parameters {#sec:class}
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The width of the cross-correlation function (CCF) is a good tool for the measurement of $v\sin i$ of a star. We used a method developed by @Pen96 to estimate the $v\sin i$ of each star composing the investigated double–lined eclipsing binary system from its CCF peak by a proper calibration based on a spectrum of a narrow-lined star with a similar spectral type. The rotational velocities of the components were obtained by measuring the FWHM of the CCF peak related to each component in five high-S/N spectra acquired near the quadratures, where the two spectra have the largest relative difference in radial velocity. The CCFs were used for the determination of $v\,sin\,i$ through a calibration of the full-width at half maximum (FWHM) of the CCF peak as a function of the $v\,sin\,i$ of artificially broadened spectra of a slowly rotating standard star ($\iota$Psc, $v\sin i \simeq$3kms$^{-1}$, e.g., @takeda) acquired with the same set up and in the same observing night as the target system. The limb darkening coefficient was fixed at the theoretically predicted values, 0.55 for the system [@Van93]. We calibrated the relationship between the CCF Gaussian width and $v\,sin\,i$ using the @Con77 data sample. This 