GRB 120707A

George Younes (NASA/USRA), report on behalf of the Fermi GBM Team:

"At 19:12:17.42 UT on 07 July 2012, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 120707A (trigger 363381140 / 120707.800).
The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 291.06, Dec = -34.44 (J2000 degrees, equivalent to
J2000 19h 24m, -34d 26'), with a statistical uncertainty of 1.0 degrees
(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 159 degrees.

The burst triggered an ARR (Automatic Repointing Request), causing 
Fermi to slew so the LAT would point to the source.  Because the burst 
was close to the Earth's limb, this maneuver was delayed, placing the 
GRB position near the LAT boresight starting about 1000 s after the GBM trigger time.

The GBM light curve shows a strong central  pulse with fainter wings
with a duration (T90) of about 50 s (50-300 keV). The time-averaged
spectrum from T0-3 to T0+57 s is best fit by a Band function with Epeak = 
174 +/- 7 keV, alpha = -1.17 +/- 0.03, and beta = -2.31 +/- 0.03.

The fluence (10-1000 keV) in this time interval is (1.1 +/- 0.007)E-4 erg/cm^2.
The 1-sec peak photon flux measured starting from T0+29.1 s in the 10-1000 keV band
is 62 +/- 2 ph/s/cm^2.

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

K. Hurley on behalf of the Mars Odyssey and MESSENGER GRB teams,

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

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

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team,

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

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

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on
behalf of the Swift-BAT team, and

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, report:

The long-duration, intense GRB 120707A (Younes, GCN 13422
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 ) has been 
observed by Fermi (GBM: trigger 363381140), Konus-Wind, INTEGRAL 
(SPI-ACS), Swift (BAT), Mars Odyssey (HEND), and Suzaku (WAM), so far, 
at about 69140 s UT (19:12:20). The burst was outside the coded field of 
view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   291.874 (19h 27m 30s) -32.770 (-32d 46' 12")
  Corners:
   293.104 (19h 32m 25s) -36.566 (-36d 33' 56")
   292.808 (19h 31m 14s) -37.093 (-37d 05' 36")
   290.585 (19h 22m 20s) -27.663 (-27d 39' 48")
   290.769 (19h 23m 05s) -26.473 (-26d 28' 23")
  ---------------------------------------------

The error box area is 3.50 sq. deg, and its maximum dimension is 10.8 deg.
This box can be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB120707_T69146/IPN/

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 long intense GRB 120707A
(GBM trigger 363381140: Younes, GCN 13422
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 ;
IPN localization: Hurley at al., GCN 13424
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 )
triggered Konus-Wind at T0=69146.810s UT (19:12:26.810)

The light curve shows a strong pulse peaked at ~T0+24 s.
A total duration of the burst is ~95 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB120707_T69146/

As observed by Konus-Wind the burst
had a fluence of 1.35(-0.15,+0.15)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+24.064 s,
of 1.05(-0.15,+0.15)x10-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+57.600 s)
is best fit in the 30 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.54 (-0.09, +0.12),
the high energy photon index beta = -2.22 (-0.24, +0.14),
the peak energy Ep = 190(-37, +41) keV,
chi2 = 74.9/82 dof.

The spectrum at the maximum count rate
(measured from T0+20.224 to T0+26.368 s)
is best fit in the 30 keV - 10 MeV range
with the GRB (Band) model, for which:
the low-energy photon index alpha = -1.30 (-0.12, +0.16),
the high energy photon index beta = -2.3 (-0.38, +0.16),
the peak energy Ep = 213(-41, +53) keV,
chi2 = 86.4/82 dof.

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