A type Ia supernova is thought to be a thermonuclear explosion of either a single carbon–oxygen white dwarf or a pair of merging white dwarfs. The explosion fuses a large amount of radioactive 56Ni (refs 1–3). After the explosion, the decay chain from 56Ni to 56Co to 56Fe generates γ-ray photons, which are reprocessed in the expanding ejecta and give rise to powerful optical emission. Here we report the detection of 56Co lines at energies of 847 and 1,238 kiloelectronvolts and a γ-ray continuum in the 200–400 kiloelectronvolt band from the type Ia supernova 2014J in the nearby galaxy M82. The line fluxes suggest that about 0.6 ± 0.1 solar masses of radioactive 56Ni were synthesized during the explosion. The line broadening gives a characteristic mass-weighted ejecta expansion velocity of 10,000 ± 3,000 kilometres per second. The observed γ-ray properties are in broad agreement with the canonical model of an explosion of a white dwarf just massive enough to be unstable to gravitational collapse, but do not exclude merger scenarios that fuse comparable amounts of 56Ni.
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Nomoto, K., Thielemann, F.-K. & Yokoi, K. Accreting white dwarf models of Type I supernovae. III - Carbon deflagration supernovae. Astrophys. J. 286, 644–658 (1984)
Woosley, S. E. & Weaver, T. A. The physics of supernova explosions. Annu. Rev. Astron. Astrophys. 24, 205–253 (1986)
Hillebrandt, W. & Niemeyer, J. C. Type Ia supernova explosion models. Annu. Rev. Astron. Astrophys. 38, 191–230 (2000)
Whelan, J. & Iben, I., Jr Binaries and supernovae of type I. Astrophys. J. 186, 1007–1014 (1973)
Iben, I., Jr & Tutukov, A. V. Supernovae of type I as end products of the evolution of binaries with components of moderate initial mass (M not greater than about 9 solar masses). Astrophys. J. Suppl. Ser. 54, 335–372 (1984)
Gilfanov, M. & Bogdán, Á. An upper limit on the contribution of accreting white dwarfs to the type Ia supernova rate. Nature 463, 924–925 (2010)
Röpke, F. K. et al. Constraining type Ia supernova models: SN 2011fe as a test case. Astrophys. J. 750, L19 (2012)
Malone, C. M. et al. The deflagration stage of Chandrasekhar mass models for type Ia supernovae. I. Early evolution. Astrophys. J. 782, 11 (2014)
Moll, R., Raskin, C., Kasen, D. & Woosley, S. E. Type Ia supernovae from merging white dwarfs. I. Prompt detonations. Astrophys. J. 785, 105 (2014)
The, L.-S. & Burrows, A. Expectations for the hard X-ray continuum and gamma-ray line fluxes from the type Ia supernova SN 2014J in M82. Astrophys. J. 786, 141 (2014)
Sunyaev, R. et al. Discovery of hard X-ray emission from supernova 1987A. Nature 330, 227–229 (1987)
Dotani, T., Hayashida, K., Inoue, H., Itoh, M. & Koyama, K. Discovery of an unusual hard X-ray source in the region of supernova 1987A. Nature 330, 230–231 (1987)
Matz, S. M., Share, G. H., Leising, M. D., Chupp, E. L. & Vestrand, W. T. Gamma-ray line emission from SN1987A. Nature 331, 416–418 (1988)
Teegarden, B. J., Barthelmy, S. D., Gehrels, N., Tueller, J. & Leventhal, M. Resolution of the 1,238-keV γ-ray line from supernova 1987A. Nature 339, 122–123 (1989)
Isern, J. et al. Observation of SN2011fe with INTEGRAL. I. Pre-maximum phase. Astron. Astrophys. 552, A97 (2013)
Fossey, S. Cooke, B. Pollack, G., Wilde, M. & Wright, T. Supernova 2014J in M82 = Psn J09554214+6940260. CBET 3792, (2014)
Zheng, W. & Filippenko, A. V. Prediscovery KAIT/LOSS detections of SN 2014J. Astron. Telegr. 5822, (2014)
Karachentsev, I. D. & Kashibadze, O. G. Masses of the local group and of the M81 group estimated from distortions in the local velocity field. Astrophysics 49, 3–18 (2006)
Winkler, C. et al. The INTEGRAL mission. Astron. Astrophys. 411, L1–L6 (2003)
Sazonov, S. Y., Lutovinov, A. A. & Krivonos, R. A. Cutoff in the hard X-ray spectra of the ultraluminous X-ray sources HoIX X-1 and M82 X-1. Astron. Lett. 40, 65–74 (2014)
Arnett, W. D. Type I supernovae. I - Analytic solutions for the early part of the light curve. Astrophys. J. 253, 785–797 (1982)
Margutti, R. et al. No X-rays from the very nearby Type Ia SN2014J: constraints on its environment. Astrophys. J. 790, 52 (2014)
Amanullah, R. et al. The peculiar extinction law of SN2014J measured with The Hubble Space Telescope. Astrophys. J. 788, L21 (2014)
Nadyozhin, D. K. The properties of NI to CO to Fe decay. Astrophys. J. Suppl. Ser. 92, 527–531 (1994)
Dwarkadas, V. V. & Chevalier, R. A. Interaction of type IA supernovae with their surroundings. Astrophys. J. 497, 807–823 (1998)
Woosley, S. E., Kasen, D., Blinnikov, S. & Sorokina, E. Type Ia supernova light curves. Astrophys. J. 662, 487–503 (2007)
Sunyaev, R. A. et al. Hard X-radiation from supernova 1987A: Roentgen Observatory observations from 1987 to 1989. Sov. Astron. Lett. 16, 171–176 (1990)
Badenes, C., Bravo, E., Borkowski, K. J. & Domínguez, I. Thermal X-ray emission from shocked ejecta in type Ia supernova remnants: prospects for explosion mechanism identification. Astrophys. J. 593, 358–369 (2003)
