We present an abundance analysis based on high resolution spectra of 8 stars selected to span the full range in metallicity in the Draco dwarf spheroidal galaxy .
We find [ Fe/H ] for the sample stars ranges from -1.5 to -3.0 dex .
Combining our sample with previously published work for a total of 14 luminous Draco giants , we show that the abundance ratios [ Na/Fe ] , [ Mg/Fe ] and [ Si/Fe ] for the Draco giants overlap those of Galactic halo giants at the lowest [ Fe/H ] probed , but are significantly lower for the higher Fe-metallicity Draco stars .
For the explosive \alpha -elements Ca and Ti , the abundance ratios for Draco giants with [ Fe/H ] > -2.4 dex are approximately constant and slightly sub-solar , well below values characteristic of Galactic halo stars .
The s -process contribution to the production of heavy elements begins at significantly lower Fe-metallicity than in the Galactic halo .

Using a toy model we compare the behavior of the abundance ratios within the sample of Draco giants with those from the literature of Galactic globular clusters , and the Carina and Sgr dSph galaxies .
The differences appear to be related to the timescale for buildup of the heavy elements , with Draco having the slowest rate .

We note the presence of a Draco giant with [ Fe/H ] < -3.0 dex in our sample , and reaffirm that the inner Galactic halo could have been formed by early accretion of Galactic satellite galaxies and dissolution of young globular clusters , while the outer halo could have formed from those satellite galaxies accreted later .