GRB 060313
GCN Circular 4884
Subject
GRB060313: Radio Observations
Date
2006-03-16T16:40:58Z (21 years ago)
From
Alicia Soderberg at Caltech <ams@astro.caltech.edu>
A. M. Soderberg (Caltech) and D. A. Frail (NRAO) report on
behalf of a large collaboration:
"We observed the field of GRB 060313 with the Very Large Array
on 2006 March 15.13 UT. No radio source is detected at the
position of the optical afterglow (GCN 4871). We place
an upper limit of 0.11 mJy (3-sigma) at 8.46 GHz."
GCN Circular 4883
Subject
GRB 060313: early afterglow NIR upper limits with REM
Date
2006-03-15T20:40:52Z (21 years ago)
From
Andrea Melandri at Rome Astro Obs <melandri@mporzio.astro.it>
A. Melandri, S. Covino, E. Palazzi, L.A. Antonelli, E. Molinari,
G. Chincarini, F.M. Zerbi,, V. Testa, G. Tosti, F. Vitali, P. Conconi,
G. Cutispoto, G. Malaspina, L. Nicastro, E. Meurs, P. Goldoni,
on behalf of the REM/ROSS Team
The field of the short hard burst GRB 060313 (GCN 4867, Pagani et al.)
was imaged by the robotic 60-cm REM telescope with the both infrared
(REMIR) and optical (ROSS) camera.
Observations started about 33 seconds after the GCN alert about 45
seconds after the burst and a total exposure time of 325, 425 and 325
seconds was obtained with J, H and Ks filter respectively. Preliminary
results on these data have been reported in GCN 4868 (Melandri et al.).
A refined analysis have been performed on the IR stacked images and
no new source is found within the XRT refined error circle (Pagani et
al., GCN 4875) and at the position of the OT-candidate suggested by
Levan and Hjorth (GCN 4871).
We derive the following upper limits for the NIR afterglow:
Filter Delta_T (days) Mag_Lim (5 sigma)
J 0.018 17.6
H 0.012 17.2
Ks 0.010 16.5
Optical images, acquired with the ROSS optical camera in the I, R and
V filters, do not allow to obtain useful information because of a large
contamination due to the Moon light. We were able to derive an upper
limit only of R > 17.5.
This message is citeable.
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[GCN OPS NOTE(15mar06): Per author's request, "030613" in the first
sentence was changed to "060313".]
GCN Circular 4881
Subject
Konus-Wind observation of GRB 060313
Date
2006-03-14T15:54:19Z (21 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team report:
The GRB 060313 (Swift-BAT trigger #201487;
Pagani et al., GCN 4867; Markwardt et al., GCN 4873)
triggered Konus-Wind at T0=726.354 s UT (00:12:06.354).
The Konus-Wind light shows several multipeaked
pulses with a total duration of ~0.8 sec.
As observed by Konus-Wind the burst had
a fluence of 1.42(-0.85, +0.10)x10^-5 erg/cm2 and
peak flux on 16-ms time scale measured from T-T0=0.560 sec
7.0(-4.3, +1.0)x10^-5 erg/cm2/sec
(both in the 20 keV - 2 MeV energy range).
The time-integrated spectrum of the GRB
is well fitted (in the 20 keV - 2 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-(2-alpha)*E/Ep)
with alpha = 0.60(-0.22, +0.19)
and Ep = 922(-177, +306) keV (chi2 = 62/59 dof).
The fitting of the spectrum of the GRB initial part
(accumulated from T-T0=0 to T-T0=0.192 sec in
the same energy range)
gives an unusual photon index alpha:
alpha = -0.33(-0.29, +0.25)
Ep = 655(-74, +84)
(chi2 = 51/59 dof).
All the quoted errors are at the 90% confidence level.
The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB060313_T00726/
GCN Circular 4880
Subject
GRB060313: SSO 40inch Observations
Date
2006-03-14T00:24:08Z (21 years ago)
From
Brian Schmidt at RSAA, ANU (MSSSO) <brian@mso.anu.edu.au>
B. Schmidt and D. Bayliss (ANU), on behalf of a larger collaboration
report,
"We have obtained a series of R-band images with 40inch telescope + WFI
starting at UT Mar 13.358 of GRB 060313 (Pagani et al. GCN 4867) of the
OT-candidate of Levan and Hjorth (GCN 4871).
