Online Material

$\begin{figure} \par\includegraphics[width=14cm,clip]{0603fg16.eps} \end{figure}$	Figure 13: Spectral Energy Distribution best-fit models for the MIPS-u sample in units of AB magnitude. The red diamonds represent the observed magnitudes from the photometric data. Non-detections are represented by upper limits. See also Table 3.
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Figure 14:

Spectral Energy Distributions of MIPS-d galaxies of our final high-z sample (on the left panels), and the correspondent $\chi ^2_{\nu }$ distributions as a function of redshift ( right panels) in $90\%$ confidence intervals. For each candidate the most probable redshifts (first and second redshift solutions: $z_{\rm phot}$ and $z_{\rm phot2}$ ) and the $\chi ^2_{\nu }$ values with the respective probability are also labeled. See also Table 4.

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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{0603fg26.eps} \end{figure}$	Figure 15: Multiwavelength images of the fifty-three galaxies of the final sample (MIPS-d+MIPS-u). The cut-outs have a size of 10'' $\times$ 10''. North is up, East is at left.
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