dc.contributor.author |
Sembolini, F
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dc.contributor.author |
Yepes, CG
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|
dc.contributor.author |
Pearce, FR
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|
dc.contributor.author |
Knebe, A
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dc.contributor.author |
Kay, ST
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dc.contributor.author |
Power, C
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|
dc.contributor.author |
Cui, W
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dc.contributor.author |
Beck, AM
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dc.contributor.author |
Borgani, S
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dc.contributor.author |
Vecchia, CD
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|
dc.contributor.author |
Dave, R
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|
dc.contributor.author |
Elahi, PJ
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dc.contributor.author |
February, S
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|
dc.contributor.author |
Huang, S
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|
dc.contributor.author |
Hobbs, A
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dc.contributor.author |
Katz, N
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dc.contributor.author |
Lau, E
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dc.contributor.author |
McCarthy, IG
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dc.contributor.author |
Murante, G
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dc.contributor.author |
Nagai, D
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dc.contributor.author |
Nelson, K
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dc.contributor.author |
Newton, RDA
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dc.contributor.author |
Puchwein, E
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dc.contributor.author |
Read, JI
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dc.contributor.author |
Saro, A
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dc.contributor.author |
Schaye, J
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dc.contributor.author |
Thacker, RJ
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|
dc.date.accessioned |
2016-10-13T12:54:55Z |
|
dc.date.available |
2016-10-13T12:54:55Z |
|
dc.date.issued |
2016-02 |
|
dc.identifier.citation |
Sembolini, F., Yepes, G., Pearce, F.R., February, S., et al. 2016. nIFTy galaxy cluster simulations I: dark matter & non-radiative models. Monthly Notices of the Royal Astronomical Society, 457(4), pp 4063-4080 |
en_US |
dc.identifier.issn |
0035-8711 |
|
dc.identifier.uri |
http://mnras.oxfordjournals.org/content/457/4/4063
|
|
dc.identifier.uri |
http://hdl.handle.net/10204/8806
|
|
dc.description |
Copyright: 2016 Oxford University Press |
en_US |
dc.description.abstract |
We have simulated the formation of a galaxy cluster in a 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. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Oxford University Press |
en_US |
dc.relation.ispartofseries |
Workflow;16876 |
|
dc.subject |
Galaxies |
en_US |
dc.subject |
Haloes |
en_US |
dc.subject |
Cosmology |
en_US |
dc.subject |
Dark matter |
en_US |
dc.title |
nIFTy galaxy cluster simulations I: dark matter & non-radiative models |
en_US |
dc.type |
Article |
en_US |
dc.identifier.apacitation |
Sembolini, F., Yepes, C., Pearce, F., Knebe, A., Kay, S., Power, C., ... Thacker, R. (2016). nIFTy galaxy cluster simulations I: dark matter & non-radiative models. http://hdl.handle.net/10204/8806 |
en_ZA |
dc.identifier.chicagocitation |
Sembolini, F, CG Yepes, FR Pearce, A Knebe, ST Kay, C Power, W Cui, et al "nIFTy galaxy cluster simulations I: dark matter & non-radiative models." (2016) http://hdl.handle.net/10204/8806 |
en_ZA |
dc.identifier.vancouvercitation |
Sembolini F, Yepes C, Pearce F, Knebe A, Kay S, Power C, et al. nIFTy galaxy cluster simulations I: dark matter & non-radiative models. 2016; http://hdl.handle.net/10204/8806. |
en_ZA |
dc.identifier.ris |
TY - Article
AU - Sembolini, F
AU - Yepes, CG
AU - Pearce, FR
AU - Knebe, A
AU - Kay, ST
AU - Power, C
AU - Cui, W
AU - Beck, AM
AU - Borgani, S
AU - Vecchia, CD
AU - Dave, R
AU - Elahi, PJ
AU - February, S
AU - Huang, S
AU - Hobbs, A
AU - Katz, N
AU - Lau, E
AU - McCarthy, IG
AU - Murante, G
AU - Nagai, D
AU - Nelson, K
AU - Newton, RDA
AU - Puchwein, E
AU - Read, JI
AU - Saro, A
AU - Schaye, J
AU - Thacker, RJ
AB - We have simulated the formation of a galaxy cluster in a 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.
DA - 2016-02
DB - ResearchSpace
DP - CSIR
KW - Galaxies
KW - Haloes
KW - Cosmology
KW - Dark matter
LK - https://researchspace.csir.co.za
PY - 2016
SM - 0035-8711
T1 - nIFTy galaxy cluster simulations I: dark matter & non-radiative models
TI - nIFTy galaxy cluster simulations I: dark matter & non-radiative models
UR - http://hdl.handle.net/10204/8806
ER -
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en_ZA |