Next exoplanet missions such as CHEOPS, TESS, K2 and PLATO will largely increase our knowledge on exoplanets, increasing the population of known planets as well as getting a better characterization of their parameters. These observations will give us semimajor axis, radius (and mass) of the planets and information about the parent star. With this motivation, we calculated an atmospheric grid for hot mini-Neptune and giant planets, that links these astrophysical observable parameters with the atmospheric composition and spectral features expected in transmission and emission spectra as observed with future instrumentation.
For calculating the composition we calculate disequilibrium chemistry for planets with temperatures between 2700K and 700K and explore the effect of empirical model parameters on the results. We use a line by line radiative transfer code (SAO98) to generate the observable spectra. Our models explore the detectable atmospheric features for a wide range of stellar types from F to M for distances between 0.01AU and 0.1 AU.
Our link between the observed parameters and atmospheric characterization can provide information for the best targets to further follow up with spectroscopy. Our grid can also be applied to characterize exoplanet atmospheres and serves as a reference to interpret atmospheric retrieval analysis results.