The distribution of luminous radio galaxies in galaxy clusters has been observed to be concentrated in the inner region .
We consider the role of dynamical friction of massive galaxies ( M \sim 10 ^ { 12.5 } M _ { \odot } ) , assuming them to be hosts of luminous radio galaxies , and show that beginning with a Navarro-Frenk-White density profile of a cluster of mass M _ { cl } \sim 10 ^ { 15 } M _ { \odot } of concentration c \sim 5 and collapsing at z \sim 1 , the density profile of radio galaxies evolve to a profile of concentration c \sim 25 , as observed , in a time scale of t \sim 3 \hbox { - - } 5 Gyr .