The effect of the environment on the Interstellar Medium of disk galaxies

星系内部恒星之间的空间充满了星际介质（ISM），其演变是一种多相，可压缩，磁化和湍流介质。其复杂和非线性的物理学涉及巨大的空间和时间尺度。计算能力的限制仍然迫使我们做出选择：要么以亚pc分辨率研究小的ISM体积，要么以~ 50 pc分辨率和亚网格模型研究未解决的物理问题。这是不幸的，因为，小尺度和大尺度都很重要：星星的形成和恒星反馈发生在次pc尺度甚至更小的尺度上。在全球范围内，星系嵌入其宇宙环境中：大多数星系不是孤立的，而是居住在星系群或星系团中，其中充满了热的，稀薄的星系团内介质（ICM）。这对星系的ISM施加了静态和冲压压力，其大小与ISM压力相当。因此，ISM响应集群环境。我们提出了两个主要步骤的ISM的集成视图：（i）我们研究的ISM的耦合到集群环境的ICM。(ii)为此目的，我们结合联合收割机ISM模拟在银河系范围内的模拟的kpc大小的体积的ISM解决到次pc尺度。因此，我们使用独特的集群环境，以获得新的见解的物理过程中的ISM。

The space between the stars inside galaxies is filled by the interstellar medium (ISM), whose evolution is that of a multi-phase, compressible, magnetised and turbulent medium. Its complex and non-linear physics involve a huge range of spatial and temporal scales. Limits in computational power still force us to a make choice: either to study small ISM volumes at sub-pc resolution, or the global ISM of a galaxy with ~ 50 pc resolution and subgrid models for unresolved physics. This is unfortunate, because, both, small and large scales are important: Star formation and stellar feedback occur on sub-pc scales or even smaller. On the global scale, galaxies are embedded in their cosmic environment: most galaxies are not isolated but reside in galaxy groups or clusters, which are filled with a hot, tenuous intra-cluster medium (ICM). This exerts static and ram pressures onto the galaxies’ ISM, with a magnitude comparable to ISM pressures. Consequently, the ISM responds to the cluster environment.We propose two major steps towards an integrated view of the ISM: (i) We study the coupling of the ISM to the ICM of the cluster environment. (ii) For this purpose, we combine ISM simulations on a galaxy-wide scale with simulations of a kpc-size volume of ISM resolved down to sub-pc scales. Thus, we use the unique cluster environment to get new insights into the physical processes in the ISM.