  Moons orbiting extrasolar planets are the next class of object to be observed
and characterized for possible habitability. Like the host-planets to their
host-star, exomoons have a limiting radius at which they may be gravitationally
bound, or the Hill radius. In addition, they also have a distance at which they
will become tidally locked and therefore in synchronous rotation with the
planet. We have examined the flux phase profile of a simulated, hypothetical
moon orbiting at a distant radius around the confirmed exoplanets mu Ara b, HD
28185 b, BD +14 4559 b, and HD 73534 b. The irradiated flux on a moon at it's
furthest, stable distance from the planet achieves it's largest flux gradient,
which places a limit on the flux ranges expected for subsequent (observed)
moons closer in orbit to the planet. We have also analyzed the effect of
planetary eccentricity on the flux on the moon, examining planets that traverse
the habitable zone either fully or partially during their orbit. Looking solely
at the stellar contributions, we find that moons around planets that are
totally within the habitable zone experience thermal equilibrium temperatures
above the runaway greenhouse limit, requiring a small heat redistribution
efficiency. In contrast, exomoons orbiting planets that only spend a fraction
of their time within the habitable zone require a heat redistribution
efficiency near 100% in order to achieve temperatures suitable for
habitability.
  Meaning, a planet does not need to spend its entire orbit within the
habitable zone in order for the exomoon to be habitable. Because the applied
systems are comprised of giant planets around bright stars, we believe that the
transit detection method is most likely to yield an exomoon discovery.
