The upcoming Laser Interferometer Space Antenna (LISA), set for launch in the mid-2030s, will enhance our capability to probe the universe through gravitational waves (GWs) emitted from binary black holes (BBHs) across a broad range of cosmological distances. LISA is projected to observe three classes of BBHs: massive BBHs (MBBHs), extreme mass-ratio inspirals (EMRIs), and stellar mass BBHs. This study focuses on MBBHs, which are anticipated to occur in gas-rich environments conducive to producing powerful electromagnetic (EM) counterparts, positioning them as excellent candidates for bright sirens. By combining GW luminosity distance measurements from these bright sirens with Baryon Acoustic Oscillation (BAO) measurements derived from galaxy clustering and sound horizon measurements from the Cosmic Microwave Background (CMB), and spectroscopic redshift measurements from observations of the electromagnetic (EM) counterpart, we propose a data-driven model-independent method to reconstruct deviations in the variation of the effective Planck mass (in conjunction with the Hubble constant) as a function of cosmic redshift. Using this multi-messenger technique, we achieve precise measurements of deviations in the effective Planck mass variation with redshift (z), with a precision ranging from approximately 2.4% to 7.2% from redshift z=1 to z=6 with a single event. Additionally, we achieved a measurement of the Hubble constant with a precision of about 1.3%, accounting for variations in the effective Planck mass over 4 years of observation time (T _obs). This assumes that EM counterparts are detected for 75% of the events. This precision improves with observation time as T _obs ^-1/2. This approach not only has the potential to reveal deviations from General Relativity but also to significantly expand our understanding of the universe's fundamental physical properties.

中文翻译：

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使用 LISA 明亮标准警报器对广义相对论进行独立于模型的精度测试


即将推出的激光干涉仪太空天线 （LISA） 定于 2030 年代中期发射，将增强我们通过双黑洞 （BBH） 在很宽的宇宙学距离范围内发射的引力波 （GW） 探测宇宙的能力。预计 LISA 将观测三类 BBH：大质量 BBH （MBBH）、极端质量比呼吸 （EMRI） 和恒星质量 BBH。本研究的重点是 MBBH，预计它们将发生在有利于产生强大电磁 （EM） 对应物的富含气体的环境中，使它们成为明亮警报器的绝佳候选者。通过将来自这些明亮警报器的 GW 光度距离测量与来自星系集群的重子声学振荡 （BAO） 测量和来自宇宙微波背景 （CMB） 的声界测量相结合，以及来自电磁 （EM） 对应物观测的光谱红移测量，我们提出了一种数据驱动的独立于模型的方法，以重建有效普朗克质量（与哈勃常数结合）变化的偏差，作为宇宙红移的函数。使用这种多信使技术，我们可以精确测量红移 （z） 有效普朗克质量变化的偏差，单个事件从红移 z=1 到 z=6 的精度范围约为 2.4% 到 7.2%。此外，我们以约 1.3% 的精度测量了哈勃常数，考虑了 4 年观测时间 （T_obs） 内有效普朗克质量的变化。这假设 75% 的事件都检测到了 EM 对应物。此精度随观测时间的延长而提高，为 T_obs-1^/2。 这种方法不仅有可能揭示与广义相对论的偏差，而且还能显著扩展我们对宇宙基本物理特性的理解。