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<!-- DOI: 10.1051/0004-6361/201014689 -->

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

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<tr><td><!-- init Label --><A NAME="Fig_spire"></A><!-- end Label--><A NAME="675"></A><A NAME="figure529" HREF="img54.png"><IMG SRC="Timg54.png" ALT="\begin{figure}
\par\includegraphics[angle=270,width=9cm,clip]{14689fg3a.eps}\par...
....eps}\par\includegraphics[angle=270,width=9cm,clip]{14689fg3c.eps}
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<td class="img-txt"><span class="bold">Figure 3:</span><p>
SPIRE 500&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m (<i> top</i>), 350&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m (<i> middle</i>), and 250&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m (<i> bottom</i>)
images of the Aquila SDP field. See details about data reduction and
map making in Sect.&nbsp;2. The corresponding PACS 160&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m and 70&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m images are shown in Bontemps et&nbsp;al. (<a href="/articles/aa/full_html/2010/10/aa14689-10/aa14689-10.html#Bontemps10">2010</a>).
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<tr><td><!-- init Label --><A NAME="Fig_mass_size"></A><!-- end Label--><A NAME="676"></A><A NAME="figure540" HREF="img55.png"><IMG SRC="Timg55.png" ALT="\begin{figure}
\par\includegraphics[angle=-90,width=9cm,clip]{14689fg4.eps} \end{figure}" HEIGHT="72" WIDTH="101"></A><!-- HTML Figure number: 4 -->
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<td class="img-txt"><span class="bold">Figure 4:</span><p>
Mass versus size diagram comparing the locations of the 452 starless cores identified with <i>Herschel</i> in the   Aquila main subfield to both models of critical isothermal Bonnor-Ebert spheres at <i>T</i> = 7&nbsp;K and <i>T</i> = 20&nbsp;K  (black solid lines) and observed prestellar cores from the ground-based  (sub)-mm continuum studies of <IMG SRC="img8.png" ALT="$\rho $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="10">
Ophiuchi and NGC&nbsp;2068/2071 by e.g., Motte et&nbsp;al. (<a href="/articles/aa/full_html/2010/10/aa14689-10/aa14689-10.html#Motte98">1998</a>). The masses of the <i>Herschel</i> cores were derived as explained in the text and their sizes measured at 250&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m.
The 314 candidate prestellar cores of the main subfield are shown as
filled triangles, while the other starless cores are shown as open
triangles. The mass-size correlation observed for diffuse CO clumps is
also displayed (shaded yellow band - Elmegreen &amp; Falgarone 1996).
The typical (5<IMG SRC="img9.png" ALT="$\sigma $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="13">)
detection 
               threshold of current ground-based (sub)mm (e.g., MAMBO, SCUBA) surveys  at <i>d</i> = 150&nbsp;pc  is shown by the dashed curve. The estimated <IMG SRC="img10.png" ALT="$5\sigma $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="19">
detection threshold of our SPIRE 250&nbsp;<IMG SRC="img7.png" ALT="$\mu $" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="11">m observations is shown by the blue curve.
               The lower and upper red diagonal lines correspond to constant 10<sup>21</sup>&nbsp;cm<sup>-2</sup> and         10<sup>22</sup>&nbsp;cm<sup>-2</sup>
mean column densities, respectively. The arrow indicates the global
shift of the sources if a distance of 400&nbsp;pc were adopted instead
of 260&nbsp;pc for the Aquila rift complex (see also Appendix A of
Andr&#xe9; et&nbsp;al. <a href="/articles/aa/full_html/2010/10/aa14689-10/aa14689-10.html#Andre10">2010</a>).
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<tr><td><!-- init Label --><A NAME="Fig_zooms"></A><!-- end Label--><A NAME="677"></A><A NAME="figure551" HREF="img57.png"><IMG SRC="Timg57.png" ALT="\begin{figure}
\par\includegraphics[width=8cm,clip]{14689fg5a.eps}\hspace*{1.5mm}
\includegraphics[width=8.4cm,clip]{14689fg5b.eps}\vspace*{7mm}
\end{figure}" HEIGHT="69" WIDTH="189"></A><!-- HTML Figure number: 5 -->
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<td class="img-txt"><span class="bold">Figure 5:</span><p>
<b>  a)</b> Close-up column density image (selected from Fig.&nbsp;<a href="/articles/aa/full_html/2010/10/aa14689-10/aa14689-10.html#Fig_coldens">1</a>a) showing a close view of several starless cores identified with <i>getsources</i>. The black ellipses mark the major and minor FWHM sizes determined by <i> getsources</i> for these cores at 
<!-- MATH: $\lambda = 250~\mu$ -->
<IMG SRC="img56.png" ALT="$\lambda = 250~\mu$" ALIGN="MIDDLE" BORDER="0" HEIGHT="26" WIDTH="59">m. Two protostars are also shown by red
             stars. <b>  b)</b> Intensity profiles returned by <i> getsources</i> for the 
             starless core marked by the arrow in Fig.&nbsp;<a href="/articles/aa/full_html/2010/10/aa14689-10/aa14689-10.html#Fig_zooms">5</a>a, at the five <i>Herschel</i> wavelengths.
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\par\includegraphics[angle=-90,width=8cm,clip]{14689fg6a.eps}\includegraphics[angle=-90,width=8cm,clip]{14689fg6b.eps}
\end{figure}" HEIGHT="82" WIDTH="181"></A><!-- HTML Figure number: 6 -->
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<td class="img-txt"><span class="bold">Figure 6:</span><p>
<b> a)</b> Column density map of the Aquila entire field derived from <i>Herschel</i> data. 
   The effective FWHM resolution is 36.9''.  
   Unlike in Fig.&nbsp;<a href="/articles/aa/full_html/2010/10/aa14689-10/aa14689-10.html#Fig_coldens">1</a>, a uniform offset  
<!-- MATH: $N_{{\rm H_{2}}}^{\rm off} =  3.8 \times 10^{21}~ \rm{cm}^{-2}$ -->
<IMG SRC="img58.png" ALT="$N_{{\rm H_{2}}}^{\rm off} = 3.8 \times 10^{21}~ \rm{cm}^{-2}$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="131">
   has been added in order to optimize the match with the near-IR extinction  shown in <b>  b)</b>.
   (Indeed, the <i>Herschel</i> mapping does not constrain the zero level of the background emission.)
   <b>  b)</b>
Near-IR extinction map of the same field based on 2MASS data (see
Bontemps et&nbsp;al. 2010) and expressed in units of column density,
using the relation<!-- MATH: $N_{{\rm H_{2}}} = 10^{21} ~ \rm{cm}^{-2} \times A_V$ -->
 <IMG SRC="img59.png" ALT="$N_{{\rm H_{2}}} = 10^{21} ~ \rm{cm}^{-2} \times A_V$" ALIGN="MIDDLE" BORDER="0" HEIGHT="30" WIDTH="132">.
   The resolution is 2<IMG SRC="img14.png" ALT="$^\prime $" align="bottom" BORDER="0" HEIGHT="14" WIDTH="7">.
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