The following appeared in IAU Circular No. 6384 (19-Apr-1996):


  GRB 960409 AND COMET C/1996 B2 (HYAKUTAKE)
       T. E. Harrison, New Mexico State University (NMSU); S. D.
  Barthelmy, Universities Space Research Association (USRA) and
  Goddard Space Flight Center, NASA; K. Hurley, University of
  California at Berkeley; G. J. Fishman, C. Kouveliotou (also USRA),
  and C. Meegan, Marshall Space Flight Center, NASA; R. M. Kippen,
  University of New Hampshire; B. J. McNamara, NMSU, report:  "The
  gamma-ray burst GRB 960409 fortuitously occurred near the position
  of comet C/1996 B2.  Thus there is the high probability that some
  C/1996 B2 observers may have serendipitously imaged the GRB error
  box while the burst was in progress, or shortly thereafter.  The
  burst started at Apr. 9.89243 UT and lasted 105 s, with the peak
  emission at Apr. 9.89289.  The Gamma Ray Observatory (GRO) BATSE
  team location is R.A. = 2h50m30s, Dec. = +41o54'.6, with a total
  (statistical + systematic) error radius of 2o.1.  This location is
  2o.6 away from the comet's location at the time of the burst.  The
  IPN annulus is centered at R.A. = 10h19m48s, Dec. = +68o54'28"; it
  has a radius of 58o.1736 and a total width of 0o.18.  The
  intersection of the IPN annulus and the BATSE error circle defines
  the corners of a error region with a confidence level of 95 percent:
  R.A. = 3h01m18s.7, Dec. = +41o22'36"; 2h40m43s.6, +42o59'59";
  3h01m31s.7, +41o33'19"; 2h41m16s.7, +43o09'10" (equinox 2000.0).
  The separation of the BATSE location and the annulus point-of-
  closest-approach is 0o.39.  The burst was independently localized
  by GRO/COMPTEL with a marginal detection (2.5-sigma significance);
  the COMPTEL localization is consistent with the BATSE and IPN
  locations (see the map at http://wwwgro.unh.edu/bursts).  We
  strongly encourage researchers to analyze their images for
  transient objects.  The importance of deep images of the GRB error
  box during the burst can not be overstressed.  Please note that
  for images made while tracking the comet, any transient emission
  from the GRB source object is likely to be short enough not to be
  trailed as much as the field stars.  Images with limiting magitudes
  9 will set new upper limits on the GRB-related optical emission.
  For further information, please contact T. Harrison at telephone
  505-646-3628 (email tharriso@nmsu.edu)."

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