标题： 活动星系核辐射反馈与大质量黑洞自旋之间的联系 显示英文标题

标题： On the connection between AGN radiative feedback and massive black hole spin

摘要： 我们提出了一种新颖的实现方法，通过代码gizmo中的超快风来实现活动星系核(AGN)反馈。 我们的反馈方案考虑了辐射反馈相对于黑洞自转的角依赖性。 我们自洽地随时间演化i)从解析尺度到未解析的AGN盘的气体吸积过程，ii)大质量黑洞(MBH)自转的演化，iii)AGN驱动风注入解析尺度，iv)整体反馈过程的自转诱导各向异性。 我们通过跟踪风驱动流出在均匀介质中的传播来测试我们的实现，并将结果与简单的解析模型进行比较。 然后，我们考虑一个孤立星系设置，在那里我们研究AGN反馈对MBH和宿主星系演化的影响力。 我们发现：i) AGN反馈限制了为MBH提供能量的气体流入，导致宿主星系的影响较弱，其核心区域的恒星形成(SF)抑制约为两倍；ii) AGN反馈对宿主星系和MBH增长的影响主要由AGN光度决定，而不是由MBH自转设定的角模式；iii) AGN辐射发射的角模式的痕迹在高吸积率下表现得更加明显。 在这些高吸积率下，更各向同性的角模式，属于较高自转值，更容易清除核心区域的气体，因此导致MBH质量和自转增长较慢以及SF的更高抑制。 我们认为，AGN反馈的自转依赖各向异性对MBH和星系演化的影响可能在那些具有高且持续的MBH吸积事件和高AGN风-星系耦合的场景中是重要的。 这些条件在星系合并和/或高红移星系中更常遇到。 显示英文摘要

摘要： We present a novel implementation for active galactic nucleus (AGN) feedback through ultra-fast winds in the code gizmo. Our feedback recipe accounts for the angular dependence of radiative feedback upon black hole spin. We self-consistently evolve in time i) the gas accretion process from resolved scales to an unresolved AGN disc, ii) the evolution of the spin of the massive black hole (MBH), iii) the injection of AGN-driven winds into the resolved scales, and iv) the spin-induced anisotropy of the overall feedback process. We test our implementation by following the propagation of the wind-driven outflow into a homogeneous medium, and we compare the results against simple analytical models. Then, we consider an isolated galaxy setup and there we study the impact of the AGN feedback on the evolution of the MBH and the of the host galaxy. We find that: i) AGN feedback limits the gas inflow that powers the MBH, with a consequent weak impact on the host galaxy characterized by a star formation (SF) suppression of about a factor of two in the nuclear region; ii) the impact of AGN feedback on the host galaxy and on MBH growth is primarily determined by the AGN luminosity, rather than by its angular pattern set by the MBH spin; iii) the imprint of the angular pattern of the AGN radiation emission manifest in a more clear way at high accretion rates. At such high rates the more isotropic angular patterns, proper to higher spin values, sweep away gas in the nuclear region more easily, hence causing a slower MBH mass and spin growths and a higher quenching of the SF. We argue that the influence of spin-dependent anisotropy of AGN feedback on MBH and galaxy evolution is likely to be relevant in those scenarios characterized by high and prolonged MBH accretion episodes and by high AGN wind-galaxy coupling. Such conditions are more frequently met in galaxy mergers and/or high redshift galaxies.