The improvements in the sensitivity of the gravitational wave (GW) network enable the detection of several large redshift GW sources by third-generation GW detectors. These advancements provide an independent method to probe the large-scale structure of the universe by using the clustering of the binary black holes (BBHs). The black hole catalogs are complementary to the galaxy catalogs because of large redshifts of GW events, which may imply that BBHs are a better choice than galaxies to probe the large-scale structure of the universe and cosmic evolution over a large redshift range. To probe the large-scale structure, we used the sky position of the BBHs observed by third-generation GW detectors to calculate the angular correlation function and the bias factor of the population of BBHs. This method is also statistically significant as 5000 BBHs are simulated. Moreover, for the third-generation GW detectors, we found that the bias factor can be recovered to within 33% with an observational time of ten years. This method only depends on the GW source-location posteriors; hence, it can be an independent method to reveal the formation mechanisms and origin of the BBH mergers compared to the electromagnetic method.

中文翻译：

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通过引力波观测探索宇宙的大尺度结构

引力波 (GW) 网络灵敏度的提高使第三代引力波探测器能够探测到几个大型红移引力波源。这些进步提供了一种独立的方法，通过使用双黑洞 (BBH) 的聚类来探测宇宙的大尺度结构。由于 GW 事件的大红移，黑洞目录与星系目录是互补的，这可能意味着 BBH 是比星系更好的选择，可以探测宇宙的大尺度结构和大红移范围内的宇宙演化。为了探测大尺度结构，我们利用第三代引力波探测器观测到的BBHs的天空位置来计算BBHs种群的角相关函数和偏差因子。由于模拟了 5000 个 BBH，因此该方法在统计上也很重要。此外，对于第三代引力波探测器，我们发现在 10 年的观测时间内，偏差因子可以恢复到 33% 以内。该方法仅依赖于 GW 源位置后验；因此，与电磁方法相比，它可以成为揭示 BBH 合并的形成机制和起源的独立方法。