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arXiv 2005.01111astro-ph.COgr-qc
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利用双黑洞引力波观测探测大尺度结构

Probing the large scale structure using gravitational-wave observations of binary black holes

Aditya Vijaykumar, M. V. S. Saketh, Sumit Kumar, Parameswaran Ajith, Tirthankar Roy Choudhury

备注：
Accepted version in Phys. Rev. D
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AI总结：

本文提出利用第三代引力波探测器观测双黑洞的空间聚集性，通过两点相关函数估计偏置因子，以探测大尺度结构并识别宿主星系类型。

摘要：

第三代引力波（GW）探测器预计将探测到大量红移较大的双黑洞（BBHs），从而利用它们的聚集性开辟对大尺度结构的独立探测途径。这一探测手段将与利用星系聚集性的探测方法互补——引力波事件可以被观测到非常大的红移（$z \sim 10$），尽管在远距离（约数十平方度）处源定位精度会差得多。我们探讨了利用观测到的双黑洞种群的空间分布（通过其两点（自）相关函数）来探测大尺度结构的可能性。我们发现，利用这些探测器进行几年的观测，可以估算出双黑洞种群的偏置因子（直至$z \sim 0.7$）。我们的方法仅依赖于从引力波事件中获得的源位置后验分布，不需要来自电磁观测的任何信息。这将有助于识别承载双黑洞种群的星系类型，从而揭示它们的起源。

英文摘要：

Third generation gravitational-wave (GW) detectors are expected to detect a large number of binary black holes (BBHs) to large redshifts, opening up an independent probe of the large scale structure using their clustering. This probe will be complementary to the probes using galaxy clustering -- GW events could be observed up to very large redshifts ($z \sim 10$) although the source localization will be much poorer at large distances ($\sim$ tens of square degrees). We explore the possibility of probing the large scale structure from the spatial distribution of the observed BBH population, using their two-point (auto)correlation function. We find that we can estimate the bias factor of population of BBH (up to $z \sim 0.7$) with a few years of observations with these detectors. Our method relies solely on the source-location posteriors obtained from the GW events and does not require any information from electromagnetic observations. This will help in identifying the type of galaxies that host the BBH population, thus shedding light on their origins.

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