K-Band Microlensing of the Inner Galaxy

Microlensing searches toward the inner galaxy $(|l|,|b|leq 22.hskip-2pt'5)$ have several major advantages. First, the event rate is strongly dominated by bulge-bulge lensing events where both the source and lens lie in the bulge. Second, these bulge-bulge events have very short time scales $t_esim 2,$days and are therefore easily distinguished from the less frequent and much longer bulge-disk and disk-disk events. Third, since the optical depth is similar to that at higher impact parameters, while the events are shorter, the event rate is high $Gammasim 3 imes 10^{-7} m day^{-1}$. Fourth, because the Einstein rings are small, $r_esim 5 imes 10^{12},$cm, and the source stars are large $r_sgsim 10^{12},$cm, the lens will transit the face of the source for a significant fraction $(sim 20%)$ of events. For these transit events it will often be possible to measure a second lens parameter, the angular Einstein radius (or proper motion). In addition to the bulge-bulge events, the optical depth of the disk is $sim 7$ times larger toward the inner Galaxy than toward Baade's Window. A microlensing search toward the inner Galaxy can be carried out by making frequent $(sim4, m day^{-1})$ K band images of a large area $sim 0.5, m deg^2$ to a depth of $Ksim 16$, and hence requires either a $1024^2$ infrared array on a dedicated 2m telescope or four such arrays on a 1m telescope.