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A type Ia supernova is thought to be a thermonuclear explosion of either asingle carbon-oxygen white dwarf or of a pair of merging white dwarfs. Theexplosion fuses a large amount of radioactive 56Ni. After the explosion, thedecay chain from 56Ni to 56Co to 56Fe generates gamma-ray photons, which arereprocessed in the expanding ejecta and give rise to powerful optical emission.Here we report the detection of 56Co lines at energies of 847 and 1238 keV anda gamma-ray continuum in the 200-400 keV band from the type Ia supernova 2014Jin the nearby galaxy M82. The line fluxes suggest that about 0.6 +/- 0.1 solarmasses of radioactive 56Ni were synthesized during the explosion. The linebroadening gives a characteristic mass-weighted ejecta expansion velocity of10000 +/- 3000 km/s. The observed gamma-ray properties are in broad agreementwith the canonical model of an explosion of a white dwarf just massive enoughto be unstable to gravitational collapse, but do not immediately exclude morecomplicated merger scenarios, which fuse comparable amount of 56Ni.

Cobalt-56 gamma-ray emission lines from the type Ia supernova 2014J