GRB 051021A, GRB 051021
GCN Circular 4294
Subject
GRB 051021 Optical Observations
Date
2005-11-20T05:37:23Z (21 years ago)
From
T.P. Prabhu at Indian Astro. Obs. <tpp@crest.ernet.in>
D.K. Sahu, G. Pandey, P. Bama and N.K. Chakradhari (Indian Institute of
Astrophysics, Bangalore,India) communicate on behalf of a larger Indian
collaboration:
We observed the error box of the HETE trigger 3947 in Bessell R and I
filters with the 2-m Himalayan Chandra Telescope, Hanle, India, between
20:25 UT and 21:00 UT, 2005 October 21 (about 7 hours after the burst).
We could clearly detect the OT of GRB 051021 reported by Fox et al. (GCN
4120) with effective exposures of 600s (2x300s) in R and 900s (3x300s) in
I band. The preliminary magnitudes for the OT, estimated using the
calibration provided by Henden (GCN 4184) are as follows:
Filter Mean Mid-UT Magnitude
R 20:43 21.51+/-0.15
I 20.43 20.93+/-0.10
This message may be cited.
GCN Circular 4180
Subject
GRB 051021A: RTT150 optical observations
Date
2005-10-30T06:41:30Z (21 years ago)
From
Rodion Burenin at IKI, Moscow <rodion@hea.iki.rssi.ru>
R. Burenin, D. Denisenko, M. Pavlinsky, R. Sunyaev (IKI), I. Khamitov,
Z. Aslan (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.),
I. Bikmaev, N. Sakhibullin (KSU/AST)
report:
The optical transient associated with GRB 051021A (Yoshida et al., GCN
4116; Fox et al., GCN 4120) was observed with Russian-Turkish 1.5-m
telescope (RTT150, Bakyrlytepe, TUBITAK National Observatory, Turkey) in
BVR filter set, starting at Oct. 21, 18:15 UT, 4.88 hours after the
burst.
Compared to USNOB, the magnitudes are about:
t-t0,h
5.34 R=21.1
9.95 R=21.8
5.70 V=22.2
10.18 V=22.6
In B the object was detected only marginally.
This message may be cited.
GCN Circular 4166
Subject
GRB 051021, Optical Observations
Date
2005-10-26T14:33:54Z (21 years ago)
From
Kuntal Mishra at ARIES,Nainital,India <kuntal@aries.ernet.in>
Kuntal Misra (ARIES, Nainital) and Atish P. Kamble (Raman Research
Institute, Bangalore) on behalf of a larger Indian GRB collaboration
We observed the field of GRB 051021 (HETE trigger 3947) using the 104 cm
reflector telescope at ARIES, Nainital. We do not find any new source upto
a limiting magnitude of 21 in our combined (exposure 3*300 sec) R band
images on October 22.675 UT with respect to five nearby USNO-A2.0 stars.
This message may be cited.
GCN Circular 4159
Subject
GRB051021a: optical observations
Date
2005-10-24T13:59:34Z (21 years ago)
From
Vasilij Rumjantsev at CrAO <rum@crao.crimea.ua>
V.Rumyantsev (CrAO), V.Biryukov (SAI, MSU), and A.Pozanenko (IKI) on behalf
of larger GRB follow up collaboration report:
We observed the SXC error box of HETE-2 GRB051021a (Yoshida et al.,
GCN4116) with 0.6 m telescope (Crimean laboratory of SAI) equipped with FLI
IMG-1001E camera. The series of 60 sec R-band exposures were taken between
October 21, 21:19:01 and October 22, 00:23:24. We clearly detect the
optical afterglow (Fox et al. GCN4120, Swan et al. GCN4120) on stacked
image. Coordinates of the source are RA=01 56 36.37 Dec=+09 04 03.27 (J2000)
with uncertainty of 0.5 arcsec. Preliminary photometry of the stacked image
is following:
Mid time (UT) Exposure R
Oct. 21 22:51 146x60 21.9 +/-0.2
Photometry and astrometry of the source are based on USNO-A2.0.
