Year: 2012
Type: article
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 M ☉ , 5–10 M ☉ of which is oxygen and 0.6–0.7 M ☉ is 56 Ni. 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.
Authors: 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
Institutions: Osservatorio Astronomico di Padova, Max Planck Institute for Astrophysics, Yerevan State University, Astronomical Observatory of Capodimonte, Queen's University Belfast, Institute of Space Sciences, Consejo Superior de Investigaciones Científicas, Stockholm University, AlbaNova, University of Hawaiʻi at Mānoa, University of Hawaii System, Princeton University
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: bronze
Awards: G1140430070, G1182715895
OpenAlex ID: W2059906956