Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 458, Issue 4, Pages 4052-4073Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw603
Keywords
methods: numerical; galaxies: clusters: general; galaxies: evolution; galaxies: formation; galaxies: haloes; cosmology: theory
Categories
Funding
- UWA Research Collaboration Award (RCA)
- Australian Research Council (ARC) Centre of Excellence for All Sky Astrophysics (CAASTRO) [CE110001020]
- ARC [DP130100117, DP140100198]
- Instituto de Fisica Teorica (IFT-UAM/CSIC in Madrid) via the Centro de Excelencia Severo Ochoa Program [SEV-2012-0249]
- UWA RCAs [PG12105017, PG12105026]
- Survey Simulation Pipeline (SSimPL)
- ARC Future Fellowship [FT130100041]
- ARC Discovery Projects [DP130100117, DP140100198]
- Ministerio de Economia y Competitividad (MINECO) in Spain [AYA2012-31101]
- Consolider-Ingenio Programme of the Spanish Ministerio de Ciencia e Innovacion (MICINN) [CSD2009-00064]
- SSimPL programme
- Sydney Institute for Astronomy (SIfA)
- Australian Research Council (ARC) [DP130100117, DP140100198]
- MINECO (Spain) [AYA 2012-31101]
- PRIN-MIUR Grant 'The Evolution of Cosmic Baryons'
- PRIN-INAF Grant 'Multiscale Simulations of Cosmic Structures' - Consorzio per la Fisica di Trieste
- DFG Cluster of Excellence 'Universe'
- DFG Research Unit 1254 'Magnetisation of interstellar and intergalactic media'
- Spanish Ministry of Economy and Competitiveness (MINECO) [AYA201346886, AYA2014-58308]
- MINECO [MINECO SEV-2011-0187]
- Kavli foundation
- ERC grant 'The Emergence of Structure during the epoch of Reionization'
- NSERC
- Canada Research Chairs programme
- CFI-NSRIT
- Australian Government
- Government of Western Australia
- Science and Technology Facilities Council [ST/P002315/1, ST/P002307/1, ST/K000373/1, ST/M006948/1, ST/M000990/1, ST/L000768/1, ST/M000966/1, ST/M007073/1] Funding Source: researchfish
- STFC [ST/M006948/1, ST/I004459/1, ST/M007073/1, ST/M000990/1, ST/I004459/2, ST/P002315/1, ST/L000768/1, ST/L000695/1, ST/P002307/1, ST/K000373/1] Funding Source: UKRI
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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-matter-only (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 (less than or similar to 20 per cent) between global properties of the cluster predicted by different codes when integrated quantities are measured within the virial radius R-200. However, we see larger differences for quantities within R-2500, 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.
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