Observations of gravitational waves (GWs) from dark sirens allow us to infer their locations and distances. Galaxies, on the other hand, have precise angular positions but no direct measurement of their distances — only redshifts. The cross-correlation of GWs, which we limit here to binary black hole mergers (BBH), in spherical shells of luminosity distance D_L , with galaxies in shells of redshift z, leads to a direct measurement of the Hubble diagram D_L (z). Since this standard ruler relies only on the statistical proximity of the dark sirens and galaxies (a general property of large-scale structures), it is essentially model-independent: the correlation is maximal when both redshift and D_L shells coincide. We forecast the constraining power of this technique, which we call Peak Sirens, for run 5 (O5) of LIGO-Virgo-KAGRA (LVK), as well as for the third-generation observatories Einstein Telescope and Cosmic Explorer. We employ thousands of full-sky light cone simulations with realistic numbers for the tracers, and include masking by the Milky Way, lensing and inhomogeneous GW sky coverage. We find that the method is not expected to suffer from some of the issues present in other dark siren methods, such as biased constraints due to incompleteness of galaxy catalogs or dependence on priors for the merger rates of BBH. We show that with Peak Sirens, given the projected O5 sensitivity, LVK can measure H ₀ with 7% precision by itself, assuming ΛCDM, and 4% precision using external datasets to constrain Ω _m . We also show that future third-generation GW detectors can achieve, without external data, sub-percent uncertainties in H ₀ assuming ΛCDM, and 3% in a more flexible w ₀ w_a CDM model. The method also shows remarkable robustness against systematic effects such as the modeling of non-linear structure formation.

中文翻译：

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来自星系和黑暗警报器交叉关联的强大宇宙标准尺


从黑暗警报器中观测引力波 （GW） 使我们能够推断它们的位置和距离。另一方面，星系有精确的角度位置，但没有直接测量它们的距离——只有红移。GW 的互相关，我们在这里仅限于双黑洞合并 （BBH），在光度距离 D_L 的球壳中，与红移 z 层中的星系，导致哈勃图 D_L （z） 的直接测量。由于这个标准标尺仅依赖于黑暗警报器和星系的统计接近性（大尺度结构的一般特性），因此它基本上与模型无关：当红移和 D_L 壳重合时，相关性是最大的。我们预测了这种技术（我们称之为峰值警报器）对 LIGO-Virgo-KAGRA （LVK） 的第 5 次运行 （O5） 以及第三代天文台爱因斯坦望远镜和宇宙探测器的约束能力。我们采用了数千个全天空光锥模拟，并为示踪剂提供了真实的数字，并包括银河系的遮罩、透镜和非均匀的 GW 天空覆盖。我们发现该方法预计不会受到其他黑暗警报器方法中存在的一些问题的影响，例如由于星系目录不完整而导致的偏向约束或 BBH 合并率对先验的依赖。我们表明，使用峰值警报器，给定预计的 O5 灵敏度，LVK 可以以 7% 的精度测量 H₀（假设 ΛCDM），并使用外部数据集将 4% 的精度限制为 Ω _m。我们还表明，未来的第三代 GW 探测器可以在没有外部数据的情况下，假设 ΛCDM 在 H₀ 中实现亚百分比不确定性，在更灵活的 w₀w_a CDM 模型中实现 3% 的不确定性。 该方法还显示出对系统效应（例如非线性结构形成建模）的显著鲁棒性。