Simulation of exoplanet spectra - first steps

The aim of my PhD work is to obtain information on the atmospheres of terrestrial planets orbiting in the inner part of the habitable zone of M-dwarf stars. This will be done by the help of radiative transfer line by line (lbl) models to calculate infrared emission and transmission spectra of the atmospheres applied on case studies for cloudy and cloud free, different gravity strengths and variable orbital distances to the inner habitable zone. For the first approach I simulated some infrared spectra of Earth like planets with a radiative transfer model to see spectra according to my expectations. Additionally, I want to see how they differ from a normal Earth spectrum. After that, the next step is the investigation of Jacobians, i.e. essentially the difference of a calculated spectrum and a similar spectrum with a perturbed molecule included or with a different temperature profile, to illustrate the request of an unknown molecule concentration on exoplanets to the radiative transfer