Accuracy of ringdown models calibrated to numerical relativity simulations

The “ringdown” stage of gravitational-wave signals from binary black hole mergers, mainly consisting of a superposition of quasinormal modes emitted by the merger remnant, is a key tool to test fundamental physics and to probe black hole dynamics. However, ringdown models are known to be accurate only in the late-time, stationary regime. A key open problem in the field is to understand if these models are robust when extrapolated to earlier times, and if they can faithfully recover a larger portion of the signal. We address this question through a systematic time-domain calculation of the mismatch between nonprecessing, quasicircular ringdown models parametrized by the progenitor binary’s degrees of freedom and full numerical relativity inspiral-merger-ringdown waveforms from the simulating extreme spacetimes (SXS) simulation catalog. For the best-performing models, the mismatch is typically in the range [ 10 − 6 , 10 − 4 ] for the ( ℓ , | m | ) = ( 2 , 2 ) harmonic, and [ 10 − 4 , 10 − 2 ] for higher-order modes. Our findings inform ongoing observational searches for quasinormal modes, and underscore the need for improved modeling of higher-order modes to meet the sensitivity requirements of future gravitational-wave detectors.