Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q=0.71 +/- 0.02, while the inclination of the system (i) is 38.degrees 45 +/- 0 degrees.22. Taking the primary component's temperature as 7 420 +/- 192 K, we found that the temperature of the secondary is 6 232 +/- 161 K. The mass of the primary component was found to be 1.74 +/- 0.05 M-circle dot, while it is 1.23 +/- 0.01 M-circle dot for the secondary. The primary component's radius was found to be 2.10 +/- 0.05 R-circle dot, while it was found as 1.80 +/- 0.01 R-circle dot for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a delta Scuti star. The period of pulsation was found to be 58.482 +/- 0.002, 58.482 +/- 0.001, 60.966 +/- 0.002, and 60.964 +/- 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log(P-orb)-log (P-pulse) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P-orb)-log (P-pulse) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P-orb) and log (P-pulse) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a delta Scuti component.