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[39.17] A Survey of OH (1720 MHz) Maser and OH (1665/7 MHz) Absorption Lines toward Supernova Remnants

J.W. Hewitt, F. Yusef-Zadeh, D.A. Roberts (Northwestern U.), R. Maddalena (NRAO)

The interaction of a SNR with an adjacent molecular cloud is responsible for the formation of OH(1720 MHz) maser emission through the heating and chemistry occurring within a shock wave driven into the cloud. Using the Green Bank Telescope, we have searched for main line OH absorption (1665/7 MHz) and OH (1720 MHz) emission with 0.3 km/s velocity resolution and 7.3 arc minute spatial resolution toward 21 supernova remnants. A large number of known maser-emitting remnants were mapped in the entirity of their extent, including SNRs W28, W44, IC443, and Sgr A East. We present preliminary results of these observations and will examine shock models for the production of extended maser emission and thermal absorption. In particular, we will discuss whether thermal OH absorption line can be used as a tracer of interacting molecular clouds.

This grant was in part supported by NSF AST-0307423

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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.