Eccentricity proxy versus orbital period of Sample 2G-A eclipsing binaries (well-detached and without ellipsoidal component) that are brighter than 12 mag in G and that have parallax uncertainties better than 15%, a corrected BP+RP flux excess factor lower than 0.5, and global rankings higher than 0.6. The colour of each marker is related to the depth of the secondary eclipse (in G magnitude) according to the colour-scale to the right of the figure, with ratios larger than 0.45 rendered in black. The size of each marker is proportional to the secondary over primary depth ratio. The vertical line segments indicate the 1σ uncertainty of the eccentricity proxy. For clarity, this error has only been drawn on the small eccentricity side. The blue dashed line is Eq. (4.4) from Mazeh (2008) with E = 0.98, A = 3.25, B = 6.3, and C = 0.23. The five sources above this line that are highlighted with open diamonds have their light curves displayed in Fig. 41.