GRB 030528
GCN Circular 2279
Subject
GRB030528(=H2724): X-ray Afterglow Identified in Second Epoch
Date
2003-06-10T12:30:19Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030528(=H2724): X-ray Afterglow Identified in Second Epoch
Observations with the Chandra X-ray Observatory
N. Butler, A. Dullighan, P. Ford, G. Ricker, R. Vanderspek (MIT); K.
Hurley , G. Jernigan (U.C.- Berkeley); and D. Lamb (U.Chicago)
on behalf of the Chandra GRB ToO Team and the HETE Science Team
write:
From 9 June 8:14 UT to 9 June 14:19 UT, the Chandra Observatory
targeted the field of the X-ray rich GRB030528, which was localized
by the HETE satellite (Atteia et al. GCN2256; Villasenor et al.
GCN2261). The 20 ksec second epoch (E2) observation with ACIS-S3 was
a follow up to the 25 ksec first epoch (E1) observation performed
with ACIS-S3 on 3 June (Butler et al. GCN 2269).
Of the 4 sources reported in GCN2269 lying within the revised SXC
error region (Villasenor et al. GCN2261) and the 7 sources lying
beyond this error region but inside the ACIS-S3 field-of-view, only
one source declined in brightness with a significance greater than 2
sigma:
# Chandra Name RA DEC E1 Cnts E2 Cnts
1 CXOU J170400.3-223710 17 4 0.31 -22 37 9.99 39 8
Thus, Chandra Source #1 faded by a factor of about 4 between our two
observations (level of significance of approximately 4 sigma; the
implied power law decay index is 2.0 +/- 0.8). Hence, we are quite
confident that Chandra Source #1 is indeed the X-ray afterglow of
GRB030528. Based on the coincidence in position and moderate early
fading in Ks reported by Greiner et al. (GCN 2271) and the faint
lower limit on Ks reported by Bogosavljevic et al. (GCN 2275),
Chandra Source #1 appears to be associated with the NIR candidate
first reported in GCN 2271.
In view of the imminent possibility of a "supernova bump" becoming
visible from GRB030528, we urge continued deep optical and IR
monitoring of Chandra Source #1.
This message may be cited.
GCN Circular 2275
Subject
GRB 030528: Infrared Observations and the Proposed IR Counterpart
Date
2003-06-06T23:49:59Z (23 years ago)
From
George Djorgovski at Caltech/Palomar <george@astro.caltech.edu>
GRB 030528: Infrared Observations and the Proposed IR Counterpart
M. Bogosavljevic, A. Mahabal, and S. G. Djorgovski (Caltech),
report on behalf of the Caltech-NRAO-CARA GRB collaboration:
On June 3, 2003, 08:30 UT we observed the field of the tentative
near-IR afterglow of GRB 030528 (Greiner et al, GCN 2271), using
the WIRC camera at the Palomar 200-inch Hale telescope. A total
of 30 min on-source exposure was obtained in the Ks band. The
average seeing was ~1.0".
The proposed afterglow of GRB 030528, Chandra source #1
(CXOU J170400.3-223710, Butler et al., GCN 2269) is not detected
down to our 3-sigma detection limit of Ks~19.5, indicating a
continued fading (see Greiner et al, GCN 2271), and strengthening
its interpretation as the afterglow of GRB 030528.
Our 8x8 arcmin FOV also covers Chandra sources #4, #9, #10, all
of which are within the SXC revised error region. All three are
detected. IR images and magnitude estimates will be placed at:
http://www.astro.caltech.edu/~milan/GRB030528/
The field also includes Chandra sources #3, #5, #8, #14, #15 and
#17, from the additional list outside the SXC error region
(Butler et al., GCN 2269 and ref. therein).
This message can be cited.
GCN Circular 2273
Subject
GRB 030528: Optical Observations
Date
2003-06-06T17:36:24Z (23 years ago)
From
Nestor Mirabal at Columbia U. <abulafia@astro.columbia.edu>
N. Mirabal & J. P. Halpern (Columbia U.) report on
behalf of the MDM Observatory GRB follow-up team:
"We obtained I-band images on the MDM 1.3m for 1.5 hours
on June 5.28, covering the positions of most of the Chandra
X-ray sources listed by Butler et al. (GCN 2269).
