{"total":17,"items":[{"citing_arxiv_id":"2606.30711","ref_index":8,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Little Red Dots as Intermediate Mass, Super-Eddington Engines: Insights from Type IIn Supernovae and The 1837-1856 Great Eruption of $\\eta$ Carinae","primary_cat":"astro-ph.GA","submitted_at":"2026-06-29T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"UNKNOWN","novelty_score":6.0,"formal_verification":"none","one_line_summary":"LRDs are reinterpreted as intermediate-mass super-Eddington systems with wind-driven pseudo-photospheres that explain their spectra and imply engine masses below 10^5 solar masses rather than overmassive black holes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.23778","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Constraints on the Gas Geometry Surrounding Little Red Dots through Narrow-Line Diagnostics","primary_cat":"astro-ph.GA","submitted_at":"2026-06-22T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Narrow-line diagnostics on ~20 LRDs indicate that stellar photoionization alone cannot explain the observed ratios in many objects, implying anisotropic ionizing radiation from complex gas geometry.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.21614","ref_index":99,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Little Red and Blue Dots: AGN-excited narrow lines, Lyman-$\\alpha$ emission, and resemblance to standard quasars","primary_cat":"astro-ph.GA","submitted_at":"2026-06-19T17:18:13+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"JWST data on LRDs and LBDs show AGN-like excitation, strong Lyα with broad components, and X-ray weakness, implying clumpy or equatorial geometries around growing black holes rather than complete gas envelopes.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.17271","ref_index":65,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Black Hole Stars Across the Universe: Identifying Central Engine Dominated Little Red Dots at $z\\sim1.5-9.5$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-15T20:31:54+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"New template-fitting selection yields 241 BH*-dominated LRD candidates at z~1.7-9.3 with number density peaking at z~5-6, demonstrating persistence to lower redshifts.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.12355","ref_index":154,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Between Degeneracy and Evolution: UV-to-optical Insights into the BH$^*$ Model in Little Red Dots","primary_cat":"astro-ph.GA","submitted_at":"2026-06-10T17:27:12+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Bayesian continuum fitting of 66 LRDs shows the BH* model fits ~6% best, rising to ~40% under AGN-disfavoring priors, with most objects stellar/AGN-dominated and possible evolutionary trends.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.09970","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Through the Veil: Ly$\\alpha$ Illuminates the Host Galaxies of Little Red Dots","primary_cat":"astro-ph.GA","submitted_at":"2026-06-08T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Lyα observations of Little Red Dots show luminosities and equivalent widths like normal star-forming galaxies but lower Lyα/Hα ratios and extended asymmetric emission, supporting a two-component model with host-scale gas.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.06585","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Population of Red Galaxies with Very Strong Emission Lines at $z > 5$ Revealed by the NIRCam Medium Bands: ''Classic'' LRDs, Dusty Star-Forming Galaxies, and a Missing Population of LRDs","primary_cat":"astro-ph.GA","submitted_at":"2026-06-04T18:00:02+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Medium-band imaging reveals red emission-line galaxies at z>5 including compact objects likely missed by classic Little Red Dot selection criteria.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2606.03522","ref_index":3,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The UV Side of Little Red Dots: Red, Compact, and Iron-Enhanced Rest-UV Emission with a Strong Downturn around Ly$\\alpha$","primary_cat":"astro-ph.GA","submitted_at":"2026-06-02T11:44:29+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Analysis of ~100 JWST LRDs finds redder, compact UV emission with Fe II/Mg II ~8-10 and correlations suggesting central red continuum (β_UV~0) beyond host galaxy contribution.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.29895","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Transient Signatures of Star-Envelope Collisions in Little Red Dots","primary_cat":"astro-ph.HE","submitted_at":"2026-05-28T13:19:59+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Red supergiant collisions with massive gaseous envelopes around SMBHs in LRDs can produce detectable transients at rates up to ~0.3 yr^{-1} per LRD for compact clusters of size ≲10 pc.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.24112","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"The Lumina Project: The Demographics of Active Galactic Nuclei from Quasars to Little Red Dots at $z\\geq 3$","primary_cat":"astro-ph.GA","submitted_at":"2026-05-22T18:18:11+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":5.0,"formal_verification":"none","one_line_summary":"Lumina simulation plus empirical SMBH-to-AGN mapping reproduces observed high-z quasar and LRD luminosity functions and places the population in a self-consistent reionization context.