Abstract

We propose simple empirical formulae to describe the final remnant mass, spin, and recoil velocity from the merger of quasi-circular black-hole binaries with arbitrary mass ratios and spins. Our formulae are based on the post-Newtonian scaling with constant parameters chosen by a least-squares fit of the available data from recent fully nonlinear numerical simulations and is relevant to statistical studies of N-body simulations of galaxy cores and clusters, and the cosmological growth of supermassive black holes.