  Metal-poor stars provide the fossil record of Galactic chemical evolution and
the nucleosynthesis processes that took place at the earliest times in the
history of our Galaxy. From detailed abundance studies of low mass, extremely
metal-poor stars ([Fe/H] < -3), we can trace and help constrain the formation
processes which created the first heavy elements in our Galaxy. Here we present
the results of a ~25-star homogeneously analysed sample of metal-poor
candidates from the Hamburg/ESO survey. We have derived abundances for a large
number of elements ranging from Li to Ba, covering production processes from
hydrostatic burning to neutron-capture. The sample includes some of the most
metal-poor stars ([Fe/H] < -4) studied to date, and also a number of stars
enhanced 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 stars
with [Fe/H] < -4.5. The progenitors of CEMP stars are still not fully
constrained; they could be a result of binary mass transfer or high-mass
explosive events in the early universe.
