GRB 030328
GCN Circular 2192
Subject
GRB030328, optical observation
Date
2003-05-02T01:23:13Z (23 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
M.A. Ibrahimov, I.M. Asfandiyarov, B.B. Kahharov (UBAI), A.Pozanenko (IKI),
V.Rumyantsev (CrAO), G.Beskin (SAO) on behalf of large collaboration
report:
We have observed the OT of GRB030328 (Peterson and Price, GCN 1974) on
Mar.29 with 1.5m telescope of Mt.Maidanak High-altitude Observatory (UBAI).
Using star "A" as a reference (GCN 1975) and photometry by A.Henden (GCN
2114) we estimate the OT magnitudes:
Mid time (UT)
Mar.29 exposure filter mag err
18:00 5x300 B 22.77 0.43
18:48 5x300 R 22.10 0.28
Obtained R-magnitude is consistent with the measurement by P. Garnavich et
al. (GCN 2036).
This message may be cited.
GCN Circular 2114
Subject
GRB030328, UBVRcIc field photometry
Date
2003-04-07T16:18:27Z (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 UBVRcIc all-sky photometry for
a 11x11 arcmin field centered at the coordinates
of the optical transient (Peterson and Price, GCN 1974)
for the HETE burst GRB030328 (GCN 1978)
with the USNOFS 1.0-m telescope on one photometric
night. Stars brighter than V=13.0 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/grb030328.dat
The astrometry in this file is based on linear plate solutions
with respect to UCAC2. The external errors are less than 100mas.
The external photometric errors are approximately 0.03mag
at this stage.
Because of scattering from the two bright stars to the south of the
optical transient, this file has many false stars. You should carefully
match the RA,DEC of any object against USNO-B to ensure that the
object is real.
There is now a README file in that directory that gives
generic observational information and file formats.
We will most likely obtain an additional night of photometry
in a week or two when the moon is no longer a concern.
As always, you should check the dates on the .dat file prior to
final publication to get the latest photometry.
GCN Circular 2103
Subject
GRB030328: R upper limit after 6 hours by MASTER
Date
2003-04-06T19:24:32Z (23 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
V. Lipunov, A. Krylov, V. Kornilov, G. Borisov, A. Belinski,
I. Chilingarian, D. Kuvshinov, M. Kuznetsov, S. Potanin, V. Vitrischak
Sternberg Astronomical Institute, Alexsandr Krylov Observatory, Moscow
report:
We had been observing the OT of GRB030328 (HETE #2650, Peterson and Price,
GCN 1974) from 17:16UT 28/03/2003 (~5h after GRB) to 00:35UT 29/03/2003
(~13h after GRB). Sky conditions were quite poor, because of low position
of the object (25 degrees above the horizont at culmination). We obtained
about 70 one- to 3-minute exposures in R filter. There is no OT on the sum
of exposures for the 1-st hour of observations up to 17.7 R magnitude (3
sigma). There is no OT on the sum of all images up to 18.3 R magnitude (3
sigma).
It agrees with the powerlaw index alpha=-1 (GCN 1977, Peterson and Price).
Summarized images avaliable at:
http://observ.pereplet.ru/images/grb030328_1.gif - 1-st hour sum
http://observ.pereplet.ru/images/grb030328_f.gif - whole sum
This message may be cited.
GCN Circular 2076
Subject
GRB030328: Full Observation, X-ray Fading and Spectrum Measured
Date
2003-04-03T00:22:56Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030328: Full Observation, X-ray Fading and Spectrum Measured with Chandra
N. R. Butler, H. L. Marshall, P. G. Ford, R. K. Vanderspek, G. R.
Ricker (MIT), J. G. Jernigan (U.C. Berkeley), and D. Q. Lamb (U. Chicago)
report:
We have analyzed the full 94.0 ksec (livetime) Chandra LETGS
observation of GRB030328 (Villasenor et al, GCN1978), lasting from
March 29.112 (t[burst] + 15.33 hr) until March 30.278 (t[burst] +
43.32 hr). The mean counting rate for the X-ray afterglow (Butler et
al. GCN2007) is 0.012 counts/s (summed over the dispersed signal from
the LETGS, and including the 0th order flux). We observe that the
brightness over the full observation decays with a slope -1.5 +/-
0.1, consistent with the value reported by Ford et al. (GCN2027).
