A Far Ultraviolet Spectrum of the Puppis A Supernova Remnant Using the Hopkins Ultraviolet Telescope

William P. Blair
Department of Physics and Astronomy, The Johns Hopkins University, 34th & Charles Streets, Baltimore, MD 21218
E-mail:wpb@pha.jhu.edu

John C. Raymond
Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138
E-mail: raymond@cfa.harvard.edu

Knox S. Long
Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218
E-mail: long@stsci.edu

and

Gerard A. Kriss
Department of Physics and Astronomy, The Johns Hopkins University, 34th & Charles Streets, Baltimore, MD 21218
E-mail: gak@pha.jhu.edu

Abstract:

We report the first successful far-ultraviolet spectroscopic observation of a filament in the Puppis A supernova remnant. We observed a position on the eastern side of the remnant near the brightest X-ray region using the Hopkins Ultraviolet Telescope during the Astro-2 space shuttle mission in March 1995. The spectrum covers the 820 - 1840 Å spectral range with 3 Å resolution and shows numerous lines of C, N, O, Ne, He, and possibly Si. Comparison of this spectrum to solar abundance shock models indicates a shock velocity of approximately 160 - 180 . A slight overabundance of N is possible for this position, consistent with a shocked ISM picture for the observed filament. This is at odds with the much larger overabundance of N indicated by optical data from other regions of the outer shell in Puppis A. Comparison with optical CCD interference filter images obtained at Las Campanas Observatory and with Einstein HRI data indicates that the region observed corresponds to a very recent encounter between the blast wave and an interstellar cloud. The interaction of the shock wave with this cloud is responsible for the bright X-ray emission in this region.

Subject headings: ISM: supernova remnants -- ISM: individual (Puppis A)



wpb@pha.jhu.edu