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<!-- DOI: 10.1051/0004-6361/201014626 -->

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

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<tr><td><!-- init Label --><A NAME="Fig:backgroundsources"></A><!-- end Label--><A NAME="903"></A><A NAME="figure761" HREF="img38.png"><IMG SRC="Timg38.png" ALT="\begin{figure}
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<td class="img-txt"><span class="bold">Figure 2:</span><p>
The 250&nbsp;<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m SPIRE map around the <IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">&nbsp;Pic disk. The 
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<IMG SRC="img11.png" ALT="$10 \times 10$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="47"><IMG SRC="img12.png" ALT="$^\prime $" align="bottom" BORDER="0" HEIGHT="14" WIDTH="7">
region delimited by the white square shows more than 50&nbsp;background
sources comparable to the cold blob seen in the southwest of the disk.
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<tr><td><!-- init Label --><A NAME="Fig:spirePsfs"></A><!-- end Label--><A NAME="906"></A><A NAME="figure771" HREF="img39.png"><IMG SRC="Timg39.png" ALT="\begin{figure}
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<td class="img-txt"><span class="bold">Figure 6:</span><p>
The 250, 350 and 500&nbsp;<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m SPIRE PSFs, rotated to match  the position angle at the time of the <IMG SRC="img1.png" ALT="$\beta $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">&nbsp;Pic
observations. The PSF images are scaled linearly, contour lines are in
steps of 10% of the peak flux. The white circle shows the beam <i>FWHM</i>.
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<p></p><p><A NAME="table:observations"></A><p class="inset-old"><a href="/articles/aa/full_html/2010/10/aa14626-10/table1.html"><span class="bold">Table 1:</span></a>&#160;&#160;
Observation log.</p>
<p></p><h2 class="sec"><a name="SECTION00090000000000000000"></a><A NAME="section:datareduction"></A>
Appendix A: Data reduction
</h2>

<p>The PACS data were processed in the <EM>Herschel</EM> interactive
analysis
environment&nbsp;HIPE (v3.0), applying the standard pipeline steps. The
flux conversion was done using version&nbsp;5 of the response
calibration.
Signal glitches due to cosmic ray impacts were masked out in two steps.
First the PACS photMMTDeglitching task in HIPE was applied on the
detector
timeline. Then a first coarse map was projected, which is then used
as a reference for the second level deglitching HIPE task
IIndLevelDeglitch. In the detector time series we masked the region
around the source
prior to applying a high-pass filter to remove the low frequency
drifts.
The scale of the high pass filter was taken to be half the length of an
individual scan leg on the sky, i.e. 3.7<IMG SRC="img12.png" ALT="$^\prime $" align="bottom" BORDER="0" HEIGHT="14" WIDTH="7">.
The detector time series signals were then summed up into a map using 
the PACS photProject task.  The pixel scale for the 70 and 100&nbsp;<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m
maps was set to 1
<!-- MATH: $^{\prime\prime}$ -->
<IMG SRC="img5.png" ALT="$^{\prime \prime }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="11">,
while the scale for the 160&nbsp;<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m map was 2
<!-- MATH: $^{\prime\prime}$ -->
<IMG SRC="img5.png" ALT="$^{\prime \prime }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="11">.
For the deep map in the 70 and 160&nbsp;<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m filter we combined
the two detector time series and projected these together.

</p><p>The SPIRE data were also reduced using HIPE and maps
were obtained via the default naiveMapper task. The SPIRE observation
consists of several repetitions of a map observation of the same
area.  As a result it was possible to project the data with a pixel size of&nbsp;4, 6, and 9
<!-- MATH: $^{\prime\prime}$ -->
<IMG SRC="img5.png" ALT="$^{\prime \prime }$" align="bottom" BORDER="0" HEIGHT="14" WIDTH="11">
while still maintaining complete sampling across the source. 
<br>
<br>
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