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Internal dark matter structure of the most massive galaxy clusters


Le Brun, A M C; Arnaud, M; Pratt, G W; Teyssier, R (2018). Internal dark matter structure of the most massive galaxy clusters. Monthly Notices of the Royal Astronomical Society. Letters, 473(1):L69-L73.

Abstract

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 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.

Abstract

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 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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Additional indexing

Item Type:Journal Article, refereed, further contribution
Communities & Collections:07 Faculty of Science > Institute for Computational Science
Dewey Decimal Classification:530 Physics
Language:English
Date:1 January 2018
Deposited On:25 Oct 2018 09:47
Last Modified:17 Sep 2019 19:39
Publisher:Oxford University Press
ISSN:1745-3933
OA Status:Green
Publisher DOI:https://doi.org/10.1093/mnrasl/slx150
Project Information:
  • : FunderFP7
  • : Grant ID340519
  • : Project TitleM2C - FOLLOWING THE MOST MASSIVE GALAXY CLUSTERS ACROSS COSMIC TIME

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