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

Sembolini, Federico and Yepes, Gustavo and Pearce, Frazer R. and Knebe, Alexander and Kay, Scott T. and Power, Chris and Cui, Weiguang and Beck, Alexander M. and Borgani, Stefano and Dalla Vecchia, Claudio and Davé, Romeel and Elahi, Pascal Jahan and February, Sean and Huang, Shuiyao and Hobbs, Alex and Katz, Neal and Lau, Erwin and McCarthy, Ian G. and Murante, Giuseppe and Nagai, Daisuke and Nelson, Kaylea and Newton, Richard D. A. and Perret, Valentin and Puchwein, Ewald and Read, Justin I. and Saro, Alexandro and Schaye, Joop and Teyssier, Romain and Thacker, Robert J. (2016) nIFTy galaxy cluster simulations – I. Dark matter and non-radiative models. Monthly Notices of the Royal Astronomical Society, 457 (4). pp. 4063-4080. ISSN 1365-2966

[img]
Preview
PDF - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (11MB) | Preview

Abstract

We have simulated the formation of a galaxy cluster in a Ʌ 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.

Item Type: Article
Additional Information: This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Keywords: Methods: numerical - galaxies: haloes - cosmology: theory - dark matter
Schools/Departments: University of Nottingham UK Campus > Faculty of Science > School of Physics and Astronomy
Identification Number: https://doi.org/10.1093/mnras/stw250
Depositing User: Eprints, Support
Date Deposited: 08 Sep 2016 07:58
Last Modified: 20 Sep 2016 18:36
URI: http://eprints.nottingham.ac.uk/id/eprint/36360

Actions (Archive Staff Only)

Edit View Edit View