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Position and parallax of the γ-ray burst of 8 May 1997

Author

Listed:
  • G. B. Taylor

    (National Radio Astronomy Observatory)

  • D. A. Frail

    (National Radio Astronomy Observatory)

  • A. J. Beasley

    (National Radio Astronomy Observatory)

  • S. R. Kulkarni

    (Mathematics and Astronomy 105-24, Caltech)

Abstract

γ-ray bursts (GRBs) have puzzled astronomers for almost three decades, primarily owing to the lack of identifications at other wavelengths. The detection of a radio counterpart1 enables application of the powerful technique of very long baseline interferometry (VLBI) to this intriguing class of objects. Here we present VLBI monitoring of VLA J065349.4 + 791619 obtained between 8 and 25 days after the initial γ-ray burst. The radio emission is found to be very compact, with an angular extent of less than 1 milliarcsecond. We derive a position for the radio counterpart accurate to 200 microarcseconds, and constrain the proper motion of VLA J065349.4 + 791619 be less than 50 milliarcseconds per year. We place an upper limit on the annual parallax of 1 milliarcsecond. These results are entirely consistent with the expectations of cosmological models.

Suggested Citation

  • G. B. Taylor & D. A. Frail & A. J. Beasley & S. R. Kulkarni, 1997. "Position and parallax of the γ-ray burst of 8 May 1997," Nature, Nature, vol. 389(6648), pages 263-265, September.
    • Handle: RePEc:nat:nature:v:389:y:1997:i:6648:d:10.1038_38456
    DOI: 10.1038/38456
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