Internal dark matter structure of the most massive galaxy clusters

We investigate the evolution of the dark matter density profiles of the most massive galaxy clusters in the Universe. Using a 'zoom-in' procedure on a large suite of cosmological simulations of total comoving volume of 3 (h(-1) Gpc) 3, we study the 25 most massive clusters in four redshift slices from z similar to 1 to the present. The minimum mass is M-500 > 5.5 x 10(14) M-circle dot at z = 1. Each system has more than two million particles within r(500). Once scaled to the critical density at each redshift, the dark matter profiles within r(500) are strikingly similar from z similar to 1 to the present day, exhibiting a low dispersion of 0.15 dex, and showing little evolution with redshift in the radial logarithmic slope and scatter. They have the running power-law shape typical of the Navarro-Frenk-White type profiles, and their inner structure, resolved to 3.8 h(-1) comoving kpc at z = 1, shows no signs of converging to an asymptotic slope. Our results suggest that this type of profile is already in place at z > 1 in the highest-mass haloes in the Universe, and that it remains exceptionally robust to merging activity.