GRB 130219A
GCN Circular 14243
Subject
GRB 130219A: Fermi GBM detection
Date
2013-02-20T19:53:04Z (12 years ago)
From
Andrew Collazzi at NASA/MSFC/ORAU <andrew.collazzi@nasa.gov>
Andrew C. Collazzi (NASA/ORAU)
reports on behalf of the Fermi GBM Team:
"At 18:35:51.73 UT on 19 February 2013, the Fermi Gamma-ray
Burst Monitor (GBM) triggered and located GRB 130219A (trigger
382991754 / 130219.775). The on-ground calculated location,
using the Fermi GBM trigger data, is RA = 303.7, DEC = +40.8
(J2000 degrees, equivalent to J2000 20h 14m, +40d 49'), with a
statistical uncertainty of 1.2 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 85 degrees.
The GBM light curve shows two distinct peaks with a total duration
(T90) of about 96 s (50-300 keV). The spectrum is taken over the
peaks, from T0+0.003 to T0+3.328 s and T+66.817 to T0+101.634,
and is well fit by a Comptonized model with Ep = 396.0 +/- 21.0 and
alpha = -1.11 +/- 0.02. This yields a fluence (10-1000 keV) in this
time interval of ���(3.18 +/- 0.05)E-05 erg/cm^2.
This interval is equally well fit to a Band function with
Ep = 343.1 +/- 25.5, alpha = -1.08 +/- 0.02, and
beta = -2.28 +/- 0.15. This yields a fluence (10 - 1000 keV) over this
interval of (3.11 +/- 0.05)E-05 erg/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 14246
Subject
IPN Triangulation of GRB 130219A
Date
2013-02-21T16:50:12Z (12 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
K. Hurley and J. Goldsten, on behalf of MESSENGER GRNS 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,
V. Connaughton, M. Briggs, C. Meegan, and V. Pelassa, 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,
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
G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, and M. Marisaldi, on
behalf of the AGILE MCAL team, report:
The long-duration GRB 130219A was observed by Fermi (GBM: trigger
382991754, Collazzi, GCN Circ. 14243), Konus-Wind, INTEGRAL (SPI-ACS),
Suzaku (WAM), Swift (BAT), AGILE (MCAL), and MESSENGER (GRNS), at about
66950 s UT (18:35:50). 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
---------------------------------------------
Corners:
311.189 (20h 44m 45s) +51.497 (+51d 29' 50")
307.440 (20h 29m 46s) +48.611 (+48d 36' 41")
296.804 (19h 47m 13s) +37.410 (+37d 24' 35")
296.474 (19h 45m 54s) +37.565 (+37d 33' 53")
---------------------------------------------
The error box area is about 2.5 sq. deg, and its maximum dimension is
17.4 deg (the minimum one is 9 arcmin).
This box may be improved.
A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB130219_T66950/IPN/
GCN Circular 14250
Subject
Konus-Wind observation of GRB 130219A
Date
2013-02-22T11:01:58Z (12 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
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-duration intense GRB 130219A
(Fermi GBM detection: Collazzi, GCN 14243;
IPN detection and localization: Hurley et al., GCN 14246)
triggered Konus-Wind at T0=66950.352.048s UT (18:35:50.352)
The burst started with a soft precursor
at ~T0-0.5s which was followed, after ~65 sec of quiescence,
by a harder intense emission pulse.
A total duration of the burst is ~117 s.
The emission in the main emission episode is seen up to ~8 MeV.
As observed by Konus-Wind, the burst
had a fluence of (4.2 � 0.4)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+81.152 s,
of (2.4 � 0.2)x10-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The energy spectrum of the precursor (measured T0 to T0+8.444 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model,
for which:
alpha = +0.11 � 0.45,
and Ep = 95 � 8 keV,
chi2 = 57.2/60 dof.
The time-integrated spectrum of the main emission episode
(measured T0+67.792 to T0+105.984 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.08 � 0.07,
the high energy photon index beta = -2.12 � 0.11,
the peak energy Ep = 280 � 35 keV,
chi2 = 90.8/96 dof.
The spectrum at the maximum count rate
(measured T0+79.984 to T0+81.408 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.10 � 0.05,
the high energy photon index beta = -3.1 � 0.2,
the peak energy Ep = 365 � 15 keV,
chi2 = 81.3/97 dof.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130219_T66950/
All the quoted results are preliminary.
GCN Circular 14253
Subject
GRB 130219A: Suzaku WAM observation of the prompt emission
Date
2013-03-01T10:21:18Z (12 years ago)
From
Makoto Tashiro at Saitama U/Swift <tashiro@phy.saitama-u.ac.jp>
A. Sakamoto, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara,
M. Asahina, S. Kobayashi, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.),
M. Akiyama, N. Ohmori, E. Mochinaga, M. Yamauchi (Univ. of Miyazaki),
K. Yamaoka, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata,
T. Kawano, K. Takaki, R. Nakamura, Y.Tanaka, M. Ohno, Y. Fukazawa
(Hiroshima U.), S. Sugita (Nagoya U.), Y. E. Nakagawa (Waseda U.),
Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:
The long GRB 130219A (Collazzi, GCN 14243; Hurley et al., GCN 14246) was
detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 2013/02/19 18:35:51.73 UT (=T0).
The observed light curve exhibited two separated pulses; which are
the 1st short pulse from T0+1 s to T0+3 s,
and the following 2nd long pulse from T0+74 s to T0+96 s,
with a total duration of 96 s. The fluence in 100 - 1000 keV was
2.06 (+0.16/-0.36) x 10^-5 erg/cm^2. The 1-s peak flux measured from
T0+81 s was 5.03 (+0.57/-0.72) photons/cm^2/s in 100 - 1000 keV.
Preliminary result shows that the time-averaged spectrum from T0-2s to
T0+98s is marginally described as a power-law with exponential cutoff
model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 1.23(-0.45 +0.39), and
Epeak 502(-96 +151) keV (chi^2/d.o.f. = 33.2/24).
On the other hand, the two separate pulse spectra are well fitted
by different models. The 1st pulse spectrum is well fitted by a single
power-law with a photon index of 2.12(+0.57/-0.37) (chi^2/d.o.f = 21.6/25).
The 2nd pulse spectrum is well fitted by a GRB Band model:
the low-energy photon index alpha: -1.16(-0.35 +0.49),
the high-energy photon index beta: -2.5(fixed),
and the peak energy Epeak: 515(-84, +145) keV (chi^2/d.o.f = 26.1/24).
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