Massive black holes as population III remnants

被引:787
作者
Madau, P [1 ]
Rees, MJ
机构
[1] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
[2] Osserv Astrofis Arcetri, I-50125 Florence, Italy
[3] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England
基金
美国国家航空航天局;
关键词
black hole physics; cosmology : theory; early universe; galaxies : formation;
D O I
10.1086/319848
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Recent numerical simulations of the fragmentation of primordial molecular clouds in hierarchical cosmogonies have suggested that the very first stars (the so-called Population III) may have been rather massive. Here we point out that a numerous population of massive black holes (MBHs)-with masses intermediate between those of stellar and supermassive holes-may be the end product of such an episode of pregalactic star formation. If only one MBH with m(.) greater than or similar to 150 M. formed in each of the "minihalos" collapsing at z approximate to 20 from 3 sigma fluctuations, then the mass density of Population III MBHs would be comparable to that of the supermassive variety observed in the nuclei of galaxies. Since they form in high-sigma rare density peaks, relic MBHs are predicted to cluster in the bulges of present-day galaxies as they become incorporated through a series of mergers into larger and larger systems. Dynamical friction would cause greater than or similar to 50 (m(.) /150 M.)(1/2) such objects to sink toward the center. The presence of a small cluster of MBHs in galaxy nuclei may have several interesting consequences associated with it, such as tidal captures of ordinary stars (likely followed by disruption), MBH capture by the central supermassive black hole, and gravitational wave radiation from such coalescences. Accreting pregalactic MBHs may be detectable as ultraluminous, off-nuclear X-ray sources.
引用
收藏
页码:L27 / L30
页数:4
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