| Issue |
A&A
Volume 535, November 2011
|
|
|---|---|---|
| Article Number | A76 | |
| Number of page(s) | 11 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201117831 | |
| Published online | 11 November 2011 | |
Online material
 |
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. |
| Open with DEXTER | |
 |
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). |
| Open with DEXTER | |
 |
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. |
| Open with DEXTER | |
© ESO, 2011
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