GRB 060210
GCN Circular 4723
Subject
GRB060210: Optical afterglow
Date
2006-02-10T05:19:16Z (19 years ago)
From
Derek Fox at PSU <dfox@astro.psu.edu>
D.B. Fox (Penn State) and S.B. Cenko (Caltech) report on behalf of
a larger collaboration:
"We have imaged the XRT localization region for GRB060210 (Swift
Trigger #180977) with the robotic Palomar 60-inch telescope, in
two 60-second exposures beginning roughly 5 minutes after the BAT
trigger. We identify a single point-like, bright, stationary
source consistent with the XRT position, at coordinates:
R.A. 03:50:57.41, Dec +27:01:34.4 (J2000)
with a coordinate uncertainty of less than 2" in each axis. The
estimated brightness of the transient at t+5.5 minutes is
R=18.3 +/- 0.1 mag by reference to USNO B-1.0 catalog magnitudes
of stars in the field."
GCN Circular 4724
Subject
GRB 060210: Swift detection of a burst
Date
2006-02-10T05:27:56Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
A. Beardmore (U Leicester), S. Barthelmy (GSFC), P. Boyd (GSFC),
D. Burrows (PSU), N. Gehrels (GSFC), C. Markwardt (GSFC/UMD),
F. Marshall (GSFC), J. Osborne (U Leicester), D. Palmer (LANL),
P. Schady (PSU/UCL-MSSL)
on behalf of the Swift team:
At 04:58:50 UT, Swift-BAT triggered and located GRB 060210 (trigger=180977).
The spacecraft slewed immediately. The BAT on-board calculated location is
RA,Dec 57.730d,+27.026d {03h 50m 55s,+27d 01' 33"} (J2000), with an uncertainty
of 3 arcmin (radius, 90% containment, stat+sys). The BAT light curve shows
a two-peak structure with a total duration of ~5 sec. The peak count rate
was ~4500 counts/sec (15-350 keV), at ~1 seconds after the trigger.
The XRT began observing the field at 05:00:25 UT, 95 seconds after the
BAT trigger. XRT found a variable, uncatalogued X-ray source
located at RA(J2000) = +03h 50m 57.2s, Dec(J2000) = +27d 01' 38.2", with an
estimated uncertainty of 5.4 arcseconds (90% confidence radius).
This location is 27 arcseconds from the BAT on-board position, within
the BAT error circle. The initial flux in the 2.50s image was
4.6e-09 erg/cm2/s (0.2-10 keV).
UVOT took a finding chart exposure of 200 seconds with the V filter starting
99 seconds after the BAT trigger. No afterglow candidate has been found in the
initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT 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 XRT 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 0.3 magnitudes.
GCN Circular 4725
Subject
GRB 060210: candidate afterglow
Date
2006-02-10T05:28:55Z (19 years ago)
From
Weidong Li at UC Berkeley KAIT/LOSS <weidong@astron.berkeley.edu>
W. Li, University of California, Berkeley, on behalf of the
KAIT GRB team, report:
The robotic 0.76-m Katzman Automatic Imaging Telescope (KAIT)
at Lick Observatory observed GRB060210 detected with Swift
(Trigger 180977). We identied an new object at the
following position in an unfiltered 15s image started at
04:59:53 UT (63.2s after the burst):
RA = 03:50:57.35 Dec = +27:01:34.1 (J2000.)
the candidate afterglow is at mag 18.1 when calibrated to
USNO B1.0 catalog. Further observations are ongoing.
GCN Circular 4726
Subject
GRB060210:Faulkes Telescope North Afterglow Confirmation
Date
2006-02-10T05:44:19Z (19 years ago)
From
Carole Mundell at ARI, JMU,Liverpool <cgm@astro.livjm.ac.uk>
C.G. Mundell, A. Melandri, A. Gomboc, C. Guidorzi, I. A. Steele,
C.J. Mottram, A. Monfardini, R.J. Smith, M.F. Bode (Liverpool JMU),
E. Rol, P. O'Brien, N. Bannister (U. Leicester) report:
"The 2-m Faulkes Telescope North robotically followed up GRB060210
(SWIFT trigger 180977) 4.18 min after the GRB trigger time.
The automatic "detection mode" procedure detected an uncatalogued
candidate at:
RA(J2000): 03:50:57.37
Dec(2000): +27:01:34.40
(positional uncertaintly 0.5")
with magnitude R = 18.1 mag (wrt USNOB1).
