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We present an approach for utilizing astrometric orbit information to improvethe yield of planetary images and spectra from a follow-on direct detectionmission. This approach is based on the notion-strictly hypothetical-that if aparticular star could be observed continuously, the instrument would in timeobserve all portions of the habitable zone so that no planet residing thereincould be missed. This strategy could not be implemented in any realisticmission scenario. But if an exoplanet's orbit is known from astrometricobservation, then it may be possible to plan and schedule a sequence of imagingobservations that is the equivalent of continuous observation. A series ofimages-optimally spaced in time-could be recorded to examine contiguoussegments of the orbit. In time, all segments would be examined, leading to theinevitable detection of the planet. In this paper, we show how astrometricorbit information can be used to construct such a sequence. Using stars fromastrometric and imaging target lists, we find that the number of observationsin this sequence typically ranges from 2 to 7, representing the maximum numberof observations required to find the planet. The probable number ofobservations ranges from 1.5 to 3.1. This is a dramatic improvement inefficiency over previous methods proposed for utilizing astrometric orbits. Weexamine how the implementation of this approach is complicated and limited byoperational constraints. We find that it can be fully implemented for internalcoronagraph and visual nuller missions, with a success rate approaching 100%.External occulter missions will also benefit, but to a lesser degree.

Utilizing Astrometric Orbits to Obtain Coronagraphic Images