论文标题
宇宙学模拟中的超质量黑洞I：M_BH-M_STAR关系和黑洞质量功能
Supermassive black holes in cosmological simulations I: M_BH-M_star relation and black hole mass function
论文作者
论文摘要
过去十年来，使用大规模宇宙学模拟理解星系形成和进化方面取得了重大进展。尽管这些模拟与观察结果总体良好地吻合，但它们采用了不同的子网格模型来用于星系和超质量黑洞（BHS）。我们研究了子网格模型对Illustris，TNG100，TNG300，Horizon-AGN，Eagle和Simba模拟的BH质量特性的影响，重点是M_BH-M_STAR关系和BH质量函数。所有模拟都预测了M_BH-M_STAR关系紧密，并难以在M_star 〜10^10.5-10^11.5 MSUN中产生最低（M_BH <10^7.5 msun）。对于所有仿真，平均M_BH-M_STAR关系的时间演变为温和（BH质量为0 <Z <5），但其线性（形状）和归一化因模拟而异。 SN反馈的强度对m_star <10^10.5 msun的线性和时间演变具有很大的影响。我们发现，低质量端是模拟模型的良好歧视性，并突出了对新观察约束的需求。在高质量端，强大的AGN反馈可以抑制关系归一化的时间演变。与当地宇宙的观察相比，在大多数模拟中，我们发现M_BH> 10^9 MSUN的BHS过量。 BH质量函数在高红移处有效积聚BHS（log10 f_edd> -2 $）的主导，并逐渐从高质量到低质量端的过渡，以不活跃的BHS控制。在模拟之间，活动BHS的过渡时间和贡献是不同的，可用于评估模型针对观察结果。
The past decade has seen significant progress in understanding galaxy formation and evolution using large-scale cosmological simulations. While these simulations produce galaxies in overall good agreement with observations, they employ different sub-grid models for galaxies and supermassive black holes (BHs). We investigate the impact of the sub-grid models on the BH mass properties of the Illustris, TNG100, TNG300, Horizon-AGN, EAGLE, and SIMBA simulations, focusing on the M_BH-M_star relation and the BH mass function. All simulations predict tight M_BH-M_star relations, and struggle to produce the lowest (M_BH< 10^7.5 Msun) in galaxies of M_star~10^10.5-10^11.5 Msun. While the time evolution of the mean M_BH-M_star relation is mild (<1 dex in BH mass for 0<z<5) for all the simulations, its linearity (shape) and normalization varies from simulation to simulation. The strength of SN feedback has a large impact on the linearity and time evolution for M_star<10^10.5 Msun. We find that the low-mass end is a good discriminant of the simulation models, and highlights the need for new observational constraints. At the high-mass end, strong AGN feedback can suppress the time evolution of the relation normalization. Compared with the observations of the local universe, we find an excess of BHs with M_BH>10^9 Msun in most of the simulations. The BH mass function is dominated by efficiently accreting BHs (log10 f_Edd >-2$) at high redshifts, and transitions progressively from the high-mass to the low-mass end to be governed by inactive BHs. The transition time and the contribution of active BHs are different among the simulations, and can be used to evaluate models against observations.
