nIFTy galaxy cluster simulations V: Investigation of the Cluster Infall Region

Abstract

We examine the properties of the galaxies and dark matter haloes residing in the cluster infall region surrounding the simulated $\Lambda$CDM galaxy cluster studied by Elahi et al. (2016) at z=0. The $1.1\times 10^{15}{h}^{-1}{\text{M}}_{\odot }$ galaxy cluster has been simulated with eight different hydrodynamical codes containing a variety of hydrodynamic solvers and subgrid 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 $m_{\text{DM}}=9.01\times 10^8{h}^{-1}{\text{M}}_{\odot }$ and $m_{\text{gas}}=1.9\times 10^8{h}^{-1}{\text{M}}_{\odot }$ respectively. We find that the synthetic cluster is surrounded by clear filamentary structures that contain ~60% of haloes in the infall region with mass ~$10^{12.5}-10^{14}{h}^{-1}{\text{M}}_{\odot }$, including 2-3 group-sized haloes ($>10^{13}{h}^{-1}{\text{M}}_{\odot }$). However, we find that only ~10% of objects in the infall region are subhaloes residing in haloes, which may suggest that there is not much ongoing preprocessing 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 subgrid schemes and calibration procedures that each model uses. Models that do not include AGN feedback typically produce too high stellar fractions compared to observations by at least ~1 order of magnitude.

arXiv comment14 pages, 9 figures, 1 table; accepted for publication in MNRAS

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