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C. E. Rakowski (Harvard Smithsonian CfA), C. Badenes, J. P. Hughes (Rutgers University), P. Slane, B. Gaensler (Harvard Smithsonian CfA)
The {\em ASCA} X-ray spectrum of supernova remnant (SNR) G337.2-0.7 showed strong X-ray emission lines, proving the remnant to be young and dominated by supernova ejecta. Its combination of high abundances in the intermediate mass elements from Si to Ca and an a-spherical morphology make it an interesting test case for supernova models. We have followed up on this result with deeper observations using {\em XMM} and {\em Chandra}. These new data show that the abundance ratios from Ne to Fe are far from solar, with little evidence for Fe-K emission, and a Ca to Si ratio that is at least 3.1 times their solar ratio at the 99% confidence. Comparing these abundances with the total production factors of a wide range of core-collapse and type Ia models, we find that it is difficult to achieve such a non-solar abundance pattern of Si, S, Ar and Ca in a core-collapse model. Although a 12 M\odot model by Woosley & Weaver 1995 cannot be ruled out, a delayed detonation type Ia model is more plausible. Furthermore, comparisons of the overall SNR spectrum with the X-ray emission from the remnant of a type Ia SN calculated by Badenes et al.\ (2003), show that a delayed detonation model may be a promising explosion mechanism. It qualitatively reproduces the continuum temperature, the absolute and relative abundances of Ne, Mg, Si, S, Ca, and Fe, and the ionization states of Si and S of G337.2-0.7 remarkably well at a reasonable age for the remnant.
C. Rakowski acknowledges support for this work from NASA GXXXXX.
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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.