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Astron. Astrophys. 361, 671-684 (2000)

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The molecular outflows in NGC 1333

L.B.G. Knee 1 and G. Sandell 2

1 National Research Council of Canada, Herzberg Institute of Astrophysics, Dominion Radio Astrophysical Observatory, 717 White Lake Road, Penticton BC V2A 6K3, Canada (lewis.knee@hia.nrc.ca)
2 National Radio Astronomy Observatory *, P.O. Box 2, Green Bank WV 24944, USA (gsandell@nrao.edu)

Received 17 February 2000 / Accepted 11 April 2000

Abstract

We present the results of [FORMULA] mapping using the James Clerk Maxwell Telescope of the active star formation region NGC 1333, supplemented by [FORMULA] mapping from the Onsala Space Observatory millimetre telescope. These maps provide a detailed overview of the complex cluster of overlapping molecular outflows associated with Herbig-Haro (HH) objects and shocked H2, and the far-infrared and submillimetre sources that drive these outflows. We identify about ten molecular outflows and in most cases their driving source. Many of the outflow-driving stars are confirmed or probable Class 0 protostellar objects which drive highly collimated CO jets.

We identify HH 12 as the leading bow shock of a large outflow driven by SSV 13 B with an orientation close to the plane of the sky.

The present rate of energy injection into molecular gas by the outflows, if maintained over a time scale [FORMULA], appears sufficient to disperse the entire NGC 1333 cloud. On the shorter time scale of the current generation of star forming activity ([FORMULA]), it appears that the star forming core has been broken up by the outflows into a number of low-density shells with star formation activity confined to dense ridges on their periphery.

Key words: stars: formation – stars: pre-main sequence – ISM: individual objects: NGC 1333 – ISM: kinematics and dynamics – ISM: molecules

* The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.

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© European Southern Observatory (ESO) 2000

Online publication: October 2, 2000
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