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Issue A&A
Volume 463, Number 1, February III 2007
Page(s) 217 - 224
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361:20065329



A&A 463, 217-224 (2007)
DOI: 10.1051/0004-6361:20065329

Discovery of an energetic bipolar molecular outflow towards IRAS 16547-4247

G. Garay1, D. Mardones1, L. Bronfman1,  K. J. Brooks2, L. F. Rodríguez3, R. Güsten4, L.-Å. Nyman5, R. Franco-Hernández6, and J. M. Moran6

1  Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
    e-mail: guido@das.uchile.cl
2  Australia Telescope National Facility, PO Box 76, Epping 1710 NSW, Australia
3  Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72, Morelia, Michoacán, 58089, México
4  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
5  European Southern Observatory, Casilla 19001, Santiago, Chile
6  Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA

(Received 30 March 2006 / Accepted 16 November 2006)

Abstract
Aims.We present molecular line observations of the molecular core associated with IRAS 16547-4247, which have allowed us to determine its physical and kinematical properties at angular resolutions of ~18´´.
Methods.The observations were made using the Atacama Pathfinder Experiment Telescope in the $J = 3 \rightarrow 2$ transitions of 12CO and 13CO, $J = 4 \rightarrow 3$ transitions of HCO+ and H13CO+, and $J = 7 \rightarrow 6$ transition of CS.
Results.Our observations reveal the presence of a collimated bipolar outflow with lobes ~0.7 pc in extent and aligned with the thermal jet located at the center of the core. The morphology and velocity structure of the flow are well described by a biconical outflow that is inclined from the line of sight by an angle of 84°, has a semi-opening angle of 14$^{\circ}$, and in which the gas moves outwards with a constant total velocity, with respect to the cone apex, of ~120 km s-1. The outflow is massive and energetic (flow mass ~110 $M_{\odot}$; mass outflow rate ~ $2\times10^{-2}$ $M_{\odot}$ yr-1; momentum ~ $2\times10^3$ $M_{\odot}$ km s-1 and kinetic energy ~ $9\times 10^{47}$ erg), and has a dynamical time scale of $6\times10^3$ yr. These parameters are consistent with the flow being driven by a young massive stellar object with $L_{\rm bol} \sim 6\times10^4$ $L_{\odot}$.


Key words: ISM: jets and outflows -- ISM: molecules -- stars: formation



© ESO 2007

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