  We report on early results from a pilot program searching for metal-poor
stars with LAMOST and follow-up high-resolution observation acquired with the
MIKE spectrograph attached to the Magellan~II telescope. We performed detailed
abundance analysis for eight objects with iron abundances [Fe/H] < -2.0,
including five extremely metal-poor (EMP; [Fe/H] < -3.0) stars with two having
[Fe/H] < -3.5. Among these objects, three are newly discovered EMP stars, one
of which is confirmed for the first time with high-resolution spectral
observations. Three program stars are regarded as carbon-enhanced metal-poor
(CEMP) stars, including two stars with no enhancement in their neutron-capture
elements, which thus possibly belong to the class of CEMP-no stars; one of
these objects also exhibits significant enhancement in nitrogen, and is thus a
potential carbon and nitrogen-enhanced metal-poor star. The [X/Fe] ratios of
the sample stars generally agree with those reported in the literature for
other metal-poor stars in the same [Fe/H] range. We also compared the abundance
patterns of individual program stars with the average abundance pattern of
metal-poor stars, and find only one chemically peculiar object with abundances
of at least two elements (other than C and N) showing deviations larger than
0.5dex. The distribution of [Sr/Ba] versus [Ba/H] agrees that an additional
nucleosynthesis mechanism is needed aside from a single r-process. Two program
stars with extremely low abundances of Sr and Ba support the prospect that both
main and weak r-process may have operated during the early phase of Galactic
chemical evolution. The distribution of [C/N] shows that there are two groups
of carbon-normal giants with different degrees of mixing. However, it is
difficult to explain the observed behavior of the [C/N] of the
nitrogen-enhanced unevolved stars based on current data.
