nIFTy galaxy cluster simulations - I. Dark matter and non-radiative models

F. Sembolini, G. Yepes, F.R. Pearce, A. Knebe, S.T. Kay, Chris Power, Weiguang Cui, A.M. Beck, S. Borgani, C.D. Vecchia, R. Davé, Pascal Elahi, S. February, S. Huang, A. Hobbs, N. Katz, E. Lau, I.G. Mccarthy, G. Murante, D. Nagai & 9 others K. Nelson, Richard Newton, V. Perret, E. Puchwein, J.I. Read, A. Saro, J. Schaye, R. Teyssier, R.J. Thacker

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Abstract

© 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. We have simulated the formation of a galaxy cluster in a Λ cold dark matter universe using 13 different codes modelling only gravity and non-radiative hydrodynamics (RAMSES, ART, AREPO, HYDRA and nine incarnations of GADGET). This range of codes includes particle-based, moving and fixed mesh codes as well as both Eulerian and Lagrangian fluid schemes. The various GADGET implementations span classic and modern smoothed particle hydrodynamics (SPH) schemes. The goal of this comparison is to assess the reliability of cosmological hydrodynamical simulations of clusters in the simplest astrophysically relevant case, that in which the gas is assumed to be non-radiative. We compare images of the cluster at z = 0, global properties such as mass and radial profiles of various dynamical and thermodynamical quantities. The underlying gravitational framework can be aligned very accurately for all the codes allowing a detailed investigation of the differences that develop due to the various gas physics implementations employed. As expected, the mesh-based codes RAMSES, ART and AREPO form extended entropy cores in the gas with rising central gas temperatures. Those codes employing classic SPH schemes show falling entropy profiles all the way into the very centre with correspondingly rising density profiles and central temperature inversions. We show that methods with modern SPH schemes that allow entropy mixing span the range between these two extremes and the latest SPH variants produce gas entropy profiles that are essentially indistinguishable from those obtained with grid-based methods.
Original languageEnglish
Pages (from-to)4063-4080
JournalMonthly Notices of the Royal Astronomical Society
Volume457
Issue number4
Early online date10 Feb 2016
DOIs
Publication statusPublished - 1 Apr 2016

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dark matter
galaxies
hydrodynamics
entropy
simulation
gas
profiles
gases
mesh
temperature inversions
temperature inversion
gas temperature
falling
code
physics
universe
grids
particle
gravity
gravitation

Cite this

Sembolini, F., Yepes, G., Pearce, F. R., Knebe, A., Kay, S. T., Power, C., ... Thacker, R. J. (2016). nIFTy galaxy cluster simulations - I. Dark matter and non-radiative models. Monthly Notices of the Royal Astronomical Society, 457(4), 4063-4080. https://doi.org/10.1093/mnras/stw250
Sembolini, F. ; Yepes, G. ; Pearce, F.R. ; Knebe, A. ; Kay, S.T. ; Power, Chris ; Cui, Weiguang ; Beck, A.M. ; Borgani, S. ; Vecchia, C.D. ; Davé, R. ; Elahi, Pascal ; February, S. ; Huang, S. ; Hobbs, A. ; Katz, N. ; Lau, E. ; Mccarthy, I.G. ; Murante, G. ; Nagai, D. ; Nelson, K. ; Newton, Richard ; Perret, V. ; Puchwein, E. ; Read, J.I. ; Saro, A. ; Schaye, J. ; Teyssier, R. ; Thacker, R.J. / nIFTy galaxy cluster simulations - I. Dark matter and non-radiative models. In: Monthly Notices of the Royal Astronomical Society. 2016 ; Vol. 457, No. 4. pp. 4063-4080.
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Sembolini, F, Yepes, G, Pearce, FR, Knebe, A, Kay, ST, Power, C, Cui, W, Beck, AM, Borgani, S, Vecchia, CD, Davé, R, Elahi, P, February, S, Huang, S, Hobbs, A, Katz, N, Lau, E, Mccarthy, IG, Murante, G, Nagai, D, Nelson, K, Newton, R, Perret, V, Puchwein, E, Read, JI, Saro, A, Schaye, J, Teyssier, R & Thacker, RJ 2016, 'nIFTy galaxy cluster simulations - I. Dark matter and non-radiative models' Monthly Notices of the Royal Astronomical Society, vol. 457, no. 4, pp. 4063-4080. https://doi.org/10.1093/mnras/stw250

nIFTy galaxy cluster simulations - I. Dark matter and non-radiative models. / Sembolini, F.; Yepes, G.; Pearce, F.R.; Knebe, A.; Kay, S.T.; Power, Chris; Cui, Weiguang; Beck, A.M.; Borgani, S.; Vecchia, C.D.; Davé, R.; Elahi, Pascal; February, S.; Huang, S.; Hobbs, A.; Katz, N.; Lau, E.; Mccarthy, I.G.; Murante, G.; Nagai, D.; Nelson, K.; Newton, Richard; Perret, V.; Puchwein, E.; Read, J.I.; Saro, A.; Schaye, J.; Teyssier, R.; Thacker, R.J.

