  The formation of self-gravitating systems is studied by simulating the
collapse of a set of N particles which are generated from several distribution
functions. We first establish that the results of such simulations depend on N
for small values of N. We complete a previous work by Aguilar and Merritt
concerning the morphological segregation between spherical and elliptical
equilibria. We find and interpret two new segregations: one concerns the
equilibrium core size and the other the equilibrium temperature. All these
features are used to explain some of the global properties of self-gravitating
objects: origin of globular clusters and central black hole or shape of
elliptical galaxies.
