The Formation of Supermassive Black Holes from Low-Mass Pop III Seeds

Details The Formation of Supermassive Black Holes from Low-Mass Pop III Seeds The Formation of Supermassive Black Holes from Low-Mass Pop III Seeds

2011-12-20

arxiv.org/abs/1112.4598v1

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

5 pages, 3 figures, submitted to ApJL

Scientific paper

The existence of 10$^9$ M$_{\odot}$ black holes (BH) in massive galaxies by $z \sim 7$ is one of the great unsolved mysteries in cosmological structure formation. One leading model argues that they originate from much smaller seeds at high redshift and then accrete at the Eddington limit down to the epoch of reionization, which requires that they have constant access to rich supplies of fuel. Because early numerical simulations suggested that many first stars had masses $\gtrsim 100$ M$_{\odot}$, the supermassive black hole (SMBH) seeds in this model were 100 - 300 M$_{\odot}$ black holes formed by Pop III stars at $z \sim 20$. However, there is growing numerical and observational evidence that most Pop III stars were tens of solar masses, not hundreds, and consequently that 20 - 140 M$_{\odot}$ black holes may have been much more plentiful at high redshift. We have examined low-mass Pop III black holes as potential seeds of SMBH and find that the mass range for possible seeds is severely constrained. Progenitors of black holes above $\sim $100 M$_{\odot}$ disperse their fuel supply prior to the birth of the BH. Natal kicks imparted to 20 - 40 M$_{\odot}$ Pop III BHs during formation eject these BHs from their halos and hence their fuel supply, precluding them from constant Eddington-limit growth. Inefficient radiative feedback and halo mass statistics favor early rapid accretion by 40 - 140 M$_{\odot}$ BH, and these may be the characteristic masses of Pop III SMBH seeds.

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