Simple schematic of the model pipeline. The surface incoming flux is first computed in order to derive the surface temperature based on the ephemeris, the Mars albedo mosaic from Christensen et al. (2001), the shape model of the targeted moon, and its albedo. The self-heating is computed iteratively after a first run of the thermal model until the convergence is reached, reinjecting the previous estimation to compute the new surface temperature. The thermal model takes the grain size D_g, the surface porosity p and density ρ, and the non-porous thermal conductivity k_m and specific heat C_p as inputs. Eventually the surface thermal emission is computed for a rough surface knowing the single scattering albedo (SSA) ϖ; the surface Hapke’s average slope angle $\overline{\theta }$; the opposition effect amplitude B₀ and angular width parameter h_s; the phase function asymmetry parameter b; and the geometry of observation regrouping i, e, and ϕ for the incidence, observation, and phase angle, respectively. This thermal emission is to be used as a reference to remove the emission component in the spectra.