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M. Sasaki, T.J. Gaetz (Harvard-Smithsonian Center for Astrophysics), W.P. Blair (The Johns Hopkins University), R.J. Edgar (Harvard-Smithsonian Center for Astrophysics), J.A. Morse (Arizona State University), P.P. Plucinsky (Harvard-Smithsonian Center for Astrophysics)
We observed the O-rich supernova remnant (SNR) 1E 0102.2-7219 in the Small Magellanic Cloud (SMC) with the Far Ultraviolet Spectroscopic Explorer (FUSE). We used the medium resolution aperture (MDRS) in three pointings which covered regions of the bright X-ray ring with different distribution of [O III] in the optical and O VII, O VIII in the X-ray. The ring is caused by the reverse shock propagating in the hot ejecta. In the northern region (N), the FUSE spectrum shows very faint O VI emission. In the northeastern (NE) and the southeastern (SE) parts of the SNR ring, there is significant UV O VI emission with broad O VI lambda lambda 1032, 1038 lines, indicating a velocity dispersion of about 1200 km/s. The emission from the SE pointing appears to be blue-shifted by a few hundred km/s relative to the emission from the NE pointing.
We also analyzed the Chandra ACIS spectra of 1E 0102.2-7219 in the same regions as in the FUSE observations. The fit with a plane-parallel shock plasma model shows that the plasma is in non-equilibrium ionization with a mean shock temperature of ~2 keV. O and Ne abundances are high (1 - 2 times solar), whereas Fe is sub-solar in all the regions. The ionization timescale ne t is highest in N (> 1011 s cm-3). The velocities and fluxes derived from the O VI emission in UV as well as from the X-ray emission will help to improve the understanding of the structure of the ejecta and thus give hints about the supernova explosion.
This work was supported by the NASA/FUSE grant NAG5-12295, CXC contract NAS8-03060, and NASA grant GO1-2060X.
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Bulletin of the American Astronomical Society, 36 #3
© 2004. The American Astronomical Soceity.