  We present the first simulations of non-headon (grazing) collisions of binary
black holes in which the black hole singularities have been excised from the
computational domain. Initially two equal mass black holes $m$ are separated a
distance $\approx10m$ and with impact parameter $\approx2m$. Initial data are
based on superposed, boosted (velocity $\approx0.5c$) solutions of single black
holes in Kerr-Schild coordinates. Both rotating and non-rotating black holes
are considered. The excised regions containing the singularities are specified
by following the dynamics of apparent horizons. Evolutions of up to $t \approx
35m$ are obtained in which two initially separate apparent horizons are present
for $t\approx3.8m$. At that time a single enveloping apparent horizon forms,
indicating that the holes have merged. Apparent horizon area estimates suggest
gravitational radiation of about 2.6% of the total mass. The evolutions end
after a moderate amount of time because of instabilities.