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21589","ref_index":2,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"A Magnetized Black Hole Envelope Model for Little Red Dots","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:00:03+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"A theoretical model of a magnetized black hole envelope is developed to explain the broad emission lines and X-ray faintness observed in little red dots using co-rotating plasma clumps and limited X-ray sources.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2605.21574","ref_index":6,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"(LRDs)$^2$: The Low-ReDshift Little Red Dots Survey. II. DESI DR1 Sample","primary_cat":"astro-ph.GA","submitted_at":"2026-05-20T18:00:00+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"The survey identifies 27 low-redshift LRDs with compact morphology, V-shaped continua, broad Balmer lines with extreme decrements, and ubiquitous outflows, matching high-z counterparts and yielding a number density lower limit of 7.5e-10 cMpc^-3.","context_count":1,"top_context_role":"method","top_context_polarity":"use_method","context_text":"In contrast, its ZTFgandrlight curves over the over- lapping 2018-2026 window are consistent with constant flux. We construct the structure function (SF; P. A. Hughes et al. 1992; S. Collier & B. M. Peterson 2001; A. Bauer et al. 2009; S. Koz lowski et al. 2010) and fit it with a power law (N. Palanque-Delabrouille et al. 2011): SF ∆trest \u0001 =A \u0012∆trest 1 yr \u0013γ .(6) As shown in the right panel of Figure 15, J1717+3807's ZTFiband shows a weakly significant rise. Both W1 and W2 exhibit an SF slope index ofγ≃1, signifi- cantly steeper than the expectation from a damped ran- dom walk model (γ∼0.5 on timescales shorter than the characteristic timescales; C. L. MacLeod et al. 2010). The SF of J1717+3807 indicates that its vari-"},{"citing_arxiv_id":"2605.07976","ref_index":2,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"Testing the BH$^*$ Model: a UV-to-Optical Spectral Fitting of The Cliff","primary_cat":"astro-ph.GA","submitted_at":"2026-05-08T16:34:53+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":6.0,"formal_verification":"none","one_line_summary":"Spectral fitting of The Cliff LRD with Bagpipes yields a BH*-like solution with a low-mass metal-poor host, moderate dust, smooth star formation history, and high BH-to-stellar mass ratio.","context_count":1,"top_context_role":"background","top_context_polarity":"background","context_text":"However, this setting does not yield a robust fit, as highlighted by the residuals and the reducedχ2 val- ues, emphasizing the need for the inclusion of the absorption component. - Stars+Nebular emission+Dust attenuation The stellar metallicity prior was set to span logZ/Z ⊙ = [0.001, 0.05] in the BH ∗+dust-free host configuration, forc- ing a low-Zsolution, and extended to [0.001, 2.5] in the BH∗+dusty host configuration. In terms of stellar mass, LRD hosts are expected to be low-mass sources (see Sect. 1), withM ⋆ ∼10 7−8 M⊙. In the BH ∗+dust-free host configuration, logM ⋆/M⊙ was set to span [4.0,8.5]. In the BH ∗+dusty host mode, this prior was broadened to [4.0,10.0]. Nebular emission was incorporated through the ionization"},{"citing_arxiv_id":"2604.03370","ref_index":1,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Holes in the BH$^\\star$? AGN signatures in the FUV spectrum of a black-hole dominated Little Red Dot at $z=7.04$","primary_cat":"astro-ph.GA","submitted_at":"2026-04-03T18:00:17+00:00","verdict":"ACCEPT","verdict_confidence":"MODERATE","novelty_score":6.0,"formal_verification":"none","one_line_summary":"FUV observations of a z=7.04 Little Red Dot show broad Lyα from the BLR and fluorescence, implying holes or clumpiness in the proposed dense covering gas.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2602.12548","ref_index":5,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"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":"2602.06954","ref_index":4,"ref_count":1,"confidence":0.98,"is_internal_anchor":true,"paper_title":"Spectral Appearance of Self-gravitating Disks Powered by Stellar Objects: Universal Effective Temperature in the Optical Continuum and Application to Little Red Dots","primary_cat":"astro-ph.HE","submitted_at":"2026-02-06T18:51:45+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Self-gravitating disks heated by stars reach a universal optical effective temperature of 4000-4500 K independent of accretion rate, black hole mass, and viscosity, explaining Little Red Dots.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null},{"citing_arxiv_id":"2508.18358","ref_index":6,"ref_count":1,"confidence":0.9,"is_internal_anchor":true,"paper_title":"The Missing Hard Photons of Little Red Dots: Their Incident Ionizing Spectra Resemble Massive Stars","primary_cat":"astro-ph.GA","submitted_at":"2025-08-25T18:00:05+00:00","verdict":"UNVERDICTED","verdict_confidence":"LOW","novelty_score":7.0,"formal_verification":"none","one_line_summary":"Little Red Dots show soft ionizing spectra consistent with massive stars, based on high H-alpha EWs and low HeII/H-beta ratios that rule out hard AGN spectra via Cloudy modeling.","context_count":0,"top_context_role":null,"top_context_polarity":null,"context_text":null}],"limit":50,"offset":0}