Pulsational and eclipsing nature of TIC 140736015

We present the discovery of $\gamma$ Doradus-type pulsations in the eclipsing binary TIC 140736015. We obtained the physical and geometrical parameters of this detached eclipsing binary hosting a pulsating component. Based on the Transiting Exoplanet Survey Satellite (TESS) observation and Gaia DR3 data of TIC 140736015, we refined the light elements of the system using $(O-C)$ analysis and found that the eclipse times varied with a period of $\sim 2048$ days, probably linked to the multiperiodic pulsational nature. We showed that essentially, only secondary eclipse is seen in the phased light curve. The frequency analysis using the out-of-eclipse data reveals that all the pulsational frequencies are located in the region lower than $5d^{-1}$. After removing the pulsational variation from the observations we analysed the residual light curve together with the radial velocity data obtained from Gaia DR3 and find the masses and radii of the primary and secondary components as $M_1=1.429\pm 0.022$ $M_{\odot }$, $M_2=1.402\pm 0.022$ $M_{\odot }$and $R_1=1.685\pm 0.001$ $R_{\odot }$, $R_2=1.393\pm 0.001$ $R_{\odot }$, respectively. Regarding the location of the components on the Hertzsprung–Russell diagram both components can be a $\gamma$ Dor/solar-like pulsator.