Close compact pairs mark ~67% of known Little Red Dots and both high-redshift BLAGNs in the A2744 field, suggesting merger-driven accretion at high redshift.
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Derives GR jump conditions and self-similar shock solutions for SIS collapse to BH, showing shocks up to 0.4c, accretion suppressed by factor 5-7, and shock energy release ~10% of enclosed rest mass.
LRDs are interpreted as high-inclination hyper-Eddington accreting SMBHs analogous to SS 433, with V-shaped SEDs, X-ray weakness, and Balmer breaks emerging from disk self-shielding geometry.
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.
UV-bright companions to Little Red Dots provide Lyman-Werner fluxes of J21 ~ 10^2.5-10^5 that can suppress H2 cooling and enable direct collapse to massive black holes.
JWST NIRSpec observations of high-redshift galaxies reveal spatial offsets in ionization structure for 12 out of 90 sources, proposed as signatures of wandering black holes.
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.
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.
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.
LILA can detect IMBH binaries at redshifts 20-30, IMRIs, and provide months-to-years early warnings with high-SNR events for gravity tests.
Little red dots are the dust-reddened, high-inclination counterparts of little blue dots under a super-Eddington unification model, with luminosity-dependent fractions peaking near 20% and obscured systems showing systematically higher black hole masses due to selection.
A PBH fraction of about 0.1 as dark matter, with 1% in stellar-mass range, produces the observed SGWB amplitude via dynamical friction and hierarchical mergers while explaining JWST early SMBHs.
Non-LTE wind atmosphere models computed with CMFGEN reproduce the SED and Balmer decrement of most Little Red Dots when dust-attenuated with Av ~2, while predicting Fe II, O I, and Ca lines, but struggle to produce both a genuine Balmer break and strong lines simultaneously.
Simulations and analytic modeling predict that the supermassive black hole to stellar mass ratio peaks at several percent around redshift 7-10 before declining toward the present day.