How Rapidly Do Supermassive Black Hole “Seeds” Grow at Early Times?

We investigate the physical conditions for the growth of intermediate mass seed black holes assumed to have formed from remnants of the first generation of massive stars. We follow the collapse of high-sigma halos with Tvir > 1e4 K using cosmological, smooth-particle hydrodynamic (SPH) simulations in the standard LCDM model. During collapse of the parent halo the seed holes are incorporated through mergers into larger systems and accrete mass from the surrounding gas. We include a self-consistent treatment of star formation, black hole accretion and associated feedback processes. Even under optimistic assumptions for the seed black hole mass and for efficient merger rates, we find that seed holes in halos M6, are therefore hard to meet in such a scenario. Without a 'jump-start' these conditions may be only achieved in extremely rare halos with Mₕalo > 1e13 Msun that collapsed before z~6. The sub-Eddington regime in which black holes holes accrete at early time implies a small contribution to the reionization by miniquasar but still sufficient to cause appreciable heating of the IGM at z<15-18.