  We present results from numerical relativity simulations of equal mass,
non-spinning binary black hole inspirals and mergers with initial
eccentricities e <= 0.8 and coordinate separations D >= 12 M of up to 9 orbits
(18 gravitational wave cycles). We extract the mass M_f and spin a_f of the
final black hole and find, for eccentricities e < 0.4, that a_f/M_f = 0.69 and
M_f/M_adm = 0.96 are independent of the initial eccentricity, suggesting that
the binary has circularized by the merger time. For e > 0.5, the black holes
plunge rather than orbit, and we obtain a maximum spin parameter a_f/M_f = 0.72
around e = 0.5.
