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Arthur, Jake; Pearce, Frazer R.; Gray, Meghan E.; Elahi, Pascal J.; Knebe, Alexander; Beck, Alexander M.; Cui, Weiguang; Cunnama, Daniel; Davé, Romeel; February, Sean; Huang, Shuiyao; Katz, Neal; Kay, Scott T.; McCarthy, Ian G.; Murante, Giuseppe; Perret, Valentin; Power, Chris; Puchwein, Ewald; Saro, Alexandro; Sembolini, Federico; Teyssier, Romain; Yepes, Gustavo (2017): nIFTy galaxy cluster simulations - V. Investigation of the cluster infall region. In: Monthly Notices of the Royal Astronomical Society, Vol. 464, No. 2: pp. 2027-2038
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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 Lambda cold dark matter galaxy cluster studied by Elahi et al. at z = 0. The 1.1 x 10(15) h(-1) M-circle dot 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 m(DM) = 9.01 x 10(8) h(-1) M-circle dot and m(gas) = 1.9 x 10(8) h(-1) M-circle dot, respectively. We find that the synthetic cluster is surrounded by clear filamentary structures that contain similar to 60 per cent of haloes in the infall region with mass similar to 10(12.5)-10(14) h(-1) M-circle dot, including 2-3 group-sized haloes (>10(13) h(-1) M-circle dot). However, we find that only similar to 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 similar to 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 similar to 1 order of magnitude.