The off-centered extended emission near three little red dots is physically associated with the dots, and for two sources it is best explained as low-density, metal-poor nebular gas photoionized by the dot's ultraviolet radiation.
Clump-fed black hole growth in the first billion years of the universe
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abstract
Understanding how supermassive black holes (SMBHs) form in the early universe is one of the most challenging problems in astrophysics. Their high abundance in the first billion years, as observed by the James Webb Space Telescope, hints towards black hole seeds that accrete mass rapidly. The origin of this accreted mass is not known. Here, we consider a billion solar mass clumpy galaxy at z=5.48 with a 30 million solar mass black hole in the center. We show that the clumps should migrate to the central region because of torques from dynamical friction with the halo, funneling in at least 14 solar masses per year. This is fast enough to grow the observed SMBH, with only 1% of the accreted mass getting in and the rest going to a bulge. Clump-fed accretion could explain most young SMBHs because young galaxies are highly irregular with massive star-forming clumps.
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The Physical Nature of the Off-centered Extended Emission Associated with the Little Red Dots
The off-centered extended emission near three little red dots is physically associated with the dots, and for two sources it is best explained as low-density, metal-poor nebular gas photoionized by the dot's ultraviolet radiation.