Internal dark matter structure of the most massive galaxy clusters - Archive ouverte HAL
Article Dans Une Revue Monthly Notices of the Royal Astronomical Society Année : 2018

Internal dark matter structure of the most massive galaxy clusters

Résumé

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 M_500 > 5.5 × 10^14 M_⊙ 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 ∼ 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.
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hal-01669554 , version 1 (09-01-2025)

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Amandine Le Brun, Monique Arnaud, Gabriel W. Pratt, Romain Teyssier. Internal dark matter structure of the most massive galaxy clusters. Monthly Notices of the Royal Astronomical Society, 2018, 473 (1), pp.L69-L73. ⟨10.1093/mnrasl/slx150⟩. ⟨hal-01669554⟩
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