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M. Sasaki, P.P. Plucinsky, T.J. Gaetz, R.K. Smith, R.J. Edgar, P.O. Slane (Harvard-Smithsonian CfA)
The Galactic supernova remnant (SNR) CTB 109 has a spectacular semi-circular morphology in both the X-ray and the radio and is associated with the anomalous X-ray pulsar 1E 2259+586. As no X-ray emission is observed from the western part of the SNR shell, the outer blast wave has apparently been stopped by a giant molecular cloud complex which is located in the west. Inside the shell, CTB 109 has an X-ray bright region in the east, known as the 'Lobe' or the 'Jet'. The analysis of the XMM AO1 data of CTB 109 shows that the emission from the 'Lobe' is thermal in origin. There are spectral variations in the 'Lobe', probably caused by differences in the ionization timescale of the plasma and the foreground absorption. Spectra of the 'Lobe' and various regions in the remnant shell do not differ significantly and clearly show Mg and Si lines. The enhanced X-ray emission of the 'Lobe' is indicative of an interaction of the SNR shock wave with a molecular cloud. From the XMM EPIC data, we derived values for, e.g., the blast wave shock velocity or the age of the SNR.
This work was supported by CXC contract NAS8-39073 and Chandra grant GO0-1127X.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.