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Models of our galaxy based on dynamical observations predict a spheroidcomponent much heavier than accounted for by direct measurements of star countsand high velocity stars. If, as first suggested by Caldwell and Ostriker, thisdiscrepancy is due to a large population of faint low-mass stars or darkobjects in the spheroid, the spheroid could be responsible for microlensingevents for sources in the Large Magellanic Cloud (LMC). We show that, althoughthe rate of events is lower than predicted by a galactic halo made ofmicrolensing objects, it is still significant for EROS/MACHO observations.Because of the different matter distributions in the halo and spheroidcomponents, a comparison between microlensing event rates in the LMC, futuremeasurements of microlensing in the galactic bulge and, possibly, in M31 canprovide information about the amounts of dark objects in the different galacticcomponents. If the EROS/MACHO collaborations find a deficiency with respect totheir halo expectation, when more statistics are available, their detectedevents could be interpreted as coming from spheroid microlenses, allowing for agalactic halo composed entirely of non-baryonic dark matter.Comment: 12 pages, CERN-TH.7127/9

Can EROS and MACHO be detecting the galactic spheroid instead of the galactic halo?