GRB 021113
GCN Circular 1686
Subject
GRB021113 (=H2449): A Long GRB Localized by HETE
Date
2002-11-13T14:32:36Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB021113 (=H2449): A Long GRB Localized by HETE
A. Yoshida, Y. Shirasaki, C. Graziani, M. Matsuoka, T. Tamagawa, K.
Torii, T. Sakamoto, E. Fenimore, M. Galassi, T. Tavenner, T. Donaghy,
Y. Nakagawa, D. Takahashi, M. Suzuki, R. Satoh, and Y. Urata, on
behalf of the HETE WXM Team;
G. Ricker, J-L Atteia, N. Kawai, D. Lamb, and S. Woosley on behalf of
the HETE Science Team;
J. Villasenor, N. Butler, G. Crew, J. Doty, G. Prigozhin, R.
Vanderspek, T. Cline, J. G. Jernigan, A. Levine, F. Martel, E.
Morgan, 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, C. Barraud and K. Hurley on behalf
of the HETE FREGATE Team;
write:
At 06:38:56.9 UTC (23936.9 s UT) on 13 Nov 2002, the HETE FREGATE and
WXM instruments detected event H2449, a long GRB.
Ground analysis of the WXM data for the burst produced a location
which was reported in a GCN Position Notice at 08:39 UT. Further
ground analysis of the WXM data produced a refined location, which
was reported in a second GCN Position Notice at 09:12 UT; an
additional refinement was reported in a third Position Notice at
13:17 UT.
The WXM localization SNR was 17. The refined WXM ground location can
be expressed as an error box (90% confidence) of 230 sq-arcmin area
centered at
RA = 01h 33m 53s, Dec = +40d 27' 45" (J2000).
The 4 corners of the WXM error box (90% confidence) are
RA = 01h 32m 44s, Dec = +40d 23' 56" (J2000)
RA = 01h 32m 47s, Dec = +40d 32' 48" (J2000)
RA = 01h 35m 02s, Dec = +40d 31' 33" (J2000)
RA = 01h 34m 58s, Dec = +40d 22' 40" (J2000)
The burst duration in the 8-40 keV band was about 20 s. In the 8-40
keV band, the peak flux was >2 x 10-7 ergs cm-2 s-1 (ie > 5 x Crab
flux; 1 s time scale) and the fluence was ~5 x 10-7 ergs cm-2 during
the brightest 4 s of the burst .
A light curve for GRB021113 is provided at the following URL:
http://space.mit.edu/HETE/Bursts/GRB021113/
This message is citable.
GCN Circular 1687
Subject
GRB 021113: Optical Observations
Date
2002-11-13T15:36:37Z (23 years ago)
From
Melissa Nysewander at UNC,Chapel Hill <mnysewan@physics.unc.edu>
M. Nysewander, D. Reichart (U. North Carolina), and M. Schwartz (Tenagra
Observatories) report:
We observed 100% of the 23 arcmin x 13 arcmin error box, but only 90% of
the revised 26 arcmin x 9 arcmin error box, of GRB 021113 (GCN 1686) with
the 32-inch Tenagra II telescope beginning 2.6 hours after the burst. We
integrated without filter for 1800 seconds per pointing x two pointings.
Visual comparison with the DSS2-Red reveals no obvious counterpart to the
limiting magnitude of the DSS. Future observations are planned.
GCN Circular 1688
Subject
GRB 021113: Optical Observations
Date
2002-11-13T17:58:48Z (23 years ago)
From
Andrew Levan at U.of Leicester <anl@star.le.ac.uk>
A.J. Levan (Leicester), J.J. Kavelaars (HIA/NRC), A.S. Fruchter and
J.E. Rhoads (STScI) report for a larger collabortaion:
The entire HETE-2 error box for GRB 021113 (GCN 1686) was imaged with the
KPNO 4-m telescope and Mosaic imager, beginning on 13th November 10:48
UT (4.17 hours after burst). 2 R-band images were obtained, dithered to
cover chip gaps. The total exposure time was 840 s.
Visual comparison with the DSS-2(R) reveals no obvious new sources.
