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A collimated molecular jet in W 43A traced by water maser emission

Published online by Cambridge University Press:  03 August 2017

Hiroshi Imai ,
Tetsuo Sasao ,
Kumiko Obara ,
Toshihiro Omodaka  and
Philip J. Diamond
Hiroshi Imai
Affiliation:
VERA Project Office, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
Tetsuo Sasao
Affiliation:
VERA Project Office, National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan
Kumiko Obara
Affiliation:
Department of Physics, Kagoshima University, Kagoshima 890-0065, Japan
Toshihiro Omodaka
Affiliation:
Department of Physics, Kagoshima University, Kagoshima 890-0065, Japan
Philip J. Diamond
Affiliation:
NRAL, Jodrell Bank Observatory, University of Manchester, Macclsfield, SK 11 9DL, U.K.

Abstract

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We present the spatial and velocity distributions of water masers in W 43A. Most of the maser features are spatially and kinematically collimated to a surprising extent. It is very likely that the jet in W 43A is predominantly composed of warm molecules traced by water maser emission. The position angle of the spatial collimation of the maser clusters is slightly different from the directions of both the cluster separation and the proper motions. We propose a model involving a precessing jet to explain the axis offsets. The discovery of a molecular jet with precession in W 43A provides important information on our understanding of the formation of collimated molecular jets and may provide clues on specific stages of stellar evolution.

Type
Part 1. Star Formation
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 80 - 83
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

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