Hoeflich, P. & Khokhlov, A. Explosion models for type Ia supernovae: a comparison with observed light curves, distances, H0, and q0 . Astrophys. J. 457, 500–528 (1996)
Woosley, S. E. & Weaver, T. A. in Supernovae (eds Audouze, J., Bludman, S., Mochkovitch, R. & Zinn-Justin, J. ) 63–154 (Elsevier, 1991)
Kuulkers, E. INTEGRAL target of opportunity observations of the type Ia SN2014J in M82. Astron. Telegr. 5835, (2014)
Vedrenne, G. et al. SPI: the spectrometer aboard INTEGRAL. Astron. Astrophys. 411, L63–L70 (2003)
Churazov, E., Sunyaev, R., Sazonov, S., Revnivtsev, M. & Varshalovich, D. Positron annihilation spectrum from the Galactic Centre region observed by SPI/INTEGRAL. Mon. Not. R. Astron. Soc. 357, 1377–1386 (2005)
Churazov, E., Sazonov, S., Tsygankov, S., Sunyaev, R. & Varshalovich, D. Positron annihilation spectrum from the Galactic Centre region observed by SPI/INTEGRAL revisited: annihilation in a cooling ISM? Mon. Not. R. Astron. Soc. 411, 1727–1743 (2011)
Weidenspointner, G. et al. First identification and modelling of SPI background lines. Astron. Astrophys. 411, L113–L116 (2003)
Churazov, E., Gilfanov, M., Forman, W. & Jones, C. Mapping the gas temperature distribution in extended X-ray sources and spectral analysis in the case of low statistics: application to ASCA observations of clusters of galaxies. Astrophys. J. 471, 673–682 (1996)
Ubertini, P. et al. IBIS: the imager on-board INTEGRAL. Astron. Astrophys. 411, L131–L139 (2003)
Lebrun, F. et al. ISGRI: the INTEGRAL Soft Gamma-Ray Imager. Astron. Astrophys. 411, L141–L148 (2003)
INTREGAL. Science Data Centre. INTEGRAL http://isdc.unige.ch/integral (2014)
Nielsen, M. T. B. Gilfanov, M. Bogdán, Á., Woods, T. E. & Nelemans, G. Upper limits on the luminosity of the progenitor of type Ia supernova SN 2014J. Mon. Not. R. Astron. Soc. 442, 3400–3406 (2014)
Kelly, P. L. et al. Constraints on the progenitor system of the type Ia supernova 2014J from pre-explosion Hubble Space Telescope imaging. Astrophys. J. 790, 3 (2014)
Perez-Torres, M. A. et al. Constraints on the progenitor system and the environs of SN 2014J from deep radio observations. Preprint at http://arxiv.org/abs/1405.4702 (2014)
Foley, R. J. et al. Extensive HST ultraviolet spectra and multi-wavelength observations of SN 2014J in M82 indicate reddening and circumstellar scattering by typical dust. Preprint at http://arxiv.org/abs/1405.3677 (2014)
This work was based on observations with INTEGRAL, an ESA project with instruments and a science data centre funded by ESA member states (especially the principal investigator countries: Denmark, France, Germany, Italy, Switzerland and Spain) and with the participation of Russia and the United States. We are grateful to the ESA INTEGRAL team and E. Kuulkers for their prompt reaction to the SN 2014J event. E.C., R.S. and S.G. wish to thank the Russian INTEGRAL advisory committee for allocating an additional 106 s of time from a regular programme to SN 2014J observations. R.S., S.G. and S.S. are partly supported by grant no. 14-22-00271 from the Russian Scientific Foundation. J.I. is supported by MINECO-FEDER and Generalitat de Catalunya grants. The SPI project has been completed under the responsibility and leadership of CNES, France. ISGRI has been realized by CEA with the support of CNES. We thank P. Höflich, K. Nomoto and S. Woosley for making available their supernova explosion models HED6, W7 and DD4.
The authors declare no competing financial interests.
Extended data figures and tables
Anti-coincidence-system count rate is shown as a function of time, expressed through the revolution number. One revolution lasts about 3 days. Periods of very high and variable background (shown in blue) due to solar flares were omitted from the analysis. Periods of quiescent background (red) were used to derive the spectrum of SN 2014J.
Extended Data Figure 2 Comparison of the SPI background spectrum and the expected type Ia supernova emission.
Typical quiescent background (black) and supernova model (red, convolved with SPI energy resolution) spectra.
The 3PAR model spectrum calculated for day 75 is used for comparison with the INTEGRAL data obtained between day 50 and 100 since the explosion. Weak lines below 200 keV correspond to 56Ni (day 50) and 57Co (day 100).
The lines are formed by γ-rays escaping the ejecta without interactions. The low-energy tail of each line is due to Compton down-scattering of the photons because of the recoil effect. The ‘humps’ in the tails correspond to the scattering by 180°. The magenta line shows the contribution of the ortho-positronium annihilation. Annihilation of para-positronium contributes to 511 keV line.
The cross shows the best-fit values. Contours are plotted at Δχ2 = 1 with respect to the best-fit value and characterize the 1 s.d. confidence interval for a single parameter of interest.
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Churazov, E., Sunyaev, R., Isern, J. et al. Cobalt-56 γ-ray emission lines from the type Ia supernova 2014J. Nature 512, 406–408 (2014). https://doi.org/10.1038/nature13672
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