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<!-- DOI: 10.1051/0004-6361/201014608 -->

<h2 class="sec">Online Material</h2>

<p><A NAME="onlTabSED"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/10/aa14608-10/table1.html"><span class="bold">Table 1:</span></a>&#160;&#160;
SED-fitting results.</p>
<p><A NAME="TabLF100"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/10/aa14608-10/table2.html"><span class="bold">Table 2:</span></a>&#160;&#160;
Rest-frame 60&nbsp;<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m luminosity function in the GOODS-N.</p>
<p><A NAME="TabLF160"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/10/aa14608-10/table3.html"><span class="bold">Table 3:</span></a>&#160;&#160;
Rest-frame 90&nbsp;<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m luminosity function in the GOODS-N.</p>
<p><A NAME="TabLFtot"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/10/aa14608-10/table4.html"><span class="bold">Table 4:</span></a>&#160;&#160;
Total IR luminosity function in the GOODS-N.</p>
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<tr><td><!-- init Label --><A NAME="Figonltempl"></A><!-- end Label--><A NAME="665"></A><A NAME="figure562" HREF="img147.png"><IMG SRC="Timg147.png" ALT="\begin{figure}
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<td class="img-txt"><span class="bold">Figure 5:</span><p>
Template SEDs of a Starburst (M&nbsp;82: cyan dot-dashed line), a
Seyfert&nbsp;2 (red dot-dot-dot-dashed) and a Sdm galaxy (green dashed)
from the Polletta et&nbsp;al. (<a href="/articles/aa/full_html/2010/10/aa14608-10/aa14608-10.html#polletta07">2007</a>) library, normalised to the <i>B</i>-band flux.
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<tr><td><!-- init Label --><A NAME="Figonlnewt2"></A><!-- end Label--><A NAME="666"></A><A NAME="figure568" HREF="img148.png"><IMG SRC="Timg148.png" ALT="\begin{figure}
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<td class="img-txt"><span class="bold">Figure 6:</span><p>
Rest-frame observed SEDs of the PEP 100- and 160-<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m sources fitted by the Polletta et&nbsp;al. (<a href="/articles/aa/full_html/2010/10/aa14608-10/aa14608-10.html#polletta07">2007</a>)
Seyfert&nbsp;2 template (orange dashed line) with underestimated FIR.
The red solid line shows the new ``FIR Seyfert&nbsp;2'' template
obtained by averaging the observed data in wavelength bins. 
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<tr><td><!-- init Label --><A NAME="Figonlratio"></A><!-- end Label--><A NAME="667"></A><A NAME="figure574" HREF="img149.png"><IMG SRC="Timg149.png" ALT="\begin{figure}
\par\includegraphics[width=10.4cm,height=6.5cm]{14608fg7.eps}
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<td class="img-txt"><span class="bold">Figure 7:</span><p>
160-<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m/100-<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m flux ratio versus <i>z</i> both observed for the differently classified PEP 160-<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m
sources (symbols) and derived from the characteristic templates
(curves): green circles and dashed line represent the normal galaxy
population; cyan stars and dot-dashed line are for SB; red triangles
and dot-dot-dot-dashed line are for AGN2; magenta squares and dotted
line are for composite objects; blue triangles and long-dashed line are
for AGN1. The upward arrows are for sources not detected at 100&nbsp;<IMG SRC="img1.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m (for which the 3&nbsp;mJy flux limit has been considered).
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