Published in

American Astronomical Society, Astrophysical Journal Letters, 2(749), p. L28, 2012

DOI: 10.1088/2041-8205/749/2/l28

Links

Tools

Export citation

Search in Google Scholar

A spectroscopically normal type Ic supernova from a very massive progenitor

Journal article published in 2012 by Stefano Valenti, Inaf-Osservatorio Astronomico di Padova, Stefan Taubenberger, Andrea Pastorello, Levon Aramyan, Maria Teresa Botticella ORCID, Morgan Fraser ORCID, Stefano Benetti, Stephen J. Smartt, Enrico Cappellaro ORCID, Nancy Elias-Rosa, Mattias Ergon, Lindsay Magill, Eugene Magnier, Rubina Kotak ORCID and other authors.
This paper is made freely available by the publisher.
This paper is made freely available by the publisher.

Full text: Download

Red circle
Preprint: archiving forbidden
Red circle
Postprint: archiving forbidden
Green circle
Published version: archiving allowed
Upload
Policy details
Data provided by SHERPA/RoMEO

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 40 days 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 Mo, 5-10 Mo of which is oxygen and 0.6-0.7 Mo is 56Ni. The physical parameters obtained for SN 2011bm suggest that its progenitor was a massive star of initial mass 30-50 Mo. The profile of the forbidden oxygen lines in the nebular spectra show no evidence of a bi-polar geometry in the ejected material. ; Comment: 3 Figures - 2 Tables - Accepted for publication in ApJL