(The chi^2 is 34.27 for 30 degrees of freedom, and the fit is
rejectable at only 73% confidence.) We see no evidence for a
temporal break. We fit the dispersed LETGS counts (+/-1 orders
summed) and the counts in 0th order jointly by minimizing chi^2,
requiring 12 or more counts per spectral bin. In the 0.5 to 3.0 keV
band, the data are well fit (chi^2/nu=48.45/48, rejectable at 54%
confidence) by an absorbed power-law:
dN/dE = A * E^ (-gamma) * exp(-NH * sigma[E]) ,
where NH = ( 5 +/- 3 ) x 10^20 cm^(-2) is the line of sight column
density, which is consistent with the anticipated galactic absorption
in the source direction; A = ( 6.8 +/- 0.9 ) x 10^(-5) ph cm^(-2)
s^(-1) keV^(-1); and gamma = 1.7 +/- 0.2 . These are 1 parameter
1-sigma confidence intervals.
Integrating the above model over the 0.5 to 3.0 keV band, the mean
flux for the duration of the Chandra observation is ~1.9 x 10^(-13)
ergs cm^(-2) s^(-1).
Our analyses are continuing, and more detailed results will be posted at:
http://space.mit.edu/HETE/
We thank Harvey Tananbaum for his generous allocation of Director's
Discretion Time to this observation, and the Chandra X-ray
Observatory Operations personnel for the impressive promptness with
which this observation was planned and carried out.
The preliminary results reported here may be cited.
GCN Circular 2036
Subject
GRB 030328, optical photometry
Date
2003-03-31T00:49:49Z (23 years ago)
From
Peter Garnavich at U of Notre Dame <pgarnavi@miranda.phys.nd.edu>
P. Garnavich (Notre Dame), P. Martini (OCIW), and K.Z. Stanek (CfA)
We imaged the optical afterglow of GRB 030328 (Peterson & Price,
GCN 1974) with the Magellan 6.5-m Clay telescope and LDSS2
imaging/spectrograph on March 30.04 (1.57 days after the
burst). The 2x180 sec R-band images provide a magnitude
estimate of 21.93 +\- 0.06 assuming star "B" (GCN 1977)
is R=16.10. Using the Magellan photometry from March 29
(Martini et al. GCN 1979), we find a powerlaw decay index of
-1.3 +/- 0.1.
Our R-band magnitude estimate 1.57 days after the burst is close
to that predicted by Price & Peterson (GCN 1977) based
on early photometry and a decay index of -1.0.
This message may be cited.
GCN Circular 2027
Subject
GRB030328: X-ray Fading and Spectrum Measured with Chandra
Date
2003-03-30T18:35:26Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030328: X-ray Fading and Spectrum Measured with Chandra
P. G. Ford, N. R. Butler, H. L. Marshall, R. K. Vanderspek, G. R.
Ricker (MIT), J. G. Jernigan (U.C. Berkeley), and D. Q. Lamb (U. Chicago)
report:
As reported in Butler et al. (GCN 2007), Chandra LETGS observations
commenced on March 29.112 (t[burst] + 15.33 hr) of a field centered
on the HETE WXM+SXC error region (Villasenor et al, GCN 1978) for
GRB030328. We report here on the first 39.7 ksec of data, which was
taken until March 29.744 (t[burst] + 30.51 hr). The relatively faint
X-ray afterglow reported in GCN 2007 is observed to fade in
brightness according to a power-law with a decay slope of -1.5 +/-
0.3. (This value is consistent with the decay slope value of -1.6
found by Andersen et al. (GCN 1993) in the optical.) The mean
counting rate was 0.023 counts/s (summed over the dispersed signal
from the LETGS, and including the 0th order flux). The source
spectrum, which we derive from our preliminary analysis of the
dispersed LETGS counts, is characterized as follows:
nH = 4.32 x 10^20 cm^(-2), fixed at the Galactic value in the source direction;
dN/dE = A * E^ (-gamma) ph cm^(-2) s^(-1) keV^(-1) ,
over the 0.8-2.7 keV range, with A = 0.0001, and gamma = 1.80
Thus, the mean flux for the 0.8 to 2.7 keV band over the duration of
the Chandra observation was ~1.7 x 10^(-13) ergs cm^(-2) s^(-1).
