  Exomoons are expected to orbit gas giant exoplanets just as moons orbit solar
system planets. Tidal heating is present in solar system satellites and it can
heat up their interior depending on their orbital and interior properties. We
aim to identify a Tidally Heated Exomoon's (THEM) orbital parameter space that
would make it observable in infrared wavelengths with MIRI/JWST around
$\epsilon$ Eridani b. We study the possible constraints on orbital eccentricity
and interior properties that a successful THEM detection in infrared
wavelengths can bring. We also investigate what exomoon properties need to be
independently known in order to place these constraints. We use a coupled
thermal-tidal model to find stable equilibrium points between the tidally
produced heat and heat transported within a moon. For the latter, we consider a
spherical and radially symmetric satellite with heat being transported via
magma advection in a sub-layer of melt (asthenosphere) and convection in the
lower mantle. We incorporate uncertainties in the interior and tidal model
parameters to assess the fraction of simulated moons that would be observable
with MIRI. We find that a $2 R_{Io}$ THEM orbiting $\epsilon$ Eridani b with an
eccentricity of 0.02, would need to have a semi-major axis of 4 planetary
Roche-radii for 100% of the simulations to produce an observable moon. These
values are comparable with the orbital properties of gas giant solar system
satellites. We place similar constraints for eccentricities up to 0.1. We
conclude that if the semi-major axis and radius of the moon are known (eg. with
exomoon transits), tidal dissipation can constrain the orbital eccentricity and
interior properties of the satellite, such as the presence of melt and the
thickness of the melt containing sub-layer.
