We use previously-published moderate-resolution spectra in combination with stellar atmosphere models to derive the first measured chemical abundance ratios in the Leo II dSph galaxy .
We find that for spectra with SNR > 24 , we are able to measure abundances from weak Ti , Fe and Mg lines located near the calcium infrared triplet ( CaT ) .
We also quantify and discuss discrepancies between the metallicities measured from Fe I lines and those estimated from the CaT features .
We find that while the most metal-poor ( [ Fe/H ] < -2.0 ] ) Leo II stars have Ca and Ti abundance ratios similar to those of Galactic globular clusters , the more metal-rich stars show a gradual decline of Ti , Mg and Ca abundance ratio with increasing metallicity .
Finding these trends in this distant and apparently dynamically stable dSph galaxy supports the hypothesis that the slow chemical enrichment histories of the dSph galaxies is universal , independent of any interaction with the Milky Way .
Combining our spectroscopic abundances with published broadband photometry and updated isochrones , we are able to approximate stellar ages for our bright RGB stars to a relative precision of 2-3 Gyr .
While the derived age-metallicity relationship of Leo II hints at some amount of slow enrichment , the data are still statistically consistent with no enrichment over the history of Leo II .