  We analyse the effects on the predictions for the microlensing searches
toward the Galactic bulge coming from the fact that not all the stars monitored
belong to the bulge itself, but that a non--negligible fraction of them
actually are in the Galactic disk.
  The different distribution and motions of these disk stars make their
associated microlensing rates and event duration distributions to be quite
different from those of the bulge stars. We discuss the uncertainties in these
predictions associated to the modeling of the Galactic components and the main
implications resulting from the inclusion of this second source population.
