The nature of the red giant branches in the Ursa Minor and Draco dwarf spheroidal galaxies

Spectra for stars located redward of the fiducial red giant branches (RGBs) of the Ursa Minor and Draco dwarf spheroidal galaxies have been obtained w ith the Hobby-Eberly telescope and the Marcario Low Resolution Spectrometer . From a comparison of our radial velocities with those reported in previou s medium-resolution studies, we find an average difference of 10 km s(-1) w ith a standard deviation of 11 km s(-1).On the basis of these radial veloci ties, we confirm the membership of five stars in Ursa Minor and find two ot hers to be nonmembers. One of the confirmed members is a known carbon star that lies redward of the RGB; three others are previously unidentified carb on stars. The fifth star is a red giant that was found previously by Shetro ne and coworkers to have [Fe/H] = -1.68 +/-0.11 dex. In Draco, we find eigh t nonmembers, confirm the membership of one known carbon star, and find two new members. One of these stars is a carbon star, while the other shows no evidence for C-2 bands or strong atomic bands, although the signal-to-nois e ratio of the spectrum is low. Thus, we find no evidence for a population of stars more metal-rich than [Fe/H]similar or equal to -1.45 dex in either of these galaxies. Indeed, our spectroscopic survey suggests that every ca ndidate suspected of having a metallicity in excess of this value based on its position in the color- magnitude diagram is, in actuality, a carbon sta r. Based on the census of 13 known carbon stars in these two galaxies, we e stimate the carbon star specific frequency to be epsilon (dSph)similar or e qual to2.4x10(-5) L-V,circle dot(-1), 25-100 times higher than that of Gala ctic globular clusters.