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R. Soule, Y. Wen, J.W. Keohane, C.M. Olbert, C.R. Clearfield (NCSSM)
Using public Chandra data of the supernova remnant Kes 75, we confirm the results of Collins, Gotthelf, & Helfand (2002) and we measure the radial velocities of the shell. Our analyses of the pulsar, the wind nebula, and the shell clumps confirm a column density of ~3.5E22/cm/cm and the existence of magnesium, silicon, and sulfur emission lines from the shell. Raymond-Smith fits of the shell clumps find magnesium, sulfur, silicon, and argon to be at least four times more concentrated than cosmic abundances in both shells. Despite these similarities, the two shell clumps have some significant differences: only the southwest clump displays aluminum and argon emission lines; the southwest clump contains significantly less magnesium; and, a comparison with radio data from the Very Large Array (data contributed by David Helfand) shows a strong spatial correlation between the X-ray and the radio in only the southwest clump. Our spectral fits indicate radial velocities of 2400km/s and 3200km/s for the southwest and southeast clumps, respectively. Because they are both moving away, we expect that the remnant is expanding into a higher density medium on its far side; however, no cloud of interstellar dust is obvious in the all-sky surveys.
The author(s) of this abstract have provided an email address for comments about the abstract: souler@ncssm.edu
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.