Abstract
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.
Original language | English |
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Pages (from-to) | 2027-2038 |
Journal | Monthly Notices of the Royal Astronomical Society |
Volume | 464 |
Issue number | 2 |
DOIs | |
Publication status | Published - 23 Sept 2016 |
Keywords / Materials (for Non-textual outputs)
- methods: numerical
- galaxies: clusters: general
- dark matter