Our analyses are continuing, and more detailed results will be posted at:
http://space.mit.edu/HETE/
We thank Harvey Tananbaum for his generous allocation of Director's
Discretion Time to this observation, and the Chandra X-ray
Observatory Operations personnel for the impressive promptness with
which this observation was planned and carried out.
The preliminary results reported here may be cited.
GCN Circular 2008
Subject
GRB030328: R optical observation
Date
2003-03-30T00:00:55Z (23 years ago)
From
Adriano Guarnieri at O.A.di Bologna <adriano@astbo3.bo.astro.it>
C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University), R. Gualandi
(Bologna Astronomical Observatory), G. Pizzichini (IASF-CNR, Bologna) report:
On 2003, March 28, 22h 32m UT we observed the optical afterglow of GRB 030328
(Peterson and Price, GCN 1974) with the 152 cm telescope in Loiano. Using
the calibration reported by Fugazza et al. (GCN 1982) we obtained R = 20.45
(1800s exposure, preliminary estimate).
This message may be cited.
GCN Circular 2007
Subject
GRB030328: X-ray Afterglow Observed with Chandra
Date
2003-03-29T23:44:47Z (23 years ago)
From
George Ricker at MIT <grr@space.mit.edu>
GRB030328: X-ray Afterglow Observed with Chandra
N. R. Butler, H. L. Marshall, P. G. Ford, R. K. Vanderspek, G. R.
Ricker (MIT), J. G. Jernigan (U.C. Berkeley), and D. Q. Lamb (U. Chicago)
report:
Beginning at March 29.112 (t[burst] + 15.33 hr) Chandra Low Energy
Transmission Grating Spectrometer (LETGS) observations commenced of
a field centered on the HETE WXM+SXC localizations (Villasenor et al,
GCN 1978) of GRB030328. We report here on the first 2.6 ksec of data
downlinked from Chandra. An X-ray source is detected at a location
consistent with that of the optical transient found by Peterson & Price
(GCN1974), and a total of 13 counts are observed in the 0.2-10 keV band in
the 0th order image. Assuming a spectrum with photon index gamma=2 and
attenuated by a Galactic absorption column (nH=4.3 x 10^(20) cm^(-2)),
this corresponds to an average flux of ~3 x 10^(-13) ergs cm^(-2) s^(-1).
Our analyses are continuing, and more detailed results will be posted at:
http://space.mit.edu/HETE/
We thank Harvey Tananbaum for his generous allocation of Director's
Discretion Time to this observation, and the Chandra X-ray
Observatory Operations personnel for the impressive promptness with
which this observation was planned and carried out.
The preliminary results reported here may be cited.
GCN Circular 1993
Subject
GRB 030328 Optical Observations
Date
2003-03-29T17:03:41Z (23 years ago)
From
Jens Hjorth at U.Copenhagen <jens@astro.ku.dk>
M. I. Andersen (Astrophysikalisches Institut Potsdam),
G. Masi (University of Rome "Tor Vergata" and ESO, Chile),
B. L. Jensen and J. Hjorth (University of Copenhagen) report:
We have obtained R-band observations of the optical afterglow of
GRB 030328 (Peterson & Price, GCN 1974), using the Danish 1.54m
telescope (La Silla) + DFOSC. Using the zero point reported by
Fugazza et al. (GCN 1982) (R = 16.31 for star B) a preliminary
analysis gives
Mar. 29, 02:59 UT 20.91 +/- 0.09
Mar. 29, 03:12 UT 20.73 +/- 0.07
Mar. 29, 03:34 UT 21.00 +/- 0.09
Mar. 29, 03:54 UT 20.85 +/- 0.06
Mar. 29, 04:15 UT 21.00 +/- 0.07
Mar. 29, 04:42 UT 20.95 +/- 0.07
Mar. 29, 05:21 UT 21.10 +/- 0.07
Mar. 29, 05:53 UT 21.03 +/- 0.07
Mar. 29, 07:17 UT 21.23 +/- 0.10
Mar. 29, 07:46 UT 21.36 +/- 0.11
A fit to this data set gives a decay index of alpha = 1.6 +/- 0.3. If
the two last data points are ignored and the two data points of Fugazza
et al. are included, a decay index of alpha = 1.2 +/- 0.2 is derived,
consistent with the early decay index of alpha = 1.0 +/- 0.1 reported
by Price & Peterson (GCN 1977). This may indicate that the light curve
steepened around t = 0.8 days.
