Rates for Color-shifted Microlensing Events

If the objects responsible for gravitational microlensing (ML) of Galactic-bulge stars are faint dwarfs, then blended light from the lens will distort the shape of the ML light curve and shift the color of the observed star during the event. The resolution in current surveys is not accurate enough to observe this effect, but it should be detected with frequent and precise followup observations. We calculate the expected rates for ML events where the shape distortions will be observable by such followup observations, assuming that the lenses are ordinary main-sequence stars in a bar and in the disk. We study the dependence of the rates for color-shifted (CS) events on the frequency of followup observations and on the precision of the photometry for a variety of waveband pairings. We find that for hourly observations in $B$ and $K$ with typical photometric errors of 0.01 mag, 28% of the events where a main-sequence bulge star is lensed, and 7% of the events where the source is a bulge giant, will give rise to a measurable CS at the 95% confidence level. For observations in $V$ and $I$, the fractions become 18% and 5%, respectively, but may be increased to 40% and 13% by improved photometric accuracy and increased sampling frequency. We outline how the mass, distance, and transverse speed of the lens can be obtained, giving examples of typical errors. We discuss how CS events can be distinguished from events where the source is blended with a binary companion.