dc.contributor.author | Peirani, S. | |
dc.contributor.author | Dubois, Y. | |
dc.contributor.author | Volonteri, M. | |
dc.contributor.author | Devriendt, J.E.G. | |
dc.contributor.author | Bundy, K. | |
dc.contributor.author | Silk, J. | |
dc.contributor.author | Pichon, C. | |
dc.contributor.author | Kaviraj, S. | |
dc.contributor.author | Gavazzi, R. | |
dc.contributor.author | Habouzit, M. | |
dc.date.accessioned | 2017-12-04T17:43:09Z | |
dc.date.available | 2017-12-04T17:43:09Z | |
dc.date.issued | 2017-12-01 | |
dc.identifier.citation | Peirani , 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 . https://doi.org/10.1093/mnras/stx2099 | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1611.09922v2 | |
dc.identifier.other | ORCID: /0000-0002-5601-575X/work/77850236 | |
dc.identifier.uri | http://hdl.handle.net/2299/19587 | |
dc.description | This 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.abstract | Using 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.extent | 17 | |
dc.format.extent | 2597100 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | astro-ph.GA | |
dc.title | Density profile of dark matter haloes and galaxies in the Horizon-AGN simulation : the impact of AGN feedback | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.contributor.institution | Centre for Astrophysics Research | |
dc.description.status | Peer reviewed | |
rioxxterms.versionofrecord | 10.1093/mnras/stx2099 | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |