GRB 111103B
GCN Circular 12519
Subject
GRB 111103B: Swift detection of a strong burst from a GRB or Galactic source
Date
2011-11-03T11:22:49Z (14 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
D. Grupe (PSU), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
S. Campana (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester),
C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), A. Melandri (INAF-OAB),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
M. Stamatikos (OSU/NASA/GSFC), M. C. Stroh (PSU) and B.-B. Zhang (PSU)
report on behalf of the Swift Team:
At 10:59:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 111103B (trigger=506903). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 265.704, +1.590 which is
RA(J2000) = 17h 42m 49s
Dec(J2000) = +01d 35' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a bright main peak from T+0 to T+20 s and continued
activity to a duration of at least 150 sec. The peak count rate
was ~15000 counts/sec (15-350 keV), at ~6 sec after the trigger.
The XRT began observing the field at 11:00:03.1 UT, 59.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 265.6955, +1.6107 which is equivalent to:
RA(J2000) = 17h 42m 46.91s
Dec(J2000) = +01d 36' 38.5"
with an uncertainty of 5.1 arcseconds (radius, 90% containment). This
location is 79 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
UVOT took a finding chart exposure of 102 seconds with the U filter starting
281 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. Data
from the list of sources generated on-board are not available at this time. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.29.
We note that this location is in a crowded field 30 degrees from the
Galactic center. In particular the XRT position is near (7.4 arcseconds)
the high proper motion star G 20-10. Thus this burst may be from a
Galactic source. We will require data from the Malindi ground link
to make this determination.
Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
GCN Circular 12520
Subject
GRB 111103B: optical observations
Date
2011-11-03T11:44:11Z (14 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev, O.Gres,
O.Chuvalaev,E.Konstantinov,
Irkutsk State University
E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski,
N.Tyurina, N.Shatskiy, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov,
D.Zimnukhov, M. Kornilov, A.Kuznetsov, D.Zimnukhov, M. Kornilov,
A.Sankovich
Sternberg Astronomical Institute, Moscow State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
V.Krushinski, I.Zalozhnich, T.Kopytova, A. Popov
Ural State University, Kourovka
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 Tunka(Siberia) was pointed to the GRB111103.46 19 sec s after
notice time and 42 sec after GRB time at 2011-11-03 10:59:45.246 UT. On
our first unfiltered 10s exposure set we haven`t found optical transient
within SWIFT error-box (Grupe et al, GCN Circ 12519).
The 5-sigma upper limit has been about 14.7mag
The message may be cited.
GCN Circular 12524
Subject
GRB 111103B: Swift-BAT refined analysis
Date
2011-11-03T15:45:44Z (14 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), D. Grupe (PSU), H. A. Krimm (GSFC/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
Using the data set from T-239 to T+418 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 111103B (trigger #506903)
(Grupe, et al., GCN Circ. 12519). The BAT ground-calculated position is
RA, Dec = 265.691, 1.605 deg which is
RA(J2000) = 17h 42m 45.8s
Dec(J2000) = +01d 36' 19.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.
The mask-weighted light curve shows at least 4 overlapping peaks in the first
group: starting at ~T-25 sec, with the brightest peak at ~T+8 sec, and ending
at ~T+90 sec. The second group of peaks starts at ~T+100 sec and ends
at ~T+250 sec. T90 (15-350 keV) is 167 +- 35 sec (estimated error
including systematics).
The time-averaged spectrum from T-6.55 to T+250.78 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.41 +- 0.05. The fluence in the 15-150 keV band is 8.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+5.48 sec in the 15-150 keV band
is 7.2 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/506903/BA/
GCN Circular 12525
Subject
GRB 111103B: Enhanced Swift-XRT position
Date
2011-11-03T16:12:22Z (14 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1541 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 111103B, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 265.69322, +1.61007 which is equivalent
to:
RA (J2000): 17h 42m 46.37s
Dec (J2000): +01d 36' 36.3"
with an uncertainty of 1.5 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 12527
Subject
GRB 111103B: optical observations from TAU, Ka-Dar
Date
2011-11-03T17:52:12Z (14 years ago)
From
Denis Denissenko at IKI, Moscow <d.v.denisenko@gmail.com>
D. Denisenko (IKI, Moscow), V. Gerke and S. Korotkiy (Ka-Dar
observatory, Russia) report:
Position of GRB 111103B (Grupe et al., GCN 12519; Barthelmy et al.,
GCN 12524; Goad et al., GCN 12525) was observed by 40-cm Djigit
telescope of Ka-Dar observatory's TAU station (Nizhniy Arkhyz,
Karachay-Cherkessia) equipped with SBIG STL-11K CCD from 15:35 UT to
16:04 UT on 2011 Nov. 03 (4.6-5.1 hr after the burst trigger). In
total, 10 unfiltered 120-sec exposures were taken.
There are no new sources detected in the error box of GRB 111103B on
the combined image, as compared to Red DSS plate of similar depth. The
limiting magnitude of the combined image (SNR=3) is R~20.2. The sum of
nine best frames (effective exposure of 18 minutes centered at 15:50
UT) is available at http://pics.livejournal.com/bigdenru/pic/000ak676/
(5'x5' crop).
