provides a guide to the characteristics of binaries in which lensing will be important. It shows, for example, that common envelope systems are more likely to be affected by lensing. We note, however, that for individual systems, the effects must be computed separately. This is because the radius of the white dwarf may larger or smaller; finite source size effects can be important; and, the range of values of R$_{E}$/R$_{WD}$ encompassed in a single panel correspond to light curves with a range of properties. 

The systems shown in the top panel Figure 4 all have R$_{E}$/R$_{WD}$ > 2 . In these cases we expect the lensing signature to be clear and for the gravitational mass to be potentially measurable. In this regime, many of the events will look like “anti-transits”. For the sake of clarity, we note that we are using the term “event” to refer to the light curve deviation associated with a single passage of the white dwarf in front of its companion star. Just as with ordinary transits, these events repeat periodically, and the ability to detect repetitions increases confidence in the physical interpretation. Figure 15 of Sahu & Gilliland (2003) shows the lensing signature for a white dwarf of 0 . 6 M ⊙ located 1 AU form a solar-type star. The light curve exhibits what we have referred to here as an anti-transit, with a significance in the Kepler data greater than 100 σ . The significance of some of the events generated by systems in the top panel of Figure 4 will be even higher, and some of these events may therefore be detectable even from the ground. 

Figure 14 of Sahu & Gilliland (2003) shows that even with R$_{E}$/R$_{WD}$ = 0 . 8, an anti- transit can be clearly detected. The second panel shows systems with 0 . 8 < R$_{E}$/R$_{WD}$ < 2 . Some of these events will be anti-transits as well; lensing should be recognizable in many. Those that are not pure anti-transits are likely to exhibit detectable deviations from base- line that exhibit significant signatures of lensing. From the perspective of studying white dwarfs and the end states of mass transfer, events from systems in these top two panels are important, because lensing provides a unique way to measure the white dwarf mass. From the perspective of Kepler’s primary goal of identifying transits by terrestrial planets, these events are also important, because the degeneracy with transits by planet-mass lenses is clearly broken. 

The third panel shows systems with 0 . 4 < R$_{E}$/R$_{WD}$ < 0 . 8 Some of these may also produce clear signatures of lensing. Others, particularly when the white dwarf is young and still larger than suggested by the mass/radius relation, may produce events that look like ordinary transits. In addition, a significant subset of the events generated by this group will exhibit some level of cancellation between diminuation due to transit and magnification caused by lensing. That is, some systems shown in the third panel generate events (combi- nations of transit and lensing) may not be detectable by Kepler. This eliminates our ability to identify and study these white dwarfs, but it also eliminates the possibility that these 

