.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.18386","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Reconstructing Galactic Gravitational Potentials from Stellar Kinematics with Physics-Informed Neural Networks","primary_cat":"astro-ph.GA","submitted_at":"2026-06-16T18:31:27+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A PINN approach learns galactic gravitational potentials from acceleration data, achieving sub-percent errors on simulations while outperforming analytic models and retaining interpretability via structured priors.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11313","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Comparison and verification methods to trace interaction-driven disturbances in galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-09T18:01:01+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"SSL model detects galaxy interaction signatures with recall 0.86 and low contamination while CAS at A>0.35 has recall 0.20 but higher precision, benchmarked on visual classification of 25.1% disturbed fraction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10028","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Learning the Universe: Constrained simulations of the Coma galaxy cluster -- I. 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cosmological simulations that computes SFR from ambient densities via PRFM theory and a modified effective EOS, producing taller stellar scale heights, slightly higher stellar mass, and morphology changes including Toomre-driven clumps compared to p","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.07230","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Study of photometric and spectral variability of the roAp star HD~210684","primary_cat":"astro-ph.SR","submitted_at":"2026-06-05T12:53:48+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Observational analysis of HD210684 yields rotational period 5.02188 d, magnetic obliquity 77°, and main-sequence age ~1.45 Gyr from photometry, LSD magnetic measurements, and MESA/GYRE 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of a Supermassive Black Hole Binary Candidate PKS 2131-0211","primary_cat":"astro-ph.HE","submitted_at":"2026-06-03T18:35:24+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Bayesian fitting of an eccentric Keplerian orbit to the radio light curve of PKS 2131-021 gives e = 0.053 ± 0.015 without red noise but favors a circular orbit plus DRW noise with e < 0.15.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04624","ref_index":93,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2606.03456","ref_index":84,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A comprehensive Rossiter-Mclaughlin Modelling Framework in TLCM: Application to HD 2685 $=$ TOI-135 system","primary_cat":"astro-ph.EP","submitted_at":"2026-06-02T10:34:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Updated RM modeling framework in TLCM validated on nine systems and applied to TOI-135 to measure sky-projected obliquity λ = 55.6° with ~11° uncertainties.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02732","ref_index":94,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Precision constraints on stellar physics from main sequence detached eclipsing binaries","primary_cat":"astro-ph.SR","submitted_at":"2026-06-01T18:00:28+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Bayesian framework with active-learning surrogate for MESA models constrains ages and α_MLT from 38 main-sequence DEBs, recovering some α_MLT values below the solar calibration.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01158","ref_index":55,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Deep Optical Follow-up Observations to IceCube Cosmic Neutrinos: a case for IC230724A with Subaru/HSC and prospects with Rubin/LSST","primary_cat":"astro-ph.HE","submitted_at":"2026-05-31T11:03:43+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Non-detection of TDE in IC230724A; LSST could constrain TDE fraction of neutrino background to ≲60% or ≳30% with 10 events.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.20835","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Evolution of compressed clouds formed by filament coalescence. I. Oblique collisions","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T07:26:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Oblique filament collisions lead to gravitational collapse of the compressed cloud when post-collision |gravitational energy| exceeds kinetic plus thermal plus magnetic energies, with lower angles and lower velocities favoring hub-filament formation.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Therefore, in order to maintain a hub-filament system, the collision velocity must not exceed a threshold at which the non-colliding segment remains gravitationally bound to the sys- tem. This limit can be reasonably estimated by comparing the ini- tial velocity with the escape velocity from the gravitational poten- tial of the shocked cloud. The escape velocityV esc is defined as Vesc ≡ p −2ϕ,(10) whereϕdenotes the gravitational potential of the compressed cloud. In this study, for simplicity, the compressed cloud is mod- eled as a sphere. In this case, for a point(x, y, z)located outside the cloud, the escape velocity is expressed as Vesc = r 2GMhub r ,(11) whererdenotes the distance between the center of mass of one of the four non-colliding segments and the center of the compressed"},{"citing_arxiv_id":"2605.19217","ref_index":11,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Taking Inventory of the Most Promising Lensed Radio Sources for Constraining Fundamental Properties of Dark Matter","primary_cat":"astro-ph.CO","submitted_at":"2026-05-19T00:43:42+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Reports results from two searches for new radio lenses in existing surveys and discusses the completeness of the population usable for constraining dark matter properties via astrometric perturbations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17708","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"BISTRO Survey: Gravity-Dominated and Magnetically Regulated Star Formation in M17 SW","primary_cat":"astro-ph.GA","submitted_at":"2026-05-18T00:07:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"High-resolution magnetic field maps of M17 SW reveal gravity-dominated energy budget with magnetic fields regulating collapse and accretion channels in a near-equipartition state.