{
  "bibcode": "2004GCN..2538....1H",
  "body": "K. Hurley and T. Cline, on behalf of the Ulysses, HETE, Mars Odyssey,\nand Konus GRB teams,\n\nI. Mitrofanov, S. Charyshnikov, V. Grinkov, A. Kozyrev, M. Litvak, and\nA. Sanin, on behalf of the HEND-Odyssey GRB team,\n\nW. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on\nbehalf of the GRS-Odyssey GRB team,\n\nE. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, and\n\nG. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R.\nVanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G.\nJernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R.\nManchanda, G.  Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T.\nTamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,\nT. Tavenner, T.  Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on\nbehalf of the HETE GRB team, report:\n\nMars Odyssey (HEND and GRS) and Konus-Wind observed H3066 (GRB040228 at\n00536 s, GCN 2536).  In addition, Konus-Wind observed H3067 (GRB040228\nat 00764 s) and the 50 s long X-ray pulse which followed it (GCN\n2536).  Neither of these was observed by Odyssey, but this is\nconsistent with the lower intensity of H3067, and the spectral softness\nof the X-ray pulse (the Odyssey lower energy threshold is ~100 keV).\nUlysses was off.\n\nWe have triangulated H3066 to an annulus centered at RA, Decl (J2000) =\n222.855, -17.387 degrees, whose radius is 31.387 +/- 0.055 degrees (3\nsigma).  The minimum distance between this annulus and the position of\nthe X-ray pulse determined by the HETE WXM is ~37 degrees; in addition,\nthis position is Mars-blocked to Odyssey.  We therefore conclude that\nH3066 and the X-ray pulse are unrelated.\n\nUsing Mars-blocking, the IPN annulus, and the Konus ecliptic latitude\ndetermination, we can restrict the arrival direction of H3066 to that\nportion of the annulus which lies between RA, Dec = 246, -42 degrees,\nand 253, -33 degrees.  This area was far outside the HETE WXM FOV,\nfurther proof that H3066 and the X-ray pulse detected by the WXM are\nunrelated.\n\nHowever, Konus-Wind data indicate that the arrival directions of H3066,\nH3067, and the X-ray pulse are all consistent with an ecliptic latitude\nof -10 to -20 degrees.  Thus H3067 may be related either to H3066 or to\nthe X-ray pulse (but not both). It may also be an independent event.\n\nFinally, we note that the Odyssey data display a strong, 5 s long pulse\n~350 s after the signal corresponding to H3066.  We are investigating\nthe possible relation of this pulse to the other bursts.",
  "circularId": 2538,
  "createdOn": 1078190117000,
  "email": "khurley@sunspot.ssl.berkeley.edu",
  "subject": "IPN triangulation of GRB040228 (H3066, H3067)",
  "submitter": "Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>",
  "eventId": "GRB 040228"
}