Python toolkit for calculating stellar limb darkening profiles and model-specific coefficients using the stellar atmosphere spectrum library by Husser et al. (2013). Described in Parviainen & Aigrain, MNRAS 453, 3821–3826 (2015).
These changes allow one to directly input samples from the posterior distributions of stellar parameters (teff, logg, and feh) instead of assuming Gaussianity and using a single value & uncertainty.
These changes allow one to directly input samples from the posterior distributions of stellar parameters (teff, logg, and feh) instead of assuming Gaussianity and using a single value & uncertainty.