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nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties

Cui, W and Power, C and Knebe, A and Kay, ST and Sembolini, F and Elahi, PJ and Yepes, G and Pearce, F and Cunnama, D and Beck, AM and Vecchia, CD and Dave, R and February, S and Huang, S and Hobbs, A and Katz, N and McCarthy, IG and Murante, G and Perret, V and Puchwein, E and Read, JI and Saro, A and Teyssier, R and Thacker, RJ (2016) nIFTy galaxy cluster simulations - IV. Quantifying the influence of baryons on halo properties. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 458 (4). pp. 4052-4073. ISSN 0035-8711

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Abstract

Building on the initial results of the nIFTy simulated galaxy cluster comparison, we compare
and contrast the impact of baryonic physics with a single massive galaxy cluster, run with 11
state-of-the-art codes, spanning adaptive mesh, moving mesh, classic and modern smoothed
particle hydrodynamics (SPH) approaches. For each code represented we have a dark-matteronly
(DM) and non-radiative (NR) version of the cluster, as well as a full physics (FP) version
for a subset of the codes. We compare both radial mass and kinematic profiles, as well as
global measures of the cluster (e.g. concentration, spin, shape), in the NR and FP runs with
that in the DM runs. Our analysis reveals good consistency (<≈
20 per cent) between global
properties of the cluster predicted by different codes when integrated quantities are measured
within the virial radius R200. However, we see larger differences for quantities within R2500,
especially in the FP runs. The radial profiles reveal a diversity, especially in the cluster centre,
between the NR runs, which can be understood straightforwardly from the division of codes
into classic SPH and non-classic SPH (including the modern SPH, adaptive and moving mesh
codes); and between the FP runs, which can also be understood broadly from the division
of codes into those that include active galactic nucleus feedback and those that do not. The
variation with respect to the median is much larger in the FP runs with different baryonic
physics prescriptions than in the NR runs with different hydrodynamics solvers.

Item Type: Article
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Divisions: Astrophysics Research Institute
Publisher: OXFORD UNIV PRESS
Related URLs:
Date Deposited: 13 Jun 2016 08:44
Last Modified: 08 Sep 2017 06:19
DOI or Identification number: 10.1093/mnras/stw603
URI: http://researchonline.ljmu.ac.uk/id/eprint/3763

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