Quenched galaxies in clusters of galaxies and their outskirts
  Based on the SDSS data, the properties of galaxies with quenched star
formation (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 galaxy
clusters and a sample of field galaxies at $0.02<z<0.045$. The radii $R_{\rm
sp}$ were defined from the observed integrated 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 $R_{\rm sp}$. About 40% of these galaxies are late-type ones with
${frac}DeV < 0.8$. Approximately 80% of galaxies with quenched star formation
have stellar masses in the range of $\log M_*/M_{\odot} = [10; 11]$. 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 clusters of galaxies than at the outskirts.
