  The analysis of the first two years of OGLE data revealed 9 microlensing
events of the galactic bulge stars, with the characteristic time scales in the
range $ 8.6 < t_0 < 62 $ days, where $ t_0 = R_E / V $. The optical depth to
microlensing is larger than $ ( 3.3 \pm 1.2 ) \times 10^{-6}$, in excess of
current theoretical estimates, indicating a much higher efficiency for
microlensing by either bulge or disk lenses. We argue that the lenses are
likely to be ordinary stars in the galactic bar, which has its long axis
elongated towards us. A relation between $ t_0 $ and the lens masses remains
unknown until a quantitative model of bar microlensing becomes available. At
this time we have no evidence that the OGLE events are related to dark matter.
The geometry of lens distribution can be determined observationally when the
microlensing rate is measured over a larger range of galactic longitudes, like
$ -10^o < l < +10^o $, and the relative proper motions of the galactic bulge
(bar) stars are measured with the HST.
