  Understanding the fate of merging supermassive black holes in galactic
mergers, and the gravitational wave emission from this process, are important
LISA science goals. To this end, we present results from numerical relativity
simulations of binary black hole mergers using the so-called Lazarus approach
to model gravitational radiation from these events. In particular, we focus
here on some recent calculations of the final spin and recoil velocity of the
remnant hole formed at the end of a binary black hole merger process, which may
constraint the growth history of massive black holes at the core of galaxies
and globular clusters.
