Coalescence remnant of spinning binary black holes

We compute the gravitational radiation generated in the evolution of a family of close binary black hole configurations, using a combination of numerical and perturbative approximation methods. We evolve the binaries with spins s aligned or counteraligned with the orbital angular momentum from near the innermost stable circular orbit down to the final single rotating black hole. For the moderately spinning holes studied here the remnant Kerr black holes formed at the end of an inspiral process have rotation parameters a/Mapproximate to0.72+0.32(s/m(H)), suggesting it is difficult (though not excluded) to end up with near maximally rotating holes from such scenarios.