Comparison of the image with those taken with Gemini-S (Schmidt et al.
GCN 4876)
shows the OT-candidate has faded by at least 0.4 magnitudes (95%
confidence).
Although not detected, using the USNOA2 star located at
RA=04:26:28.906 DEC=-10:51:00.16 (J2000) R=18.1
as a reference, we estimate the OT to be fainter than R=20.5 (95%
confidence). This variability confirms the association of the OT with
GRB060313."
GCN Circular 4879
Subject
GRB 060313: Further analysis of the Swift-BAT bright short hard burst
Date
2006-03-14T00:11:51Z (21 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
S. Barthelmy (GSFC), J. Cummings (GSFC/NRC), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), J. Norris (GSFC), T. Sakamoto (GSFC/NRC),
D. Palmer (LANL
on behalf of the Swift-BAT team:
Using the data set from T-300 to T+300 sec from additional telemetry
downlinks, we report further analysis of BAT GRB 060313 (trigger #201487)
(Pagani, et al., GCN 4867; Markwardt, et al., 4873). This short burst
does not show any sign of extended emission in the T+1 to T+300 sec range
at an upper limit of 0.001 cnt/detector/sec. This corresponds to a
flux ratio upper limit between the initial peak and the peak of any
potential extended emission of 2000. We reference SHBs 050724 and 051227
which had ratios of 46 and ~10, respectively.
The lag analysis shows this burst to be cleanly in the short hard burst class
(Norris and Bonnell, 2006, ApJ, accepted; see, Figure 3).
Specifically, the measured lags are:
50-100 keV to 15-25 keV: 0.8 ms +- 0.6 ms
100-350 keV to 25-50 keV: 0.3 ms +- 0.7 ms
We further note that the lightcurve has multiple structures. There are
at least 20 statistically significant peaks with FWHM in the 5-15 msec range.
There is no perdiodic structure in the lightcurve for at least
the first 100 sec.
GCN Circular 4878
Subject
GRB 060313: PROMPT Observations
Date
2006-03-13T19:53:36Z (21 years ago)
From
Melissa Nysewander at UNC,Chapel Hill <mnysewan@physics.unc.edu>
M. Nysewander, J. Haislip, D. Reichart, K. Ivarsen, A. LaCluyze, J. A.
Crain, A. Foster, J. Kirschbrown, C. MacLeod, and A. Trotter report on
behalf of the UNC team of the FUN GRB Collaboration:
Skynet observed the localization of GRB 060313 (Pagani et al., GCN 4867)
with two of the 16-inch PROMPT telescopes at CTIO beginning 43.7 min after
the burst in r'i'I.
A preliminary analysis of the data shows the candidate afterglow first
reported by Levan & Hjorth (GCN 4871) to be at r' = 19.9 +- 0.3 and I =
19.7 +- 0.3 at mean times of 1.3 hours and 1.4 hours after the burst.
PROMPT also made a marginal detection (~2 sigma) of i' ~ 20.5 at a mean
time of 1.5 hours after the burst. We used five calibration stars that
were taken from the USNO-B1.0 and NOMAD catalogues and transformed to the
SDSS filters via Smith et al. 2002.
PROMPT is currently being built and commissioned.
GCN Circular 4877
Subject
GRB 060313: Swift/UVOT Observations
Date
2006-03-13T10:29:02Z (21 years ago)
From
Patricia Schady at MSSL/Swift <ps@mssl.ucl.ac.uk>
P. Schady (PSU/MSSL-UCL) C. Pagani (PSU) on behalf of the Swift/UVOT team
The Swift/UVOT began taking data on the field of GRB 060313 at 00:13:23 UT on
2006-03-13, approximately 79s after the BAT trigger (Pagani et al., GCN 4867).
The afterglow is detected above the 2-sigma level in the V, B and UVW2 filter
at a position consistent with that reported by Cobb et al. (GCN 4872), and
there is a tenuous detection in the U and UVW1 band coadded exposures at the
1.4 and 1.2 sigma level, respectively. The detection in UVW2 implies that
the Lyman limit must be blueward of ~2500 A, providing a redshift upper
limit of z <~1.7.
