https://doi.org/10.1051/epjconf/202225700026
Internal dark matter structure of the most massive galaxy clusters since redshift 1
1 PSL Fellow, LUTh, Observatoire de Paris, PSL Research University, CNRS, Université de Paris, 92195 Meudon, France
2 Laboratoire AIM, IRFU/Département d’Astrophysique – CEA/DRF – CNRS – Université de Paris, Bât. 709, CEA-Saclay 91191 Gif-sur-Yvette Cedex, France
3 Institute for Computational Science, University of Zürich, CH-8057 Zürich, Switzerland
* e-mail: amandine.le-brun@obspm.fr (AMCLB)
Published online: 17 January 2022
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 ~ 1 to the present. The minimum mass is M500 > 5:5 × 1014 M⊙ at z = 1. Each system has more than two million particles within r500. Once scaled to the critical density at each redshift, the dark matter profiles within r500 are strikingly similar from z ~ 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 NFW-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.
© The Authors, published by EDP Sciences, 2022
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
