EDP Sciences
Free access
Issue
A&A
Volume 417, Number 2, April II 2004
Page(s) 605 - 613
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20034087


A&A 417, 605-613 (2004)
DOI: 10.1051/0004-6361:20034087

L183 (L134N) Revisited

II. The dust content
L. Pagani1, A. Bacmann2, F. Motte3, L. Cambrésy4, M. Fich5, G. Lagache6, M.-A. Miville-Deschênes6, 7, J.-R. Pardo8 and A. J. Apponi9

1  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

(Received 16 July 2003 / Accepted 12 November 2003 )

Abstract
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. (2003b) is confirmed, and the ISOPHOT data are shown to be inappropriate for finding such cores. In the inner core, $T_\mathrm{dust} \approx 7.5$ 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

Offprint request: L. Pagani, laurent.pagani@obspm.fr

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