We present the first numerical simulations of an initially nonspinning black-hole binary with mass ratio as large as $10:1$ in full general relativity. The binary completes approximately three orbits prior to merger and radiates $(0.415\pm 0.017)\%$ of the total energy and $(12.48\pm 0.62)\%$ of the initial angular momentum in the form of gravitational waves. The single black hole resulting from the merger acquires a kick of $(66.7\pm 3.3)\mathrm{km}/\mathrm{s}$ relative to the original center of mass frame. The resulting gravitational waveforms are used to validate existing formulas for the recoil, final spin, and radiated energy over a wider range of the symmetric mass ratio parameter $\eta =M_1{M}_2/(M_1+M_2{)}^2$ than previously possible. The contributions of $\ell >2$ multipoles are found to visibly influence the gravitational wave signal obtained at fixed inclination angles.

• Received 24 November 2008

DOI:https://doi.org/10.1103/PhysRevD.79.124006