The highly energetic expansion of SN 2010bh associated with GRB 100316D

Filomena Bufano, Elena Pian, Jesper Sollerman, Stefano Benetti, Giuliano Pignata, Stefano Valenti, Stefano Covino, Paolo D'Avanzo, Daniele Malesani, Enrico Cappellaro, Massimo Della Valle, Johan Fynbo, Jens Hjorth, Paolo A. Mazzali, Daniel E. Reichart, Rhaana L.C. Starling, Massimo Turatto, Susanna D. Vergani, Klass Wiersema, Lorenzo AmatiDavid Bersier, Sergio Campana, Zach Cano, Alberto J. Castro-Tirado, Guido Chincarini, Valerio D'Elia, Antonio De Ugarte Postigo, Jinsong Deng, Patrizia Ferrero, Alexei V. Filippenko, Paolo Goldoni, Javier Gorosabel, Jochen Greiner, Francois Hammer, Pall Jakobsson, Lex Kaper, Koji S. Kawabata, Sylvio Klose, Andrew J. Levan, Keiichi Maeda, Nicola Masetti, Bo Milvang-Jensen, Felix I. Mirabel, Palle Moller, Ken'Ichi Nomoto, Eliana Palazzi, Silvia Piranomonte, Ruben Salvaterra, Giulia Stratta, Gianpiero Tagliaferri, Masaomi Tanaka, Nial R. Tanvir, Ralph A.M.J. Wijers

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Abstract

We present the spectroscopic and photometric evolution of the nearby (z = 0.059) spectroscopically confirmed Type Ic supernova, SN2010bh, associated with the soft, long-duration gamma-ray burst (X-ray flash) GRB100316D. Intensive follow-up observations of SN2010bh were performed at the ESO Very Large Telescope (VLT) using the X-shooter and FORS2 instruments. Thanks to the detailed temporal coverage and the extended wavelength range (3000-24800Å), we obtained an unprecedentedly rich spectral sequence among the hypernovae, making SN2010bh one of the best studied representatives of this SN class. We find that SN2010bh has a more rapid rise to maximum brightness (8.0 ± 1.0 rest-frame days) and a fainter absolute peak luminosity (L bol ≈ 3 × 1042 erg s-1) than previously observed SN events associated with GRBs. Our estimate of the ejected 56Ni mass is 0.12 ± 0.02 M o. From the broad spectral features, we measure expansion velocities up to 47,000kms-1, higher than those of SNe 1998bw (GRB980425) and 2006aj (GRB060218). Helium absorption lines He I λ5876 and He I 1.083 μm, blueshifted by 20,000-30,000kms-1 and 28,000-38,000kms-1, respectively, may be present in the optical spectra. However, the lack of coverage of the He I 2.058 μm line prevents us from confirming such identifications. The nebular spectrum, taken at 186days after the explosion, shows a broad but faint [O I] emission at 6340Å. The light curve shape and photospheric expansion velocities of SN2010bh suggest that we witnessed a highly energetic explosion with a small ejected mass (E k ≈ 1052 erg and M ej ≈ 3 Mo). The observed properties of SN2010bh further extend the heterogeneity of the class of GRB SNe.

Original languageEnglish
Article number67
JournalAstrophysical Journal
Volume753
Issue number1
DOIs
Publication statusPublished - 2012 Jul 1

Keywords

  • supernovae: general
  • supernovae: individual (SN 2010bh, GRB 100316D)

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Bufano, F., Pian, E., Sollerman, J., Benetti, S., Pignata, G., Valenti, S., Covino, S., D'Avanzo, P., Malesani, D., Cappellaro, E., Della Valle, M., Fynbo, J., Hjorth, J., Mazzali, P. A., Reichart, D. E., Starling, R. L. C., Turatto, M., Vergani, S. D., Wiersema, K., ... Wijers, R. A. M. J. (2012). The highly energetic expansion of SN 2010bh associated with GRB 100316D. Astrophysical Journal, 753(1), [67]. https://doi.org/10.1088/0004-637X/753/1/67