标题： ROGER III：大X射线星系团周围投影相空间中的星系演化模式 显示英文标题

标题： Reconstructing Orbits of Galaxies in Extreme Regions (ROGER) III: galaxy evolution patterns in projected phase space around massive X-ray clusters

摘要： 我们使用de los Rios等人开发的ROGER代码，根据投影相空间图中的位置，将X射线星系团周围的星系分为五类：团星系、回溅星系、近期落入星系、正在落入星系和误掩星系。为了理解团环境对星系演化的影响，我们在五类中比较了恒星质量、比恒星形成率、大小和形态。按照Coenda等人的指导方针，对红色和蓝色星系进行了单独分析。对于红色星系，团星系与其他类别不同，具有抑制的比恒星形成率、更小的尺寸，并更可能被归类为椭圆星系。然而，其他类别之间的差异较小，回溅星系的比恒星形成率显著低于早期或近期落入星系。对于蓝色星系，我们发现近期落入星系比正在落入星系和误掩星系更小，而后者两者在大小上是相当的。我们的结果提供了证据，表明在一次通过后，团环境可以减少星系的恒星形成，改变其形态，并且还可以减小蓝色星系的尺寸。我们发现证据表明，对于所有类别，熄灭发生的速度快于从螺旋星系到椭圆星系的形态转变。虽然一旦星系进入团，熄灭明显增强，但显著的形态转变需要星系经历团的物理机制更长时间尺度的作用。 显示英文摘要

摘要： We use the ROGER code by de los Rios et al. to classify galaxies around a sample of X-ray clusters into five classes according to their positions in the projected phase space diagram: cluster galaxies, backsplash galaxies, recent infallers, infalling galaxies, and interlopers. To understand the effects of the cluster environment to the evolution of galaxies, we compare across the five classes: stellar mass, specific star formation rate, size, and morphology. Following the guidelines of Coenda et al., a separate analysis is carried out for red and blue galaxies. For red galaxies, cluster galaxies differ from the other classes, having a suppressed specific star formation rate, smaller sizes, and are more likely to be classified as ellipticals. Differences are smaller between the other classes, however backsplash galaxies have significantly lower specific star formation rates than early or recent infalling galaxies. For blue galaxies, we find evidence that recent infallers are smaller than infalling galaxies and interlopers, while the latter two are comparable in size. Our results provide evidence that, after a single passage, the cluster environment can diminish a galaxy's star formation, modify its morphology, and can also reduce in size blue galaxies. We find evidence that quenching occurs faster than morphological transformation from spirals to ellipticals for all classes. While quenching is evidently enhanced as soon as galaxies get into clusters, significant morphological transformations require galaxies to experience the action of the physical mechanisms of the cluster for longer timescales.