Galaxy clusters and their outskirts: the "red sequence", star formation rate, stellar mass

Abstract

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 $M_{\ast }/M_{\odot }\propto (L_K/L_{\odot }{)}^{1.010\pm 0.004}$ ($M_K<-21.{}^{\mathrm{m}}5$, $R<R_{200c}$). We also found the dependence of the galaxy cluster stellar mass on halo mass: $M_{\ast }/M_{\odot }\propto (M_{200c}/M_{\odot }{)}^{0.77\pm 0.01}$}. Our results show that the fraction of galaxies with quenched star formation ($M_K<-21.{}^{\mathrm{m}}5$) is maximal in the central regions of the galaxy clusters and equals, on the average, $0.81\pm 0.02$; it decreases to $0.44\pm 0.02$ 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 $0.54\pm 0.02$ in the center to $0.24\pm 0.01$ beyond $R_{\mathrm{sp}}$, reaching its field value.

arXiv comment16 pages, 7 figures, 3 tables

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