Luminosities of cool stars

Planetary sizes and bulk compositions rely fundamentally on the stellar masses and radii. For the vast majority of stars, these parameters cannot be directly measured and must be inferred from temperature and luminosity. Therefore, reliable stellar luminosities are essential for a proper characterisation of the planetary companions. Once the flux of a star in multiple passbands (from UV to mid-IR) is known, one can produce a low-resolution spectrum or spectral energy distribution (SED) and derive empirically the bolometric luminosity from it. We did this in Cifuentes et al. (2020) on almost 2500 cool stars. We determined the average values of very important astrophysical parameters, including colours, absolute magnitudes, luminosities, temperatures, masses and radii.