Accuracy of ringdown models calibrated to numerical relativity simulations

TL;DR

This paper evaluates the accuracy of ringdown gravitational-wave models calibrated to numerical relativity, focusing on their robustness at earlier times and implications for future detector sensitivity.

Contribution

It provides a systematic time-domain mismatch analysis between ringdown models and numerical relativity waveforms, highlighting the models' limitations and areas for improvement.

Findings

Mismatch for dominant mode typically between 10^{-6} and 10^{-4}

Higher-order modes have larger mismatch, up to 10^{-2}

Results inform the development of more accurate models for gravitational-wave detection

Abstract

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 non-precessing, quasi-circular ringdown models parameterised 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 $(\ell,|m|)= (2,2)$ 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.