751. nIFTy galaxy cluster simulations II: radiative models
- Author
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A. M. Beck, Alexander Knebe, V. Perret, Scott T. Kay, Pascal J. Elahi, Richard Newton, Giuseppe Murante, Frazer R. Pearce, Neal Katz, Shuiyao Huang, Federico Sembolini, Daniel Cunnama, Stefano Borgani, Sean February, Weiguang Cui, Gustavo Yepes, Ewald Puchwein, Romeel Davé, Chris Power, Joop Schaye, Alexandro Saro, Romain Teyssier, Ian G. McCarthy, ITA, GBR, FRA, DEU, University of Zurich, Sembolini, Federico, Elahi, Pascal Jahan, Pearce, Frazer R., Power, Chri, Knebe, Alexander, Kay, Scott T., Cui, Weiguang, Yepes, Gustavo, Beck, Alexander M., Borgani, Stefano, Cunnama, Daniel, Davé, Romeel, February, Sean, Huang, Shuiyao, Katz, Neal, Mccarthy, Ian G., Murante, Giuseppe, Newton, Richard D. A., Perret, Valentin, Puchwein, Ewald, Saro, Alexandro, Schaye, Joop, and Teyssier, Romain
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,530 Physics ,Cosmology: theory ,Dark matter ,Galaxies: haloes ,Methods: numerical ,Astronomy and Astrophysics ,Space and Planetary Science ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,01 natural sciences ,haloe [Galaxies] ,1912 Space and Planetary Science ,theory [Cosmology] ,0103 physical sciences ,Cluster (physics) ,Radiative transfer ,Entropy (information theory) ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,QB ,Physics ,numerical [Methods] ,010308 nuclear & particles physics ,Star formation ,methods: numerical, galaxies: haloes, cosmology: theory,dark matter ,Limiting ,Astronomy and Astrophysic ,Astrophysics - Astrophysics of Galaxies ,Astrophysics of Galaxies (astro-ph.GA) ,10231 Institute for Computational Science ,3103 Astronomy and Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We have simulated the formation of a massive galaxy cluster (M$_{200}^{\rm crit}$ = 1.1$\times$10$^{15}h^{-1}M_{\odot}$) in a $\Lambda$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., Comment: 20 pages, 13 figures, submitted to MNRAS