Cluster density slopes from dark matter–baryons energy transfer

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