Abstract

Fast radio bursts are millisecond-duration astronomical radio pulses of unknown physical origin that appear to come from extragalactic distances1,2,3,4,5,6,7,8. Previous follow-up observations have failed to find additional bursts at the same dispersion measure (that is, the integrated column density of free electrons between source and telescope) and sky position as the original detections9. The apparent non-repeating nature of these bursts has led to the suggestion that they originate in cataclysmic events10. Here we report observations of ten additional bursts from the direction of the fast radio burst FRB 121102. These bursts have dispersion measures and sky positions consistent with the original burst4. This unambiguously identifies FRB 121102 as repeating and demonstrates that its source survives the energetic events that cause the bursts. Additionally, the bursts from FRB 121102 show a wide range of spectral shapes that appear to be predominantly intrinsic to the source and which vary on timescales of minutes or less. Although there may be multiple physical origins for the population of fast radio bursts, these repeat bursts with high dispersion measure and variable spectra specifically seen from the direction of FRB 121102 support an origin in a young, highly magnetized, extragalactic neutron star11,12.

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Acknowledgements

We thank the staff of the Arecibo Observatory, and in particular A. Venkataraman, H. Hernandez, P. Perillat and J. Schmelz, for their continued support and dedication to enabling observations like those presented here. We also thank our commensal observing partners from the Arecibo ‘Zone of Avoidance’ team, in particular T. McIntyre and T. Henning. We thank M. Kramer for suggestions. The Arecibo Observatory is operated by SRI International under a cooperative agreement with the National Science Foundation (AST-1100968), and in alliance with Ana G. Méndez-Universidad Metropolitana, and the Universities Space Research Association. These data were processed using the McGill University High Performance Computing Centre operated by Compute Canada and Calcul Québec. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. The research leading to these results has received funding from the European Research Council (ERC) under the European Union’s Seventh Framework Programme (FP7/2007-2013). L.G.S., P.C.C.F. and P.L. gratefully acknowledge financial support from the ERC Starting Grant BEACON under contract number 279702. J.W.T.H. is an NWO Vidi Fellow and gratefully acknowledges funding for this work from ERC Starting Grant DRAGNET under contract number 337062. Work at Cornell (J.M.C., S.C., A.B.) was supported by NSF grants AST-1104617 and AST-1008213. V.M.K. holds the Lorne Trottier Chair in Astrophysics and Cosmology and a Canadian Research Chair in Observational Astrophysics and received additional support from NSERC via a Discovery Grant and Accelerator Supplement, by FQRNT via the Centre de Recherche Astrophysique de Québec, and by the Canadian Institute for Advanced Research. J.v.L. acknowledges funding for this research from an ERC Consolidator Grant under contract number 617199. Pulsar research at UBC is supported by an NSERC Discovery Grant and by the Canadian Institute for Advanced Research.

Author information

Affiliations

  1. Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, B-53121 Bonn, Germany

    • L. G. Spitler
    • , P. C. C. Freire
    • , P. Lazarus
    •  & W. W. Zhu
  2. Department of Physics and McGill Space Institute, McGill University, 3600 University Street, Montreal, Quebec H3A 2T8, Canada

    • P. Scholz
    • , R. D. Ferdman
    • , V. M. Kaspi
    • , E. C. Madsen
    • , C. Patel
    •  & I. H. Stairs
  3. ASTRON, Netherlands Institute for Radio Astronomy, Postbus 2, 7990 AA Dwingeloo, The Netherlands

    • J. W. T. Hessels
    •  & J. van Leeuwen
  4. Anton Pannekoek Institute for Astronomy, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands

    • J. W. T. Hessels
    •  & J. van Leeuwen
  5. Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA

    • S. Bogdanov
    •  & F. Camilo
  6. Department of Astronomy and Space Sciences, Cornell University, Ithaca, New York 14853, USA

    • A. Brazier
    • , S. Chatterjee
    •  & J. M. Cordes
  7. Cornell Center for Advanced Computing, Cornell University, Ithaca, New York 14853, USA

    • A. Brazier
  8. Square Kilometre Array South Africa, Pinelands, 7405, South Africa

    • F. Camilo
  9. Department of Physics and Astronomy, Franklin and Marshall College, Lancaster, Pennsylvania 17604-3003, USA

    • F. Crawford
  10. National Research Council, Naval Research Laboratory, 4555 Overlook Avenue SW, Washington DC 20375, USA

    • J. Deneva
  11. National Radio Astronomy Observatory, PO Box 2, Green Bank, West Virginia 24944, USA

    • R. Lynch
  12. Department of Physics and Astronomy, West Virginia University, Morgantown, West Virginia 26506, USA

    • R. Lynch
    •  & M. A. McLaughlin
  13. National Radio Astronomy Observatory, Charlottesville, West Virginia 22903, USA

    • S. M. Ransom
  14. Arecibo Observatory, HC3 Box 53995, Arecibo, Puerto Rico 00612, USA

    • A. Seymour
  15. Department of Physics and Astronomy, University of British Columbia, 6224 Agricultural Road, Vancouver, British Columbia V6T 1Z1, Canada

    • I. H. Stairs
  16. Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK

    • B. W. Stappers

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Contributions

L.G.S. and J.W.T.H. led the design and execution of the observing campaign described here. P.S. performed the analysis that discovered the radio bursts. More detailed analysis of the signal properties was done by L.G.S., P.S., S.M.R., M.A.M., J.W.T.H., S.C. and J.M.C. L.G.S., J.W.T.H., P.S. and V.M.K. led the writing of the manuscript. All authors contributed substantially to the interpretation of the analysis results and to the final version of the manuscript.

Competing interests

The authors declare no competing financial interests.

Corresponding author

Correspondence to J. W. T. Hessels.

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DOI

https://doi.org/10.1038/nature17168

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