KIC 11401845 eclipse timings

Light-curve synthesis shows that the binary star is a short-period detached system with a very low mass ratio of q=0.070 and filling factors of F_1_=45% and F_2_=99%. Multiple-frequency analyses were applied to the light residuals after subtracting the synthetic eclipsing curve from the observed data.

We detected 23 frequencies with signal-to-noise ratios larger than 4.0, of which the orbital harmonics (f_4_, f_6_, f_9_, f_15_) in the low-frequency domain may originate from tidally excited modes. For the high frequencies of 13.7-23.8day^-1^, the period ratios and pulsation constants are in the ranges of P_pul_/P_orb_=0.020-0.034 and Q=0.018-0.031days, respectively. These values and the position on the Hertzsprung-Russell diagram demonstrate that the primary component is a {delta} Sct pulsating star.