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dc.contributor.authorCioni, M-R.L.
dc.contributor.authorGirardi, L.
dc.contributor.authorMarigo, P.
dc.contributor.authorHabing, H.J.
dc.date.accessioned2008-07-14T12:59:21Z
dc.date.available2008-07-14T12:59:21Z
dc.date.issued2006
dc.identifier.citationCioni , M-RL , Girardi , L , Marigo , P & Habing , H J 2006 , ' AGB stars in the Magellanic Clouds II. The rate of star formation across the LMC ' , Astronomy and Astrophysics , vol. 448 , pp. 77-91 . https://doi.org/10.1051/0004-6361:20053933
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 156941
dc.identifier.otherPURE UUID: 9056f33f-2bf1-4ae9-a396-48035fb403b9
dc.identifier.otherdspace: 2299/2215
dc.identifier.otherScopus: 33644925912
dc.identifier.urihttp://hdl.handle.net/2299/2215
dc.descriptionOriginal article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory (ESO)
dc.description.abstractThis article compares the distribution of Ks magnitudes of Large Magellanic Cloud (LMC) asymptotic giant branch (AGB) stars obtained from the DENIS and 2MASS data with theoretical distributions. These have been constructed using up-to-date stellar evolution calculations for low and intermediate-mass stars, and in particular for thermally pulsing AGB stars. A fit of the magnitude distribution of both carbon- and oxygen-rich AGB stars allowed us to constrain the metallicity distribution across the LMC and its star formation rate (SFR). The LMC stellar population is found to be on average 5 − 6 Gyr old and is consistent with a mean metallicity corresponding to Z = 0.006. These values may however be affected by systematic errors in the underlying stellar models, and by the limited exploration of the possible SFR histories. Instead our method should be particularly useful for detecting variations in the mean metallicity and SFR across the LMC disk. There are well defined regions where both the metallicity and the mean-age of the underlying stellar population span the whole range of grid parameters. The C/M ratio discussed in paper I is a tracer of the metallicity distribution if the underlying stellar population is older than about a few Gyr. A similar study across the Small Magellanic Cloud is given in paper III of this series.en
dc.language.isoeng
dc.relation.ispartofAstronomy and Astrophysics
dc.rightsOpen
dc.titleAGB stars in the Magellanic Clouds II. The rate of star formation across the LMCen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
dcterms.dateAccepted2006
rioxxterms.versionofrecordhttps://doi.org/10.1051/0004-6361:20053933
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeOpen


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