  We estimate the observed distribution of chirp masses of compact object
binaries for the gravitational wave detectors. The stellar binary evolution is
modeled using the {\em StarTrack} population synthesis code. The distribution
of the predicted "observed" chirp masses vary with variation of different
parameters describing stellar binary evolution. We estimate the sensitivity of
the observed distribution to variation of these parameters and show which of
the parameters can be constrained after observing 20, 100, and 500 compact
object mergers. As a general feature of all our models we find that the
population of observed binaries is dominated by the double black hole mergers.