GCN Circular 1992
Subject
GRB030328: Decay index
Date
2003-03-29T15:48:00Z (23 years ago)
From
Michael I. Andersen at Astrophys.Inst.Potsdam <mandersen@aip.de>
M. I. Andersen (Astrophysikalisches Institut Potsdam)
G. Masi (University of Rome "Tor Vergata" and European Southern Observatory,
Chile), B. L. Jensen and J. Hjorth (Copenhagen University) report:
We have obtained R-band observations of the afterglow of GRB030328,
initially reported by Peterson & Price (GCN 1974), using the Danish 1.54m
telescope (La Silla) + DFOSC. Using the zero point reported by Fugazza et al.
(GCN 1982) (star B=16.31) a preliminary analysis gives
Mar. 29, 02:59 UT 20.91 +/- 0.09
Mar. 29, 03:12 UT 20.73 +/- 0.07
Mar. 29, 03:34 UT 21.00 +/- 0.09
Mar. 29, 03:54 UT 20.85 +/- 0.06
Mar. 29, 04:15 UT 21.00 +/- 0.07
Mar. 29, 04:42 UT 20.95 +/- 0.07
Mar. 29, 05:21 UT 21.10 +/- 0.07
Mar. 29, 05:53 UT 21.03 +/- 0.07
Mar. 29, 07:17 UT 21.23 +/- 0.10
Mar. 29, 07:46 UT 21.36 +/- 0.11
A fit to this data set gives a decay index of alpha = 1.6 +/- 0.3.
If the two last data points are ignored and the two data points
from Fugazza et al. are included, a decay index of alpha = 1.2 +/- 0.2
is derived. This is consistent with the early decay index of
alpha = 1.0 +/- 0.1 reported by Price and Peterson (GCN 1977) and
may indicate that the light curve encountered a break around t=0.8 days.
This message may be cited.
GCN Circular 1991
Subject
GRB 030328: Optical observations
Date
2003-03-29T15:31:57Z (23 years ago)
From
Vasilij Rumjantsev at CrAO <rum@crao.crimea.ua>
V.Rumyantsev (CrAO), V.Biryukov(SAI) and A.Pozanenko (IKI) report:
We have obtained 44 unfiltered exposures (120-s each) of the GRB 030228
error box (HETE Trigger #2650). The images were taken with the AT-64
telescope of Crimean Astrophysical observatory and cover the period
(UT) 18:46 - 23:07 March 28, 2003. We used CCD SBIG ST-8 with
maximum of sensitivity in the red spectral band.
In a co-added image the OT is visible at the position of reported by B.A.
Peterson and P.A. Price (GCN 1974). The brightness was estimated in
respect to the star B (GCN 1982) as R = 20.9 +/- 0.2.
Start time exposure OT
March 28 18:46 44x120 s 20.9 +- 0.2
Detailed calibration is underway.
The image is available at http://grb.rssi.ru/GRB030228
This message can be cited.
GCN Circular 1990
Subject
GRB 030328: optical observations
Date
2003-03-29T15:15:55Z (23 years ago)
From
Denis Denissenko at IKI, Moscow <denis@hea.iki.rssi.ru>
R. Burenin, D. Denissenko, M. Pavlinsky, R. Sunyaev, O. Terekhov, A.
Tkachenko (IKI); Z. Aslan, I. Khamitov, K. Uluc (TUG); U. Kiziloglu, A.
Alpar, A. Baykal (METU); I. Bikmaev, N. Sakhibullin, V. Suleymanov (KSU)
report:
Error box of GRB030328 (HETE Trigger #2650, GCN 1978) was observed with
1.5-m Russian-Turkish Telescope RTT150 at Bakyrlytepe (TUBITAK National
Observatory, Turkey) between Mar. 28.80 and 29.02 UT, starting appr.
9-10 hours after the burst. A set of 300-second exposures in BVRI Bessel
filters was obtained under poor photometric conditions.
