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dc.contributor.authorTaylor, Philip
dc.contributor.authorKobayashi, Chiaki
dc.contributor.authorFederrath, Christoph
dc.date.accessioned2019-03-26T15:11:27Z
dc.date.available2019-03-26T15:11:27Z
dc.date.issued2019-03-06
dc.identifier.citationTaylor , P , Kobayashi , C & Federrath , C 2019 , ' The metallicity and elemental abundance maps of kinematically atypical galaxies for constraining minor merger and accretion histories ' , Monthly Notices of the Royal Astronomical Society , vol. 485 , no. 3 , pp. 3215–3223 . https://doi.org/10.1093/mnras/stz630
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 16459215
dc.identifier.otherPURE UUID: 20852fb6-cb4f-4a87-9c34-6f9ca149aff1
dc.identifier.otherArXiv: http://arxiv.org/abs/1903.01597v1
dc.identifier.otherScopus: 85063151480
dc.identifier.otherORCID: /0000-0002-4343-0487/work/62750487
dc.identifier.urihttp://hdl.handle.net/2299/21225
dc.description© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.description.abstractExplaining the internal distribution and motions of stars and gas in galaxies is a key aspect in understanding their evolution. In previous work we identified five well-resolved galaxies with atypical kinematics from a cosmological simulation; two had kinematically distinct cores (KDCs), and three had counter-rotating gas and stars (CRGD). In this paper, we show that (i) the KDC galaxies have flattening of stellar [O/Fe] at large galactocentric radii due to the minor mergers that gave rise to the KDCs, and (ii) the CRGD galaxies have an abrupt transition in the gas metallicity maps, from high metallicity in the centre to very low metallicity further out. These galaxies are embedded in dark matter filaments where there is a ready supply of near-pristine gas to cause this effect. The non-linear increase in gas metallicity is also seen in the radial profiles, but when the metallicity gradients are measured, the difference is buried in the scatter of the relation. We also find that all five galaxies are fairly compact, with small effective radii given their stellar masses. This is because they have not experienced major mergers that kinematically heat the stars, and would have destroyed their unusual kinematics. In order to detect these signatures of minor mergers or accretion, the galaxy scaling relations or radial metallicity profiles are not enough, and it is necessary to obtain the two-dimensional maps with integral field spectroscopy observations.en
dc.format.extent9
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectastro-ph.GA
dc.subjectGalaxies: evolution
dc.subjectGalaxies: kinematics and dynamics
dc.subjectMethods: numerical
dc.subjectAstronomy and Astrophysics
dc.subjectSpace and Planetary Science
dc.titleThe metallicity and elemental abundance maps of kinematically atypical galaxies for constraining minor merger and accretion historiesen
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.identifier.urlhttp://www.scopus.com/inward/record.url?scp=85063151480&partnerID=8YFLogxK
dc.identifier.urlhttps://arxiv.org/abs/1903.01597
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1093/mnras/stz630
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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