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GCN Circular 2357

Summary of recent IPN and HETE detections of SGR bursts
2003-08-20T17:48:01Z (20 years ago)
Kevin Hurley at UCBerkeley/SSL <>
K. Hurley and T. Cline, on behalf of the Ulysses, HETE, Mars Odyssey,
and KONUS GRB teams,

G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R.
Vanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G.
Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R.
Manchanda, G.  Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T.
Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
T. Tavenner, T.  Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on
behalf of the HETE GRB team,

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, 

I. Mitrofanov, S. Charyshnikov, V. Grinkov, A. Kozyrev, M. Litvak, and
A. Sanin, on behalf of the HEND-Odyssey GRB team,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team, 

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, and

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team, report:

The IPN and HETE have observed numerous SGR-like bursts between August
10 and 18.  The following table summarizes them.  In the one case below
where the burst was only observed by Ulysses, the true Earth-crossing
time is uncertain by about +/- 3000 s.  The time given below is under
the assumption that the arrival direction was the general region near

Date,	Earth	   Observed		           Localized?  GCN Circular
August 	Crossing   by				               Number
2003    Time, s.

10	27050	   Ulysses, Konus	           Yes***
11	57988	   Ulysses, HETE (2800)	           Yes*
12	31339	   Ulysses, Konus	           Yes***
13	35523	   HETE (2802), Konus	           Yes**       2351
15	40524	   HETE (2806), RHESSI	           Yes***
16	82760	   Ulysses		           No
18	41499	   HETE (2810)		           Yes***
18	50231	   Ulysses, HEND, INTEGRAL, Konus  Yes*	       2354, 2355		

*Localization indicates that the most likely source is SGR1806-20
**Localization indicates that the most likely source is SGR1808-20
***Localization cannot be used to distinguish between SGR1806 and SGR1808
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