Caux, E.; Ceccarelli, C.; Castets, A.; Vastel, C.; Liseau, R.; Molinari, S.; Nisini, B.; Saraceno, P. and White, G. J.
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 spectroscopic ISO-LWS observations of the [OI] (63 μm and 145 μm), the [CII] (158 μm) and the H2O (179 μm) lines towards the molecular cloud L1689N. From the observed ratio of the two [OI] lines, we deduce a mean gas temperature of (26±0.5) K, an H2 density ≥ 3 x 104 cm-3 and an [OI] column density ≥ 5 x 1019 cm-2. Combining these observations with previous CO observations, we obtain [OI]/[CO] ~ 50. This ratio implies that up to 98% of oxygen abundance is in atomic form in the gas phase. Furthermore, assuming all the gaseous carbon is locked into the CO, carbon has to be depleted by more than a factor 24. Finally, the upper limit derived for the H2O (179 μm) line (3 x 10-13 erg s-1 cm-2 ) implies that the water abundance in this region is less than 6 x 10-7 with respect to H nuclei.
|Item Type:||Journal Article|
|Copyright Holders:||1999 European Southern Observatory|
|Keywords:||stellar formation; jets and outflows; lines and bands|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||G. J. White|
|Date Deposited:||26 Apr 2012 14:25|
|Last Modified:||05 Oct 2016 00:26|
|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.