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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 (₁) on the heavier mass (m₁). We trained this model on waveform data generated from point particle black hole perturbation theory (ppBHPT) with mass ratios varying from 3 q 1000 and spins from -0. 8 ₁ 0. 8. The waveforms are 13, 500 \ m₁ long and include all spin-weighted spherical harmonic modes up to = 4 except the (4, 1) and m = 0 modes. We find that for binaries with ₁ -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 10^-5. We then calibrate our model with numerical relativity (NR) data in the comparable mass regime (3 q 10). By comparing with spin-aligned BBH NR simulations at q = 15, we find that the dominant quadrupolar (subdominant) modes agree to better than 10^-3 \ (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 10^-2 for systems with mass ratios between 6 q 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.
Rink et al. (Thu,) studied this question.