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dc.contributor.authorCioni, M-R.L.
dc.contributor.authorHabing, H.J.
dc.date.accessioned2008-07-14T12:19:20Z
dc.date.available2008-07-14T12:19:20Z
dc.date.issued2003
dc.identifier.citationCioni , M-RL & Habing , H J 2003 , ' AGB stars in the Magellanic Clouds I: The C/M ratio ' , Astronomy and Astrophysics , vol. 402 , no. 1 , pp. 133-140 . https://doi.org/10.1051/0004-6361:20030226
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 151698
dc.identifier.otherPURE UUID: 94a56fa1-8d35-42c1-812b-ccf48560e518
dc.identifier.otherdspace: 2299/2209
dc.identifier.otherScopus: 0038222532
dc.identifier.urihttp://hdl.handle.net/2299/2209
dc.descriptionOriginal article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory
dc.description.abstractRegions of different metallicity have been identified in the Magellanic Clouds by using the ratio between Asymptotic Giant Branch stars of spectral type C and M. In the Large Magellanic Cloud the ratio appears to decrease radially while in the Small Magellanic Cloud (SMC) there is no clear trend, reflecting either the large extension of the SMC along the line of sight or a more complex star formation history. The distribution of the C/M ratio is clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There is an indication of increasing C/M ratio, thus decreasing metallicity, towards the Bridge region connecting the two Clouds.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsOpen
dc.titleAGB stars in the Magellanic Clouds I: The C/M ratioen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2003
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361:20030226
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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