GRB 110120A
GCN Circular 11588
Subject
GRB 110120A: MASTER optical observations
Date
2011-01-20T18:04:51Z (14 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University
V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka
K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk was pointed to the GRB110120.67 24 sec s after
notice time and 63 sec after GRB time at 2011-01-20 16:00:42.913 UT. On
our first (10s exposure) set we haven`t found optical transient within
FERMI LAT error-box (ra=04 22 36 dec=-18 21 00 r=0.016667).
The 5-sigma upper limit has been about 13 mag.
The message generated automaticaly.
*Add: The observations was done at high zenith distance.
mailto: lipunov@sai.msu.ru
GCN Circular 11591
Subject
GRB 110120A: Fermi GBM detection
Date
2011-01-21T16:23:22Z (14 years ago)
From
Lin Lin at UAH/NAOC <ll0005@uah.edu>
Lin Lin (UAH)
reports on behalf of the Fermi GBM Team:
"At 15:59:39.23 UT on 20 January 2011, the Fermi Gamma-Ray Burst
Monitor triggered and located GRB 110120A (trigger 317231981 /
110120666).
The on-ground calculated location, using the GBM trigger
data, is RA = 64.54, DEC = -17.06 (J2000 degrees,
equivalent to 04 h 18 m 09.6 s, -17 d 03 ' 36.0 "), with an
uncertainty of 1.08 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 15 degrees.
This burst triggered the Fermi spacecraft slew because of high
peak flux.
The GBM light curve shows a ~5 s peak followed by a ~40 s
tail with a duration (T90) of about 27 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+43.393 s is
acceptably fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.87 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 1156 +/- 172 keV
(C-Stat 666.26 for 487 d.o.f.).
The event fluence (10-1000 keV) in this time interval is
(2.55 +/- 0.05)E-5 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.384 s in the 10-1000 keV band
is 15.03 +/- 1.35 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 11595
Subject
IPN triangulation of GRB 110120A
Date
2011-01-23T00:07:18Z (14 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team,
S. Golenetskii, R. Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline, on behalf of the Konus-Wind team,
V. Connaughton, M. Briggs, and C. Meegan, on behalf of the Fermi GBM team,
J. Cummings, D. Palmer, S. Barthelmy, N. Gehrels, and H. Krimm, 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:
Fermi (GBM), Konus-Wind, Swift (BAT), MESSENGER (GRNS), and Suzaku (WAM)
observed the long, hard GRB 110120A at about 15:59:39 UT (Fermi/GBM
trigger 317231981: Lin, GCN 11591). The burst was outside the coded
field of view of the BAT.
We have triangulated it to a 3 sigma error box whose coordinates are:
-----------------------------------------------
RA(2000), deg Dec(2000), deg
-----------------------------------------------
Center:
60.481 (04h 01m 55s) -10.548 (-10d 32' 51")
Corners:
56.433 (03h 45m 44s) -5.247 (-05d 14' 48")
62.714 (04h 10m 51s) -13.354 (-13d 21' 16")
64.578 (04h 18m 19s) -14.953 (-14d 57' 11")
58.278 (03h 53m 07s) -7.456 (-07d 27' 21")
-----------------------------------------------
The error box area is 2.548 sq. deg.
This error box may be improved.
Because the Earth, the Wind, and the MESSENGER satellites are nearly
aligned at the moment (the angular distance between Wind and MESSENGER
is only 5.7 deg), the annuli intersect at grazing incidence and the
resulting 3-sigma box is long.
A map is posted at http://www.ioffe.ru/LEA/GRBs/GRB110120_T57582/IPN/
showing the GBM best-fit position (blue star and circle), the IPN annuli
(solid lines with centers dot-dashed), and the box (solid black closed
polyline).
GCN Circular 11597
Subject
GRB 110120A: Fermi LAT detection
Date
2011-01-24T07:50:35Z (14 years ago)
From
Nicola Omodei at Standford <nicola.omodei@slac.stanford.edu>
Nicola Omodei (Stanford University), James Chiang (SLAC/KIPAC),
Valerie Connaughton (UAH) and Yasuyuki Tanaka (ISAS/JAXA)
report on behalf of the Fermi Large Area Telescope (LAT) collaboration.
Based on an on-ground analysis, the Large Area Telescope (LAT),
on-board the Fermi Gamma-ray Space Telescope, detected high energy emission
up to ~2 GeV associated with the GBM-detected burst GRB 110120A (Lin, GCN 11591).
The emission in the LAT lasts over 100 seconds, with the highest-energy photon
arriving 72 sec after the GBM trigger time.
The best localization is RA, DEC (J2000 deg) = 61.6, -12.0 (04h 06m 24s, -12d 00' 00"),
with an error of 0.4 deg (68% CL), compatible with the IPN triangulation
from Hurley et al. (GCN 11595).
