具有罕见和频繁暗物质自相互作用的宇宙学模拟
Cosmological simulations with rare and frequent dark matter self-interactions
摘要：
具有自相互作用的暗物质（DM）是解决标准宇宙学模型小尺度问题的一个很有前途的方案。在这里，我们进行频繁的DM自相互作用，对应于小角度DM散射的第一个宇宙学模拟。我们分析的重点在于发现和理解传统上假设的罕见DM（大角度）自散射的差异。为此，我们计算了DM密度分布、物质功率谱、两点关联函数以及晕和次晕质量函数。此外，我们还研究了DM晕的密度分布及其形状。我们发现，整体的大角度和小角度散射的行为相当相似，有几个例外。特别是，卫星的数量是相当大的抑制频繁相比，罕见的自相互作用具有相同的横截面。总的来说，我们观察到，虽然这两种情况之间的差异可能很难建立使用一个单一的措施，简并可以通过多种措施的组合突破。例如，卫星计数与晕密度或形状轮廓的组合可以允许区分罕见和频繁的自我相互作用。作为我们分析的副产品，我们首次提供了频繁自相互作用的横截面上限。
英文摘要：
Dark matter (DM) with self-interactions is a promising solution for the small-scale problems of the standard cosmological model. Here we perform the first cosmological simulation of frequent DM self-interactions, corresponding to small-angle DM scatterings. The focus of our analysis lies in finding and understanding differences to the traditionally assumed rare DM (large-angle) self scatterings. For this purpose, we compute the distribution of DM densities, the matter power spectrum, the two-point correlation function and the halo and subhalo mass functions. Furthermore, we investigate the density profiles of the DM haloes and their shapes. We find that overall large-angle and small-angle scatterings behave fairly similarly with a few exceptions. In particular, the number of satellites is considerably suppressed for frequent compared to rare self-interactions with the same cross-section. Overall we observe that while differences between the two cases may be difficult to establish using a single measure, the degeneracy may be broken through a combination of multiple ones. For instance, the combination of satellite counts with halo density or shape profiles could allow discriminating between rare and frequent self-interactions. As a by-product of our analysis, we provide - for the first time - upper limits on the cross-section for frequent self-interactions.
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