Issue |
A&A
Volume 412, Number 3, December IV 2003
|
|
---|---|---|
Page(s) | 751 - 765 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20031406 | |
Published online | 08 December 2003 |
The Trumpler 14 photodissociation region in the Carina Nebula
1
Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
2
European Southern Observatory, Casilla 19001 Santiago, Chile
3
Institut d'Astrophysique Spatiale, Université de Paris-Sud, 91405 Orsay Cedex, France
4
Observatoire de Bordeaux, Université de Bordeaux I, 33270 Floirac Cedex, France
5
School of Physics, University of New South Wales, Sydney 2052, NSW, Australia
6
Max Planck für Extraterrestrische Physik, Garching bei München, Germany
Corresponding author: K. J. Brooks, kbrooks@das.uchile.cl
Received:
23
June
2003
Accepted:
9
September
2003
We report the results of observations of the fine-structure
emission lines [] 158
and [
] 63
using
FIFI on the Kuiper Airborne Observatory (KAO) and the Long Wavelength
Spectrometer (LWS) on board ISO, towards the molecular cloud
associated with the stellar cluster Trumpler 14 (Tr 14) in the Carina
Nebula. These data are compared with selected CO and CS transitions
obtained with the SEST as well as IRAS and MSX images to produce
a detailed view of the morphology and the physical conditions
prevailing in the photodissociation region (PDR) at the interface
between the ionized gas and the molecular dust lane. The relative
intensity distribution observed for the various tracers is consistent
with the stratification expected for a molecular cloud seen edge-on
and exposed to a radiation field of ≈
, which
is dominated by the most massive stars of Tr 14. The grain
photoelectric heating efficiency, ϵ, is estimated to be
≈
and is comparable to other galactic
PDRs. The molecular gas has a complicated velocity structure with a
high velocity dispersion resulting from the impact of the stellar
winds arising from Tr 14. There is evidence of small-scale clumping
with a very low volume filling factor. Despite the rich concentration
of massive O stars in Tr 14 we find that the parameters of the PDR are
much less-extreme than those of the Orion and M 17 massive
star-forming regions.
Key words: stars: formation / ISM: lines and bands / ISM: clouds / ISM: individual objects: Carina nebula
© ESO, 2003
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