Exploring supermassive black hole physics and galaxy quenching across halo mass in FIRE cosmological zoom simulations
Exploring supermassive black hole physics and galaxy quenching across halo mass in FIRE cosmological zoom simulations
复制标题
在 FIRE 宇宙学变焦模拟中探索超大质量黑洞物理和晕质量上的星系猝灭
DOI：
10.1093/mnras/stad511
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发表时间：
2023
影响因子：
4.8
通讯作者：
Wetzel, Andrew
中科院分区：
文献类型：
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作者：
Wellons, Sarah;Faucher-Giguère, Claude-André;Hopkins, Philip F.;Quataert, Eliot;Anglés-Alcázar, Daniel;Feldmann, Robert;Hayward, Christopher C.;Kereš, Dušan;Su, Kung-Yi;Wetzel, Andrew
来自吸积超大质量黑洞（SMBH）的反馈被认为是大质量星系淬火的主要驱动力，但如何最好地将SMBH物理学应用于星系形成模拟仍然是模糊的。作为现实环境反馈（FIRE）项目的一部分，我们探索了不同的建模选择的影响SMBH吸积和反馈在一套1010- 1013 M的晕质量（1010- 1013 M）的范围广泛的宇宙放大模拟。在套件中，我们不同的数值方案BH吸积和反馈，吸积效率，和强度的机械，辐射和宇宙射线反馈独立。然后，我们将结果与观测到的星系尺度关系进行比较。我们发现几个模型满足观测约束的能量在不同的反馈通道是物理上合理的。有趣的是，由SMBH加速的宇宙射线在许多合理的模型中起着重要作用。然而，它是不平凡的复制跨晕质量的标度关系，许多模型的变化产生定性不正确的结果，无论参数的选择。恒星和黑洞质量的增长是密切相关的：例如，超大质量的黑洞往往会使星系过度猝灭。BH质量在高质量晕中受吸积效率选择的影响最大，但在低质量晕中受反馈效率的影响最大。低质量晕中SMBH反馈对星星形成的抑制量主要取决于时间积分反馈能量。对于大质量星系，模型的“响应性”（BH对可供吸积的气体的响应有多快和多强）是淬灭的另一个重要因素。
Feedback from accreting supermassive black holes (SMBHs) is thought to be a primary driver of quenching in massive galaxies, but how to best implement SMBH physics into galaxy formation simulations remains ambiguous. As part of the Feedback in Realistic Environments (FIRE) project, we explore the effects of different modelling choices for SMBH accretion and feedback in a suite of ∼500 cosmological zoom-in simulations across a wide range of halo mass (1010–1013M⊙). Within the suite, we vary the numerical schemes for BH accretion and feedback, accretion efficiency, and the strength of mechanical, radiative, and cosmic ray feedback independently. We then compare the outcomes to observed galaxy scaling relations. We find several models satisfying observational constraints for which the energetics in different feedback channels are physically plausible. Interestingly, cosmic rays accelerated by SMBHs play an important role in many plausible models. However, it is non-trivial to reproduce scaling relations across halo mass, and many model variations produce qualitatively incorrect results regardless of parameter choices. The growth of stellar and BH mass are closely related: for example, overmassive BHs tend to overquench galaxies. BH mass is most strongly affected by the choice of accretion efficiency in high-mass haloes, but by feedback efficiency in low-mass haloes. The amount of star formation suppression by SMBH feedback in low-mass haloes is determined primarily by the time-integrated feedback energy. For massive galaxies, the ‘responsiveness’ of a model (how quickly and powerfully the BH responds to gas available for accretion) is an additional important factor for quenching.