GRB 060403
GCN Circular 4945
Subject
GRB 060403: Swift detection of a burst
Date
2006-04-03T13:40:52Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
P. T. Boyd (NASA/GSFC), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
J. R. Cummings (NASA/ORAU), N. Gehrels (NASA/GSFC),
C. Gronwall (PSU), S. T. Holland (GSFC/USRA), J. A. Kennea (PSU),
H. A. Krimm (GSFC/USRA), V. La Parola (INAF-IASFPA),
V. Mangano (INAF-IASFPA), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-OAB)
and T. Sakamoto (NASA/ORAU) report on behalf of the Swift Team:
At 13:12:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 060403 (trigger=203755). Swift slewed immediately to the burst.
The BAT on-board calculated location is RA,Dec 282.306, +8.330
{18h 49m 13s, +08d 19' 47"} (J2000) with an uncertainty of 3 arcmin
(radius, 90% containment, including systematic uncertainty).
The BAT light curve shows a single FRED-like peak structure
with a duration of about 25 sec. The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began taking data at 13:15:59 UT, 222 seconds after the BAT
trigger. The XRT on-board centroid algorithm did not find a source in
the image. However downlinked image data show the presence of a
uncatalogued point source at the following position:
RA(J2000): 18:49:21.2
Dec(J2000): +08:19:39.3
with an error radius of 8 arcseconds (90% containment). This position
lies 116 arcseconds from the BAT position.
UVOT took a finding chart exposure of 100 seconds with the White
filter starting 63 seconds after the BAT trigger. No afterglow
candidate has been found in the initial data products. The XRT
position is not covered by the 2.7'x2.7'sub-image. The typical 3-sigma
upper limit has been about 18.5 mag. The 8'x8' region for the list of
sources generated on-board covers 100% of the XRT error circle. The
list of sources is typically complete to about 18.1 mag. No
correction has been made for the large, but uncertain expected extinction.
We note that this is a crowded field.
GCN Circular 4947
Subject
GRB060403: Swift XRT refined position
Date
2006-04-03T18:37:52Z (19 years ago)
From
Vanessa Mangano at INAF-IASFPA <vanessa@ifc.inaf.it>
V. Mangano (INAF-IASFPA), J. Kennea (PSU), V. La Parola, T. Mineo,
G. Cusumano (INAF-IASFPA), D.N. Burrows (PSU), P. Boyd (NASA/GSFC)
on behalf of the Swift XRT team
We analysed 840 s exposure in Photon Counting mode from
the first orbit of the Swift observation of GRB060403
(Boyd et al. 2006, GCN 4945).
The refined coordinates of the X-ray source are:
RA(J2000) = 18 49 21.8
Dec(J2000) = +08 19 45.3
with an estimated uncertainty of 5.5 arcseconds radius
(90% containment). This position is 11 arcseconds from
the preliminary position given in GCN 4945.
The X-ray light curve shows a standard afterglow decay.
Further analysis is on-going.
This circular is an official product of the Swift XRT team.
GCN Circular 4948
Subject
GRB 060403: Refined analysis of the Swift-BAT burst
Date
2006-04-03T21:47:08Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
J. Tueller (GSFC), L. Barbier (GSFC), S.D. Barthelmy (GSFC),
J. Cummings (GSFC/NRC), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (BYU-Idaho), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
J. Norris (GSFC), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/NRC), G. Sato (ISAS)
on behalf of the Swift-BAT team:
Using the data set from T-119 to T+183 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 060403 (trigger #203755)
(Boyd, et al., GCN 4945). The BAT ground-calculated position is RA,Dec =
282.336, 8.328 deg {18h 49m 20.7s, 8d 19' 39.8"} (J2000) +- 1.1 arcmin,
(radius, sys+stat, 90% containment). The partial coding was 100%.
The mask-weighted light curve shows a single FRED-like peak starting at
T-8 sec and extending out to about T+32 sec. T90 (15-350 keV) is
30 +- 3 sec (estimated error including systematics).
The spectral lags place this burst in the long-burst class
(Norris et al. 2005, ApJ, 627, 324):
1.23 +- 0.55 s (15-25 keV vs. 50-100 keV) and
0.80 +- 0.24 s (25-50 keV vs. 50-100 keV).
The time-averaged spectrum from T-6.2 to T+32.1 is best fit by
a simple power-law model. The power law index of the time-averaged
spectrum is 1.08 +- 0.09. The fluence in the 15-150 keV band is
1.4 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured
from T-1.22 sec in the 15-150 keV band is 1.0 +- 0.1 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
GCN Circular 4951
Subject
GRB 060403: Swift/UVOT upper limits
Date
2006-04-04T07:43:16Z (19 years ago)
From
Tracey Poole at MSSL <tsp@mssl.ucl.ac.uk>
T. S. Poole (UCL-MSSL), and P. T. Boyd (NASA/GSFC) on behalf of the
Swift/UVOT team.
The Swift/UVOT began observing the field of GRB060403 (BAT Trigger=203755,
P. T. Boyd, et. al, GCN 4945) at 13:13:00 UT, 43s after the BAT trigger
(which includes the 10s V filter settling exposure). No new source is
detected at the XRT position (V. Mangano, GCN 4947) in coadded images with
any of the filters. The following 5-sigma magnitude upper limits are not
corrected for Galactic extinction; E(B-V) = 1.270.
Filter T_range(s) T_exp(s) 5sigma(mag)
V 43-10090 1220.0 19.25
B 4011-16788 1299.0 20.41
U 3807-15876 1299.0 20.16
UVW1 3602-11845 1242.6 20.18
UVM2 3397-10994 1299.4 20.59
UVW2 4421-6052 399.6 19.99
WHITE 63-17630 1329.8 20.37
Where T_range is time post-trigger, and T_exp is the exposure time of
the observation. A 6 arcsec radius was used for all filters.
This message may be cited.
GCN Circular 4952
Subject
GRB060403: XRT refined analysis
Date
2006-04-04T12:43:28Z (19 years ago)
From
Vanessa Mangano at INAF-IASFPA <vanessa@ifc.inaf.it>
T. Mineo, V. Mangano, V. La Parola, G. Cusumano (INAF-IASFPA),
J. Kennea (PSU), P.T. Boyd (NASA/GSFC), D.N. Burrows (PSU)
report on behalf of the Swift XRT team:
We analyzed the Swift XRT data of GRB 060403 (Boyd et al. GCN 4945).
The observation started 52 s after the BAT trigger in Windowed Timing (WT)
mode because before slewing to the GRB position, XRT was observing
SGR1900+14 in manual state. The instrument then switched to auto state,
taking the initial image frame for on board centroiding 222 s after the
trigger, as reported in GCN 4945.
The data we report on consisted of 5.5 ks exposure in WT mode
and 15 ks exposure in Photon Counting (PC) mode.
The 0.2-10 keV light curve shows a clear power law decay with
slope -1.49+/-0.04.
The average WT spectrum accumulated during the first orbit (from 52 s
to 300 s after the trigger) is well fitted by a power law with photon
index 1.61+/-0.22, absorbed at lower energies by a column of
(8.1+/-2.1) x 10^21 cm^-2, higher than the galactic value (4.9 x 10^21
cm^-2).
The 0.2-10 keV unabsorbed flux is 1.61 x 10^-11 ergs cm^-2 s^-1.
If the burst continues decaying at the current rate we
estimate an XRT count rate of 1 x 10^-4 counts/s at T+48hr,
which corresponds to an unabsorbed 0.2-10 keV flux
of 1x 10^-14 ergs cm^-2 s^-1.
This circular is an official product of the Swift XRT team.
GCN Circular 4953
Subject
GRB060403: Optical Limit
Date
2006-04-05T02:28:16Z (19 years ago)
From
Adalberto Piccioni at Astronomy, Bologna U. <adb@piccio.org>
F. Terra, (Second University of Roma "Tor Vergata"), C.
Bartolini, G. Greco, A. Guarnieri, A. Piccioni (Bologna
University), D. Nanni (INAF/OAR and Second University
of Roma "Tor Vergata"), S. Galleti, R. Gualandi (INAF
Bologna) and G. Pizzichini (INAF/IASF Bologna) report:
Using the 152 cm Loiano telescope equipped with the
BFOSC camera system, we obtained in poor sky conditions
(seeing = 2.7 arcsecs) two Rc-band images (2 x 900 sec) of
the field of the GRB060403 (Boyd et al., GCN 4945, Mangano
et al., GCN 4947) starting at April 4.0778 and 4.0898
respectively. A preliminary comparison with the DSS-2 does
not reveal any new source brighter than the DSS-2 limit
within 1' from the XRT location. Our co-added image reaches
a detection limit slightly deeper than Rc=19.
The Rc co-added image has been posted in our public
directory from where it can be retrieved by sftp using:
hostname: ermione.bo.astro.it
username: publicGRB
password: GRB_bo.
GCN Circular 4954
Subject
GRB 060403: MITSuME optical observation
Date
2006-04-05T06:08:19Z (19 years ago)
From
Nobuyuki Kawai at Tokyo Tech <nkawai@hp.phys.titech.ac.jp>
K. Yanagisawa (OAO/NAO) and N. Kawai (Tokyo Tech) report on
behalf of the Mitsume Collaboration:
"The field of GRB060403 (Boyd et al. GCN 4945, Mangano et al. GCN 4947)
was observed with the 3-color MITSuME 50cm Telescope at Okayama, Japan
starting at 16:59 UT until 16:22 UT (mid-epoch 16:10 UT, t_burst+3 hr)
in g', Rc, and Ic bands simultaneously.
With the total effective exposure of 18 min (60s x 18 frames),
we did not detect a source brighter than g'=18.3, Rc=18.3, and Ic=17.9.
(3 sigma) at the position of the XRT error circle.
We placed the images at
http://bragi.oao.nao.ac.jp/support/telescope/grb50/images/GRB060403.png"
GCN Circular 4955
Subject
GRB 060403 Optical observations
Date
2006-04-07T09:30:20Z (19 years ago)
From
Yuji Urata at RIKEN <urata@crab.riken.go.jp>
Y.Q. Lou, X.F. Wang (THCA), W.K. Zheng, Y.L. Qiu(NAOC),
I.C. Yen (NTNU), C.S. Lin, H.C. Lin, K.Y. Huang (NCU),
Y. Urata (Saitama U/RIKEN) on behalf of EAFON report
"We have observed GRB 060403 X-ray afterglow position (Boyd et
al. GCN 4945, Mangano et al. GCN 4947) using Xinglong (China) 0.8m and
Lulin (Taiwan) 1.0m telescopes on April 3 and 5. In I-band images
taken at Lulin, we found two sources at the X-ray error region which
do not appear in DSSII images. Since our I-band images are deeper than
DSSII, we have monitored the sources. These sources do not show any
significant variabilities in our observational period. Thus we
conclude that these two sources do not related with GRB afterglow.
The limiting magnitude are summarize below.
-------------------------------------------------------
Date Delay (h) Site Filter Exp.(s) Limit mag
-------------------------------------------------------
Apr. 3 6.07 Xinglong R 600s x 12 20.4
Apr. 3 5.87 Lulin I 300s x 5 21.0
Apr. 5 55.63 Lulin I 300s x 2 19.6
-------------------------------------------------------
This message may be cited."
GCN Circular 4956
Subject
GRB060403: optical observations
Date
2006-04-11T19:50:37Z (19 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
D. Sharapov (MAO, and NOT, La Palma), A. Pozanenko (IKI), E. Klunko (ISTP),
M. Ibrahimov (MAO), and V. Rumyantsev (CrAO) on behalf of larger GRB follow
up collaboration report:
We observed the error-box of GRB060403 (Boyd et al. GCN 4945) with 1.5m
telescope of Sayan Observatory (Mondy) in R and V-bands on Apr.3 between
(UT) 19:44 and 21:10 under poor weather conditions and with 1.5m telescope
of Maidanak Astronomical Observatory on Apr. 03 (UT) 22:36 - 22:59 and on
Apr. 05 in R-band. Several images were obtained in each epochs. Telescope
of Sayan Observatory equipped with SC3 CCD camera 1040x1160, 16mkm, FOV =
2'x2'.
Observations of Maidanak observatory are deeper than DSS2 and within
refined XRT error box (Mangano et al. GCN 4947) few objects were found which
are not presented in DSS2 R. All found objects are presented in both epochs
and most probably are not related with GRB060403.
The limiting magnitudes of the observations are based on USNO A2.0:
Mid. time, Filter, Limit, Seeing
(UT)
Apr.3.819 R 17.5 ~2.5"
Apr.3.876 V 18.8 ~2.0"
Apr.3.942 R 21.2 ~1.1"
Apr.5.994 R 20.5 ~1.4"
Results are preliminary; the images can be found in
http://grb.rssi.ru/GRB060403/