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Title:
Shock-excited Maser Emission from Supernova Remnants: G32.8-0.1, G337.8-0.1, G346.6-0.2, and the HB 3/W3 Complex
Authors:
Koralesky, Barron; Frail, D. A.; Goss, W. M.; Claussen, M. J.; Green, A. J.
Affiliation:
AA(School of Physics and Astronomy, University of Minnesota, 116 Church Street, SE, Minneapolis, MN 55455; ), AB(National Radio Astronomy Observatory/Array Operations Center, P.O. Box O, Socorro, NM 87081; , , ), AC(National Radio Astronomy Observatory/Array Operations Center, P.O. Box O, Socorro, NM 87081; , , ), AD(National Radio Astronomy Observatory/Array Operations Center, P.O. Box O, Socorro, NM 87081; , , ), AE(School of Physics, University of Sydney, A28, Sydney, NSW 2006, Australia; )
Publication:
The Astronomical Journal, Volume 116, Issue 3, pp. 1323-1331. (AJ Homepage)
Publication Date:
09/1998
Origin:
AJ
AJ Keywords:
ISM: CLOUDS, ISM: MAGNETIC FIELDS, ISM: MOLECULES, ISM: SUPERNOVA REMNANTS
DOI:
10.1086/300508
Bibliographic Code:
1998AJ....116.1323K

Abstract

We present the results of VLA observations in the ground-state hydroxyl (OH) transition at 1720 MHz toward 20 supernova remnants (SNRs). We detect compact emission from four objects. For three of these objects (G32.8-0.1, G337.8-0.1, and G346.6-0.2), we argue that the emission results from masers that are shock-excited due to the interaction of the SNR and an adjacent molecular cloud. We observe a characteristic Zeeman profile in the Stokes V spectrum, which allows us to derive a magnetic field of 1.5 and 1.7 mG for G32.8-0.1 and G346.6-0.2, respectively. The velocity of the masers also allows us to determine a kinematic distance to the supernova remnants (SNRs). Our criteria for a maser to be associated with an SNR along the line of sight are that the position and velocity of the maser and SNR must agree and the OH (1720) emission must be unaccompanied by other OH lines.
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