The ASTRID simulation: the evolution of Supermassive Black Holes
The ASTRID simulation: the evolution of Supermassive Black Holes
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ASTRID 模拟：超大质量黑洞的演化
DOI：
10.1093/mnras/stac351
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发表时间：
2021
期刊：
影响因子：
14.1
通讯作者：
Yin Li
中科院分区：
文献类型：
--
作者：
Y. Ni;T. Matteo;Simeon Bird;R. Croft;Yu Feng;Nianyi Chen;M. Tremmel;C. Degraf;Yin Li
我们介绍了Astrid中黑洞的演化及其与宿主星系的关系，Astrid是一个大体积宇宙学流体动力学模拟，盒子大小为250 h− 1 Mpc，包含2 × 55003个粒子，演化到z = 3。Astrid统计模型BH气体吸积和AGN反馈到他们的环境，适用于BH种子质量MSD的幂律分布，使用BH动力学摩擦模型和执行BH合并的物理处理。BH人口是广泛一致的BH质量函数，亮度函数的亮端，BH质量和吸积率密度的时间演化的经验约束。黑洞的质量和吸积与宿主恒星的质量和星星的形成速率密切相关。我们追踪了在z > 10之前播种的BH，直到z = 3，发现BH几乎没有初始Msd的印记，除了那些具有最小Msd的BH，其中不到50%的BH在质量上翻了一番。气体吸积是BH增长的主要渠道相比，BH合并。与动力摩擦，阿斯特丽德预测BH合并后，第一次遇到一个BH对显着的延迟，一个典型的流逝时间约为200万年。在z > 3的阿斯特丽德星系中总共有4.5 × 105个BH合并，其中10103个有X射线可探测到的EM对应物：一个明亮的kpc尺度的活动星系核，LX > 1043 erg s−1。MBH为107 - 8 M的BH经历了最频繁的合并。主持BH并合的Galerkin是整个MBH-M关系的无偏示踪剂。大质量（> 1011 M）星系有很高的黑洞占据数（& 10），因此拥有大多数的黑洞合并。
We present the evolution of black holes (BHs) and their relationship with their host galaxies in Astrid , a large-volume cosmological hydrodynamical simulation with box size 250 h−1Mpc containing 2 × 55003 particles evolved to z = 3. Astrid statistically models BH gas accretion and AGN feedback to their environments, applies a power-law distribution for BH seedmass Msd, uses a dynamical friction model for BH dynamics and executes a physical treatment of BH mergers. The BH population is broadly consistent with empirical constraints on the BH mass function, the bright end of the luminosity functions, and the time evolution of BH mass and accretion rate density. The BH mass and accretion exhibit a tight correlation with host stellar mass and star formation rate. We trace BHs seeded before z > 10 down to z = 3, finding that BHs carry virtually no imprint of the initial Msd except those with the smallest Msd, where less than 50% of them have doubled in mass. Gas accretion is the dominant channel for BH growth compared to BH mergers. With dynamical friction, Astrid predicts a significant delay for BH mergers after the first encounter of a BH pair, with a typical elapse time of about 200 Myrs. There are in total 4.5 × 105 BH mergers in Astrid at z > 3, ∼ 103 of which have X-ray detectable EM counterparts: a bright kpc scale dual AGN with LX > 1043 erg s−1. BHs with MBH ∼ 107−8 M experience the most frequent mergers. Galaxies that host BH mergers are unbiased tracers of the overall MBH − M∗ relation. Massive (> 1011 M ) galaxies have a high occupation number (& 10) of BHs, and hence host the majority of BH mergers.