Stacked image can be found in http://grb.rssi.ru/GRB051021a/.
Taken R-band magnitudes (GCNs 4120, 4123) and upper limit reported in
GCN4138 (Eastman et al.) our results is compatible within statistical error
with single power-law decay light curve alpha ~ -1.6. Also extrapolating
backward J-band (Reichart et al., GCN 4144) observations to our epoch (Oct.
21 22:51) we found R-J ~ 1.0 which do not imply a high redshift source.
This message may be cited.
GCN Circular 4151
Subject
GRB051021A: Swift XRT refined analysis
Date
2005-10-23T18:34:01Z (21 years ago)
From
Judith Racusin at PSU <racusin@astro.psu.edu>
J. Racusin, D. Fox, D. Burrows (PSU), N. Gehrels (GSFC) on behalf of the
Swift XRT team:
We have analyzed the first four orbits of data after XRT began observing
the field of GRB051021A (Yoshida et al., GCN 4116) at 16:28:28 UT. The
refined XRT coordinates are:
RA(J2000): 01 56 36.5
Dec(J2000): +09 04 6.1
with an estimated uncertainty of 4 arcseconds (90% containment), including
corrections for the XRT boresight offset. This position is 1 arcsecond
from the position we quoted in Racusin et al. (GCN 4125), and 2.9
arcseconds from the optical afterglow candidate reported by Fox et al.
(GCN 4120).
The XRT light curve shows a steady decline with a power-law fit decay
index of 1.06+/-0.16.
The Photon Counting mode spectra can be fit with an absorbed power-law
with a photon index of 2.17+/-0.18 and a column density of 1.4+/-0.5 E21
cm-2 which is in excess of the Galactic column density of 0.56E21 cm-2 in
this direction. The observed 0.2-10 keV flux is 2.02E-12 ergs cm-2 s-1,
corresponding to an unabsorbed flux of 2.28E-12 ergs cm-2 s-1.
GCN Circular 4147
Subject
GRB 051021: PROMPT RcIc Observations
Date
2005-10-23T06:53:44Z (21 years ago)
From
Melissa Nysewander at UNC,Chapel Hill <mnysewan@physics.unc.edu>
M. Nysewander, C. Macleod, D. Reichart, A. Crain, A. Foster report on
behalf of the UNC team of the FUN GRB Collaboration:
Under the control of Skynet, PROMPT observed the localization of GRB 051021
(Yoshida et al., GCN 4116; Fox et al., GCN 4120) beginning 12.9 hours after
the burst, in Rc and Ic simultaneously.
We do not detect the afterglow of the burst. In two 90 x 60 sec
integrations of mean epoch 14.2 hours after the burst, we measure 3-sigma
limiting magnitudes of Rc = 20.7 and Ic = 20.4 based on 5 USNO-B1.0 stars.
PROMPT is still being built and commissioned.
GCN Circular 4144
Subject
GRB 051021: Correction
Date
2005-10-23T03:52:56Z (21 years ago)
From
Daniel E. Reichart at U.North Carolina <reichart@physics.unc.edu>
D. Reichart reports on behalf of the UNC team of the FUN GRB Collaboration:
Cobb & Bailyn (GCN 4142) are correct. The correct J magnitude at 12.3
hours after the burst is 20.3 +/- 0.2 mag.
Using 4.1m SOAR, we observed the afterglow in BVRIYJHKs. We will report on
the SFD in a forthcoming GCN.
GCN Circular 4142
Subject
GRB 051021, SMARTS optical/IR observations
Date
2005-10-23T01:56:24Z (21 years ago)
From
Bethany Cobb at Yale U <cobb@astro.yale.edu>
B. E. Cobb and C. D. Bailyn (Yale), part of the larger SMARTS
consortium, report:
Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 051021
(GCN 4116, Yoshida et al.) with a mid-exposure time of
2005-10-22 02:53 UT, which is ~13.5 hours post-burst.
Total summed exposure times amounted to 36 minutes in I and 30
minutes in J.
