  We discuss the prospects of gravitational lensing of gravitational waves
(GWs) coming from core-collapse supernovae (CCSN). As the CCSN GW signal can
only be detected from within our own Galaxy and the local group by current and
upcoming ground-based GW detectors, we focus on microlensing. We introduce a
new technique based on analysis of the power spectrum and association of peaks
of the power spectrum with the peaks of the amplification factor to identify
lensed signals. We validate our method by applying it on the CCSN-like mock
signals lensed by a point mass lens. We find that the lensed and unlensed
signal can be differentiated using the association of peaks by more than one
sigma for lens masses M$_{\rm L} {>} 150{\rm M}_{\odot}$. We also study the
correlation integral between the power spectra and corresponding amplification
factor. This statistical approach is able to differentiate between unlensed and
lensed signals for lenses as small as M$_{\rm L} {\sim} 15{\rm M}_{\odot}$.
Further, we demonstrate that this method can be used to estimate the mass of a
lens in case the signal is lensed. The power spectrum based analysis is general
and can be applied to any broad band signal and is especially useful for
incoherent signals.
