从暗物质-重子能量转移计算团密度的斜率
Cluster density slopes from Dark Matter-Baryons Energy Transfer
摘要：
在本文中，我们推广了前人关于暗物质密度剖面中质量与内斜率关系的工作。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反馈的能量转移模型，以及通过重子团的动力学摩擦。我们表明，在星系质量以上的质量范围内（星系群和星系团），内部斜率-质量关系改变了其趋势。它在对应于星系群的质量周围变陡（朝向不太尖的轮廓），在大质量的星系团中再次变陡。这种扁平化是由活动星系核的外流（活动星系核反馈）产生的。$α$上的单$ σ$散射在所有质量范围内（$Δα\simeq 0.3$）近似恒定。这是第一篇论文扩展的内部密度轮廓斜率质量关系的星系团，占重子的作用。结果可以用来获得一个完整的密度分布，也考虑到重子。这种密度分布以前只适用于星系。
英文摘要：
In this paper, we extend previous works on the relation between mass and the inner slope in dark matter density profiles. We calculate that relation in the mass range going from dwarf galaxies to cluster of galaxies. This was done thanks to a modeling of energy transfer via SN and AGN feedback, as well as via dynamical friction of baryon clumps. We show that, in the mass range above galaxy masses (Groups and clusters), the inner slope-mass relation changes its trend. It flattens (towards less cuspy profile) around masses corresponding to groups of galaxies and steepens again for large galaxy cluster masses. The flattening is produced by the AGN outflows (AGN feedback). The one-$ σ$ scatter on $α$ is approximately constant in all the mass range ($Δα\simeq 0.3$). 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.
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