2026ApJ..1000...90I

The birth of seeds of massive black holes (BHs) and nascent galaxies at cosmic dawn takes place in dense gaseous environments, which play a crucial role in shaping their coevolution and radiation spectra. We investigate gas accretion during the assembly of massive halos with M_h ≳ 10¹⁰-10¹¹M_⊙ at redshifts z ≃ 4-10, driving both rapid BH feeding and concurrent nuclear starbursts. As the BH grows to ∼10⁶-10⁷M_⊙ via super-Eddington accretion, the accretion power inflates a dense envelope whose effective temperature approaches the Hayashi limit at T_eff ≃ 5000 K, producing red optical emission, while a coeval young stellar population of ∼10⁷M_⊙ provides blue UV emission. This early coevolving system naturally reproduces the characteristic spectral features of the so-called little red dots (LRDs), a population of broad-line active galactic nuclei (AGNs), including the V-shaped UV-to-optical spectra and weakness of X-ray, infrared, and radio emission. Massive stars in the nuclear starburst soon explode as supernovae, injecting energy and momentum that expel gas from the nucleus, quench gas supply to the BH envelope, and ultimately drive a transition into normal AGN phases. For individual LRDs, the optical-to-UV luminosity ratio remains nearly constant at L_opt/L_UV ≃ 2-10 from the onset of accretion bursts for ≃15 Myr, one-third of the Salpeter time, until quenching by stellar feedback. While this ratio is sustained for the LRD population at z ≃ 4-8, it declines toward lower redshifts, as BHs can no longer maintain red envelopes, thereby losing the LRD characteristics.