In this paper we study the density profiles of self-interacting dark matter (SIDM) haloes spanning the full observable mass range, from dwarf galaxies to galaxy clusters. Using realistic simulations that model the baryonic physics relevant for galaxy formation, we compare the density profiles of haloes simulated with either SIDM or cold and collisionless dark matter (CDM) to those inferred from observations of stellar velocity dispersion, gas rotation curves, weak and strong gravitational lensing, and/or X-ray maps. We make our comparison in terms of the maximal surface density of haloes, circumventing the need for semi-analytic or parametric models for dark matter density profiles. We find that the maximal surface density as a function of halo mass is well reproduced by simulations of CDM that include baryons, and that a SIDM cross-section of 1 cm$^2/$g is marginally excluded. This constraint is driven mainly by galaxy clusters, with less massive systems being relatively less affected by DM self-interactions with velocity-independent cross-section.

中文翻译：

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从矮星系到星系团：晕质量超过 7 个数量级的自相互作用暗物质

在本文中，我们研究了自相互作用暗物质 (SIDM) 晕的密度分布，涵盖了从矮星系到星系团的整个可观测质量范围。使用模拟与星系形成相关的重子物理学的现实模拟，我们比较了用 SIDM 或冷无碰撞暗物质 (CDM) 模拟的晕圈的密度分布与从恒星速度色散、气体旋转曲线、弱和强的观测推断的那些引力透镜和/或 X 射线图。我们根据光晕的最大表面密度进行比较，避免了对暗物质密度剖面的半解析或参数模型的需要。我们发现最大表面密度作为晕质量的函数可以通过包含重子的 CDM 模拟得到很好的再现，并且略微排除了 1 cm$^2/$g 的 SIDM 横截面。这种约束主要由星系团驱动，质量较小的系统受具有与速度无关的横截面的 DM 自相互作用的影响相对较小。