The non-Gaussian distribution of galaxies gravitational fields
  We perform a theoretical analysis of the observational dependence between
angular momentum of the galaxy clusters and their mass (richness), based on the
method introduced in our previous paper. For that we obtain the distribution
function of astronomical objects (like galaxies and/or smooth halos of
different kinds) gravitational fields due to their tidal interaction. Within
the statistical method of Chandrasekhar we are able to show that the
distribution function is determined by the form of interaction between objects
and for multipole (tidal) interaction it is never Gaussian. Our calculation
permits to demonstrate how the alignment of galaxies angular momenta depend on
the cluster richness. The specific form of the corresponding dependence is due
to assumptions made about cluster morphology. Our approach also predicts the
time evolution of stellar objects angular momenta within CDM and $\Lambda$CDM
models. Namely, we have shown that angular momentum of galaxies increases with
time.
