nIFTy galaxy cluster simulations - II. Radiative models

F. Sembolini, Pascal Elahi, F.R. Pearce, Chris Power, A. Knebe, S.T. Kay, Weiguang Cui, G. Yepes, A.M. Beck, S. Borgani, D. Cunnama, R. Davé, S. February, S. Huang, N. Katz, I.G. Mccarthy, G. Murante, R.D.A. Newton, V. Perret, E. Puchwein & 3 others A. Saro, J. Schaye, R. Teyssier

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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 massive galaxy cluster (M200crit = 1.1 × 1015 h-1 M⊙) in a Λ cold dark matter universe using 10 different codes (RAMSES, 2 incarnations of arepo and 7 of gadget), modelling hydrodynamics with full radiative subgrid physics. These codes include smoothed-particle hydrodynamics (SPH), spanning traditional and advanced SPH schemes, adaptive mesh and moving mesh codes. Our goal is to study the consistency between simulated clusters modelled with different radiative physical implementations - such as cooling, star formation and thermal active galactic nucleus (AGN) feedback. We compare images of the cluster at z = 0, global properties such as mass, and radial profiles of various dynamical and thermodynamical quantities. We find that, with respect to non-radiative simulations, dark matter is more centrally concentrated, the extent not simply depending on the presence/absence of AGN feedback. The scatter in global quantities is substantially higher than for non-radiative runs. Intriguingly, adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in Sembolini et al.: radiative physics + classic SPH can produce entropy cores, at least in the case of non cool-core clusters. Furthermore, the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content - for whether a code produces an unrealistic temperature inversion and a falling central entropy profile. However, AGN feedback does strongly affect the overall stellar distribution, limiting the effect of overcooling and reducing sensibly the stellar fraction.
Original languageEnglish
Pages (from-to)2973-2991
JournalMonthly Notices of the Royal Astronomical Society
Volume459
Issue number3
Early online date7 Apr 2016
DOIs
Publication statusPublished - Jul 2016

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active galactic nuclei
galaxies
hydrodynamics
entropy
physics
simulation
mesh
dark matter
profiles
temperature inversions
temperature inversion
falling
star formation
universe
code
inclusions
cooling
modeling
particle

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Sembolini, F. ; Elahi, Pascal ; Pearce, F.R. ; Power, Chris ; Knebe, A. ; Kay, S.T. ; Cui, Weiguang ; Yepes, G. ; Beck, A.M. ; Borgani, S. ; Cunnama, D. ; Davé, R. ; February, S. ; Huang, S. ; Katz, N. ; Mccarthy, I.G. ; Murante, G. ; Newton, R.D.A. ; Perret, V. ; Puchwein, E. ; Saro, A. ; Schaye, J. ; Teyssier, R. / nIFTy galaxy cluster simulations - II. Radiative models. In: Monthly Notices of the Royal Astronomical Society. 2016 ; Vol. 459, No. 3. pp. 2973-2991.
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abstract = "{\circledC} 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.We have simulated the formation of a massive galaxy cluster (M200crit = 1.1 × 1015 h-1 M⊙) in a Λ cold dark matter universe using 10 different codes (RAMSES, 2 incarnations of arepo and 7 of gadget), modelling hydrodynamics with full radiative subgrid physics. These codes include smoothed-particle hydrodynamics (SPH), spanning traditional and advanced SPH schemes, adaptive mesh and moving mesh codes. Our goal is to study the consistency between simulated clusters modelled with different radiative physical implementations - such as cooling, star formation and thermal active galactic nucleus (AGN) feedback. We compare images of the cluster at z = 0, global properties such as mass, and radial profiles of various dynamical and thermodynamical quantities. We find that, with respect to non-radiative simulations, dark matter is more centrally concentrated, the extent not simply depending on the presence/absence of AGN feedback. The scatter in global quantities is substantially higher than for non-radiative runs. Intriguingly, adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in Sembolini et al.: radiative physics + classic SPH can produce entropy cores, at least in the case of non cool-core clusters. Furthermore, the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content - for whether a code produces an unrealistic temperature inversion and a falling central entropy profile. However, AGN feedback does strongly affect the overall stellar distribution, limiting the effect of overcooling and reducing sensibly the stellar fraction.",
author = "F. Sembolini and Pascal Elahi and F.R. Pearce and Chris Power and A. Knebe and S.T. Kay and Weiguang Cui and G. Yepes and A.M. Beck and S. Borgani and D. Cunnama and R. Dav{\'e} and S. February and S. Huang and N. Katz and I.G. Mccarthy and G. Murante and R.D.A. Newton and V. Perret and E. Puchwein and A. Saro and J. Schaye and R. Teyssier",
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Sembolini, F, Elahi, P, Pearce, FR, Power, C, Knebe, A, Kay, ST, Cui, W, Yepes, G, Beck, AM, Borgani, S, Cunnama, D, Davé, R, February, S, Huang, S, Katz, N, Mccarthy, IG, Murante, G, Newton, RDA, Perret, V, Puchwein, E, Saro, A, Schaye, J & Teyssier, R 2016, 'nIFTy galaxy cluster simulations - II. Radiative models' Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3, pp. 2973-2991. https://doi.org/10.1093/mnras/stw800

