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R. Sankrit, W. P. Blair, J. Cheng (JHU), J. C. Raymond, T. Gaetz, A. Szentgyorgyi (SAO), C. W. Danforth (U. Colorado)
The XA region on the eastern limb of the Cygnus Loop supernova remnant has been formed by a shock-cloud interaction. We present spectra of the XA region obtained with the Far Ultraviolet Spectroscopic Explorer, which operates in the 900--1200Å\ wavelength region. Six locations were observed in order to study different parts of the shocked region, from the dense cloud core to associated lower density gas. The spectra show numerous emission lines from several elements and a range of ionization stages. The measured line strengths and line ratios show the presence of shocks with velocities ranging from about 120~km~s-1 to over 180~km~s-1. They also indicate that elemental abundances are probably solar. By comparing the measurements at the six locations observed by FUSE with ground based images, we find that the O~VI~\lambda1032 emission is more uniformly distributed than the [Ne~V]~\lambda3426 emission, though both O5+ and Ne4+ trace gas at similar levels of ionization. The difference could be due to resonance line scattering of O~VI, or because [Ne~V] comes from a more restricted temperature range.
We acknowledge support from NASA grant NAG5-11581 to the Johns Hopkins University.
The author(s) of this abstract have provided an email address for comments about the abstract: ravi@pha.jhu.edu
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Bulletin of the American Astronomical Society, 36 5
© 2004. The American Astronomical Society.