The objective-prism surveys such as HK and Hamburg ESO (HES)
discovered numerous Very Metal-Poor (VMP; [Fe/H] < -2.0) stars
in the Milky Way. Recently, the number of VMP stars has been
dramatically increased to many tens of thousands, thanks to
Sloan Digital Sky Survey (SDSS) and Sloan Extension for Galactic
Understand and Exploration (SEGUE). Detailed chemical-abundance
analyses, based on high-resolution
spectroscopic follow-up, have revealed that, while most VMP stars
exhibit similar abundance patterns, there are numerous examples of
objects with peculiar chemical patterns. Among the chemically
peculiar stars with [Fe/H] < -2.0, objects with enhanced
carbon abundance are the most common variety. These are
called Carbon-Enhanced Metal-Poor (CEMP) stars. One of the
most interesting aspects of the CEMP stars is that the fraction of
the CEMP stars increases as the metallicity decreases. In this talk, I
will review the current understanding of the CEMP stars and discuss
their implication to the first-generation stars and the origin of the
Milky Way galaxy.