Orbital evolution of satellite galaxies in self-interacting dark matter models
Orbital evolution of satellite galaxies in self-interacting dark matter models
复制标题
DOI：
10.1103/physrevd.107.043014
复制
发表时间：
2021-08
影响因子：
5
通讯作者：
O. Slone;F. Jiang;M. Lisanti;M. Kaplinghat
中科院分区：
文献类型：
--
作者：
O. Slone;F. Jiang;M. Lisanti;M. Kaplinghat
暗物质的自相互作用可以在银河系周围的卫星星系的性质上留下独特的特征-就像它们对潮汐剥离、冲压压力和重力热坍缩的影响一样。我们描绘了自相互作用的暗物质参数空间的区域-指定的相互作用截面和速度尺度-在这些影响中的每一个占主导地位，并显示相对质量损失如何取决于卫星的初始质量，密度分布和轨道。我们获得了新的，保守的约束，在这个参数空间使用银河系卫星星系有显着高的中心密度和小的近心距离。我们的结果自相互作用的暗物质模型，结合星系团的约束，有利于速度依赖的横截面，导致重力热核心崩溃的dennis卫星，或小的横截面，更接近冷和无碰撞的暗物质。
Dark matter self interactions can leave distinctive signatures on the properties of satellite galaxies around Milky Way--like hosts through their impact on tidal stripping, ram pressure, and gravothermal collapse. We delineate the regions of self-interacting dark matter parameter space -- specified by interaction cross section and a velocity scale -- where each of these effects dominates, and show how the relative mass loss depends on the satellite's initial mass, density profile and orbit. We obtain novel, conservative constraints in this parameter space using Milky Way satellite galaxies with notably high central densities and small pericenter distances. Our results for self-interacting dark matter models, in combination with constraints from clusters of galaxies, favor either velocity-dependent cross sections that lead to gravothermal core collapse in the densest satellites, or small cross sections which more closely resemble cold and collisionless dark matter.