Shapes of Milky-Way-mass galaxies with self-interacting dark matter
Shapes of Milky-Way-mass galaxies with self-interacting dark matter
复制标题
具有自相互作用暗物质的银河系质量星系的形状
DOI：
10.1093/mnras/stac2069
复制
发表时间：
2022
影响因子：
4.8
通讯作者：
Graus, Andrew
中科院分区：
文献类型：
--
作者：
Vargya, Drona;Sanderson, Robyn;Sameie, Omid;Boylan-Kolchin, Michael;Hopkins, Philip F.;Wetzel, Andrew;Graus, Andrew
自相互作用暗物质（SIDM）模型提供了一种方法来调和观测结果与矮星系尺度上无碰撞冷暗物质（CDM）模型预测之间的不一致性。为了结合重子和SIDM相互作用的影响，我们研究了一套来自现实环境反馈（FIRE-2）项目的银河系（MW）质量星系的宇宙学-重子模拟，其中我们改变了SIDM自相互作用截面σ/m。在相同的初始条件下，我们比较了SIDM模拟预测的主暗物质（DM）晕在红移系数= 0时（σ/m= 0.1, 1和10 cm2g−1）与CDM模拟的形状。在重子反馈效应存在的情况下，我们发现SIDM模型并没有产生仅SIDM模型预测的毫微米质量星系内部结构的大差异。然而，我们确实发现总质量分布的形状开始与恒星质量分布的形状不同的半径依赖于σ/m。这种转换可能被用于设置MW中SIDM横截面的限制。
Self-interacting dark matter (SIDM) models offer one way to reconcile inconsistencies between observations and predictions from collisionless cold dark matter (CDM) models on dwarf-galaxy scales. In order to incorporate the effects of both baryonic and SIDM interactions, we study a suite of cosmological-baryonic simulations of Milky-Way (MW)-mass galaxies from the Feedback in Realistic Environments (FIRE-2) project where we vary the SIDM self-interaction cross-section σ/m. We compare the shape of the main dark matter (DM) halo at redshiftz= 0 predicted by SIDM simulations (at σ/m= 0.1, 1, and 10 cm2g−1) with CDM simulations using the same initial conditions. In the presence of baryonic feedback effects, we find that SIDM models do not produce the large differences in the inner structure of MW-mass galaxies predicted by SIDM-only models. However, we do find that the radius where the shape of the total mass distribution begins to differ from that of the stellar mass distributionisdependent on σ/m. This transition could potentially be used to set limits on the SIDM cross-section in the MW.