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Filomena Bufano et al. 2012 ApJ 753 67 doi:10.1088/0004-637X/753/1/67
Filomena Bufano1,2,38, Elena Pian3,4,5, Jesper Sollerman6, Stefano Benetti7, Giuliano Pignata2, Stefano Valenti7, Stefano Covino8, Paolo D'Avanzo8, Daniele Malesani9, Enrico Cappellaro7, Massimo Della Valle10,11, Johan Fynbo9, Jens Hjorth9, Paolo A. Mazzali7,12, Daniel E. Reichart13, Rhaana L. C. Starling14, Massimo Turatto3, Susanna D. Vergani8, Klass Wiersema14, Lorenzo Amati15, David Bersier16, Sergio Campana8, Zach Cano16, Alberto J. Castro-Tirado17, Guido Chincarini18, Valerio D'Elia19,20, Antonio de Ugarte Postigo9, Jinsong Deng21, Patrizia Ferrero22, Alexei V. Filippenko23, Paolo Goldoni24,25, Javier Gorosabel17, Jochen Greiner26, Francois Hammer27, Pall Jakobsson28, Lex Kaper29, Koji S. Kawabata30, Sylvio Klose31, Andrew J. Levan32, Keiichi Maeda33, Nicola Masetti34, Bo Milvang-Jensen9, Felix I. Mirabel25,35, Palle Møller36, Ken'ichi Nomoto33, Eliana Palazzi34, Silvia Piranomonte19, Ruben Salvaterra37, Giulia Stratta19, Gianpiero Tagliaferri8, Masaomi Tanaka33, Nial R. Tanvir14, and Ralph A. M. J. Wijers29
Show affiliationsWe present the spectroscopic and photometric evolution of the nearby (z = 0.059) spectroscopically confirmed Type Ic supernova, SN 2010bh, associated with the soft, long-duration gamma-ray burst (X-ray flash) GRB 100316D. Intensive follow-up observations of SN 2010bh 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 (3000-24800 Å), we obtained an unprecedentedly rich spectral sequence among the hypernovae, making SN 2010bh one of the best studied representatives of this SN class. We find that SN 2010bh 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 ☉. From the broad spectral features, we measure expansion velocities up to 47,000 km s–1, higher than those of SNe 1998bw (GRB 980425) and 2006aj (GRB 060218). Helium absorption lines He I λ5876 and He I 1.083 μm, blueshifted by ~20,000-30,000 km s–1 and ~28,000-38,000 km s–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 ~186 days after the explosion, shows a broad but faint [O I] emission at 6340 Å. The light curve shape and photospheric expansion velocities of SN 2010bh suggest that we witnessed a highly energetic explosion with a small ejected mass (E k 1052 erg and M ej 3 M ☉). The observed properties of SN 2010bh further extend the heterogeneity of the class of GRB SNe.
supernovae: general; supernovae: individual (SN 2010bh, GRB 100316D)
Issue 1 (2012 July 1)
Received 2011 November 8, accepted for publication 2012 May 1
Published 2012 June 14
Total article downloads: 690
Filomena Bufano et al. 2012 ApJ 753 67
E. Göğüş et al. 2010 ApJ 718 331
A. J. Levan et al. 2014 ApJ 781 13
Adria C. Updike et al. 2008 ApJ 685 361
A. J. van der Horst et al. 2011 ApJ 726 99
