L183 (L134N) Revisited^*

II. The dust content

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

Corresponding author: L. Pagani, laurent.pagani@obspm.fr

Received: 16 July 2003
Accepted: 12 November 2003

Abstract

We present here a complete dust map of L183 (=L134N) with opacities ranging from A_V = 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.