are presented here for the benefit of those who can share the task of characterising these binary systems and as a useful indicator of the number and properties of long-period eclipsing binaries that will be found in future large-scale photometric surveys.

Analysis
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Note that where we refer to the primary and secondary stars in the following description (star 1 and 2, respectively) these labels refer to the star eclipsed during the deeper and shallower eclipses in the K2 light curve, respectively, irrespective of the stars’ effective temperatures, masses, radii, etc.

Target selection
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Targets were identified by visual inspection of the detrended light curves generated by the [k2sff]{} algorithm [@2014PASP..126..948V]. We downloaded the light curve data from the Mikulski Archive for Space Telescopes[^3] (MAST) and used a simple script to plot the data for each system while making a note of any stars showing eclipse-like features in the light curve at least 5% deep and with orbital periods $P\ga 5.5$ days. We excluded stars from our list with a strong ellipsoidal effect in the light curve, i.e., a quasi-sinusoidal variation in flux with two maxima per orbital cycle due to the gravitational distortion of the stars in a close 