  Carbon-enhanced metal-poor (CEMP) stars represent a sizeable fraction of all
known metal-poor stars in the Galaxy. Their formation and composition remains a
significant topic of investigation within the stellar astrophysics community.
We analysed a sample of low-resolution spectra of 30 dwarf stars, obtained
using the the visual and near UV FOcal Reducer and low dispersion Spectrograph
for the Very Large Telescope (FORS/VLT) of the European Southern Observatory
(ESO) and the Gemini Multi-Object Spectrographs (GMOS) at the GEMINI telescope,
to derive their metallicity and carbon abundance. We derived C and Ca from all
spectra, and Fe and Ba from the majority of the stars. We have extended the
population statistics of CEMP stars and have confirmed that in general, stars
with a high C abundance belonging to the high C band show a high Ba-content
(CEMP-s or -r/s), while stars with a normal C-abundance or that are C-rich, but
belong to the low C band, are normal in Ba (CEMP-no).
