论文标题
Chex-Mate:样品的形态分析
CHEX-MATE: Morphological analysis of the sample
论文作者
论文摘要
在这项工作中,我们对118个Chex-Mate(带有XMM-Newton的群集遗产项目的X射线形态进行分析 - 结构形成的终点)的X射线形态)Galaxy簇,旨在提供其动力状态的分类。为了研究X射线外观与动态状态之间的联系,我们考虑了四个形态学参数:表面亮度浓度,质心移位和二阶和三阶功率比率。这些指标的结果是:彼此之间密切相关,在识别受干扰和放松的人群方面有力,其特征是单峰分布,不受系统不确定性的强烈影响。为了获得Chex-Mate对象的连续分类,我们将这四个参数组合为单个数量M,该参数表示系统的放松等级。在M值的基础上,我们确定了样品中最极端的系统,发现15个非常放松和27个非常干扰的星系簇。通过与先前对X射线选定样品的分析进行比较,我们证实了Sunyaev-Zeldovich(SZ)簇往往会受到更加干扰。最后,通过将我们的分析应用于模拟样本,我们发现了观察到的结果和模拟结果之间的一般一致性,而浓度的唯一除外。后一种行为与在模拟簇的中央区域中具有高平滑粒子流体动力学密度的颗粒的存在部分相关,这是由于理想化的各向同性热活性循环核(AGN)反馈的作用。
In this work, we performed an analysis of the X-ray morphology of the 118 CHEX-MATE (Cluster HEritage project with XMM-Newton - Mass Assembly and Thermodynamics at the Endpoint of structure formation) galaxy clusters, with the aim to provide a classification of their dynamical state. To investigate the link between the X-ray appearance and the dynamical state, we considered four morphological parameters: the surface brightness concentration, the centroid shift, and the second- and third-order power ratios. These indicators result to be: strongly correlated with each other, powerful in identifying the disturbed and relaxed population, characterised by a unimodal distribution and not strongly influenced by systematic uncertainties. In order to obtain a continuous classification of the CHEX-MATE objects, we combined these four parameters in a single quantity, M, which represents the grade of relaxation of a system. On the basis of the M value, we identified the most extreme systems of the sample, finding 15 very relaxed and 27 very disturbed galaxy clusters. From a comparison with previous analysis on X-ray selected samples, we confirmed that the Sunyaev-Zeldovich (SZ) clusters tend to be more disturbed. Finally, by applying our analysis on a simulated sample, we found a general agreement between the observed and simulated results, with the only exception of the concentration. This latter behaviour, is partially related to the presence of particles with high smoothed-particle hydrodynamics density in the central regions of the simulated clusters due to the action of the idealised isotropic thermal Active Galactic Nuclei (AGN) feedback.