At the position of the reported afterglow (GCN 4120, Fox et al.), an
object is marginally detected in our I-band images. The preliminary
magnitude of this object is determined to be I = 22.0 +/- 0.4, in
comparison with several nearby USNO B1.0 stars.
The afterglow candidate is not, however, detected in the J-band. Using
several 2MASS comparison stars, the limiting magnitude of this image
is determined to be J > 19.9 +/- 0.1.
There is an object near to the position of the afterglow candidate
(at RA = 1:56:35.6, Dec = 9:04:26.2) that is measured in our image
to have a magnitude of J = 17.2 +/- 0.1. This object is below the
detection limits of 2MASS, so it is not detected in the 2MASS
images (though it is present in the USNO B1.0 survey). Possibly, this is
the object reported by Haislip et al. (GRB 4127). Therefore, in agreement
with Cenko et al. (GCN 4140), there is not yet clear evidence
to suggest that this is a high redshift event.
GCN Circular 4140
Subject
GRB 051021: P200 Ks Observations
Date
2005-10-22T21:41:37Z (21 years ago)
From
S. Bradley Cenko at Caltech <cenko@srl.caltech.edu>
S. Bradley Cenko, Chris Conselice, Kevin Bundy, (Caltech), Derek B. Fox
(Penn State), and Edo Berger (Carnegie), report on behalf of the
Caltech-NRAO-Carnegie GRB collaboration:
"We have imaged the field of GRB 051021 (Yoshida et al., GCN 4116) with
the Wide Field Infrared Camera mounted on the Palomar 200" Hale Telescope.
Our images consisted of 9 x 120 s exposures taken in the Ks filter at a
mean epoch of approximately 22 October 5:24 UT (~ 16 hours after the
burst). We find at best a marginal (< 3-sigma) detection at the location
of the OT (Fox et al., GCN 4120). Our 3-sigma limiting magnitude,
calculated with respect to several 2mass stars in the field, is
approximately Ks > 19.0.
We note that under the standard afterglow model, our result is
inconsistent with the J-band detection reported by Haislip et. al (GCN
4127), and therefore calls into question the interpreration of GRB 051021
as a high redshift event."
GCN Circular 4138
Subject
GRB 051021: MDM Upper Limit
Date
2005-10-22T18:37:45Z (21 years ago)
From
Jules Halpern at Columbia U. <jules@astro.columbia.edu>
J. Eastman, D. L. Depoy (Ohio State U.), A. P. Crotts, & D. J. Beirne
(Columbia U.) observed the afterglow (Fox et al., GCN 4120) of
HETE GRB 051021 (Yoshida et al., GCN 4116; Olive et al., GCN 4124)
in the R band using the MDM 1.3m, and in SDSS r using the MDM 2.4m.
On Oct. 22 04:45 UT, 15.4 hours after the burst, they report a 5-sigma
upper limit of R > 23.0. Compared with the Lulin measurement of R=19.8
at 2.5 hours (Hsieh et al., GCN 4123), this indicates a mean temporal
decay index steeper than -1.6, possibly a jet break. In combination
with the bright near-IR detection by Haislip et al. (GCN 4127), J=17.16
at 12.4 hours, and if the decay index between 12.4 and 15.4 hours is
not steeper than -3.5, the implied R-J color is greater than 5, which
requires a high redshift.
GCN Circular 4136
Subject
GRB051021: Swift/UVOT Upper Limits
Date
2005-10-22T17:01:06Z (21 years ago)
From
Peter Brown at PSU <pbrown@astro.psu.edu>
P. J. Brown (PSU), D. Fox (PSU), M. Trippico (GSFC-SSAI),
J. Nousek (PSU), & N. Gehrels (GSFC)
on behalf of the Swift/UVOT team report:
The Swift-UVOT began observing the field of
GRB 051021 (HETE Trigger H3947; Yoshida et al. GCN 4116)
at 2005-10-21 16:28:27, about 3 hours after the burst.
