  Once a star leaves the main sequence and becomes a red giant, its Habitable
Zone (HZ) moves outward, promoting detectable habitable conditions at larger
orbital distances. We use a one-dimensional radiative-convective climate and
stellar evolutionary models to calculate post-MS HZ distances for a grid of
stars from 3,700K to 10,000K (~M1 to A5 stellar types) for different stellar
metallicities. The post-MS HZ limits are comparable to the distances of known
directly imaged planets. We model the stellar as well as planetary atmospheric
mass loss during the Red Giant Branch (RGB) and Asymptotic Giant Branch (AGB)
phases for super-Moons to super-Earths. A planet can stay between 200 million
years up to 9 Gyr in the post-MS HZ for our hottest and coldest grid stars,
respectively, assuming solar metallicity. These numbers increase for increased
stellar metallicity. Total atmospheric erosion only occurs for planets in
close-in orbits. The post-MS HZ orbital distances are within detection
capabilities of direct imaging techniques.
