  We study velocity moments of elliptical galaxies in the Coma cluster using
Jeans equations. The dark matter distribution in the cluster is modelled by a
generalised formula based upon the results of cosmological N-body simulations.
Its inner slope (cuspy or flat), concentration, and mass within the virial
radius are kept as free parameters, as well as the velocity anisotropy, assumed
independent of position. We show that the study of line-of-sight velocity
dispersion alone does not allow to constrain the parameters. By a joint
analysis of the observed profiles of velocity dispersion and kurtosis we are
able to break the degeneracy between the mass distribution and velocity
anisotropy. We determine the dark matter distribution at radial distances
larger than 3% of the virial radius and we find that the galaxy orbits are
close to isotropic. Due to limited resolution, different inner slopes are found
to be consistent with the data and we observe a strong degeneracy between the
inner slope $\alpha$ and concentration $c$: the best-fitting profiles have the
two parameters related with $c=19 - 9.6 \alpha$. Our best-fitting NFW profile
has concentration $c=9$, which is 50% higher than standard values found in
cosmological simulations for objects of similar mass. The total mass within the
virial radius of $2.9 h_{70}^{-1}$ Mpc is $1.4 \times 10^{15} h_{70}^{-1}
M_{\sun}$ (with 30% accuracy), 85% of which is dark. At this distance from the
cluster centre, the mass-to-light ratio in the blue band is $351 h_{70}$ solar
units. The total mass within the virial radius leads to estimates of the
density parameter of the Universe, assuming that clusters trace the
mass-to-light ratio and baryonic fraction of the Universe, with $\Omega_0=0.29
\pm 0.1$.
