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[112.22] The Chemical Composition of the Magellanic Bridge

J.A. Vermedahl (University of Minnesota), K.A. Venn (Macalester College), W.R.J. Rolleston (The Queen's University of Belfast), A. Brooks (University of Washington), T. Mendel, C. Baldner (Macalester College)

We present differential abundance results for four A-type supergiants in the Magellanic Bridge. VLT UVES, CTIO 4m, and AAT high resolution spectra of these stars have been analyzed using ATLAS9 model atmosphere and NIST atomic data. The metallicities of the four A stars range from SMC-like to an underabundance of 0.5 dex relative to the SMC. These results support the low silicon/oxygen abundances determined from B-type Bridge stars (Rolleston et al. 2003), but extends the work to the iron-group and heavier elements. Thus, the [alpha/Fe] ratio of the Bridge appears to be near solar. Also, these results indicate a metallicity gradient of 0.13 dex/kpc in the Bridge, extending from the SMC wing towards the LMC.

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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.