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OH maser emission toward the young planetary nebula K3-35

Published online by Cambridge University Press:  15 December 2006

Y. Gómez ,
D. Tafoya ,
G. Anglada ,
R. Franco-Hernández ,
J. M. Torrelles  and
L. F. Miranda
Y. Gómez
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72, 58089, Morelia, Michoacán, México email: y.gomez@astrosmo.unam.mx
D. Tafoya
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72, 58089, Morelia, Michoacán, México email: y.gomez@astrosmo.unam.mx Harvard-Smithsonian, CfA, Cambridge, MA, USA
G. Anglada
Affiliation:
Instituto de Astrofísica de Andalucía, Granada, Spain
R. Franco-Hernández
Affiliation:
Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal 3-72, 58089, Morelia, Michoacán, México email: y.gomez@astrosmo.unam.mx Harvard-Smithsonian, CfA, Cambridge, MA, USA
J. M. Torrelles
Affiliation:
Instituto de Ciencias del Espacio, Barcelona, Spain
L. F. Miranda
Affiliation:
Instituto de Astrofísica de Andalucía, Granada, Spain
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Abstract

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We present VLA (Very Large Array) observations of the 1720, 1667, 1665 and 1612 MHz OH maser emission from the central region of K 3–35. Circular polarization was found in the 1720, 1665, and 1612 MHz transitions. An estimate of the magnitude of the magnetic field, derived from the 1665 lines, toward this young planetary nebula is $\sim$ 0.14 mG at a radius of $\sim$ 250 AU.

Keywords

Planetary NebulaeMagnetic FieldsIndividual: K 3–35
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S234: Planetary Nebulae in our Galaxy and Beyond , April 2006 , pp. 403 - 404
Copyright
© 2006 International Astronomical Union