K)$ relation in this regime. The empirical colour – temperature relations we have used are valid over the approximate range T$_{\rm eff} = 3450$K to 8600K. Our results may be biased in systems where one of the stars has an effective temperature near either of these limits because we exclude trial solutions with any T$_{\rm
eff, i}$ value outside this range. Between these limits we use uniform priors on the values of T$_{\rm eff, i}$. We also use uniform priors for g$^{\prime}_{0, 1}$ and g$^{\prime}_{0, 2}$.

In systems where there is evidence of third light from the light curve analysis and the star appears unresolved in sky survey images we compare solutions with a uniform prior on g$^{\prime}_{0, 3}$ and with a constraint on g$^{\prime}$$_{0, 3}$ assuming that the third light is due to a main-sequence star at the same distance as the eclipsing binary star. We use the stellar model from the Dartmouth stellar evolution database [@2008ApJS..178...89D] for solar composition to define the limits of the main sequence in the T$_{\rm eff}$ – $M_{\rm g^{\prime}}$ plane, where $M_{\rm g^{\prime}}$ is the absolute magnitude of star $i$ in the g$^{\prime}$ band. For each trial solution we use interpolation between these 