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

Arthur, J and Pearce, FR and Gray, ME and Elahi, PJ and Knebe, A and Beck, AM and Cui, W and Cunnama, D and Dave, R and February, S and Huang, S and Katz, N and Kay, ST and McCarthy, IG and Murante, G and Perret, V and Power, C and Puchwein, E and Saro, A and Sembolini, F and Teyssier, R and Yepes, G (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 0035-8711

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We examine the properties of the galaxies and dark matter haloes residing in the cluster infall region surrounding the simulated Λ cold dark matter galaxy cluster studied by Elahi et al. at z = 0. The 1.1 × 1015 h−1 M⊙ 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−1 M⊙ and mgas = 1.9 × 108 h−1 M⊙, 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−1 M⊙, including 2–3 group-sized haloes (>1013 h−1 M⊙). 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 ©: 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
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Date Deposited: 13 Apr 2017 11:06
Last Modified: 06 Sep 2017 20:43
DOI or Identification number: 10.1093/mnras/stw2424
URI: http://researchonline.ljmu.ac.uk/id/eprint/6254

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