Volume 588, April 2016
|Number of page(s)||11|
|Published online||18 March 2016|
Gamma-ray emission from SN2014J near maximum optical light ⋆
1 Institut de Ciències de l’Espai (ICE-CSIC/IEEC), Campus UAB, 08193 Bellaterra, Barcelona, Spain
2 Université de Toulouse, UPS-OMP, IRAP, 31028 Toulouse, France
3 IRAP, 9 Av colonel Roche, BP44346, 31028 Toulouse Cedex 4, France
4 E.T.S.A.V., Univ. Politècnica de Catalunya, c/Pere Serra 1-15, 08173 Sant Cugat del Valles, Spain
5 APC, Univ. Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs. de Paris, Sorbonne Paris Cité, 10 rue Alice Domon et Leonie Duquet, 75205 Paris Cedex 13, France
6 Space Research Institute (IKI), Proufsouznaya 84/32, 117997 Moscow, Russia
7 Max-Planck-Institut for Astrophysics, Karl-Schwarzschild-Strasse 1, 85741 Garching, Germany
8 Centro de Astrobiología (CAB-CSIC/INTA), PO Box 78, 28691 Villanueva de la Cañada, Madrid, Spain
9 Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics and Cosmology Center (PITT-PACC), University of Pittsburgh, Pittsburgh PA15260, USA
10 Department of Physics and Astronomy, Clemson University, Clemson, SC 29634, USA
11 Physics Department, Florida State University, Tallaharssee, FL32306, USA
12 Laboratoire Univers et Particules de Montpellier (LUPM), UMR 5299, Université de Montpellier II, 34095 Montpellier, France
13 INAF–Osservatorio Astronomico di Padua, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
14 Universidad de Granada, Cuesta del Hospicio sn, 18071 Granada, Spain
15 Dept. Fisica, UPC, Compte d’Ugell 187, 08036 Barcelona, Spain
16 Max-Planck-Institut for Extraterrestrial Physics, Giessenbachstrasse 1, 85741 Garching, Germany
Received: 11 July 2015
Accepted: 8 February 2016
Context. The optical light curve of Type Ia supernovae (SNIa) is powered by thermalized gamma-rays produced by the decay of 56Ni and 56Co, the main radioactive isotopes synthesized by the thermonuclear explosion of a C/O white dwarf.
Aims. Gamma-rays escaping the ejecta can be used as a diagnostic tool for studying the characteristics of the explosion. In particular, it is expected that the analysis of the early gamma emission, near the maximum of the optical light curve, could provide information about the distribution of the radioactive elements in the debris.
Methods. The gamma data obtained from SN2014J in M 82 by the instruments on board INTEGRAL were analysed paying special attention to the effect that the detailed spectral response has on the measurements of the intensity of the lines.
Results. The 158 keV emission of 56Ni has been detected in SN2014J at ~5σ at low energy with both ISGRI and SPI around the maximum of the optical light curve. After correcting the spectral response of the detector, the fluxes in the lines suggest that, in addition to the bulk of radioactive elements buried in the central layers of the debris, there is a plume of 56Ni, with a significance of ~3σ, moving at high velocity and receding from the observer. The mass of the plume is in the range of ~0.03−0.08 M⊙.
Conclusions. No SNIa explosion model has ever predicted the mass and geometrical distribution of 56Ni suggested here. According to its optical properties, SN2014J looks like a normal SNIa, so it is extremely important to discern whether it is also representative in the gamma-ray band.
Key words: supernovae: individual: SN2014J / gamma rays: stars
© ESO, 2016
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