GRB 140329A

Andreas von kienlin (MPE) and George Younes (USRA/MSFC)
report on behalf of the Fermi GBM Team:

"At 07:04:38.33 UT on 29 03 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140329A (trigger 417769481 / 140329295).
The trigger resulted in an Autonomous Repoint Request (ARR), but FERMI
went into SAA 120 seconds after trigger.

The on-ground calculated location, using the GBM trigger
data, is RA = 149.8, DEC = -27.44 (J2000 degrees), with an uncertainty
of 1 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).

The angle from the Fermi LAT boresight is 114 degrees.

This burst was also independently detected by INTEGRAL SPI-ACS.

The GBM light curve consists of two pulses seperated by about 25 seconds
with a duration (T90) of about 21.5 s (50-300 keV).
The time-averaged spectrum from T0-2.3 s to T0+33.6 s is
best fit by a Band function with Epeak = 244 +/- 5 keV,
alpha = -0.83 +/- 0.01, and beta = -2.38 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(7.07 +/- 0.05)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+23.6 s in the 8-1000 keV band
is 102.0 +/- 1.0 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."

K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and 
T. Cline, on behalf of the Konus-Wind team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. 
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

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

The long-duration, bright GRB 140329A (von Kienlin and Younes, GCN Circ. 
16042
Loading...
 
 ) has been observed by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), 
MESSENGER (GRNS), and Mars Odyssey (HEND), so far, at about 25478 s UT 
(07:04:38).

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   146.246 (09h 44m 59s) -32.103 (-32d 06' 09")
  Corners:
   145.867 (09h 43m 28s) -31.797 (-31d 47' 49")
   145.948 (09h 43m 47s) -32.076 (-32d 04' 33")
   146.627 (09h 46m 31s) -32.404 (-32d 24' 13")
   146.544 (09h 46m 10s) -32.127 (-32d 07' 39")
  ---------------------------------------------
The error box area is 491 sq.arcmin, and its maximum dimension is 53 
arcmin (the minimum one is 12 arcmin).

The center of the GBM ground position (von Kienlin and Younes, GCN Circ. 
16042
Loading...
 
 ) is 5.6 deg from the center of the box.

This box can be improved.

A triangulation map is posted at 
http://www.ioffe.ru/LEA/GRBs/GRB140329_T25481/IPN/

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

A long-duration, very intense GRB 140329A
(Fermi-GBM detection: von Kienlin & Younes, GCN 16042
Loading...
 
 ;
IPN triangulation: Hurley at al., GCN 16045
Loading...
 
 )
triggered Konus-Wind at T0=25481.877 s UT (07:04:41.877).

The burst light curve starts with a short pulse at ~T0 followed
by a bright multi-peaked complex from ~T0+19 s to ~T0+30 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had a fluence
of 8.5(-0.7,+0.7)x10^-5 erg/cm2, and a 64-ms peak flux,
measured from T0+23.744 s, of 2.7(-0.3,+0.3)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+33.024 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.04 (-0.09,+0.11),
the high energy photon index beta = -2.30 (-0.17,+0.11),
the peak energy Ep = 238 (-28,+32) keV,
chi2 = 132/95 dof.

The spectrum near the maximum count rate
(measured from T0+23.296 to T0+23.808 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.90 (-0.11,+0.13),
the high energy photon index beta = -2.7 (-1.1,+0.3),
the peak energy Ep = 388 (-66,+75) keV,
chi2 = 68.0/80 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140329_T25481/

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

D. Kocevski (NASA/Goddard), G. Vianello (Stanford U.),  E. Bissaldi (University & INFN Trieste), and J. McEnery (NASA/Goddard)

report on behalf of the Fermi-LAT team:

An on-ground analysis of the IPN triangulation of GRB 140329A (Hurley et. al. GCN16045
Loading...
 
 ), which was detected by Fermi-GBM (trigger 417769481, GCN 16042
Loading...
 
 ) and initiated an autonomous repoint of the spacecraft, has revealed long-lived high-energy emission detected by Fermi-LAT.  The best LAT on-ground location is found to be:

RA, Dec 145.698,  -32.229 (J2000)

with an error radius of 0.2 deg (90% containment, statistical error only). The burst was outside the LAT field of view at the time of trigger and remained so for an additional 2000 seconds.  The analysis above covers a period from 2000s to 5000s post GBM trigger and an energy range of 100 MeV to 10 GeV.

The Fermi-LAT point of contact for this burst is D. Kocevski (daniel.kocevski@nasa.gov<mailto:daniel.kocevski@nasa.gov>).

The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.