English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We investigate the evolution of the dark matter density profiles of the mostmassive galaxy clusters in the Universe. Using a `zoom-in' procedure on a largesuite of cosmological simulations of total comoving volume of $3\,(h^{-1}\,\rmGpc)^3$, we study the 25 most massive clusters in four redshift slices from$z\sim 1$ to the present. The minimum mass is $M_{500} > 5.5 \times 10^{14}$M$_{\odot}$ at $z=1$. Each system has more than two million particles within$r_{500}$. Once scaled to the critical density at each redshift, the darkmatter profiles within $r_{500}$ are strikingly similar from $z\sim1$ to thepresent day, exhibiting a low dispersion of 0.15 dex, and showing littleevolution with redshift in the radial logarithmic slope and scatter. They havethe running power law shape typical of the NFW-type profiles, and their innerstructure, resolved to $3.8\,h^{-1}$ comoving kpc at $z=1$, shows no signs ofconverging to an asymptotic slope. Our results suggest that this type ofprofile is already in place at $z>1$ in the highest-mass haloes in theUniverse, and that it remains exceptionally robust to merging activity.

Internal dark matter structure of the most massive galaxy clusters since redshift 1