Parametrized spin-precessing inspiral-merger-ringdown waveform model for tests of general relativity

Abstract: The coalescence of binary black holes (BBHs) provides a unique arena to test general relativity (GR) in the dynamical, strong-field regime. To this end, we present pSEOBNRv5PHM, a parametrized, multipolar, spin-precessing waveform model for BBHs in quasicircular orbits, built within the effective-one-body formalism. Compared to its predecessor, pSEOBNRv4HM, our model introduces parametrized deviations from GR not only in the plunge-merger-ringdown stages, but also in the inspiral phase through modifications to the conservative dynamics. Additionally, it incorporates, for the first time, spin-precession effects. The free deviation parameters can be used to perform null tests of GR using current and future gravitational-wave observations. We validate pSEOBNRv5PHM through Bayesian parameter estimation, focusing on the quasinormal-mode frequency and damping time of the $(\ell,m,n) = (2,2,0)$ mode. Our analysis of synthetic signals from numerical-relativity (NR) simulations of highly precessing BH mergers shows that, while pSEOBNRv5PHM correctly recovers consistency with GR, neglecting spin precession can lead to false detections of deviations from GR even at current detector sensitivity. Conversely, when analyzing a synthetic signal from a NR simulation of a binary boson-star merger, the model successfully identifies a deviation from a GR BBH signal. Finally, we reanalyze 12 events from the third Gravitational-Wave Transient Catalog. Using a hierarchical combination of these events, we constrain fractional deviations in the frequency and damping time of the $(2,2,0)$ quasinormal-mode to $\delta f_{220}=0.00_{-0.06}^{+0.06}$ and $\delta \tau_{220}=0.15_{-0.24}^{+0.26}$ at 90% credibility. These results are consistent with those from the LIGO-Virgo-KAGRA Collaboration, which did not account for spin-precession effects.