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Magnetic fields in supernova remnants from OH (1720 MHz) masers

Published online by Cambridge University Press:  03 August 2017

Crystal L. Brogan ,
Mark J. Claussen  and
William M. Goss
Crystal L. Brogan
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Rd, Socorro, NM 87801
Mark J. Claussen
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Rd, Socorro, NM 87801
William M. Goss
Affiliation:
National Radio Astronomy Observatory, 1003 Lopezville Rd, Socorro, NM 87801

Abstract

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Supernovae have a profound effect on the morphology, kinematics, and metallicity of galaxies. The impact of supernova shocks on surrounding molecular clouds is also thought to trigger new generations of star formation. A critical ingredient in such interactions and, indeed, all aspects of supernova remnant (SNR) evolution are magnetic fields. In recent years, OH (1720 MHz) masers have been used as signposts for the interaction of SNRs with molecular gas. In addition to tracing SNR/molecular cloud interactions, the OH (1720 MHz) maser line also provides a unique opportunity to measure the strength of the post-shock magnetic field via Zeeman splitting. Recent results from efforts to both detect the magnetic fields and resolve the maser spot sizes of OH (1720 MHz) masers toward W51C using the VLBA and W44 using MERLIN are presented. These observations have yielded magnetic field detections between 0.5 and 2.5 mG and large maser spot sizes of about 1015 cm.

Type
Part 1. Star Formation
Information
Symposium - International Astronomical Union , Volume 206: Cosmic Masers: From Protostars to Blackholes , 2002 , pp. 217 - 220
Copyright
Copyright © Astronomical Society of the Pacific 2002 

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