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An ultraluminous X-ray source powered by an accreting neutron star

Author

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  • M. Bachetti

    (Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
    CNRS, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France)

  • F. A. Harrison

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • D. J. Walton

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • B. W. Grefenstette

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • D. Chakrabarty

    (MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology)

  • F. Fürst

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • D. Barret

    (Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
    CNRS, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France)

  • A. Beloborodov

    (Columbia University, 538 West 120th Street, New York, New York 10027, USA)

  • S. E. Boggs

    (Space Sciences Laboratory, University of California)

  • F. E. Christensen

    (DTU Space, National Space Institute, Technical University of Denmark, Elektrovej 327, DK-2800 Lyngby, Denmark)

  • W. W. Craig

    (Lawrence Livermore National Laboratory)

  • A. C. Fabian

    (Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK)

  • C. J. Hailey

    (Columbia Astrophysics Laboratory, Columbia University)

  • A. Hornschemeier

    (NASA Goddard Space Flight Center)

  • V. Kaspi

    (McGill University, Montreal, Quebec H3A 2T8, Canada)

  • S. R. Kulkarni

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • T. Maccarone

    (Texas Tech University)

  • J. M. Miller

    (University of Michigan, 500 Church Street, Ann Arbor, Michigan 48109-1042, USA)

  • V. Rana

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • D. Stern

    (Jet Propulsion Laboratory, California Institute of Technology)

  • S. P. Tendulkar

    (Cahill Center for Astrophysics, 1216 East California Boulevard, California Institute of Technology)

  • J. Tomsick

    (Space Sciences Laboratory, University of California)

  • N. A. Webb

    (Université de Toulouse, UPS-OMP, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France
    CNRS, Institut de Recherche en Astrophysique et Planétologie, 9, Avenue du Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France)

  • W. W. Zhang

    (NASA Goddard Space Flight Center)

Abstract

X-ray pulsations with an average period of 1.37 seconds have been detected from a known ultraluminous X-ray source hitherto thought to be a black hole; the pulsations instead unequivocally identify the source as an accreting magnetized neutron star ten times brighter than any previously known.

Suggested Citation

  • M. Bachetti & F. A. Harrison & D. J. Walton & B. W. Grefenstette & D. Chakrabarty & F. Fürst & D. Barret & A. Beloborodov & S. E. Boggs & F. E. Christensen & W. W. Craig & A. C. Fabian & C. J. Hailey , 2014. "An ultraluminous X-ray source powered by an accreting neutron star," Nature, Nature, vol. 514(7521), pages 202-204, October.
    • Handle: RePEc:nat:nature:v:514:y:2014:i:7521:d:10.1038_nature13791
    DOI: 10.1038/nature13791
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