Abstract—Based on the SDSS catalog data the properties of galaxies with quenched star formation (QGs) within the “splashback”-radius of galaxy clusters R_sp and beyond it have been studied. We used a sample of 40 groups and galaxy clusters and a sample of field galaxies at 0.02 < z < 0.045. The radii R_sp were defined from the observed integral distribution of the number of galaxies as a function of the squared distance from the center of the galaxy systems. We show that in galaxy clusters 72% of the QGs we have found are within R_sp. About 40% of these galaxies are late type ones with fracDeV < 0.8. Approximately 80% of galaxies with quenched star formation have stellar masses in the range of log M_∗/M_⊙ = [10; 11]. We found that QGs of late types and of early types in a less degree have maximum angular radii R_90,r and R_50,r near the “splashback”-radius of groups and clusters of galaxies. Our results confirm the assumption that in the filaments directed toward clusters the quenched galaxies are more massive near the boundaries of the clusters of galaxies than at their ourskirts.

摘要—基于SDSS目录数据，研究了在星系团R _sp的“后退”半径范围内及以后的具有淬灭恒星形成（QG）的星系的性质。我们使用了40个星系团和星系团的样本以及0处的野外星系的样本。02 <z < 0 。045.半径R _sp是根据观察到的星系数量的积分分布定义的，该积分分布是距星系系统中心距离的平方的函数。我们显示，在星系群集中，我们发现的QG的72％位于R _sp内。这些星系中约40％是fracDeV < 0的晚类型星系。8.猝灭恒星形成星系的大约80％的具有在日志的范围恒星群众 中号_* /中号_⊙ = [10; 11]。我们发现，较晚类型和较早类型的QG的最大角半径R _90，r和R _50，r接近星系组和星团的“反向飞溅”半径。我们的结果证实了这样一个假设：在指向星团的细丝中，淬灭星系在星团簇的边界附近比在我们的裙边处更大。