MICROLENSING OF DISK SOURCES

We analyze the effects on the predictions for the microlensing searche s toward the Galactic bulge arising from the fact that not all the sta rs monitored belong to the bulge itself, but a nonnegligible fraction of them are actually in the Galactic disk. The different distribution and motions of these disk stars make their associated microlensing rat es and event duration distributions quite different from those of the bulge stars. We discuss the uncertainties in these predictions associa ted with the modeling of the Galactic components and the main implicat ions resulting from the inclusion of this second source population.