Abstract

Decades ago, γ-ray observatories identified diffuse Galactic emission at 1.809 MeV1,2,3 originating from β+ decays of an isotope of aluminium, 26Al, that has a mean lifetime of 1.04 million years4. Objects responsible for the production of this radioactive isotope have never been directly identified owing to insufficient angular resolutions and sensitivities of the γ-ray observatories. Here, we report observations of millimetre-wave rotational lines of the isotopologue of aluminium monofluoride that contains the radioactive isotope (26AlF). The emission is observed towards CK Vul, which is thought to be a remnant of a stellar merger5,6,7. Our constraints on the production of 26Al, combined with the estimates on the merger rate, make it unlikely that objects similar to CK Vul are major producers of Galactic 26Al. However, the observation may be a stepping stone for unambiguous identification of other Galactic sources of 26Al. Moreover, a high content of 26Al in the remnant indicates that, before the merger, the CK Vul system contained at least one solar-mass star that evolved to the red giant branch.

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Acknowledgements

We are grateful to the directors K. Schuster, P. Cox, S. Dougherty, T. van Zeeuw, R. Blundell and T. Beasley for granting us discretionary time at NOEMA, ALMA, APEX, SMA and JVLA. T.K. thanks L. Matrá for an introduction to Markov chain Monte Carlo methods. R.T. acknowledges support from grant 2017/27/B/ST9/01128, financed by the Polish National Science Centre. A.A.B. and T.F.G. acknowledge funding through the DFG priority programme 1573 (Physics of the Interstellar Medium) under grants GI 319/3-1 and GI 319/3-2, and the University of Kassel through P/1052 Programmlinie ‘Zukunft’. K.T.W. acknowledges support from the International Max Planck Research School for Astronomy and Astrophysics at the Universities of Bonn and Cologne, and also from the Bonn–Cologne Graduate School of Physics and Astronomy. This study made use of APEX, which is a collaboration between the Max-Planck-Institut für Radioastronomie, European Southern Observatory and Onsala Space Observatory. Some of the APEX data were collected under the programmes 095.F-9543(A) and 296.D-5009(A). This paper makes use of the following ALMA data: ADS/JAO.ALMA#2015.A.00013.S and #2017.A.00030.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities. The IRAM 30 m observations were carried out under projects 183-14, 161-15 and D07-14, and those with NOEMA under W15BN, E15AE, S16AV and E16AC. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain). The IRAM observations were supported by funding from the European Commission Seventh Framework Programme (FP/2007-2013) under grant agreement number 283393 (RadioNet3).

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Affiliations

  1. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, USA

    • Tomasz Kamiński
    •  & Nimesh A. Patel
  2. Department for Astrophysics, Nicolaus Copernicus Astronomical Center, Toruń, Poland

    • Romuald Tylenda
  3. Max-Planck-Institut für Radioastronomie, Bonn, Germany

    • Karl M. Menten
  4. Monash Centre for Astrophysics, School of Physics and Astronomy, Monash University, Clayton, Victoria, Australia

    • Amanda Karakas
  5. IRAM, Domaine Universitaire de Grenoble, Grenoble, France

    • Jan Martin Winters
    •  & Ka Tat Wong
  6. Laborastrophysik, Institut für Physik, Universität Kassel, Kassel, Germany

    • Alexander A. Breier
    •  & Thomas F. Giesen

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Contributions

T.K. wrote the text and analysed the observations. A.A.B. and T.F.G. prepared the spectroscopic data. J.M.W. prepared, executed and calibrated the NOEMA observations. K.T.W. prepared and reduced the JVLA observations. T.K. prepared and reduced the ALMA and all single-dish observations. N.A.P. prepared and calibrated the SMA observations. R.T. and A.K. ran stellar-evolution models. All authors contributed to the interpretation of the data.

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The authors declare no competing interests.

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Correspondence to Tomasz Kamiński.

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https://doi.org/10.1038/s41550-018-0541-x