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Water and OH Maser Emission from the Planetary Nebula K3-35

Published online by Cambridge University Press:  26 May 2016

Yolanda Gómez ,
Luis F. Miranda ,
Guillem Anglada  and
JosÉ M. Torrelles
Yolanda Gómez
Affiliation:
Instituto de Astronomía, UNAM-Morelia, Apdo. Postal 3-72 (Xangari), 58089 Morelia, Michoacán, México
Luis F. Miranda
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Apdo. Correos 3004, E-18080 Granada, Spain
Guillem Anglada
Affiliation:
Instituto de Astrofísica de Andalucía, CSIC, Apdo. Correos 3004, E-18080 Granada, Spain, and Harvard-Smithsonian CfA, 60 Garden Street, Cambridge, MA 02138, USA
JosÉ M. Torrelles
Affiliation:
Institut d'Estudis Espacials de Catalunya (IEEC/CSIC) and Instituto de Ciencias del Espacio (CSIC), Edifici Nexus, C/ Gran Capità 2-4, E-08034 Barcelona, Spain

Abstract

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Water-vapour masers, typical of the envelopes in giant stars, are not expected to persist in planetary nebulae due to the ultraviolet radiation of the remnant star that progressively destroys the molecules. Recently, we have reported the first unambiguous detection of water maser emission in a planetary nebula, K 3–35 (Miranda et al. 2001). The water masers in K3–35 were detected at the center of the nebula, along the minor axis, at a radius of ~85 AU and also at the surprisingly large distance of 5000 AU from the star, at the tips of the bipolar lobes. The existence of these water molecules is puzzling, and probably we are observing the very moment of transformation of a giant star into a planetary nebula. Miranda et al. (2001) also report the presence of polarization in the OH 1665 MHz masers, which are distributed towards the central star in a torus-like structure. Here we review the main results on this source.

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. 263 - 266
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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