Surrogate model for gravitational wave signals from nonspinning, comparable-to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity
Surrogate model for gravitational wave signals from nonspinning, comparable-to large-mass-ratio black hole binaries built on black hole perturbation theory waveforms calibrated to numerical relativity
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DOI：
10.1103/physrevd.106.104025
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发表时间：
2022-04
影响因子：
5
通讯作者：
Tousif Islam;Scott E. Field;S. Hughes;G. Khanna;V. Varma;M. Giesler;M. Scheel;Lawrence E. Kidder;H. Pfeiffer
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文献类型：
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作者：
Tousif Islam;Scott E. Field;S. Hughes;G. Khanna;V. Varma;M. Giesler;M. Scheel;Lawrence E. Kidder;H. Pfeiffer
我们提出了一个降阶代理模型的引力波形从非旋转的二元黑洞系统具有可比的大质量比的配置。这个代理模型，\texttt{BHPTNRSur 1dq 1 e4}，是在点粒子黑洞微扰理论（ppBHPT）产生的波形数据上训练的，质量比从2.5到10，000不等。\texttt{BHPTNRSur 1dq 1 e4}通过使用更新的过渡到坍落模型扩展了早期的波形模型\texttt{EMRISur 1dq 1 e4}，覆盖了长达30，500 $m_1$（其中m_1 $是主黑洞的质量）的更长持续时间，包括几个球谐模，最高可达$\ell=10$，并根据数值相对论（NR）数据校准次主导模。在可比的质量比制度，包括质量比低至2.5美元，通过ppBHPT产生的重力波形同意令人惊讶的是，以及从NR后，这个简单的校准步骤。我们还比较了我们的模型与最近的SXS和RIT NR模拟的质量比范围从15 $到32 $，并发现占主导地位的四极模同意优于$\approximately 10^{-3}$。我们希望我们的模型是有用的，以研究当前和未来的引力波探测器中的中间质量比的二元系统。
We present a reduced-order surrogate model of gravitational waveforms from non-spinning binary black hole systems with comparable to large mass-ratio configurations. This surrogate model, \texttt{BHPTNRSur1dq1e4}, is trained on waveform data generated by point-particle black hole perturbation theory (ppBHPT) with mass ratios varying from 2.5 to 10,000. \texttt{BHPTNRSur1dq1e4} extends an earlier waveform model, \texttt{EMRISur1dq1e4}, by using an updated transition-to-plunge model, covering longer durations up to 30,500 $m_1$ (where $m_1$ is the mass of the primary black hole), includes several more spherical harmonic modes up to $\ell=10$, and calibrates subdominant modes to numerical relativity (NR) data. In the comparable mass-ratio regime, including mass ratios as low as $2.5$, the gravitational waveforms generated through ppBHPT agree surprisingly well with those from NR after this simple calibration step. We also compare our model to recent SXS and RIT NR simulations at mass ratios ranging from $15$ to $32$, and find the dominant quadrupolar modes agree to better than $\approx 10^{-3}$. We expect our model to be useful to study intermediate-mass-ratio binary systems in current and future gravitational-wave detectors.