The impact of environment on distant spiral galaxy evolution: velocity fields and Tully-Fisher relation of intermediate-redshift cluster galaxies; observations and numerical simulations

星系团在理解宇宙结构增长方面发挥着重要作用。除了CDM理论中预期的星系通过合并的聚集外，其他相互作用现象在星系团环境中也很重要（星系之间，还有星系团内介质和星系气体之间的流体动力学过程，以及星系团作为一个整体的影响）。为了测试这些过程的重要性，我们研究的恒星种群（大小，光度，形态），在很大程度上取决于当前的星星形成活动，但也通过其内部运动学的总引力势的影响，发光和暗物质。我们追踪星系团中z = 0.5的星系可能的相互作用机制，通过它们的结构特征（使用我们的HST/ACS图像）和全二维速度场（使用我们的VLT 3D光谱）。为了解开各种相互作用机制及其对集群人口演化的重要性，我们直接将我们的观测结果与我们在星系尺度和集群尺度上进行的N体/流体动力学模拟进行比较。在规则运动学的情况下，可以高精度地确定塔利-费舍尔关系的演变。我们在这里要求资助完成2个正在进行的博士论文研究（1个观察，1个数值）。

Galaxy clusters play a fundamental role for the understanding of structure growth in the Universe. Besides the expected assembly of galaxies via mergers in the CDM theory, other interaction phenomena are important in the cluster environment (among galaxies but also hydrodynamic processes between the Intracluster Medium and the galaxy gas, and the influence of a cluster as a whole). To test the importance of these processes we study the stellar populations (sizes, luminosities, morphologies) that heavily depend on the current star formation activity, but also the total gravitational potential via their internal kinematics which are influenced by both luminous and dark matter. We trace possible interaction mechanisms of galaxies in clusters at z ≈ 0.5 by their signatures in structure (with our HST/ACS images) and in the full 2-dimensional velocity field (with our VLT 3D-spectroscopy). To disentangle the various interaction mechanisms and their importance for the evolution of the cluster population, we compare our observations directly with N-body/hydrodynamic simulations we perform both on galaxy scales and cluster scales. In the case of regular kinematics, the evolution of the Tally-Fisher relation can be determined with high accuracy. We ask here for funding to finish 2 ongoing PhD thesis studies (1 observational, 1 numerical).