Determining the local dark matter density with LAMOST data
  Measurement of the local dark matter density plays an important role in both
Galactic dynamics and dark matter direct detection experiments. However, the
estimated values from previous works are far from agreeing with each other. In
this work, we provide a well-defined observed sample with 1427 G \& K type
main-sequence stars from the LAMOST spectroscopic survey, taking into account
selection effects, volume completeness, and the stellar populations. We apply a
vertical Jeans equation method containing a single exponential stellar disk, a
razor thin gas disk, and a constant dark matter density distribution to the
sample, and obtain a total surface mass density of $\rm {78.7 ^{+3.9}_{-4.7}\
M_{\odot}\ pc^{-2}}$ up to 1 kpc and a local dark matter density of
$0.0159^{+0.0047}_{-0.0057}\,\rm M_{\odot}\,\rm pc^{-3}$. We find that the
sampling density (i.e. number of stars per unit volume) of the spectroscopic
data contributes to about two-thirds of the uncertainty in the estimated
values. We discuss the effect of the tilt term in the Jeans equation and find
it has little impact on our measurement. Other issues, such as a
non-equilibrium component due to perturbations and contamination by the thick
disk population, are also discussed.
