GRB 051109A
GCN Circular 4212
Subject
GRB 051109a: IR Detections
Date
2005-11-09T02:09:23Z (20 years ago)
From
Josh Bloom at UC Berkeley <jbloom@astron.berkeley.edu>
J. S. Bloom, on behalf of a larger collaboration, reports:
"The Peters Automated Infrared Imaging Telescope (PAIRITEL)
autonomously began observing the field of GRB 051109a (Swift trigger
163136) at 2005-11-09 01:13:55.59 UTC (1min35 sec after the trigger).
In the first several individual 7.8 second exposures we detected the
candidate afterglow proposed by Rykoff et al. (GCN #4211) in
simultaneous J, H, and Ks imaging. Further observations are in
progress as well as analysis."
Josh
GCN Circular 4214
Subject
GRB 051109A: ROTSE-III Decline rate for Optical Counterpart
Date
2005-11-09T02:38:04Z (20 years ago)
From
Brad Schaefer at LSU <schaefer@grb.phys.lsu.edu>
B. E. Schaefer (Louisiana State), E.S. Rykoff (U Mich), W. Rujopakarn (U
Mich), F. Yuan (U Mich), R. Quimby (U Texas), K. Alatalo (Berkeley), T.A.
McKay (U Mich), C. Akerlof (U Mich), report on behalf of the ROTSE
collaboration:
A fast fading optical transient has been discovered inside the error
circle for GRB 051109A (Swift trigger 163136) by the ROTSE-IIIb telescope,
located at McDonald Observatory (cf. Rykoff et al. GCN 4211). The source
faded as a power law. At the central time of UT 01:16:05 (228 seconds
after the Swift trigger), the magnitude was 16.21. (Magnitudes are
unfiltered and calibrated against R-band magnitudes for nearby comparison
stars.) The source is continuing to fade, but accurate magnitudes will
have to await a more detailed analysis due to nearby faint stars.
With these magnitudes, the power law index for the decline is -0.4. If
this decline continues unbroken, then at a time around two hours after the
burst (UT 03:12), the magnitude should be 17.7. Eight hours after the
burst (UT 09:12), a magnitude of 18.3 might be expected.
GCN Circular 4215
Subject
GRB 051109a: MDM Observations
Date
2005-11-09T03:52:12Z (20 years ago)
From
Jules Halpern at Columbia U. <jules@astro.columbia.edu>
N. Mirabal (U. Michigan), J. P. Halpern, and S. Tonnesen (Columbia U.)
report on behalf of the MDM Observatory GRB follow-up team:
"We are observing the afterglow of Swift GRB 051109 detected by ROTSE-IIIb
(Rykoff et al. GCN #4211, Schaefer et al. GCN #4214) using the MDM 2.4m
telescope and a Gunn r filter under partly cloudy conditions. From 38 minutes
to 148 minutes after the burst, the OT faded from R = 18.21 +/- 0.05 to
R = 19.22 +/- 0.08. Magnitudes are referenced to a USNO B1.0 star at
22h01m14.60s +40d49'25.3" (J2000) having R=17.23. This corresponds to a
power-law decay index of -0.68. Observations are continuing."
GCN Circular 4216
Subject
GRB 051109a: IR Photometry and Astrometry
Date
2005-11-09T04:17:16Z (20 years ago)
From
Josh Bloom at UC Berkeley <jbloom@astron.berkeley.edu>
J. S. Bloom (UC Berkeley), C. H. Blake (Harvard), D. Starr (Gemini)
and K. Alatalo (UC Berkeley) report:
"We have continued to observe the field of GRB 051109a (Tagliaferri
et al. 4213) at the position of the optical transient (GCNs 4211,
4214, 4215). Using a stack of PAIRITEL imaging from 2005-11-09
01:18:42.25 to 2005-11-09 01:33:14.94 UTC we find a 2MASS calibrated
photometry of J = 15.69 +/- 0.03, H = 14.95 +/- 0.03, Ks = 14.44
+/- 0.04. We also find an astrometric position of (J2000)
22:01:15.313, +40:49:23.31 with an uncertainty of 100 mas in each
axis. This is consistent with the Rykoff et al. position."
This message may be cited
GCN Circular 4227
Subject
GRB 051109a: BOOTES R & I-band detection of the early afterglow
Date
2005-11-09T12:52:27Z (20 years ago)
Edited On
2024-11-18T09:45:35Z (7 months ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
M. Jelínek, A. de Ugarte Postigo, A. J. Castro-Tirado,
S. Vitek, J. Gorosabel, S. B. Pandey and S. S. Guziy
(IAA-CSIC Granada), P. Kubanek (ISDC Versoix, and
ASU AV CR Ondrejov) and R. Hudec (ASU AV CR)
report:
"BOOTES-1B in El Arenosillo (southern Spain), responded
to the GRB 051109a trigger (Tagliaferri et al. GCNC 4213).
A sequence of exposures started at 01:13:15.3 UT (54.8s
after the GRB, 27s after the GCN notice), simultaneously
in the R and I-bands. We detect the optical afterglow first
reported by Rykoff et al. (GCNC 4211) in both passbands.
The approximate magnitude on the first 10s R-band image
is 16.2 calibrated against USNO-A2.0. Further analysis is in
progress."
This message may be cited.
GCN Circular 4228
Subject
GRB051109A: XRT refined analysis
Date
2005-11-09T13:40:11Z (20 years ago)
From
Sergio Campana at INAF-OAB <campana@merate.mi.astro.it>
S. Campana (INAF-OAB), T. Mineo (INAF-IASFPA), G. Tagliaferri (INAF-OAB),
V. Mangano (INAF-IASFPA), P. Romano (INAF-OAB), D.N. Burrows (PSU)
on behalf of the Swift/XRT team:
We have analysed 10 ks of XRT observations of GRB051109
(Tagliaferri et al., GCN 4213). The afterglow is bright and well
detected. The refined coordinates for this X-ray afterglow are:
RA(J2000): 22 01 15.3
Dec(J2000): +40 49 24
with an estimated uncertainty of 3.5 arcsec (90% containment) and
including the latest XRT boresight correction. The position is 3.2
arcsec from the on-board position reported by Tagliaferri et al.
(and 1.2 arcsec from the one by UVOT, ibid.) and 0.9 arcsec from
the optical afterglow first detected by ROTSE (Rykoff et al., GCN 4211).
The X-ray light-curve shows a clear break between the first and the second
Swift orbit (close to the end of the first orbit). In the first part the
decay is very steep with index alpha_1=-3.1 +/- 0.6 (90% containment)
whereas in the second part it flattens to alpha_2=-0.6 +/- 0.2.
The spectrum of the full data (WT and PC) can be modelled
with a power-law with photon index Gamma = 2.07 +/- 0.08 (90% containment).
There is evidence for an absorbing column higher than the Galactic value
(1.9e21 cm^-2) at a level of (8.2+/-5.2)e21 cm^-2 at the observed redshift
z=2.346 (Quimby et al., GCN 4221).
At 150 s the 0.5-10 keV unabsorbed flux was 3.2e-10 erg cm^-2 s^-1.
At 5000 s the afterglow had faded to flux level of 2.4e-11 erg cm^-2 s^-1.
Assuming the currect decay (which is very flat) we predict a flux
of ~5e-12 erg cm^-2 s^-1 at 1 d from the burst.
GCN Circular 4229
Subject
GRB051109A: further steepening in the X-ray light curve
Date
2005-11-09T16:49:51Z (20 years ago)
From
Sergio Campana at INAF-OAB <campana@merate.mi.astro.it>
S. Campana (INAF-OAB), T. Mineo (INAF-IASFPA), G. Tagliaferri (INAF-OAB),
V. Mangano (INAF-IASFPA), P. Romano (INAF-OAB) on behalf of the
Swift/XRT team:
After the analysis of the full initial dataset, we see that the
light curve of GRB051109A shows a further break besides the one
already highlighted previously (Campana et al., GCN 4228).
This second break is relatively unconstrained occurring between
the first (<200 s) and the second (>3000 s) Swift orbit.
In the first part the decay is very steep with index
alpha_1=-3.1 +/- 0.6 (90% containment, as reported). The second
power law contains basically no data and it is only loosely
constrained. The third power law has alpha_3=-1.2 +/- 0.1.
The reduced chi2 is 1.2 (57 dof).
The expected flux at 1 day is 8e-13 erg cm^-2 s^-1.
[GCN_OPS_NOTE(09nov05): Per author's request, the Subject line
was changed from "050911A" to "051109A".]
