| Issue |
A&A
Volume 533, September 2011
|
|
|---|---|---|
| Article Number | A94 | |
| Number of page(s) | 9 | |
| Section | Interstellar and circumstellar matter | |
| DOI | https://doi.org/10.1051/0004-6361/201117315 | |
| Published online | 07 September 2011 | |
Online material
Appendix A:
 |
Fig. A.1
The 5 Herschel wavebands of Vela C, from top to bottom, 70, 160, 250, 350 and 500 μm. The observed rms level of cirrus noise in Vela C is ~6 mJy and 20 mJy, at λ = 70 and 160 μm, respectively and ~200–500 mJy at the SPIRE 250, 350 and 500 μm bands. At shorter wavelengths only those warmer objects, such as protostars and HII regions are seen. At longer wavelengths Herschel detects cold, deeply embedded filaments and the progenitors of high-mass stars. |
| Open with DEXTER | |
 |
Fig. A.1
continued. |
| Open with DEXTER | |
© ESO, 2011
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