2000MNRAS.315...51W

Gravitational microlensing at cosmological distances is potentially a powerful tool for probing the mass functions of stars and compact objects in other galaxies. In the case of multiply imaged quasars, microlensing data have been used to determine the average microlens mass. However, the measurements have relied on an assumed transverse velocity for the lensing galaxy.

Since the measured mass scales with the square of the transverse velocity, published mass limits are quite uncertain. In the case of Q2237+0305 we have properly constrained this uncertainty. The distribution of light-curve derivatives allows a quantitative treatment of the relative rates of microlensing arising from proper motions of microlenses, the orbital stream motion of microlenses and the bulk galactic transverse velocity. By demanding that the microlensing rate arising from the motions of microlenses is the minimum that should be observed we determine lower limits for the average mass of stars and compact objects in the bulge of Q2237+0305. If microlenses are assumed to move in an orbital stream the lower limit ranges between 0.005 and 0.023M_☉, where the systematic dependence arises from the fraction of smooth matter and the size of photometric error assumed for the published monitoring data. However, if the microlenses are assumed to move according to an isotropic velocity dispersion then a larger lower limit of 0.019-0.11M_☉ is obtained. A significant contribution of Jupiter-mass compact objects to the mass distribution of the galactic bulge of Q2237+0305 is therefore ruled out unambiguously.