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dc.contributor.author Sembolini, F
dc.contributor.author Elahi, PJ
dc.contributor.author Pearce, FR
dc.contributor.author Power, C
dc.contributor.author Knebe, A
dc.contributor.author February, Sean
dc.date.accessioned 2017-05-17T07:21:04Z
dc.date.available 2017-05-17T07:21:04Z
dc.date.issued 2016-04
dc.identifier.citation Sembolini, F., Elahi, P.J., Pearce, F.R. et al. 2016. nIFTy galaxy cluster simulations II: radiative models. Monthly Notices of the Royal Astronomical Society, 459(3): 2973-2991. DOI: https://doi.org/10.1093/mnras/stw800 en_US
dc.identifier.issn 0035-8711
dc.identifier.uri https://academic.oup.com/mnras/article-abstract/459/3/2973/2595204/nIFTy-galaxy-cluster-simulations-II-Radiative?redirectedFrom=fulltext
dc.identifier.uri DOI: https://doi.org/10.1093/mnras/stw800
dc.identifier.uri http://hdl.handle.net/10204/9092
dc.description © 2016 The Authors en_US
dc.description.abstract We have simulated the formation of a massive galaxy cluster (M(supcrit)(sub200) = 1.1×10(sup15)h(sup-1)M) in a CDM universe using 10 different codes (RAMSES, 2 incarnations of AREPO and 7 of GADGET), modeling 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 modeled with different radiative physical implementations - such as cooling, star formation and 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. (2015): radiative physics + classic SPH can produce entropy cores. 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. en_US
dc.language.iso en en_US
dc.publisher Oxford University Press on behalf of the Royal Astronomical Society en_US
dc.relation.ispartofseries Worklist;16643
dc.subject Galaxies: clusters: general en_US
dc.subject Galaxies: haloes en_US
dc.subject Galaxies: evolution en_US
dc.subject Cosmology: theory en_US
dc.subject Galaxies: formation en_US
dc.title nIFTy galaxy cluster simulations II: radiative models en_US
dc.type Article en_US


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