This source is coincident with that of Fox et al. (GCN 4723) and Li et
al. (GCN 4725) and found to be fading, thus confirming it as the
afterglow.
Observations and analysis are ongoing.
This message may be cited"
GCN Circular 4727
Subject
GRB 060210: optical evolution
Date
2006-02-10T07:12:35Z (19 years ago)
From
Weidong Li at UC Berkeley KAIT/LOSS <weidong@astron.berkeley.edu>
W. Li, University of California, Berkeley, on behalf of the
KAIT GRB team, report:
We report further analysis of the KAIT observations of
GRB 060210 between 1 to 48 minutes after the burst.
The optical afterglow showed an interesting evolution:
it was nearly flat (with unfiltered mag of about 18.1)
between t = 1 to 5 minutes, brightened to mag 17.7
at t = 9 minutes, then began a fast power-law decline
between t = 10 to 48 minutes with an index of -1.05 +/- 0.05.
A light curve for the optical afterglow is at
http://astron.berkeley.edu/~weidong/grb060210.lc.gif
The figure showed both the unfiltered and I-band light
curve of the OA, both calibrated to USNO B1.0 red magnitudes.
This message can be cited.
GCN Circular 4728
Subject
GRB060210: Early Optical Observations
Date
2006-02-10T07:29:15Z (19 years ago)
From
Grant Williams at Steward Observatory <ggwilli@mmto.org>
G. G. Williams (MMTO) and P. A. Milne (Steward Observatory), on behalf of
the Super-LOTIS Collaboration, report:
The robotic 0.6-m Super-LOTIS telescope began observing the error box of
GRB060210 (Swift Trigger 180977, GCN 4724) at 04:59:44.9 UT, 55 seconds
after the burst. Our initial observations include 5 x 10s exposures, 5 x
20s exposures, and 30 x 60s exposures, all in the R-band. We do not
detect the afterglow reported by Fox et al. (GCN 4723) and Li et al. (GCN
4725) in our earliest exposure to the following 5-sigma limiting magnitude
using USNO-B1 stars:
t obs (UT) exp t (s) t-t_0 (s) Limit
--------------------------------------------------------
04:59:44.9 10 55.1 R > 17.5
Additional multi-band observations and analysis including image stacking
are ongoing.
GCN Circular 4729
Subject
GRB060210: Gemini absorption spectroscopy
Date
2006-02-10T09:12:53Z (19 years ago)
From
Antonino Cucchiara at PSU <cucchiara@astro.psu.edu>
A. Cucchiara (Penn State), D. B. Fox (Penn State), and E. Berger
(Carnegie Observatories) report on behalf of a larger collaboration:
"We have observed the optical afterglow (Fox & Cenko, GCN 4723) of GRB
060210 (Beardmore et al., GCN 4724) with the GMOS instrument on
Gemini-North. Examination of a reduced 1500-s spectrum of the
afterglow reveals a strong continuum break at roughly 6000 Angstroms,
with only intermittent transmission blueward of this wavelength and
multiple strong absorption features to the red, including the NV
1239,1243 doublet, the CIV 1548,1550 doublet, and an array of Si
transitions, at the common redshift of z=3.91. We propose this as the
redshift of GRB 060210."
We acknowledge the rapid response effort of Gemini personnel that
yielded these data, and in particular observer I. Song.
GCN Circular 4730
Subject
GRB060210: Optical Observations
Date
2006-02-10T09:36:40Z (19 years ago)
From
Grant Williams at Steward Observatory <ggwilli@mmto.org>
G. G. Williams (MMTO) and P. A. Milne (Steward Observatory), on behalf of
the Super-LOTIS collaboration, report:
Further analysis of the 0.6-m Super-LOTIS observations (GCN 4728) of the
error box of GRB060210 (GCN 4724) yield detections of the optical
afterglow (GCN 4723 and GCN 4725) in the summed R-band data. The summed
images include a stack of five 10s exposures and a stack of five 20s
exposures. The following table lists the mid-time of the stacked
exposures and the resulting photometry using USNO-B1 stars:
t_mid (UT) exp_t t_mid - t0 (s) R
-----------------------------------------------------------------
05:00:24.3 5 x 10 s 94.5 R = 18.25 +- 0.29
05:02:14.5 5 x 20 s 204.7 R = 18.30 +- 0.21
Analysis is ongoing.
