标题： SEOBNRv5PHM: 二黑洞 binaries 的下一代精确且高效的多极进动自旋有效一體波形 显示英文标题

标题： SEOBNRv5PHM: Next generation of accurate and efficient multipolar precessing-spin effective-one-body waveforms for binary black holes

摘要： 自旋进动是揭示地面和空间引力波（GW）探测器所检测到的紧凑双星起源的关键物理效应之一，并有助于阐明它们可能的形成通道。 有效地且准确地建模这些系统发射的引力波信号对于提取其属性至关重要。 在这里，我们提出了SEOBNRv5PHM，这是有效一阶（EOB）形式主义下的一种多极预cession自旋波形模型，适用于二元黑洞（BBH）的完整信号（即，螺旋阶段、合并和回响阶段）。 在非预cession极限情况下，该模型简化为SEOBNRv5HM，后者经过校准以匹配1$442$数值相对论（NR）模拟、来自黑洞扰动理论的13个波形以及二阶引力自力理论中的非旋转能量流。 我们指出，SEOBNRv5PHM并未经过旋转预cession数值相对论波形的校准，这些波形来自Simulating eXtreme时空合作组织。 我们通过计算与1543个旋转预cession数值相对论波形的不忠实度来验证SEOBNRv5PHM，并发现，在总质量范围20-300$M_\odot$的情况下，有99.8%（84.4%）的案例中，最大值低于3%（1%）。 当使用SEOBNR家族的前一版本SEOBNRv4PHM时，这些数字减少到95.3%（60.8%），而当使用最先进的频率域多极旋转预cession现象学IMRPhenomXPHM模型时，减少到78.2%（38.3%）。 由于SEOBNRv5PHM相比SEOBNRv4PHM具有更好的计算效率，我们还能够对LIGO-Virgo探测器观测到的合成信号和引力波事件进行广泛的贝叶斯参数估计。 我们展示了SEOBNRv5PHM可以作为标准工具用于推断分析，以提取大量BBH目录的天文学和宇宙学信息。 显示英文摘要

摘要： Spin precession is one of the key physical effects that could unveil the origin of the compact binaries detected by ground- and space-based gravitational-wave (GW) detectors, and shed light on their possible formation channels. Efficiently and accurately modeling the GW signals emitted by these systems is crucial to extract their properties. Here, we present SEOBNRv5PHM, a multipolar precessing-spin waveform model within the effective-one-body (EOB) formalism for the full signal (i.e. inspiral, merger and ringdown) of binary black holes (BBHs). In the non-precessing limit, the model reduces to SEOBNRv5HM, which is calibrated to $442$ numerical-relativity (NR) simulations, 13 waveforms from BH perturbation theory, and non-spinning energy flux from second-order gravitational self-force theory. We remark that SEOBNRv5PHM is not calibrated to precessing-spin NR waveforms from the Simulating eXtreme Spacetimes Collaboration. We validate SEOBNRv5PHM by computing the unfaithfulness against 1543 precessing-spin NR waveforms, and find that for 99.8% (84.4%) of the cases, the maximum value, in the total mass range 20-300 $M_\odot$, is below 3% (1%). These numbers reduce to 95.3% (60.8%) when using the previous version of the SEOBNR family, SEOBNRv4PHM, and to 78.2% (38.3%) when using the state-of-the-art frequency-domain multipolar precessing-spin phenomenological IMRPhenomXPHM model. Due to much better computational efficiency of SEOBNRv5PHM compared to SEOBNRv4PHM, we are also able to perform extensive Bayesian parameter estimation on synthetic signals and GW events observed by LIGO-Virgo detectors. We show that SEOBNRv5PHM can be used as a standard tool for inference analyses to extract astrophysical and cosmological information of large catalogues of BBHs.