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dc.contributor.authorCioni, M-R.L.
dc.date.accessioned2009-11-25T13:57:11Z
dc.date.available2009-11-25T13:57:11Z
dc.date.issued2009-11
dc.identifier.citationCioni , M-RL 2009 , ' The metallicity gradient as a tracer of history and structure : the Magellanic Clouds and M33 galaxies ' , Astronomy and Astrophysics , vol. 506 , no. 3 , pp. 1137-1146 . https://doi.org/10.1051/0004-6361/200912138
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 154373
dc.identifier.otherPURE UUID: 802c94a9-ea0d-46c4-8522-846c64e8044e
dc.identifier.otherdspace: 2299/4013
dc.identifier.otherScopus: 70350780563
dc.identifier.urihttp://hdl.handle.net/2299/4013
dc.descriptionOriginal article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory (ESO) DOI: 10.1051/0004-6361/200912138
dc.description.abstractContext. The stellar metallicity and its gradient place constraints on the formation and evolution of galaxies. Aims. This is a study of the metallicity gradient of the LMC, SMC and M33 galaxies derived from their asymptotic giant branch (AGB) stars. Methods. The [Fe/H] abundance was derived from the ratio between C- and M-type AGB stars and its variation analysed as a function of galactocentric distance. Galaxy structure parameters were adopted from the literature. Results. The metallicity of the LMC decreases linearly as −0.047±0.003 dex kpc−1 out to ∼8 kpc from the centre. In the SMC, [Fe/H] has a constant value of ∼−1.25 ± 0.01 dex up to ∼12 kpc. The gradient of the M33 disc, until ∼9 kpc, is −0.078 ± 0.003 dex kpc−1 while the outer disc/halo, out to ∼25 kpc, has [Fe/H] ∼ −1.7 dex. Conclusions. The metallicity of the LMC, as traced by different populations, bears the signature of two major star forming episodes: the first one constituting a thick disc/halo population and the second one a thin disc and bar due to a close encounter with the Milky Way and SMC. The [Fe/H] of the recent episode supports an LMC origin for the Stream. The metallicity of the SMC supports star formation, ∼3 Gyr ago, as triggered by LMC interaction and sustained by the bar in the outer region of the galaxy. The SMC [Fe/H] agrees with the present-day abundance in the Bridge and shows no significant gradient. The metallicity of M33 supports an “insideout” disc formation via accretion of metal poor gas from the interstellar medium.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rights/dk/atira/pure/core/openaccesspermission/open
dc.titleThe metallicity gradient as a tracer of history and structure : the Magellanic Clouds and M33 galaxiesen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.contributor.institutionScience & Technology Research Institute
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.versionVoR
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361/200912138
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeclosedAccess


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