  The Kepler mission found hundreds of planet candidates within the habitable
zones (HZ) of their host star, including over 70 candidates with radii larger
than 3 Earth radii ($R_\oplus$) within the optimistic habitable zone (OHZ)
(Kane et al. 2016). These giant planets are potential hosts to large
terrestrial satellites (or exomoons) which would also exist in the HZ. We
calculate the occurrence rates of giant planets ($R_p =$~3.0--25~$R_\oplus$) in
the OHZ and find a frequency of $(6.5 \pm 1.9)\%$ for G stars, $(11.5 \pm
3.1)\%$ for K stars, and $(6 \pm 6)\%$ for M stars. We compare this with
previously estimated occurrence rates of terrestrial planets in the HZ of G, K
and M stars and find that if each giant planet has one large terrestrial moon
then these moons are less likely to exist in the HZ than terrestrial planets.
However, if each giant planet holds more than one moon, then the occurrence
rates of moons in the HZ would be comparable to that of terrestrial planets,
and could potentially exceed them. We estimate the mass of each planet
candidate using the mass-radius relationship developed by Chen & Kipping
(2016). We calculate the Hill radius of each planet to determine the area of
influence of the planet in which any attached moon may reside, then calculate
the estimated angular separation of the moon and planet for future imaging
missions. Finally, we estimate the radial velocity semi-amplitudes of each
planet for use in follow up observations.
