The iron abundance in the Magellanic Clouds and Bridge

Details The iron abundance in the Magellanic Clouds and Bridge The iron abundance in the Magellanic Clouds and Bridge

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9130d&link_type=abstract

HST Proposal ID #9130

Physics

Hst Proposal Id #9130 Hot Stars

Scientific paper

The spectra of early-type main-sequence stars provide excellent probes of the current chemical composition of galaxies. The physics of their atmospheres are well understood, while their surfaces will normally be unaffected by the products of interior nuclear reactions. We have previously used optical spectra of such targets to map the abundances of light metals {such as C, N, O, Mg, Si} in our Galaxy, in the Magellanic Clouds and in a Bridge of material connecting the latter. However, we have been unable to obtain iron group abundances for the Magellanic System due to the intrinsic weakness of the optical Fe II/III spectra and the system's low metallicity. Here we propose observations of strong Fe III ultraviolet lines for two Bridge stars, plus an LMC target. These will be supplemented by AAT and ESO optical spectroscopy plus HST spectra for two previously observed targets in the middle of the Bridge and in the SMC. Using non-LTE model atmosphere and careful differential methods, relative abundances accurate to 0.1 dex should be achievable. These five stars will allow us to determine key element abundances and ratios {eg. O/Fe} in both Clouds and across the Bridge. As well as providing the first detailed comparison of the Bridge's metallicity with those of its parent Clouds, it will clarify the evolutionary history of this system.

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