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 modelling 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.

在本文中，我们扩展了先前关于暗物质密度剖面中质量与内斜率之间关系的工作。我们计算了从矮星系到星系团的质量范围内的关系。这要归功于通过 SN 和 AGN 反馈以及通过重子团块的动态摩擦对能量转移进行建模。我们表明，在星系质量（群和星团）之上的质量范围内，内部斜率-质量关系会改变其趋势。它在对应于星系群的质量周围变平（朝向不那么尖的轮廓），并在较大的星系团质量处再次变陡。扁平化是由 AGN 流出（AGN 反馈）产生的。唯一的那个-$\sigma$ 散落在 $\alpha$ 在所有质量范围内近似恒定 ($\Delta \alpha \simeq 0.3$）。这是第一篇将内部密度剖面斜率-质量关系扩展到星系团的论文，解释了重子的作用。结果可用于获得完整的密度分布，同时考虑重子。这种密度分布以前只适用于星系。