Measuring the local matter density using Gaia DR2
  We determine the total dynamical matter density in the solar neighbourhood
using the second Gaia data release (DR2). The dynamical matter density
distribution is inferred in a framework of a Bayesian hierarchical model, which
accounts for position and velocity of all individual stars, as well as the full
error covariance matrix of astrometric observables, in a joint fit of the
vertical velocity distribution and stellar number density distribution. This
was done for eight separate data samples, with different cuts in observed
absolute magnitude, each containing about 25,000 stars. The model for the total
matter density does not rely on any underlying baryonic model, although we
assumed that it is symmetrical, smooth, and monotonically decreasing with
distance from the mid-plane. We infer a density distribution which is strongly
peaked in the region close to the Galactic plane ($\lesssim 60$ pc), for all
eight stellar samples. Assuming a baryonic model and a dark matter halo of
constant density, this corresponds to a surplus surface density of
approximately 5--9 M$_\odot$/pc$^2$. For the Sun's position and vertical
velocity with respect to the Galactic plane, we infer $Z_\odot = 4.76\pm 2.27$
pc and $W_\odot = 7.24\pm 0.19$ km/s. These results suggest a surplus of matter
close to the Galactic plane, possibly explained by an underestimated density of
cold gas. We discuss possible systematic effects that could bias our result,
for example unmodelled non-equilibrium effects, and how to account for such
effects in future extensions of this work.
