  The habitable zone for exomoons with Earth-like properties is a non-trivial
manifold, compared to that of Earth-like exoplanets. The presence of tidal
heating, eclipses and planetary illumination in the exomoon energy budget
combine to produce both circumstellar and circumplanetary habitable regions.
Analytical calculations suggest that the circumplanetary habitable region is
defined only by an inner edge (with its outer limits determined by orbital
stability). Subsequent calculations using 1D latitudinal climate models
indicated that the combined effect of eclipses and ice-albedo feedback can
produce an outer edge to the circumplanetary habitable zone. But is this outer
edge real, or an artefact of the climate model's relative simplicity?
  We present an upgraded 1D climate model of Earth-like exomoon climates,
containing the carbonate-silicate cycle and viscoelastic tidal heating. We
conduct parameter surveys of both the circumstellar and circumplanetary
habitable zones, and we find that the outer circumplanetary habitable edge
remains provided the moon's orbit is not inclined relative to that of the
planet. Adding the carbonate-silicate cycle pushes the circumplanetary
habitable zone outward, by allowing increases in atmospheric partial pressure
of carbon dioxide to boost the greenhouse effect. Viscoelastic tidal heating
widens the habitable zone compared to standard, fixed-Q models. Weakening the
tidal heating effect due to melting allows moons to be habitable at higher
eccentricity, and pushes the inner circumstellar and circumplanetary habitable
zone boundary inward.
