  Coalescing binary black-hole systems are among the most promising sources of
gravitational waves for ground-based interferometers. While the \emph{inspiral}
and \emph{ring-down} stages of the binary black-hole coalescence are
well-modelled by analytical approximation methods in general relativity, the
recent progress in numerical relativity has enabled us to compute accurate
waveforms from the \emph{merger} stage also. This has an important impact on
the search for gravitational waves from binary black holes. In particular,
while the current gravitational-wave searches look for each stage of the
coalescence separately, combining the results from analytical and numerical
relativity enables us to \emph{coherently} search for all three stages using a
single template family. `Complete' binary black-hole waveforms can now be
produced by matching post-Newtonian waveforms with those computed by numerical
relativity. These waveforms can be parametrised to produce analytical waveform
templates. The `complete' waveforms can also be used to estimate the efficiency
of different search methods aiming to detect signals from black-hole
coalescences. This paper summarises some recent efforts in this direction.