GCN Circular 1690
Subject
GRB 021113: Optical observations
Date
2002-11-14T15:46:02Z (23 years ago)
From
Vasilij Rumjantsev at CrAO <rum@crao.crimea.ua>
V.Rumyantsev (CrAO) and A.Pozanenko (IKI)
report:
We have observed the field of GRB021113 / HETE2449
with the 0.64-m Richter-Slefogt telescope of Crimean Astrophysical Observatory
(field 53x35 arcminutes) beginning on 13th November 15:50 UT (6.3 hours after the burst).
We do not identify any afterglow candidate on visual
comparison with the DSS2 to a limit approximately V ~ 18.0 mag.
GCN Circular 1692
Subject
IPN triangulation of GRB021113 (=H2449; annulus)
Date
2002-11-14T18:40:49Z (23 years ago)
From
Kevin Hurley at UCBerkeley/SSL <khurley@sunspot.ssl.berkeley.edu>
K. Hurley and T. Cline, on behalf of the Ulysses, Konus, and HETE GRB teams,
E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, and
G. Ricker, J-L Atteia, N. Kawai, D. Lamb, S. Woosley, J. Doty, R.
Vanderspek, J. Villasenor, G. Crew, G. Monnelly, N. Butler, J.G.
Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin, J. Braga, R.
Manchanda, G. Pizzichini, Y. Shirasaki, C. Graziani, M. Matsuoka, T.
Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
T. Tavenner, T. Donaghy, M. Boer, J-F Olive, and J-P Dezalay, on
behalf of the HETE GRB team, report:
Ulysses and Konus-Wind also observed this GRB (HETE 2449, GCN 1686).
We have triangulated it to a preliminary annulus centered at RA, Decl(2000)=
1.104, -35.210 degrees, whose radius is 78.410 +/- 0.078 degrees (3 sigma ).
This intersects the WXM error box given in GCN 1686 at four points, and
reduces its area by about 30%. The intersection points are:
RA(2000) DECL(2000)
1 h 32 m 44.80 s 40 o 26 ' 18.72 "
1 h 33 m 46.40 s 40 o 32 ' 15.63 "
1 h 35 m 00.19 s 40 o 27 ' 32.32 "
1 h 33 m 28.89 s 40 o 23 ' 31.68 "
This annulus can be improved, but as Mars Odyssey was recovering
from safe mode, a small error box cannot be derived for it.
A map will be posted shortly at ssl.berkeley.edu/ipn3/021113.
GCN Circular 1694
Subject
GRB021113: Kiso Observations
Date
2002-11-15T08:13:45Z (23 years ago)
From
Yuji Urata at RIKEN <urata@crab.riken.go.jp>
M. Ishiguro, M. Abe, Y. Sarugaku (ISAS)
W. Tanaka, S. Nishiura, H. Mito, Y. Urata on behalf of the KISO GRB Team:
"We have observed the entire HETE-2 error box of GRB021113
(A. Yoshida et al., GCN1686) with the KISO observatory 1.05m schmidt
telescope starting at Nov 13.607 UT.
Our data;
Date Time (UT) Exposure Limiting mag.(R, SN=3)
11-13 14:34:37 300 s 19.8
11-13 16:02:34 300 s x 2 20.3
# Limiting magnitude was estimated by comparison with
# U1275_00933819 01:34:13.836 +40:30:31.62 17.6mag .
Comparison with DSS II red images, no new object was detected down to
the limiting magnitude."
GCN Circular 1699
Subject
GRB 021113: Evidence for a Dark Optical Afterglow
Date
2002-11-19T18:54:16Z (23 years ago)
From
Melissa Nysewander at UNC,Chapel Hill <mnysewan@astro.unc.edu>
M. Nysewander, D. Reichart (U. North Carolina), and M. Schwartz (Tenagra
Observatories) report on behalf of a larger collaboration:
We observed 100% of the 23 arcmin x 13 arcmin error box, but only 90% of
the revised 26 arcmin x 9 arcmin error box, of GRB 021113 (GCN 1686) with
the 32-inch Tenagra II telescope beginning 2.6 hours (GCN 1687) and 22.3
hours after the burst. For each epoch, we integrated without filter for
1800 seconds per pointing x two pointings under photometric conditions.
