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A Collimated Molecular Jet in W 43A Traced by Water Maser Emission

Published online by Cambridge University Press:  26 May 2016

Hiroshi Imai ,
Tetsuo Sasao ,
Kumiko Obara ,
Toshihiro Omodaka  and
Philip J. Diamond
Hiroshi Imai
Affiliation:
VERA Project Office, National Astronomical Observatory, Japan
Tetsuo Sasao
Affiliation:
VERA Project Office, National Astronomical Observatory, Japan
Kumiko Obara
Affiliation:
Department of Physics, Kagoshima University, Japan
Toshihiro Omodaka
Affiliation:
Department of Physics, Kagoshima University, Japan
Philip J. Diamond
Affiliation:
Jodrell Bank Observatory, University of Manchester, United Kingdom

Abstract

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We present VLBA observations of the spatial and velocity distributions of 22 GHz H2O and 1612 MHz OH masers in the OH/IR star W 43A. These masers have the same systemic velocity and are, therefore, likely to be associated with the common stellar object. However, the kinematical structures of them are quite different and independent. Most of the H2O masers are extremely collimated spatially and kinematically. The H2O maser jet also seems to be precessing. On the other hand, the OH masers exhibit clear arc-shaped structures indicating a spherically-expanding shell with weak collimation. The W 43A jet is very likely to be predominantly composed of hot molecules traced by H2O maser emission and formed in the immediate vicinity of an unknown star next to another OH/IR star. Such a “molecular jet” is likely to appear only during the short period before a star forms an elongated planetary nebula.

Type
Part V: Dust and Molecules in Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 267 - 268
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

Diamond, P.J., & Nyman, L.-A. 1988, in IAU Symp. 129, VLBI and their impact on Astrophysics, ed. Moran, J.M. & Reid, M.J. (Dordrecht: Reidel), 249 Google Scholar