Volume 518, July-August 2010
Herschel: the first science highlights
Article Number L106
Number of page(s) 7
Section Letters
Published online 16 July 2010

Online Material

\end{figure} Figure 3:

SPIRE 500 $\mu $m ( top), 350 $\mu $m ( middle), and 250 $\mu $m ( bottom) images of the Aquila SDP field. See details about data reduction and map making in Sect. 2. The corresponding PACS 160 $\mu $m and 70 $\mu $m images are shown in Bontemps et al. (2010).

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\par\includegraphics[angle=-90,width=9cm,clip]{14689fg4.eps} \end{figure} Figure 4:

Mass versus size diagram comparing the locations of the 452 starless cores identified with Herschel in the Aquila main subfield to both models of critical isothermal Bonnor-Ebert spheres at T = 7 K and T = 20 K (black solid lines) and observed prestellar cores from the ground-based (sub)-mm continuum studies of $\rho $ Ophiuchi and NGC 2068/2071 by e.g., Motte et al. (1998). The masses of the Herschel cores were derived as explained in the text and their sizes measured at 250 $\mu $m. The 314 candidate prestellar cores of the main subfield are shown as filled triangles, while the other starless cores are shown as open triangles. The mass-size correlation observed for diffuse CO clumps is also displayed (shaded yellow band - Elmegreen & Falgarone 1996). The typical (5$\sigma $) detection threshold of current ground-based (sub)mm (e.g., MAMBO, SCUBA) surveys at d = 150 pc is shown by the dashed curve. The estimated $5\sigma $ detection threshold of our SPIRE 250 $\mu $m observations is shown by the blue curve. The lower and upper red diagonal lines correspond to constant 1021 cm-2 and 1022 cm-2 mean column densities, respectively. The arrow indicates the global shift of the sources if a distance of 400 pc were adopted instead of 260 pc for the Aquila rift complex (see also Appendix A of André et al. 2010).

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\end{figure} Figure 5:

a) Close-up column density image (selected from Fig. 1a) showing a close view of several starless cores identified with getsources. The black ellipses mark the major and minor FWHM sizes determined by getsources for these cores at $\lambda = 250~\mu$m. Two protostars are also shown by red stars. b) Intensity profiles returned by getsources for the starless core marked by the arrow in Fig. 5a, at the five Herschel wavelengths.

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\end{figure} Figure 6:

a) Column density map of the Aquila entire field derived from Herschel data. The effective FWHM resolution is 36.9''. Unlike in Fig. 1, a uniform offset $N_{{\rm H_{2}}}^{\rm off} = 3.8 \times 10^{21}~ \rm{cm}^{-2}$ has been added in order to optimize the match with the near-IR extinction shown in b). (Indeed, the Herschel mapping does not constrain the zero level of the background emission.) b) Near-IR extinction map of the same field based on 2MASS data (see Bontemps et al. 2010) and expressed in units of column density, using the relation $N_{{\rm H_{2}}} = 10^{21} ~ \rm{cm}^{-2} \times A_V$. The resolution is 2$^\prime $.

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