  We analyze the properties of VIRGO detector with the aim of studying its
ability to search for coalescing black hole binaries. We focus on the remnants
of the Population III stars, which currently should be massive black holes
($\sim 100-1000 M_\odot$), some of them bound in binary systems. The
coalescence of such binaries due to emission of gravitational waves may be
currently observable. We use a binary population synthesis to model the
evolution of Population III binaries. We calculate the signal to noise ratios
of gravitational waves emitted by the system in each of the coalescence phase:
inspiral, merger and ringdown, and provide simple formulae for the signal to
noise ratio as a function of masses of the binaries. We estimate the detection
rates for the VIRGO interferometer and also compare them with the estimates for
the current LIGO. We show that these expected rates are similar to, or larger
than the expected rates from coalescences of Population I and II compact object
binaries.
