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Most of our knowledge of planets orbiting nearby stars comes from Dopplersurveys. For spaced-based, high-contrast imaging missions, nearby stars withDoppler-discovered planets are attractive targets. The known orbits tellimaging missions where and when to observe, and the dynamically-determinedmasses provide important constraints for the interpretation of planetaryspectra. Quantifying the set of planet masses and orbits that could have beendetected will enable more efficient planet discovery and characterization. Weanalyzed Doppler measurements from Lick and Keck Observatories collected by theCalifornia Planet Survey. We focused on stars that are likely targets for threespace-based planet imaging mission concepts studied by NASA--WFIRST-AFTA,Exo-C, and Exo-S. The Doppler targets are primarily F8 and later main sequencestars, with observations spanning 1987-2014. We identified 76 stars withDoppler measurements from the prospective mission target lists. We developed anautomated planet search and a methodology to estimate the pipeline completenessusing injection and recovery tests. We applied this machinery to the Dopplerdata and computed planet detection limits for each star as a function of planetminimum mass and semi-major axis. For typical stars in the survey, we aresensitive to approximately Saturn-mass planets inside of 1 AU, Jupiter-massplanets inside of ~3 AU, and our sensitivity declines out to ~10 AU. For thebest Doppler targets, we are sensitive to Neptune-mass planets in 3 AU orbits.Using an idealized model of Doppler survey completeness, we forecast theprecision of future surveys of non-ideal Doppler targets that are likelytargets of imaging missions.

Limits on Planetary Companions from Doppler Surveys of Nearby Stars