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Metal-poor stars provide the fossil record of Galactic chemical evolution andthe nucleosynthesis processes that took place at the earliest times in thehistory of our Galaxy. From detailed abundance studies of low mass, extremelymetal-poor stars ([Fe/H] < -3), we can trace and help constrain the formationprocesses which created the first heavy elements in our Galaxy. Here we presentthe results of a ~25-star homogeneously analysed sample of metal-poorcandidates from the Hamburg/ESO survey. We have derived abundances for a largenumber of elements ranging from Li to Ba, covering production processes fromhydrostatic burning to neutron-capture. The sample includes some of the mostmetal-poor stars ([Fe/H] < -4) studied to date, and also a number of starsenhanced in carbon. The so called CEMP (carbon enhanced metal-poor) stars,these stars make up ~20% of the stars with [Fe/H] < -3, and 80% of the starswith [Fe/H] < -4.5. The progenitors of CEMP stars are still not fullyconstrained; they could be a result of binary mass transfer or high-massexplosive events in the early universe.

New Abundances From Very Old Stars