Spectrophotometry of young supernova remnants

Details Spectrophotometry of young supernova remnants Spectrophotometry of young supernova remnants

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...282..135d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 282, July 1, 1984, p. 135-141.

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38

Astronomical Spectroscopy, Magellanic Clouds, Spectrophotometry, Supernova Remnants, Abundance, Neon, Oxygen Spectra

Scientific paper

Spectrophotometric data are presented for four young oxygen-rich supernova remnants: G292.0 + 1.8 in the Galaxy, N132D and 0540-69.3 in the Large Magellanic Cloud, and 1E 0102.2-7219 in the Small Magellanic Cloud. Although these data are insufficient to derive unique physical conditions and chemical abundances in the remnants, they serve to show that a common physical process is responsible for the excitation in all four remnants. Sensitive upper limits are also derived on emission from elements other than oxygen and neon from global spectra of N132D and 1E 0102.2-7219 of very high signal-to-noise ratio, and it is shown that 0540-69.3 is peculiar in its chemical composition, probably resulting from optical excitation of material from the innermost zones of the ejecta from a massive precursor star.

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