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.
[GCN OPS NOTE(24jan11): Per author's request, his affilation and address were updated.]
GCN Circular 11598
Subject
GRB 110120A: MASTER optical observations
Date
2011-01-24T14:56:32Z (14 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski, N.Shatskiy, N.Tyurina,
D.Kuvshinov, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, V.Shumkov, S.Shurpakov
Sternberg Astronomical Institute, Moscow State University
V.Krushinski, I.Zalozhnich, A. Popov
Ural State University, Kourovka
K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
MASTER very wide field cameras (MASTER-Net:
http://observ.pereplet.ru, 6 cameras 11 Mpix, 85, 1/1.2. 1 sec
exposition, comonn FOW is 2400 square degrees)
located in Kislovodsk was pointed to the GRB110120A 24 sec s after
notice time and 64 sec after GRB time at 2011-01-20 16:00:42.913 UT.
The sky near horizont is not clear.
On our 60 coaded images we haven`t found optical transient within
common area of the FERMI LAT error-box (Nicola Omodei et al., GCN Circ
11597) and (Hurley et al., GCN 11595).
The 5-sigma upper limit has been about 10 mag (mean time = 94 sec after
trigger).
The image is available at
http://observ.pereplet.ru/images/GRB110120A/grb.html
The MASTER II telescopes FOW was out
of the final error box and our previous results (Gorbovskoy et al., GCN
Circ 11588) not valid.
The observations was done at high zenith distance.
mailto: lipunov@sai.msu.ru
GCN Circular 11601
Subject
Konus-Wind observation of GRB 110120A
Date
2011-01-25T14:44:44Z (14 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 hard GRB 110120A,
(Fermi/GBM trigger 317231981/
110120666: Lin Lin, GCN 11591;
localized by IPN: Hurley et.al, GCN 11595;
detected by Fermi/LAT: Omodei et al., 11597)
triggered Konus-Wind at T0=57582.268s UT (15:59:42.268)
The burst light curve starts with a hard bright pulse,
followed by a softer decaying tail.
The total duration of the burst is ~42 s.
The emission is seen up to ~5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB110120_T57582/
As observed by Konus-Wind the burst
had a fluence of (3.1 � 0.3)x10-5 erg/cm2,
and a 64-ms peak flux, measured from T0+0.128s,
of (1.6 � 0.5)x10-5 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).
The time-integrated spectrum of the burst
(from T0 to T0+41.216 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = -0.6 (-0.2, +0.2),
and Ep = 680(-120, +160) keV,
chi2 = 64.5/74 dof.
The spectrum at the initial part of the burst
(measured from T0 to T0+0.256 s) is best fit
in the 20 keV - 5 MeV range by a power law
with exponential cutoff model, for which
alpha = 0.0 (-0.3, +0.4),
and Ep = 1193(-244, +349) keV,
chi2 = 18.0/23 dof.
All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.
GCN Circular 11609
Subject
GRB 110120A: Suzaku WAM observation of the prompt emission
Date
2011-01-28T14:57:51Z (14 years ago)
From
Yuji Urata at Nat. Central U. <urata@astro.ncu.edu.tw>
P. Tsai, Y. Urata (NCU), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa
(Hiroshima U.), N. Vasquez (Tokyo Tech.), K. Yamaoka (Aoyama Gakuin U.),
S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, S. Hong, W. Iwakiri, K. Takahara,
T. Yasuda (Saitama U.), M. Ohno, M. Serino, M. Kokubun, T. Takahashi (ISAS/JAXA),
Y. E. Nakagawa, T. Tamagawa (RIKEN), N. Ohmori, A. Daikyuji, Y. Nishioka,
M. Yamauchi (Univ. of Miyazaki), K. Nakazawa, K. Makishima (Univ. of Tokyo),
on behalf of the Suzaku WAM team, report:
The log GRB 110120A (Fermi/GBM trigger 317231981 / 110120666 ; Lin et
al., GCN 11591; Omodei et al., GCN 11597) triggered the Suzaku
Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV
- 5 MeV at 2011/01/20 15:59:39.22 UT (=T0).
The observed light curve shows a multi-peaked structure starting at
T0-0.7s, ending at T0+8s, with a duration (T90) of about 6.4
seconds. The fluence in 100 - 1000 keV was 2.32 (+/-0.16) x 10^-5
ergs/cm^2. The 1-s peak flux measured from T0+0.38s was 30.40
(+/-0.93) photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from T0-0.7s
to T0+8s is well fitted by a power-law with exponential cutoff
model:
dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
alpha 1.34 (-0.51, +0.40), and
Epeak 418.60 (-84.64, +110.46) keV (chi^2/d.o.f. = 39.92/40).
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