Summary and Conclusion

Abstract

Almost a decade ago, we used this statement as motivation to approach the challenge of studying exoplanet host stars by using as few assumptions as possible. The use of interferometry to determine their diameters meets this challenge despite its being limited to nearby and bright stars and the fact that it is intrinsically a complicated method (Sect. 2.1). Imperfect accuracy and/or precision of the method due to calibration challenges as function of atmospheric conditions, consequent characterization of associated uncertainties, and random errors in limb-darkening corrections certainly appear to outweigh the caveats of any other method of determining stellar diameters, at least for single stars (Sect. 2.3).

In order to understand the planet, you need to understand its parent star.