  Combining recent techniques giving non-perturbative re-summed estimates of
the damping and conservative parts of the two-body dynamics, we describe the
transition between the adiabatic phase and the plunge, in coalescing binary
black holes with comparable masses moving on quasi-circular orbits. We give
initial dynamical data for numerical relativity investigations, with a fraction
of an orbit left, and provide, for data analysis purposes, an estimate of the
gravitational wave-form emitted throughout the inspiral, plunge and coalescence
phases.
