  Using inspiral and plunge trajectories we construct with a generalized
Ori-Thorne algorithm, we use a time-domain black hole perturbation theory code
to compute the corresponding gravitational waves. The last cycles of these
waveforms are a superposition of Kerr quasinormal modes. In this paper, we
examine 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's
inspiral and plunge. We find that the mixture of quasinormal modes that
characterize the final gravitational waves from a coalescence is entirely
determined by the spin $a$ of the larger black hole, an angle $I$ which
characterizes the misalignment of the orbital plane from the black hole's spin
axis, a second angle $\theta_{\rm fin}$ which describes the location at which
the small body crosses the black hole's event horizon, and the direction
sgn$(\dot\theta_{\rm fin})$ of the body's final motion. If these
large-mass-ratio results hold at less extreme mass ratios, then measuring
multiple ringdown modes of binary black hole coalescence gravitational waves
may provide important information about the source's binary properties, such as
the misalignment of the orbit's angular momentum with black hole spin. This may
be particularly useful for large mass binaries, for which the early inspiral
waves are out of the detectors' most sensitive band.
