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We present SEOBNRv5HM, a more accurate and faster inspiral-merger-ringdowngravitational waveform model for quasi-circular, spinning, nonprecessing binaryblack holes within the effective-one-body (EOB) formalism. Compared to itspredecessor, SEOBNRv4HM, the waveform model i) incorporates recent high-orderpost- Newtonian results in the inspiral, with improved resummations, ii)includes the gravitational modes (l, |m|) = (3, 2), (4, 3), in addition to the(2, 2), (3, 3), (2, 1), (4, 4), (5, 5) modes already implemented in SEOBNRv4HM,iii) is calibrated to larger mass-ratios and spins using a catalog of 442numerical-relativity (NR) simulations and 13 additional waveforms fromblack-hole perturbation theory, iv) incorporates information from second-ordergravitational self-force (2GSF) in the nonspinning modes and radiation-reactionforce. Computing the unfaithfulness against NR simulations, we find that forthe dominant (2, 2) mode the maximum unfaithfulness in the total mass range$10-300 M_{\odot}$ is below $10^{-3}$ for 90% of the cases (38% forSEOBNRv4HM). When including all modes up to l = 5 we find 98% (49%) of thecases with unfaithfulness below $10^{-2} (10^{-3})$, while these numbers reduceto 88% (5%) when using SEOBNRv4HM. Furthermore, the model shows improvedagreement with NR in other dynamical quantities (e.g., the angular momentumflux and binding energy), providing a powerful check of its physicalrobustness. We implemented the waveform model in a high-performance Pythonpackage (pySEOBNR), which leads to evaluation times faster than SEOBNRv4HM by afactor 10 to 50, depending on the configuration, and provides the flexibilityto easily include spin-precession and eccentric effects, thus making it thestarting point for a new generation of EOBNR waveform models (SEOBNRv5) to beemployed for upcoming observing runs of the LIGO-Virgo-KAGRA detectors.

Laying the foundation of the effective-one-body waveform models  SEOBNRv5: improved accuracy and efficiency for spinning non-precessing binary  black holes