The Assembly of the First Massive Black Holes
The Assembly of the First Massive Black Holes
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DOI：
10.1146/annurev-astro-120419-014455
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发表时间：
2019-11
期刊：
影响因子：
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通讯作者：
K. Inayoshi;E. Visbal;Z. Haiman
中科院分区：
文献类型：
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作者：
K. Inayoshi;E. Visbal;Z. Haiman
在宇宙形成的第一个十亿年中，大约10^9 Msun的超大质量黑洞（SMBH）的存在激发了许多关于黑洞在早期宇宙中迅速形成和快速增长的想法。在这里，我们回顾了大质量黑洞的种子可能首先组装的方式，它们如何随后增长到大约10^9 Msun的质量，以及多信使观测如何区分不同的SMBH组装场景。我们得出以下结论：（1）超罕见的10^9美元Msun SMBH仅代表冰山一角。早期的黑洞很可能填充了恒星质量的连续体（大约）。10 Msun）到超大质量（约10^9 Msun）区域，反映了一系列初始质量和生长历史。(2)恒星质量的黑洞很可能是由第一代红移高达z=30的恒星留下的，但由于宿主星系的浅势威尔斯，它们最初的生长通常受到阻碍。(3)一些较大的贫金属星系中的条件很快变得有利于通过气体吸积和致密星团中的合并快速形成和增长大质量的“种子”洞。(4)黑洞的质量取决于周围的环境（例如附近辐射源的数量和性质以及当地的重子流速度），以及宿主星系的金属富集和组装历史。(5)区分组装机制将是困难的，但丽莎（通过合并探测大规模BH生长）和深多波长电磁观测（通过气体吸积探测生长）的组合观测特别有前途。
The existence of $\approx$10^9 Msun supermassive black holes (SMBHs) within the first billion year of the universe has stimulated numerous ideas for the prompt formation and rapid growth of BHs in the early universe. Here we review ways in which the seeds of massive BHs may have first assembled, how they may have subsequently grown as massive as $\approx$10^9 Msun, and how multi-messenger observations could distinguish between different SMBH assembly scenarios. We conclude the following: (1) The ultra-rare $\approx$10^9 Msun SMBHs represent only the tip of the iceberg. Early BHs likely fill a continuum from stellar-mass (approx. 10 Msun) to the super-massive ($\approx$10^9 Msun) regime, reflecting a range of initial masses and growth histories. (2) Stellar-mass BHs were likely left behind by the first generation of stars at redshifts as high as z=30, but their initial growth was typically stunted due to the shallow potential wells of their host galaxies. (3) Conditions in some larger, metal-poor galaxies soon became conducive to the rapid formation and growth of massive `seed' holes, via gas accretion and by mergers in dense stellar clusters. (4) BH masses depend on the environment (such as the number and properties of nearby radiation sources and the local baryonic streaming velocity), and on the metal enrichment and assembly history of the host galaxy. (5) Distinguishing between assembly mechanisms will be difficult, but a combination of observations by LISA (probing massive BH growth via mergers) and by deep multi-wavelength electromagnetic observations (probing growth via gas accretion) is particularly promising.