Bibcode
Barnes, D. J.; Kay, Scott T.; Bahé, Yannick M.; Dalla Vecchia, C.; McCarthy, Ian G.; Schaye, Joop; Bower, Richard G.; Jenkins, Adrian; Thomas, Peter A.; Schaller, Matthieu; Crain, Robert A.; Theuns, Tom; White, Simon D. M.
Bibliographical reference
Monthly Notices of the Royal Astronomical Society, Volume 471, Issue 1, p.1088-1106
Advertised on:
10
2017
Citations
204
Refereed citations
186
Description
We introduce the Cluster-EAGLE (c-eagle) simulation project, a set of
cosmological hydrodynamical zoom simulations of the formation of 30
galaxy clusters in the mass range of 1014 <
M200/M⊙ < 1015.4 that
incorporates the Hydrangea sample of Bahé et al. (2017). The
simulations adopt the state-of-the-art eagle galaxy formation model,
with a gas particle mass of 1.8 × 106 M⊙
and physical softening length of 0.7 kpc. In this paper, we introduce
the sample and present the low-redshift global properties of the
clusters. We calculate the X-ray properties in a manner consistent with
observational techniques, demonstrating the bias and scatter introduced
by using estimated masses. We find the total stellar content and black
hole masses of the clusters to be in good agreement with the observed
relations. However, the clusters are too gas rich, suggesting that the
active galactic nucleus (AGN) feedback model is not efficient enough at
expelling gas from the high-redshift progenitors of the clusters. The
X-ray properties, such as the spectroscopic temperature and the
soft-band luminosity, and the Sunyaev-Zel'dovich properties are in
reasonable agreement with the observed relations. However, the clusters
have too high central temperatures and larger-than-observed entropy
cores, which is likely driven by the AGN feedback after the cluster core
has formed. The total metal content and its distribution throughout the
intracluster medium are a good match to the observations.
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