spectra. [@or] showed, by measuring the average fitted full width half maximum ([FWHM]{}) values of the echelle orders in the selected spectral domains, which include several photometric absorption lines. In this study we have disregarded very broad lines, such as H$_{\beta}$ and H$_{\alpha}$, because their broad wings affect the CCF and lead to large errors. Inspection of the CCFs showed that the two components are visible and well separated from each other near the quadratures. Following the method proposed by [@or], the two-Gaussian fits of the well–separated CCFs using the de-blending procedure in the IRAF routine SPLOT. The average fitted FWHMs are 120$\pm$2 and 65$\pm$3 [kms$^{-1}$]{}for the primary and secondary components. Fig.3 shows a sample of the double-Gaussian fit. Indeed, the shapes and velocities corresponding to the peaks of the CCFs are slightly changed. We estimated the intensity ratio $\ell_1$ /($\ell_{1}+\ell_{2}$)=0.649$\pm$0.032 from the two-Gaussian fits of the well-separated CCFs.

Light curve analysis {#sec:lc}
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The photometric data collected from the ASAS catalogue. We analyzed the light curve using the Wilson-Devinney code [hereafter WD; e.g., @Wil71; @Wil79; @Wil03; @Wil06] implemented into the software [phoebe]{} [@Prs05]. The WD code is widely used for determination of the orbital parameters of the eclipsing binaries. 