Intermediate-mass Black Holes on the Run from Young Star Clusters
Intermediate-mass Black Holes on the Run from Young Star Clusters
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DOI：
10.3847/1538-4357/ac9b0f
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发表时间：
2022-08
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通讯作者：
Elena Gonz'alez Prieto;K. Kremer;G. Fragione;Miguel A. S. Martinez;Newlin C. Weatherford;M. Zevin;F. Rasio
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作者：
Elena Gonz'alez Prieto;K. Kremer;G. Fragione;Miguel A. S. Martinez;Newlin C. Weatherford;M. Zevin;F. Rasio
质量介于恒星残骸和超大质量黑洞之间的黑洞（BH）的存在直到最近才得到明确的证实。由LIGO/Virgo合作探测到的引力波信号GW 190521为这种中等质量黑洞（IMBHs）的存在提供了第一个直接证据。这一事件引发并继续推动关于这种大规模BH可能形成渠道的讨论。探测显示，IMBHs可以通过BH在“上质量间隙”（120 - 140 M）中的二元合并形成。或者，IMBH可能是由一颗非常大质量的星星的坍缩形成的，这颗恒星是在密集的星星团中通过恒星碰撞和合并形成的。在这项研究中，我们探讨了形成的IMBHs的质量在120和500 M之间的年轻，大质量的星星集群使用国家的最先进的集群蒙特卡罗模型。我们研究的演化IMBHs在其整个动力学寿命，结束与他们的弹射从母集群由于重力辐射反冲BH合并，或动力学反冲踢从几个身体散射遇到。我们发现，在我们的模型中，所有的IMBHs从主机集群内弹出的第一个500万年，表明在这个质量范围内的球状星团今天的IMBHs的保留概率低。我们估计IMBH的合并速率峰值在红移z = 2时为2Gpc− 3 yr −1。
The existence of black holes (BHs) with masses in the range between stellar remnants and supermassive BHs has only recently become unambiguously established. GW190521, a gravitational wave signal detected by the LIGO/Virgo Collaboration, provides the first direct evidence for the existence of such intermediate-mass BHs (IMBHs). This event sparked and continues to fuel discussion on the possible formation channels for such massive BHs. As the detection revealed, IMBHs can form via binary mergers of BHs in the “upper mass gap” (≈40–120 M ⊙). Alternatively, IMBHs may form via the collapse of a very massive star formed through stellar collisions and mergers in dense star clusters. In this study, we explore the formation of IMBHs with masses between 120 and 500 M ⊙ in young, massive star clusters using state-of-the-art Cluster Monte Carlo models. We examine the evolution of IMBHs throughout their dynamical lifetimes, ending with their ejection from the parent cluster due to gravitational radiation recoil from BH mergers, or dynamical recoil kicks from few-body scattering encounters. We find that all of the IMBHs in our models are ejected from the host cluster within the first ∼500 Myr, indicating a low retention probability of IMBHs in this mass range for globular clusters today. We estimate the peak IMBH merger rate to be ≈2Gpc−3yr−1 at redshift z ≈ 2.