We detect optical counterparts of three of the four
sources within the revised SXC region reported by Villasenor
et al. (GCN 2261). The source CXOU J170400.3-223710,
tentatively proposed as the GRB afterglow by Greiner et al.
(GCN 2271), is not detected in any of our images to a preliminary
limiting magnitude I > 21.5. Comparison with prior observations
and deeper optical images of this location would be useful."
This message may be cited.
GCN Circular 2271
Subject
GRB 030528: tentative NIR counterpart
Date
2003-06-05T15:21:43Z (23 years ago)
From
Jochen Greiner at MPI <jcg@mpe.mpg.de>
J. Greiner, A. Rau (both MPE Garching) and S. Klose
(Thueringer Landessternwarte Tautenburg) report for the GRACE collaboration:
We have observed the original, 2 arcmin radius error box of GRB 030528
(=H2724) (Atteia et al, GCN 2256) with the near-infrared camera SOFI
at the NTT (La Silla, ESO) on three epochs as given below:
Date (Start UT) Filters Exposure time Seeing
-------------------------------------------------------
2003-05-29 04:58 JHKs 15 min each 0.6"
2003-05-30 04:54 JHKs 20 min each 1.0"
2003-06-01 04:07 Ks 60 min 0.7"
The Chandra sources #1 and #10 (Butler et al., GCN 2269) are within
our field of view, the other two Chandra sources from within the
shifted GRB location (Villasenor et al, GCN 2261) are outside our
images. Comparing the Ks band images of the first and third epoch
reveals a counterpart for each of the two Chandra sources. One of
these two sources, i.e. #1 = CXOU J170400.3-223710 shows a fading
by about 0.9 mag. The other of these two Chandra sources,
#10 = CXOU J170354.0-223654 is about 4 magnitudes brighter in Ks, and
constant to within 0.1 mag (provisional photometric calibration was
done against the 2MASS catalog, taken from the NASA/ IPAC Infrared
Science Archive).
We therefore propose Chandra source #1 = CXOU J170400.3-223710 and
its near-infrared counterpart as the tentative afterglow of GRB 030528.
K band images of two epochs for this source will be displayed at
http://www.mpe.mpg.de/~jcg/grb030528.html
Since we are missing two of the Chandra sources due to the shift of the
GRB location, only a second Chandra observation can (dis)prove this
tentative counterpart. We note, that the proposed counterpart is
the brightest X-ray source in the previous Chandra image, so a second
Chandra observation of the same exposure time can already be decisive.
GCN Circular 2270
Subject
GRB 030528, radio observations
Date
2003-06-04T15:41:50Z (23 years ago)
From
Dale A. Frail at NRAO <dfrail@nrao.edu>
D. A. Frail (NRAO) and E. Berger (Caltech) report on behalf of a
larger collaboration:
"On 2003 June 3.32 UT we used the VLA to image the 2.5-arcmin error
circle of the HETE SXC of GRB 030528 (GCN#2261). A 15-minute
integration was taken at a frequency of 8.46 GHz with the VLA in the
A-array configuration, producing a synthesized beam of 0.5" x 0.25".
There are no sources in the SXC error circle above a level of 350 uJy
(about 5-sigma). We have made a deeper search in the vicinity of the
four Chandra X-ray sources (GCN#2269) but we find no significant
(>3-sigma) detections."
This message may be cited.
GCN Circular 2269
Subject
GRB030528(=H2724): Observations with the Chandra X-ray Observatory
Date
2003-06-04T14:56:11Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030528(=H2724): Observations with the Chandra X-ray Observatory
N. Butler, A. Dullighan, P. Ford, G. Ricker, R. Vanderspek (MIT);
K. Hurley , G. Jernigan (U.C.- Berkeley); and D. Lamb (U.Chicago)
on behalf of the Chandra GRB ToO Team and the HETE Science Team
write:
On 3 June, the Chandra Observatory targeted the field of GRB030528,
which was localized by the HETE satellite (Atteia et al, GCN2256).
