A path to creating intermediate-mass-ratio binary waveforms from self-force and numerical relativity

In the past few decades, the waveform community has made advances in producing waveforms that span the inspiral-merger-ringdown of comparable-mass-ratio black hole binaries using numerical relativity (NR) as well as state-of-the-art gravitational wave models. Current methods in NR, though, fail to produce stable simulations with intermediate mass ratios of 1:100-1:1000. Even within the range of mass ratios that allow stable waveforms, the computational cost becomes prohibitively expensive as the mass ratio and the length of the simulation increases. The self-force (SF) community has developed waveform models that can not only generate extreme mass ratio inspiral (EMRI) waveforms but also generate near-equal-mass-ratio waveforms with surprising accuracy. To assess the limits of both the NR and SF waveforms and alleviate computational costs, we present hybridized NR-SF waveforms with the inspiral of SF for non-spinning black hole binary systems. In the talk, I will present multiple of these hybridized waveforms and evaluate their accuracy with different hybridization settings. We also present preliminary parameter estimation results using our hybridized waveforms as simulated signals and recovering with state-of-the-art EMRI models.