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

Show simple item record

dc.creator Cui, Weiguang
dc.creator Power, Chris
dc.creator Knebe, Alexander
dc.creator Kay, Scott T.
dc.creator Sembolini, Federico
dc.creator Elahi, Pascal J.
dc.creator Yepes, Gustavo
dc.creator Pearce, Frazer
dc.creator Cunnama, Daniel
dc.creator Beck, Alexander M.
dc.creator Thacker, Robert John, 1970-
dc.date.accessioned 2018-02-13T13:45:48Z
dc.date.available 2018-02-13T13:45:48Z
dc.date.issued 2016-06-01
dc.identifier.issn 0035-8711
dc.identifier.uri http://library2.smu.ca/handle/01/27272
dc.description Publisher's Version/PDF
dc.description.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-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[subscript 200]. However, we see larger differences for quantities within R[subscript 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. en_CA
dc.language.iso en en_CA
dc.publisher Oxford University Press en_CA
dc.relation.uri https://dx.doi.org/10.1093/mnras/stw603
dc.rights 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.
dc.subject.lcsh Galaxies -- Clusters
dc.subject.lcsh Baryons
dc.subject.lcsh Galactic halos
dc.subject.lcsh Galaxies -- Evolution
dc.subject.lcsh Galaxies -- Formation
dc.title nIFTy galaxy cluster simulations – IV. Quantifying the influence of baryons on halo properties en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Monthly Notices of the Royal Astronomical Society 458(4), 4052-4073. (2016) en_CA


Files in this item


 

Copyright statement:

 
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.
 
Published Version: https://dx.doi.org/10.1093/mnras/stw603
 
 

This item appears in the following Collection(s)

Show simple item record