In: Monthly Notices of the Royal Astronomical Society, Vol. 457, No. 4, 01.04.2016, p. 4063-4080.

Research output: Contribution to journalArticle

TY - JOUR

T1 - nIFTy galaxy cluster simulations - I. Dark matter and non-radiative models

AU - Sembolini, F.

AU - Yepes, G.

AU - Pearce, F.R.

AU - Knebe, A.

AU - Kay, S.T.

AU - Power, Chris

AU - Cui, Weiguang

AU - Beck, A.M.

AU - Borgani, S.

AU - Vecchia, C.D.

AU - Davé, R.

AU - Elahi, Pascal

AU - February, S.

AU - Huang, S.

AU - Hobbs, A.

AU - Katz, N.

AU - Lau, E.

AU - Mccarthy, I.G.

AU - Murante, G.

AU - Nagai, D.

AU - Nelson, K.

AU - Newton, Richard

AU - Perret, V.

AU - Puchwein, E.

AU - Read, J.I.

AU - Saro, A.

AU - Schaye, J.

AU - Teyssier, R.

AU - Thacker, R.J.

PY - 2016/4/1

Y1 - 2016/4/1

N2 - © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. We have simulated the formation of a galaxy cluster in a Λ cold dark matter universe using 13 different codes modelling only gravity and non-radiative hydrodynamics (RAMSES, ART, AREPO, HYDRA and nine incarnations of GADGET). This range of codes includes particle-based, moving and fixed mesh codes as well as both Eulerian and Lagrangian fluid schemes. The various GADGET implementations span classic and modern smoothed particle hydrodynamics (SPH) schemes. The goal of this comparison is to assess the reliability of cosmological hydrodynamical simulations of clusters in the simplest astrophysically relevant case, that in which the gas is assumed to be non-radiative. We compare images of the cluster at z = 0, global properties such as mass and radial profiles of various dynamical and thermodynamical quantities. The underlying gravitational framework can be aligned very accurately for all the codes allowing a detailed investigation of the differences that develop due to the various gas physics implementations employed. As expected, the mesh-based codes RAMSES, ART and AREPO form extended entropy cores in the gas with rising central gas temperatures. Those codes employing classic SPH schemes show falling entropy profiles all the way into the very centre with correspondingly rising density profiles and central temperature inversions. We show that methods with modern SPH schemes that allow entropy mixing span the range between these two extremes and the latest SPH variants produce gas entropy profiles that are essentially indistinguishable from those obtained with grid-based methods.

AB - © 2016 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. We have simulated the formation of a galaxy cluster in a Λ cold dark matter universe using 13 different codes modelling only gravity and non-radiative hydrodynamics (RAMSES, ART, AREPO, HYDRA and nine incarnations of GADGET). This range of codes includes particle-based, moving and fixed mesh codes as well as both Eulerian and Lagrangian fluid schemes. The various GADGET implementations span classic and modern smoothed particle hydrodynamics (SPH) schemes. The goal of this comparison is to assess the reliability of cosmological hydrodynamical simulations of clusters in the simplest astrophysically relevant case, that in which the gas is assumed to be non-radiative. We compare images of the cluster at z = 0, global properties such as mass and radial profiles of various dynamical and thermodynamical quantities. The underlying gravitational framework can be aligned very accurately for all the codes allowing a detailed investigation of the differences that develop due to the various gas physics implementations employed. As expected, the mesh-based codes RAMSES, ART and AREPO form extended entropy cores in the gas with rising central gas temperatures. Those codes employing classic SPH schemes show falling entropy profiles all the way into the very centre with correspondingly rising density profiles and central temperature inversions. We show that methods with modern SPH schemes that allow entropy mixing span the range between these two extremes and the latest SPH variants produce gas entropy profiles that are essentially indistinguishable from those obtained with grid-based methods.

U2 - 10.1093/mnras/stw250

DO - 10.1093/mnras/stw250

M3 - Article

VL - 457

SP - 4063

EP - 4080

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 4

ER -