Saraceno, P.; Benedettini, M.; di Giorgio, A. M.; Giannini, T.; Nisini, B.; Lorenzetti, D.; Molinari, S.; Pezzuto, S.; Spinoglio, L.; Tommasi, E.; Clegg, P. E.; Correia, J. C.; Griffin, M. J.; Kaufman, M. J.; Leeks, S. J.; White, G.; Caux, E.; Liseau, R. and Smith, H.
PDF (Version of Record)
- Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
|Google Scholar:||Look up in Google Scholar|
We present the results obtained with the ISO Long Wavelength Spectrometer on a sample of Pre-MS sources, where several molecular lines of CO, H2O and OH have been detected. The analysis of the CO lines indicates that gas temperatures as low as 200 K are consistent with the data. This would be in agreement with the relatively low abundance of water in the gas phase measured in most of the objects.
|Item Type:||Conference Item|
|Copyright Holders:||1999 Not known|
|Extra Information:||The Physics and Chemistry of the Interstellar Medium, Proceedings of the 3rd Cologne-Zermatt Symposium,
held in Zermatt, September 22-25, 1998,
Eds.: V. Ossenkopf, J. Stutzki, and G. Winnewisser,
|Academic Unit/Department:||Science > Physical Sciences
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||25 Apr 2012 09:42|
|Last Modified:||25 Feb 2016 12:00|
|Share this page:|
Download history for this item
These details should be considered as only a guide to the number of downloads performed manually. Algorithmic methods have been applied in an attempt to remove automated downloads from the displayed statistics but no guarantee can be made as to the accuracy of the figures.