We have also measured the light curve of the nearby star G 20-10 =
2MASS 17424702+0136326 (J=11.060+/-0.023, K=10.232+/-0.023) to check
for its variability. The star has remained constant within 0.01 mag
during our 0.5 hr observations. It is far from saturation with no more
than 13000 ADU on the individual images.
This message can be cited.
GCN Circular 12528
Subject
GRB111103B Swift/UVOT Upper Limits
Date
2011-11-03T21:26:25Z (14 years ago)
From
Patricia Schady at MPE/Swift <msslba@googlemail.com>
S. R. Oates (MSSL-UCL) and D. Grupe (PSU) report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 111103B
68 s after the BAT trigger (Grupe et al., GCN Circ. 12519).
No optical afterglow consistent with the XRT position (Goad et al., GCN Circ. 12525)
is detected in the initial UVOT exposures. The lack of an optical detection at the XRT
refined position excludes the possibility that the trigger is associated with the high proper
motion star (v~15mag) mentioned in Grupe et al. (GCN Circ. 12519) confirming that
the BAT trigger 506903 is a GRB.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC)
exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 68 218 147 >20.6
white 68 5055 344 >21.1
v 5266 5466 197 >19.1
b 4650 6161 270 >20.0
u 281 6081 297 >20.2
w1 5677 5876 197 >19.9
m2 5471 5670 197 >19.8
w2 5061 5261 197 >20.3
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.29 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 12530
Subject
GRB 111103B: Swift-XRT refined Analysis
Date
2011-11-04T02:24:06Z (14 years ago)
From
Dirk Grupe at PSU/Swift-XRT <dxg35@psu.edu>
D. Grupe (PSU) reports on behalf of the Swift-XRT team:
We have analysed 5.1 ks of XRT data for GRB 111103B (Grupe et al. GCN
Circ. 12519), from 49 s to 33.3 ks after the BAT trigger. The data
comprise 335 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN. Circ 12525).
The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=3.1 (+0.4, -0.3). At T+94.2 s the decay
flattens to an alpha of 0.59 (+0.05, -0.07) before breaking again at
T+8356 s to a final decay with index alpha=1.32 (+0.13, -0.14).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.97 (+0.05, -0.04). The
best-fitting absorption column is 2.90 (+0.16, -0.15) x 10^21 cm^-2,
in excess of the Galactic value of 9.1 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.85 (+0.13, -0.12)
and a best-fitting absorption column of 2.7 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.4 x 10^-11 (6.3 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 2.7 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 9.1 x 10^20 cm^-2
Excess significance: 9.8 sigma
Photon index: 1.85 (+0.13, -0.12)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00506903.
This circular is an official product of the Swift-XRT team.
GCN Circular 12531
Subject
GRB 111103B : WIYN 3.5m NIR observations
Date
2011-11-05T00:57:24Z (14 years ago)
From
Atish Kamble at U. of Wisconsin <atish@gravity.phys.uwm.edu>
Ralf Kotulla, Atish Kamble, David Kaplan (UW-Milwaukee) and Nial Tanvir (U.
Leicester) report :
We observed the field of strong GRB 111103B (Palmer et al., GCN 12519)
using the WIYN High Resolution Infrared Camera (WHIRC) on the WIYN 3.5m
telescope, beginning at November 4.08 (UT), approximately 15 hours after
the burst. Observations were carried out using the Ks filter, and the seeing
was about 1 arcsec.
We detect a faint object within the improved XRT error circle (Goad et al.,
GCN 12525). The preliminary magnitude of this source is K = 18.6 +/- 0.4,
but our observations do not allow us to make any statement about variability.
The source appears point-like, but the poor signal-to-noise means we could
not rule out it being slightly extended.
Further deep observations are encouraged for variability check and possible
association with the GRB.
The combined WIYN image of the field is available at :
http://members.galev.org/shared/GRB_111103B/whirc_zoom.jpg
We acknowledge the support from the staff of WIYN-3.5m telescope, and
especially from Greg Mosby in carrying out these observations.
GCN Circular 12532
Subject
Konus-Wind observation of GRB 111103B
Date
2011-11-05T13:12:31Z (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 GRB 111103B (Swift-BAT trigger #505054:
Grupe et al., GCN 12519; Barthelmy et al., GCN 12524)
triggered Konus-Wind at T0=39541.020s UT (10:59:01.020)
The light curve shows a ~15 s long pulse followed by
a weaker activity continuing till ~(T0+40)s. The second group
of peaks observed by Swift/BAT after T0+100
is poorly determined in the Konus-Wind light curves
against the background of a rising M2.5 Solar flare.
The emission in the initial peak complex is seen up to ~4 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB111103_T39541/
As observed by Konus-Wind the burst
had a fluence of (2.0 +/-0.3)x10-5 erg/cm2,
and a 256-ms peak flux, measured from T0+5.120 s,
of (2.7 +/-0.4)x10-6 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).
