Effective-one-body waveforms for precessing coalescing compact binaries with post-Newtonian twist

Spin precession is a generic feature of compact binary coalescences that leaves clear imprints in the gravitational waveforms. Building on previous work, we present an efficient time domain inspiral-mergerringdown effective-one-body model for precessing binary black holes, which incorporates subdominant modes beyond l 1/4 2, and the first effective-one-body frequency domain approximant for precessing binary neutron stars. We validate our model against 99 ???short??? numerical relativity precessing waveforms, where we find median mismatches of 5 ?? 10???3, 7 ?? 10???3 at inclinations of 0, ??/3, and 21 ???long??? waveforms with median mismatches of 4 ?? 10???3 and 5 ?? 10???3 at the same inclinations. Further comparisons against the state-of-the-art NRSur7dq4 waveform model yield median mismatches of 4 ?? 10???3, 1.8 ?? 10???2 at inclinations of 0; ??/3 for 5000 precessing configurations with the precession parameter ??p up to 0.8 and mass ratios up to 4. To demonstrate the computational efficiency of our model we apply it to parameter estimation and reanalyze the gravitational-wave events GW150914, GW190412, and GW170817.