Other
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aas...204.7407b&link_type=abstract
American Astronomical Society Meeting 204, #74.07; Bulletin of the American Astronomical Society, Vol. 36, p.803
Other
Scientific paper
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 λ 1032 to Fabry-Perot data of [OIII λ 5007] emission. The velocity structure is clearly similar in both emission lines. We note that there is no detected C III λ 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.
Beasley Matthew
Blair William Patrick
Dopita Mike A.
Green James C.
Morse Jon A.
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