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Title:
The Type IC Supernova 1994I in M51: Detection of Helium and Spectral Evolution
Authors:
Filippenko, Alexei V.; Barth, Aaron J.; Matheson, Thomas; Armus, Lee; Brown, Michael; Espey, Brian R.; Fan, Xiao-Ming; Goodrich, Robert W.; Ho, Luis C.; Junkkarinen, Vesa T.; Koo, David C.; Lehnert, Matthew D.; Martel, Andre R.; Mazzarella, Joseph M.; Miller, Joseph S.; Smith, Graeme H.; Tytler, David; Wirth, Gregory D.
Publication:
Astrophysical Journal Letters v.450, p.L11 (ApJ Homepage)
Publication Date:
09/1995
Origin:
APJ; KNUDSEN
ApJ Keywords:
STARS: BINARIES: CLOSE, STARS: EVOLUTION, STARS: MASS LOSS, STARS: SUPERNOVAE: GENERAL, STARS: SUPERNOVAE: INDIVIDUAL ALPHANUMERIC: SN 1984L, STARS: SUPERNOVAE: INDIVIDUAL ALPHANUMERIC: SN 1987M, STARS: SUPERNOVAE: INDIVIDUAL ALPHANUMERIC: SN 1994I
DOI:
10.1086/309659
Bibliographic Code:
1995ApJ...450L..11F

Abstract

We present a series of spectra of SN 1994I in M51, starting 1 week prior to maximum brightness. The nebular phase began about 2 months after the explosion; together with the rapid decline of the optical light, this suggests that the ejected mass was small. Although lines of He I in the optical region are weak or absent, consistent with the Type Ic classification, we detect strong He I lambda 10830 absorption during the first month past maximum. Thus, if SN 1994I is a typical Type Ic supernova, the atmospheres of these objects cannot be completely devoid of helium. The emission-line widths are smaller than predicted by the model of Nomoto and coworkers, in which the iron core of a low-mass carbon-oxygen star collapses. They are, however, larger than in Type Ib supernovae.

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