The time-integrated spectrum of the burst
(measured from T0 to T0+41.216 s)
is best fitted in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.97 (-0.18, +0.19),
and Ep = 372(-69, +109) keV,
chi2 = 77.2/77 dof.
Fitting this spectrum by the GRB (Band) function yields
the same alpha and Ep with a high energy photon index
beta < -2.2 (chi2 = 77.1/76 dof).
The spectrum at the maximum count rate
(measured from T0 to T0+6.144 s)
is best fitted in the 20 keV - 5 MeV range
by a power law with exponential cutoff model, for which
alpha = -0.97 (-0.12, +0.14),
and Ep = 393(-55, +76) keV,
chi2 = 70.2/77 dof.
All the observed properties are typical for a moderately intense
long gamma-ray burst and don't argue for a Galactic transient hypothesis.
All the quoted results are preliminary.
All the quoted errors are at the 90% confidence level.
GCN Circular 12533
Subject
GRB 111103B: MITSuME Akeno Optical upper limits
Date
2011-11-05T13:40:02Z (14 years ago)
From
Yoichi Yatsu at Tokyo Tech. <yatsu@hp.phys.titech.ac.jp>
S. Song, Y. Aoki, R. Usui, K. Kawakami, M. Hayashi, K. Tokoyoda,
Y. Saito, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of
the MITSuME collaboration:
We observed GRB 111103B (D. Grupe et al, GCN12519) with the
optical three color (g, Rc, and Ic) CCD camera attached to the MITSuME
50 cm telescope of Akeno Observatory, Yamanashi, Japan.
We started the observation about ~10.5 hour after the BAT trigger
from 2011-11-04 9:35:15 UT. And we did not find any new point source
within the XRT error circle (S. D. Barthelmy et al, GCN12524) in three bands.
The results of photometry (3sigma upper limits) are listed below.
#The photon flux were calibrated against GSC2.3 catalog.
T0+[day] MID-UT T-EXP[sec] g' Rc Ic
---------------------------------------------------------------------------------
3.7�10^4 9:44:05 1020 ----- >17.9 >18.0
---------------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 12546
Subject
GRB 111103B: optical upper limit of Mt. Terskol observatory
Date
2011-11-08T22:20:22Z (14 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A.Volnova (SAI MSU), M. Andreev, A. Sergeev (Terskol Branch of INASAN), V.
Petkov (Baksan Neutrino Observatory of INR), N. Karpov, O. Andrienko, K.
Martynyuk-Lototsky, N. Parakhin, N. Borachok, V. Kozlov, G. Butenko, V.
Godunova (IC AMER, NASU), A. Pozanenko (IKI) report:
We observed field of the Swift GRB 111103B (Grupe et al. GCN 12519) with
Zeiss-600 telescope of Mt.Terskol observatory in R filter between Nov. 3
(UT) 15:07:44 - 15:17:50. We took 10 images of 60 exposure under good
weather conditions and mean seeing (FWHW) of about 1.6". We do not detect
any source within enhanced XRT position (Goad et al., GCN 12525). A
photometry is based on the USNO B1.0 nearby stars.
T0+ Filter, Exposure, OT, UpperLimit
(mid, d) (s)
0.17619 R 10x60 n/d 17.5
GCN Circular 12547
Subject
GRB 111103B: optical upper limit of CrAO
Date
2011-11-08T22:24:22Z (14 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
V. Rumyantsev, N. Pit (CrAO), A. Pozanenko (IKI) report on behalf of larger
GRB follow-up collaboration:
We observed field of the Swift GRB 111103B (Grupe et al. GCN 12519) with
AZT-11 telescope of CrAO in R filter between Nov. 3 (UT) 16:12:05 -
17:00:21. We took several images of 180 exposure under unfavorable weather
conditions and mean seeing (FWHW) of about 4". We do not detect any source
within enhanced XRT position (Goad et al., GCN 12525). A photometry is
based on the USNO B1.0 nearby stars.
T0+ Filter, Exposure, OT, UpperLimit
(mid, d) (s)
0.2352 R 16x180 n/d 19.4
GCN Circular 12708
Subject
GRB 111103B: optical upper limit
Date
2011-12-20T13:00:59Z (13 years ago)
From
Alina Volnova at SAI MSU <alinusss@gmail.com>
V. Rumyantsev (CrAO), V. Biryukov (SAI MSU, CrAO), A. Pozanenko (IKI)
report on behalf of larger GRB follow-up collaboration:
We observed field of the Swift GRB 111103B (Grupe et al. GCN 12519)
with Zeiss-600 telescope of Crimean branch of SAI MSU in R filter
between Nov. 3 (UT) 15:44:07 - 17:02:29. We took 73 images of 60
exposure under bad weather conditions and mean seeing (FWHW) of about
3.4". We do not detect any source within enhanced XRT position (Goad
et al., GCN 12525). A photometry is based on the USNO B1.0 star
0916-0323572 (RA = 17:42:46.95, Dec = +01:36:05.2, J2000) assuming R
= 15.67.
T0+ Filter, Exposure, OT, UpperLimit
(mid, d) (s)
0.22517 R 73x60 n/d 20.4