Статья

XRF 100316D/SN 2010bh AND THE NATURE OF GAMMA-RAY BURST SUPERNOVAE

Z. CanoAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]D. BersierAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]C. GuidorziAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]S. KobayashiAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]A. J. LevanDepartment of Physics, University of Warwick, Coventry, UKN. R. TanvirDepartment of Physics and Astronomy, University of Leicester, Leicester, UKK. WiersemaDepartment of Physics and Astronomy, University of Leicester, Leicester, UKP. D’AvanzoINAF-Osservatorio Astronomico di Brera, 23807 Merate, LC, ItalyA. S. FruchterSpace Telescope Science Institute, Baltimore, MD, USAP. GarnavichPhysics Department, University of Notre Dame, Notre Dame, IN, USAA. GombocCentre of Excellence SPACE-SI, SI-1000 Ljubljana, SloveniaJ. GorosabelInstituto de Astrofísica de Andalucía (IAA-CSIC), Granada, SpainDaniel KasenDepartment of Astronomy and Astrophysics, UC Berkeley, Berkeley CA, USAD. KopačFaculty of Mathematics and Physics, University of Ljubljana, Ljubljana, SloveniaR. MarguttiINAF-Osservatorio Astronomico di Brera, 23807 Merate, LC, ItalyP. A. MazzaliINAF Oss. Astron. Padova, Padova, ItalyA. MelandriAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]C. G. MundellAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]P. NugentComputational Cosmology Center, Lawrence Berkeley National Laboratory, Berkeley, CA, USAE. PianINAF Oss. Astron. Padova, Padova, ItalyR. J. SmithAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]I. A. SteeleAstrophysics Research Institute, Liverpool John Moores University, Liverpool, UK; [email protected]R. A. M. J. WijersAstronomical Institute, University of Amsterdam, XH Amsterdam, The NetherlandsS. E. WoosleyDepartment of Physics, University of California, Santa Cruz, CA, USA

2011en

ABI

Аннотация

We present ground-based and HST optical and infrared observations of XRF 100316D / SN 2010bh. It is seen that the optical light curves of SN 2010bh evolve at a faster rate than the archetype GRB-SN 1998bw, but at a similar rate to SN 2006aj, a supernova that was spectroscopically linked with XRF 060218, and at a similar rate to non-GRB associated type Ic SN 1994I. We estimate the rest-frame extinction of this event from our optical data to be E(B-V)=0.18 +/- 0.08 mag. We find the V-band absolute magnitude of SN 2010bh to be M_{V}=-18.62 +/- 0.08, which is the faintest peak V-band magnitude observed to-date for a spectroscopically-confirmed GRB-SNe. When we investigate the origin of the flux at t-t_{o}=0.598 days, it is shown that the light is not synchrotron in origin, but is likely coming from the supernova shock break-out. We then use our optical and infrared data to create a quasi-bolometric light curve of SN 2010bh which we model with a simple analytical formula. The results of our modeling imply that SN 2010bh synthesized a nickel mass of M_{Ni}=0.10 +/- 0.01 M_{\\odot}, ejected M_{ej}=2.24 +/- 0.08 M_{\\odot} and has an explosion energy of E_{k}=1.39 +/- 0.06 x 10^{52} erg (where the quoted errors are statistical only; we discuss the potential sources of the systematic errors in the text). Finally, for a sample 20 GRB-SNe we check for a correlation between the stretch factors and luminosity factors in the R band and conclude that no statistically-significant correlation exists.

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Идентификаторы

DOI: 10.1088/0004-637x/740/1/41

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Цитирований: 2Использованных источников: 0

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