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Compaction-driven black hole growth
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2021-04-26 , DOI: 10.1093/mnras/stab1205
Sharon Lapiner 1 , Avishai Dekel 1, 2, 3 , Yohan Dubois 3
Affiliation  

We study the interplay between galaxy evolution and central black hole (BH) growth using the NewHorizon cosmological simulation. BH growth is slow when the dark-matter halo is below a golden mass of $M_{\rm v}\sim 10^{12}\, \rm M_\odot$, and rapid above it. The early suppression is primarily due to gas removal by supernova (SN) feedback in the shallow potential well, predicting that BHs of ${\sim}10^5\, \rm M_\odot$ tend to lie below the linear relation with bulge mass. Rapid BH growth is allowed when the halo is massive enough to lock in the SN ejecta by its deep potential well and its heated circumgalactic medium (CGM). The onset of BH growth between these two zones is triggered by a wet-compaction event, caused, e.g. by mergers or counter-rotating streams. It brings gas that lost angular momentum into the inner-$1\, {\rm kpc}$ ‘blue nugget’ and causes major transitions in the galaxy structural, kinematic, and compositional properties, including the onset of star-formation quenching. The compaction events are confined to the golden mass by the same mechanisms of SN feedback and hot CGM. The onset of BH growth is associated with its sinkage to the centre due to the compaction-driven deepening of the potential well and the associated dynamical friction. The galaxy golden mass is thus imprinted as a threshold for rapid BH growth, allowing the AGN feedback to keep the CGM hot and maintain long-term quenching. AGN feedback is not causing the onset of quenching; they are both caused by a compaction event when the mass is between the SN and hot-CGM zones.

中文翻译:

压实驱动的黑洞增长

我们使用 NewHorizo​​n 宇宙学模拟研究了星系演化和中心黑洞 (BH) 增长之间的相互作用。当暗物质晕低于 $M_{\rm v}\sim 10^{12}\, \rm M_\odot$ 的黄金质量时,BH 的增长是缓慢的,并且在它之上快速增长。早期抑制主要是由于浅势阱中超新星(SN)反馈的气体去除,预测${\sim}10^5\,\rm M_\odot$的BHs往往低于与凸起的线性关系大量的。当光晕足够大以通过其深势阱和加热的环银河介质 (CGM) 锁定 SN 喷射物时,允许 BH 快速增长。这两个区域之间 BH 增长的开始是由湿压实事件触发的,例如由合并或反向旋转流引起。它将失去角动量的气体带入内部$1\,{\rm kpc}$ 'blue nugget' 并导致星系结构、运动学和组成特性的重大转变,包括恒星形成淬火的开始。通过 SN 反馈和热 CGM 的相同机制,压实事件被限制在黄金块中。由于压实驱动的势井加深和相关的动力摩擦,BH 增长的开始与其向中心下沉有关。因此,星系黄金质量被印记为 BH 快速增长的阈值,允许活动星系核反馈保持 CGM 热并保持长期淬火。AGN 反馈不会引起猝灭;当质量位于 SN 和热 CGM 区域之间时,它们都是由压实事件引起的。包括恒星形成猝灭的开始。通过 SN 反馈和热 CGM 的相同机制,压实事件被限制在黄金块中。由于压实驱动的势井加深和相关的动力摩擦,BH 增长的开始与其向中心下沉有关。因此,星系黄金质量被印记为 BH 快速增长的阈值,允许活动星系核反馈保持 CGM 热并保持长期淬火。AGN 反馈不会引起猝灭;当质量位于 SN 和热 CGM 区域之间时,它们都是由压实事件引起的。包括恒星形成猝灭的开始。通过 SN 反馈和热 CGM 的相同机制,压实事件被限制在黄金块中。由于压实驱动的势井加深和相关的动力摩擦,BH 增长的开始与其向中心下沉有关。因此,星系黄金质量被印记为 BH 快速增长的阈值,允许活动星系核反馈保持 CGM 热并保持长期淬火。AGN 反馈不会引起猝灭;当质量位于 SN 和热 CGM 区域之间时,它们都是由压实事件引起的。由于压实驱动的势井加深和相关的动力摩擦,BH 增长的开始与其向中心下沉有关。因此,星系黄金质量被印记为 BH 快速增长的阈值,允许活动星系核反馈保持 CGM 热并保持长期淬火。AGN 反馈不会引起猝灭;当质量位于 SN 和热 CGM 区域之间时,它们都是由压实事件引起的。由于压实驱动的势井加深和相关的动力摩擦,BH 增长的开始与其向中心下沉有关。因此,星系黄金质量被印记为 BH 快速增长的阈值,允许活动星系核反馈保持 CGM 热并保持长期淬火。AGN 反馈不会引起猝灭;当质量位于 SN 和热 CGM 区域之间时,它们都是由压实事件引起的。
更新日期:2021-04-26
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