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We introduce the Hydrangea simulations, a suite of 24 cosmologicalhydrodynamic zoom-in simulations of massive galaxy clusters (M_200c =10^14-10^15 M_Sun) with baryon particle masses of ~10^6 M_Sun. Designed tostudy the impact of the cluster environment on galaxy formation, they are a keypart of the `Cluster-EAGLE' project (Barnes et al. 2017). They use a galaxyformation model developed for the EAGLE project, which has been shown to yieldboth realistic field galaxies and hot gas fractions of galaxy groups consistentwith observations. The total stellar mass content of the simulated clustersagrees with observations, but central cluster galaxies are too massive, by upto 0.6 dex. Passive satellite fractions are higher than in the field, and atstellar masses Mstar > 10^10 M_Sun this environmental effect is quantitativelyconsistent with observations. The predicted satellite stellar mass functionmatches data from local cluster surveys. Normalized to total mass, there arefewer low-mass (Mstar < 10^10 M_Sun) galaxies within the virial radius ofclusters than in the field, primarily due to star formation quenching.Conversely, the simulations predict an overabundance of massive galaxies inclusters compared to the field that persists to their far outskirts (>5r_200c). This is caused by a significantly increased stellar mass fraction of(sub-)haloes in the cluster environment, by up to ~0.3 dex even well beyondr_200c. Haloes near clusters are also more concentrated than equally massivefield haloes, but these two effects are largely uncorrelated.

The Hydrangea simulations: galaxy formation in and around massive clusters