  We report the discovery of one extremely metal-poor (EMP; [Fe/H]<-3) and one
ultra metal-poor (UMP; [Fe/H]<-4) star selected from the SDSS/SEGUE survey.
These stars were identified as EMP candidates based on their medium-resolution
(R~2,000) spectra, and were followed-up with high-resolution (R~35,000)
spectroscopy with the Magellan-Clay Telescope. Their derived chemical
abundances exhibit good agreement with those of stars with similar
metallicities. We also provide new insights on the formation of the UMP stars,
based on comparison with a new set of theoretical models of supernovae
nucleosynthesis. The models were matched with 20 UMP stars found in the
literature, together with one of the program stars (SDSS J1204+1201), with
[Fe/H]=-4.34. From fitting their abundances, we find that the supernovae
progenitors, for stars where carbon and nitrogen are measured, had masses
ranging from 20.5 M_sun to 28 M_sun and explosion energies from 0.3 to
0.9x10^51 erg. These results are highly sensitive to the carbon and nitrogen
abundance determinations, which is one of the main drivers for future
high-resolution follow-up of UMP candidates. In addition, we are able to
reproduce the different CNO abundance patterns found in UMP stars with a single
progenitor type, by varying its mass and explosion energy.
