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ID 34778
file
creator
Bufano, Filomena
Pian, Elena
Sollerman, Jesper
Benetti, Stefano
Pignata, Giuliano
Valenti, Stefano
Covino, Stefano
Avanzo, Paolo D'
Malesani, Daniele
Cappellaro, Enrico
Valle, Massimo Della
Fynbo, Johan
Hjorth, Jens
Mazzali, Paolo A.
Reichart, Daniel E.
Starling, Rhaana L. C.
Turatto, Massimo
Vergani, Susanna D.
Wiersema, Klass
Amati, Lorenzo
Bersier, David
Campana, Sergio
Cano, Zach
Castro-Tirado, Alberto J.
Chincarini, Guido
Elia, Valerio D'
Postigo, Antonio de Ugarte
Deng, Jinsong
Ferrero, Patrizia
Filippenko, Alexei V.
Goldoni, Paolo
Gorosabel, Javier
Greiner, Jochen
Hammer, Francois
Jakobsson, Pall
Kaper, Lex
Kawabata, Koji S.
Klose, Sylvio
Levan, Andrew J.
Maeda, Keiichi
Masetti, Nicola
Milvang-Jensen, Bo
Mirabel, Felix I.
Moller, Palle
Nomoto, Ken'ichi
Palazzi, Eliana
Piranomonte, Silvia
Salvaterra, Ruben
Stratta, Giulia
Tagliaferri, Gianpiero
Tanaka, Masaomi
Tanvir, Nial R.
Wijers, Ralph A. M. J.
subject
supernovae: general
supernovae: individual (SN 2010bh, GRB 100316D)
NDC
Astronomy. Space sciences
abstract
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 angstrom), 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 approximate to 3 x 10(42) erg s(-1)) than previously observed SN events associated with GRBs. Our estimate of the ejected Ni-56 mass is 0.12 +/- 0.02 M-circle dot. 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 lambda 5876 and He I 1.083 mu m, blueshifted by similar to 20,000-30,000 km s(-1) and similar to 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 mu m line prevents us from confirming such identifications. The nebular spectrum, taken at similar to 186 days after the explosion, shows a broad but faint [O I] emission at 6340 angstrom. 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 approximate to 10(52) erg and M-ej approximate to 3 M-circle dot). The observed properties of SN 2010bh further extend the heterogeneity of the class of GRB SNe.
journal title
Astrophysical Journal
volume
Volume 753
issue
Issue 1
start page
67
date of issued
2012
publisher
IOP Publishing Ltd
issn
0004-637X
ncid
publisher doi
language
eng
nii type
Journal Article
HU type
Journal Articles
DCMI type
text
format
application/pdf
text version
publisher
rights
(c) 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A.
relation url
department
Hiroshima Astrophysical Science Center



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