Seismic mass vs. radius from grid modelling (filled circles) and direct computations from scaling relations (open circles) based on ν_max and Δν_cor (from Eq. (4)) as seismic input. Symbol colours are the same as in Fig. 10. Also plotted are BaSTI isochrones (dotted, dashed, and dashed-dotted lines) for solar metallicity in the top panel and [Fe/H] = 0.26 in the bottom panel with the numbers indicating the age of the isochrones as well as a number of eclipsing binaries (red squares), with the labels indicating: Aa → WOCS23009 A; Ba, Bb → WOCS24009 A & B; Ca, Cb → WOCS40007 A & B; Da, Db → V18 A & B; Ea, Eb → V20 A & B; Fa → V80 A. The inset in the top panel zooms onto the position of the primary component of WOCS40007 (Ca). The bottom panel shows the star’s position in the HR-diagram along with a 3 (dotted line) and 10 Gyr (dashed line) BaSTI isochrone for NGC 6791 and NGC 6819, respectively.