Issue |
A&A
Volume 409, Number 1, October I 2003
|
|
---|---|---|
Page(s) | 135 - 146 | |
Section | Galactic structure, stellar clusters, and populations | |
DOI | https://doi.org/10.1051/0004-6361:20030884 | |
Published online | 17 November 2003 |
Morphology and kinematics of Lynds 1642 *,**
Multivariate analysis of CO maps of a translucent cloud
1
Helsinki University Observatory, Tähtitorninmäki, PO Box 14, 00014 University of Helsinki, Finland
2
Laboratoire d'Astrophysique de Marseille, 2 place Le Verrier, 13004 Marseille, France
3
University of Helsinki, Department of Physical Sciences, PO Box 64, 00014 University of Helsinki, Finland
Corresponding author: D. Russeil, delphine.russeil@oamp.fr
Received:
30
August
2002
Accepted:
28
May
2003
The high latitude translucent molecular cloud L1642 has been mapped
in the –0 and
–1 transitions of 12CO, 13CO and C18O using
the SEST radio telescope. We have analysed the morphology and velocity
structure of the cloud using the Positive Matrix Factorization (PMF) method.
The results show that L1642 is composed of a main structure at radial velocity 0.2 km s-1 while the higher velocity components at ~0.5 and 1.0 km s-1 form an incomplete ring around it, suggesting an expanding
shell structure.
Fainter emission extends to the north with a still higher velocity of up to 1.6 km s-1. Such a velocity structure suggests an elongated morphology
in the line of sight direction. The physical properties of the cloud have been
investigated assuming LTE conditions, but non-LTE radiative transfer models
are also constructed for the 13CO observations. We confirm that L1642
follows an r-1 density distribution in its outer parts while the
distribution is considerably flatter in the core. The cloud is close to virial
equilibrium.
In an Appendix the PMF results are compared with the view obtained through the
analysis of channel maps and by the use of Principal Component Analysis (PCA).
Both PMF and PCA present the observations as a linear combination of
basic spectral shapes that are extracted from the data. Comparison of the
methods shows that the PMF method in particular is able to produce a presentation
of the complex velocity that is both compact and easily interpreted.
Key words: ISM: clouds / ISM: molecules / ISM: individual objects: L1642, MBM20
© ESO, 2003
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