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

被引：21

作者：

Banik, Nilanjan ^{[1
,2
,3
,4
,5
]}

Tan, Jonathan C. ^{[6
,7
]}

Monaco, Pierluigi ^{[8
,9
,10
]}

机构：

[1] Univ Florida, Dept Phys, Gainesville, FL 32611 USA

[2] Fermilab Natl Accelerator Lab, Batavia, IL 60510 USA

[3] Univ Amsterdam, Inst Theoret Phys Amsterdam, GRAPPA Inst, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[4] Univ Amsterdam, Delta Inst Theoret Phys, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands

[5] Leiden Univ, Lorentz Inst, Niels Bohrweg 2, NL-2333 CA Leiden, Netherlands

[6] Chalmers Univ Technol, Dept Space Earth & Environm, SE-41293 Gothenburg, Sweden

[7] Univ Virginia, Dept Astron, 530 McCormick Rd, Charlottesville, VA 22904 USA

[8] Univ Trieste, Dipartimento Fis, Sez Astron, Via Tiepolo 11, I-34143 Trieste, Italy

[9] INAF, Osservatorio Astron Trieste, Via Tiepolo 11, I-34143 Trieste, Italy

[10] INAF, Via Valerio 2, I-34127 Trieste, Italy

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2019年 / 483卷 / 03期

基金：

芬兰科学院;

关键词：

astroparticle physics; black hole physics; stars: formation; stars: Population III; galaxies: formation; dark matter; X-RAY SOURCE; 1ST STARS; PRIMORDIAL STAR; DARK-MATTER; COSMOLOGICAL SIMULATIONS; LUMINOSITY FUNCTION; RUNAWAY COLLISIONS; FEEDBACK PROCESSES; DIRECT COLLAPSE; BULGE MASS;

D O I：

10.1093/mnras/sty3298

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 similar to 10(6) M-circle dot 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. similar to 10(5) M-circle dot. Exploring d(iso) from 10 to 100 kpc (proper distances), we predict the redshift evolution of Pop III.1 source and SMBH remnant number densities. The local, z = 0 density of SMBH sconstrains d(iso) less than or similar to 100 kpc (i.e. 3 Mpc comoving distance at z similar or equal to 30). In our simulated (similar to 60 Mpc)(3) comoving volume, Pop III.1 stars start forming just after z = 40. Their formation is largely complete by z similar or equal to 25-20 for d(iso) = 100-50 kpc. We follow source evolution to z = 10, by which point most SMBHs reside in haloes with greater than or similar to 10(8) M-circle dot. 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.

引用

页码：3592 / 3606

页数：15

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