THE HIGHLY ENERGETIC EXPANSION OF SN 2010bh ASSOCIATED WITH GRB 100316D
- INAF-Osservatorio Astronomico di Catania, Via Santa Sofia, I-95123, Catania (Italy)
- INAF-Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11, I-34143 Trieste (Italy)
- Oskar Klein Centre, Department of Astronomy, AlbaNova, SE-106 91 Stockholm (Sweden)
- INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, I-35122 Padova (Italy)
- Departamento de Ciencias Fisicas, Universidad Andres Bello, Av. Republica 252, Santiago (Chile)
- INAF-Osservatorio Astronomico di Brera, Via Emilio Bianchi 46, Merate I-23807 (Italy)
- Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen (Denmark)
- INAF-Osservatorio Astronomico di Capodimonte, Salita Moiariello, 16, I-8013 Napoli (Italy)
- Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Campus Box 3255, Chapel Hill, NC 27599-3255 (United States)
- Department of Physics and Astronomy, University of Leicester, University Road, Leicester LE1 7RH (United Kingdom)
- INAF-Istituto di Astrofisica Spaziale e Fisica cosmica, Via Gobetti 101, I-40129 Bologna (Italy)
We 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 A), 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{sub bol} Almost-Equal-To 3 Multiplication-Sign 10{sup 42} erg s{sup -1}) than previously observed SN events associated with GRBs. Our estimate of the ejected {sup 56}Ni mass is 0.12 {+-} 0.02 M{sub Sun }. From the broad spectral features, we measure expansion velocities up to 47,000 km s{sup -1}, higher than those of SNe 1998bw (GRB 980425) and 2006aj (GRB 060218). Helium absorption lines He I {lambda}5876 and He I 1.083 {mu}m, blueshifted by {approx}20,000-30,000 km s{sup -1} and {approx}28,000-38,000 km s{sup -1}, respectively, may be present in the optical spectra. However, the lack of coverage of the He I 2.058 {mu}m line prevents us from confirming such identifications. The nebular spectrum, taken at {approx}186 days after the explosion, shows a broad but faint [O I] emission at 6340 A. 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{sub k} Almost-Equal-To 10{sup 52} erg and M{sub ej} Almost-Equal-To 3 M{sub Sun }). The observed properties of SN 2010bh further extend the heterogeneity of the class of GRB SNe.
- OSTI ID:
- 22036886
- Journal Information:
- Astrophysical Journal, Vol. 753, Issue 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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