The 25 ksec observation spanned the interval 12:22-20:08 UT, 5.97 -
6.29 days after the burst. The revised SXC error region from
Villasenor et al. (GCN2261) was completely contained within the
field-of-view of the Chandra ACIS-S3 chip (see planning comments in
Ricker et al. GCN2264).
Within the revised SXC error region, we detected four sources in the
0.5-8 keV band:
# Chandra Name RA DEC dR(s) dD(") Cts
1 CXOU J170400.3-223710 17 4 0.31 -22 37 9.99 0.053 0.91 39
4 CXOU J170348.4-223826 17 3 48.39 -22 38 25.93 0.054 0.92 30
9 CXOU J170400.1-223548 17 4 0.11 -22 35 48.10 0.053 0.92 11
10 CXOU J170354.0-223654 17 3 53.95 -22 36 53.67 0.054 0.93 9
The # column refers to the source's relative ranking (in terms of
total counts) among all the sources detected in the entire ACIS-S3
field-of-view. For completeness, we tabulate below seven additional
sources that are within the ACIS-S3 field-of-view but are outside the
revised SXC error region:
# Chandra Name RA DEC dR(s) dD(") Cts
2 CXOU J170358.7-224237 17 3 58.67 -22 42 36.67 0.063 0.94 31
3 CXOU J170355.7-223503 17 3 55.73 -22 35 2.66 0.053 0.92 23
5 CXOU J170342.8-223548 17 3 42.81 -22 35 48.19 0.053 0.92 24
8 CXOU J170403.9-223543 17 4 3.87 -22 35 43.30 0.053 0.92 13
14 CXOU J170341.4-223646 17 3 41.44 -22 36 46.07 0.053 0.95 6
15 CXOU J170411.2-224032 17 4 11.24 -22 40 32.01 0.055 0.96 11
17 CXOU J170345.8-224133 17 3 45.81 -22 41 32.71 0.060 1.00 10
The astrometry was calibrated using six stars with detectable X-ray
emission from the list generated by A. Henden (GCN2267) that lay
within the ACIS-S3 field-of-view.
In the above 2 tables, dR, the uncertainty in RA, and dD, the
uncertainty in DEC, were established by summing the following in
quadrature for each coordinate: the X-ray centroiding error, the
correlation error between the X-ray and optical positions, and the
error estimates from the reference stars.
We gratefully acknowledge the timely assistance of the personnel at
the Chandra Science Center in the acquisition and preliminary
processing of these data.
This message may be cited.
GCN Circular 2267
Subject
GRB030528, BVRI field photometry
Date
2003-06-03T22:38:31Z (23 years ago)
From
Arne A. Henden at USNO/USRA <aah@nofs.navy.mil>
A. Henden (USRA/USNO) reports on behalf of the USNO GRB team:
We have acquired BVRcIc all-sky photometry for
a 11x11 arcmin field centered at the coordinates
of the SXC error box for the HETE burst GRB030528 (Villasenor
et al., GCN 2261) with the USNOFS 1.0-m telescope on one
photometric night. Stars brighter than V=13.5 are saturated and
should be used with care. We have placed the photometric data
on our anonymous ftp site:
ftp://ftp.nofs.navy.mil/pub/outgoing/aah/grb/grb030528.dat
The astrometry in this file is based on linear plate solutions
with respect to UCAC2. The external errors are less than 100mas.
However, due to the crowding in this galactic field, only
isolated stars will have decent astrometry or photometry.
As always, you should check the dates on the .dat file prior to
final publication to get the latest photometry. We anticipate
one more night of photometry to be acquired during this week.
GCN Circular 2264
Subject
GRB030528: Chandra TOO Planned
Date
2003-06-02T00:45:42Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030528: Planned Target of Opportunity Observations with Chandra
X-ray Observatory
G. Ricker, P. Ford, N. Butler, R. Vanderspek, J. Villasenor (MIT), D.
Lamb (U. Chicago), and J.G. Jernigan (UCB), on behalf of a Chandra
GRB ToO Team,
write:
Chandra target-of-opportunity observations of the HETE SXC error
circle for GRB030528 (=H2724: Atteia et al, GCN 2256; Villasenor et
al, GCN 2261) are currently planned. The region to be imaged with
ACIS will extend +/- 4 arcmin about the revised location reported by
Villasenor et al (GCN2261). The first epoch observation should take
place near 3-4 June, with a second epoch observation ~1 week later.
