nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties

Weiguang Cui, Chris Power, A. Knebe, S.T. Kay, F. Sembolini, Pascal Elahi, G. Yepes, F. Pearce, D. Cunnama, A.M. Beck, C.D. Vecchia, R. Davé, S. February, S. Huang, A. Hobbs, N. Katz, I.G. Mccarthy, G. Murante, V. Perret, E. Puchwein & 4 others J.I. Read, A. Saro, R. Teyssier, R.J. Thacker

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Abstract

© 2016 The Authors. Building on the initial results of the nIFTy simulated galaxy cluster comparison, we compare and contrast the impact of baryonic physics with a single massive galaxy cluster, run with 11 state-of-the-art codes, spanning adaptive mesh, moving mesh, classic and modern smoothed particle hydrodynamics (SPH) approaches. For each code represented we have a dark-matter-only (DM) and non-radiative (NR) version of the cluster, as well as a full physics (FP) version for a subset of the codes. We compare both radial mass and kinematic profiles, as well as global measures of the cluster (e.g. concentration, spin, shape), in the NR and FP runs with that in the DM runs. Our analysis reveals good consistency ≲20 per cent) between global properties of the cluster predicted by different codes when integrated quantities are measured within the virial radius R200. However, we see larger differences for quantities within R2500, especially in the FP runs. The radial profiles reveal a diversity, especially in the cluster centre, between the NR runs, which can be understood straightforwardly from the division of codes into classic SPH and non-classic SPH (including the modern SPH, adaptive and moving mesh codes); and between the FP runs, which can also be understood broadly from the division of codes into those that include active galactic nucleus feedback and those that do not. The variation with respect to the median is much larger in the FP runs with different baryonic physics prescriptions than in the NR runs with different hydrodynamics solvers.
Original languageEnglish
Pages (from-to)4052-4073
JournalMonthly Notices of the Royal Astronomical Society
Volume458
Issue number4
Early online dateApr 2016
DOIs
Publication statusPublished - 2016

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baryons
halos
physics
galaxies
hydrodynamics
simulation
mesh
division
dark matter
profiles
code
active galactic nuclei
set theory
kinematics
radii
particle

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Cui, Weiguang ; Power, Chris ; Knebe, A. ; Kay, S.T. ; Sembolini, F. ; Elahi, Pascal ; Yepes, G. ; Pearce, F. ; Cunnama, D. ; Beck, A.M. ; Vecchia, C.D. ; Davé, R. ; February, S. ; Huang, S. ; Hobbs, A. ; Katz, N. ; Mccarthy, I.G. ; Murante, G. ; Perret, V. ; Puchwein, E. ; Read, J.I. ; Saro, A. ; Teyssier, R. ; Thacker, R.J. / nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties. In: Monthly Notices of the Royal Astronomical Society. 2016 ; Vol. 458, No. 4. pp. 4052-4073.
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abstract = "{\circledC} 2016 The Authors. Building on the initial results of the nIFTy simulated galaxy cluster comparison, we compare and contrast the impact of baryonic physics with a single massive galaxy cluster, run with 11 state-of-the-art codes, spanning adaptive mesh, moving mesh, classic and modern smoothed particle hydrodynamics (SPH) approaches. For each code represented we have a dark-matter-only (DM) and non-radiative (NR) version of the cluster, as well as a full physics (FP) version for a subset of the codes. We compare both radial mass and kinematic profiles, as well as global measures of the cluster (e.g. concentration, spin, shape), in the NR and FP runs with that in the DM runs. Our analysis reveals good consistency ≲20 per cent) between global properties of the cluster predicted by different codes when integrated quantities are measured within the virial radius R200. However, we see larger differences for quantities within R2500, especially in the FP runs. The radial profiles reveal a diversity, especially in the cluster centre, between the NR runs, which can be understood straightforwardly from the division of codes into classic SPH and non-classic SPH (including the modern SPH, adaptive and moving mesh codes); and between the FP runs, which can also be understood broadly from the division of codes into those that include active galactic nucleus feedback and those that do not. The variation with respect to the median is much larger in the FP runs with different baryonic physics prescriptions than in the NR runs with different hydrodynamics solvers.",
author = "Weiguang Cui and Chris Power and A. Knebe and S.T. Kay and F. Sembolini and Pascal Elahi and G. Yepes and F. Pearce and D. Cunnama and A.M. Beck and C.D. Vecchia and R. Dav{\'e} and S. February and S. Huang and A. Hobbs and N. Katz and I.G. Mccarthy and G. Murante and V. Perret and E. Puchwein and J.I. Read and A. Saro and R. Teyssier and R.J. Thacker",
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Cui, W, Power, C, Knebe, A, Kay, ST, Sembolini, F, Elahi, P, Yepes, G, Pearce, F, Cunnama, D, Beck, AM, Vecchia, CD, Davé, R, February, S, Huang, S, Hobbs, A, Katz, N, Mccarthy, IG, Murante, G, Perret, V, Puchwein, E, Read, JI, Saro, A, Teyssier, R & Thacker, RJ 2016, 'nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties' Monthly Notices of the Royal Astronomical Society, vol. 458, no. 4, pp. 4052-4073. https://doi.org/10.1093/mnras/stw603

nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties. / Cui, Weiguang; Power, Chris; Knebe, A.; Kay, S.T.; Sembolini, F.; Elahi, Pascal; Yepes, G.; Pearce, F.; Cunnama, D.; Beck, A.M.; Vecchia, C.D.; Davé, R.; February, S.; Huang, S.; Hobbs, A.; Katz, N.; Mccarthy, I.G.; Murante, G.; Perret, V.; Puchwein, E.; Read, J.I.; Saro, A.; Teyssier, R.; Thacker, R.J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 458, No. 4, 2016, p. 4052-4073.

Research output: Contribution to journalArticle

TY - JOUR

T1 - nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties

AU - Cui, Weiguang

AU - Power, Chris

AU - Knebe, A.

AU - Kay, S.T.

AU - Sembolini, F.

AU - Elahi, Pascal

AU - Yepes, G.

AU - Pearce, F.

AU - Cunnama, D.

AU - Beck, A.M.

AU - Vecchia, C.D.

AU - Davé, R.

AU - February, S.

AU - Huang, S.

AU - Hobbs, A.

AU - Katz, N.

AU - Mccarthy, I.G.

AU - Murante, G.

AU - Perret, V.

AU - Puchwein, E.

AU - Read, J.I.

AU - Saro, A.

AU - Teyssier, R.

AU - Thacker, R.J.

PY - 2016

Y1 - 2016

N2 - © 2016 The Authors. Building on the initial results of the nIFTy simulated galaxy cluster comparison, we compare and contrast the impact of baryonic physics with a single massive galaxy cluster, run with 11 state-of-the-art codes, spanning adaptive mesh, moving mesh, classic and modern smoothed particle hydrodynamics (SPH) approaches. For each code represented we have a dark-matter-only (DM) and non-radiative (NR) version of the cluster, as well as a full physics (FP) version for a subset of the codes. We compare both radial mass and kinematic profiles, as well as global measures of the cluster (e.g. concentration, spin, shape), in the NR and FP runs with that in the DM runs. Our analysis reveals good consistency ≲20 per cent) between global properties of the cluster predicted by different codes when integrated quantities are measured within the virial radius R200. However, we see larger differences for quantities within R2500, especially in the FP runs. The radial profiles reveal a diversity, especially in the cluster centre, between the NR runs, which can be understood straightforwardly from the division of codes into classic SPH and non-classic SPH (including the modern SPH, adaptive and moving mesh codes); and between the FP runs, which can also be understood broadly from the division of codes into those that include active galactic nucleus feedback and those that do not. The variation with respect to the median is much larger in the FP runs with different baryonic physics prescriptions than in the NR runs with different hydrodynamics solvers.

AB - © 2016 The Authors. Building on the initial results of the nIFTy simulated galaxy cluster comparison, we compare and contrast the impact of baryonic physics with a single massive galaxy cluster, run with 11 state-of-the-art codes, spanning adaptive mesh, moving mesh, classic and modern smoothed particle hydrodynamics (SPH) approaches. For each code represented we have a dark-matter-only (DM) and non-radiative (NR) version of the cluster, as well as a full physics (FP) version for a subset of the codes. We compare both radial mass and kinematic profiles, as well as global measures of the cluster (e.g. concentration, spin, shape), in the NR and FP runs with that in the DM runs. Our analysis reveals good consistency ≲20 per cent) between global properties of the cluster predicted by different codes when integrated quantities are measured within the virial radius R200. However, we see larger differences for quantities within R2500, especially in the FP runs. The radial profiles reveal a diversity, especially in the cluster centre, between the NR runs, which can be understood straightforwardly from the division of codes into classic SPH and non-classic SPH (including the modern SPH, adaptive and moving mesh codes); and between the FP runs, which can also be understood broadly from the division of codes into those that include active galactic nucleus feedback and those that do not. The variation with respect to the median is much larger in the FP runs with different baryonic physics prescriptions than in the NR runs with different hydrodynamics solvers.

U2 - 10.1093/mnras/stw603

DO - 10.1093/mnras/stw603

M3 - Article

VL - 458

SP - 4052

EP - 4073

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -