GRB 020305
GCN Circular 1261
Subject
GRB 020305: Optical observations
Date
2002-03-06T12:57:59Z (23 years ago)
From
Paul Price at RSAA, ANU at CIT <pap@srl.caltech.edu>
P.A. Price and D.W. Fox (Caltech) with S. Pravdo, E. Helin,
K. Lawrence, and M. Hicks of the NEAT/Palomar team report on
behalf of the REACT GRB collaboration:
We have observed the error box of GRB 020305 / HETE #1939 with the
Palomar 48-inch telescope + unfiltered CCD at two epochs. Exposures
consisted of 6x120 sec at 2002 March 6.33 UT and 3x120 sec at March
6.47 UT (20 and 23.5 hours after the GRB respectively) each of which
covered the entire error box to approximately the plate limit of the
DSS (R ~ 20 mag). Apart from identifying several asteroids, we do not
detect any variable object within the error box upon manual inspection
of the subtracted images.
Further observations are planned.
This message may be cited.
GCN Circular 1262
Subject
GRB020305 (=H1939): Localization of a GRB by HETE
Date
2002-03-06T18:45:56Z (23 years ago)
From
Don Lamb at U.Chicago <lamb@oddjob.uchicago.edu>
GRB020305 (=H1939): Localization of a GRB by HETE
G. Ricker, J-L Atteia, N. Kawai, D. Lamb, and S. Woosley on behalf of
the HETE Science Team;
J. Villasenor, R. Vanderspek, G. Crew, J. Doty, G. Monnelly, N. Butler,
T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G.
Prigozhin, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of
the HETE Operations and HETE Optical-SXC Teams;
M. Matsuoka, Y. Shirasaki, T. Tamagawa, K. Torii, T. Sakamoto,
A. Yoshida, E. Fenimore, M. Galassi, T. Tavenner, T. Donaghy, and
C. Graziani, on behalf of the HETE WXM Team;
M. Boer, J-F Olive, J-P Dezalay, P. Lestrade, and K. Hurley on behalf
of the HETE FREGATE Team;
write:
At 11:55:25.05 UTC (42925.05 s UT) on 5 March 2002, the HETE FREGATE
and WXM instruments detected a GRB. The burst, H1939, was promptly
reported as a GCN Alert Notice within 42 seconds of the detection time.
The main part of the burst began at 11:59:04 UTC (43144 s UT), just as
the spacecraft reached the dawn terminator and the WXM high voltage was
turning off. Accurate aspect was derived for H1939 from a full data
set on the ground. Ground analysis produced a location which can be
expressed as a circle with a 90% confidence radius of 25 arcminutes
centered at
RA = +12h 43m 03s, Dec = -14d 33' 06" (J2000)
This location was reported in a GCN Alert Notice (issued at 5 Mar 2002
21:51:55 UT)
GRB020305 (=H1939) has a duration in the FREGATE 32-400 keV band of
T90 = 252 seconds. In the 8-40 keV FREGATE band, the peak flux in 3 s
was approximately 7 x 10-8 ergs cm-2 s-1 (i.e., approximately
2.5 x Crab flux). No duration or peak flux can be derived in the
2-25 keV WXM band because only the first 12 seconds of the main (second)
peak were observed by the WXM before high voltage turnoff. The
statistical significance of the burst in the 2-25 keV WXM band in this
12-second interval was 5 sigma.
Further information (including light curves) on GRB020305 is provided at
the following URL:
http://space.mit.edu/HETE/Bursts/
This message is citable.
GCN Circular 1263
Subject
IPN triangulation of GRB020305 (HETE 1939)
Date
2002-03-06T19:01:57Z (23 years ago)
From
Kevin Hurley at UCBerkeley/SSL <khurley@sunspot.ssl.berkeley.edu>
K. Hurley and T. Cline, on behalf of the Ulysses and HETE
GRB teams;
G. Ricker, D. Lamb, and S. Woosley on behalf of the HETE Science Team;
R. Vanderspek, G. Crew, J. Doty, G. Monnelly, J. Villasenor, N.
Butler, T. Cline, J.G. Jernigan, A. Levine, F. Martel, E. Morgan, G.
Prigozhin, J. Braga, R. Manchanda, and G. Pizzichini, on behalf of
the HETE Operations and HETE Optical-SXC Teams;
N. Kawai, M. Matsuoka, Y. Shirasaki, T. Tamagawa, K. Torii, T.
Sakamoto, A. Yoshida, E. Fenimore, M. Galassi, T. Donaghy, C. Graziani,
and T. Tavenner, on behalf of the HETE WXM Team;
J-L Atteia, M. Boer, J-F Olive, P. Lestrade, and J-P Dezalay, on behalf
of the HETE FREGATE Team;
report:
Ulysses observed GRB020305 (=H1939). As observed by both Ulysses and
FREGATE, this event consists of two distinct episodes of emission
separated by an ~ 200 s long quiescent period, raising the question of
whether both episodes are from the same source. As the Ulysses and
FREGATE time histories are identical to within statistics, we conclude
that both episodes indeed had the same origin, and that the duration of
this event is therefore ~280 s.
As observed by Ulysses, the 25-100 keV fluence and peak flux over 0.5 s
are ~7x10^-6 erg cm^-2 and 4.7 x 10^-7 erg cm^-2 s^-1. Triangulation
using the FREGATE data gives an annulus centered at RA(2000)= 71.966
deg., Decl.(2000)= -81.411 deg., with radius 79.798 +/- 0.180 deg. (3
sigma). The center line of this annulus passes ~0.1 degrees from the
center of the HETE WXM error circle, and the annulus intersects the
error circle at:
RA(2000) Dec(2000)
191.118 -14.317
190.483 -14.235
191.169 -14.687
190.332 -14.578
The combined annulus/error circle has an area approximately 2.4 times
smaller than the error circle alone, or approximately 800 square
arcminutes. A plot has been posted at ssl.berkeley.edu/ipn3/020305.
GCN Circular 1264
Subject
GRB020305: Optical Observations
Date
2002-03-08T23:57:37Z (23 years ago)
From
Daniel E. Reichart at U.Chicago/Astro <reichart@oddjob.uchicago.edu>
J. Moran, M. Nysewander, K. Shella, C. Yeates, J. Rose, W. Christiansen
(UNC-CH), and D. Reichart (Caltech) report:
We observed the central 30 arcmin x 30 arcmin of the 50 arcmin diameter error
circle of GRB 020305 (HETE 1939) with the Morehead Observatory 0.6 m telescope
beginning ~ 16 hours after the burst.
Visual comparison with the DSS reveals no new sources down to R ~ 18 and V ~ 17.
GCN Circular 1265
Subject
GRB020305, optical observations
Date
2002-03-09T21:40:49Z (23 years ago)
From
Rene Hudec at AIO <rhudec@asu.cas.cz>
M. Jelinek, P. Kubanek, M. Nekola, R. Hudec & BART team,
Astronomical Institute, Academy of Sciences of the Czech Republic,
Ondrejov, report:
The BART robotic telescope at the Ondrejov Observatory observed
the error box of the GRB020305 (HETE trigger 1939) at March
5.93249 UT i.e. 10.45 hours after the burst.
Observation was done by two different cameras in six groups
of eleven (pairs of) images, with 120s exposures. Every
group of images took approx. 35 minutes (0.02430d) to
obtain. Series were beginning at: 2002 March 5.93249, 5.96767,
6.01779, 6.06597, 6.11422 and 6.16356 UT.
The observing conditions were not optimal due to some sort
of cirrus on the sky.
No new optical object was found in reported error box.
Following magnitude limits were obtained:
Wide Field Camera (D=64mm, f/1.7), unfiltered, full HETE error
box coverage, gives single image limiting magnitude 14.5 in 2 minute
integration.
Narrow Field Camera (D=254mm, f/6.3), Johnson R-band,
single-image limiting magnitude 17.0, when combining all 66
obtained NF images there is a limiting magnitude of
18.5 with effective integration time of 132 min. The Narrow Field
Camera FOV is 20 x 20 arcmin (~ 20% of the HETE and ~50%
of the combined HETE/IPN error box)
centered approx 7 arcmin to the west and 4 arcmin to the
south from the center of the HETE reported position (the image
center has RA12:42:30, DEC -14:37).
Further image analysis is planned.
GCN Circular 1267
Subject
GRB 020305: Candidate optical afterglow
Date
2002-03-12T10:03:43Z (23 years ago)
From
Paul Price at RSAA, ANU at CIT <pap@srl.caltech.edu>
P.A. Price, D.W. Fox (Caltech) report on behalf of the
REACT GRB Collaboration:
We have observed the error box of GRB 020305 (GCN ##1262,1263)
with the Palomar 48-inch + unfiltered CCD at 2002 Mar 9.34.
Our 7 x 120 sec exposures cover the entire IPN+HETE error box.
PSF-matched image subtraction of our combined image from Mar 6.33
(GCN #1261) reveals the presence of a point-like source that
was present on Mar 6 and not detected on Mar 9 to a limiting
magnitude of R ~ 21.5 mag. The source is not present on the DSS.
Coordinates of the source are:
RA: 12:42:27.94 DEC: -14:18:11.8 J2000
with an estimated uncertainty of approximately 1 arcsec.
Further observations are underway to ascertain the veracity of
this afterglow candidate.
This message may be cited.
GCN Circular 1270
Subject
GRB 020305: Optical observations
Date
2002-03-13T22:03:32Z (23 years ago)
From
Paul Price at RSAA, ANU at CIT <pap@srl.caltech.edu>
D.W. Fox, P.A. Price (Caltech) and J. Darling (Cornell) report on
behalf of the REACT GRB Collaboration:
We have observed the afterglow candidate of GRB 020305 (GCN #1267)
with the Palomar 200-inch telescope + COSMIC re-imager at 2002
Mar 13.8 UT. Our exposures consisted of 3x600 sec images in Gunn-i.
The afterglow candidate is well detected in the combined image, with
an estimated magnitude of R ~ 22.1 mag. Since this value is little
different from our upper limit from Mar 9, this source may be the
quiescent component (host galaxy?). Due to the large error box, we
cannot as yet rule out the possibility that this object is unrelated
to the GRB.
Further observations are planned.
This message may be cited.
GCN Circular 1271
Subject
GRB020305: Subaru Optical Observations
Date
2002-03-14T19:02:06Z (23 years ago)
From
George Kosugi at Subaru Telescope <george@subaru.naoj.org>
Y. Ohyama, M. Yoshida, K. S. Kawabata, Y. Saito, A. D. Saga, and
S. Harasawa
on behalf of the FOCAS Team:
G. Kosugi, Y. Mizumoto, M. Iye, R. Ogasawara, T. Takata, K. Sekiguchi,
T. Yamada, N. Kobayashi, J. Watanabe, T. Totani, A. Yoshida, N. Kawai,
Y. Urata, T. Tamagawa, K. Torii, J. Noumaru, Y. Komiyama, W. Aoki, and
K. Motohara
on behalf of the Subaru GRB Team:
We have observed the afterglow candidate of GRB 020305 (GCN #1267)
with the Subaru 8.2m telescope atop Mauna Kea at 2002 March 12.6 UT
(7 days after the burst). Several R and I-band images were taken
with the observing instrument FOCAS. The limitting magnitudes were
approximately R=26 and I=25, respectively.
We detected a point source of R=22.6 and I=22.1 within 1 arcsec
from the position reported in GCN #1267. 7 USNO stars were used
for R-band relative photometry. The magnitude in I-band, however,
was estimated by simply converting the observed intensities
empirically to the magnitude. Elongated diffuse nebulosity can be
seen toward the northeast direction from the candidate.
R and I-band images may be found at:
http://www.naoj.org/staff/george/Distribute/GRB020305/GRB020305.html
This message may be cited.
GCN Circular 1275
Subject
GRB020305: Properties of the Candidate Optical Afterglow
Date
2002-03-19T02:12:18Z (23 years ago)
From
Don Lamb at U.Chicago <lamb@oddjob.uchicago.edu>
B. C. Lee, D. Q. Lamb, D. L. Tucker, D. E. Vanden Berk, J. Krzesinski,
D. Long, P. R. Newman, A. Nitta, and S. A. Snedden, on behalf of the
SDSS GRB team, report:
We observed the field of GRB020305 (= H1939) (Ricker et al., GCN 1262)
using the SDSS 0.5-m "Photometric Telescope" (PT) at APO under partly
cloudy conditions beginning at UTC 2002 March 6.33 (20 hours after the
GRB). We obtained three sets of three 400-second g'-band, r'-band, and
i'-band exposures (41.5' x 41.5' field of view) centered on the
reported best-fit location of GRB020305 (Ricker et al., GCN 1262).
These exposures covered the entire combined HETE/IPN error box for the
burst (Hurley et al., GCN 1263).
Co-adding the images taken in each filter, we find an object with
estimated magnitudes of g* = 20.3 +/- 0.5, r* = 20.1 +/- 0.5, and i* =
19.8 +/- 0.5, within 1 arcsec the location of the candidate optical
afterglow reported by Price et al. (GCN 1267). These errors are
conservative, and reflect the fact that we do not yet fully understand
our systematics. The magnitudes we measure are consistent with a
power-law spectrum having a slope of roughly -1, which is typical of
GRB afterglows. Combining our results with the limiting magnitude of R
~ 21.5 at UTC 2002 Mar 9.34 reported by Price et al. (GCN 1267) and the
magnitudes of R = 22.6 and I = 22.1 at UTC 2002 Mar 12.6 reported by
Ohyama et al. (GCN 1271), we find that the candidate afterglow faded
between UTC 2002 Mar 6.33 and Mar 12.6 at a rate that is consistent
with a temporal slope of roughly -1.3, which is also typical of GRB
afterglows. Thus both the spectral and temporal behavior of the
candidate afterglow identified by Price et al. (GCN 1267) support its
identification as the optical afterglow of GRB020305.
This message may be cited.
GCN Circular 1279
Subject
GRB 020305: Optical Observations
Date
2002-03-19T23:36:55Z (23 years ago)
From
Daniel E. Reichart at U.Chicago/Astro <reichart@oddjob.uchicago.edu>
M. Lopez-Morales, J. C. Clemens (UNC-CH), and D. E. Reichart (Caltech) report:
On March 5, we observed the entire 50 arcmin diameter error circle of
GRB 020305 (HETE 1939; GCN 1262) with the automated 8" Pisgah Survey Telescope
at PARI (Pisgah Astronomical Research Institute) in Rosman, North Carolina.
Observations began 15.8 hours after the burst. Visual comparison with the DSS
revealed no new sources at that time.
At the location of the candidate afterglow (GCN 1267), we are partially
contaminated by light from a nearby, bright (I = 14.7 +- 0.1 mag) star.
Consequently, we reimaged the field on March 15. Comparison of aperture
photometry between the two epochs allows us to place the following limits at
the location of the candidate afterglow on March 5: I > 17.6 mag (1 sigma),
I > 16.8 mag (2 sigma), and I > 16.4 (3 sigma).
GCN Circular 1283
Subject
GRB020305: NIR observations
Date
2002-03-21T14:36:13Z (23 years ago)
From
Ingunn Burud at Space Telescope Science Inst <burud@stsci.edu>
I. Burud, J. Rhoads, A. Fruchter, D. Griep
We observed the location of the candidate OT of GRB020305
on 2002 March 13.43 and 14.39 in the K' filter
with the NASA IRTF + NSFCam.
A source is found at the location of the afterglow reported by
Price et al. (GCN 1267) with estimated magnitudes K' = 19.7 and K'=19.8
on March 13.43 and March 14.39 respectively.
The photometric uncertainty is estimated to be 0.2 mag.
For the star U0750_07926230 located 7.5 arcsec South and 12.1 arcsec
East
of the OT we measure a magnitude K'= 13.53 +/- 0.04.
GCN Circular 1302
Subject
GRB020305 BVRI field photometry
Date
2002-03-23T18:41:04Z (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
an 11x11 arcmin field in the error box for GRB020305
(Ricker et al. GCN 1262; Hurley et al. GCN 1263)
with the USNOFS 1.0-m telescope on one marginally photometric
night. The field is approximately centered on
the position of the candiate optical transient reported
by Price et al. (GCN 1267). 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/grb020305.dat
The conditions were basically clear, but early evening clouds
prevented field acquisition until it was near airmass 2.0.
For that reason, there is a slight possibility that the
photometry has larger than the expected 0.02mag external
error, but all tests (such as color consistency) seem reasonable.
The astrometry in this file is based on linear plate solutions
with respect to USNO-A2.0. The internal errors are less than 100mas.
Note that the source mentioned in GCN 1267 is near the northwestern
edge of the error circle, and so the current field photometry does
not do a good job of calibrating small-field images centered on
the error circle. We intend to take another shallower dataset
in the near future centered at the HETE coordinates.
GCN Circular 1542
Subject
GRB 020305: HST/STIS observations
Date
2002-09-16T15:27:24Z (23 years ago)
From
Ingunn Burud at Space Telescope Science Inst <burud@stsci.edu>
J. Gorosabel (IAA-CSIC), J. Fynbo (Univ. of Aarhus), I. Burud (STScI),
A. Fruchter (STScI), J. Hjorth (Univ. of Copenhagen), report for the
larger GOSH (GRB Optical Studies with HST) collaboration:
We have observed the position of the optical afterglow (GCN 1267) of
GRB 020305 (GCN 1262) with HST/STIS. The GRB field was visited four
times; on April 12.7-12.9 UT (Clear filter), April 14.1-14.4 UT
(Long-Pass), June 16.4-16.5 UT (Clear filter), and June 16.6-16.8 UT
(Long-Pass).
Subtraction of the two epoch HST/STIS images taken for each filter
reveals a fading point source. The centroids of the Long-Pass and
Clear filter residuals are consistent with the afterglow position
independently derived registering an afterglow NOT image (taken on
March 16) on our HST/STIS frames.
The magnitudes of the afterglow (AB system) are: 24.693+/-0.008
(Clear, April 12.7-12.9 UT), 24.452+/-0.013 (Long-Pass, April
14.1-14.4 UT), 26.197+/-0.027 (Clear, June 16.4-16.5 UT) and
25.951+/-0.047 (Long-Pass, June 16.6-16.8 UT). The decay indexes
associated to the Clear and Long-Pass filters are, respectively;
Alpha_Clear = 1.40+/-0.03, Alpha_Long-Pass = 1.45+/-0.05. So, the
optical decay is consistent with being achromatic.
The afterglow position is consistent with an extended (~1.2"x0.5")
faint galaxy which shows a complex morphology. A preliminary aperture
photometry (AB system, considering a 0.675" aperture radius and the
corresponding aperture correction) of the whole host galaxy system
yields 25.771+/-0.054 (Clear filter) and 25.464+/-0.087 (Long-Pass
filter), respectively.
Several gifs of the HST/STIS images and the afterglow light curve can
be seen at:
http://www.stsci.edu/~fruchter/GRB/020305/
The optical measurements reported to date (our HST/STIS data points
and the ones given in the GCNs; 1264, 1265, 1267, 1270, 1271, 1275,
1279, 1283) might suggest the presence of a break ~10 days after the
burst. However, a final confirmation would require a more careful
analysis.