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The bulge is a region of the Galaxy which is of tremendous interest forunderstanding Galaxy formation. However, measuring photometry and kinematics init raises several inherent issues, like high extinction in the visible andsevere crowding. Here we attempt to estimate the problem of the visibility ofthe bulge at optical wavelengths, where large CCD mosaics allow to easily coverwide regions from the ground, and where future astrometric missions areplanned. Assuming the Besancon Galaxy model and high resolution extinctionmaps, we estimate the stellar density as a function of longitude, latitude andapparent magnitude and we deduce the possibility of reaching and measuringbulge stars. The method is applied to three Gaia instruments, the BBP and MBPphotometers, and the RVS spectrograph. We conclude that, while in the BBP mostof the bulge will be accessible, in the MBP there will be a small butsignificant number of regions where bulge stars will be detected and accuratelymeasured in crowded fields. Assuming that the RVS spectra may be extracted inmoderately crowded fields, the bulge will be accessible in most regions apartfrom the strongly absorbed inner plane regions, because of high extinction, andin low extinction windows like the Baades's window where the crowding is toosevere.Comment: 11 pages, 9 figures, accepted for publication in A&A, latex using A&A  macro

The visibility of the Galactic bulge in optical surveys. Application to the Gaia mission