{"total":11,"items":[{"citing_arxiv_id":"2606.28497","ref_index":150,"ref_count":1,"confidence":0.88,"is_internal_anchor":true,"paper_title":"Stellar discs and intermediate-mass black holes in galactic nuclei I. Fragmenting the disc in an isotropic stellar potential","primary_cat":"astro-ph.GA","submitted_at":"2026-06-26T18:00:08+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Simulations demonstrate that a retrograde IMBH with mass ratio ~0.67 to the disc mass fragments a stellar disc into inner, misaligned, and outer components within 10-20 Myr.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.11939","ref_index":37,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Detection of a parsec-scale, compact, and fading ejecta from an accreting massive black hole","primary_cat":"astro-ph.HE","submitted_at":"2026-06-10T11:11:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"VLBI at 4.9 GHz plus multi-epoch survey data reveal a fading parsec-scale radio component near the optical center of a dwarf galaxy, interpreted as transient ejecta from IMBH accretion.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.05808","ref_index":124,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Galaxy morphology dependent (black hole mass)-(velocity dispersion) relations: implications for gravitational wave forecasts and cosmological simulations","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T07:39:50+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Morphology-dependent M_bh-σ0 relations are reported: shallow (2.5-3.1) for dust-poor S0 galaxies and steep (7.8) for massive ellipticals, using new SCOPE Bayesian regression on 137 galaxies.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.04090","ref_index":48,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Mapping the nuclear environments of extreme coronal line emitting galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Multi-epoch spectroscopy of 33 ECLEs shows coronal lines emitted at intermediate radii with log(distance)-log(black hole mass) slopes of 0.63 and 0.69 for [O III] and [Fe VII], consistent with photoionization setting the radii.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.02699","ref_index":115,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A New Record Census of Dwarf AGN and a Bimodal $M_{\\rm BH}$-$M_{\\star}$ Scaling Relation with DESI DR1","primary_cat":"astro-ph.GA","submitted_at":"2026-06-01T18:00:00+00:00","verdict":"CONDITIONAL","verdict_confidence":"UNKNOWN","novelty_score":6.0,"formal_verification":"none","one_line_summary":"DESI DR1 yields 314k high-mass and 9.6k dwarf AGN, extending the M_BH-M_star relation to log M_star ~7.8 and suggesting two evolutionary pathways for galaxies and black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.00992","ref_index":53,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Understanding the Broad-line Region of Active Galactic Nuclei with Photoionization. II. Slim disks, Self-shadowing, and BLR sizes","primary_cat":"astro-ph.GA","submitted_at":"2026-05-31T04:15:31+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Slim-disk self-shadowing plus accretion-rate-dependent BLR density enhancement explains the observed offsets of high-Eddington AGNs below the canonical R-L relation.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.18161","ref_index":289,"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":"2605.11083","ref_index":215,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"FLAMINGO: The thermal history of the Universe from tSZ effect cross-correlations and its dependencies on cosmology and baryon physics","primary_cat":"astro-ph.CO","submitted_at":"2026-05-11T18:00:10+00:00","verdict":"CONDITIONAL","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"tSZ cross-correlations with large-scale structure tracers prefer low S8 and strong baryonic feedback, yielding S8 = 0.72 and low group baryon fraction in FLAMINGO simulations.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.03577","ref_index":134,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Optical Variability Structure Function of Low-Luminosity AGN using ATLAS Lightcurves","primary_cat":"astro-ph.GA","submitted_at":"2026-05-05T09:45:16+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Low-luminosity AGN exhibit structure function slopes rising from 0.1 to 0.3 with black hole mass, no breaks on decadal scales, amplitude anticorrelated with luminosity and positively correlated with mass.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.02663","ref_index":286,"ref_count":2,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Jet-driven shocks and turbulence in radio-loud Active Galactic Nuclei observed with JWST MIRI/MRS","primary_cat":"astro-ph.GA","submitted_at":"2026-05-04T14:43:32+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST spectroscopy reveals radio jets in nearby AGN drive multiphase ISM turbulence and shock-dominated H2 excitation both along and perpendicular to the jet direction.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2604.25560","ref_index":108,"ref_count":1,"confidence":0.88,"is_internal_anchor":false,"paper_title":"Massive black holes and their galaxies","primary_cat":"astro-ph.GA","submitted_at":"2026-04-28T12:31:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":0.0,"formal_verification":"none","one_line_summary":"A review summarizing detection methods, population statistics, and coevolution of supermassive black holes with host galaxies from early universe observations and simulations.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"Note that accretion disc simulations have shown that BH can easily achieve super-Eddington accretion rates if fed at sufficiently high rates from the galaxy (Inayoshi et al., 2020), providing in principle a formation pathway for SMBH observed at high redshift (Schneider et al., 2023). There are observations of potentially Super- 8Massive black holes and their galaxies -3 -2 -1 0 log10([Lbol / LEdd) 0.001 0.010 0.100 1.000Fraction of sources D(4000) < 1.4 106.75 < MBH < 107.00 107.00 < MBH < 107.25 107.25 < MBH < 107.50 107.50 < MBH < 107.75 107.75 < MBH < 108.00 D(4000) > 1.7 107.0 < MBH < 107.5 107.5 < MBH < 108.0 108.0 < MBH < 108.5 108.5 < MBH < 109.0 Fig. 3Distribution of Eddington ratiosλ Edd for AGN in the local Universe split into star-forming galaxies (blue) and quenched galaxies (red) from Heckman and Best (2014). More massive BH (lighter colours) have lower Eddington ratios for both popula- tions. Modified with permission from the Annual Review of Astronomy and Astrophysics, Volume 58 © 2020 by Annual Reviews, http://www.annualreviews.org Eddington MBH in the early Universe (Trakhtenbrot et al., 2011; Lupi et al., 2024). Unfortunately, cosmological simulations suggest that the conditions for sustained super-Eddington accretion are rare even in the early Universe (Regan et al., 2019; Massonneau et al., 2023) and that allowing for Super-Eddington accretion can actually stunt MBH growth in the long run due to strong feedback effects. 4.2 Massive black hole growth in the local Universe In the local Universe, both accretion modes are present but they are not uniformly distributed with BH mass. The highest Eddington ratios are found for MBH in the mass range 10 6 −10 8 M⊙ which accrete in the radiatively efficient quasar mode (Heckman et al., 2004). Peak Eddington ratios for radiatively efficient AGN in the local Universe rarely exceedλEdd =0.1, with 99.8 % of AGN having Eddington ratios smaller than that (see Fig. 3) (Heckman et al., 2004). When study"}],"limit":50,"offset":0}