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

Jake Arthur, Frazer R. Pearce, Meghan E. Gray, Pascal J. Elahi, Alexander Knebe, Alexander M. Beck, Weiguang Cui, Daniel Cunnama, Romeel Davé, Sean February, Shuiyao Huang, Neal Katz, Scott T. Kay, Ian G. McCarthy, Giuseppe Murante, Valentin Perret, Chris Power, Ewald Puchwein, Alexandro Saro, Federico Sembolini & 2 others Romain Teyssier, Gustavo Yepes

Research output: Contribution to journalArticle

10 Citations (Scopus)
161 Downloads (Pure)

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 languageEnglish
Pages (from-to)2027-2038
JournalMonthly Notices of the Royal Astronomical Society
Volume464
Issue number2
DOIs
Publication statusPublished - 11 Jan 2017

Fingerprint

halos
galaxies
simulation
dark matter
physics
hydrodynamics
preprocessing
calibration
active galactic nuclei
grids
gas
gases
code

Cite this

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. / nIFTy galaxy cluster simulations - V. Investigation of the cluster infall region. In: Monthly Notices of the Royal Astronomical Society. 2017 ; Vol. 464, No. 2. pp. 2027-2038.
@article{5d0500bb2c6341d984af6e800fb1cf29,
title = "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 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.",
keywords = "methods: numerical, galaxies: clusters: general, dark matter",
author = "Jake Arthur and Pearce, {Frazer R.} and Gray, {Meghan E.} and Elahi, {Pascal J.} and Alexander Knebe and Beck, {Alexander M.} and Weiguang Cui and Daniel Cunnama and Romeel Dav{\'e} and Sean February and Shuiyao Huang and Neal Katz and Kay, {Scott T.} and McCarthy, {Ian G.} and Giuseppe Murante and Valentin Perret and Chris Power and Ewald Puchwein and Alexandro Saro and Federico Sembolini and Romain Teyssier and Gustavo Yepes",
year = "2017",
month = "1",
day = "11",
doi = "10.1093/mnras/stw2424",
language = "English",
volume = "464",
pages = "2027--2038",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "OXFORD UNIV PRESS UNITED KINGDOM",
number = "2",

}

Arthur, J, Pearce, FR, Gray, ME, Elahi, PJ, Knebe, A, Beck, AM, Cui, W, Cunnama, D, Davé, R, February, S, Huang, S, Katz, N, Kay, ST, McCarthy, IG, Murante, G, Perret, V, Power, C, Puchwein, E, Saro, A, Sembolini, F, Teyssier, R & Yepes, G 2017, 'nIFTy galaxy cluster simulations - V. Investigation of the cluster infall region' Monthly Notices of the Royal Astronomical Society, vol. 464, no. 2, pp. 2027-2038. https://doi.org/10.1093/mnras/stw2424

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 journalArticle

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 -