2018MNRAS.476.5016L -
Mon. Not. R. Astron. Soc., 476, 5016-5025 (2018/June-1)
Early growth of typical high-redshift black holes seeded by direct collapse.
LATIF M.A., VOLONTERI M. and WISE J.H.
Abstract (from CDS):
Understanding the growth of high-redshift massive black holes (MBHs) is a problem of great astrophysical interest. The most luminous quasars at z > 6 are frequently observed but they represent only the tip of the iceberg as the majority of the low-luminosity active galactic nuclei (AGN) population remains undetected. In this study, we perform a radiation hydrodynamics cosmological simulation to study the growth of 'normal' black holes in the high-redshift universe. In our simulation, we model the formation of Pop III and Pop II stars along with their chemical, mechanical, and radiative feedback. We consider both UV and X-ray emission from an accreting BH to simulate its radiative feedback. The selected halo has a mass of 3 ×1010 M☉ at z = 7.5 and we turn on radiative feedback from a MBH seed of 10^5 M^☉ along with in situ star formation at z = 12 when the halo mass reaches well above the atomic cooling limit. We find that the MBH accretes only about 2200 M☉ during 320 Myr and the average mass accretion on to the MBH is a few times 10–6 M☉yr–1. Our results suggest that the stunted growth of MBH is a consequence of supernovae in tandem with MBH feedback which drive large outflows and evacuate the gas from MBH vicinity. This may explain why a population of low-luminosity AGN has not been detected so-far at z > 6; the large contrast between the star formation rate and the MBH accretion rate may make then hard to detect even in upcoming deep surveys.
Abstract Copyright:
© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Journal keyword(s):
black hole physics - methods: numerical - galaxies: formation - early Universe - cosmology: theory
Simbad objects:
1
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