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Using inspiral and plunge trajectories we construct with a generalizedOri-Thorne algorithm, we use a time-domain black hole perturbation theory codeto compute the corresponding gravitational waves. The last cycles of thesewaveforms are a superposition of Kerr quasinormal modes. In this paper, weexamine how the modes' excitations vary as a function of source parameters,such as the larger black hole's spin and the geometry of the smaller body'sinspiral and plunge. We find that the mixture of quasinormal modes thatcharacterize the final gravitational waves from a coalescence is entirelydetermined by the spin $a$ of the larger black hole, an angle $I$ whichcharacterizes the misalignment of the orbital plane from the black hole's spinaxis, a second angle $\theta_{\rm fin}$ which describes the location at whichthe small body crosses the black hole's event horizon, and the directionsgn$(\dot\theta_{\rm fin})$ of the body's final motion. If theselarge-mass-ratio results hold at less extreme mass ratios, then measuringmultiple ringdown modes of binary black hole coalescence gravitational wavesmay provide important information about the source's binary properties, such asthe misalignment of the orbit's angular momentum with black hole spin. This maybe particularly useful for large mass binaries, for which the early inspiralwaves are out of the detectors' most sensitive band.

Exciting black hole modes via misaligned coalescences: II. The mode content of late-time coalescence waveforms