The formation of supermassive black holes from Population III.1 seeds. I. Cosmic formation histories and clustering properties
[1];
- Department of Physics, University of Florida, Gainesville, FL 32611, USA; Fermi National Accelerator Laboratory, Batavia, IL 60510-0500, USA; GRAPPA Institute, Institute for Theoretical Physics Amsterdam and Delta Institute for Theoretical Physics, University of Amsterdam, Science Park 904, NL-1098 XH Amsterdam, the Netherlands; Lorentz Institute, Leiden University, Niels Bohrweg 2, Leiden, NL-2333 CA, the Netherlands
- Department of Space, Earth and Environment, Chalmers University of Technology, SE-412 93 Gothenburg, Sweden; Department of Astronomy, University of Virginia, 530 McCormick Road, Charlottesville, VA 22904-4325, USA
- Dipartimento di Fisica, Sezione di Astronomia, Università di Trieste, via Tiepolo 11, I-34143 Trieste, Italy; INAF – Osservatorio Astronomico di Trieste, via Tiepolo 11, I-34143 Trieste, Italy; INFN, via Valerio 2, I-34127 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 centers of most large galaxies. Pop III.1 stars are defined to form from primordial composition gas in dark matter minihalos with $$\sim10^6\:M_\odot$$ that are isolated from neighboring astrophysical sources by a given isolation distance, $$d_{\rm{iso}}$$. 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., $$\sim10^5\:M_\odot$$. Exploring $$d_{\rm{iso}}$$ from $$10 - 100\:\rm{kpc}$$ (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 $$z\simeq30$$). In our simulated ($$\sim60\:\rm{Mpc}$$)$$^3$ comoving volume, Pop III.1 stars start forming just after $z=40$. Their formation is largely complete by $$z\simeq25$$ to $20$ for $$d_{\rm{iso}}=100$$ to $$50\:\rm{kpc}$$. We follow source evolution to $z=10$, by which point most SMBHs reside in halos with $$\gtrsim10^8\:M_\odot$$. Over this period, there is relatively limited merging of SMBHs for these values of $$d_{\rm{iso}}$$. We also predict SMBH clustering properties at $z=10$: feedback suppression of neighboring sources leads to relatively flat angular correlation functions.
- Research Organization:
- Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
- Sponsoring Organization:
- USDOE Office of Science (SC), High Energy Physics (HEP)
- DOE Contract Number:
- AC02-07CH11359
- OSTI ID:
- 1374712
- Report Number(s):
- arXiv:1608.04421; FERMILAB-PUB-16-322-A-AE-PPD-T; 1481372
- Journal Information:
- Monthly Notices of the Royal Astronomical Society, Vol. 483, Issue 3; ISSN 0035-8711
- Publisher:
- Royal Astronomical Society
- Country of Publication:
- United States
- Language:
- English
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