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