Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo
Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo
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DOI：
10.3847/2041-8213/ab3800
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发表时间：
2019-09-10
影响因子：
7.9
通讯作者：
Zweizig, J.
中科院分区：
文献类型：
--
作者：
Abbott, B. P.;Abbott, R.;Zweizig, J.
我们目前的质量，自旋和红移分布的结果与现象学的人口模型使用10个二元黑洞（BBH）合并检测到的第一和第二次观测运行完成先进的LIGO和先进的处女座。我们约束的BBH质量和自旋分布的参数化的范围内使用模型的BBH质谱的属性。我们发现，在这样的双星中，质量更大的黑洞的质量分布很好地近似于模型，其中不超过1%的黑洞质量超过45 M（圆点），幂律指数α = 1.3（-1.7）（+1.4）（90%的可信度）。我们还表明，BBHs是不太可能组成的BH与大自旋对准的轨道角动量。通过对BBH并合率随红移的演化进行模拟，我们发现，BBH并合率以93%的概率随红移的增加而增加或保持不变。将BBH总体的不确定性边缘化，我们发现BBH合并率密度的稳健估计为R = 53.2（-28.2）（+55.8）Gpc（-3）yr（-1）（90%可信度）。随着BBH目录在未来观测运行中的增长，我们预计人口模型参数的不确定性将缩小，可能通过超新星形成BH，大质量恒星的二元相互作用，星团动力学以及宇宙时间内BH的形成历史提供见解。
We present results on the mass, spin, and redshift distributions with phenomenological population models using the 10 binary black hole (BBH) mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the BBH mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive BH in such binaries is well approximated by models with no more than 1% of BHs more massive than 45M(circle dot) and a power-law index of alpha = 1.3(-1.7)(+1.4) (90% credibility). We also show that BBHs are unlikely to be composed of BHs with large spins aligned to the orbital angular momentum. Modeling the evolution of the BBH merger rate with redshift, we show that it is flat or increasing with redshift with 93% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of R = 53.2(-28.2)(+55.8) Gpc(-3) yr(-1) (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of BHs via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of BHs across cosmic time.