We revisit the modeling of the properties of the remnant black hole resulting from 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 nonspinning .
In addition to evolving families of binaries with different spin-inclination angles , we also evolved binaries with mass ratios as small as q = M _ { 1 } / M _ { 2 } = 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 .