  We present both binarity and pulsation of KIC 6220497 from the {\it 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 $P_{\rm pul}/P_{\rm orb}$ =
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.
