model isochrones to define limits to g$^{\prime}_{0, 3}$ assuming that the fainter star in the eclipsing binary is a main-sequence star, i.e., we reject solutions where the combination of T$_{\rm eff, 3}$, T$_{\rm eff, B}$, g$^{\prime}_{0, 3}$ and g$^{\prime}_{0, B}$ cannot be reproduced by two stars between the zero-age main sequence and terminal-age main-sequence in the T$_{\rm eff}$ – $M_{{\rm g}^{\prime}}$ plane, where $B = 1$ or 2 is the index for the star in the eclipsing binary that is fainter in the g$^{\prime}$-band. Systems where we adopted solutions including this constraint are noted with a $\star$ symbol in Table \[TeffTable\], together with the median and standard deviation of the model parameters derived using [emcee]{}.

Our method requires an estimate of the apparent g$^{\prime}$ magnitude. In cases where no such estimate is available from APASS9 we either use the SDSS g$^{\prime}$ magnitude or infer a value from the Tycho-2 B$_{\rm T}$ and V$_{\rm T}$ magnitudes using equation (6a) from @2011AJ....142..112B. In either case, we assign an nominal standard error of 0.5 magnitudes to this estimate. We also found for some stars that the magnitudes from the DENIS and 2MASS surveys were significantly different. In general, we used the 2MASS magnitudes 