We study the radial number density and stellar mass density distributions of satellite galaxies in a sample of 60 massive clusters at 0.04 < z < 0.26 selected from the Multi-Epoch Nearby Cluster Survey ( MENeaCS ) and the Canadian Cluster Comparison Project ( CCCP ) .
In addition to \sim 10 , 000 spectroscopically confirmed member galaxies , we use deep ugri -band imaging to estimate photometric redshifts and stellar masses , and then statistically subtract fore- and background sources using data from the COSMOS survey .
We measure the galaxy number density and stellar mass density distributions in logarithmically spaced bins over 2 orders of magnitude in radial distance from the BCGs .
For projected distances in the range 0.1 < R / R _ { 200 } < 2.0 , we find that the stellar mass distribution is well-described by an NFW profile with a concentration of c = 2.03 \pm 0.20 .
However , at smaller radii we measure a significant excess in the stellar mass in satellite galaxies of about 10 ^ { 11 } \mathrm { M _ { \odot } } per cluster , compared to these NFW profiles .
We do obtain good fits to generalised NFW profiles with free inner slopes and to Einasto profiles .
To examine how clusters assemble their stellar mass component over cosmic time , we compare this local sample to the GCLASS cluster sample at z \sim 1 , which represents the approximate progenitor sample of the low- z clusters .
This allows for a direct comparison , which suggests that the central parts ( R < 0.4 Mpc ) of the stellar mass distributions of satellites in local galaxy clusters are already in place at z \sim 1 , and contain sufficient excess material for further BCG growth .
Evolving towards z = 0 , clusters appear to assemble their stellar mass primarily onto the outskirts , making them grow in an inside-out fashion .