Open Access
Volume 535, November 2011
Article Number A76
Number of page(s) 11
Section Interstellar and circumstellar matter
Published online 11 November 2011

Online material

thumbnail Fig. 9

Herschel images of W48: a) PACS 70  μm (HPBW ~ 6); b) PACS 160 μm (HPBW ~ 12); c) SPIRE 250  μm (HPBW ~ 18); d) SPIRE 350  μm (HPBW ~ 25); and e) SPIRE 500 μm (HPBW37). The bright diffuse emission on the right of each panel is from the Galactic plane. Plus signs (+) indicate the location of supernova remnants.

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thumbnail Fig. 10

Zooms towards MDC #6 (upper rows) and MDC #17 (lower rows) at 8–250  μm. Cloud fragments with mass  < 20 M are marked as white and MDCs as black ellipses. SiO contours are the same as in Fig. 8 (from 0.01 to 0.05 K kms-1 by 0.01 K kms-1 from Jiménez-Serra et al. 2010).

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thumbnail Fig. 11

SEDs built from Herschel and other wavelengths for sources lying towards the SiO peaks (except for those shown in Fig. 4). The curves are grey-body models fitted for data at wavelengths  ≥ 160  μm. The one-temperature grey-body fit (black curve) is consistent with two-temperature grey-body fits (green curve). Error bars correspond to 30% of the integrated fluxes. No model can reasonably fit source #27.

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© ESO, 2011

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