The formation of galaxies is significantly influenced by galactic winds, possibly driven by cosmic rays due to their long cooling times and better coupling to plasma compared to radiation. In this study, we compare the radio observations of the edge-on galaxy NGC 4217 from the CHANG-ES collaboration catalog with a mock observation of an isolated galaxy based on the arepo simulation that adopts the state-of-the-art two-moment cosmic ray transport treatment and multiphase interstellar medium model. We find significant agreement between the simulated and observed images and spectroscopic data for reasonable model parameters. Specifically, we find that (i) the shape of the intensity profiles depends weakly on the magnitude of the magnetic field, the distance of the simulated galaxy, and the normalization of the CR electron spectrum. The agreement between the mock and actual observations is degenerate with respect to these factors; (ii) the multiwavelength spectrum above 0.1 GHz is in agreement with the radio observations and its slope is also only weakly sensitive to the magnetic field strength; (iii) the magnetic field direction exhibits X-shaped morphology, often seen in edge-on galaxies, which is consistent with the observations and indicates the presence of a galactic-scale outflow. Our results highlight the importance of incorporating advanced cosmic ray transport models in simulations and provide a deeper understanding of galactic wind dynamics and its impact on galaxy evolution.

中文翻译：

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模拟宇宙射线驱动的银河风的射电同步加速器形态、光谱和极化


星系的形成受到星系风的显着影响，可能是由宇宙射线驱动的，因为它们的冷却时间长，而且与辐射相比，它们与等离子体的耦合效果更好。在这项研究中，我们将 CHANG-ES 合作目录中边缘星系 NGC 4217 的射电观测与基于 arepo 模拟的孤立星系的模拟观测进行了比较，该模拟采用了最先进的两矩宇宙射线传输处理和多相星际介质模型。我们发现，对于合理的模型参数，模拟和观测图像与光谱数据之间存在显著的一致性。具体来说，我们发现 （i） 强度分布的形状对磁场的大小、模拟星系的距离和 CR 电子谱的归一化有微弱的影响。就这些因素而言，模拟观测值和实际观测值之间的一致性是退化的;（ii） 0.1 GHz 以上的多波长光谱与射电观测一致，其斜率对磁场强度也仅弱敏感;（iii） 磁场方向呈现出 X 形形态，这在边缘星系中很常见，这与观测结果一致，表明存在银河系尺度的流出。我们的结果强调了在模拟中纳入高级宇宙射线传输模型的重要性，并提供了对银河系风动力学及其对星系演化影响的更深入理解。