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-merger-ringdown effective-one-body model for precessing binary black holes, which incorporates subdominant modes beyond =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 510^-3, 710^-3 at inclinations of 0, /3, and 21 ``long'' waveforms with median mismatches of 410^-3 and 510^-3 at the same inclinations. Further comparisons against the state-of-the-art nrsur7dq4 waveform model yield median mismatches of 410^-3, 1. 810^-2 at inclinations of 0, /3 for 5000 precessing configurations with the precession parameter ₏ 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.