标题： 用于广义相对论检验的参数化自旋进动螺旋-合并-振铃波形模型 显示英文标题

标题： Parametrized spin-precessing inspiral-merger-ringdown waveform model for tests of general relativity

摘要： 双黑洞（BBH）的并合为检验广义相对论（GR）在动态强场区域提供了一个独特平台。 为此，我们提出了pSEOBNRv5PHM，这是一种针对准圆轨道BBH的参数化、多极、自旋进动波形模型，基于有效一体重力理论构建。 与前代模型pSEOBNRv4HM相比，我们的模型不仅在坠落-合并-回响阶段引入了对广义相对论的参数化偏离，还在通过保守动力学修改的启发阶段也进行了这种偏离。 此外，它首次包含了自旋进动效应。 自由偏离参数可以用于使用当前和未来的引力波观测对广义相对论进行零假设检验。 我们通过贝叶斯参数估计验证了pSEOBNRv5PHM，重点关注$(\ell,m,n) = (2,2,0)$模式的准正则模频率和阻尼时间。 我们对高度进动的黑洞并合数值相对论（NR）模拟产生的合成信号的分析表明，虽然pSEOBNRv5PHM正确地恢复了与广义相对论的一致性，但忽略自旋进动可能导致即使在当前探测器灵敏度下也会错误检测到与广义相对论的偏差。 相反，当分析来自双玻色子星并合的数值相对论模拟的合成信号时，该模型成功识别出与广义相对论BBH信号的偏差。 最后，我们重新分析了第三次引力波瞬态目录中的12个事件。 通过这些事件的层次组合，我们在90%可信度下限制了$(2,2,0)$模式准正则模频率和阻尼时间的分数偏离至$\delta f_{220}=0.00_{-0.06}^{+0.06}$和$\delta \tau_{220}=0.15_{-0.24}^{+0.26}$。 这些结果与LIGO-Virgo-KAGRA合作的结果一致，后者没有考虑自旋进动效应。 显示英文摘要

摘要： The coalescence of binary black holes (BBHs) provides a unique arena to test general relativity (GR) in the dynamical, strong-field regime. To this end, we present pSEOBNRv5PHM, a parametrized, multipolar, spin-precessing waveform model for BBHs in quasicircular orbits, built within the effective-one-body formalism. Compared to its predecessor, pSEOBNRv4HM, our model introduces parametrized deviations from GR not only in the plunge-merger-ringdown stages, but also in the inspiral phase through modifications to the conservative dynamics. Additionally, it incorporates, for the first time, spin-precession effects. The free deviation parameters can be used to perform null tests of GR using current and future gravitational-wave observations. We validate pSEOBNRv5PHM through Bayesian parameter estimation, focusing on the quasinormal-mode frequency and damping time of the $(\ell,m,n) = (2,2,0)$ mode. Our analysis of synthetic signals from numerical-relativity (NR) simulations of highly precessing BH mergers shows that, while pSEOBNRv5PHM correctly recovers consistency with GR, neglecting spin precession can lead to false detections of deviations from GR even at current detector sensitivity. Conversely, when analyzing a synthetic signal from a NR simulation of a binary boson-star merger, the model successfully identifies a deviation from a GR BBH signal. Finally, we reanalyze 12 events from the third Gravitational-Wave Transient Catalog. Using a hierarchical combination of these events, we constrain fractional deviations in the frequency and damping time of the $(2,2,0)$ quasinormal-mode to $\delta f_{220}=0.00_{-0.06}^{+0.06}$ and $\delta \tau_{220}=0.15_{-0.24}^{+0.26}$ at 90% credibility. These results are consistent with those from the LIGO-Virgo-KAGRA Collaboration, which did not account for spin-precession effects.