The Redshift Evolution of the Binary Black Hole Merger Rate: A Weighty Matter
The Redshift Evolution of the Binary Black Hole Merger Rate: A Weighty Matter
复制标题
DOI：
10.3847/1538-4357/ac64a3
复制
发表时间：
2021-10
期刊：
影响因子：
--
通讯作者：
L. V. van Son;S. D. de Mink;T. Callister;S. Justham;M. Renzo;T. Wagg;F. Broekgaarden;F. Kummer;R. Pakmor;I. Mandel
中科院分区：
文献类型：
--
作者：
L. V. van Son;S. D. de Mink;T. Callister;S. Justham;M. Renzo;T. Wagg;F. Broekgaarden;F. Kummer;R. Pakmor;I. Mandel
引力波探测器开始揭示双黑洞（BBH）合并速率R BBH（z）的红移演化。我们作出预测的R BBH（z）作为一个函数的黑洞质量的系统起源于孤立的双星。为此，我们调查的延迟时间和黑洞质量之间的相关性，通过套件的二进制人口合成模拟，COMPAS。我们区分两种渠道：公共包络（CE）和稳定罗氏瓣溢出（RLOF）信道，其特征在于系统是否经历了公共包络。我们发现CE通道优先产生质量低于30 M Ω和短延迟时间（t延迟1Gyr）的BH，而稳定的RLOF通道主要形成质量高于30 M Ω和长延迟时间（t延迟1Gyr）的BH系统。我们提供了一个新的适合的金属度依赖的特定星星形成率密度的基础上的Illustris TNG模拟，并使用它来转换的延迟时间分布到R BBH（z）的预测。这导致了高和低的原始BH质量的R BBH（z）的不同红移演化。我们进一步发现，在高红移时，RBBH（z）主要由CE通道所控制，而在低红移时，它包含了一个很大的贡献（约40%）来自稳定的RLOF通道。我们的研究结果预测，增加红移，BBH与组件质量超过30兆焦耳将变得越来越稀少相对于质量较低的BBH系统。对于不同的BH质量，R BBH（z）的这种不同演化的证据可以用未来的探测器进行测试。
Gravitational-wave detectors are starting to reveal the redshift evolution of the binary black hole (BBH) merger rate, R BBH(z). We make predictions for R BBH(z) as a function of black hole mass for systems originating from isolated binaries. To this end, we investigate correlations between the delay time and black hole mass by means of the suite of binary population synthesis simulations, COMPAS. We distinguish two channels: the common envelope (CE), and the stable Roche-lobe overflow (RLOF) channel, characterized by whether the system has experienced a common envelope or not. We find that the CE channel preferentially produces BHs with masses below about 30 M ⊙ and short delay times (t delay ≲ 1 Gyr), while the stable RLOF channel primarily forms systems with BH masses above 30 M ⊙ and long delay times (t delay ≳ 1 Gyr). We provide a new fit for the metallicity-dependent specific star formation rate density based on the Illustris TNG simulations, and use this to convert the delay time distributions into a prediction of R BBH(z). This leads to a distinct redshift evolution of R BBH(z) for high and low primary BH masses. We furthermore find that, at high redshift, R BBH(z) is dominated by the CE channel, while at low redshift, it contains a large contribution (∼40%) from the stable RLOF channel. Our results predict that, for increasing redshifts, BBHs with component masses above 30 M ⊙ will become increasingly scarce relative to less massive BBH systems. Evidence of this distinct evolution of R BBH(z) for different BH masses can be tested with future detectors.