The study of velocity fields of the hot gas in galaxy clusters can help to unravel details of microphysics on small scales and to decipher the nature of feedback by active galactic nuclei (AGN). Likewise, magnetic fields as traced by Faraday rotation measurements (RMs) inform about their impact on gas dynamics as well as on cosmic ray production and transport. We investigate the inherent relationship between large-scale gas kinematics and magnetic fields through non-radiative magnetohydrodynamical simulations of the creation, evolution, and disruption of AGN jet-inflated lobes in an isolated Perseus-like galaxy cluster, with and without pre-existing turbulence. In particular, we connect cluster velocity measurements with mock RM maps to highlight their underlying physical connection, which opens up the possibility of comparing turbulence levels in two different observables. For single-jet outbursts, we find only a local impact on the velocity field, i.e. the associated increase in velocity dispersion is not volume-filling. Furthermore, in a setup with pre-existing turbulence, this increase in velocity dispersion is largely hidden. We use mock X-ray observations to show that at arcmin resolution, the velocity dispersion is therefore dominated by existing large-scale turbulence and is only minimally altered by the presence of a jet. For the velocity structure of central gas uplifted by buoyantly rising lobes, we find fast, coherent outflows with low velocity dispersion. Our results highlight that projected velocity distributions show complex structures, which pose challenges for the interpretation of observations.

中文翻译：

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将星系团模拟中的湍流速度和磁场与活动星系核喷流联系起来

对星系团中热气体速度场的研究有助于揭示小尺度微观物理学的细节，并破译活动星系核（AGN）反馈的性质。同样，由法拉第旋转测量 (RM) 追踪的磁场可以告知它们对气体动力学以及宇宙射线产生和传输的影响。我们通过非辐射磁流体动力学模拟在孤立的类似英仙座的星系团中，AGN 喷射膨胀叶的产生、演化和破坏，研究了大规模气体运动学和磁场之间的内在关系，有和没有预先存在的湍流. 特别是，我们将集群速度测量与模拟 RM 地图连接起来，以突出它们潜在的物理连接，这开辟了比较两个不同观测值的湍流水平的可能性。对于单喷流爆发，我们发现只有局部对速度场的影响，即速度分散的相关增加不是体积填充。此外，在预先存在湍流的设置中，这种速度分散的增加在很大程度上是隐藏的。我们使用模拟 X 射线观测结果表明，在 arcmin 分辨率下，速度色散因此受现有大尺度湍流的支配，并且仅因射流的存在而发生微小变化。对于由浮力上升的裂片抬升的中心气体的速度结构，我们发现快速、连贯的流出物具有低速度分散。我们的研究结果强调，预计的速度分布显示出复杂的结构，这对解释观测结果提出了挑战。