A code for retrieving three-dimensional maps of exoplanets.
The code constructs 2-dimensional maps for each light given light curve, places those maps vertically in an atmosphere, runs radiative transfer to calculate emission from the planet over a latitude/longitude grid, and integrates over the grid (combined with the visibility function) to generate light curves. These light curves are compared against the input light curves behind MCMC to explore parameter space.
Ryan C. Challener ([email protected])
Emily Rauscher
Lucas Brefka
If you use this code in your work, please cite our paper. Thanks!
https://ui.adsabs.harvard.edu/abs/2021arXiv211008159C/abstract