AI 中文总结
本研究通过全物理模拟探究SIDM对星系晕的印记，发现重子与投影效应削弱其核心形成效应，弱引力透镜或可探测大质量星系晕的SIDM特征，为相关研究提供基线。
AI 中文摘要
本研究结合未来光学巡天，探究自相互作用暗物质（SIDM）对模拟星系群和星系团结构的印记。研究发现，重子效应和投影效应均会显著缓解SIDM在质量与密度分布上形成核心的行为，导致其与标准无碰撞暗物质的偏差极小（≤5%）；但对于质量最大的星系晕，SIDM反而会显著增强中心密度。研究将这些晕与两个星系团（MACS J1206和Abell S1063）的观测暗物质分布对比，发现考虑当前运动学质量测量的小观测误差时，SIDM可能在星系团核心留下可潜在探测的印记。此外，研究发现弱引力透镜观测是测试星系团尺度SIDM的有前景工具：在系统误差可控的理想场景中，对于M₂₀₀≥10¹³M⊙的星系晕，弱引力透镜剪切分布表现出高达约20%的偏差；而投影浓度-质量关系仅被SIDM模型轻微改变。研究还讨论了分析的局限性、模拟分辨率的影响及本工作的可能扩展。总体而言，本研究为未来SIDM研究提供了基线：尽管视线投影和重子效应显著降低了SIDM在星系晕质量分布上的印记，但星系团中的弱引力透镜和运动学分析，或可从兆秒差距到千秒差距尺度，实现对大质量结构中暗物质自相互作用的可靠探测与约束。
英文摘要
In this work we explore the imprints of self-interacting dark matter (SIDM) on the structure of simulated galaxy groups and clusters in view of future optical surveys. We find that both baryonic and projection effects lead to a significant alleviation of the SIDM core-forming behavior on the mass and density profiles, resulting in very small ($\lesssim 5\%$) deviations from standard collisionless dark matter. The opposite trend emerges for our most massive halos, where SIDM tends to significantly enhance the central density instead; we compare those halos with the observed dark matter profiles of two galaxy clusters, MACS J1206 and Abell S1063, finding that SIDM may leave potentially detectable imprints on cluster cores when considering the small observational uncertainty of current kinematic mass measurements. Finally, we find that weak lensing observations provide a promising tool for testing SIDM on cluster scales: in an idealized scenario where systematics are under control, weak lensing shear profiles exhibit up to $\sim 20\%$ level deviations for $M_{200} \gtrsim 10^{13}\ \text{M}_\odot$ halos. Conversely, the projected concentration-mass relation is only slightly modified by our SIDM models. We also discuss the limitiations of our analysis and the impact of the simulation resolution, as well as possible extension of this work. Overall, our results provide a baseline for future SIDM studies: although line-of-sight projection and baryonic effects significantly reduce SIDM imprints on halo mass profiles, weak lensing and kinematic analyses in galaxy clusters may potentially allow for robust detection and constraining of dark matter self-interactions in massive structures from megaparsec down to kiloparsec scales.
Comments17 pages, 15 figures, submitted to Astronomy and Astrophysics