The scheduling of contemporaneous observations at other wavelengths
is strongly encouraged.
GCN Circular 2261
Subject
GRB030528(=H2724): Revised SXC Localization
Date
2003-05-31T23:04:24Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030528(=H2724): Revised SXC Localization
J. Villasenor, N. Butler, G. Crew, J. Doty, G. Prigozhin, R.
Vanderspek, T. Cline, J. G. Jernigan, A. Levine, F. Martel, E.
Morgan, G. Monnelly, G. Azzibrouck, J. Braga, R. Manchanda, and G.
Pizzichini, on behalf of the HETE Operations and HETE Optical-SXC
Teams;
G. Ricker, J-L Atteia, N. Kawai, D. Lamb, and S. Woosley on behalf of
the HETE Science Team;
C. Barraud, M. Boer, J-F Olive, J-P Dezalay, and K. Hurley on behalf
of the HETE FREGATE Team;
K. Torii, C. Graziani, Y. Shirasaki, T. Donaghy, M. Matsuoka, M.
Suzuki, T. Tamagawa, T. Sakamoto, A. Yoshida, E. Fenimore, M.
Galassi, Y. Nakagawa, R. Satoh, Y. Urata, T. Yamazaki and Y.
Yamamoto, on behalf of the HETE WXM Team;
write:
Further analysis of the spacecraft aspect data near the time of
GRB030528 indicates that an additional systematic correction to the
HETE SXC localization reported in GCN2256 (Atteia et al) is required.
This analysis uses the known position of Sco X-1, which was within
the SXC field-of-view at the time of GRB030528. We conclude that a
best estimate location for GRB030528 is:
RA (J2000) = 17h 03m 58s, Dec (J2000) = -22d 38m 00s
with an error radius of 2.5 arcminutes. This revised location is
displaced by 1.3 arcmin from the one reported in GCN2256.
This message may be cited.
GCN Circular 2258
Subject
GRB 030528, Teramo optical observation
Date
2003-05-29T15:49:05Z (23 years ago)
From
Eliana Palazzi at IASF/CNR,Bologna <palazzi@bo.iasf.cnr.it>
G. Valentini, G. Alleva, E. Brocato (INAF-OACT), E. Palazzi (IASF/CNR,
Bologna) report:
"Three unfiltered optical images of error box of the GRB030528 (GCN
2256) were acquired starting on 2003 May 29.04, with the 0.72-m TNT
telescope of the Astronomical Observatory of Collurania - Teramo (Italy),
for a total exposure time of 2200 seconds.
The average seeing was 4.5 arcsec.
No new or noticeable object down to a magnitude of about 20.5 is detected
inside the error circle when we compare our summed frame with the DSS-II
Digital Sky Survey.
This message is citeable."
GCN Circular 2257
Subject
GRB 030528 Bisei optical observation
Date
2003-05-29T13:11:57Z (23 years ago)
From
Hitoshi Yamaoka at Kyushu U., VSNET-GRB collab. <yamaoka@rc.kyushu-u.ac.jp>
K. Ayani (Bisei Astronomical Observatory) and H. Yamaoka (Kyushu
Univ.) report:
"R-filtered CCD images of the field of GRB 030528 (GCN 2256) were
taken with a 1.01-m telescope at Bisei Astronomical Observatory.
The Stacked image of 5 exposures (60 seconds each) taken on
15:22-15:28 UT (139 - 145 minutes after burst) fully contains the SXC
error circle (GCN 2256). Visual examination with DSS red image
revealed no new object down to R ~ 18.7 (based on GSC-2.2 F
magnitudes) within the error circle.
This message can be cited.
