  This report summarises progress made in estimating the local density of dark
matter ($\rho_{\mathrm{DM,\odot}}$), a quantity that is especially important
for dark matter direct detection experiments. We outline and compare the most
common methods to estimate $\rho_{\mathrm{DM,\odot}}$ and the results from
recent studies, including those that have benefited from the observations of
the ESA/Gaia satellite. The result of most local analyses coincide within a
range of $\rho_{\mathrm{DM,\odot}} \simeq \text{0.4--0.6}\,\mathrm{GeV/cm^3} =
\text{0.011--0.016}\,\mathrm{M_\odot / pc^3}$, while a slightly lower range of
$\rho_{\mathrm{DM,\odot}} \simeq \text{0.3--0.5}\,\mathrm{GeV/cm^3} =
\text{0.008--0.013}\,\mathrm{M_\odot / pc^3}$ is preferred by most global
studies. In light of recent discoveries, we discuss the importance of going
beyond the approximations of what we define as the Ideal Galaxy (a steady-state
Galaxy with axisymmetric shape and a mirror symmetry across the mid-plane) in
order to improve the precision of $\rho_{\mathrm{DM,\odot}}$ measurements. In
particular, we review the growing evidence for local disequilibrium and broken
symmetries in the present configuration of the Milky Way, as well as
uncertainties associated with the Galactic distribution of baryons. Finally, we
comment on new ideas that have been proposed to further constrain the value of
$\rho_{\mathrm{DM,\odot}}$, most of which would benefit from Gaia's final data
release.
