Multi-element Abundance Measurements from Medium-resolution Spectra. I. the Sculptor Dwarf Spheroidal Galaxy

We present measurements of Fe, Mg, Si, Ca, and Ti abundances for 388 radial velocity member stars in the Sculptor dwarf spheroidal galaxy (dSph), a satellite of the Milky Way. This is the largest sample of individual α element (Mg, Si, Ca, Ti) abundance measurements in any single dSph. The measurements are made from Keck/DEIMOS medium-resolution spectra (6400–9000 Å, R ∼ 6500). Based on comparisons to published high-resolution (R & 20000) spectroscopic measurements, our measurements have uncertainties of σ[Fe/H] = 0.14 and σ[α/Fe] = 0.13. The Sculptor [Fe/H] distribution has a mean 〈[Fe/H]〉 = −1.58 and is asymmetric with a long, metal-poor tail, indicative of a history of extended star formation. Sculptor has a larger fraction of stars with [Fe/H] < −2 than the Milky Way halo. We have discovered one star with [Fe/H] = −3.80±0.28, which is the most metalpoor star known anywhere except the Milky Way halo, but high-resolution spectroscopy is needed to measure this star’s detailed abundances. As has been previously reported based on high-resolution spectroscopy, [α/Fe] in Sculptor falls as [Fe/H] increases. The metal-rich stars ([Fe/H] ∼ −1.5) have lower [α/Fe] than Galactic halo field stars of comparable metallicity. This indicates that star formation proceeded more gradually in Sculptor than in the Galactic halo. We also observe radial abundance gradients of −0.030± 0.003 dex per arcmin in [Fe/H] and +0.013 ± 0.003 dex per arcmin in [α/Fe] out to 11 arcmin (275 pc). Together, these measurements cast Sculptor and possibly other surviving dSphs as representative of the dwarf galaxies from which the metal-poor tail of the Galactic halo formed. Subject headings: galaxies: individual (Sculptor dwarf) — galaxies: dwarf — galaxies: abundances — Galaxy: evolution — Local Group