GRB 101014A

Dave Tierney (UCD) and Adam Goldstein (UAH) 
report on behalf of the Fermi GBM Team: 

"At 04:11:52.62 UT on 14 October 2010, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 101014A (trigger 308722314 / 101014175 ).

The on-ground calculated location, using the GBM trigger 
data, is RA = 26.94, DEC = -51.07 (J2000 degrees, 
equivalent to 01 h 47 m, -51 d 04 '), with an 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 54 degrees.
This burst resulted in a Fermi spacecraft repointing maneuver.

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

The GBM light curve consists of multiple pulses
with a T90 of about 450 s (50-300 keV). 
The time-averaged spectrum from T0+1.5 s to T0+473.6 s is 
best fit by a Band function with Epeak = 181.40 (+5.66/-5.44) keV, 
alpha = -1.27 (+0.01/-0.01), and beta = -2.07 (+0.02/-0.02)
(C-stat of 2499.1 for 591 d.o.f.).

The event fluence (10-1000 keV) in this time interval is 
(2.072 +/- 0.009)E-04 erg/cm^2. The 1-sec peak photon flux measured 
starting from T0+208.77 s in the 8-1000 keV band 
is 58.96 +/- 0.42 ph/s/cm^2.



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

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 very long bright GRB 101014A (Fermi/GBM
trigger 308722314 / 101014175: Tierney & Goldstein, GCN 11341
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triggered Konus-Wind at T0=15115.250s UT (04:11:55.250)

The burst light curve shows a complex multi-peaked
structure with a total duration of ~480 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/GRB101014_T15115/

As observed by Konus-Wind the burst
had a fluence of (2.5 � 0.7)x10-4 erg/cm2,
and a 256-ms peak flux, measured from T0+208.896s,
of (2.6 � 0.2)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+445.184 s) is best fit
in the 20 keV - 10 MeV range by the GRB (Band) model,
for which:
the low-energy photon index alpha = -1.26 (-0.13, +0.15),
the high energy photon index beta = -2.2 (-1.4, +0.2),
the peak energy Ep = 220(-47, +76)keV (chi2 = 64/84 dof).

The spectrum at the maximum count rate
(measured from T0+208.128 to T0+210.176 s) is best fit
in the 20 keV - 10 MeV range by the GRB (Band) model,
for which:
the low-energy photon index alpha = -1.12 (-0.05, +0.06),
the high energy photon index beta = -2.45 (-0.65, +0.30),
the peak energy Ep = 920(-170, +180)keV (chi2 = 79/69 dof).

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

Yasuyuki Tanaka, Masanori Ohno (ISAS/JAXA), Johan Bregeon (INFN,
Pisa), Elena Moretti (KTH), Giacomo Vianello (CIFS, SLAC) and
Nicola Omodei (Stanford) report on behalf of the Fermi LAT collaboration.

The Fermi Large Area Telescope (LAT) detected emission from GRB
101014A, which was also detected by GBM at 04:11:52.62 UT, 14 October
2010 (GBM trigger 308722314, GCN 11341
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This burst was initially at an angle of ~54 degrees to the LAT
boresight and triggered an autonomous repoint of the spacecraft.
Because of the burst's proximity to the orbital pole, there was
substantial contamination in the surrounding region owing to gamma-ray
emission from the Earth's limb. A significant excess above background
was not seen using standard analysis procedures.

Using a non-standard data selection that increases the low energy
acceptance at the cost of a greater background (~13 Hz), the LAT
light curve consists of a single, narrow pulse with ~3 s width,
containing over 200 counts above background. This pulse was detected
approximately 210 s after the GBM trigger time. A spectral fit of the
LAT data in the 3 s pulse window yields a photon index of -2.6 +/-
0.1 (stat) and a flux of 0.020 +/- 0.014 ph/s-cm^2 in the 10-100 MeV
band. These data have insufficient spatial resolution to provide a
reliable LAT localization.

Further analysis is ongoing.

The Fermi LAT point of contact for this burst is Yasuyuki Tanaka
(tanaka@astro.isas.jaxa.jp).

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.