Splashback in galaxy clusters as a probe of cosmic expansion and gravity
Splashback in galaxy clusters as a probe of cosmic expansion and gravity
复制标题
DOI：
10.1088/1475-7516/2018/11/033
复制
发表时间：
2018-06
影响因子：
6.4
通讯作者：
S. Adhikari;Jeremy Sakstein;B. Jain;N. Dalal;Baojiu Li
中科院分区：
文献类型：
--
作者：
S. Adhikari;Jeremy Sakstein;B. Jain;N. Dalal;Baojiu Li
回溅半径是暗物质晕中的一个物理尺度，由最近吸积的壳层的引力动力学决定。我们使用解析模型和N体模拟来研究回溅对暗能量的依赖性和筛选的修正引力理论。在改进的重力模型中，从屏蔽区到非屏蔽区的过渡通常发生在星团外围，这表明在回溅特征中可能存在可观察到的特征。我们研究了在变色龙和Vainshtein屏蔽模型中回溅的位置，并发现与ΛCDM预测相比有显着差异。我们还发现了一个有趣的动力学摩擦和修改后的重力之间的相互作用，提供了一个独特的签名修改后的重力模型在作为星系光度的函数的回溅功能的行为。
The splashback radius is a physical scale in dark matter halos that is set by the gravitational dynamics of recently accreted shells. We use analytical models and N-body simulations to study the dependence of splashback on dark energy and screened modified gravity theories. In modified gravity models, the transition from screened to unscreened regions typically occurs in the cluster outskirts, suggesting potentially observable signatures in the splashback feature. We investigate the location of splashback in both chameleon and Vainshtein screened models and find significant differences compared with ΛCDM predictions. We also find an interesting interplay between dynamical friction and modified gravity, providing a distinctive signature for modified gravity models in the behavior of the splashback feature as a function of galaxy luminosity.