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M Beasley, J. A. Morse (Arizona State University), J. C. Green, E Wilkinson (University of Colorado at Boulder), W. P. Blair (Johns Hopkins University), M. A. Dopita (Institute of Advanced Studies), J. C. Raymond (Harvard Smithsonian Center for Astrophysics), P. F. Winkler (Middlebury College)
N132D, a young oxygen-rich supernova remnant (SNR) in the Large Magellanic Cloud is an excellent laboratory to study FUV emission from shocked ejecta. Most oxygen-rich SNR lie in the galactic plane thus with relatively high extinction. The low extinction toward the LMC, as compared to galactic oxygen-rich SNR, allow us to make FUV observations of shocked metal-rich stellar ejecta.
We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations of filaments within N132D and compare the velocity structure in OVI \lambda 1032 to Fabry-Perot data of [OIII \lambda 5007] emission. The velocity structure is clearly similar in both emission lines. We note that there is no detected C III \lambda 977 from this source, as compared to the Puppis A SNR. In addition, the relative lack of Carbon lines imply that the observed filament may have a different chemical composition that other ejecta filaments within the same SNR.
This work was supported by NASA grants NAG5-8955, NAG5-10319, and NAG5-50340.
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Bulletin of the American Astronomical Society, 36 #2
© YEAR. The American Astronomical Soceity.