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H2O maser polarization of the water fountains IRAS 15445–5449 and IRAS 18043–2116

Published online by Cambridge University Press:  30 August 2012

Andrés F. Pérez-Sánchez ,
Wouter H. T. Vlemmings  and
Jessica M. Chapman
Andrés F. Pérez-Sánchez
Affiliation:
Argelander Institute for Astronomy, University of Bonn, Auf dem Huegel 71, 53121 Bonn, Germany email: [email protected], [email protected]
Wouter H. T. Vlemmings
Affiliation:
Argelander Institute for Astronomy, University of Bonn, Auf dem Huegel 71, 53121 Bonn, Germany email: [email protected], [email protected]
Jessica M. Chapman
Affiliation:
CSIRO Astronomy and Space Science, Australia Telescope National Facility, PO Box 76, Epping, NSW 1710, Australia email: [email protected]
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Abstract

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We present the morphology and linear polarization of the 22-GHz H2O masers in the high-velocity outflow of two post-AGB sources, d46 (IRAS 15445–5449) and b292 (IRAS 18043–2116). The observations were performed using The Australia Telescope Compact Array. Different levels of saturated maser emission have been detected for both sources. We also present the mid-infrared image of d46 overlaid with the distribution of the maser features that we have observed in the red-shifted lobe of the bipolar structure. The relative position of the observed masers and a previous radio continuum observation suggests that the continnum is produced along the blue-shifted lobe of the jet. It is likely due to synchrontron radiation, implying the presence of a strong magnetic field in the jet. The fractional polarization levels measured for the maser features of d46 indicate that the polarization vectors are tracing the poloidal component of the magnetic field in the emitting region. For the H2O masers of b292 we have measured low levels of fractional linear polarization. The linear polarization in the H2O maser region of this source likely indicates a dominant toroidal or poloidal magnetic field component.

Keywords

maserspolarizationstars: AGB and post-AGBstars: late-typestars: magnetic fieldsstars: circumstellar matter
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 474 - 475
Copyright
Copyright © International Astronomical Union 2012

References

Bains, I., Cohen, M., Chapman, J. M., Deacon, R. M., & Redman, M. P. 2009, MNRAS, 397, 1386 CrossRefGoogle Scholar
Gomez, J. F., Rizzo, J. R., Suarez, O., Miranda, L. F., Guerrero, M. A., & Ramos-Larios, G. 2011, arXiv:1105.5202 Google Scholar
Habing, H. J. & Olofsson, H. 2003, Asymptotic giant branch stars, by Habing, Harm J. and Olofsson, Hans. Astronomy and astrophysics library, New York, Berlin: Springer, 2003.Google Scholar
Lagadec, E., et al. 2011, arXiv:1102.4561 Google Scholar
Likkel, L. & Morris, M. 1988, ApJ, 329, 914 CrossRefGoogle Scholar
Perez-Sanchez, A. F., Vlemmings, W. H. T., & Chapman, J. M. 2011, arXiv:1108.1911Google Scholar
Vlemmings, W. H. T., Diamond, P. J., & Imai, H. 2006, Nature, 440, 58 CrossRefGoogle Scholar