  We present a catalog of 166 spectroscopically identified hot subdwarf stars
from LAMOST DR1, 44 of which show the characteristics of cool companions in
their optical spectra. Atmospheric parameters of 122 non-composite spectra
subdwarf stars were measured by fitting the profiles of hydrogen (H) and helium
(He) lines with synthetic spectra from non-LTE model atmospheres. Most of the
sdB stars scatter near the Extreme Horizontal Branch in the $T_{\rm
eff}-\log{g}$ diagram and two well defined groups can be outlined. A clustering
of He-enriched sdO stars appears near $T_{\rm eff}=45\,000$ K and $\log(g) =
5.8$. The sdB population separates into several nearly parallel sequences in
the $T_{\rm eff}-{\rm He}$ abundance diagram with clumps corresponding to those
in the $T_{\rm eff}-\log{g}$ diagram. Over $38\,000$ K (sdO) stars show
abundance extremes, they are either He-rich or He-deficient and we observe only
a few stars in the $ -1 < \log(y) < 0$ abundance range. With increasing
temperature these extremes become less prominent and the He abundance
approaches to $\log(y)\sim-0.5$. A unique property of our sample is that it
covers a large range in apparent magnitudes and galactic latitudes, therefore
it contains a mix of stars from different populations and galactic
environments. Our results are consistent with the findings of Hirsch (2009) and
we conclude that He-rich and He-deficient sdB stars ($\log(y) < 1$) probably
origin from different populations. We also find that most sdO and sdB stars lie
in a narrow strip in the luminosity and helium abundance plane, which suggests
that these atmospheric parameters are correlated.
