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We revisit the modeling of the properties of the remnant black hole resultingthe merger of a black-hole binary as a function of the parameters of thebinary. We provide a set of empirical formulas for the final mass, spin andrecoil velocity of the final black hole as a function of the mass ratio andindividual spins of the progenitor. In order to determine the fittingcoefficients for these formulas, we perform a set of 128 new numericalevolutions of precessing, unequal-mass black-hole binaries, and fit to theresulting remnant mass, spin, and recoil. In order to reduce the complexity ofthe analysis, we chose configurations that have one of the black holesspinning, with dimensionless spin alpha=0.8, at different angles with respectto the orbital angular momentum, and the other non-spinning. In addition toevolving families of binaries with different spin-inclination angles, we alsoevolved binaries with mass ratios as small as q=1/6. We use the resultingempirical formulas to predict the probabilities of black hole mergers leadingto a given recoil velocity, total radiated gravitational energy, and finalblack hole spin.

Modeling the remnant mass, spin, and recoil from unequal-mass, precessing black-hole binaries: The Intermediate Mass Ratio Regime