No source is detected at the position of the optical
counterpart found by Fox, McNaught, & Peterson (GCN 4120)
in any of our 6 filters down to the following 3-sigma
upper limits:
Filter T_range(hours) Exp(sec) 3sigUL
V 3.36-8.34 1988 20.2
B 5.30-6.71 1304 21.1
U 5.04-5.29 900 20.5
W1 4.79-5.04 900 20.8
M2 3.61-3.80 900 20.9
W2 3.11-6.96 1800 21.7
Where T_range is time post-trigger.
GCN Circular 4129
Subject
GRB 051021,optical observation
Date
2005-10-22T09:08:20Z (21 years ago)
From
Eri Sonoda at U of Miyazaki/Japan <sonoda@astro.miyazaki-u.ac.jp>
E.Sonoda,S.Maeno,Y.Tokunaga, M.Yamauchi
(University of Miyazaki)
"We have observed the field covering the SXC error box of
GRB051021(HETE trigger 3947; trigger time 13:21:5 UT ) with the
unfiltered CCD camera on the 30-cm telescope at University of
Miyazaki.The observation was started 13:22:30 UT on Oct.21.
We have compared our image with the USNO A2.0 catalog .
Preliminary analysis shows there is no new source brighter than 14.3 mag.
at the position reported by D.B.Fox et al.(GCN4120). "
GCN Circular 4127
Subject
GRB 051021: SOAR NIR Observations
Date
2005-10-22T03:54:03Z (21 years ago)
From
Josh Haislip at U.North Carolina <haislip@physics.unc.edu>
J. Haislip, M. Nysewander, E. Cypriano, D. Reichart, M. Bayliss report on
behalf of the UNC Team of the FUN GRB Collaboration:
The SOAR-4.1m Telescope at CTIO began imaging the afterglow of the HETE GRB
051021 (Yoshida et al., GCN 4116; Fox et al., GCN 4120) at 01:38:51 UT,
12.3 hours after the burst in YJHKs.
We detect the afterglow at a magnitude of J = 17.16 +- 0.06 based on three
2MASS stars at a mean time of 01:47:19.2 UT, 12.4 hours after the GRB.
GCN Circular 4125
Subject
GRB051021: Swift XRT analysis
Date
2005-10-21T21:52:23Z (21 years ago)
From
Judith Racusin at PSU <racusin@astro.psu.edu>
J. Racusin, J. Kennea, D. Morris, D. Fox, D. Burrows (PSU), N. Gehrels
(GSFC) on behalf of the Swift XRT team:
XRT began observing GRB051021 (Yoshida et al., GCN 4116) at 16:28:28 UT,
approximately 3 hours after the HETE trigger. From the first 2 orbits of
data, we detect an uncatlogued fading X-ray source at:
RA(J2000): 01:56:36.4
Dec(J2000): +09:04:06.3
with an estimated uncertainty of 4 arcseconds (90% containment).
This position is 4.3 arcminutes from the HETE position reported by Yoshida
et al.(GCN 4116), and 2.7 arcseconds from the optical afterglow position
reported by Fox et al.(GCN 4120).
At the time of these observations using 4.7 ks of data, the measured flux
was 2.7x10^-12 ergs/cm^2/s. Further observations are necessary to measure
the lightcurve decay slope.
GCN Circular 4124
Subject
GRB051021 (=H3947): Refined Analysis
Date
2005-10-21T20:57:21Z (21 years ago)
From
Carlo Graziani at U.Chicago <carlo@oddjob.uchicago.edu>
J-F Olive, G. Ricker, J-L. Atteia, N. Kawai, D. Lamb, and S. Woosley,
on behalf of the HETE Science Team;
M. Arimoto, T. Donaghy, E. Fenimore, M. Galassi, C. Graziani,
N. Ishikawa, A. Kobayashi, J. Kotoku, M. Maetou, M. Matsuoka,
Y. Nakagawa, T. Sakamoto, R. Sato, T. Shimokawabe, Y. Shirasaki,
S. Sugita, M. Suzuki, T. Tamagawa, K. Tanaka, and A. Yoshida, on behalf
of the HETE WXM Team;
N. Butler, G. Crew, J. Doty, G. Prigozhin, R. Vanderspek,
J. Villasenor, J. G. Jernigan, A. Levine, G. Azzibrouck, J. Braga,
R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and
HETE Optical-SXC Teams;
M. Boer, J-P Dezalay, and K. Hurley, on behalf of the HETE FREGATE
Team;
report:
We have analyzed the full FREGATE+WXM data for HETE trigger H3934
(GRB051021.56).
