  The measurements of the possible gravitational microlensing events are
analysed with a simple yet accurate disc--halo model of the Milky Way Galaxy.
This comprises a luminous exponential disc embedded in a flattened dark matter
halo with density varying like ${\rm distance}^{-1.8}$. Including a disc has
the important effect of lowering the implied masses of the dark matter objects.
For the possible detection reported by Alcock et al (1993), the inferred mass
of the lens lies in the range $\sim 0.01 - 0.15 M_\odot$. The candidate events
of Aubourg et al (1993) have slightly larger implied masses of $\sim 0.025 -
0.35\ M_\odot$ and $\sim 0.03 - 0.45\ M_\odot$ respectively. These are
consistent with the deflecters being either brown dwarfs or low mass stars. If
there is no disc dark matter and the halo is completely composed of baryonic
dark objects of typical mass $ \sim 0.08\ M_\odot$, then the monitoring of $1.8
\times 10^6$ stars in the Large Magellanic Cloud will provide at least $8-9$
detections a year, in the limit of $100 \%$ efficiency.
