  We calculate the linear momentum flux from merging black holes (BHs) with
arbitrary masses and spin orientations, using the effective-one-body (EOB)
model. This model includes an analytic description of the inspiral phase, a
short merger, and a superposition of exponentially damped quasi-normal ringdown
modes of a Kerr BH. By varying the matching point between inspiral and
ringdown, we can estimate the systematic errors generated with this method.
Within these confidence limits, we find close agreement with previously
reported results from numerical relativity. Using a Monte Carlo implementation
of the EOB model, we are able to sample a large volume of BH parameter space
and estimate the distribution of recoil velocities. For a range of mass ratios
1 <= m_1/m_2 <= 10, spin magnitudes of a_{1,2}=0.9, and uniform random spin
orientations, we find that a fraction f_{500}=0.12^{+0.06}_{-0.05} of binaries
have recoil velocities greater than 500 km/s and
f_{1000}=0.027^{+0.021}_{-0.014} have kicks greater than 1000 km/s. These
velocities likely are capable of ejecting the final BH from its host galaxy.
Limiting the sample to comparable-mass binaries with m_1/m_2 <= 4, the typical
kicks are even larger, with f_{500}=0.31_{-0.12}^{+0.13} and
f_{1000}=0.079^{+0.062}_{-0.042}.
