  We present new techniqes for evolving binary black hole systems which allow
the accurate determination of gravitational waveforms directly from the wave
zone region of the numerical simulations. Rather than excising the black hole
interiors, our approach follows the "puncture" treatment of black holes, but
utilzing a new gauge condition which allows the black holes to move
successfully through the computational domain. We apply these techniques to an
inspiraling binary, modeling the radiation generated during the final plunge
and ringdown. We demonstrate convergence of the waveforms and good conservation
of mass-energy, with just over 3% of the system's mass converted to gravitional
radiation.
