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tokens: data point density of a photometric LC (i.e. order of several thousands). However, in order to obtain a more realistic error value for q , the mass function is taken into account using the P orb and K 1 values and their errors: where M 1 , M 2 , K 1 , i , and P orb are explained in Table 1 and G is the gravitational constant. Following the error propagation method and assuming M 1 = 1.6 M ⊙ , then according to the definition of mass ratio (Table 1 ), the error of q is derived as 0.0031, which is adopted as the final value. The parameters of the set (c) were calculated using the software A BS P AR EB ( Liakos 2015 ) in mode 2 and they have the usual meaning. In Fig. 6 , we show the photometric model on one LC and the three-dimensional (3D) Roche geometry representation of the system, while in Fig. 7 (upper and middle panels) and Fig. 8 we illustrate the SC data and their residuals after the subtraction of the theoretical LCs for the two data sets. Fig. 6. Upper panel : theoretical (solid line) over observed (points) LC for KIC 8553788. Lower panel : 3D representation of the Roche geometry of the system at orbital phase 0.75. Fig. 7. Upper panel : short cadence LCs of Q5 for KIC 8553788. Middle panel : LC residuals after the subtraction of the binary models. Bottom panel : LC residuals after the subtraction of the pulsation model. Fig. 8. Upper panel : short cadence LCs of Q14 for KIC 8553788. Bottom panel : LC residuals after the subtraction of the binary models. During the modelling of the individual LCs, it was noticed that the spots migrate from one day to another; although this is a by-product result and a detailed study is not an aim of the present paper, their parameters are listed in Table B.1 . Moreover, in the same appendix, plots are given showing the location changes of the spots as well as their location on the surface of the secondary component on the first and the last days of each data set (Figs. B.1 – B.3 ). The reliability of the solution, especially for the extremely low value of the mass ratio, may be checked in the future using the RVs of the secondary component. However, it should to be noted that according to Kallrath Milone ( 1999 , their Sect. 4.1.1.1) the photometric mass ratio can be determined with great confidence for lobe-filling or overcontact systems when at least one light curve and one RV curve exist. Moreover, another useful and recent example regarding the reliability of the “ q -search” method concerns the semidetached systems KIC 10581918 and KIC 10619109. Liakos (2017) determined their mass ratio values based only on their Kepler LCs and without any use of RVs. These photometric values of q were later seen to be in very close agreement with the spectroscopically determined ones of Matson et al. (2017) . Concluding, KIC 8553788 was found to be in a semi-detached state, with the less massive and cooler component filling its Roche lobe, and to have a very low mass ratio of 0.043. Its primary component is a