  We have used N-body simulations to develop two independent methods to
quantify redshift distortions known as the Bull's Eye effect (large scale
infall plus small scale virial motion). This effect depends upon the mass
density, $\Omega_0$, so measuring it can in principle give an estimate of this
important cosmological parameter. We are able to measure the effect and
distinguish between its strength for high and low values of $\Omega_0$. Unlike
other techniques which utilize redshift distortions, one of our methods is
relatively insensitive to bias. In one approach, we use path lengths between
contour crossings of the density field. The other is based upon percolation. We
have found both methods to be successful in quantifying the effect and
distinguishing between values of $\Omega_0$. However, only the path lengths
method exhibits low sensitivity to bias.