GCN Circular 2256
Subject
GRB030528 (H2724): A long GRB localized by HETE
Date
2003-05-29T02:14:54Z (23 years ago)
From
Roland Vanderspek at MIT <roland@space.mit.edu>
J-L Atteia, N. Kawai, D. Lamb, G. Ricker, and S. Woosley on behalf of
the HETE Science Team;
C. Barraud, M. Boer, J-F Olive, J-P Dezalay, and K. Hurley on behalf of
the HETE FREGATE Team;
N. Butler, G. Crew, J. Doty, G. Prigozhin, R. Vanderspek, J. Villasenor,
T. Cline, J. G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Monnelly,
G. Azzibrouck, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of
the HETE Operations and HETE Optical-SXC Teams;
K. Torii, C. Graziani, Y. Shirasaki, T. Donaghy, M. Matsuoka, M. Suzuki,
T. Tamagawa, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
T. Tavenner, Y. Nakagawa, R. Satoh, Y. Urata, T. Yamazaki and
Y. Yamamoto, on behalf of the HETE WXM Team;
At 13:03:02.83 UTC (46982.83 UT) on 28 May 2003, the HETE FREGATE, SXC,
and WXM instruments detected event H2724, a long GRB.
The burst triggered FREGATE in the 30-400 keV energy band. The WXM
flight software detected the GRB and calculated a location, which was
reported in a GCN Notice at 13:03:40, 37 seconds after the beginning of
the burst and while the burst was still in progress. The flight
localization was strong in the X detector, but weak in the Y detector:
the low S/N in the Y localization resulted in a reported error circle
of 30' radius.
Ground analysis of the SXC data produced a refined location which was
reported in a GCN Notice at 14:50:02, 107 minutes after the beginning of
the burst. The SXC localization SNR was 5. The SXC localization may be
expressed as a 90% confidence circle that is 2 arcminutes in radius and is
centered at:
R.A. = 17h 04m 02s, Dec. = -22d 38' 59" (J2000).
The fluence of the burst was 4.3 x 10^-6 erg cm^-2 in the 7-30 keV energy
band, and 4.8 x 10^-6 erg cm^-2 in the 30-400 keV energy band. The peak
flux over 1 s is 1.1 x 10^-7 erg/cm2/s in the 7-30 keV band, and
4.9 x 10^-8 erg/cm2/s in the 30-400 keV band.
The T90 duration of the burst in the 30-400 keV energy band was 21.6 seconds;
in the 7-30 keV band, T90 was > 60s.
A light curve and a skymap for GRB030528 are available at the following URL:
http://space.mit.edu/HETE/Bursts/GRB030528
GCN Circular 2253
Subject
GRB 030528: Optical observations at RIKEN
Date
2003-05-28T18:12:52Z (23 years ago)
From
Ken ichi Torii at RIKEN <torii@crab.riken.go.jp>
K. Torii (RIKEN) reports:
The entire SXC error region of GRB 030528 (HETE trigger 2724,
Sequence number 6) was observed by the automated system at
RIKEN. Observations with 0.20-m telescope (f/4.0, equipped with
unfiltered AP7p) and 0.25-m telescope (f/6.8, equipped with unfiltered
AP6E) started at 13:04:48 UT and 13:05:31 UT on 2003 May 28,
respectively.
Preliminary inspection of the first frame from the 0.25-m telescope
(60-s integration) does not show an optical transient candidate
brighter than about 15.8 mag (USNO-A2.0 red magnitude). Further
analysis and observation are in progress.
GCN Circular 2252
Subject
GRB 030528 (=H2724) Kyoto optical observation
Date
2003-05-28T16:20:47Z (23 years ago)
From
Hitoshi Yamaoka at Kyushu U., VSNET-GRB collab. <yamaoka@rc.kyushu-u.ac.jp>
M. Uemura, R. Ishioka, T. Kato, (Kyoto U) and H. Yamaoka (Kyushu U)
report:
"We have been performing the unfiltered CCD imaging of the field of
GRB 030528 (=H2724) with a 25-cm telescope at Kyoto University,
starting at 13:07:15 UT (252 seconds after burst). The first five
images (30 seconds exposure each) fully covered the SXC error circle
(Seq_Num 6). The visual comparison with the DSS 2 red image revealed
no new source up to 16.0 mag (based on USNO-A2.0 red magnitudes) on
each image. Further observation and analysis is underway.
This message can be cited."