  We discuss the transition from quasi-circular inspiral to plunge of a system
of two nonrotating black holes of masses $m_1$ and $m_2$ in the extreme mass
ratio limit $m_1m_2\ll (m_1+m_2)^2$. In the spirit of the Effective One Body
(EOB) approach to the general relativistic dynamics of binary systems, the
dynamics of the two black hole system is represented in terms of an effective
particle of mass $\mu\equiv m_1m_2/(m_1+m_2)$ moving in a (quasi-)Schwarzschild
background of mass $M\equiv m_1+m_2$ and submitted to an ${\cal O}(\mu)$
radiation reaction force defined by Pad\'e resumming high-order Post-Newtonian
results. We then complete this approach by numerically computing, \`a la
Regge-Wheeler-Zerilli, the gravitational radiation emitted by such a particle.
Several tests of the numerical procedure are presented. We focus on
gravitational waveforms and the related energy and angular momentum losses. We
view this work as a contribution to the matching between analytical and
numerical methods within an EOB-type framework.