All detections above 2-sigma and the 2-sigma upper limits from the coadded
image of a set of exposure for each filter are as follows:
Filter T_range(s) Exp(s) Average mag/UL sigma
V 177-6963 933 20.03+/-0.39 2.9
B 469-5453 953 20.69+/-0.48 2.7
U 415-844 100 > 19.95
UVW1 361-790 100 > 18.91
UVM2 307-736 100 > 18.89
UVW2 578-900 950 20.98+/-0.5 2.2
These magnitudes are uncorrected for Galactic extinction;
E(B-V) = 0.067.
GCN Circular 4876
Subject
GRB060313:Gemini South Observations
Date
2006-03-13T09:55:02Z (21 years ago)
From
Brian Schmidt at RSAA, ANU (MSSSO) <brian@mso.anu.edu.au>
B. Schmidt (ANU), Derek Fox (Penn State), and Edo Berger (OCIW), on
behalf of a larger collaboration report,
"We have obtained a series of r-band images with Gemini-S + GMOS between
UT Mar 13.058 and March 13.096 of GRB 060313 (Pagani et al. GCN 4867) of
the OT-candidate of Levan and Hjorth (GCN 4871). Comparison with USNOA2
star located at
RA=04:26:28.906 DEC=-10:51:00.16 (J2000) R=18.1
shows the OT-candidate to be 2.19 magnitudes fainter than the star at
Mar 13.058, and 2.26 mags fainter at Mar 13.096, a marginally
significant difference. It is possible that an underlying host galaxy is
significantly affecting the photometry.
We would like to thank the Gemini Staff for their help in executing
these Target of Opportunity observations."
GCN Circular 4875
Subject
GRB 060313: Swift-XRT team refined analysis
Date
2006-03-13T06:38:57Z (21 years ago)
From
Claudio Pagani at PSU/Swift-XRT <pagani@astro.psu.edu>
C. Pagani (PSU), D. Morris (PSU), D. Grupe (PSU) and D. Burrows (PSU) report on
behalf of the Swift XRT team:
We have analyzed the first two orbits of Swift XRT data of GRB 060313 (Pagani et
al., GCN 4867). The revised XRT position is
RA(J2000) = 04h 26m 28.5s
Dec(J2000) = -10d 50m 40.2s
We estimate an uncertainty of 4 arcseconds radius (90% containment).
The revised position is 2 acrseconds from the suggested optical afterglow
reported by Levan et al. (GCN 4871) and 1.5 arcseconds form the previously
reported XRT position (GCN 4870).
The X-ray spectrum of the data can be fitted by a single absorbed power law with
a photon index Gamma=1.70+/-0.10 and an absorption column density nH consistent
with the Galactic value of 4.7e20cm-2; Dickey & Lockman 1990.
The light curve shows a decay during with alpha=1.50+/-0.18. Assuming this decay
slope the prediction for the flux 24 hours after the trigger is 1.2e-13
ergs/s/cm2.
This circular is an official product of the Swift XRT Team.
GCN Circular 4874
Subject
GRB060313: optical observations of the afterglow candidate
Date
2006-03-13T06:16:28Z (21 years ago)
From
Christina Thoene at Niels Bohr Institute,DARK Cosmo Ctr <cthoene@astro.ku.dk>
Christina Thoene, Chloe Feron, Jens Hjorth and Brian L. Jensen (Dark
Cosmology Centre) report
We obtained R and I band observations of GRB 060313 (GCN 4867) with the
Danish 1.5m telescope and DFOSC at La Silla. Observations started at UT
00:23:53 (11min after the burst) until UT 02:11:10. Inside the XRT error
circle (GCN 4870) we detect a new, previously uncatalogued source at the
position (J2000)
RA = : 04:26:28.42
Dec =-10:50:39.84
This is consistent with the position reported in GCN 4871 and GCN 4872.
