Galaxy Clusters and Their Outskirts: the "Red Sequence", Star Formation Rate, Stellar Mass

We study the nearest outskirts (R < 3R(200c)) of 40 groups and clusters of galaxies of the local Universe (0.02 < z < 0.045 and 300 km s(-1) < sigma < 950 km s(-1)). Using the SDSSDR10 catalog data, we determined the stellar mass of galaxy clusters corresponding to K-s-luminosity (which we determined earlier based on the 2MASX catalog data) (M-*/M-circle dot) proportional to (L-K/L-circle dot)(1.010 +/- 0.004) (M-K < -21.(m)5, R < R-200c). We also found the dependence of the galaxy cluster stellar mass on halo mass: (M-*/M-circle dot) proportional to (M-200c/M-circle dot)(0.77 +/- 0.01). Our results show that the fraction of galaxies with quenched star formation (M-K < -21.(m)5) is maximal in the central regions of the galaxy clusters and equals, on the average, 0.81 +/- 0.02; it decreases to 0.44 +/- 0.02 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 +/- 0.02 in the center to 0.24 +/- 0.01 beyond R-sp, reaching its field value.