GCN Circular 15257

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), D. M. Palmer (LANL),
T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC),
T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+7152 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130925A (trigger #571830)
(Lien, et al., GCN Circ. 15246
Not found
 
 
).  The BAT ground-calculated position is
RA, Dec = 41.186, -26.146 deg which is
    RA(J2000)  =  02h 44m 44.5s
    Dec(J2000) = -26d 08' 47.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 9%.

The mask-weighted light curve covers only a small part of this exceptionally
long GRB (if indeed it is a GRB at all).  As reported by the Fermi-GBM team
(Fitzpatrick, GCN Circ. # 15255) the event may have begun 17 minutes prior to
the BAT trigger, and the source was still detected in BAT at T+2 hours.  Thus
we cannot estimate a T90 at this time.  There were multiple peaks and several
late-time flares.

In the current analysis, the burst was first detected by BAT at T-59 sec, when
the target entered the BAT field of view already emitting, and last detected by
BAT in a survey interval ending at T+7152 sec.

BAT also detected a flux increase during the first flare detected by XRT (Evans
et al. GCN Circ. # 15254) that peaked at about T+1000 seconds.  BAT did not see
a significant increase at the time of the next flare (brightest in XRT), peaking
at about T+1380 seconds, though the source was still detected.  BAT did strongly
detect increases during the XRT-observed flares that peaked at approximately
T+4950 and T+7100 seconds.  BAT did not detect emission during another, smaller,
flare observed by XRT that peaked at about T+11000 seconds.

BAT has not detected significant flux from this location in the 15-50 keV band
prior to the current event.

The time-averaged spectrum from T-59 to T+903 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.85 +- 0.14,
and Epeak of 33.4 +- 20.0 keV (chi squared 38.18 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 4.1 +- 0.1 x 10^-05 erg/cm2
and the 1-sec peak flux measured from T-35.64 sec in the 15-150 keV band is
7.3 +- 0.6 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.09 +- 0.04 (chi squared 45.62 for 57 d.o.f.).  The flares at T+4950 and
T+7100 seconds have photon indices in simple power-law fits of 2.19 +- 0.36
and 2.34 +- 0.28 respectively.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/571830/BA/