Probing Multiple Populations of Compact Binaries with Third-generation Gravitational-wave Detectors
Probing Multiple Populations of Compact Binaries with Third-generation Gravitational-wave Detectors
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DOI：
10.3847/2041-8213/abf8be
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发表时间：
2020-12
期刊：
影响因子：
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通讯作者：
K. Ng;S. Vitale;W. Farr;C. Rodriguez
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文献类型：
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作者：
K. Ng;S. Vitale;W. Farr;C. Rodriguez
第三代（3G）引力波探测器将能够观测到红移高达3000的双黑洞合并（BBH）。这使得前所未有的进入整个宇宙历史的BBH的形成和演化。在本文中，我们考虑了三个子群的BBH起源于不同的演化通道：孤立的形成在银河领域，动力学形成的球状星团，并合并的黑洞形成的人口III（流行III）的恒星在非常高的红移。使用从人口合成分析的输入，我们创建了一个由两个宇宙探索者和一个爱因斯坦望远镜组成的3G探测器网络的2个月的模拟数据，该网络由16,000个场和集群BBH以及1400个Pop III BBH组成。首先，我们展示了如何使用非参数模型来推断合并率分布中作为红移函数的主峰和次峰的存在和特征。特别是，由Pop III残留物合并产生的z 12附近的次峰的位置和高度可以限制在水平（95%可信区间）。然后，我们进行了建模分析，使用现象学模板的合并率的三个子群体和提取的分支比和特征参数的合并率密度的个别形成通道。用这种建模方法，测量的不确定性的Pop III BBHs的分数可以提高到100%，而现场和集群BBHs之间的比例可以测量的不确定性为100%。
Third-generation (3G) gravitational-wave detectors will be able to observe binary black hole mergers (BBHs) up to a redshift of ∼30. This gives unprecedented access to the formation and evolution of BBHs throughout cosmic history. In this paper, we consider three subpopulations of BBHs originating from the different evolutionary channels: isolated formation in galactic fields, dynamical formation in globular clusters, and mergers of black holes formed from Population III (Pop III) stars at very high redshift. Using input from population synthesis analyses, we create 2 months of simulated data of a network of 3G detectors made of two Cosmic Explorers and one Einstein Telescope consisting of ∼16,000 field and cluster BBHs, as well as ∼400 Pop III BBHs. First, we show how one can use a nonparametric model to infer the existence and characteristics of a primary and secondary peak in the merger rate distribution as a function of redshift. In particular, the location and height of the secondary peak around z ≈ 12, arising from the merger of Pop III remnants, can be constrained at the level (95% credible interval). Then we perform a modeled analysis using phenomenological templates for the merger rates of the three subpopulations and extract the branching ratios and characteristic parameters of the merger rate densities of the individual formation channels. With this modeled method, the uncertainty on the measurement of the fraction of Pop III BBHs can be improved to ≲10%, while the ratio between field and cluster BBHs can be measured with an uncertainty of ∼100%.