We report the abundance analysis of new high S/N spectra of the most metal-poor ( [ Fe/H ] = -2.95 ) star presently known to be a member of a dwarf galaxy , the Draco dSph red giant , D119 .
No absorption lines for elements heavier than Ni are detected in two Keck HIRES spectra covering the \lambda \lambda 3850–6655 Å wavelength range , phenomenon not previously noted in any other metal-poor star .
We present upper limits for several heavy element abundances .
The most stringent limits , based on the non-detection of Sr ii and Ba ii lines , indicate that the total s- and r-process enrichment of D119 is at least 100 times smaller than Galactic stars of similar metallicity .
The light element abundances are consistent with the star having formed out of material enciched primarily by massive Type II supernovae ( M > 20 – 25 M _ { \odot } ) .
If this is the case , we are forced to conclude that massive , metal-poor Type II supernovae did not contribute to the r-process in the proto-Draco environment .
We compare the abundance pattern observed in D119 to current predictions of prompt enrichement and pair-instability supernovae and find that the model predictions fail by an order or maginitude or more for many elements .