标题： 宇宙学模拟中的超大质量黑洞 第I部分：M_BH-M_star关系和黑洞质量函数 显示英文标题

标题： Supermassive black holes in cosmological simulations I: M_BH-M_star relation and black hole mass function

摘要： 过去十年中，通过大规模宇宙学模拟，在理解星系形成和演化方面取得了显著进展。 尽管这些模拟产生的星系总体上与观测结果一致，但它们对星系和超大质量黑洞（BHs）采用了不同的亚网格模型。 我们研究了亚网格模型对Illustris、TNG100、TNG300、Horizon-AGN、EAGLE和SIMBA模拟中的BH质量特性的影响，重点研究M_BH-M_star关系和BH质量函数。 所有模拟都预测了紧密的M_BH-M_star关系，并且在M_star~10^10.5-10^11.5 Msun的星系中难以产生最低的（M_BH< 10^7.5 Msun）BH。 虽然所有模拟的平均M_BH-M_star关系的时间演化较温和（0<z<5时BH质量变化小于1 dex），但其线性度（形状）和归一化在不同模拟之间有所变化。 SN反馈的强度对M_star<10^10.5 Msun的线性度和时间演化有较大影响。 我们发现低质量端是区分模拟模型的良好指标，并突显了需要新的观测约束。 在高质量端，强烈的AGN反馈可以抑制关系归一化的演化。 与本地宇宙的观测相比，我们发现大多数模拟中存在过多的M_BH>10^9 Msun的BH。 在高红移时，BH质量函数由高效吸积的BH（log10 f_Edd >-2）主导，并逐渐从高质最端过渡到低质量端，由不活跃的BH主导。 过渡时间和活跃BH的贡献在不同模拟中有所不同，可用于根据观测评估模型。 显示英文摘要

摘要： 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.