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nIFTy galaxy cluster simulations – IV. Quantifying the influence of baryons on halo properties

Cui, Weiguang; Power, Chris; Knebe, Alexander; Kay, Scott T.; Sembolini, Federico; Elahi, Pascal J.; Yepes, Gustavo; Pearce, Frazer; Cunnama, Daniel; Beck, Alexander M.; Vecchia, Claudio Dalla; Davé, Romeel; February, Sean; Huang, Shuiyao; Hobbs, Alex; Katz, Neal; McCarthy, Ian G.; Murante, Giuseppe; Perret, Valentin; Puchwein, Ewald; Read, Justin I.; Saro, Alexandro; Teyssier, Romain; Thacker, Robert J.

Authors

Weiguang Cui

Chris Power

Alexander Knebe

Scott T. Kay

Federico Sembolini

Pascal J. Elahi

Gustavo Yepes

Daniel Cunnama

Alexander M. Beck

Claudio Dalla Vecchia

Romeel Davé

Sean February

Shuiyao Huang

Alex Hobbs

Neal Katz

Ian G. McCarthy

Giuseppe Murante

Valentin Perret

Ewald Puchwein

Justin I. Read

Alexandro Saro

Romain Teyssier

Robert J. Thacker



Abstract

Building on the initial results of the nIFTy simulated galaxy cluster comparison, we compare and contrast the impact of baryonic physics with a single massive galaxy cluster, run with 11 state-of-the-art codes, spanning adaptive mesh, moving mesh, classic and modern smoothed particle hydrodynamics (SPH) approaches. For each code represented we have a dark-matter-only (DM) and non-radiative (NR) version of the cluster, as well as a full physics (FP) version for a subset of the codes. We compare both radial mass and kinematic profiles, as well as global measures of the cluster (e.g. concentration, spin, shape), in the NR and FP runs with that in the DM runs. Our analysis reveals good consistency ⪅20 per cent) between global properties of the cluster predicted by different codes when integrated quantities are measured within the virial radius R200. However, we see larger differences for quantities within R2500, especially in the FP runs. The radial profiles reveal a diversity, especially in the cluster centre, between the NR runs, which can be understood straightforwardly from the division of codes into classic SPH and non-classic SPH (including the modern SPH, adaptive and moving mesh codes); and between the FP runs, which can also be understood broadly from the division of codes into those that include active galactic nucleus feedback and those that do not. The variation with respect to the median is much larger in the FP runs with different baryonic physics prescriptions than in the NR runs with different hydrodynamics solvers.

Journal Article Type Article
Publication Date Mar 15, 2016
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Electronic ISSN 1365-2966
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 458
Issue 4
APA6 Citation Cui, W., Power, C., Knebe, A., Kay, S. T., Sembolini, F., Elahi, P. J., …Thacker, R. J. (2016). nIFTy galaxy cluster simulations – IV. Quantifying the influence of baryons on halo properties. Monthly Notices of the Royal Astronomical Society, 458(4), https://doi.org/10.1093/mnras/stw603
DOI https://doi.org/10.1093/mnras/stw603
Keywords methods: numerical, galaxies: clusters: general, galaxies: evolution, galaxies: formation, galaxies: haloes, cosmology: theory
Publisher URL https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw603
Copyright Statement Copyright information regarding this work can be found at the following address: http://eprints.nottingh.../end_user_agreement.pdf

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Copyright Statement
Copyright information regarding this work can be found at the following address: http://eprints.nottingham.ac.uk/end_user_agreement.pdf





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