GCN Circular 4731
Subject
GRB 060210 : Xinglong and Lulin optical limit
Date
2006-02-10T12:09:44Z (19 years ago)
From
Yuji Urata at RIKEN <urata@crab.riken.go.jp>
W. Zhou (BAO), C.S. Lin (NCU) Y. Urata (RIKEN), K.Y. Huang (NCU) and
Y. Qiu (BAO) on behalf of RAFON report:
"The 0.8-m telescope at Xinglong Observatory, China and 1.0-m
telescope at Lulin Observatory, Taiwan started to observe GRB 060210
afterglow (Fox et al. # 4723; Li #4725) at 10.73 UT (~ 5.75 hours
after burst) and 11.07 UT (~6.08 hours), respectively. No source was
detected at afterglow position of our R and I images. Compare with
USNO-B1.0, 3-sigma limiting magnitude are summarized as below :
Delay time (hour) Filter Exp. limit site
Mean time (SN=3)
---------------------------------------------------------------------
5.79 R 600s x 1 19.5 Xinglong
5.97 I 600s x 1 18.7 Xinglong
6.18 R 300s x 3 20.8 Lulin
6.46 I 300s x 3 20.0 Lulin
This message may be cited."
GCN Circular 4733
Subject
GRB060210: Swift XRT Refined Analysis
Date
2006-02-10T13:36:53Z (19 years ago)
From
Andy Beardmore at U Leicester <apb@star.le.ac.uk>
A.P. Beardmore, S. Mateos, K.L. Page (UL), D.N. Burrows (PSU) report on
behalf of the Swift XRT Team.
We have analysed the Swift XRT data from the first 3 orbits of GRB
060210 (Beardmore et al, GCN 4724). The refined XRT position from 2.5 ks
of photon counting mode data is
RA(J2000) = 3h 50m 57.4s
Dec(J2000) = +27d 01' 36.4"
with an estimated uncertainty of 3.6 arcsec (90% containment).
This position is 29.5 arcseconds from the BAT position given in GCN 4724
and 2.0 arcseconds from the optical afterglow position reported in GCN
4726 (Mundell et al).
The fading X-ray light curve shows 2 strong flares 200 s and 385 s
after the BAT trigger. Fitting a power law to the data
after the flares gives a late time decay slope of 0.7.
The X-ray spectrum from the first orbit (T+103s to T+600s) is well fit
by an absorbed power law, with a photon index of 1.93+/-0.03 and a
column density of 1.64+/-0.3 e22 cm**-2 in the rest frame of the burst
(assuming z = 3.91; Cucchiara et al, GCN 4729), in addition to the
Galactic value of 8.5e20 cm**-2. The observed 0.2-10 keV flux is
9.4e-10 ergs cm**-2 s**-1, which corresponds to an unabsorbed flux of
1.3e-09 ergs cm**-2 s**-1.
Assuming the X-ray emission from the GRB continues to decay at the
same rate, the predicted count rate 24 hrs after the burst trigger is
0.1 count/s, which corresponds to an observed (unabsorbed) 0.2-10 keV
flux of 3.4e-12 (4.8e-12) ergs cm**-2 s**-1.
This circular is an official product of the Swift XRT Team.
GCN Circular 4734
Subject
GRB 060210: Refined analysis of the Swift-BAT burst
Date
2006-02-10T16:13:38Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
A. Parsons (GSFC), L. Barbier (GSFC), S. Barthelmy (GSFC),
J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (GSFC/UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
D. Palmer (LANL), T. Sakamoto (GSFC/ORAU), G. Sato (ISAS),
J. Tueller (GSFC)
on behalf of the Swift-BAT team:
Using the data set from T-61 to T+122 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 060210 (trigger #180977)
(Beardmore, et al., GCN 4724). The BAT ground-calculated position
is (RA,Dec) = 57.728, 27.022 deg {3h 50m 54.8s, 27d 1' 18.9"} (J2000)
+- 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 41%.
There is significant emission starting at T-45 sec, lasting all the way
to a spike at T_zero. Then there is decaying emission out to ~T+15
(with a small peak at ~T+10), and then there is flat soft emission
out to at least T+122 sec. We currently have data downlinked out to T+122,
so we can not say what the lightcurve looks like past that point, although it
seems likely there is emision beyond T+122. T90 (15-350 keV) is 46 +- 10 sec
(estimated error including systematics). We will issue a another circular
when the full data set becomes available (probably Saturday).
