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Published August 2017 | Submitted + Published
Journal Article Open

Rhapsody-G simulations I: the cool cores, hot gas and stellar content of massive galaxy clusters

Abstract

We present the RHAPSODY-G suite of cosmological hydrodynamic zoom simulations of 10 massive galaxy clusters at the M_(vir) ∼ 10^(15) M⊙ scale. These simulations include cooling and subresolution models for star formation and stellar and supermassive black hole feedback. The sample is selected to capture the whole gamut of assembly histories that produce clusters of similar final mass. We present an overview of the successes and shortcomings of such simulations in reproducing both the stellar properties of galaxies as well as properties of the hot plasma in clusters. In our simulations, a long-lived cool-core/non-cool-core dichotomy arises naturally, and the emergence of non-cool cores is related to low angular momentum major mergers. Nevertheless, the cool-core clusters exhibit a low central entropy compared to observations, which cannot be alleviated by thermal active galactic nuclei feedback. For cluster scaling relations, we find that the simulations match well the M_(500)–Y_(500) scaling of Planck Sunyaev–Zeldovich clusters but deviate somewhat from the observed X-ray luminosity and temperature scaling relations in the sense of being slightly too bright and too cool at fixed mass, respectively. Stars are produced at an efficiency consistent with abundance-matching constraints and central galaxies have star formation rates consistent with recent observations. While our simulations thus match various key properties remarkably well, we conclude that the shortcomings strongly suggest an important role for non-thermal processes (through feedback or otherwise) or thermal conduction in shaping the intracluster medium.

Additional Information

© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 January 3. Received 2016 December 22; in original form 2015 September 15. Published: 25 January 2017. We thank Yohan Dubois, James Bartlett, Pawel Biernacki, Elena Rasia and Amandine Le Brun for discussions and comments. We are grateful to Peter Behroozi for kindly making his ROCKSTAR-GALAXIES code available to us for further modifications, and for providing data shown in Figs 9 and 10. Finally, we thank the anonymous referee for a careful reading of our draft as well as insightful and valuable suggestions. OH acknowledges support from the Swiss National Science Foundation (SNSF) through the Ambizione fellowship. H-YW acknowledges the support by the US Department of Energy under contract number DE-FG02-95ER40899. DM acknowledges support from the Swiss National Science Foundation. RHW received support from the US Department of Energy contract to SLAC no. DE-AC02-76SF0051. This work was supported by a grant from the Swiss National Supercomputing Centre (CSCS) under project ID s416.

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Created:
August 19, 2023
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October 17, 2023