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We use Monte Carlo simulations to estimate the number of extrasolar planetsthat are directly detectable in the solar-neighborhood using current andforthcoming high-contrast imaging instruments. Our calculations take intoaccount the important factors that govern the likelihood for imaging a planet,including the statistical properties of nearby stars, correlations between starand planet properties, observational effects, and selection criteria. Weconsider several different ground-based surveys and express the resultingyields as a function of stellar mass. Selecting targets based on their youth,visual brightness, and proximity to the Sun, we find that strong correlationsbetween star mass and planet properties are required to reproduce high-contrastimaging results to date. Using the most recent empirical findings for theoccurrence rate of planets from RV surveys, our simulations indicate thatextrapolation of the Doppler planet population to separations accessible tohigh-contrast instruments provides excellent agreement between simulations andobservations using present-day contrast levels. In addition to beingintrinsically young and bright to serve as their own beacon for AO correction,A-stars have a high planet occurrence rate and propensity to form massiveplanets in wide orbits, making them ideal targets. The same effects responsiblefor creating a multitude of detectable planets around massive stars conspire toreduce the number orbiting low-mass stars. However, in the case of a youngstellar cluster, MK-stars can dominate the number of detections because of anobservational bias related to small number statistics. The degree to whichlow-mass stars produce the most detections in this special case depends uponformation mechanism. [Abridged]

Estimates of the Planet Yield from Ground-Based High-Contrast Imaging Observations as a Function of Stellar Mass