have performed a second fit, excluding the band that contains the emission line. Alternatively we estimate the  line contribution to the corresponding broad band flux (B-band for $z < 2.9$ and V band for the rest) following eq. (2) of Papovich et al. (2001) and perform a third fit including the full set of 14 bands. This method is actually somewhat more uncertain, since the EW are estimated from the 1-dimensional spectra, while the broad band magnitudes are measured from aperture photometry, and we have no information on the relative spatial distribution of the line emitting gas and the stars in each individual object. In any case both fits give results that are entirely consistent with the initial one: this indicates that the  line does not influence significantly the SED-fitting outcome, also because none of the LBG is a strong emitter/absorber. It also confirms the solidity of the fit: the results do not depend on the individual band, thanks to the large number of bands that we are using in the fits. Finally we also checked if the \[OIII\]5007 line contribution could somehow change the results of the SED-fit: the \[OIII\] line is harder to model, since its strenght is 