  We study the non-Gaussian tail of the probability distribution function of
density in cosmological N-Body simulations for a variety of initial conditions.
We compare the behaviour of the non-Gaussian tail in the real space with that
in the redshift space. The form of the PDF in redshift space is of great
significance as galaxy surveys probe this and not the real space analogue
predicted using theoretical models. We model the non-Gaussian tail using the
halo model. In the weakly non-linear regime the moments of counts in cells in
the redshift space approach the values expected from perturbation theory for
moments in real space. We show that redshift space distortions in the
non-linear regime dominate over signatures of initial conditions or the
cosmological background. We illustrate this using Skewness and higher moments
of counts in cells, as well as using the form of the non-Gaussian tail of the
distribution function. We find that at scales smaller than the scale of
non-linearity the differences in Skewness, etc. for different models are very
small compared to the corresponding differences in real space. We show that
bias also leads to smaller values of higher moments, but the redshift space
distortions are typically the dominant effect.
