论文标题
模拟银河系群中的几乎边缘斜率Abell 2199
Simulating nearly edge-on sloshing in the galaxy cluster Abell 2199
论文作者
论文摘要
星系簇之间的外轴碰撞可能会诱发晃动的现象，从而导致浓烈的气体从簇的凉爽核心中拖动，从而导致增强的X射线发射。 Abell 2199在其核心中显示晃动的签名，并且可能几乎可以看到碰撞的轨道平面。我们的目的是评估Abell 2199的特征是否可以通过在较大的倾斜角度下看到的宽度螺旋来解释。为了解决这个问题，我们与$ M_ {200} = 1.6 \ times10^{13} \，{\ rm m _ {\ odot}} $的星系组进行了量身定制的流体动力学$ n $ body模拟。我们获得了一个合适的方案，其中小组通过主簇核心0.8 Gyr以前，而山间分离为292 kpc。从温度图以及从$β$模型拟合到模拟X射线发射的残差中获得了良好的一致性。我们发现，在$ i = 70^{\ circ} $的倾向下，仿真结果与观测值保持一致。
Off-axis collisions between galaxy clusters may induce the phenomenon of sloshing, causing dense gas to be dragged from the cool core of a cluster, resulting in a spiral of enhanced X-ray emission. Abell 2199 displays signatures of sloshing in its core and it is possible that the orbital plane of the collision is seen nearly edge-on. We aim to evaluate whether the features of Abell 2199 can be explained by a sloshing spiral seen under a large inclination angle. To address this, we perform tailored hydrodynamical $N$-body simulations of a non-frontal collision with a galaxy group of $M_{200}=1.6\times10^{13}\,{\rm M_{\odot}}$. We obtain a suitable scenario in which the group passed by the main cluster core 0.8 Gyr ago, with a pericentric separation of 292 kpc. Good agreement is obtained from the temperature maps as well as the residuals from a $β$-model fit to the simulated X-ray emission. We find that under an inclination of $i=70^{\circ}$ the simulation results remain consistent with the observations.
