Quenched Galaxies in Clusters of Galaxies and their Outskirts
Based on the SDSS catalog data the properties of galaxies with quenched star formation (QGs) within the jjsplashback-radius of galaxy clusters Rg<sub>p</sub> 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 Rg<sub>p</sub> 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<sub>sp</sub>. 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 lg M*/M© = [10; 11]. We found that QGs of late types and of early types in a less degree have maximum angular radii Rg<sub>0</sub>,<sub>r</sub> and R<sub>50</sub>,<sub>r</sub> near the jjsplashback-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 to the boundaries than at the outskirts.