M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
L. M. Z. Hagen (PSU), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU),
C. B. Markwardt (GSFC), J. Norris (BSU), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), J. Tueller (GSFC),
T. N. Ukwatta (MSU) (i.e. the Swift-BAT team):
Using the data set from T30 to T+62 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 131004A (trigger #573190)
(Hagen, et al., GCN Circ. 15303). The BAT ground-calculated position is
RA, Dec = 296.108, -2.952 deg which is
RA(J2000) = 19h 44m 26.0s
Dec(J2000) = -02d 57' 05.6"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
The mask-weighted light curve shows a single short spike starts at ~T-0.18,
peaks at ~T0, and ends at ~T+1.35. T90 (15-350 keV) is 1.54 +- 0.33 sec
(estimated error including systematics).
The time-averaged spectrum from T-0.25 to T+1.80 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.81 +- 0.11. The fluence in the 15-150 keV band is 2.8 +- 0.2 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T-0.27 sec in the 15-150 keV band
is 3.4 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence
The burst spectrum appears at the softer end of short bursts, which have
an average spectral index of 1.2 when fitting with a simple power-law model
(Sakamoto et al. 2011). The spectral lag for this burst is 0.130 s +- 0.020 s
(for the 50-100 keV and 15-25 keV bands), which is significantly longer
than those of regular short bursts.
The results of the batgrbproduct analysis are available at