标题： 通过引力波观测探测宇宙的大尺度结构 显示英文标题

标题： Probing the large-scale structure of the universe through gravitational-wave observations

摘要： 引力波（GW）网络的灵敏度提高使得第三代GW探测器能够探测到多个大红移GW源。 这些进展提供了一种独立的方法，通过双黑洞的聚类来研究宇宙的大尺度结构。 由于GW事件的大红移，黑洞目录与星系目录是互补的，这可能意味着双黑洞（BBHs）比星系更适合在大红移范围内探测宇宙的大尺度结构和宇宙演化。 为了研究大尺度结构，我们使用第三代GW探测器观测到的双黑洞天区位置计算角相关函数（ACF）和双黑洞种群的偏置因子。 这种方法在统计上也是显著的，因为模拟了5000个BBHs。 此外，对于第三代GW探测器，我们发现经过十年的观测时间，偏置因子可以恢复到33$\%$以内。 此方法仅依赖于GW源位置后验分布；因此，与电磁方法相比，它可以作为一种独立的方法来揭示BBH并合的形成机制和起源。 显示英文摘要

摘要： 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. The black hole catalogs are complementary to the galaxy catalogs because of large redshifts of GW events, which may imply that binary black holes (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 binary black holes observed by third-generation GW detectors to calculate the angular correlation function (ACF) and the bias factor of the population of binary black holes. 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.