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17377","ref_index":41,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Precise and Rapid Parameter Inference of Kilonova with Conditional Variational Autoencoder","primary_cat":"astro-ph.HE","submitted_at":"2026-05-17T10:40:18+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A conditional variational autoencoder is trained on public kilonova light curves to enable rapid parameter inference for binary neutron star merger models in under three hours total.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17195","ref_index":18,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the Nature of Candle-Flame-Shaped Solar Flares and Sub-Alfv\\'enic Supra-Arcade Plasma Downflows","primary_cat":"astro-ph.SR","submitted_at":"2026-05-16T23:40:23+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":"2605.17040","ref_index":28,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"PEARLS: JWST Counterparts of Micro-Jy Radio Sources in the NEP Time Domain Field. II. All Four Spokes","primary_cat":"astro-ph.GA","submitted_at":"2026-05-16T15:21:05+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"JWST finds infrared counterparts for nearly all micro-Jy radio sources, with star formation explaining the radio output in roughly 79% of cases after accounting for non-linear luminosity relations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.17024","ref_index":237,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The ${}^{13}\\mathrm{CO}(2{-}1)/^{12}\\mathrm{CO}(2{-}1)$ Line Ratio from 100 Molecular Clouds in the Large Magellanic Cloud","primary_cat":"astro-ph.GA","submitted_at":"2026-05-16T14:53:41+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Observational study of 100 LMC GMCs finds median 13CO(2-1)/12CO(2-1) line ratio of 0.078, nearly linear with luminosity, and higher in clouds hosting IR-bright young stellar objects.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.16495","ref_index":196,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A 14-year-old Mystery: The Peculiar Case of the Engine-driven SN 2012ap","primary_cat":"astro-ph.HE","submitted_at":"2026-05-15T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Late-time radio rebrightening in SN 2012ap is consistent with either progenitor mass-loss variation producing a density enhancement or an off-axis energetic jet viewed at large angle, potentially reclassifying it as GRB-like rather than weakly engine-driven.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13966","ref_index":135,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Massive Galaxies Form Early and Gray: Stellar Assembly and Dust Attenuation at $\\mathbf{z>3.5}$ from CAPERS","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T18:00:04+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Massive galaxies at z>3.5 assembled stars earlier than theoretical models predict and exhibit gray dust attenuation, especially at the highest masses.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13514","ref_index":10,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"COOL-LAMPS IX: A Rare Duo of Quasars Each Lensed by a Single Massive Galaxy Cluster","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T13:33:24+00:00","verdict":"ACCEPT","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"A single galaxy cluster lenses two quasars (one Type I at z=1.524, one dust-obscured Type II at z=1.939) into four images each, yielding a projected mass of ~3.3e14 solar masses within 500 kpc and time delays of hundreds to over 1000 days.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.11074","ref_index":97,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":1,"top_context_role":"background","top_context_polarity":"background","context_text":"and agree with former ones in Hannaford et al. (1985), which were used to successfully reproduce the solar meteoritic abun- dance A(Nb)=1.41 dex (Anders & Ebihara 1982). Despite some blending, both lines yield consistent abundances (see Fig- ure C.1). Biases arising from 1D LTE modelling and noise ef- fects cannot be ruled out as contributing to an overestimation. 17 IAU 2015 RESOLUTION B3 18 https://github.com/casaluca/bolometric-corrections 19 Online toolhttps://irsa.ipac.caltech.edu/applications/ DUST/ 20 Using the codeColte(Casagrande et al. 2021) athttps://github. com/casaluca/colte. Article number, page 14 of 18 R. E. Giribaldi et al.: Observational Signatures and Constraints on the Intermediate Neutron-Capture Process"},{"citing_arxiv_id":"2605.08353","ref_index":116,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Empirical estimates of how massive galaxies can be in {\\Lambda}CDM","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T18:05:26+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Corrected empirical limits show the most massive galaxies never exceed the theoretical baryonic maximum of 0.16 times halo virial mass, keeping observations consistent with LambdaCDM at all redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2502.11625","ref_index":50,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Comparative Analysis of EMCEE, Gaussian Process, and Masked Autoregressive Flow in Constraining the Hubble Constant Using Cosmic Chronometers Dataset","primary_cat":"astro-ph.CO","submitted_at":"2025-02-17T10:15:22+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":3.0,"formal_verification":"none","one_line_summary":"EMCEE outperforms GP and MAF in recovering true H0 from mock cosmic chronometer datasets, with GP most sensitive to data points via delete-d jackknife analysis.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}