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.
Quasi-star models using Cloudy radiative transfer reproduce the UV-NIR continuum shape, Balmer break, and hydrogen line luminosities in some LRDs when combined with host galaxy emission, but fail to account for broad helium lines and hot dust without added components.
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.
A review of theoretical models for the first stars and observational strategies including JWST searches, near-field studies, and lensing, noting growing candidates and narrowing parameter space.
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