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Based on the SDSS data, the properties of galaxies with quenched starformation (QGs) within the "splashback"-radius of galaxy clusters $R_{\rm sp}$and beyond it have been studied. We used a sample of 40 groups and galaxyclusters and a sample of field galaxies at $0.02<z<0.045$. The radii $R_{\rmsp}$ were defined from the observed integrated distribution of the number ofgalaxies as a function of the squared distance from the center of the galaxysystems. We show that in galaxy clusters 72% of the QGs we have found arewithin $R_{\rm sp}$. About 40% of these galaxies are late-type ones with${frac}DeV < 0.8$. Approximately 80% of galaxies with quenched star formationhave stellar masses in the range of $\log M_*/M_{\odot} = [10; 11]$. We foundthat QGs of late types and of early types in a less degree have maximum angularradii $R_{90,r}$ and $R_{50,r}$ near the "splashback"-radius of groups andclusters of galaxies. Our results confirm the assumption that in the filamentsdirected toward clusters, the quenched galaxies are more massive near theboundaries of clusters of galaxies than at the outskirts.

Quenched galaxies in clusters of galaxies and their outskirts