Extracting the second-order self-force in Kerr from numerical relativity

Comparisons between self-force (SF) and numerical relativity (NR) waveforms have been done for quasicircular, equatorial orbits on a Schwarzschild background, during the inspiral and recover the results of NR simulations for mass ratios of ~1:10. While modelling extreme mass ratio inspirals was the original goal of SF theory, it is now a promising candidate for producing fast and accurate waveforms for intermediate mass ratio inspirals. Second-order SF waveforms for spinning black holes, however do not exist yet. By fitting inspiral quantities across mass ratios using a series of NR simulations, I will present a method for extracting second-order SF corrections from NR for quasicircular orbits on a Kerr background. This will provide a calculation of the second-order SF approximation to the orbital dynamics of a binary with intermediate mass ratios and spinning primary.