The atmospheric model that we fit, using Bayesian nested sampling, to the MIRI LRS eclipse spectrum of LTT 1445A b. The top half of the figure is the full forward model and the bottom half details the atmospheric and surface component. The output is eclipse depth vs. wavelength, which can be compared to MIRI spectra. Inputs (black dashed box) include R_p/R_⋆, the stellar effective temperature (T_eff), and seven inputs to the atmosphere/surface model. The five atmosphere/surface model inputs in blue text are specific to the atmosphere and are not considered in our bare-rock fit to the MIRI data (Section 2.3).