A spectroscopically normal type Ic supernova from a very massive progenitor

Stefano Valenti, Stefan Taubenberger, Andrea Pastorello, Levon Aramyan, Maria Teresa Botticella, Morgan Fraser, Stefano Benetti, Stephen J. Smartt, Enrico Cappellaro, Nancy Elias-Rosa, Mattias Ergon, Lindsay Magill, Eugene Magnier, Rubina Kotak, Paul A. Price, Jesper Sollerman, Lina Tomasella, Massimo Turatto, Darryl E. Wright

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Abstract

We present observations of the Type Ic supernova (SN Ic) 2011bm spanning a period of about one year. The data establish that SN 2011bm is a spectroscopically normal SN Ic with moderately low ejecta velocities and with a very slow spectroscopic and photometric evolution (more than twice as slow as SN 1998bw). The Pan-STARRS1 retrospective detection shows that the rise time from explosion to peak was 40days in the R band. Through an analysis of the light curve and the spectral sequence, we estimate a kinetic energy of 7-17 foe and a total ejected mass of 7-17 M , 5-10 M of which is oxygen and 0.6-0.7 M is 56Ni. The physical parameters obtained for SN 2011bm suggest that its progenitor was a massive star of initial mass 30-50 M . The profile of the forbidden oxygen lines in the nebular spectra shows no evidence of a bi-polar geometry in the ejected material.

Original languageEnglish (US)
Article numberL28
JournalAstrophysical Journal Letters
Volume749
Issue number2
DOIs
StatePublished - Apr 20 2012

Keywords

  • supernovae: general
  • supernovae: individual (SN 2011bm)

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