Marigo & Girardi (2007). As shown first by Maraston (2005, M05) and Maraston et al. (2006), TP-AGB stars are especially important in galaxies whose spectra are dominated by emission from these intermediate age stars.\
As already shown by several authors (e.g. Marchesini et al. 2009, Eminian et al. 2008, Lamareille et al. 2008) the CB09 models give masses that are, on average, lower than the BC03 ones. In particular, the recent study by Salimbeni et al. (2009) on a sample that partially overlaps with the present one showed that the average mass difference in their highest redshift bin (which includes the range z $\sim$ 2.5-3.5, see their figure 4) is around $\sim 30$%, with a slight dependence on mass.\
Examples of SED fitting for some of the galaxies, spanning the entire redshift range, are shown in Figure \[fig:sed\].

While \[OII\] and H$\alpha$ emission are included in the models, with strenght proportional to the SFR, according to the Kennicutt (1998) relations, the  and \[OIII\] emission line are more difficult to model. In particular the  line could contaminate the photometry of the B or V-band (depending on the redshift) and therefore change the result of the SED fitting. To check this, we 