GCN Circular 4230
Subject
GRB 051109A : Lulin BVRI Optical afterglow observation
Date
2005-11-09T17:49:22Z (20 years ago)
From
Yuji Urata at RIKEN <urata@crab.riken.go.jp>
GRB 051109A : Lulin BVRI Optical afterglow observation
F.Y. Huang, K.Y. Huang, W.H. Ip (NCU), Y. Urata(RIKEN),
Y. Qiu (BAO), Y.Q. Lou (THCA) on behalf of EAFON report:
"We have observed GRB 051109A afterglow (Rykoff et al. GCN4211) using
Lulin 1-m telescope from 9.59 to 13.34 hours after ther burst. The
afterglow was detected in our B,V,R,I band images. The R band
magnitude of afterglow at 10.97 UT is estimated as R=20.3 calibrated
against USNO-B1.0 catalog.
Further analysis is in progress.
This message may be cited."
GCN Circular 4235
Subject
GRB 051109A: Swift-UVOT Observations
Date
2005-11-09T19:55:43Z (20 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <sholland@milkyway.gsfc.nasa.gov>
GRB 051109A: Swift-UVOT Observations
S. T. Holland (GSFC/USRA), S. Campana (INAF-OAB), P. Smith (UCL/MSSL),
H. Huckle (UCL/MSSL), & N. Gehrels (GSFC) on behalf of
the Swift-UVOT team report:
The Swift-UVOT began observing the field of GRB 051109A (BAT
Trigger 163136; Palmer, et al. GCN Circular 4213) at
2005-11-09T01:14:09, 109 seconds after the burst.
We detect an optical transient at
RA(J2000) = 22:01:15.32
Dec(J2000) = +40:49:23.7
with a positional uncertainty of +/-0.5 arcsec (90% confidence),
in agreement with the position of Rykoff, et al. (2005, GCN Circular
4211). The transient has V = 16.49 +/- 0.07 (1-sigma, statistical)
in an 89 s exposure starting at 2005-11-09T01:14:23, 123 seconds after
the BAT trigger. This value supercedes the approximate magnitude given
in Palmer, et al. (2005, GCN Circular 4213). This magnitude has not
been
corrected for Galactic extinction.
Further observations and analysis are underway.
GCN Circular 4238
Subject
Konus-Wind observation of GRB 051109A
Date
2005-11-09T23:00:13Z (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 report:
The long soft GRB 051109A (Swift-BAT trigger #163136;
Tagliaferri et al., GCN 4213, E. Fenimore et al., GCN 4217)
triggered Konus-Wind at T0= 4342.541 s UT (01:12:22.541).
As observed by Konus-Wind it had a single pulse with a duration
about ~11 sec and a long decaying tail.
This tail was seen up to ~130 sec after T0.
The preliminary analysis of the Konus-Wind
data gave the burst fluence 4.0(-3.4, +0.3)10^-6 erg/cm2,and
peak flux on 256-ms time scale 5.8(-4.9, +0.3)10^-7 erg/cm2/sec
(both in the 20 - 500 keV energy range).
These values are very uncertain due to weakness and softness
of the burst.
The K-W spectrum integrated over the most intense part of the GRB
(from T0 to T0+8.448 s) is well fitted (in the 20 - 500 keV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-E/E0)
with alpha = 1.25 (-0.59, +0.44)
and E0 = 213 (-126, +246) keV (chi^2 = 56/56 dof).
The peak energy Ep = 161 (-58, +224) keV.
All the quoted errors are at the 90% confidence level.
Assuming z = 2.346 (Quimby et al., GCN 4221) and a standard cosmology
model with H_0 = 70 km/s/Mpc, Omega_M = 0.3, Omega_\Lambda = 0.7,
the isotropic energy release is E_iso ~5x10^52 erg,
the maximum luminosity is (L_iso)_max ~2.4x10^52 erg/s.
Further analysis and refinement is in progress.
GCN Circular 4239
Subject
Early RAPTOR measurements of GRB 051109a - the movie.
Date
2005-11-10T00:37:54Z (20 years ago)
From
Przemyslaw R. Wozniak at LANL <wozniak@lanl.gov>
P.R. Wozniak, W.T. Vestrand, J. Wren, R. White, S. Evans
on behalf of the RAPTOR team report:
Starting at 01:12:54.42 UT on November 9, 33.9 seconds after
the Swift BAT trigger, the Raptor-S robotic telescope at
Los Alamos National Laboratory responded to Swift trigger 163136
(Tagliaferri et al., GCN 4213). The automated response was
composed of a series of ten 5-second duration exposures followed
by 20 10-second exposures and finally by 183 30-second exposures.
