Forbidden lines of SI I - an alternate interpretation for an infrared emission feature in the spectrum of SN 1983N (M83)

Details Forbidden lines of SI I - an alternate interpretation for an infrared emission feature in the spectrum of SN 1983N (M83) Forbidden lines of SI I - an alternate interpretation for an infrared emission feature in the spectrum of SN 1983N (M83)

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987apj...321l..45o&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 321, Oct. 1, 1987, p. L45-L49.

Astronomy and Astrophysics

Astrophysics

15

Forbidden Transitions, Infrared Spectra, Silicon, Stellar Models, Supernovae, Abundance, Spectroscopic Analysis, Stellar Composition, Stellar Spectra

Scientific paper

An alternate interpretation for the IR spectral feature observed in SN 1983N is presented and analyzed. The low-resolution CVF spectrum published by Graham et al. in 1986 around 1.644 microns, originally interpreted in terms of forbidden Fe II lines, can be fitted assuming pure forbidden Si I emission (1.6454 and 1.6068-micron lines) obtaining a result as good as that of a synthetic forbidden Fe II spectrum. The mass of silicon inferred from the observed 1.6454-micron flux is consistent with carbon deflagration models. The Si/O relative abundance is significantly lower than the standard solar value, in agreement with current ideas concerning Type Ib supernovae. As forbidden optical lines (below 8000 A) of both Si I and Fe II are intrinsically faint, no evidence capable of distinguishing between the two hypotheses can be found in the existing observational data. Future ground-based IR spectral observations should, therefore, include the 1.10 and 1.26-micron spectral regions where bright and clean forbidden lines of Si I and Fe II (respectively) lie.

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