  The inner slope (gammadm) of the dark matter (DM) density profile of
cosmological halos carries information about the properties of DM and/or
baryonic processes affecting the halo gravitational potential. Cold DM
cosmological simulations predict steep inner slopes, gammadm~1. We test this
prediction on the MACS J1206.2-0847 cluster at redshift z=0.44, whose DM
density profile was claimed to be cored at the center. We determine the cluster
DM density profile from 2 kpc from the cluster center to the virial radius (~2
Mpc), using the velocity distribution of ~500 cluster galaxies and the internal
velocity dispersion profile of the Brightest Cluster Galaxy (BCG), obtained
from VIMOS@VLT and MUSE@VLT data. We solve the Jeans equation of dynamical
equilibrium using an upgraded version of the MAMPOSSt method. The total mass
profile is modeled as a sum of a generalized-NFW profile that describes the DM
component, allowing for a free inner slope of the density profile, a Jaffe
profile that describes the BCG stellar mass component, and a non-parametric
baryonic profile that describes the sum of the remaining galaxy stellar mass
and of the hot intra-cluster gas mass. Our total mass profile is in remarkable
agreement with independent determinations based on X-ray observations and
strong lensing. We find gammadm=0.7 (-0.1 +0.2) (68\% confidence levels),
consistent with predictions from recent LambdaCDM cosmological numerical
simulations.
