The Nature OH Maser Emission From Supernova Remnants

Details The Nature OH Maser Emission From Supernova Remnants The Nature OH Maser Emission From Supernova Remnants

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.6304y&link_type=abstract

American Astronomical Society Meeting 208, #63.04; Bulletin of the American Astronomical Society, Vol. 38, p.143

Astronomy and Astrophysics

Astronomy

Scientific paper

There is compelling evidence that OH(1720 MHz) masers trace shocked molecular gas in regions of interaction between expanding supernova remnants (SNRs) and molecular clouds. This evidence is also supported by the fact that many of the SNR masers are correlated with mixed-morphology supernova remnants in which X-rays play an importatnt role in enhancing the abundance of OH behind a shock front. The OH(1720 MHz) maser emission is not only rare to detect but also unusual in that extended but weak OH (1720 MHz) emission accompanies the strong compact maser sources. I will describe our recent detection of extended OH(1720 MHz) maser emission from W28 and W44 as well as their magnetic field measurements of compact sources due to Zeeman splitting. I also present the preliminary results of our radio recombination line observations of W28 and W44 using the Green Bank Telescope. These observations present the kinematics of ionized gas towardthese remnants.

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