Gravitational wave surrogate model for spinning, intermediate mass ratio binaries based on perturbation theory and numerical relativity

Abstract

We present BHPTNRSur2dq1e3, a reduced order surrogate model of gravitational waves emitted from binary black hole (BBH) systems in the comparable to large mass ratio regime with aligned spin (${\chi }_1$) on the heavier mass ($m_1$). We trained this model on waveform data generated from point particle black hole perturbation theory (ppBHPT) with mass ratios varying from $3\le q\le 1000$ and spins from $-0.8\le {\chi }_1\le 0.8$. The waveforms are $13,500m_1$ long and include all spin-weighted spherical harmonic modes up to $\ell =4$ except the $(4,1)$ and $m=0$ modes. We find that for binaries with ${\chi }_1\lesssim -0.5$, retrograde quasi-normal modes are significantly excited, thereby complicating the modeling process. To overcome this issue, we introduce a domain decomposition approach to model the inspiral and merger-ringdown portion of the signal separately. The resulting model can faithfully reproduce ppBHPT waveforms with a median time-domain mismatch error of $8\times 10^{-5}$. We then calibrate our model with numerical relativity (NR) data in the comparable mass regime $(3\le q\le 10)$. By comparing with spin-aligned BBH NR simulations at $q=15$, we find that the dominant quadrupolar (subdominant) modes agree to better than $\approx 10^{-3}(\approx 10^{-2})$ when using a time-domain mismatch error, where the largest source of calibration error comes from the transition-to-plunge and ringdown approximations of perturbation theory. Mismatch errors are below $\approx 10^{-2}$ for systems with mass ratios between $6\le q\le 15$ and typically get smaller at larger mass ratio. Our two models - both the ppBHPT waveform model and the NR-calibrated ppBHPT model - will be publicly available through gwsurrogate and the Black Hole Perturbation Toolkit packages.

20 pages, 17 figures

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