Abstract
| Original language | English |
|---|---|
| Pages (from-to) | 2027-2038 |
| Journal | Monthly Notices of the Royal Astronomical Society |
| Volume | 464 |
| Issue number | 2 |
| DOIs | |
| Publication status | Published - 11 Jan 2017 |
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nIFTy galaxy cluster simulations - V. Investigation of the cluster infall region. / 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.
In: Monthly Notices of the Royal Astronomical Society, Vol. 464, No. 2, 11.01.2017, p. 2027-2038.Research output: Contribution to journal › Article
TY - JOUR
T1 - nIFTy galaxy cluster simulations - V. Investigation of the cluster infall region
AU - Arthur, Jake
AU - Pearce, Frazer R.
AU - Gray, Meghan E.
AU - Elahi, Pascal J.
AU - Knebe, Alexander
AU - Beck, Alexander M.
AU - Cui, Weiguang
AU - Cunnama, Daniel
AU - Davé, Romeel
AU - February, Sean
AU - Huang, Shuiyao
AU - Katz, Neal
AU - Kay, Scott T.
AU - McCarthy, Ian G.
AU - Murante, Giuseppe
AU - Perret, Valentin
AU - Power, Chris
AU - Puchwein, Ewald
AU - Saro, Alexandro
AU - Sembolini, Federico
AU - Teyssier, Romain
AU - Yepes, Gustavo
PY - 2017/1/11
Y1 - 2017/1/11
N2 - 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.
AB - 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.
KW - methods: numerical
KW - galaxies: clusters: general
KW - dark matter
U2 - 10.1093/mnras/stw2424
DO - 10.1093/mnras/stw2424
M3 - Article
VL - 464
SP - 2027
EP - 2038
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -