{"total":12,"items":[{"citing_arxiv_id":"2606.31998","ref_index":235,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Radiation-pressure instability is an artifact of constant-$\\alpha$ closure","primary_cat":"astro-ph.HE","submitted_at":"2026-06-30T17:33:19+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Requiring thermal stability and single-valuedness in the thin-disk Ṁ-Σ plane produces a viscosity law α(X) with X = P_gas/P_rad that eliminates the radiation-pressure dominated instability while preserving the effective-temperature profile.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.31515","ref_index":208,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The metallicities of little red dot host galaxies: LRDs are metal poor, but not pristine","primary_cat":"astro-ph.GA","submitted_at":"2026-06-30T11:29:36+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"LRD host galaxies show average metallicity 0.08 Z_sun with narrow stable range, challenging pristine-gas formation models while ruling out typical local AGN.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23476","ref_index":206,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"TeV-PeV Gamma-ray and Neutrino Emission in the Galactic Plane","primary_cat":"astro-ph.HE","submitted_at":"2026-06-22T15:22:06+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":3.0,"formal_verification":"none","one_line_summary":"Alternative ISRF models produce only modest changes to the LHAASO diffuse gamma-ray fit; the associated pp neutrinos remain consistent with IceCube all-sky data and compatible with ANTARES/KM3NeT limits.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.13393","ref_index":39,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Direct detection of cool molecular gas in a star-forming galaxy at $z=7.31$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-11T14:24:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Direct detection of CO(3-2) at z=7.31 in REBELS-25 gives M_mol ~ 10^11 M_sun with f_gas ~0.95, confirming a massive molecular reservoir and showing low-J CO remains detectable in the Epoch of Reionization.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.10027","ref_index":160,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Learning the Universe: The Structure of Dust Attenuation Curves in Galaxy Simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T18:08:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Four parameters suffice to describe dust attenuation curve diversity in TNG simulations, yielding a new symbolic-regression model that recovers curves and fluxes better than existing parameterizations while linking parameters to SFR surface density, metallicity, and geometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06108","ref_index":212,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Grain-size evolution and rapid dust growth in high-redshift galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T12:53:53+00:00","verdict":"CONDITIONAL","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"A multiphase ISM grain-size model with low supernova dust yield reproduces observed dust-to-stellar mass ratios and UV luminosity functions at z=7-12 by letting small grains seed rapid metal accretion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.01088","ref_index":15,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The First Glimpse of Water Ice Absorption Map in the Milky Way","primary_cat":"astro-ph.GA","submitted_at":"2026-05-31T08:16:14+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":8.0,"formal_verification":"none","one_line_summary":"The paper derives the first Milky Way-scale map of water ice absorption in the W1 band from photometric color corrections, validated against spectroscopic measurements.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.19661","ref_index":174,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"COSMOS-Web: Star formation along the early Hubble sequence and the evolution of dust over the redshift range 0<z<12","primary_cat":"astro-ph.GA","submitted_at":"2026-05-19T10:55:34+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Stacking analysis shows mean SFR in massive galaxies at 2<z<4.5 declines along the Hubble sequence from ~280 M⊙/yr in irregulars to ~80 M⊙/yr in spheroids, with a simple chemical evolution model explaining the rise in dust-to-stellar mass ratio out to z~8.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18062","ref_index":230,"ref_count":2,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Chemistry and IR emission of acetylene in planet-forming regions of T Tauri disks. Impact of elemental abundances and dust properties","primary_cat":"astro-ph.EP","submitted_at":"2026-05-18T08:48:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Updated DALI models reproduce observed C2H2 fluxes with solar C/O and find the C2H2/H2O flux ratio sensitive to elemental abundances and small-grain abundance in planet-forming disk regions.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.15263","ref_index":71,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"On the quenching of LRD X-ray emission by both Compton-thick gas and high accretion rates","primary_cat":"astro-ph.GA","submitted_at":"2026-05-14T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"LRDs require Compton-thick gas at moderate metallicity plus high accretion rates producing weak X-rays to explain their non-detection, implying they are not chemically pristine.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.13966","ref_index":104,"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":"2605.13472","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"First Light And Reionization Epoch Simulations (FLARES) XXI: The UV Indices of Galaxies in the Early Universe","primary_cat":"astro-ph.GA","submitted_at":"2026-05-13T12:59:22+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":4.0,"formal_verification":"none","one_line_summary":"Simulations of high-redshift galaxies show the 1719 Å UV index reliably traces stellar metallicity while others are more sensitive to star formation history.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"2015), it does not necessarily trace the metallic- ity of the young or UV-bright stars that dominate the formation of UV absorption features. The upper panel of Figure 9 shows the UV-luminosity- weighted metallicity,Z UV, as a function of the to- tal mass-weighted stellar metallicity,Z total. The UV- weighted metallicity is defined as ZUV = P i Li,UVZiP i Li,UV ,(5) whereL i,UV andZ i denote the intrinsic UV luminos- ity and metallicity of thei-th stellar particle, respec- tively. This weighting more directly traces the stellar populations responsible for shaping UV absorption in- dices. Each point corresponds to a singleFlaresgalaxy, weighted by total stellar mass (∼10 8-1011 M⊙). A strong positive correlation is observed, with the binned"}],"limit":50,"offset":0}