Reducing eccentricity in black-hole binary evolutions with initial parameters from post-Newtonian inspiral

Standard choices of quasicircular orbit parameters for black-hole binary evolutions result in eccentric inspiral. We introduce a conceptually simple method, which is to integrate the post-Newtonian equations of motion through hundreds of orbits, and read off the values of the momenta at the separation at which we wish to start a fully general relativistic numerical evolution. For the particular case of nonspinning equal-mass inspiral with an initial coordinate separation of D=11M we show that this approach reduces the eccentricity by at least a factor of 5 to e<0. 002 as compared to using standard quasicircular initial parameters.