  We present a detailed abundance analysis based on high resolution and high
signal-to-noise spectra of eight extremely metal poor (EMP) stars with [Fe/H] <
-3.5$ dex, four of which are new. Only stars with 4900 < Teff< 5650 K are
included. Two stars of the eight are outliers in each of several abundance
ratios. The most metal poor star in this sample, HE1424-0241, has [Fe/H] ~ -4
dex and is thus among the most metal poor stars known in the Galaxy. It has
highly anomalous abundance ratios unlike those of any other known EMP giant,
with very low Si, Ca and Ti relative to Fe, and enhanced Mn and Co, again
relative to Fe. Only (low) upper limits for C and N can be derived from the
non-detection of the CH and NH molecular bands. HE0132$-$2429, another sample
star, has excesses of N and Sc with respect to Fe. The strong outliers in
abundance ratios among the Fe-peak elements in these C-normal stars, not found
at somewhat higher metallicities, are definitely real. They suggest that at
such low metallicities we are beginning to see the anticipated and long sought
stochastic effects of individual supernova events contributing to the Fe-peak
material within a single star. A detailed comparison of the results of the
analysis procedures adopted by our 0Z project compared to those of the First
Stars VLT Large Project finds a systematic difference for [Fe/H] of ~0.3 dex,
our values always being higher.
