  We revisit the modeling of the properties of the remnant black hole resulting
the merger of a black-hole binary as a function of the parameters of the
binary. We provide a set of empirical formulas for the final mass, spin and
recoil velocity of the final black hole as a function of the mass ratio and
individual spins of the progenitor. In order to determine the fitting
coefficients for these formulas, we perform a set of 128 new numerical
evolutions of precessing, unequal-mass black-hole binaries, and fit to the
resulting remnant mass, spin, and recoil. In order to reduce the complexity of
the analysis, we chose configurations that have one of the black holes
spinning, with dimensionless spin alpha=0.8, at different angles with respect
to the orbital angular momentum, and the other non-spinning. In addition to
evolving families of binaries with different spin-inclination angles, we also
evolved binaries with mass ratios as small as q=1/6. We use the resulting
empirical formulas to predict the probabilities of black hole mergers leading
to a given recoil velocity, total radiated gravitational energy, and final
black hole spin.
