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 10 ^ { 14 } < M _ { 200 } / \mathrm { M } _ { \astrosun } < 10 ^ { 15.4 } 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 \times 10 ^ { 6 } \mathrm { M } _ { \astrosun } and physical softening length of 0.7 \mathrm { 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 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 ICM are a good match to the observations .