  KIC 5359678 is a 6.231-d period F-type eclipsing binary system whose
component stars both show starspot activity. It was observed by the Kepler
satellite in long cadence for the full four-year duration of the mission. Wang
et al (2021) obtained radial velocity measurements of the two stars and
analysed these plus the Kepler data to study their spot activity and measure
their physical properties, but left several questions unanswered. We have
performed an independent analysis and determined the masses (1.252 +/- 0.018
and 1.065 +/- 0.013 Msun) and radii (1.449 +/- 0.012 and 1.048 +/- 0.017 Rsun)
of the stars to high precision. The distance we find to the system is slightly
shorter than that from Gaia EDR3 for unknown reason(s). We also investigated
the precision of the numerical integration applied to the model light curve to
match the 1765-s sampling cadence of the Kepler observations. We found that
ignoring this temporal smearing leads to biased radius measurements for the
stars: that for the primary is too small by 4 sigma and that for the secondary
is too large by 10 sigma. Doubling the sampling rate of the model light curve
is sufficient to remove most of this bias, but for precise results a minimum of
five samples per observed datapoint is required.
