We study the outskirts ($R<3R_{ 200c}$) of 40 groups and clusters of galaxies of the local Universe ($0.02<z<0.045$) with 300~km~s$^{ -1}<\sigma<950$~km~s$^{ -1}$. Using the SDSS DR10 catalog data, we measured the stellar mass of galaxy clusters in accordance with the previously determined $K_s$-luminosity (2MASX data) and found their correlation in the form $M_*/M_{ \odot} \propto (L_K/L_{ \odot})^{ 1.010\pm0.004}$ ($M_K<-21\,.\!\!^{ \rm m}5$, $R<R_{ 200c}$). We also found the dependence of the galaxy cluster stellar mass on halo mass: $M_*/M_{ \odot} \propto (M_{ 200c}/M_{ \odot})^{ 0.77\pm0.01}$}. Our results show that the fraction of galaxies with quenched star formation ($M_K<-21\,.\!\!^{ \rm m}5$) is maximal in the central regions of the galaxy clusters and equals, on the average, $0.81\pm0.02$; it decreases to $0.44\pm0.02$ outside of the projected radius $R_{ sp}$ ($2<R/R_{ 200c}<3$), which we found from the observed profile, but still remains higher than that in the field by 27\%. The fraction of early-type "red sequence" galaxies decreases from $0.54\pm0.02$ in the center to $0.24\pm0.01$ beyond $R_{ \rm sp}$, reaching its field value.
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