A self-consistent method to estimate the rate of compact binary coalescences with a Poisson mixture model
A self-consistent method to estimate the rate of compact binary coalescences with a Poisson mixture model
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DOI：
10.1088/1361-6382/ab5f2d
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发表时间：
2019-03
影响因子：
3.5
通讯作者：
S. Kapadia;S. Caudill;J. Creighton;W. Farr;G. Mendell;A. Weinstein;K. Cannon;H. Fong;P. Godwin;R. K. Lo;R. Magee;D. Meacher;C. Messick;S. Mohite;D. Mukherjee;S. Sachdev
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作者：
S. Kapadia;S. Caudill;J. Creighton;W. Farr;G. Mendell;A. Weinstein;K. Cannon;H. Fong;P. Godwin;R. K. Lo;R. Magee;D. Meacher;C. Messick;S. Mohite;D. Mukherjee;S. Sachdev
最近发表的 GWTC-1（Abbott B P 等人（LIGO Scientific Collaboration 和 Virgo Collaboration）2019 Phys. Rev. X 9 031040）是一篇期刊文章，总结了从 LIGO-Virgo 地面探测器网络在第一次和第二次观测运行期间产生的数据中合并致密双星搜索引力波 (GW) 的过程，引用了对双星速率的估计 中子星、中子星黑洞双星和双星黑洞合并，以及各种重要和边缘引力波候选事件的天体物理起源的指定概率。在本文中，我们描述了用于计算这些速率和概率的形式主义，它假设高于低排名统计阈值的触发，无论是陆地还是天体物理起源，都作为独立的泊松过程发生。特别是，我们通过基于质量的模板加权重新分配候选事件的前景概率，在源类中包含任意数量的天体物理类别。我们在合成引力波数据上评估了这种形式，并证明这种方法对于第一次和第二次观测运行期间观测到的引力波信号类型非常有效。
The recently published GWTC-1 (Abbott B P et al (LIGO Scientific Collaboration and Virgo Collaboration) 2019 Phys. Rev. X 9 031040)—a journal article summarizing the search for gravitational waves (GWs) from coalescing compact binaries in data produced by the LIGO-Virgo network of ground-based detectors during their first and second observing runs—quoted estimates for the rates of binary neutron star, neutron star black hole binary, and binary black hole mergers, as well as assigned probabilities of astrophysical origin for various significant and marginal GW candidate events. In this paper, we delineate the formalism used to compute these rates and probabilities, which assumes that triggers above a low ranking statistic threshold, whether of terrestrial or astrophysical origin, occur as independent Poisson processes. In particular, we include an arbitrary number of astrophysical categories by redistributing, via mass-based template weighting, the foreground probabilities of candidate events, across source classes. We evaluate this formalism on synthetic GW data, and demonstrate that this method works well for the kind of GW signals observed during the first and second observing runs.