Due to more favorable airmasses, the second epoch observations went deeper.
Calibration images of M67 suggest that unfiltered magnitudes measured with
this CCD best mimic R magnitudes (Henden 2000). Using the image
subtraction routine ISIS2 (Alard 2000), we find no transients to the
limiting magnitude of our first epoch image, which we measure to be R =
21.5 mag (5 sigma), 22.1 mag (3 sigma), and 23.2 mag (1 sigma) using the
following three USNO-A2.0 stars:
RA (hrs) DEC (deg) R (mag)
23.353 40.522 13.8
23.425 40.341 13.9
23.342 40.483 16.7
This is the deepest non-detection of an optical afterglow within four
hours of a burst.
Alard, C., 2000, A&AS 114, 363
Henden, A., 2000, JAAVSO 29, 35
GCN Circular 1700
Subject
GRB021113: optical observations at Bisei
Date
2002-11-20T12:29:37Z (23 years ago)
From
Yuji Urata at RIKEN <urata@crab.riken.go.jp>
T. Kawabata, K. Ayani (BAO), H. Yamaoka (Kyushu Univ.), N. Kawai, and Y.
Urata (Titech / RIKEN), report:
"We performed R-band observations of GRB 021113 (Yoshida et al., GCN
1686) field with the Bisei Astronomical Observatory (BAO) 1.01-m
telescope starting at Nov. 13 11:13 UT (4.6 hrs after the burst). The
six-field mosaic images were obtained, which cover about 85% of refined
error box (Hurley et al., GCN 1692) during 11:13-12:39 UT. From 14:05
UT, we imaged eight-field mosaic covering the entire error box. The
limiting magnitudes of the first six and later eight mosaic images based
on USNO-A2.0 red magnitudes were R ~ 17.6 and R ~ 18.1, respectively. No
new object was detected in comparison with DSS II red image."
This message may be cited.
GCN Circular 1703
Subject
GRB021113, SPI ACS observation
Date
2002-11-21T08:52:38Z (23 years ago)
From
Arne Rau at MPI <arau@xray.mpe.mpg.de>
A. Rau, V. Schoenfelder, A.v. Kienlin, G. Lichti G., N. Arend,
on behalf of the MPE INTEGRAL SPI-team;
J.-P. Roques on behalf of the Toulouse INTEGRAL
SPI-team;
J. Borkowski, R. Walter, N. Produit on behalf of the INTEGRAL Science Data
Center (ISDC) Geneve;
K. Hurley on behalf of the IPN team
report:
The Anticoincidence Shield (ACS) of the Spectrometer onboard the
INTEGRAL satellite (SPI) was switched on on the 26th of October 2002.
Since then, besides the major calibration and verification activities,
the ACS rates have already been monitored for GRBs. The ACS has
registered approximately 1 GRB per day, among them also the following
IPN-localized GRBs 021027 (GCN#1658), 021102 (GCN#1667) and 021108
(GCN#1679).
The first HETE-localized GRB detected by SPI ACS was GRB 021113
(=H2449; GCN #1686). The ACS lower energy threshold during this burst was
set to ~100 keV, but this threshold is broad; there exists no high-energy
threshold. GRB 021113 was seen in the total ACS rate (all 91 BGO crystals)
with 4 sigma on a 1s time scale.
The ACS lightcurve of GRB 021113
(http://www.mpe.mpg.de/gamma/instruments/integral/spi/acs/grb/021113_acs.html)
shows a single, smooth peak (similar to the HETE light curve), with a
maximum occuring at 6:38:58 UT. The absolute timing of the ACS is known
int the moment with an accuracy of ~100ms.
Continued "tuning" of the energy threshold and burst verification
algorithm is anticipated over the coming weeks, before the ACS will be
fully implemented into the INTEGRAL Burst Alert System (IBAS).
Acknowledgement is given to INTEGRAL Science Working Team for making these
burst data public.
This message is citable.