Caux, E.; Ceccarelli, C.; Castets, A.; Loinard, L.; Molinari, S.; Saraceno, P.; Smith, H. A. 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|
Using the Long Wavelength Spectrometer aboard ISO, we have observed three very young sources (Class 0 or I) in the molecular cloud NGC1333. We discuss in this contribution the FIR CO line emission observed towards the sources themselves and conclude that both a rather warm (~ 1500 K) and dense (~ 105 cm-3) gas or a colder (~ 300 K) and much denser (≥ 108 cm-3) gas are consistent with the data. Based on this analysis only we cannot distinguish between the two cases and therefore assess whether the observed emission originates in a shock associated with the outflow or in the innermost, dense and warm regions of the envelopes that surround these sources.
|Item Type:||Conference Item|
|Copyright Holders:||1999 European Space Agency|
|Extra Information:||The Universe as Seen by ISO.
Eds. P. Cox & M. F. Kessler.
|Keywords:||molecular lines; star formation|
|Academic Unit/Department:||Science > Physical Sciences|
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Glenn White|
|Date Deposited:||03 May 2012 14:40|
|Last Modified:||04 May 2012 03:49|
|Share this page:|