  We examine the most recent observational constraints arising from i)
small-scale and large-scale Galactic dynamical properties, ii) star counts at
faint magnitude and iii) microlensing experiments. From these constraints, we
determine the halo and disk stellar mass functions and stellar content down to
the bottom of the main sequence, which yields the normalization of the
halo/disk total stellar population, and we infer the contributions of
sub-stellar objects to the mass budget of the various Galactic regions.
  The consistent analysis of star counts and of the overall microlensing
observations in the Bulge are compatible with a small contribution of brown
dwarfs to the Galactic mass budget $\rho_{BD}/\rho_* \leq 0.2 $. However the
separate bulge/disk analysis based on the bulge clump giants is compatible with
a substantial population of disk brown dwarfs, $\Sigma_{BD}/\Sigma_*\leq 1 $.
More statistics of microlensing events towards the Galactic center and a better
determination of the velocity dispersions in the bulge should break this
degeneracy of solutions.
  For the halo, we show that a steep mass-function in the dark halo is excluded
and that low-mass stars and brown dwarfs represent a negligible fraction of the
halo dark matter, and thus of the observed events towards the LMC. The nature
of these events remains a puzzle and halo white dwarfs remain the least
unlikely candidates.
