The formation of supermassive black holes from Population III.1 seeds. I. Cosmic formation histories and clustering properties

Journal Article · 05 December 2018 · Monthly Notices of the Royal Astronomical Society

DOI: https://doi.org/10.1093/mnras/sty3298 · OSTI ID:1488992

Banik, Nilanjan  ^[1]; Tan, Jonathan C ^[2]; Monaco, Pierluigi ^[3]

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1. Univ. of Florida, Gainesville, FL (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Univ. of Amsterdam (Netherlands). GRAPPA Institute; Leiden Univ. (Netherlands)
2. Chalmers University of Technology, Gothenburg (Sweden); Univ. of Virginia, Charlottesville, VA (United States)
3. Univ. of Trieste (Italy); Istituto Nazionale di Astrofisica (INAF), Trieste (Italy). Osservatorio Astronomico di Trieste; Istituto Nazionale di Fisica Nucleare (INFN), Trieste (Italy)

We calculate cosmic distributions in space and time of the formation sites of the first, ‘Pop III.1’ stars, exploring a model in which these are the progenitors of all supermassive black holes (SMBHs), seen in the centres of most large galaxies. Pop III.1 stars are defined to form from primordial composition gas in dark matter minihaloes with |$${\sim }10^6\, \mathrm{M}_\odot$$| that are isolated from neighbouring astrophysical sources by a given isolation distance, d_iso. We assume Pop III.1 sources are seeds of SMBHs, based on protostellar support by dark matter annihilation heating that allows them to accrete a large fraction of their minihalo gas, i.e. |$${\sim }10^5\, \mathrm{M}_\odot$$|⁠. Exploring d_iso from 10 to |$$100\, \rm {kpc}$$| (proper distances), we predict the redshift evolution of Pop III.1 source and SMBH remnant number densities. The local, |$$z$$| = 0 density of SMBHs constrains |$$d_{\rm {iso}}\lesssim 100\, \rm {kpc}$$| (i.e. |$$3\, \rm {Mpc}$$| comoving distance at |$$z$$| ≃ 30). In our simulated (⁠|$${\sim }60\, \rm {Mpc})^3$$| comoving volume, Pop III.1 stars start forming just after |$$z$$| = 40. Their formation is largely complete by |$$z$$| ≃ 25–20 for d_iso = 100–|$$50\, \rm {kpc}$|⁠. We follow source evolution to |$$z$$| = 10, by which point most SMBHs reside in haloes with |$${\gtrsim }10^8\, \mathrm{M}_\odot$$|⁠. Over this period, there is relatively limited merging of SMBHs for these values of d_iso. We also predict SMBH clustering properties at |$$z$$| = 10: feedback suppression of neighbouring sources leads to relatively flat angular correlation functions.

• Research Organization: Oak Ridge National Laboratory (ORNL), Oak Ridge, TN (United States)
• Sponsoring Organization: European Research Council; National Science Foundation; USDOE
• Grant/Contract Number: 89243024CSC000002; AC02-07CH11359
• OSTI ID: 1488992
• Report Number(s): FERMILAB-PUB-16-322-A-AE-PPD-T; oai:inspirehep.net:1481372; arXiv:1608.04421
• Journal Information: Monthly Notices of the Royal Astronomical Society, Journal Name: Monthly Notices of the Royal Astronomical Society Journal Issue: 3 Vol. 483; ISSN 0035-8711; ISSN 1365-2966
• Publisher: Oxford University PressCopyright Statement
• Country of Publication: United States
• Language: English