通过星系团团块吸积形成高红移盘状星系中的超大质量黑洞

詹姆斯·韦伯太空望远镜（JWST）的最新观测结果表明，在高红移星系中发现了超大质量黑洞（OMBHs）。本文提出了一种新的形成机制，即基于在紧凑盘状星系中吸积星系团块（GCs）。我们推导了 OMBHs 形成的条件，关注关键参数，如暗核质量、红移和暗核自转参数。我们的结果表明，在红移 $z = 10$ 时，一个质量为 $10^{11}~M_{\odot}$ 且自旋参数约为 0.02 的暗核，可以通过 GC 迁移和通过潮汐破坏事件（TDEs）吸积形成质量为 $2.3 \times 10^{8}~M_{\odot}$ 的黑洞。 resulting black hole-to-stellar mass ratio can reach $\sim 0.1$, corresponding to the fraction of GC mass accreted onto the black hole. This mechanism thus provides a plausible explanation for the OMBHs observed by JWST. Furthermore, by combining our model with the halo mass function and the spin-parameter distribution, we construct black hole mass functions that reproduce the number densities of the massive BH candidates UHZ1 and GHZ9 at $z \approx 10$, as well as the abundances of BHs with masses $\gtrsim 10^{8}~\rm{M_\odot}$ at $z \approx 5$ inferred from JWST observations. However, our model overpredicts the abundance of BHs with masses $< 10^{8}~\rm{M_\odot}$, suggesting that moderately massive, inactive BHs are more frequent.