The unfiltered images show an optical transient at the position
identifed by Rykoff et al. (GCN 4211) that fades from magnitude
R ~15.1 to ~17.5 over the course of 20 minutes. The unfiltered
magnitudes were transformed to the R2 magnitude scale of the
USNO B1.0 catalog. Short animations derived from the RAPTOR images
can be viewed at:
EPISODE I: "The First Four Minutes"
http://www.raptor.lanl.gov/images/GRB051109a/grb051109a_early_movie.gif
EPISODE II: "The Next Half Hour"
http://www.raptor.lanl.gov/images/GRB051109a/grb051109a_late_movie.gif
GCN Circular 4240
Subject
GRB 051109A: KAIT optical observations
Date
2005-11-10T05:42:17Z (20 years ago)
From
Weidong Li at UC Berkeley KAIT/LOSS <weidong@astron.berkeley.edu>
W. Li, University of California, Berkeley, on behalf of the
KAIT GRB team, report:
We remotely observed GRB 051109A (Tagliaferri et al., GCN 4213)
with the 0.76-m Katzman Automatic Imaging Telescope (KAIT) at
Lick Observatory, and detected the afterglow (Rykoff et al., GCN 4211)
in a series of unfiltered exposures. The following photometry
are measured (calibrated to the USNO B1.0 catalog):
Start UT Exp(s) mag err
2005-11-09 02:25:48 120.0 18.67 0.04
2005-11-09 02:28:28 120.0 18.73 0.06
2005-11-09 02:31:05 240.0 18.75 0.05
2005-11-09 02:35:37 240.0 18.82 0.04
2005-11-09 02:40:14 360.0 18.80 0.04
2005-11-09 02:46:48 360.0 18.88 0.04
2005-11-09 02:53:27 600.0 18.93 0.04
Within this period (74.5 to 106.1 minutes after the burst),
the afterglow declined with a power-law decay index of
-0.62 +/- 0.07, consistent with the result resported by Mirabal
et al. (GCN 4215).
GCN Circular 4243
Subject
GRB051109A - radio observations
Date
2005-11-10T10:21:05Z (20 years ago)
From
Guy Pooley at MRAO, Cambridge, UK <ggp1@cam.ac.uk>
Guy Pooley, MRAO, Cavendish Lab, University of Cambridge reports:
The Ryle Telescope (Cambridge, UK) was used to map the field
containing GRB051109A (GCN 4211) at 15GHz. The observation ran from
2005Nov09 12h57m to 2005Nov10 00h54m, centred 17h45m after the
initial detection.
No source was detected at the position of the GRB
(Rykoff et al, GCN 4211; Holland et al, GCN 4235);
the formal value was S = 0.40 mJy with rms noise 0.16 mJy.
When the data were divided into two halves,
the resulting estimates of flux density were
First half (centred on 2005Nov09.75) 0.25 +- 0.23 mJy
Second half (centred on 2005Nov10.25) 0.54 +- 0.23 mJy
GCN Circular 4244
Subject
GRB 051109A
Date
2005-11-10T19:04:56Z (20 years ago)
From
Dale A. Frail at NRAO <dfrail@nrao.edu>
Dale A. Frail (NRAO), P. Brian Cameron (Caltech), and Alicia
M. Soderberg (Caltech) report on behalf of a larger collaboration:
"We observed the field of GRB 051109A (GCN 4213) with the Very Large
Array at 8.5 GHz around November 11.15 UT. At the position of the
optical transient (GCN 4211) there is a weak radio source with flux
density 117 � 24 uJy. We identify this as the radio afterglow of
GRB 051109A.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."