We confirm the presence of the optical transient (OT) reported by
Peterson and Price (GCN 1974). R magnitude of the OT on Mar. 28.952
(0.480 day after the burst) is estimated to be 20.35, assuming that Star
B in GCN 1975 is R=16.1. This is brighter than the extrapolation of the
power law from Price and Peterson (GCN 1977).
OT is clearly visible in other filters in every 300-s exposure. The
magnitudes in BVI will be obtained after we calibrate the field.
The R image can be found at: http://hea.iki.rssi.ru/~br/r.gif
Preliminary lightcurve in R: http://hea.iki.rssi.ru/~br/lc_r.ps
This message may be cited.
GCN Circular 1984
Subject
GRB 030328: OT photometry
Date
2003-03-29T12:34:20Z (23 years ago)
From
Avishay Gal-Yam at Tel Aviv U, Israel <avishay@wise1.tau.ac.il>
A. Gal-Yam, E. O. Ofek and D. Polishook (Wise observatory, TAU) report:
We have observed the OT (Peterson & Price 2003, GCN 1974)
of GRB 030328 (Villasenor et al. 2003, GCN 1978) using the Wise observatory 1m
telescope + SITe CCD camera, starting March 28, 21:48 UT (10 hours after
the burst). B, V and R-band frames (300 s each) were obtained under fair
to moderate conditions, but incoming clouds prevented further observations.
We detect the OT on the R-band image, at magnitude about 20.5, roughly
consistent with the predictions of Price (GCN 1977) and the observations
of Fugazza et al. (GCN 1982). Further analysis is underway, and B and
V-band upper limits will be derived once the field is calibrated.
GCN Circular 1983
Subject
GRB030328: optical spectroscopy at TNG
Date
2003-03-29T12:07:20Z (23 years ago)
From
Angelo Antonelli at Obs. Astro. di Roma <angelo@coma.mporzio.astro.it>
D. Fugazza (TNG), F. Fiore, M. Cocchia, L.A. Antonelli (INAF-OAR),
S. Covino (INAF-OAB), E. Pian (INAF-OATs), N. Masetti (CNR-IASF),
A. Buzzoni, G. Tessicini (TNG), on behalf of a larger collaboration,
report:
"Starting on March 29 2002 00:28 UT we have obtained low resolution
(R~1000) spectra of the optical afterglow of GRB030328 (Peterson &
Price GCN #1974) using DOLORES at TNG. Observations consisted of four
exposures, for a total of 2 hours, and cover the full spectral range
3800-8000 Angstrom, in good seeing conditions (between 1" and 1.5").
At the time of the observations the afterglow magnitude was R~20.7
(Fugazza et al. GCN #1982).
A preliminary analysis of the spectra reveals several absorption lines
associated with the z=1.52 system reported by Martini et al. (GCN
#1980), in particular MgII2803, MgII2796, FeII2600 and FeII2382.
Other narrow absorption lines are present in the spectra, but
a more detailed analysis is needed to their identification.
We are particularly grateful to the TNG staff for their remarkable
support to these observations."
This message is citeable.
GCN Circular 1982
Subject
GRB030328: optical photometry at the TNG
Date
2003-03-29T11:51:16Z (23 years ago)
From
Angelo Antonelli at Obs. Astro. di Roma <angelo@coma.mporzio.astro.it>
D. Fugazza (TNG), L.A. Antonelli, F. Fiore,(INAF-OAR), S. Covino,
G. Ghisellini (INAF-OAB), E. Pian (INAF-OAT), N. Masetti (CNR-IASF),
A. Buzzoni, Tessicini (TNG) on behalf of a larger collaboration, report:
"On March 29 2003 we have obtained R band photometry of the optical
afterglow of GRB030328 (Peterson & Price GCN #1974) using DOLORES at
TNG. Observations were performed under moderate seeing conditions
(between 1" and 1.5").
A preliminary analysis of the images allowed us to derive the following
photometry for the OT calibrated by means of a Landolt standard field:
20.59 +/- 0.07 at UT 00:10:14, 12.82 hours after the burst
20.79 +/- 0.08 at UT 02:34:41, 15.23 hours after the burst
The photometry for the star "B" reported in GCN #1977 (Price and Peterson)
turns out to be:
16.31 +/- 0.06
We are particularly grateful to the TNG staff for their remarkable support to
these observations."
This message is citeable.
