Cluster density slopes from Dark Matter-Baryons Energy Transfer
  In this paper, we extend previous works on the relation between mass and the
inner slope in dark matter density profiles. We calculate that relation in the
mass range going from dwarf galaxies to cluster of galaxies. This was done
thanks to a modeling of energy transfer via SN and AGN feedback, as well as via
dynamical friction of baryon clumps. We show that, in the mass range above
galaxy masses (Groups and clusters), the inner slope-mass relation changes its
trend. It flattens (towards less cuspy profile) around masses corresponding to
groups of galaxies and steepens again for large galaxy cluster masses. The
flattening is produced by the AGN outflows (AGN feedback). The one-$ \sigma$
scatter on $\alpha$ is approximately constant in all the mass range
($\Delta\alpha\simeq 0.3$). This is the first paper extending the inner density
profile slope-mass relationship to clusters of galaxies, accounting for the
role of baryons. The result can be used to obtain a complete density profile,
also taking baryons into account. Such kind of density profile was previously
only available for galaxies.