GCN Circular 4259
Subject
GRB 051109A Optical Observations
Date
2005-11-11T12:26:41Z (20 years ago)
From
Kuntal Mishra at ARIES,Nainital,India <kuntal@aries.ernet.in>
Kuntal Misra (ARIES, Nainital), Atish P. Kamble (Raman Research
Institute, Bangalore), D. K. Sahu, S. Srividya, P. Bama, G.C. Anupama and
Mr. S. Vanniarajan (Indian Institute of Astrophysics, Bangalore) on behalf
of a larger Indian GRB collaboration
We observed the field of GRB 051109A (swift trigger=163136) using the 1-m
Sampurnanand Telescope (ST) at ARIES, Naini Tal in Cousins R and I filters
and the 2-m Himalayan Chandra Telescope (HCT), IAO, Hanle in Bessell B and
V filters, starting nearly 12 hours after the burst. The Optical Transient
(OT) mentioned by Rykoff et al. (GCN 4211) is clearly seen in images of
10 minutes exposure time. The preliminary magnitude of the OT in different
bands in comparison to 5 nearby USNO-B1.0 stars is:
UT Magnitude error Band Telescope used
Nov 09.5681 19.449 0.08 I ST
Nov 09.5796 20.715 0.09 R ST
Nov 09.5463 22.044 0.09 B HCT
The OT decayed by ~ 0.6 mag from Nov 09.5681 to Nov 09.7201 UT
in R band and by 0.28 mag in B in ~2.4 hrs. Further analysis is in
progress.
This message may be cited.
GCN Circular 4265
Subject
GRB 051109A Milagro GeV/TeV Observations
Date
2005-11-11T22:18:05Z (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 GRB
051109A (GCN Circ 4213, G. Tagliaferri et al.), during the burst duration
(36 s) reported by the Swift team (GCN Circ 4217, E. Fenimore et al.).
No evidence for prompt GeV/TeV emission was found. A preliminary analysis,
assuming a differential photon spectral index of -2.4, gives an upper
limit on E^2dN/dE at 99% confidence of:
E^2dN/dE at 2.5 TeV < 8.4 * 10^(-8) erg cm^(-2) (No EBL absorption assumed)
The spectrum of the host galaxy of the proposed afterglow of GRB 051109A
implies a redshift of 2.346 (GCN Circ 4221, R. Quimby et al.). TeV photons
are attenuated by pair production with infrared photons in intergalactic
space so we also calculate upper limits assuming different extragalactic
infrared background light (EBL) absorption models, one by Kneiske et al.
2004 (A&A 413, 807) and one by Primack et al. 2005 (AIP Conf. Proc. 745,
p. 23). We find 99% confidence level upper limits on E^2dN/dE of:
E^2dN/dE at 55 GeV < 1.7 * 10^(-3) erg cm^(-2) (Primack et al. EBL model)
E^2dN/dE at 60 GeV < 2.3 * 10^(-4) erg cm^(-2) (Kneiske et al. EBL model)
The energies quoted represent the approximate median energy of the events
that would be detected assuming a power law spectrum with differential
index -2.4 convolved with each of the absorption models. These upper
limits are preliminary and will be refined with further analysis.
GCN Circular 4273
Subject
GRB051109A optical observations
Date
2005-11-15T06:34:42Z (20 years ago)
From
Vasilij Rumjantsev at CrAO <rum@crao.crimea.ua>
E. Pavlenko (CrAO), K. Berezovsky (�SAS), V.Rumyantsev (CrAO),
A.Pozanenko (IKI) on behalf of larger GRB follow up collaboration report:
We observed GRB051109A afterglow (Rykoff et al. GCN4211) with 0.38-m
telescope in R band on Nov.9 between 15:51 and 17:34 (UT).
Preliminary photometry of a stacked image against of USNO A2.0 is following:
Mid time, Exposure, Filter, Mag.
(UT) (s)
Nov. 9 16:43 120x50 R 20.7 +/- 0.2
The message may be cited.
GCN Circular 4295
Subject
GRB 051109A : GAO 150cm telescope Rc-band detection
Date
2005-11-22T06:10:34Z (20 years ago)
From
Kenzo Kinugasa at Gunma Astro. Obs/Japan <kinugasa@astron.pref.gunma.jp>
K. Kinugasa (Gunma Astronomical Observatory) and K. Torii (Osaka U.) report:
The error region of GRB 051109A (Tagliaferri et al. GCN 4213) was imaged by
the LN2 cooled CCD camera atattched on the 150 cm telescope of the Gunma
Astronomical Observatory.
Starting at 2005 November 9, 14:56 UT (0.57 days after the burst), nine 30 s
and five 180 s exposures in Rc band were obtained.
In a stacked frame, the optical afterglow (Rykoff et al. GCN 4211) is
detected as follows, relative to USNO-B1.0 R2 magnitude.
------------------------
MidUT Filter Mag
------------------------
15:08 Rc 20.5
------------------------