  From analytical studies of tidal heating, eclipses and planetary
illumination, it is clear that the exomoon habitable zone (EHZ) - the set of
moon and host planet orbits that permit liquid water on an Earthlike moon's
surface - is a manifold of higher dimension than the planetary HZ.
  This paper outlines the first attempt to produce climate models of exomoons
which possess all the above sources and sinks of energy. We expand on our
previous 1D latitudinal energy balance models (LEBMs), which follow the
evolution of the temperature on an Earthlike moon orbiting a Jupiterlike
planet, by adding planetary illumination.
  We investigate the EHZ in four dimensions, running two separate suites of
simulations. The first investigates the EHZ by varying the planet's orbit,
keeping the moon's orbit fixed, to compare the EHZ with planetary habitable
zones. In general, planetary illumination pushes EHZs slightly further away
from the star.
  Secondly, we fix the planet's orbit and vary the moon's orbit, to investigate
the circumplanetary inner habitable edge. We demonstrate that an outer edge can
exist due to eclipses (rather than merely orbital stability), but this edge may
be pushed outwards when the effect of the carbonate-silicate cycle is taken
into account.
