  Building up on previous work, we present a new calculation of the
gravitational wave (GW) emission generated during the transition from
quasi-circular inspiral to plunge, merger and ringdown by a binary system of
nonspinning black holes, of masses $m_1$ and $m_2$, in the extreme mass ratio
limit, $m_1 m_2\ll(m_1+m_2)^2$. The relative dynamics of the system is computed
{\it without making any adiabatic approximation} by using an effective one body
(EOB) description, namely by representing the binary by an effective particle
of mass $\mu=m_1 m_2/(m_1+m_2)$ moving in a (quasi-)Schwarzschild background of
mass $M=m_1+m_2$ and submitted to an $\O(\nu)$ 5PN-resummed analytical
radiation reaction force, with $\nu=\mu/M$. The gravitational wave emission is
calculated via a multipolar Regge-Wheeler-Zerilli type perturbative approach
(valid in the limit $\nu\ll 1$). We consider three mass ratios,
$\nu={10^{-2},10^{-3},10^{-4}}$,and we compute the multipolar waveform up to
$\ell=8$. We estimate energy and angular momentum losses during the
quasi-universal and quasi-geodesic part of the plunge phase and we analyze the
structure of the ringdown. We calculate the gravitational recoil, or "kick",
imparted to the merger remnant by the gravitational wave emission and we
emphasize the importance of higher multipoles to get a final value of the
recoil $v/(c\nu^2)=0.0446$. We finally show that there is an {\it excellent
fractional agreement} ($\sim 10^{-3}$) (even during the plunge) between the 5PN
EOB analytically-resummed radiation reaction flux and the numerically computed
gravitational wave angular momentum flux. This is a further confirmation of the
aptitude of the EOB formalism to accurately model extreme-mass-ratio inspirals,
as needed for the future space-based LISA gravitational wave detector.
