A&A 426, 941-949 (2004)
DOI: 10.1051/0004-6361:20041163

The dense molecular cores in the IRAS 21391+5802 region

M. T. Beltrán^{1, 2}, J. M. Girart^{3, 4}, R. Estalella³ and P. T. P. Ho<sup>2

1</sup>  Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy
    e-mail: mbeltran@arcetri.astro.it
²  Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
³  Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Av. Diagonal 647, 08028 Barcelona, Catalunya, Spain
⁴  Institut de Ciències de l'Espai (CSIC)-IEEC, Gran Capità 2, 08034 Barcelona, Catalunya, Spain

(Received 26 April 2004 / Accepted 2 July 2004)

Abstract
We present a detailed kinematical study and modeling of the emission of the molecular cores at ambient velocities surrounding IRAS 21391+5802, an intermediate-mass protostar embedded in IC 1396N. The high-density gas emission is found in association with three dense cores associated with the YSOs BIMA 1, BIMA 2, and BIMA 3. The CS ( ) and CH ₃OH ( ) emission around BIMA 1 has been modeled by considering a spatially infinitely thin ring seen edge-on by the observer. From the model we find that CS is detected over a wider radii range than CH ₃OH. A bipolar outflow is detected in the CS ( ) line centered near BIMA 1. This outflow could be powered by a yet undetected YSO, BIMA 1W, or alternatively could be part of the BIMA 1 molecular outflow. The CS and CH ₃OH emission associated with the intermediate-mass protostar BIMA 2 is highly perturbed by the bipolar outflow even at cloud velocities, confirming that the protostar is in a very active stage of mass loss. For YSO BIMA 3 the lack of outflow and of clear evidence of infall suggests that both outflow and infall are weaker than in BIMA 1, and that BIMA 3 is probably a more evolved object.

Key words: ISM: individual objects: IC 1396N -- ISM: individual objects: IRAS 21391+5802 -- ISM: jets and outflows -- ISM: molecules -- radio lines: ISM -- stars: formation

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© ESO 2004

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