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<!-- DOI: 10.1051/0004-6361/201014585 -->

<h2 class="sec">Online Material</h2>
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<tr><td><!-- init Label --><A NAME="fig3"></A><!-- end Label--><A NAME="561"></A><A NAME="figure478" HREF="img21.png"><IMG SRC="Timg21.png" ALT="\begin{figure}
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<td class="img-txt"><span class="bold">Figure 3:</span><p>
The derived 70-850-<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m
spectral energy distributions of the components contributing to the
observed emission from Cas&nbsp;A.
See Sect.&nbsp;3 for a description of how the flux densities from
each
component at each wavelength were estimated.
Red: nonthermal flux densities estimated from a power-law fit between
the 6-cm and 3.6-<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m
flux densities; Green: warm dust component flux densities; Blue: flux
densities for the cold interstellar dust component. Also
shown are a<!-- MATH: $\lambda^{-2}$ --> <IMG SRC="img4.png" ALT="$\lambda ^{-2}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="22">
emissivity 17-K fit to the cold
IS dust flux densities (blue dashed line), and a comparison with
the Dwek et&nbsp;al. (<A NAME="aaref8"></A><a href="/articles/aa/full_html/2010/10/aa14585-10/aa14585-10.html#Dwek1997">1997</a>)
COBE DIRBE/FIRAS average ISM spectral
energy distribution (turquoise; shown with the quoted
<IMG SRC="img5.png" ALT="$\pm $" align="bottom" BORDER="0" HEIGHT="14" WIDTH="13">20% 1<IMG SRC="img6.png" ALT="$\sigma $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="12">
uncertainty limits). Magenta: the derived
flux densities for the cool dust component, together with a 35-K<!-- MATH: $\lambda^{-2}$ --> <IMG SRC="img4.png" ALT="$\lambda ^{-2}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="22">
emissivity fit (dashed magenta line). The blue points show the PACS and
SPIRE 70-500-<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m
total flux densities measured for Cas&nbsp;A, as well as the SCUBA
850-<IMG SRC="img2.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">m flux
density measured by Dunne et&nbsp;al. (<a href="/articles/aa/full_html/2010/10/aa14585-10/aa14585-10.html#Dunne2003">2003</a>). The black
dashed line corresponds to the sum of the fits to
the nonthermal, warm dust, cool dust and cold IS dust components.
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