GCN Circular 1981
Subject
VLT spectra of GRB 030328
Date
2003-03-29T08:29:12Z (23 years ago)
From
Paul Vreeswijk at ESO <pvreeswi@eso.org>
Evert Rol (U. of Amsterdam), Paul Vreeswijk & Andreas Jaunsen (ESO)
report for the GRACE collaboration:
The optical afterglow, discovered by Peterson & Price (GCN 1974), of
GRB 030328 (HETE trigger 2650, see GCN 1978), was observed around
March 29.08 UT with FORS1 at telescope unit 1 of the VLT. A total of
one hour of spectra were taken with the grism 300V and a slit width of
1 arcsecond, at a position angle of 104 degrees to also include object
B of Price & Peterson (GCN 1975) in the slit.
A preliminary reduction shows significant absorption lines, most of
which we identify with typical metal lines at a redshift of z=1.520.
We also find some hints for another system at z=1.29, but an improved
analysis is needed to confirm this.
We are thankful for the assistance of the ESO staff at Paranal; in
particular that of Andreas Kaufer.
GCN Circular 1980
Subject
GRB 030328, optical spectroscopy
Date
2003-03-29T08:13:10Z (23 years ago)
From
Peter Garnavich at U of Notre Dame <pgarnavi@miranda.phys.nd.edu>
P. Martini (OCIW), P. Garnavich (Notre Dame) and K.Z. Stanek (CfA)
Spectra of the optical afterglow of GRB 030328 (Peterson & Price,
GCN 1974) were obtained with the Magellan 6.5-m Clay telescope and
LDSS2 imaging/spectrograph starting at March 29.19 (UT). The
five spectra cover the wavelength range of 4000 to 9000 Ang.
with a resolution of 13 Ang. FWHM. Preliminary reduction of
the images reveals narrow absorption features which we identify
with a single absorption system at z=1.52:
observed (Ang) ID z
7069.6 MgII 2802.7 1.522
7049.2 MgII 2795.5 1.522
6554.6 FeII 2599.4 1.522
6005.7 FeII 2382.0 1.521
5987.6 FeII 2373.7 1.522
4207.9 AlII 1670.8 1.518
This suggests that the redshift of the GRB is at least z=1.52.
This message may be cited.
GCN Circular 1979
Subject
GRB 030328, optical observations
Date
2003-03-29T06:16:34Z (23 years ago)
From
Peter Garnavich at U of Notre Dame <pgarnavi@miranda.phys.nd.edu>
P. Martini (OCIW), P. Garnavich (Notre Dame) and K.Z. Stanek (CfA)
We imaged the optical afterglow of GRB 030328 (Peterson & Price,
GCN 1974) with the Magellan 6.5-m Clay telescope and LDSS2
imaging/spectrograph on March 29.181 (0.708 days after the
burst). The R-band magnitude is estimated to be 20.8
assuming star "B" (GCN 1977) is R=16.1. This is slightly
brighter than the extrapolation of a powerlaw with alpha=1.0
found by Price & Peterson (GCN 1977).
This message may be cited.
GCN Circular 1978
Subject
GRB030328 (=H2650): A Long, Bright GRB Localized by the HETE WXM and SXC
Date
2003-03-28T20:31:07Z (23 years ago)
From
Don Lamb at U.Chicago <lamb@oddjob.uchicago.edu>
J. Villasenor, G. Crew, R. Vanderspek, J. Doty, G. Monnelly, N. Butler,
T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G. Prigozhin,
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;
T. Donaghy, M. Suzuki, Y. Shirasaki, C. Graziani, M. Matsuoka, T.
Tamagawa, K. Torii, T. Sakamoto, A. Yoshida, E. Fenimore, M. Galassi,
T. Tavenner, Y. Nakagawa, D. Takahashi, R. Satoh, and Y. Urata, on
behalf of the HETE WXM Team;
M. Boer, J-F Olive, J-P Dezalay, C. Barraud and K. Hurley on behalf
of the HETE FREGATE Team;
write:
At 11:20:58.34 UTC (40858.34 s UT) on 28 Mar 2003, the HETE FREGATE,
WXM, and SXC instruments detected event H2650, a long, bright GRB.
