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Title: The Formation of Supermassive Black Holes from Population III.1 Seeds. I. Cosmic Formation Histories and Clustering Properties

Abstract

We calculate the 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). 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., $$\sim 10^5\:M_\odot$$. 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$$: feedback suppression of neighboring sources leads to relatively flat angular correlation functions. Finally, we consider a simple "Str\"omgren" model for $$d_{\rm iso}$, based on ionizing feedback from zero age main sequence supermassive Pop III.1 stars that may be the direct progenitors of SMBHs in this scenario. Such models naturally produce feedback effects on scales of $$\sim100\:$$kpc and thus self-consistently generate a SMBH number density similar to the observed value.

Authors:
; ;
Publication Date:
Research Org.:
Fermi National Accelerator Lab. (FNAL), Batavia, IL (United States)
Sponsoring Org.:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
OSTI Identifier:
1374712
Report Number(s):
FERMILAB-PUB-16-322-A-AE-PPD-T; arXiv:1608.04421
1481372
DOE Contract Number:
AC02-07CH11359
Resource Type:
Journal Article
Resource Relation:
Journal Name: TBD
Country of Publication:
United States
Language:
English
Subject:
79 ASTRONOMY AND ASTROPHYSICS

Citation Formats

Banik, Nilanjan, Tan, Jonathan C., and Monaco, Pierluigi. The Formation of Supermassive Black Holes from Population III.1 Seeds. I. Cosmic Formation Histories and Clustering Properties. United States: N. p., 2016. Web.
Banik, Nilanjan, Tan, Jonathan C., & Monaco, Pierluigi. The Formation of Supermassive Black Holes from Population III.1 Seeds. I. Cosmic Formation Histories and Clustering Properties. United States.
Banik, Nilanjan, Tan, Jonathan C., and Monaco, Pierluigi. Mon . "The Formation of Supermassive Black Holes from Population III.1 Seeds. I. Cosmic Formation Histories and Clustering Properties". United States. doi:. https://www.osti.gov/servlets/purl/1374712.
@article{osti_1374712,
title = {The Formation of Supermassive Black Holes from Population III.1 Seeds. I. Cosmic Formation Histories and Clustering Properties},
author = {Banik, Nilanjan and Tan, Jonathan C. and Monaco, Pierluigi},
abstractNote = {We calculate the 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). 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., $\sim 10^5\:M_\odot$. 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. Finally, we consider a simple "Str\"omgren" model for $d_{\rm iso}$, based on ionizing feedback from zero age main sequence supermassive Pop III.1 stars that may be the direct progenitors of SMBHs in this scenario. Such models naturally produce feedback effects on scales of $\sim100\:$kpc and thus self-consistently generate a SMBH number density similar to the observed value.},
doi = {},
journal = {TBD},
number = ,
volume = ,
place = {United States},
year = {Mon Aug 15 00:00:00 EDT 2016},
month = {Mon Aug 15 00:00:00 EDT 2016}
}