shown in Fig.6, we used [Period04]{}[^5]. Figure6 displays the amplitude spectra in the frequency range from 0.6 to 2.0 d$^{-1}$, $\gamma$ Dor oscillation frequencies indeed are typically detected in this range [@balo].

The amplitude spectra after the analysis are presented in Fig.6. Clearly visible is the only a peak around 1.0 d$^{-1}$. The light variation is dominated with a frequency $f_1$=1.0029(19) and a full amplitude of about 60 mmag. The uncertainty of the frequency was derived according to [@kallinger]. No significant peaks are present in the region higher than 5 d$^{-1}$ and smaller than 0.6 d$^{-1}$. One sees that V2653Oph pulsates in the frequency range of $\gamma$ Dor type variables [@gri].

Investigation of $\gamma$-Dor type pulsating variables in close eclipsing binary systems is a relatively new area of the stellar astrophysics. The first $\gamma$ Dor type pulsation was discovered by [@iban] in the more massive primary star of the eclipsing binary system VZCVn. Following this discovery new $\gamma$-Dor pulsators were revealed by precise photometric studies. We collected the eclipsing binaries with $\gamma$-Dor pulsators and presented in Table6. So far, 11 eclipsing binary systems containing a $\gamma$-Dor type pulsating component have been discovered. Unfortunately, spectroscopic observations of only six systems have 