Volume 417, Number 2, April II 2004
|Page(s)||605 - 613|
|Section||Interstellar and circumstellar matter|
|Published online||19 March 2004|
L183 (L134N) Revisited*
II. The dust content
LERMA & UMR 8112 du CNRS, Observatoire de Paris, 61 Av. de l'Observatoire, 75014 Paris, France
2 ESO, Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany
3 CEA, DSM, DAPNIA, Service d'Astrophysique, CE Saclay, 91191 Gif-sur-Yvette Cedex, France
4 Observatoire Astronomique de Strasbourg, UMR 7550, Université Louis Pasteur, 67000 Strasbourg, France
5 Physics Department, University of Waterloo, Waterloo, Ontario, N2L 3G1, Canada
6 IAS, Bât. 121, Université Paris-Sud, 91435 Orsay Cedex, France
7 CITA, University of Toronto, 60 St. George Street, Toronto, Ontario, M5S 3H8, Canada
8 Instituto de Estructura de la Materia, Dpto de Astrofísica Molecular e Infrarroja CSIC, Madrid, Spain
9 University of Arizona, Steward Observatory, 933 N. Cherry Ave., Tucson, AZ 85721, USA
Corresponding author: L. Pagani, email@example.com
Accepted: 12 November 2003
We present here a complete dust map of L183 (=L134N) with opacities ranging from AV = 3 to 150 mag. Five peaks are identified as being related to known molecular peaks and among these dust peaks two are liable to form stars. The main peak is a prestellar core with a density profile proportional to r-1 up to a radius of ~4500 AU and the northern peak could possibly be on its way to form a prestellar core. If true, this is the first example of the intermediate steps between cloud cores and prestellar cores during the quasi-static contraction. Additionally, the low dust temperature of the core reported in Pagani et al. ([CITE]) is confirmed, and the ISOPHOT data are shown to be inappropriate for finding such cores. In the inner core, K and could be as low as 6.7 K.
Key words: ISM: abundances / ISM: molecules / ISM: dust, extinction / ISM: structure / ISM: individual: L134N / ISM: individual: L183
© ESO, 2004
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