GRB 051103
GCN Circular 4197
Subject
IPN triangulation and Konus spectrum of the bright short/hard GRB051103
Date
2005-11-05T19:37:26Z (20 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team,
S. Barthelmy, J. Cummings, N. Gehrels
on behalf of the Swift team,
K. Hurley and T. Cline, on behalf of the Ulysses, HETE, Mars Odyssey,
and Konus GRB teams,
I. Mitrofanov, A. Kozyrev, M. Litvak, A. Sanin, V. Tret'yakov and A.
Parshukov, on behalf of the HEND-Odyssey GRB team,
W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team,
D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team,
J-L. Atteia, C. Graziani, and R. Vanderspek on behalf
of the HETE team report:
A very bright hard short GRB triggered the Konus-Wind instrument
at T0=33943.785 s UT (09:25:43.785) on November 3.
It was also observed by HETE-Fregate, Mars Odyssey (GRS and HEND),
RHESSI, and Swift-BAT.
We have triangulated this burst to the 3sigma
confidence error box:
RA(2000) Dec(2000)
----------------------------------------
ERROR BOX CENTER: 148.142 68.845
ERROR BOX CORNER 1: 148.563 69.189
ERROR BOX CORNER 2: 147.570 68.115
ERROR BOX CORNER 2: 147.731 68.499
ERROR BOX CORNER 4: 148.738 69.564
---------------------------------------
The area of the error box is 120 sq. arcmin.
The error box is consistent with a source in M81.
As observed by Konus-Wind the burst had a duration of 0.17 sec,
fluence 2.34(-0.28, +0.31)10^-5 erg/cm2,
and peak flux on 2ms time scale 1.89 (-0.35, +0.25)10^-3 erg/cm2/sec
(both in 20 keV - 10 MeV range).
The Epeak of the time-integrated spectrum is 1920 +/- 400 keV.
Assuming this burst originated from a source in M81 (D = 4 Mpc),
the isotrpoic energy release of this GRB is ~4.5x10^46 erg,
which consistent with the energy release of
27 December giant flare from SGR 1806-20.
The peak flux of this GRB is the largest ever observed for
the Konus-Wind short GRBs.
The burst light curve had a very steep rise ~4 msec and a decaying tail,
similar to the initial pulses of SGR giant flares.
All the quoted errors are at the 90% confidence level.
The K-W light curve of this GRB and IPN triangulation map can be seen
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB051103_T33943/
GCN Circular 4198
Subject
GRB051103:_MASTER_optical_observations
Date
2005-11-05T21:04:01Z (20 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Lipunov, V.Kornilov, D.Kuvshinov, N.Tyurina, A.Belinski, E.Gorbovskoy,
A.Krylov, G.Borisov, A.Sankovich, G.Antiov, V.Vladimirov
Sternberg Astronomical Institute, Moscow Union 'Optic'
MASTER robotic system (http://observ.pereplet.ru) responded to
GRB051103.4 (GRB_TIME is 2005-11-03 09:25:43.785, GCN4197 )at several
minutes after sms about new GCN Circ.
The first image (6 square degrees) was at 2005-11-05 19:55:47 UT, 2 days
10:30:03.215 after the GRB time
The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B).
The robot not find OT-candidate in error box.
Our upper limit is about 17.0 m.
The JPG-image will be available at
http://observ.pereplet.ru/images/GRB051103.4/1.jpg
The log JPG-image will be available at
http://observ.pereplet.ru/images/GRB051103.4/1_log.jpg
The reduction is continuing.
This work is supported by RFFI 04-02-16411 grant.
This message can be cited.
Mailto: lipunov@sai.msu.ru
GCN Circular 4206
Subject
GRB051103: MASTER: OT limit and host galaxy candidates
Date
2005-11-07T14:34:45Z (20 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Lipunov, V.Kornilov, D.Kuvshinov, N.Tyurina, A.Belinski, E.Gorbovskoy,
A.Krylov, G.Borisov, A.Sankovich, G.Antipov, V.Vladimirov
Sternberg Astronomical Institute, Moscow Union 'Optic'
MASTER robotic system (http://observ.pereplet.ru) responded to
GRB051103.4 (GRB_TIME is 2005-11-03 09:25:43.785, S. Golenetskii et al.,
GCN4197) at several minutes after GCN Circ4197 time (GCN4198).
The first image (6 square degrees) was at 2005-11-05 19:55:47 UT, 2 days
10:30:03.215 after the GRB time.
We have 36 images with total exposition 1080 s between 19:55:47 -
21:45:17 on 6 square degrees area. The robot not find
OT-candidate in IPN error box.
Our upper limit of the sum is about 18.5 m (the wether was not very
good).
The unfiltered images are calibrated
relative to USNO A2.0 (0.8 R + 0.2 B).
There are 4 galaxies overlaps and inside IPN error box (see image):
Name Type Coordinates (J2000) Magnitude Redchift Diameter
B MASTER 25isophot
NGC3031 (M81) Sab - 7.8 - 0.000376 big
NGC3034 (M82) S? - 9.2 - 0.000677 big
PGC2719634 ? 09 51 32.25 +68 31 23.4 17.8 16.7 ? 16".9
PGC028505 E 09 53 10.17 +69 00 02.1 ? 14.8 ? 6".0
M81 as candidate (S. Golenetskii et al., GCN4197) for SGR host
galaxy is high probable, but we note that
error box placed outside spiral arms region, where the progenitor of high
magnetized Neutron Star formated. However structure of the galaxy is
distorted by tidal intaractions. For example there is Ultraluminous X-ray source
M81 X-9 (see Wang, 2002, http://arxiv.org/abs/astro-ph/0201230 ) on same
distance from M81 center (this source is not in error box and belong to
high mass binary population). There is now known SN remnants in error
box (see for example D.Matonick and R.Fessen, ApJ SS 112,49,1997 which
not investigated IPN error box region).