The R magnitude obtained from stacked images with a mean time of about 1h
after the burst is
R = 20.4 (based on preliminary photometric zero points)
A finding chart can be found at:
http://www.astro.ku.dk/~brian_j/grb/grb060313.008/
GCN Circular 4873
Subject
GRB 060313: Refined analysis of the Swift-BAT bright short hard burst
Date
2006-03-13T05:43:42Z (21 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
C. Markwardt (GSFC/UMD), L. Barbier (GSFC), S. Barthelmy (GSFC),
J. Cummings (GSFC/NRC), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (BYU-Idaho), H. Krimm (GSFC/USRA), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS),
J. Tueller (GSFC)
on behalf of the Swift-BAT team:
Using the data set from T-60 to T+123 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 060313 (trigger #201487)
(Pagani, et al., GCN 4867). The BAT ground-calculated position is RA,Dec =
66.624,-10.859 deg {04h 26m 29.8s,-10d 51' 30.9"} (J2000) +- 1.0 arcmin,
(radius, sys+stat, 90% containment). The partial coding was 54%.
The lightcurve shows 3 or 4 overlapping peaks. They start with a very fast
rise (less than 40 msec). There is a possibility of further faint emission
past the end of the last peak (T+1 to T+2 sec). T90 (15-350 keV) is
0.7 +- 0.1 sec (estimated error including systematics).
The time-averaged spectrum from T+0.06 to T+0.94 is best fit by a simple
power-law model. The power law index of the time-averaged spectrum
is 0.71 +- 0.07. The fluence in the 15-150 keV band is
1.13 +- 0.05 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+0.01 sec in the 15-150 keV band is 12.1 +- 0.4 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
GCN Circular 4872
Subject
GRB 060313, SMARTS optical counterpart?
Date
2006-03-13T04:49:22Z (21 years ago)
From
Bethany Cobb at Yale U <cobb@astro.yale.edu>
B. E. Cobb, part of the larger SMARTS consortium, reports:
Following the report of a possible X-ray afterglow to GRB 060313,
the SMARTS imaging described in GCN 4869 was re-examined.
The X-ray position is unfortunately outside our NIR imaging. In our
R and I band images, however, there is a possible optical counterpart
within the X-ray detection error region, at preliminary coordinates of:
RA = 4:26:28.45
Dec = -10:50:39.9
The source is only detected at the 1 sigma level, but the fact
that it is visible in both R and I suggests the source is not
spurious. The source is not detected in the DSS images.
In comparison with several nearby USNO-B1.0 stars, the
source has a magnitude of R ~ 19.9 +/- 0.3.
GCN Circular 4871
Subject
GRB 060313: Possible optical counterpart
Date
2006-03-13T04:26:31Z (21 years ago)
From
Andrew Levan at U.of Leicester <anl@star.le.ac.uk>
A.J. Levan (U. Hertfordshire), J. Hjorth (Dark Cosmology Centre) report
for the GRACE collaboration:
We observed the location of the short hard GRB 060313 (Pagani et al.
GCN 4867) with the VLT and FORS2 beginning at 01:28 UT. At the location
of the X-ray afterglow reported by Pagani et al. (GCN 4870) we find a
point source which is not visible in the DSSII (red) although is somewhat
brighter than its limiting magnitude. We suggest this is the afterglow of
GRB 060313.
The location of the source is:
RA = 04:26:28.4
Dec = -10:50:40.1
Currrently we estimate our uncertainty in this position is ~0.5" in each axis.
Further observations are planned.
GCN Circular 4870
Subject
GRB 060313: Swift XRT position
Date
2006-03-13T03:43:51Z (21 years ago)
From
Claudio Pagani at PSU/Swift-XRT <pagani@astro.psu.edu>
C. Pagani (PSU), D. Burrows (PSU) report on behalf of the Swift XRT
team:
We have analyzed the Swift XRT data from the first orbit of observation of GRB
060313 (Pagani et al., GCN 4867). We find an uncatalogued source at the
following location:
RA(J2000) = 04h 26m 28.4s
Dec(J2000) = -10d 50m 41.5s
We estimate an uncertainty of 8 arcseconds radius (90% containment).
This position is 103 arcseconds from the BAT position given in GCN 4867. A full
analysis of the XRT data will follow.
This circular is an official product of the Swift XRT Team.
