We present both binarity and pulsation of KIC 6220497 from the Kepler observations .
The light curve synthesis shows that the eclipsing system is a semi-detached Algol with parameters of q = 0.243 \pm 0.001 , i = 77.3 \pm 0.3 deg , and \Delta T = 3,372 \pm 58 K , in which the detached primary component fills its Roche lobe by \sim 87 % .
A multiple frequency analysis of the eclipse-subtracted light residuals reveals 33 frequencies in the range of 0.75 - 20.22 d ^ { -1 } with amplitudes between 0.27 and 4.56 mmag .
Among these , four are pulsation frequencies in fundamental ( f _ { 1 } , f _ { 5 } ) and p ( f _ { 2 } , f _ { 7 } ) modes , and six are orbital frequency ( f _ { 8 } , f _ { 31 } ) and its harmonics ( f _ { 6 } , f _ { 11 } , f _ { 20 } , f _ { 24 } ) , which can be attributed to tidally excited modes .
For the pulsation frequencies , the pulsation constants of 0.16 - 0.33 d and the period ratios of P _ { pul } / P _ { orb } = 0.042 - 0.089 indicate that the primary component is a \delta Sct pulsating star and , thus , KIC 6220497 is an oscillating eclipsing Algol ( oEA ) star .
The dominant pulsation period of 0.1174051 \pm 0.0000004 d is significantly longer than that expected from empirical relations that link the pulsation period with the orbital period .
The surface gravity of \log g _ { 1 } = 3.78 \pm 0.03 is clearly smaller than those of the other oEA stars with similar orbital periods .
The pulsation period and the surface gravity of the pulsating primary demonstrate that KIC 6220497 would be the more evolved EB , compared with normal oEA stars .