  The local density of dark matter is an important quantity. On the one hand,
its value is needed for dark matter direct detection searches. On the other
hand, a precise and robust determination of the local dark matter density would
help us learn about the shape of the dark matter halo of our Galaxy, which
plays an important role in dark matter indirect detection searches, as well as
in many studies in astrophysics and cosmology. There are different methods
available to determine the local dark matter density. Among them, it is common
to study either the vertical kinematics of a selected group of tracers or the
rotation curve of the Milky Way. Recent estimates of the local dark matter
density have used the precise observations conducted by the ESA/Gaia mission.
However, in spite of the quality of the data released by Gaia's observations,
different analyses of the local dark matter density produce dissimilar results.
After a brief review of the most common methods to estimate the local density
of dark matter, here we argue about different explanations for the
discrepancies in the results of recent analyses. We finish by presenting new
approaches that have been proposed in the literature and could help us improve
our knowledge of this important quantity.