The burst triggered FREGATE in the 8-80 keV energy band; the flight
software incorrectly attributed the burst to particles, and therefore
the WXM and SXC flight localizations were not sent out. The operations
team quickly validated the SXC flight localization and disseminated it
in a GCN Notice at 12:14:13 UT, 53 minutes after the burst. The SXC
flight localization SNR was 6. The SXC flight localization can be
expressed as a 90% confidence circle that is 2 arcminutes in radius and
is centered at
SXC-Flight: RA = +12h 10m 46s, Dec = -09d 22' 29" (J2000).
Ground analysis of the WXM data and the SXC data for the burst produced
refined WXM and SXC localizations, which were reported in a GCN Notice
at 13:21:46 UT, 121 minutes after the burst. The WXM ground
localization SNR was 25. The WXM location can be expressed as a 90%
confidence circle that is 4.6 arcminutes in radius and is centered at
WXM-Ground: RA = +12h 10m 53s, Dec = -09d 23' 30" (J2000).
The SXC ground localization SNR was 10. The SXC ground localization
can be expressed as a 90% confidence circle that is 52 arcseconds in
radius and is centered at
SXC-Ground: RA = +12h 10m 51s, Dec = -09d 21' 05" (J2000).
The burst duration t_90 in the 30-400 keV band was ~ 100 s. The fluence
of the burst was 3.0 x 10-5 ergs cm-2 and the peak flux over 5.2 s was
7.3 x 10-7 ergs cm-2 s-1 in the same energy band.
A light curve and skymap for GRB030328 is provided at the following URL:
http://space.mit.edu/HETE/Bursts/GRB030328
GCN Circular 1977
Subject
GRB 030328: Optical observations
Date
2003-03-28T16:37:09Z (23 years ago)
From
Paul Price at RSAA, ANU <pap@mso.anu.edu.au>
P.A. Price and B.A. Peterson (RSAA, ANU) report:
We have observed the afterglow of GRB 030328 with the 40-inch telescope at
Siding Spring Observatory + Wide-Field Imager in R-band. From two
un-flattened frames taken at Mar 28.54 and 28.63, we derive a power-law
decay:
R/mag ~ 21.5 + 2.6 log(t/days)
based on assuming that the star at J2000 coordinates 12:10:50.7 -9:21:00
(Star B in GCN #1975) is R ~ 16.1 (as in USNO A2.0).
The corresponding decay index is alpha = 1.0 +/- 0.1.
This message may be cited.
GCN Circular 1976
Subject
Re: GRB 030328: Finding chart
Date
2003-03-28T14:36:28Z (23 years ago)
From
Paul Price at RSAA, ANU <pap@mso.anu.edu.au>
P.A. Price (RSAA, ANU) reports:
The offset from Star B is 34.04" W, 8.50" N (*not* S).
My apologies for this typo.
GCN Circular 1975
Subject
GRB 030328: Finding chart
Date
2003-03-28T14:20:28Z (23 years ago)
From
Paul Price at RSAA, ANU <pap@mso.anu.edu.au>
P.A. Price and B.A. Peterson (RSAA, ANU) report:
A finding chart for the optical afterglow candidate (GCN #1974) is
available from:
http://www.mso.anu.edu.au/~pap/grb030328finder.ps
The following offsets may be useful for spectroscopy:
Star RA (2000) Dec (2000)
A 12:10:53.8 -9:19:22.9
B 12:10:50.7 -9:20:59.8
A -> OT: 79.92" W, 88.40" S (PA -137.883 degrees)
B -> OT: 34.04" W, 8.50" S (PA -75.981 degrees)
This message may be cited.
GCN Circular 1974
Subject
GRB 030328: Optical afterglow candidate
Date
2003-03-28T13:53:06Z (23 years ago)
From
Paul Price at RSAA, ANU <pap@mso.anu.edu.au>
B.A. Peterson and P.A. Price (RSAA, ANU) report:
We have observed the error box of GRB 030328 (HETE #2650) with the SSO
40-inch telescope + WFI in B and R filters at Mar 28 12:37 UT. We
identify a source not present on the DSS 2 red plate. The coordinates of
this source are:
RA: 12:10:48.4 Dec: -9:20:51.3 (J2000)
with an error of 0.4 arcsec in each coordinate. At this stage, we
estimate that the afterglow candidate is roughly 18th magnitude.
Further observations are planned, and a finding chart will follow.
This message may be cited.