Accreting black holes can drive fast and energetic nuclear winds that may be an important feedback mechanism associated with active galactic nuclei (AGN). In this paper, we implement a scheme for capturing feedback from these fast nuclear winds and examine their impact in simulations of isolated disk galaxies. Stellar feedback is modeled using the FIRE physics and produces a realistic multiphase interstellar medium (ISM). We find that AGN winds drive the formation of a low-density, high-temperature central gas cavity that is broadly consistent with analytic model expectations. The effects of AGN feedback on the host galaxy are a strong function of the wind kinetic power and momentum. Low and moderate luminosity AGN do not have a significant effect on their host galaxy: the AGN winds inefficiently couple to the ambient ISM and instead a significant fraction of their energy vents in the polar direction. For such massive black holes, accretion near the Eddington limit can have a dramatic impact on the host galaxy ISM: if AGN wind feedback acts for ≳ 20 − 30 Myr, the inner ∼1 − 10 kpc of the ISM is disrupted and the global galaxy star formation rate is significantly reduced. We quantify the properties of the resulting galaxy-scale outflows and find that the radial momentum in the outflow is boosted by a factor ∼2 − 3 relative to that initially supplied in the AGN wind for strong feedback scenarios, decreasing below unity for less energetic winds. In contrast to observations, however, the outflows are primarily hot, with very little atomic or molecular gas. We conjecture that merging galaxies and high-redshift galaxies, which have more turbulent and thicker disks and very different nuclear gas geometries, may be even more disrupted by AGN winds than found in our simulations.

中文翻译：

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AGN风反馈在多相ISM隔离星系模拟中的影响

积聚的黑洞可以驱动快速而充满活力的核风，这可能是与活跃银河核（AGN）相关的重要反馈机制。在本文中，我们实现了一种从这些快速核风中获取反馈的方案，并研究了它们在孤立盘状星系模拟中的影响。使用FIRE物理模型对恒星反馈进行建模，并产生逼真的多相星际介质（ISM）。我们发现，AGN风推动了低密度高温中央气腔的形成，该气腔与分析模型的期望大体一致。AGN反馈对宿主星系的影响是风动能和动量的强大函数。中低亮度AGN对其宿主星系没有明显影响：AGN的风无法有效地耦合到周围的ISM，相反，它们的能量排放口中有很大一部分是沿极向传播的。对于如此巨大的黑洞，在爱丁顿极限附近的积聚可能会对主星系ISM产生巨大影响：如果AGN风反馈作用于− 20-30 Myr，则ISM的内部〜1-10 kpc受到干扰，全球星系恒星形成率大大降低。我们对产生的星系规模外流的性质进行了量化，发现对于强反馈情形，外流的径向动量相对于最初在AGN风中提供的动量增加了约2 − 3倍，对于能量较小的风，则减小到小于1 。但是，与观察结果相反，流出的气体主要是热的，几乎没有原子或分子气体。