论文标题
跨宇宙时间II的黑洞质量功能。重种子和（超级）巨大的黑洞
The Black Hole Mass Function Across Cosmic Times II. Heavy Seeds and (Super)Massive Black Holes
论文作者
论文摘要
这是旨在对黑洞（BH）质量函数进行建模的系列中的第二篇论文，从恒星到（超级）大规模制度。在目前的工作中，我们专注于（超级）大规模BHS，并在宇宙时代提供了其质量功能的Ab-Initio计算。我们考虑了两个主要的BH中央BH的主要机制，这些机制有望在当地大型星系的高红移星形祖细胞中进行合作。第一个是气体动力学摩擦过程，它可能导致向恒星质量BH的核区域迁移，起源于富含气体的宿主祖先星系的恒星形成，并建立了中央重型bh seed $ m_ \ seed $ m_ \ bullet \ sim \ sim 10^{3-5} {3-5} \，M $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $ $。年。第二种机制是在重BH种子上积聚的标准Eddington型气盘，中央BH可以通过它变成（超级）巨大的$ M_ \ bullet \ sim 10^{6-10} \，M_ \ odot $，M_ \ odot $在典型的星体形态范围内$ \ bys主机1 $ gyr。我们通过再现观察到的红移依赖性隆隆测量光度函数和爱丁顿比率分布以及恒星形成与积分中央BH的降压光度之间的关系来验证我们的半经验方法。然后，我们通过广泛的连续性方程方法在不同的红移处得出了遗物（超级）巨大的BH质量功能，并将其与当前的观察估计进行了比较。最后，我们重建了从恒星到（超级）大规模政权的总体BH质量函数，在BH质量中超过十个阶段。
This is the second paper in a series aimed at modeling the black hole (BH) mass function, from the stellar to the (super)massive regime. In the present work we focus on (super)massive BHs and provide an ab-initio computation of their mass function across cosmic times. We consider two main mechanisms to grow the central BH, that are expected to cooperate in the high-redshift star-forming progenitors of local massive galaxies. The first is the gaseous dynamical friction process, that can cause the migration toward the nuclear regions of stellar-mass BHs originated during the intense bursts of star formation in the gas-rich host progenitor galaxy, and the buildup of a central heavy BH seed $M_\bullet\sim 10^{3-5}\, M_\odot$ within short timescales $\lesssim$ some $10^7$ yr. The second mechanism is the standard Eddington-type gas disk accretion onto the heavy BH seed, through which the central BH can become (super)massive $M_\bullet\sim 10^{6-10}\, M_\odot$ within the typical star-formation duration $\lesssim 1$ Gyr of the host. We validate our semi-empirical approach by reproducing the observed redshift-dependent bolometric AGN luminosity functions and Eddington ratio distributions, and the relationship between the star-formation and the bolometric luminosity of the accreting central BH. We then derive the relic (super)massive BH mass function at different redshifts via a generalized continuity equation approach, and compare it with present observational estimates. Finally, we reconstruct the overall BH mass function from the stellar to the (super)massive regime, over more than ten orders of magnitudes in BH mass.
