GRB 140306A
GCN Circular 15935
Subject
GRB 140306A: Fermi GBM detection
Date
2014-03-06T11:44:43Z (11 years ago)
From
Gerard Fitzpatrick at UCD <gerard.fitzpatrick@ucdconnect.ie>
G. Fitzpatrick (UCD) and M. Stanbro (UAH)
report on behalf of the Fermi GBM Team:
At 03:29:44.95 UT on 06 March 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140306A (trigger 415769387/140306146).
The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location.
The on-ground calculated location, using the GBM trigger
data, is RA = 31.3 , DEC = +45.9 (J2000 degrees,
equivalent to 02h 05m, +45d 54.0'), with an uncertainty
of 1.00 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which is currently estimated to be 2 to 3 degrees).
The initial angle from the Fermi LAT boresight was 61 degrees.
The GBM light curve consists of several peak
with a duration (T90) of about 68 s (50-300 keV).
The time-averaged spectrum from T0-1.21601 s to T0+69.6s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.10 +/- 0.01 and
the cutoff energy, parameterized as Epeak, is 1580 +/- 100 keV
The event fluence (10-1000 keV) in this time interval is
(6.9 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+6.5 s in the 10-1000 keV band is 11.7 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.
GCN Circular 15938
Subject
IPN Triangulation of GRB 140306A
Date
2014-03-07T10:36:13Z (11 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks,
D. Svinkin, and T. Cline, on behalf of the Konus-Wind team,
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,
W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on
behalf of the GRS-Odyssey GRB team,
A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C.
Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB 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, and
S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on
behalf of the Swift-BAT team, report:
The long-duration, intense GRB 140306A (Fitzpatrick and Stanbro, GCN
Circ. 15935) was observed by Fermi (GBM), INTEGRAL (SPI-ACS),
Konus-Wind, MESSENGER (GRNS), Suzaku (WAM), Swift (BAT), and Mars
Odyssey (HEND) at about 12585 s UT (03:29:45). 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:
27.943 (01h 51m 46s) +48.975 (+48d 58' 31")
Corners:
28.544 (01h 54m 11s) +48.781 (+48d 46' 52")
28.271 (01h 53m 05s) +49.135 (+49d 08' 06")
27.339 (01h 49m 21s) +49.163 (+49d 09' 47")
27.617 (01h 50m 28s) +48.814 (+48d 48' 50")
---------------------------------------------
The error box area is 0.209 sq. deg, and its maximum
dimension is 53 arcmin (the minimum one is 20 arcmin).
This box may be improved.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB140306_T12581/IPN/
GCN Circular 15939
Subject
Konus-Wind observation of GRB 140306A
Date
2014-03-07T12:17:50Z (11 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
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:
The long-duration GRB 140306A (localized by IPN: Golenetskii et al., GCN
15938; GBM detection: Fitzpatrick, GCN 15935) triggered Konus-Wind at
T0=12581.686 s UT (03:29:41.686).
The burst light curve shows an bright multi-peaked pulse with
a duration of ~75 s. The emission is seen up to ~8 MeV.
As observed by Konus-Wind, the burst had a fluence of (1.35 +/-
0.12)x10^-4 erg/cm2, and a 256-ms peak flux, measured from T0+4.592 s,
of (2.3 +/- 0.2)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum (measured from T0 to T0+78.848 s)
is best fit (in the 20 keV - 15 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.21 (-0.04, 0.05)
and Ep = 1305 (-210,+273) keV (chi2 = 106/98 dof).
Fit with the GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.37 (chi2 = 106/97 dof).
The spectrum near the maximum count rate
(measured from T0 to T0+6.656 s)
is best fit (in the 20 keV - 15 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.77 (-0.05, 0.05)
and Ep = 1524 (-142,+158) keV (chi2 = 76/98 dof).
Fit with the GRB (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy
photon index: beta < -2.74 (chi2 = 76/97 dof).
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140306_T12581/
All the quoted errors are at the 90% confidence level.
All the quoted results are preliminary.
GCN Circular 15940
Subject
GRB 140306A: Suzaku WAM observation of the prompt emission
Date
2014-03-09T07:28:58Z (11 years ago)
From
Tetsuya Yasuda at Saitama U <yasuda@heal.phy.saitama-u.ac.jp>
T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno,
S. Sugimoto, S. Koyama, S. Takeda, T. Nagayoshi (Saitama U.),
M. Yamauchi, N. Ohmori, M. Akiyama, R. Kinoshita (Univ. of Miyazaki),
M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.),
K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun,
T. Takahashi (ISAS/JAXA), W. Iwakiri (RIKEN), Y. Hanabata (ICRR),
Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo)
on behalf of the Suzaku WAM team, report:
The bright long-duration GRB 140306A (localized by IPN: Golenetskii et al., GCN 15938;
and by Fermi-GBM: Fitzpatrick and Stanbro, GCN 15935;
and Konus-Wind detection: Golenetskii et al., GCN 15939)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 03:29:44.404 UT (=T0).
The observed light curve shows a multi-peaked structure starting at T0 and
followed by a long weak tail seen up to T0+60 s with a duration (T90) of about 54 seconds.
The fluence in 100 - 1000 keV was 5.38 (+0.09 / -0.13) x10^-5 erg/cm^2.
The 1-s peak flux measured from T0+4.5 s was 6.86 (+0.25 / -0.36) photons/cm^2/s
in the same energy range.
Preliminary result shows that the time-averaged spectrum from
T0-5 s to T0+60 s is well fitted by a power-law with exponential cutoff model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 0.91 (+0.05 / -0.05), and
Epeak 1426 (+87 / -81) keV (chi^2/d.o.f. = 63.5/51).
All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html