Dark and visible matter distribution in Coma cluster: theory vs
  observations
  We investigate dark and visible matter distribution in the Coma cluster in
the case of the Navarro-Frenk-White (NFW) profile. A toy model where all
galaxies in the cluster are concentrated inside a sphere of an effective radius
$R_{\mathrm{eff}}$ is considered. It enables us to obtain the mean velocity
dispersion as a function of $R_{\mathrm{eff}}$. We show that, within the
observation accuracy of the NFW parameters, the calculated value of
$R_{\mathrm{eff}}$ can be rather close to the observable cutoff of the galaxy
distribution. Moreover, the comparison of our toy model with the observable
data and simulations leads to the following preferable NFW parameters for the
Coma cluster: $R_{200} \approx 1.77\,h^{-1} \, \mathrm{Mpc} = 2.61\,
\mathrm{Mpc}$, $c=3\div 4$ and $M_{200}= 1.29h^{-1}\times10^{15}M_{\odot}$. In
the Coma cluster the most of galaxies are concentrated inside a sphere of the
effective radius $R_{\mathrm{eff}}\sim 3.7$ Mpc and the line-of-sight velocity
dispersion is $1004\, \mathrm{km}\, \mathrm{s}^{-1}$.
