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Kepler's quest for other Earths need not end just yet: it remains capable ofcharacterizing cool Earth-mass planets by microlensing, even given its degradedpointing control. If Kepler were pointed at the Galactic bulge, it couldconduct a search for microlensing planets that would be virtuallynon-overlapping with ground-based surveys. More important, by combining Keplerobservations with current ground-based surveys, one could measure the"microlens parallax" \pi_E for a large fraction of the known microlensingevents. Such parallax measurements would yield mass and distance determinationsfor the great majority of microlensing planets, enabling much more precisestudy of the planet distributions as functions of planet and host mass,planet-host separation, and Galactic position (particularly bulge vs. disk). Inaddition, rare systems (such as planets orbiting brown dwarfs or black holes)that are presently lost in the noise would be clearly identified. In contrastto Kepler's current primary hunting ground of close-in planets, itsmicrolensing planets would be in the cool outer parts of solar systems,generally beyond the snow line. The same survey would yield a spectacularcatalog of brown-dwarf binaries, probe the stellar mass function in a uniqueway, and still have plenty of time available for asteroseismology targets.

Kepler Microlens Planets and Parallaxes