2009A&A...508L...1F

We establish the mean metallicity from high-resolution spectroscopy for the recently found dwarf spheroidal galaxy BooetesI and test whether it is a common feature for ultra-faint dwarf spheroidal galaxies to show signs of inhomogeneous chemical evolution (e.g. as found in the Hercules dwarf spheroidal galaxy). We analyse high-resolution, moderate signal-to-noise spectra for seven red giant stars in the BooetesI dSph galaxy using standard abundance analysis techniques. In particular, we assume local thermodynamic equilibrium and employ spherical model atmospheres and codes that take the sphericity of the star into account when calculating the elemental abundances. We confirm previous determinations of the mean metallicity of the BooetesI dwarf spheroidal galaxy to be -2.3dex. Whilst five stars are clustered around this metallicity, one is significantly more metal-poor, at -2.9dex, and one is more metal-rich at, -1.9dex. Additionally, we find that one of the stars, Boo-127, shows an atypically high [Mg/Ca] ratio, indicative of stochastic enrichment processes within the dSph galaxy. Similar results have previously only been found in the Hercules and Draco dSph galaxies and appear, so far, to be unique to this type of galaxy.