Far-infrared CO line emission of protostars in NGC 1333

Details Far-infrared CO line emission of protostars in NGC 1333 Far-infrared CO line emission of protostars in NGC 1333

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..643c&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 643

Physics

1

Molecular Lines, Star Formation

Scientific paper

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.

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