Hard-X-ray emission lines from the decay of 44Ti in the remnant of supernova 1987A

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Abstract

It is assumed1,2,3 that the radioactive decay of 44Ti powers the infrared, optical and ultraviolet emission of supernova remnants after the complete decay of 56Co and 57Co (the isotopes that dominated the energy balance during the first three to four years after the explosion) until the beginning of active interaction of the ejecta with the surrounding matter. Simulations4,5 show that the initial mass of 44Ti synthesized in core-collapse supernovae is (0.02–2.5) × 10−4 solar masses (). Hard X-rays and γ-rays from the decay of this 44Ti have been unambiguously observed from Cassiopeia A only6,7,8, leading to the suggestion that values of the initial mass of 44Ti near the upper bound of the predictions occur only in exceptional cases9. For the remnant of supernova 1987A10,11, an upper limit to the initial mass of 44Ti of <10−3 has been obtained from direct X-ray observations12, and an estimate of (1–2) × 10−4 has been made from infrared light curves and ultraviolet spectra by complex and model-dependent computations13,14,15. Here we report observations of hard X-rays from the remnant of supernova 1987A in the narrow band containing two direct-escape lines of 44Ti at 67.9 and 78.4 keV. The measured line fluxes imply that this decay provided sufficient energy to power the remnant at late times. We estimate that the initial mass of 44Ti was (3.1 ± 0.8) × 10−4, which is near the upper bound of theoretical predictions.

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Figure 1: Hard-X-ray images indicating the detection of 44 Ti emission lines from SNR 1987A.
Figure 2: Hard-X-ray spectra of SNR 1987A measured with IBIS/ISGRI in 2003–2011.
Figure 3: γ-ray spectrum of SNR 1987A measured with SPI in 2003–2011.

References

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Acknowledgements

We thank R. A. Sunyaev for reading the manuscript and for comments; V. S. Imshennik, D. K. Nadezhin and N. N. Chugai for discussions about aspects of the physics of the supernova 1987A explosion; R. A. Krivonos for information regarding the analysis of INTEGRAL/IBIS data; and M. Coe for allowing us access to his INTEGRAL data of the LMC observations (1 Ms) before the end of the proprietary period. This work is based on data obtained through the Russian and European INTEGRAL science data centres, and was supported by grants RFBR-11-02-12285ofi-m-2011 and RAS-P20 ‘The origin, structure and evolution of objects of the Universe’.

Author information

S.A.G. was Principal Investigator of the proposal requesting INTEGRAL time (3.5 Ms) to observe SNR 1987A; made a preliminary analysis of the IBIS/ISGRI data and detected an excess at the SNR 1987A position; and wrote a draft of the text. A.A.L. was Co-investigator of the proposal, and participated in the analysis of IBIS/SIGRI data and the verification of the result. S.S.T. carried out the analysis of SPI data. C.W. provided general support for this project and participated in its different aspects, and C.W. and A.A.L. contributed substantially to the final text. All authors discussed the results and their presentation.

Correspondence to S. A. Grebenev.

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Grebenev, S., Lutovinov, A., Tsygankov, S. et al. Hard-X-ray emission lines from the decay of 44Ti in the remnant of supernova 1987A. Nature 490, 373–375 (2012) doi:10.1038/nature11473

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