Stellar radius as a function of the stellar mass. The sample includes stars with interferometric measurements of their radii from BO12 and von Braun et al. (2014) as well as low-mass eclipsing binaries from Hartman et al. (2014, Table 5). The best fit is also shown. A 3σ clipping procedure was used to remove outliers. Upper panel: differences between the radius derived with our fit and the radius given in the literature. Median errors in radius (not shown in the plot) are of about 0.006 R_⊙.