distribution at its extremal values in the @Draine2007 model.\

Evolution of the specific star formation rate
---------------------------------------------

From the fit of the SEDs, we can easily derive the evolution of the mean specific star formation rate of our mass-selected sample with redshift. The results are presented in Fig.\[fig:ssfr\]. The strong starbursts lie about a factor of 10 above the main-sequence, demonstrating that this population is dominated by objects just above our cut of 10 sSFR$_{\rm MS}$. Our results can be fitted by an evolution in redshift as (0.061$\pm$0.006Gyr$^{-1}$)$\times$(1+z)$^{2.82\pm0.12}$ at z$<$2 and as (1+z)$^{2.2\pm0.3}$ at z$>$2. We compared our results with the compilation of measurements of @Sargent2014 at M$_\star = 5 \times 10^{10}$M$_\odot$. At z$<$1.5, our results agree well with the previous measurements. Between z=1.5 and z=3.5, our new measurements follow the lower envelop of the previous measurements. This mild disagreement could have several causes.\
First of all, the clustering effect was not taken into account by the previous analyses based on stacking. This effect is stronger at high redshift, because the bias[^5] of both infrared and mass-selected galaxies increases with redshift [e.g., @Bethermin2013]. In addition, the SEDs peak at a longer wavelength, where the bias is stronger owing to beam 