with those associated with the calibration and the clustering correction.\

Mean physical properties from SED fitting {#sect:sedfit}
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We interpreted our measurements of the mean SEDs using the @Draine2007 model as in @Magdis2012b. This model, developed initially to study the interstellar medium in the Milky Way and in nearby galaxies, takes into account the heterogeneity of the intensity of the radiation field. The redshift slices we used have a non-negligible width. To account for this, we convolve the model by the redshift distribution of the galaxies before fitting the data. The majority of the redshifts in our sample are photometric. We thus sum the probability distribution function (PDF) of the redshifts of all the sources in a sub-sample to estimate its intrinsic redshift distribution. The uncertainties on the physical parameters are estimated using the same Monte Carlo method as in @Magdis2012b. The uncertainties on each parameter takes into account the potential degeneracies with the others, i.e., they are the marginalized uncertainties on each individual parameters. Our good sampling of the dust SEDs (8 photometric points between 24$\mu$m and 1.1mm including at least six detections) allows us to break the degeneracy between the dust temperature and the dust mass which is 