Volume 396, Number 1, December II 2002
|Page(s)||53 - 64|
|Section||Cosmology (including clusters of galaxies)|
|Published online||22 November 2002|
The present-day chemical composition of the LMC
Department of Pure & Applied Physics, The Queen's University of Belfast, BT7 1NN, Northern Ireland, UK
Corresponding author: W. R. J. Rolleston, R.Rolleston@qub.ac.uk
Accepted: 24 July 2002
High-resolution observations of five OB-type main-sequence stars in the Large Magellanic Cloud (LMC) have been obtained with the UCL échelle spectrograph on the 3.9-m Anglo-Australian Telescope. These spectra have been analysed using LTE model-atmosphere techniques, to derive stellar atmospheric parameters and chemical compositions. As these stars are located within the hydrogen burning main-sequence band, their surface abundances should reflect those of the present-day interstellar medium. Detailed line-by-line differential analyses have been undertaken relative to Galactic comparison stars. We conclude that there exists a general metal deficiency of dex within the LMC, and find no significant abundance variations between cluster and field stars. There is also tentative evidence to suggest a lower oxygen to iron abundance ratio, and an over-deficiency of magnesium relative to the other α–elements. These are discussed in terms of previous abundance analyses and models of discontinuous (or bursting) star formation within the LMC. Finally, there is some evidence to suggest a greater chemical enrichment of material within the region LH 104.
Key words: stars: abundances / stars: atmospheres / stars: early-type / galaxies:individual: Large Magellanic Cloud
© ESO, 2002
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