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The Type I[CLC]c[/CLC] Supernova 1994I in M51: Detection of Helium and Spectral Evolution

A. V. FilippenkoCenter for Particle Astrophysics, University of California, Berkeley, CA 94720Aaron J. BarthDepartment of Astronomy, University of California, Berkeley, CA 94720T. MathesonDepartment of Astronomy, University of California, Berkeley, CA 94720L. ArmusDowns Laboratory of Physics, 320-47 Caltech, Pasadena, CA 91125Michael E. BrownCurrent address: Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721B. R. EspeyCenter for Astrophysical Sciences, Johns Hopkins University, Baltimore, MD 21218Xiao-Ming FanCenter for Astrophysics and Space Sciences, University of California, San Diego, CA 92093Robert W. GoodrichCurrent address: Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218Luis C. HoDepartment of Astronomy, University of California, Berkeley, CA 94720V. T. JunkkarinenCenter for Astrophysics and Space Sciences, University of California, San Diego, CA 92093David C. KooLick Observatory, University of California, Santa Cruz, CA 95064M. D. LehnertInstitute of Geophysics and Planetary Physics, Lawrence Livermore National Laboratory, P.O. Box 808, L-413, Livermore, CA 94550A. R. MartelLick Observatory, University of California, Santa Cruz, CA 95064J. M. MazzarellaInfrared Processing and Analysis CenterJoseph S. MillerLick Observatory, University of California, Santa Cruz, CA 95064Graeme H. SmithLick Observatory, University of California, Santa Cruz, CA 95064David TytlerCenter for Astrophysics and Space Sciences, University of California, San Diego, CA 92093Gregory D. WirthLick Observatory, University of California, Santa Cruz, CA 95064

1995en

ABI

Annotatsiya

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 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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DOI: 10.1086/309659

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