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<!-- DOI: 10.1051/0004-6361/200810630 -->

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<tr><td><!-- init Label --><A NAME="fig:fig13">&#160;</A><!-- end Label--><A NAME="3397"></A><A NAME="figure3041"
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\par\includegraphics[width=14cm,clip]{0603fg16.eps}
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<td class="img-txt"><span class="bold">Figure 13:</span><p>
Spectral Energy Distribution best-fit models for the MIPS-u&nbsp;sample in  units of AB&nbsp;magnitude. The red diamonds represent the observed magnitudes from the photometric data. Non-detections are represented by upper limits. See also Table&nbsp;<a href="/articles/aa/full_html/2009/23/aa10630-08/aa10630-08.html#table:tab3">3</a>.</p></td>
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continued.</p></td>
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continued.</p></td>
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\par\includegraphics[width=14cm,clip]{0603fg19.eps}
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continued.</p></td>
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<tr><td><!-- init Label --><A NAME="fig:fig14">&#160;</A><!-- end Label--><A NAME="3398"></A><A NAME="figure3068"
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 ALT="\begin{figure}
\par\includegraphics[width=14cm,clip]{0603fg20.eps}
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<td class="img-txt"><span class="bold">Figure 14:</span><p>
Spectral Energy Distributions of MIPS-d galaxies of our final high-<I>z</I> sample (on <I> the left panels</I>), and the correspondent 
<!-- MATH: $\chi^2_{\nu}$ -->
<IMG
 WIDTH="16" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img26.png"
 ALT="$\chi ^2_{\nu }$">&nbsp;distributions as a function of redshift (<I> right panels</I>) in <IMG
 WIDTH="29" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img27.png"
 ALT="$90\%$">&nbsp;confidence intervals.  For each candidate the most probable redshifts (first and second redshift solutions: 
<!-- MATH: $z_{\rm phot}$ -->
<IMG
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 ALT="$z_{\rm phot}$">
and&nbsp;
<!-- MATH: $z_{\rm phot2}$ -->
<IMG
 WIDTH="31" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img28.png"
 ALT="$z_{\rm phot2}$">)
and the 
<!-- MATH: $\chi^2_{\nu}$ -->
<IMG
 WIDTH="16" HEIGHT="30" ALIGN="MIDDLE" BORDER="0"
 SRC="img26.png"
 ALT="$\chi ^2_{\nu }$">&nbsp;values with the respective probability are also labeled. See also Table&nbsp;<a href="/articles/aa/full_html/2009/23/aa10630-08/aa10630-08.html#table:tab4">4</a>.</p></td>
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<td class="img-txt"><span class="bold">Figure 14:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 14:</span><p>
continued.</p></td>
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continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 14:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 14:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 15:</span><p>
Multiwavelength images of the fifty-three galaxies of the final sample (MIPS-d+MIPS-u). The cut-outs have a size of 10''&nbsp;<IMG
 WIDTH="12" HEIGHT="26" ALIGN="MIDDLE" BORDER="0"
 SRC="img10.png"
 ALT="$\times $">
10''. North is up, East is at <I> left</I>.</p></td>
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\par\includegraphics[width=17.5cm,clip]{0603fg27.eps}
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<td class="img-txt"><span class="bold">Figure 15:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 15:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 15:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 15:</span><p>
continued.</p></td>
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<td class="img-txt"><span class="bold">Figure 15:</span><p>
continued.</p></td>
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