The time-averaged spectrum from T-45.0 to T+9.3 is best fit by
a simple power-law model. The power law index of the time-averaged spectrum
is 1.47 +- 0.07. The fluence in the 15-150 keV band is
(4.0 +- 0.2) x 10^-06 erg/cm2. The 1-sec peak photon flux measured
from T-0.02 sec in the 15-150 keV band is (2.7 +- 0.3) ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
GCN Circular 4742
Subject
GRB 060210: Optical Observations
Date
2006-02-11T17:54:44Z (19 years ago)
From
Kuntal Mishra at ARIES,Nainital,India <kuntal@aries.ernet.in>
Kuntal Misra (ARIES, Nainital) on behalf of a larger Indian GRB
collaboration
We observed the field of GRB 060210 (swift trigger = 180977) using the 1-m
reflector at ARIES, Nainital. The afterglow candidate reported by Fox and
Cenko (#GCN 4723) is seen in our R band frame of 900 sec exposure, ~8.8
hrs after the burst, at a magnitude of 20.5 +/- 0.2 in comparison to four
nearby USNO-B1.0 stars.
GCN Circular 4746
Subject
GRB060210: Swift/UVOT Upper Limits
Date
2006-02-11T23:29:28Z (19 years ago)
From
Peter Brown at PSU <pbrown@astro.psu.edu>
P. J. Brown (PSU), A. Beardmore (U Leicester),
P. Schady (PSU/UCL-MSSL), N. Gehrels (GSFC)
on behalf of the Swift/UVOT team report:
The Swift/UVOT began taking data on the field
of GRB 060210 at 05:00:28 UT on 2006-02-10,
approximately 98 s after the BAT trigger
(Beardmore et al., GCN 4724). No source is
detected in the refined XRT error circle
(Beardmore et al., GCN 4733) or at the position
of the afterglow identified by Fox & Cenko (GCN 4723)
in either the 200s finding chart images or summed
images down to the following 3-sigma magnitude
upper limits:
Filter T_range(s) Exp(s) 3sigUL(mag)
V 98-297 200 18.9
V 98-17151 1574 20.1
B 305-504 200 19.9
B 305-28728 2557 21.3
U 3750-27815 1594 20.6
UVW1 606-12060 1289 20.8
UVM2 582-17970 1402 21.1
UVW2 535-23754 2231 21.5
White 510-29539 2170 21.4
These magnitudes are uncorrected for
Galactic extinction; E(B-V) = 0.09.
These non-detections are consistent
with the spectrum described by
Cucchiara, Fox & Berger (GCN 4729)
GCN Circular 4748
Subject
GRB 060210: Further refined analysis of the Swift-BAT burst
Date
2006-02-12T00:57:32Z (19 years ago)
From
Takanori Sakamoto at NASA/GSFC <takanori@milkyway.gsfc.nasa.gov>
T. Sakamoto (GSFC/ORAU), L. Barbier (GSFC), S. Barthelmy (GSFC),
J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
D. Palmer (LANL), A. Parsons (GSFC), G. Sato (ISAS), J. Tueller (GSFC),
A. Beardmore (U Leicester)
on behalf of the Swift-BAT team:
Using the data set from T-299.8 to T+302.2 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 060210
(trigger #180977) (Beardmore, et al., GCN 4724; Parsons, et al., GCN 4734).
The BAT ground-calculated position is (RA,Dec)
= 57.729, 27.024 deg {3h 50m 55.1s, 27d 1' 27.5"} (J2000)
+- 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.
The mask-weighted lightcurve shows many peaks with significant emission
peaks starting at T-230 sec and the last peak at T+200. We caution that
this on-going activity is a significant fraction of the t-300 to T+300 sec
data interval we have received so far. This burst may have earlier or
later activity. The main activity is from T-75 to T+20 sec with the
brightest peak at T_zero.
T90 (15-350 keV) is (255 +- 10) sec (estimated error including systematics).
The time-averaged spectrum from T-227.5 to T+205.8 is best fit by
a simple power-law model. The power law index of the time-averaged
spectrum is 1.52 +- 0.09. The fluence in the 15-150 keV band is
(7.7 +- 0.4) x 10^-06 erg/cm2. The 1-sec peak photon flux measured
from T+0.00 sec in the 15-150 keV band is (2.8 +- 0.3) ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
[GCN OPS NOTE(11feb06): Per author's request, the Beardmore author was added.]
