Volume 426, Number 3, November II 2004
|Page(s)||941 - 949|
|Section||Interstellar and circumstellar matter|
|Published online||18 October 2004|
The dense molecular cores in the IRAS 21391+5802 region
Osservatorio Astrofisico di Arcetri, Largo E. Fermi, 5, 50125 Firenze, Italy e-mail: email@example.com
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
Accepted: 2 July 2004
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 CH3OH () 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 CH3OH. 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 CH3OH 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
© ESO, 2004
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