L183 (L134N) Revisited. II. The dust content

Laurent Pagani (1) , Aurore Bacmann (2) , F. Motte (3) , L. Cambrésy (4) , Michael Fich (5) , Guilaine Lagache (6) , Marc-Antoine Miville-Deschenes (6, 7) , Juan R. Pardo (8) , A. J. Apponi (9)

1 LERMA - Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique
2 ESO - European Southern Observatory
3 AIM (UMR_7158 / UMR_E_9005 / UM_112) - Astrophysique Interprétation Modélisation
4 OAS - Observatoire astronomique de Strasbourg
5 University of Waterloo [Waterloo]
6 IAS - Institut d'astrophysique spatiale
7 CITA - Canadian Institute for Theoretical Astrophysics
8 Departamento de Astrofisica Molecular e Infrarroja-Instituto de Estructura de la Materia, Consejo Superior de Investigaciones Científica (CSIC)
9 Steward Observatory, University of Arizona

We present here a complete dust map of L183 (=L134N) with opacities ranging from A_Vb = 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{Pagani03b}) is confirmed, and the ISOPHOT data are shown to be inappropriate for finding such cores. In the inner core, T_dust ≈ 7.5 K and could be as low as 6.7 K.

Domaines: Astrophysique [astro-ph]

Laurent Pagani, Aurore Bacmann, F. Motte, L. Cambrésy, Michael Fich, et al.. L183 (L134N) Revisited. II. The dust content. Astronomy and Astrophysics - A&A, 2004, 417, pp.605-613. ⟨10.1051/0004-6361:20034087⟩. ⟨hal-03785686⟩