The 30-400 keV light curve has two sharp peaks, separated by about 10 s,
superposed on a gentler rise-and-fall. The burst had a T90 duration of 38s
in the 7-40 keV band, and of 27s in the 30-400 keV band. Emission in the
2-25 keV band appears to continue for at least 90s post-trigger, mostly
below 10 keV.
The integrated spectrum is well-fit by a cutoff power-law function. The
best-fit parameters are:
alpha = -1.16 --- 90% confidence interval is [-1.25 -1.06]
Epeak = 94.2 --- 90% confidence interval is [76.7 , 111.7]
The 2-30 keV fluence is 3x10^-6 erg/cm2, while the 30-400 keV fluence is
6 x 10^-6 keV. Since the ratio S(2-30)/S(30-400) is 0.41, this event is
classified as an X-Ray Rich GRB.
The pseudo-redshift estimated for this burst is pz = 1.4.
A light curve, a skymap, and spectral information for this event are
provided at the following URL:
http://space.mit.edu/HETE/Bursts/GRB051021
GCN Circular 4123
Subject
GRB 051021 : optical afterglow observation at Lulin
Date
2005-10-21T19:19:48Z (21 years ago)
From
Kuiyun Huang at IANCU <d919003@astro.ncu.edu.tw>
GRB 051021 : optical afterglow observation at Lulin
H.H. Hsieh (IfAUH), M.S. Chang, K.Y. Huang, W.H. Ip (NCU), Y. Urata
(RIKEN), Y. Qiu (BAO) on behalf of the East Asian collaboration
report:
The R-band observations of GRB 051021 (Yoshida et al., GCN 4116) were
taken by Lulin 1-m telescope, Taiwan. The optical afterglow reported
by Fox et al.(GCN 4120) was detected clearly in our R-band
images. Compared with USNOB stars, the R band magnitude of afterglow
is about 19.8 at 15.859 UT (~ 2.48 hrs after the burst).
Further observations are on going.
This message may be cited.
GCN Circular 4122
Subject
GRB 051021: Optical observations
Date
2005-10-21T18:04:54Z (21 years ago)
From
Sergei Guziy at IAA <gss@iaa.es>
P. Tristram (Univ. of Canterbury, New Zealand),S. Guziy,
A. de Ugarte Postigo, Shashi. B. Pandey, A. J. Castro-Tirado,
M. Jelinek, J. Gorosabel (IAA-CSIC, Granada, Spain),
and Ph. Yock (Univ. of Auckland, New Zealand)
report:
"We have observed the region centered around the HETE error box
for GRB 051021 (Yoshida et al.2005, GCN 4116) with
0.6 m telescope at Mount John observatory (New Zealand), starting
on October 21 ( 14:10 UT, 45 minutes after the GRB). We confirm the
optical candidate reported by Fox et al. (GCN, 4120)."
Further observations are in progress.
This massage can be cited.
GCN Circular 4121
Subject
GRB 051021: ROTSE-III Confirmation of Optical Counterpart
Date
2005-10-21T17:37:42Z (21 years ago)
From
Heather Swan at U.of Michigan/ROTSE <hflewell@umich.edu>
H. Swan (U Mich), T.A. McKay (U Mich), D.A. Smith (Guilford), B.
Schaefer (Louisiana State), E.S. Rykoff (U Mich), F. Yuan (U Mich),
report on behalf of the ROTSE collaboration:
ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded
to GRB 051021 (HETE trigger 3947). The first image was at 13:22:28.4 UT,
31.8 s after the burst (6.6 s after the GCN notice time). The unfiltered
images are calibrated relative to USNO A2.0. We confirm the presence of
the source detected by Fox et. al. GCN # 4120. We observe the source to
rise to 16.9 magnitude, at about 180 seconds, and then fade by half a
magnitude over a period of 150 seconds.
