Multipolar effective-one-body waveforms for precessing binary black holes: Construction and validation
Multipolar effective-one-body waveforms for precessing binary black holes: Construction and validation
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DOI：
10.1103/physrevd.102.044055
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发表时间：
2020-04
影响因子：
5
通讯作者：
S. Ossokine;A. Buonanno;S. Marsat;R. Cotesta;S. Babak;T. Dietrich;R. Haas;I. Hinder;H. Pfeiffer;M. Pürrer;Charles J. Woodford;M. Boyle;Lawrence E. Kidder;M. Scheel;B. Szil'agyi
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作者：
S. Ossokine;A. Buonanno;S. Marsat;R. Cotesta;S. Babak;T. Dietrich;R. Haas;I. Hinder;H. Pfeiffer;M. Pürrer;Charles J. Woodford;M. Boyle;Lawrence E. Kidder;M. Scheel;B. Szil'agyi
随着引力波探测器变得更加灵敏，我们将获得紧凑型双星系统发出的更多种类的信号，从而揭示其天体物理起源和环境。可以区分形成情况的一个关键物理效应是自旋与轨道角动量的错位，导致自旋和双星轨道平面进动。为了准确地模拟此类系统，至关重要的是在主要四极杆之外包含多极杆。在这里，我们开发了第一个有效单体（EOB）形式的多极进动波形模型，用于双黑洞的吸气、合并和振铃（IMR）：SEOBNRv4PHM。在非进动极限下，模型简化为 SEOBNRv4HM，并根据数值相对论 (NR) 模拟和微扰理论波形进行了校准。我们通过将 SEOBNRv4PHM 与模拟极限时空 (SXS) 协作的 1405 个进动 NR 波形的公共目录以及新的 118 个进动 NR 波形（其质量比跨度为 1-4，旋转高达 0.9）进行比较来对其进行验证。我们强调，SEOBNRv4PHM 并未针对加工领域的 NR 模拟进行校准。我们计算了 1523 个 SXS 进动 NR 波形的不忠实度，发现对于 $94\%$ ($57\%$) 的情况，总质量范围 $20-200 M_\odot$ 中的最大值低于 $3\%$ ($1\%$)。当使用 IMR、多极、进动唯象模型 IMRPhenomPv3HM 时，这些数字变为 $83\%$ ($20\%$)。我们通过两项参数估计研究来研究这种不忠实值对合成信号的影响。我们还计算这些波形模型之间的不忠实性，并确定它们在参数空间的哪个部分差异最大。我们还针对多极、进动 NR 代理模型 NRSur7dq4 对其进行了验证，发现 SEOBNRv4PHM 模型优于 IMRPhenomPv3HM。
As gravitational-wave detectors become more sensitive, we will access a greater variety of signals emitted by compact binary systems, shedding light on their astrophysical origin and environment. A key physical effect that can distinguish among formation scenarios is the misalignment of the spins with the orbital angular momentum, causing the spins and the binary's orbital plane to precess. To accurately model such systems, it is crucial to include multipoles beyond the dominant quadrupole. Here, we develop the first multipolar precessing waveform model in the effective-one-body (EOB) formalism for the inspiral, merger and ringdown (IMR) of binary black holes: SEOBNRv4PHM. In the nonprecessing limit, the model reduces to SEOBNRv4HM, which was calibrated to numerical-relativity (NR) simulations, and waveforms from perturbation theory. We validate SEOBNRv4PHM by comparing it to the public catalog of 1405 precessing NR waveforms of the Simulating eXtreme Spacetimes (SXS) collaboration, and also to new 118 precessing NR waveforms, which span mass ratios 1-4 and spins up to 0.9. We stress that SEOBNRv4PHM is not calibrated to NR simulations in the precessing sector. We compute the unfaithfulness against the 1523 SXS precessing NR waveforms, and find that, for $94\%$ ($57\%$) of the cases, the maximum value, in the total mass range $20-200 M_\odot$, is below $3\%$ ($1\%$). Those numbers become $83\%$ ($20\%$) when using the IMR, multipolar, precessing phenomenological model IMRPhenomPv3HM. We investigate the impact of such unfaithfulness values with two parameter-estimation studies on synthetic signals. We also compute the unfaithfulness between those waveform models and identify in which part of the parameter space they differ the most. We validate them also against the multipolar, precessing NR surrogate model NRSur7dq4, and find that the SEOBNRv4PHM model outperforms IMRPhenomPv3HM.