We report the { \it Kepler } photometry of KIC 11401845 displaying multiperiodic pulsations , superimposed on binary effects .
Light-curve synthesis represents 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 amplitude 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 - 23.8 day ^ { -1 } , the period ratios and pulsation constants are in the ranges of P _ { pul } / P _ { orb } = 0.020 - 0.034 and Q = 0.018 - 0.031 d , respectively .
These values and the position on the Hertzsprung-Russell diagram demonstrate that the primary component is a \delta Sct pulsating star .
We examined the eclipse timing variation of KIC 11401845 from the pulsation-subtracted data and found a delay of 56 \pm 17 s in the arrival times of the secondary eclipses relative to the primary eclipses .
A possible explanation of the time shift may be some combination of a light-travel-time delay of about 34 s and a very small eccentricity of e \cos { \omega } < 0.0002 .
This result represents the first measurement of the Rømer delay in non-compact binaries .