  Gas giant planets are far easier than terrestrial planets to detect around
other stars, and are thought to form much more quickly than terrestrial
planets. Thus, in systems with giant planets, the late stages of terrestrial
planet formation are strongly affected by the giant planets' dynamical
presence. Observations of giant planet orbits may therefore constrain the
systems that can harbor potentially habitable, Earth-like planets. We present
results of 460 N-body simulations of terrestrial accretion from a disk of Moon-
to Mars-sized planetary embryos. We systematically vary the orbital semimajor
axis of a Jupiter-mass giant planet between 1.6 and 6 AU, and eccentricity
between 0 and 0.4. We find that for Sun-like stars, giant planets inside
roughly 2.5 AU inhibit the growth of 0.3 Earth-mass planets in the habitable
zone. If planets accrete water from volatile-rich embryos past 2-2.5 AU, then
water-rich habitable planets can only form in systems with giant planets beyond
3.5 AU. Giant planets with significant orbital eccentricities inhibit both
accretion and water delivery. The majority of the current sample of extra-solar
giant planets appears unlikely to form habitable planets.
