nIFTy星系团模拟VI：气态星系团外围子结构的动力学印记
nIFTy Galaxy Cluster simulations VI: The dynamical imprint of substructure on gaseous cluster outskirts
摘要：
星系团外围标志着从轻度非线性宇宙网到高度非线性、维里化的星系团内部的过渡区域。正是在这个过渡区，星系团内介质（ICM）开始影响吸积星系和星系团的性质，因为冲压压力影响星系的冷气含量和随后的恒星形成率。相反，在这个过渡区的ICM的物理性质也应该感受到吸积子结构（即星系和集团）的影响，其通过可以驱动冲击。在本文中，我们使用一套宇宙学流体动力学变焦模拟的一个单一的星系团，从NIFTY比较项目，研究如何从宇宙网吸积的子结构的动力学影响的ICM在集群的外围的物理性质。我们演示了如何在ICM（如气体密度和温度）的径向配置文件中明显的功能可以链接到强冲击，瞬态和短暂的性质，驱动通过的子结构。在我们的比较中，天体物理学代码和星系形成模型的范围在它们的预测中大体上是一致的（例如，在冲击发生的时间和地点上是一致的，但在冲击的强度上是不同的）;这是我们对由大尺度引力动力学和强的、低效的辐射冲击驱动的过程的预期。这表明，在一个集群的外围ICM映射这样的冲击结构（通过例如无线电同步辐射）可以提供一个补充措施，其最近的合并和吸积的历史。
英文摘要：
Galaxy cluster outskirts mark the transition region from the mildly non-linear cosmic web to the highly non-linear, virialised, cluster interior. It is in this transition region that the intra-cluster medium (ICM) begins to influence the properties of accreting galaxies and groups, as ram pressure impacts a galaxy's cold gas content and subsequent star formation rate. Conversely, the thermodynamical properties of the ICM in this transition region should also feel the influence of accreting substructure (i.e. galaxies and groups), whose passage can drive shocks. In this paper, we use a suite of cosmological hydrodynamical zoom simulations of a single galaxy cluster, drawn from the nIFTy comparison project, to study how the dynamics of substructure accreted from the cosmic web influences the thermodynamical properties of the ICM in the cluster's outskirts. We demonstrate how features evident in radial profiles of the ICM (e.g. gas density and temperature) can be linked to strong shocks, transient and short-lived in nature, driven by the passage of substructure. The range of astrophysical codes and galaxy formation models in our comparison are broadly consistent in their predictions (e.g. agreeing when and where shocks occur, but differing in how strong shocks will be); this is as we would expect of a process driven by large-scale gravitational dynamics and strong, inefficiently radiating, shocks. This suggests that mapping such shock structures in the ICM in a cluster's outskirts (via e.g. radio synchrotron emission) could provide a complementary measure of its recent merger and accretion history.
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