Another Channel to detect Close-in Binary Companions via Gravitational Microlensing

Gaudi & Gould (1997) showed that close companions of remote binary systems can be efficiently detected by using gravitational microlensing via the deviations in the lensing light curves induced by the existence of the lens companions. In this paper, we introduce another channel to detect faint close-in binary companions by using microlensing. This method utilizes a caustic-crossing binary lens event with a source also composed of binary stars, where the companion is a faint star. Detection of the companion is possible because the flux of the companion can be highly amplified when it crosses the lens caustic. The detection is facilitated since the companion is more amplified than the primary because it, in general, has a smaller size than the primary, and thus experiences less finite source effect. The method is extension of the previous one suggested to detect close-in giant planets by Graff & Gaudi (2000) and Lewis & Ibata (2000) and further developed by Ashton & Lewis (2001). From the simulations of realistic Galactic bulge events, we find that companions of K-type main sequence or brighter can be efficiently detected from the current type microlensing followup observations by using the proposed method. We also find that compared to the method of detecting lens companions for which the efficiency drops significantly for binaries with separations $\lesssim 0.2$ of the angular Einstein ring radius, the proposed method has an important advantage of being able to detect companions with substantially smaller separations down to order of 0.01 \theta_E.