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

G. B. Taylor (), D. A. Frail, A. J. Beasley and S. R. Kulkarni
Additional contact information
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

Nature, 1997, vol. 389, issue 6648, 263-265

Abstract: 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.

Date: 1997
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DOI: 10.1038/38456

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