nIFTy galaxy cluster simulations – V. Investigation of the cluster infall region

Arthur, Jake and Pearce, Frazer R. and Gray, Meghan E. and Elahi, Pascal J. and Knebe, Alexander and Beck, Alexander M. and Cui, Weiguang and Cunnama, Daniel and Davé, Romeel and February, Sean and Huang, Shuiyao and Katz, Neal and Kay, Scott T. and McCarthy, Ian G. and Murante, Giuseppe and Perret, Valentin and Power, Chris and Puchwein, Ewald and Saro, Alexandro and Sembolini, Federico and Teyssier, Romain and Yepes, Gustavo (2017) nIFTy galaxy cluster simulations – V. Investigation of the cluster infall region. Monthly Notices of the Royal Astronomical Society, 464 (2). pp. 2027-2038. ISSN 1365-2966

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Abstract

We examine the properties of the galaxies and dark matter haloes residing in the cluster infall region surrounding the simulated _ cold dark matter galaxy cluster studied by Elahi et al. at z = 0. The 1.1 × 1015 h−1M_ galaxy cluster has been simulated with eight different hydrodynamical codes containing a variety of hydrodynamic solvers and sub-grid schemes. All models completed a dark-matter-only, non-radiative and full-physics run from the same initial conditions. The simulations contain dark matter and gas with mass resolution mDM = 9.01 × 108 h−1M_ and mgas = 1.9 × 108 h−1M_, respectively. We find that the synthetic cluster is surrounded by clear filamentary structures that contain ∼60 per cent of haloes in the infall region with mass ∼1012.5–1014 h−1M_, including 2–3 group-sized haloes (>1013 h−1M_). However, we find that only ∼10 per cent of objects in the infall region are sub-haloes residing in haloes, which may suggest that there is not much ongoing pre-processing occurring in the infall region at z = 0. By examining the baryonic content contained within the haloes, we also show that the code-to-code scatter in stellar fraction across all halo masses is typically ∼2 orders of magnitude between the two most extreme cases, and this is predominantly due to the differences in sub-grid schemes and calibration procedures that each model uses. Models that do not include active galactic nucleus feedback typically produce too high stellar fractions compared to observations by at least ∼1 order of magnitude.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Keywords: methods: numerical, galaxies: clusters: general, dark matter
Schools/Departments: University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy
Identification Number: 10.1093/mnras/stw2424
Depositing User: Eprints, Support
Date Deposited: 03 May 2017 13:06
Last Modified: 04 May 2017 14:33
URI: http://eprints.nottingham.ac.uk/id/eprint/42479

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