First spectroscopic variability in a z~7 LRD shows rapid changes in both narrow and broad line regions, implying direct ionization from the central source to surrounding nebular gas.
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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.
Derives idealized P-L-T relation from hydrostatic envelope model for LRDs and uses sparse data to obtain preliminary H0 = 120.7 with large errors as proof-of-concept.
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.
Confirmation of 77 new heavily reddened quasars at 1.5 < z < 3.9 with high luminosities and extinctions, showing they are deficient in hot and warm dust relative to blue quasars and supporting a blow-out feedback phase.
Little Red Dots can contribute ~30% of the diffuse neutrino background at TeV-sub-PeV energies through photomeson production in black hole envelopes, with modified flavor ratios at higher energies.
LRDs transition from underdense low-halo-mass environments at z>4 to typical galaxy conditions by z~3.5, with halo growth leading to larger sizes and SED changes that explain their disappearance at lower redshifts.
Primordial black holes and heavy astrophysical seeds with super-Eddington accretion reproduce JWST-observed black hole masses, stellar masses, and low metallicities at z~7-10, while light seeds with Eddington-limited accretion are ruled out; PBHs uniquely show a decreasing black hole-to-stellar mass
Coevolving super-Eddington black holes and nuclear starbursts in high-redshift halos naturally generate the V-shaped UV-to-optical spectra and weak high-energy emission of little red dots.
A source 660 million years after the Big Bang is interpreted as a black hole star with a dust-free dense gas atmosphere, implying Little Red Dots have black hole masses overestimated by orders of magnitude.
Five LRDs at z≈2 yield number density ≈7×10^{-6} cMpc^{-3}, confirming a decline from the z≈5 peak but gentler than prior photometric estimates.
A sample of 36 spectroscopically confirmed LRDs shows broad-line detections in >90%, spectral variety including Balmer breaks and blackbody fits, H-alpha to 5100A continuum correlation, no redshift evolution, declining space density toward z~2 opposite normal AGNs, and clustering in ~10^11 solar mas
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.
Super-Eddington accretion boosts predicted LISA detections of high-redshift black hole binaries to ~64 per year while dropping ET detections to ~4 per year, compared to ~32 and ~64 under Eddington-limited growth.
Rapid halo growth in SEEDZ simulations enables heavy black hole seed formation via supermassive stars at a comoving number density of 0.1 cMpc^{-3} by z=10, with most seeds in near-solar metallicity gas.
High-resolution simulations produce compact galaxies where gas inflows and dynamical processes accumulate enough mass in 10 Myr to form ~10^6 solar mass central black holes under 10% feedback efficiency.
A model seeds supermassive black holes from Pop-III stars in mini-halos at z~20-30 with masses 10-10^5 solar masses and grows them via episodic super-Eddington accretion from nuclear bursts, sustained sub-Eddington accretion from sub-clouds, and mergers, producing a multi-piece redshift-dependent M_
Stellar-mass primordial black holes have minor impact on primordial star formation while supermassive ones can seed massive early structures explaining apparent overabundance of high-redshift galaxies.
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