in these cases and excluded the DENIS photometry from the fit – these cases are noted in Table \[TeffTable\].

Results
=======

The parameters derived from our analysis of the K2 light curves for each target are given in Tables \[ellcpar1\] and \[ellcpar2\]. The best fits to the K2 light curves are shown in Figs. \[lcfit1\], \[lcfit2\], \[lcfit3\] and \[lcfit4\]. The effective temperature estimates for the components of each system are given in Table \[TeffTable\]. In Table \[TrhoTable\] we give an estimate of the mean stellar density ($\rho_{\star}$) for the two stars in each eclipsing binary calculated using the following expression derived from Kepler’s third law. $$\mbox{$\rho_{\star}$} =
   \frac{3\mbox{M$_{\star}$}}{4\pi R_{\star}^3} =
   \frac{3\pi}{GP^2(1+q)}
    \left(\frac{a}{\mbox{R$_{\star}$}}\right)^3.$$ Here, $P$ and $a$ are the period and semi-major axis of the Keplerian orbit, and $q = M_\mathrm{c}/\mbox{$M_{\star}$}$ is the mass ratio for a companion with mass $M_\mathrm{c}$ to a star with mass $M_{\star}$ and radius $R_{\star}$. The value of $q$ was estimated by calculating the position of the stars in Fig. \[TeffDensity\] for various values of $q$ and then choosing the value which is consistent with the approximate masses inferred from the stellar evolution tracks shown in this figure.

![image](Figs/TeffDensity-eps-converted-to.pdf){width="99.00000%"}

Notes on individual objects \[notes\_sec\]
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