Show simple item record

dc.contributor.authorArthur, Jake
dc.contributor.authorPearce, Frazer R.
dc.contributor.authorGray, Meghan E.
dc.contributor.authorElahi, Pascal J.
dc.contributor.authorKnebe, Alexander
dc.contributor.authorBeck, Alexander M.
dc.contributor.authorCui, Weiguang
dc.contributor.authorCunnama, Daniel
dc.contributor.authorDave, Romeel
dc.date.accessioned2018-11-15T07:17:50Z
dc.date.available2018-11-15T07:17:50Z
dc.date.issued2016
dc.identifier.citationArthur, J. et al. (2016). nIFTy galaxy cluster simulations – V. Investigation of the cluster infall region. Monthly Notices of the Royal Astronomical Society, 464: 2027 - 2038.en_US
dc.identifier.issn0035-8711
dc.identifier.urihttp://dx.doi.org/10.1093/mnras/stw2424
dc.identifier.urihttp://hdl.handle.net/10566/4203
dc.description.abstractWe examine the properties of the galaxies and dark matter haloes residing in the cluster infall region surrounding the simulated cold dark matter galaxy cluster studied by Elahi et al. at z = 0. The 1.1 × 1015 h−1M galaxy cluster has been simulated with eight different hydrodynamical codes containing a variety of hydrodynamic solvers and sub-grid schemes. All models completed a dark-matter-only, non-radiative and full-physics run from the same initial conditions. The simulations contain dark matter and gas with mass resolution mDM = 9.01 × 108 h−1M and mgas = 1.9 × 108 h−1M , respectively. We find that the synthetic cluster is surrounded by clear filamentary structures that contain ∼60 per cent of haloes in the infall region with mass ∼1012.5–1014 h−1M , including 2–3 group-sized haloes (>1013 h−1M ). However, we find that only ∼10 per cent of objects in the infall region are sub-haloes residing in haloes, which may suggest that there is not much ongoing pre-processing occurring in the infall region at z = 0. By examining the baryonic content contained within the haloes, we also show that the code-to-code scatter in stellar fraction across all halo masses is typically ∼2 orders of magnitude between the two most extreme cases, and this is predominantly due to the differences in sub-grid schemes and calibration procedures that each model uses. Models that do not include active galactic nucleus feedback typically produce too high stellar fractions compared to observations by at least ∼1 order of magnitude.en_US
dc.language.isoenen_US
dc.publisherOxford University Pressen_US
dc.rightsThis article is open access and copyright lies with the authors
dc.subjectNumericalen_US
dc.subjectGalaxiesen_US
dc.subjectClustersen_US
dc.subjectGeneralen_US
dc.subjectDark matteren_US
dc.titlenIFTy galaxy cluster simulations – V. Investigation of the cluster infall regionen_US
dc.typeArticleen_US
dc.privacy.showsubmitterFALSE
dc.status.ispeerreviewedTRUE
dc.description.accreditationISI


Files in this item

Thumbnail

This item appears in the following Collection(s)

Show simple item record