nIFTy galaxy cluster simulations - II. Radiative models. / Sembolini, F.; Elahi, Pascal; Pearce, F.R.; Power, Chris; Knebe, A.; Kay, S.T.; Cui, Weiguang; Yepes, G.; Beck, A.M.; Borgani, S.; Cunnama, D.; Davé, R.; February, S.; Huang, S.; Katz, N.; Mccarthy, I.G.; Murante, G.; Newton, R.D.A.; Perret, V.; Puchwein, E.; Saro, A.; Schaye, J.; Teyssier, R.

In: Monthly Notices of the Royal Astronomical Society, Vol. 459, No. 3, 07.2016, p. 2973-2991.

Research output: Contribution to journalArticle

TY - JOUR

T1 - nIFTy galaxy cluster simulations - II. Radiative models

AU - Sembolini, F.

AU - Elahi, Pascal

AU - Pearce, F.R.

AU - Power, Chris

AU - Knebe, A.

AU - Kay, S.T.

AU - Cui, Weiguang

AU - Yepes, G.

AU - Beck, A.M.

AU - Borgani, S.

AU - Cunnama, D.

AU - Davé, R.

AU - February, S.

AU - Huang, S.

AU - Katz, N.

AU - Mccarthy, I.G.

AU - Murante, G.

AU - Newton, R.D.A.

AU - Perret, V.

AU - Puchwein, E.

AU - Saro, A.

AU - Schaye, J.

AU - Teyssier, R.

PY - 2016/7

Y1 - 2016/7

N2 - © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.We have simulated the formation of a massive galaxy cluster (M200crit = 1.1 × 1015 h-1 M⊙) in a Λ cold dark matter universe using 10 different codes (RAMSES, 2 incarnations of arepo and 7 of gadget), modelling hydrodynamics with full radiative subgrid physics. These codes include smoothed-particle hydrodynamics (SPH), spanning traditional and advanced SPH schemes, adaptive mesh and moving mesh codes. Our goal is to study the consistency between simulated clusters modelled with different radiative physical implementations - such as cooling, star formation and thermal active galactic nucleus (AGN) feedback. We compare images of the cluster at z = 0, global properties such as mass, and radial profiles of various dynamical and thermodynamical quantities. We find that, with respect to non-radiative simulations, dark matter is more centrally concentrated, the extent not simply depending on the presence/absence of AGN feedback. The scatter in global quantities is substantially higher than for non-radiative runs. Intriguingly, adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in Sembolini et al.: radiative physics + classic SPH can produce entropy cores, at least in the case of non cool-core clusters. Furthermore, the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content - for whether a code produces an unrealistic temperature inversion and a falling central entropy profile. However, AGN feedback does strongly affect the overall stellar distribution, limiting the effect of overcooling and reducing sensibly the stellar fraction.

AB - © 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society.We have simulated the formation of a massive galaxy cluster (M200crit = 1.1 × 1015 h-1 M⊙) in a Λ cold dark matter universe using 10 different codes (RAMSES, 2 incarnations of arepo and 7 of gadget), modelling hydrodynamics with full radiative subgrid physics. These codes include smoothed-particle hydrodynamics (SPH), spanning traditional and advanced SPH schemes, adaptive mesh and moving mesh codes. Our goal is to study the consistency between simulated clusters modelled with different radiative physical implementations - such as cooling, star formation and thermal active galactic nucleus (AGN) feedback. We compare images of the cluster at z = 0, global properties such as mass, and radial profiles of various dynamical and thermodynamical quantities. We find that, with respect to non-radiative simulations, dark matter is more centrally concentrated, the extent not simply depending on the presence/absence of AGN feedback. The scatter in global quantities is substantially higher than for non-radiative runs. Intriguingly, adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in Sembolini et al.: radiative physics + classic SPH can produce entropy cores, at least in the case of non cool-core clusters. Furthermore, the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content - for whether a code produces an unrealistic temperature inversion and a falling central entropy profile. However, AGN feedback does strongly affect the overall stellar distribution, limiting the effect of overcooling and reducing sensibly the stellar fraction.

U2 - 10.1093/mnras/stw800

DO - 10.1093/mnras/stw800

M3 - Article

VL - 459

SP - 2973

EP - 2991

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -