Rhapsody-G simulations –II. Baryonic growth and metal enrichment in massive galaxy clusters
Abstract
We study the evolution of the stellar component and the metallicity of both the intracluster medium and of stars in massive (M_(vir) ≈ 6 × 10^(14) M_⊙ h^(−1)) simulated galaxy clusters from the Rhapsody-G suite in detail and compare them to observational results. The simulations were performed with the AMR code ramses and include the effect of active galactic nucleus (AGN) feedback at the subgrid level. AGN feedback is required to produce realistic galaxy and cluster properties and plays a role in mixing material in the central regions and regulating star formation in the central galaxy. In both our low- and high-resolution runs with fiducial stellar yields, we find that stellar and ICM metallicities are a factor of 2 lower than in observations. We find that cool core clusters exhibit steeper metallicity gradients than non-cool core clusters, in qualitative agreement with observations. We verify that the ICM metallicities measured in the simulation can be explained by a simple 'regulator' model in which the metallicity is set by a balance of stellar yield and gas accretion. It is plausible that a combination of higher resolution and higher metal yield in AMR simulation would allow the metallicity of simulated clusters to match observed values; however, this hypothesis needs to be tested with future simulations. Comparison to recent literature highlights that results concerning the metallicity of clusters and cluster galaxies might depend sensitively on the scheme chosen to solve the hydrodynamics.
Additional Information
© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 April 14. Received 2016 April 14; in original form 2015 October 2. We thank Peter Behroozi for making the rockstar-galaxies software available for us. We would also like to thank Robert Feldmann for the useful discussions on the 'regulator model'. DM acknowledges support from the Swiss National Science Foundation (SNSF) through the SNSF Early. Postdoc and Advanced. Postdoc Mobility Fellowships. OH acknowledges support from the SNSF through the Ambizione fellowship. HW acknowledges support by the U.S. Department of Energy under contract number DE-FG02-95ER40899. RHW received support from the U.S. 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.Attached Files
Published - MNRAS-2016-Martizzi-4408-27.pdf
Submitted - 1510.00718v2.pdf
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Additional details
- Eprint ID
- 70251
- Resolver ID
- CaltechAUTHORS:20160909-131218142
- Swiss National Science Foundation (SNSF)
- DE-FG02-95ER40899
- Department of Energy (DOE)
- DE-AC02-76SF00515
- Department of Energy (DOE)
- s416
- Swiss National Supercomputing Centre (CSCS)
- Created
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2016-09-09Created from EPrint's datestamp field
- Updated
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2021-11-11Created from EPrint's last_modified field