GCN Circular 4753
Subject
GRB 060210: ARC NIR Detection of Afterglow and Possible Host Galaxy
Date
2006-02-13T04:27:48Z (19 years ago)
From
Don Lamb at U.Chicago <lamb@oddjob.uchicago.edu>
GRB 060210: ARC NIR Detection of Afterglow and Possible Host Galaxy
F. Hearty (Colorado), M. Bayliss (Chicago), D. Q. Lamb (Chicago), R.
McMillan (APO), B. Ketzeback (APO), J. Barentine (APO), J. Dembicky
(APO), and D. G. York (Chicago) report:
We observed the afterglow (Fox and Cenko, GCN 4723; Li, GCN 4725, 2727;
Williams and Milne, GCN 4728, 4730; Misra, GCN 4742) of GRB 060210, a
bright burst localized by Swift (Beardmore et al. GCN 4724, 4733;
Takamoto et al. GCN 4748), on the night of February 10, using NIC-FPS
on the ARC 3.5-meter telescope at Apache Point Observatory. The
observation began at 2.65 UT on 11 February (21.75 hours after the
burst) and ended at 3.35 UT on 11 February (22.37 hours after the
burst). The observation consisted of a series of 90 20-second
exposures in Ks. Using these exposures, we have constructed a stacked
image of the GRB field, corresponding to a 30-minute exposure. Further
20-second exposures amounting to a total of 3300 seconds of exposure
were taken immediately following this and are being processed.
We detect an object at greater than the 5-sigma confidence level at the
location of the optical afterglow to within 0.5". The PSF of the
object overlaps with that of an adjacent extended source, but appears
to be consistent with that of a point source. We identify the object
as the NIR afterglow of GRB 060210. We measure Ks = 19.3 � 0.2 mag,
calibrated relative to the 2MASS stars in the field.
We also detect an extended object centered 2"-3" to the north and
immediately adjacent to the afterglow at Ks = 20.2 � 0.3 mag, which may
be the host galaxy of the burst.
NIC-FPS is currently in its commissioning phase.
GCN Circular 4761
Subject
GRB 060210: Radio Observations
Date
2006-02-14T18:17:12Z (19 years ago)
From
Dale A. Frail at NRAO <dfrail@nrao.edu>
Dale A. Frail (NRAO) reports on behalf of a larger collaboration:
"We used the Very Large Array to observe the GRB060210 (GCN 4724; GCN
4733; GCN 4734) at a frequency of 8.46 GHz on 2006 February 14.16 UT.
No radio emission is detected within the +/-0.5 arcsecond error radius
of the optical afterglow (GCN 4726) with a 3-sigma limit of 72 uJy.
No further observations are planned.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."
GCN Circular 5147
Subject
GRB 060210: Jet Break in the XRT light curve
Date
2006-05-18T00:59:16Z (19 years ago)
From
Xinyu Dai at Ohio State U <xinyu@astronomy.ohio-state.edu>
X. Dai and K. Z. Stanek (Ohio State Univ.)
We analyzed the Swift-XRT light curve of GRB 060210 (Beardmore et al. 2006
GCN 4724). We added new data points to the X-ray light curve presented in
Stanek et al. 2006 (astro-ph/0602495 v1) up to 1.e6 sec after
the BAT trigger. We detected a smooth jet break (t_j = 7.9^{+2.2}_{-1.6}
hr, observed) with the extended XRT light curve.
We fitted both a single power-law and a broken power-law model to the XRT
light curve from 3.e3 sec to 1.e6 sec after the BAT trigger. For the
single power-law model we found alpha=1.09 and chi^2(dof) = 292.3(69).
For the broken power-law model we found alpha1 = 0.7, alpha2 = 1.4, t_j =
7.9 hr, and chi^2(dof) = 64.8(67). We note that the power-law decay index
for the X-ray light curve before the jet break (alpha1 ~ 0.7) is not
consistent with the optical index (alpha_o ~ 1.3, Stanek et al. 2006
astro-ph/0602495). The XRT light curve for GRB 060210 is at
http://www.astronomy.ohio-state.edu/~xinyu/grb/060210.jpg
This message may be cited.