GCN Circular 4869
Subject
GRB 060313, SMARTS optical/IR observations
Date
2006-03-13T01:46:32Z (21 years ago)
From
Bethany Cobb at Yale U <cobb@astro.yale.edu>
B. E. Cobb, part of the larger SMARTS consortium, reports:
Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 060313
(Pagani et al. GCN 4867) beginning ~0.3 hours post-burst
(2006-03-13 00:31 UT). Optical imaging in B,V,R and I has a
field of view of 6'x6' and, therefore, covers the entire GRB
error circle. IR imaging in J, H, K and Y has a smaller field
of view (2.4'x2.4') and covers a region totaling 5.8 square arcminutes in
the middle of the quoted error region. Several dithered images
were obtained in each filter, with total summed exposure times
of 180s in each of BRIYJK and 120s in each of H and V.
Preliminary visual comparison of the optical images to the DSS
and the IR images to 2MASS frames does not reveal any new sources.
The detection limits of the combine ANDICAM images are slightly
shallower than that of MASS and the DSS.
GCN Circular 4868
Subject
GRB060313: optical and near infrared observations with REM
Date
2006-03-13T01:27:51Z (21 years ago)
From
Andrea Melandri at Rome Astro Obs <melandri@mporzio.astro.it>
A. Melandri, S. Covino, E. Molinari, G. Chincarini, F.M. Zerbi,
V. Testa, G. Tosti, F. Vitali, L.A. Antonelli, P. Conconi, G. Cutispoto,
G. Malaspina, L. Nicastro, E. Palazzi, E. Meurs, P. Goldoni,
on behalf of the REM/ROSS Team
We imaged the field of the short hard burst GRB 030613 (GCN 4867,
Pagani et al.) with the robotic 60-cm REM telescope located at
La Silla, Chile.
The observations were performed both with the optical and the
infrared camera of the REM telescope and started about 33 seconds
after the GCN alert and about 45 seconds after the burst.
First inspection of visual and infrared images do not reveal any new
source inside the Swift-BAT error circle (GCN 4867, Pagani et al.)
down to the limiting magnitude of the 2MASS catalog.
Further observations and analises are still ongoing.
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GCN Circular 4867
Subject
GRB 060313: Swift-BAT detection of a bright short hard burst
Date
2006-03-13T00:47:42Z (21 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
C. Pagani (PSU), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), N. Gehrels (GSFC),
D. Grupe (PSU), S.T. Holland (GSFC/USRA), S. Hunsberger (PSU),
C. Markwardt (GSFC/UMD), F. Marshall (GSFC), D. Palmer (LANL)
on behalf of the Swift team:
At 00:12:06 UT, Swift-BAT triggered and located GRB 060313 (trigger=201487).
The spacecraft slewed immediately. The BAT on-board calculated location is
RA,Dec 66.609d,-10.872d {04h 26m 26s,-10d 52' 19"} (J2000), with an uncertainty
of 3 arcmin (radius, 90% containment, stat+sys). The BAT light curve shows
two slightly overlapping peaks with a total duration of ~1.6 sec.
The first peak start at ~T-0.7 sec and the second peak ends by T+0.9 sec.
The peak count rate was ~40,000 counts/sec (15-350 keV), at ~0.0 seconds
after the trigger. This is definitely a short hard burst.
The XRT began taking data at 00:13:24 UT, 79 seconds after the BAT trigger.
The XRT on-board centroid algorithm did not find a source in the image and
no prompt position is available. We are waiting for down-linked data
to detect and determine a position for the source.
UVOT took a finding chart exposure of 200 seconds with the V filter starting
78 seconds after the BAT trigger. No afterglow candidate has been found
in the initial data products. The 2.7'x2.7' sub-image covers 25% of the
BAT error circle. The typical 3-sigma upper limit has been about 18th mag.
The 8'x8' region for the list of sources generated on-board covers 100%
of the BAT error circle. The list of sources is typically complete to
about 18.0 mag. No correction has been made for the expected extinction
of about 0.2 magnitudes.
We note that the magnitude B=16.3 galaxy LEDA 3093309 (aka NPM1G -10.0175)
is within 5 arcminutes of the BAT position, however there is currently
no evidence for a physical association between these two objects.