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dc.contributor.authorPeirani, S.
dc.contributor.authorDubois, Y.
dc.contributor.authorVolonteri, M.
dc.contributor.authorDevriendt, J.E.G.
dc.contributor.authorBundy, K.
dc.contributor.authorSilk, J.
dc.contributor.authorPichon, C.
dc.contributor.authorKaviraj, S.
dc.contributor.authorGavazzi, R.
dc.contributor.authorHabouzit, M.
dc.date.accessioned2017-12-04T17:43:09Z
dc.date.available2017-12-04T17:43:09Z
dc.date.issued2017-12-01
dc.identifier.citationPeirani , S , Dubois , Y , Volonteri , M , Devriendt , J E G , Bundy , K , Silk , J , Pichon , C , Kaviraj , S , Gavazzi , R & Habouzit , M 2017 , ' Density profile of dark matter haloes and galaxies in the Horizon-AGN simulation : the impact of AGN feedback ' Monthly Notices of the Royal Astronomical Society , vol 472 , no. 2 , stx2099 , pp. 2153-2169 . DOI: 10.1093/mnras/stx2099
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 12744850
dc.identifier.otherPURE UUID: 8e6f1e12-640f-4fa9-b72c-c3ba39273050
dc.identifier.otherArXiv: http://arxiv.org/abs/1611.09922v2
dc.identifier.urihttp://hdl.handle.net/2299/19587
dc.descriptionThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. ©: 2017 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society.
dc.description.abstractUsing a suite of three large cosmological hydrodynamical simulations, Horizon-AGN, Horizon-noAGN (no AGN feedback) and Horizon-DM (no baryons), we investigate how a typical sub-grid model for AGN feedback affects the evolution of the inner density profiles of massive dark matter haloes and galaxies. Based on direct object-to-object comparisons, we find that the integrated inner mass and density slope differences between objects formed in these three simulations (hereafter, H_AGN, H_noAGN and H_DM) significantly evolve with time. More specifically, at high redshift (z~5), the mean central density profiles of H_AGN and H_noAGN dark matter haloes tend to be much steeper than their H_DM counterparts owing to the rapidly growing baryonic component and ensuing adiabatic contraction. By z~1.5, these mean halo density profiles in H_AGN have flattened, pummelled by powerful AGN activity ("quasar mode"): the integrated inner mass difference gaps with H_noAGN haloes have widened, and those with H_DM haloes have narrowed. Fast forward 9.5 billion years, down to z=0, and the trend reverses: H_AGN halo mean density profiles drift back to a more cusped shape as AGN feedback efficiency dwindles ("radio mode"), and the gaps in integrated central mass difference with H_noAGN and H_DM close and broaden respectively. On the galaxy side, the story differs noticeably. Averaged stellar profile central densities and inner slopes are monotonically reduced by AGN activity as a function of cosmic time, resulting in better agreement with local observations. As both dark matter and stellar inner density profiles respond quite sensitively to the presence of a central AGN, there is hope that future observational determinations of these quantities can be used constrain AGN feedback models.en
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.subjectastro-ph.GA
dc.titleDensity profile of dark matter haloes and galaxies in the Horizon-AGN simulation : the impact of AGN feedbacken
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dc.description.versiontypeFinal Published version
dcterms.dateAccepted2017-08-11
rioxxterms.versionAM
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stx2099
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeopenAccess


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