This source is not visible in DSS (second epoch), 2MASS or the MPChecker
database.
Continuing observations are in progress.
>
GCN Circular 4120
Subject
GRB 051021: Optical observations and candidate afterglow
Date
2005-10-21T16:59:15Z (21 years ago)
From
Derek Fox at PSU <dfox@astro.psu.edu>
D.B. Fox (Penn State), with R. McNaught and B. Peterson (RSAA/ANU),
report on behalf of a larger collaboration:
"We have observed the HETE localization region for GRB051021 (Yoshida
et al., GCN 4116) with the 40-inch telescope at Siding Spring
Observatory, in a sequence of R-band exposures beginning at 13:48:48
UT (26m51s after the burst). Comparison of a coadded image with mean
epoch 14:34:33 (1h12m post-burst) to the Digitized Sky Survey reveals
the presence of a new R~18.5 mag source, at coordinates:
R.A. 01:56:36.39, Dec +9:04:03.7 (J2000)
with a coordinate uncertainty, relative to USNO-B1.0 catalog
astrometry, of <0.5". Inspection of our individual images suggests
fading of the source over the ~1 hour span of our observations.
However, in the absence of a more sophisticated reduction of these
data it is not possible to make a firm conclusion as to variability at
this time. Moreover, the presence of a cosmetic defect at the source
position in one image introduces significant uncertainty to our
mean photometric estimate, above.
We suggest that this source may be the optical afterglow of
GRB051021."
GCN Circular 4116
Subject
GRB051021: A GRB Localized by HETE
Date
2005-10-21T15:14:48Z (21 years ago)
From
Carlo Graziani at U.Chicago <carlo@oddjob.uchicago.edu>
A. Yoshida, G. Ricker, J-L. Atteia, N. Kawai, D. Lamb, and S. Woosley,
on behalf of the HETE Science Team;
M. Arimoto, T. Donaghy, E. Fenimore, M. Galassi, C. Graziani,
N. Ishikawa, A. Kobayashi, J. Kotoku, M. Maetou, M. Matsuoka,
Y. Nakagawa, T. Sakamoto, R. Sato, T. Shimokawabe, Y. Shirasaki,
S. Sugita, M. Suzuki, T. Tamagawa, and K. Tanaka, on behalf of the HETE
WXM Team;
N. Butler, G. Crew, J. Doty, G. Prigozhin, R. Vanderspek,
J. Villasenor, J. G. Jernigan, A. Levine, G. Azzibrouck, J. Braga,
R. Manchanda, and G. Pizzichini, on behalf of the HETE Operations and
HETE Optical-SXC Teams;
M. Boer, J-F Olive, J-P Dezalay, and K. Hurley, on behalf of the HETE
FREGATE Team;
report:
The HETE FREGATE, WXM, and SXC instruments detected GRB 051021
(=H3947) at 13:21:57 UT (48117 SOD) on 21 October 2005. The
WXM flight localization was first reported in a GCN Notice issued
at 13:22:11 UT, which was 14s after the burst trigger.
Ground analysis of the WXM data produced a refined WXM localization that
was issued in a GCN Notice at 14:25:34 UT. This ground WXM localization
can be expressed as a circle of 7.5 arcminutes radius (90% confidence),
centered at
R.A. = 01h 56m 24s ; Dec. = +09d 07' 05" (J2000).
The SXC detected this event in its Y camera. Ground analysis of the SXC
data therefore produced a 1-dimensional location. The intersection of
this location with the WXM ground location was issued in a GCN Notice at
14:59:49 UT. This location can be expressed as a box with corners:
R.A. = 01h 56m 01.92s ; Dec. = +09d 02' 02.4"
R.A. = 01h 56m 54.00s ; Dec. = +09d 05' 16.4"
R.A. = 01h 56m 54.72s ; Dec. = +09d 07' 22.8"
R.A. = 01h 59m 57.12s ; Dec. = +09d 03' 46.8" (J2000).
Further analysis is in progress.