  Studying a range of old metal-poor stars provides information over
cosmological timescales of our Galaxy. Such studies are indicative of the
pristine gases and evolution of the Milky Way. Deriving stellar parameters and
abundances from high-resolution observations of stars at various stellar
evolution stages (including old dwarfs and RR Lyrae), allows us to use these
abundances as tracers of an even earlier progenitor population. Here, we carry
out a detailed abundance study of mainly heavy elements (Z > 38), i.e.
neutron-capture elements, which we at low metallicities ([Fe/H] < -2.5) take as
pure supernova type II products. A comparison of the derived abundances to type
II supernova yields of heavy elements provides knowledge of the old stellar
generations as well as properties of neutron-capture formation sites.
