dc.contributor.author Taylor, Philip dc.contributor.author Kobayashi, Chiaki dc.date.accessioned 2018-09-12T15:20:52Z dc.date.available 2018-09-12T15:20:52Z dc.date.issued 2017-11-11 dc.identifier.citation Taylor , P & Kobayashi , C 2017 , ' The Metallicity and Elemental Abundance Gradients of Simulated Galaxies, and their Environmental Dependence ' Monthly Notices of the Royal Astronomical Society , vol 471 , no. 4 , pp. 3856–3870 . DOI: 10.1093/mnras/stx1860 dc.identifier.issn 0035-8711 dc.identifier.other PURE: 14856458 dc.identifier.other PURE UUID: 6616db4b-5ced-4cfa-932d-dd1695214590 dc.identifier.other ArXiv: http://arxiv.org/abs/1707.06488v1 dc.identifier.other Scopus: 85043591566 dc.identifier.uri https://arxiv.org/abs/1707.06488 dc.description This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society. © 2018 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. dc.description.abstract The internal distribution of heavy elements, in particular the radial metallicity gradient, offers insight into the merging history of galaxies. Using our cosmological, chemodynamical simulations that include both detailed chemical enrichment and feedback from active galactic nuclei (AGN), we find that stellar metallicity gradients in the most massive galaxies ($\sim3\times10^{10}$M$_\odot$) are made flatter by mergers and are unable to regenerate due to the quenching of star formation by AGN feedback. The fitting range is chosen on a galaxy-by-galaxy basis in order to mask satellite galaxies. The evolutionary paths of the gradients can be summarised as follows; i) creation of initial steep gradients by gas-rich assembly, ii) passive evolution by star formation and/or stellar accretion at outskirts, iii) sudden flattening by mergers. There is a significant scatter in gradients at a given mass, which originates from the last path, and therefore from galaxy type. Some variation remains at given galaxy mass and type because of the complexity of merging events, and hence we find only a weak environmental dependence. Our early-type galaxies (ETGs), defined from the star formation main sequence rather than their morphology, are in excellent agreement with the observed stellar metallicity gradients of ETGs in the SAURON and ATLAS3D surveys. We find small positive [O/Fe] gradients of stars in our simulated galaxies, although they are smaller with AGN feedback. Gas-phase metallicity and [O/Fe] gradients also show variation, the origin of which is not as clear as for stellar populations. en dc.language.iso eng dc.relation.ispartof Monthly Notices of the Royal Astronomical Society dc.rights /dk/atira/pure/core/openaccesspermission/open dc.subject astro-ph.GA dc.title The Metallicity and Elemental Abundance Gradients of Simulated Galaxies, and their Environmental Dependence en dc.contributor.institution Centre for Astrophysics Research dc.contributor.institution School of Physics, Astronomy and Mathematics dc.description.status Peer reviewed dc.identifier.url https://arxiv.org/abs/1707.06488 dc.relation.school School of Physics, Astronomy and Mathematics dc.description.versiontype Final Accepted Version dcterms.dateAccepted 2017-07-20 rioxxterms.version AM rioxxterms.versionofrecord https://doi.org/10.1093/mnras/stx1860 rioxxterms.type Journal Article/Review herts.preservation.rarelyaccessed true herts.rights.accesstype openAccess
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