  We present a highly accurate, fully analytical model for the late inspiral,
merger, and ringdown of black-hole binaries with arbitrary mass ratios and spin
vectors, including the contributions of harmonics beyond the fundamental mode.
This model assumes only that nonlinear effects remain small throughout the
entire coalescence, and is developed based on a physical understanding of the
dynamics of late stage binary evolution, in particular on the tendency of the
dynamical binary spacetime to behave like a linear perturbation of the static
merger-remnant spacetime, even at times before the merger has occurred. We
demonstrate that our model agrees with the most accurate numerical relativity
results to within their own uncertainties throughout the merger-ringdown phase,
and it does so for example cases spanning the full range of binary parameter
space that is currently testable with numerical relativity. Furthermore, our
model maintains accuracy back to the innermost stable circular orbit of the
merger-remnant spacetime over much of the relevant parameter space, greatly
decreasing the need to introduce phenomenological degrees of freedom to
describe the late inspiral.
