GCN Circular 15278
Subject
IPN Observations of GRB 130925A
Date
2013-09-30T22:05:33Z (11 years ago)
From
Kevin Hurley at UCBerkeley/SSL <khurley@ssl.berkeley.edu>
K. Hurley, on behalf of the IPN team,
S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline, on behalf of the Konus-Wind team,
I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,
W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team,
D. M. Smith, J. McTiernan, R. Schwartz, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro,
Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team,
S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of
the Swift-BAT team,
J. Goldsten, on behalf of the MESSENGER NS GRB team, and
V. Connaughton, M. S. Briggs, C. Meegan, and V. Pelassa, on behalf of the Fermi
GBM team, report:
Eight IPN spacecraft observed GRB 130925A (Lien et al. GCN 15246,
Markwardt et al. 15247). When the responses of all the spacecraft are
considered, the IPN had an uninterrupted view of this event from
roughly 900 s before the Swift BAT trigger, to ~7100 s after it.
Constraints on the arrival directions of the four main emission
episodes strengthen the case for their common origin, as suggested by
Savchenko et al. (GCN 15259). The following table details the
observations. The times are relative to the BAT trigger at 15084 s UT
(04:11:24). N/O means the episode was not observable.
----------------------------------------------------------------------------
Instrument/ | Precursor | 1st | 2nd | 3rd
spacecraft | -900 s | episode | episode | episode*
| | -130 -> +170 s|+1750 -> +2950 s|+3730 -> +4360 s
----------------------------------------------------------------------------
Swift BAT No Trig N/O No
Fermi GBM Trig Trig N/O No
INTEGRAL SPI-ACS No Yes Yes Yes
Konus Wind Yes Yes Yes Yes
MESSENGER No Yes Yes No
Mars Odyssey No N/O Yes No
Suzaku WAM No No Yes No
RHESSI Yes Yes N/O No
------------------------------------------------------------------------------
*also observed and localized by MAXI (Suzuki et al. GCN 15248)
We conclude from these observations that the total duration of this
event in >25 keV gamma-rays above the IPN flux/fluence threshold was
at least 5260 s, and ~7150 s long when the later episodes, observed only
by BAT (GCN 15257), are included.