  The TRAPPIST-1 system is home to at least seven terrestrial planets and is a
target of interest for future James Webb Space Telescope (JWST) observations.
Additionally, these planets will be of interest to future missions making
observations in the ultraviolet (UV). Although several of these planets are
located in the traditional habitable zone, where liquid water could exist on
the surface, TRAPPIST-1h is interesting to explore as a potentially habitable
ocean world analog. In this study, we evaluate the observability of a
Titan-like atmosphere on TRAPPIST-1h. The ability of the JWST or a future UV
mission to detect specific species in the atmosphere at TRAPPIST-1h will depend
on how far each species extends from the surface. In order to understand the
conditions required for detection, we evaluate the input parameters used in
one-dimensional models to simulate the structure of Titan-like atmospheres.
These parameters include surface temperature and pressure, temperature profile
as a function of distance from the surface, composition of the minor species
relative to N 2, and the eddy diffusion coefficient. We find that JWST
simulated spectra for cloud- and haze-free atmospheres are most sensitive to
surface temperature, temperature gradients with altitude, and surface pressure.
The importance of temperature gradients in JWST observations shows that a
simple isothermal scale height is not ideal for determining temperature or
atmospheric mean molecular mass in transit spectra from exoplanet atmospheres.
We demonstrate that UV transmission spectra are sensitive to the upper
atmosphere, where the exobase can be used to approximate the vertical extent of
the atmosphere.
