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We present the results of a low-resolution spectral abundance study of 25stars in the Bootes I dwarf spheroidal (dSph) galaxy. The data were obtainedwith the LRIS instrument at Keck Observatory, and allow us to measure [Fe/H],[C/Fe], and [alpha/Fe] for each star. We find both a large spread inmetallicity (2.1 dex in [Fe/H]) as well as the low average metallicity in thissystem, <[Fe/H]>=-2.59, matching previous estimates. This sample includes anewly discovered extremely metal-poor star, with [Fe/H]=-3.8, that is one ofthe most metal-poor stars yet found in a dSph. We compare the metallicitydistribution function of Bootes I to analytic chemical evolution models. Whilethe metallicity distribution function of Bootes I is best fit by an Extra Gaschemical evolution model, leaky-box models also provide reasonable fits. Wealso find that the [alpha/Fe] distribution and the carbon-enhanced metal-poorfraction of our sample (12%) are reasonable matches to Galactic halo starsamples in the same metallicity range, indicating that at these lowmetallicities, systems like the Bootes I ultra-faint dSph could have beencontributors to the Galactic halo.

The [Fe/H], [C/Fe], and [alpha/Fe] distributions of the Bootes I Dwarf Spheroidal Galaxy