  We use data on the local 3-dimensional galaxy distribution for studying the
statistics of the detection rates of gravitational waves (GW) coming from
supernova explosions. We consider both tensor and scalar gravitational waves
which are possible in a wide range of relativistic and quantum gravity
theories. We show that statistics of GW events as a function of sidereal time
can be used for distinction between scalar and tensor gravitational waves
because of the anisotropy of spatial galaxy distribution. For calculation of
the expected amplitudes of GW signals we use the values of the released GW
energy, frequency and duration of GW pulse which are consistent with existing
scenarios of SN core collapse. The amplitudes of the signals produced by Virgo
and the Great Attractor clusters of galaxies is expressed as a function of the
sidereal time for resonant bar detectors operating now (IGEC) and for
forthcoming laser interferometric detectors (VIRGO).Then, we calculate the
expected number of GW events as a function of sidereal time produced by all the
galaxies within 100 Mpc. In the case of axisymmetric rotational core collapse
which radiates a GW energy of $10^{-9}M_{\odot}c^2$, only the closest
explosions can be detected. However, in the case of nonaxisymmetric supernova
explosion, due to such phenomena as centrifugal hangup, bar and lump formation,
the GW radiation could be as strong as that from a coalescing neutron-star
binary. For radiated GW energy higher than $10^{-6}M_{\odot}c^2$ and
sensitivity of detectors at the level $h \approx 10^{-23}$ it is possible to
detect Virgo cluster and Great Attractor, and hence to use the statistics of GW
events for testing gravity theories.
