known to vary considerably for a given H$\alpha$ flux (e.g. Moustakas et al. 2006), and this precludes its suitability as a SF indicator. If we include it in the SED fitting assuming a mean \[OIII\] flux as inferred in local star-burst galaxies corresponding to a ratio f(\[OIII\])/f(\[OII\])=0.32, the output of the fit do not change.

Physical properties: results
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Total stellar masses, ages, dust extinction
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We present here the main results for stellar masses and ages of our sample. The values are those obtained with the CB09 models. For reference and comparison to previous work we also report the relative values obtained with the BC03 (between parenthesis). The total stellar masses that are found span a range $10^9 -10^{11} M_\odot$ , with a median value of $5.3 (7.5) \times 10^9 M_\odot$. These values are similar to those found by Shapley et al. 2003 (which were obtained with the even older BC96 models). The median age of our sample is 320 (500) Myrs, very similar to the Shapley et al. value, while the E(B-V) best fit parameter is smaller 0.06(0.06) vs 0.15. The discrepancies in the best fit E(B-V) raise in part from the different model of star formation history 