We stress on elliptical galaxy PGC028505.
This galaxy close to center of the IPN error box.
The distance to PGC028505 can be estimated as about 80 Mpc.
Assuming this burst originated from a source PGC028505,
the isotrpoic energy release of this GRB is ~2x10^49 erg.
This energy is about 1 order more than GRB050509b one associated with
elliptical galaxy (Barthelmy et al., GCN3385).
In any case X-ray and optical observations (for search SNR) highly needed.
The sum JPG-image is available at
http://observ.pereplet.ru/images/GRB051103.4/sum36.jpg .
The IPN error box and galaxies are presented.
This work is supported by RFFI 04-02-16411 grant.
This message can be cited.
Mailto: lipunov@sai.msu.ru
GCN Circular 4207
Subject
GRB 051103, optical observations
Date
2005-11-07T18:14:59Z (20 years ago)
From
Sylvio Klose at TLS Tautenburg <klose@tls-tautenburg.de>
S. Klose, P. Ferrero, D. A. Kann, B. Stecklum, and U. Laux,
Thueringer Landessternwarte Tautenburg,
report:
Tautenburg observed the error box of the short/hard GRB 051103
(Golenetskii et al. 2005, GCN 4197) on Nov 6/7 in R (23:15 UT - 23:59
UT) and V (00:01 UT - 0:44 UT) using the prime focus CCD camera.
These observations were motivated by the fact that we had imaged
M81 in June 2005 using the same instrumental setup and the same
filters. The combined R-band images of both runs go notably deeper
than the DSS2 red, the combined V-band images are of similar depth.
Following the suggestion by Lipunov et al. (GCN 4206), we have
analyzed if there is evidence for a brightening of the galaxy PGC
028505 in the GRB error box due to an underlying transient source. No
such evidence has been found. In addition, we set a conservative upper
limit of R=21 on any transient within a radius of 30 arcsec around
PGC 028505, excluding its bright bulge.
This message may be cited.
GCN Circular 4208
Subject
GRB051103: optical observations
Date
2005-11-07T23:53:33Z (20 years ago)
From
Eran Ofek at Tel Aviv U. <eran@wise1.tau.ac.il>
E. O. Ofek, S. B. Cenko, A. M. Soderberg, S. R. Kulkarni (Caltech), D. B.
Fox (Penn State) report on behalf of the Caltech-NRAO-Carnegie
Collaboration:
We have observed the entire error box of the IPN short hard burst GRB
051103 (Golenetskii et al. 2005, GCN 4197) using the Robotic Palomar
60-inch telescope. We acquired 8 pointings (3-9 180sec R-band images
each) that cover the entire IPN error box over epochs between 2.96 and
3.16 days after the GRB trigger.
A comparison between the Palomar 60-inch image and POSS2 R-band image
did not reveal any new source brighter than limiting magnitude of about
R=19.5. Our images are deeper than the POSS images, and there are
several possible fainter variable/defects sources within the error box.
Second epoch images are scheduled.
Assuming that the GRB is related with the M81/M82 group, and using a
distance modulus of 27.8 (Freedman et al. 1994), and A_R=0.2 Galactic
extinction (Schlegel et al. 1998), we can set an upper limit of -8.5
(comparable to the absolute magnitude of novae) on the R-band absolute
magnitude of an optical transient.
GCN Circular 4249
Subject
GRB 051103 Milagro GeV/TeV Observations
Date
2005-11-11T06:45:36Z (20 years ago)
From
Pablo Saz Parkinson at UCSC/Milagro <pablo@scipp.ucsc.edu>
Pablo Saz Parkinson (UC Santa Cruz) on behalf of the Milagro Collaboration
reports:
We have searched Milagro data for emission at GeV/TeV energies from the
IPN short hard burst GRB 051103 (GCN Circ 4197, S. Golenetskii et al.),
during the 0.17 s burst duration observed by the Konus-Wind experiment. No
evidence for prompt GeV/TeV emission was found. This burst occurred at a
relatively large zenith angle of 50 degrees, where the sensitivity of
Milagro is degraded. A preliminary analysis, assuming a differential
photon spectral index of -2.4, gives an upper limit on the fluence at 99%
confidence of:
Fluence < 4.2 * 10^(-6) erg cm^(-2) (0.25 - 25 TeV)
If the burst originated from a source in the nearby galaxy M81, at
a distance of less than 4 Mpc (GCN Circ 4197, S. Golenetskii et al.)
the attenuation due to the extra-galactic background light (EBL) would
be negligible. This upper limit is preliminary and will be refined with
further analysis.
GCN Circular 4266
Subject
GRB051103: Radio Observations
Date
2005-11-12T00:01:27Z (20 years ago)
From
Patrick B. Cameron at Caltech <pbc@astro.caltech.edu>
P. Brian Cameron (Caltech) and Dale A. Frail (NRAO) report on behalf of a
larger collaboration:
"We observed the field of GRB 051103 (GCN 4197) with the Very Large Array
(VLA) at a frequency of 1.4 GHz beginning November 6.3 UT. We imaged the
entire IPN error region with three VLA pointings. We found no new sources
to the limit of the NRAO VLA Sky Survey (NVSS, Condon et al., ApJS, 117,
361). The rms noise varied from 0.5 mJy at the southern edge of the IPN
error box, to 1.5 mJy at the northern end (due to residual flux from M82).
We also observed a 5-arcmin radius around M82 on November 8.45 UT at a
frequency of 4.86 GHz. A comparison between this image and the the NVSS
image of the same region did not reveal any new sources above 1.5 mJy
(3-sigma).
No further observations are planned.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."