GRB 101129A

J. R. Cummings (GSFC/UMBC/CRESST), D. M. Palmer (LANL),
S. D. Barthelmy (GSFC), and T. Sakamoto (GSFC/UMBC/CRESST) on
behalf of the BAT team,

Valentin Pal'shin (Ioffe Inst) and K. Hurley (UCB) on behalf of
the IPN,

V. Connaughton, M.S. Briggs, and C.A. Meegan on behalf of the
Fermi GBM team,

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

A. P. Beardmore (U Leicester) and J. A. Kennea (PSU) on behalf of
the Swift-XRT 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,

J. Goldsten, on behalf of the MESSENGER NS GRB team:


At 15:39:31 UTC, Swift-BAT detected a rate increase due to GRB 101129A
(BAT trigger #439471. Only a sub-threshold image source was found
onboard.  This event corresponds to Fermi GBM trigger #312737973. The
IPN was alerted.  In ground analysis, the source was detected with
slightly greater confidence at RA, Dec 155.921, -17.645 which is:

RA (J2000)       10h 23m 41s
Dec (J2000)    -17d 38m 42s

with an estimated uncertainty radius of 3 arcmin (90% containment).
Correlation of Swift-BAT counting rates and SPI-ACS counting rates,
and SPI-ACS with Messenger yielded intersecting annuli consistent with
this position. The burst was also detected by Suzaku-WAM.

As seen in BAT, the burst consisted of a single pulse with a T90 of about
0.35 +- 0.05 sec.

The burst was faint and short. The low-number statistics in BAT make a
fit to the spectrum very uncertain. The photon index was approximately
0.8 +- 0.5.  The fluence was approximately (9 +- 5) x 10^-08 ergs/cm^2.

A Swift TOO observation was executed at 11 hours after the burst.  The
location of the burst was observed by the Swift-XRT and Swift-UVOT for
a total of about 1400 seconds.  No afterglow was detected.  No further
observations are planned.

S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:

The short hard GRB 101129A
(localized by BAT and IPN: Cummings  et al. GCN 11436
Loading...
 
 )
triggered Konus-Wind at T0=56370.759s UT (15:39:30.759)

The burst light curve consists of a single pulse
with a total duration of ~0.4 s.
The emission is seen up to 5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB101129_T56370/

As observed by Konus-Wind the burst
had a fluence of 3.5(+1.4/-1.1)x10-6 erg/cm2,
and a 16-ms peak flux measured from T0-0.096s
of 1.7(+0.7/-0.5)x10-5 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+0.128 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.4 (-0.4, +0.5),
and Ep = 1210(-400, +680) keV (chi2 = 8.1/12 dof).

All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level

[GCN OPS NOTE(06dec10): Per authors's request, the author list was added.]

N. Ohmori, A. Daikyuji, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki),
M. Ohno, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka (Aoyama Gakuin U.), 
S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, 
T. Yasuda (Saitama U.),P. Tsai, Y. Urata, H.M. Lin (NCU), 
T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), 
N. Vasquez (Tokyo Tech.), Y. E. Nakagawa, M. Serino, T. Tamagawa (RIKEN), 
K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.), 
on behalf of the Suzaku WAM team, report:


The short GRB 101129A (localized by Swift/BAT and IPN; Cummings et al., 
GCN11436
Loading...
 
 ) triggered the Suzaku Wide-band  All-sky Monitor (WAM) which 
covers an energy range of 50 keV - 5 MeV at 2010-11-29 15:39:31.92 UT (=T0).

The observed light curve shows a multi-peaked structure starting at T0+0.2s,
ending at T0+0.6s, with a duration (T90) of about 0.31 seconds. The fluence
in 100 - 1000 keV was 1.54 (-0.47, +0.12) x 10^-6 erg/cm^2.
The 1-s peak flux measured from T0s was 2.50 (-0.89, +0.30) photons/cm^2/s
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to
T0+1s is well fitted by a power-law with exponential cutoff model:
dN/dE =  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha       0.43 (-0.62, +0.46), and
Epeak       1027 (-215, +292)  keV (chi^2/d.o.f. = 40.2/54).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves for this burst will be available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html