GRB 090328B
GCN Circular 9056
Subject
GRB 090328B: Fermi GBM Detection
Date
2009-03-30T18:06:00Z (16 years ago)
From
Adam Goldstein at Fermi-GBM/UAH <adam.m.goldstein@msfc.nasa.gov>
A. Goldstein (UAH) reports on behalf of the Fermi GBM Team:
"At 17:07:04.94 UT on 28 March 2009, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 090328B (trigger 259952826 / 090328713).
The Fermi Observatory executed a maneuver following this trigger and
tracked the burst location for the next 5 hours, subject to
Earth-angle constraints.
The on-ground calculated location, using the GBM trigger
data, is RA = 155.72, DEC = +33.40 (J2000 degrees,
equivalent to 10h 23m, 33d 24'), with an uncertainty
of 7.94 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 74 degrees.
The GBM light curve consists of a single bright peak
with a duration (T90) of about 0.32 s (8-1000 keV).
The time-averaged spectrum from T0-0.13 s to T0+0.13 s is
well fit by a Band function with Epeak = 1967.0 +/- 701.0 keV,
alpha = -0.92 +/- 0.06, and beta = -2.48 +/- 0.66
(chi squared 452.6 for 482 d.o.f.).
The event fluence (8-1000 keV) in this time interval is
(9.61 +/- 0.31)E-07 erg/cm^2. The 0.064-sec peak photon flux measured
starting from T0+0.0 s in the 8-1000 keV band
is 29.83 +/- 2.38 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 9065
Subject
GRB 090328B: MASTER-Irkutsk prompt optical short burst observations
Date
2009-04-01T08:47:35Z (16 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
K.Ivanov, S.Yazev,
Irkutsk State University
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko,
Kislovodsk Solar Station of the Pulkovo Observatory
V.Krushinski, I.Zalognikh, T.Kopytova
Ural State University, Kourovka
There are 6 MASTER Very Wide Field cameras located at Kislovodsk and
Irkutsk with common FOW = 6000 square degrees
(http://observ.pereplet.ru/).
One of the two MASTER Very Wide Field Cameras located at Irkutsk
(D=50 mm, 2x1000 square degrees, 11 Mpx) has observed ~20% 1-sigma Fermi
error box (A. Goldstein, GCN 9056) with 1s exposure
during all night: befoure, during and after GRB Time
without time gap between images.
Our unfiltered images are calibrated relative to Tycho stars (V).
The magnitude limit of the each emage is ~9.1 m at the edge of FOW (some
ising was attend at this night).
We do not detect OT inside 20% part of the error box.
We conclude (in the case that GRB inside our FOW ):
1). the optical fluence during the short 0.3 s GRBurst is limited by
~<= 3 x 10E-9 erg/cm_2
excluding possible host galaxy absorbtion.
The event fluence (8-1000 keV) in this time interval is
(9.61 +/- 0.31)E-07 erg/cm^2 (A. Goldstein, GCN 9056).
So:
2). Optical-Fluence/Gamma-Fluence(8-1000 keV) ~ < 1/300
The same ratio for long GRB080319B is
Optical-Fluence/Gamma-Fluence(8 - 1000 keV) ~ 1/140
(Naked Eye GRB, Racusin, Karpov et al., Nature, vol.455, 183, 2008).
The film of our observations is available at
http://observ.pereplet.ru/images/GRB090320B/GRB090328B.gif
Black circles are the 1-sigma and 3-sigma
error boxes (A. Goldstein, GCN 9056).
The reduction is continued.
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 9124
Subject
GRB 090328b: IPN Triangulation
Date
2009-04-12T09:28:01Z (16 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
and T. Cline on behalf of the Konus-Wind and Konus-RF teams,
K. Hurley and T. Cline, on behalf of the Mars Odyssey
and Konus GRB teams,
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, G. Lichti, and A. Rau, and K. Hurley on behalf of the
INTEGRAL SPI-ACS team,
E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci,
I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta,
for the SuperAGILE team,
G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi,
on behalf of the AGILE MCAL team report:
Konus-Wind, Konus-RF, Mars-Odyssey (GRS and HEND), and INTEGRAL-SPI-ACS
observed the intense GRB 090408b (Golenetskii et al., GCN 9121). It was
also observed by AGILE-MCAL and SuperAGILE (outside the coded field of view).
We have triangulated it to the following 3-sigma error box:
-----------------------------------------------
RA(2000), deg Dec(2000), deg
-----------------------------------------------
Center:
43.98 (02h 55m 56s) +26.61 (+26d 36' 36")
Corners:
43.95 (02h 55m 48s) +27.59 (+27d 35' 24")
42.98 (02h 51m 55s) +27.78 (+27d 46' 48")
44.05 (02h 56m 12s) +25.64 (+25d 38' 24")
44.97 (02h 59m 53s) +25.49 (+25d 29' 24")
-----------------------------------------------
The error box area is 1.48 sq. deg.
This error box may be improved.
IPN triangulation map is avalable at
at http://www.ioffe.ru/LEA/GRBs/GRB090408_T71198/IPN
--