GRB 060110
GCN Circular 4755
Subject
GRB060110: optical observations
Date
2006-02-13T15:08:38Z (20 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
D. Sharapov (MAO, and NOT La Palma), M. Ibrahimov, (MAO), A. Pozanenko
(IKI) and V. Rumyantsev (CrAO) on behalf of larger GRB follow up
collaboration report:
We observed error box of GRB060110 (Zane et al., GCN 4463) with 1.5m
telescope of Maidanak Astronomical Observatory in R-band on Jan. 10 between
(UT) 18:30 and 19:18 under bad weather conditions. We do not detect OT
identified by Bloom (GCN 4466, 4471). Limiting magnitude is based on USNO
B1.0 is following:
Obs. time, Exp., Mag.(UL), Seeing
(UT) (s)
Jan. 10 18:30-19:18 30x60 18.8 1.8"
GCN Circular 4525
Subject
GRB 060110: XRT position and analysis
Date
2006-01-16T17:09:49Z (20 years ago)
From
Kim Page at U.of Leicester <kpa@star.le.ac.uk>
K.L. Page, M.R. Goad, A.P. Beardmore (U. Leicester), D.N. Burrows (PSU),
A. Smale (NASA HQ) and L. Cominsky (Sonoma State U.) report on behalf of
the Swift-XRT Team:
Swift performed a Target of Opportunity observation of GRB 060110 once it
came out of the Moon constraint, approximately 2.4e5 seconds (2.8 days)
after the BAT trigger (Zane et al., GCN 4463).
A faint, fading, uncatalogued X-ray source was identified at a position
of:
RA(J2000) = 04h 50m 57.85s
Dec(J2000) = +28d 25' 53.88"
with an uncertainty of 4.1 arcsec (90% containment, including the latest
XRT boresight correction). This is 0.7" from the position given by Torii
in GCN 4468 for a potential, low signal-to-noise source and 6.9" from the
IR position in GCN 4467 (Bloom & Li). The XRT position is also 21 arcsec
from the refined BAT position (Parsons et al., GCN 4477)
Using 41.7 ks of data, the source is fading with a decay slope of alpha =
2.0 +/- 1.2. The spectrum can be modelled with a power-law of Gamma = 2.27
+/- 0.58, with absorption consistent with the Galactic value in this
direction (2.4e21 cm^-2). The time averaged 0.3-10 keV observed
(unabsorbed) flux between 2.4e5 and 4.8e5 seconds is 6.45e-14 (1.13e-13)
erg cm^-2 s^-1.
GCN Circular 4499
Subject
GRB 060110: KAIT observations
Date
2006-01-13T06:54:33Z (20 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 GRB060110 detected with Swift
(Trigger 176702; Zane et al. GCN 4463). A series of
images was automatically obtained starting at 08:02:35 UT
(78s after the burst). The OT identified by Bloom (GCN
4471) was outside the field of view for the first several
images. Our first image containing the OT was a 120-s
unfiltered image started at 08:14:24 UT (787s after the burst),
and the OT was at mag 17.9 +/- 0.1 when calibrated to 65 nearby
USNO B1.0 stars.
GCN Circular 4491
Subject
GRB 060110: MARGE observations
Date
2006-01-12T01:50:15Z (20 years ago)
From
Heather Swan at U.of Michigan/ROTSE <hflewell@umich.edu>
H. Swan (U Mich), I. Smith (Rice), C. Akerlof (U Mich), S. Yost (U
Mich), and M. Skinner (Boeing) report on behalf of the MARGE
collaboration:
The AEOS Burst Camera (ABC) on the AEOS telescope, located at the
Maui Space Surveillance System on Haleakala, observed the fading
counterpart to GRB060110 (Swift trigger 176702 (GCN 4463)). The
images are unfiltered, 10s exposures which started at 08:05:19.18 UT
(~5 minutes after the trigger) and ended at 09:37:53.68. Because the
FoV of the ABC is 6 arc-minutes across, and because the OT was
located outside of the BAT error box, the first image containing the
OT occurred at 09:06:50.
After a comparison of our images with the USNO B 2.0 R catalog, we
see the OT found by Bloom (GCN 4471). A preliminary analysis gives an R
magnitude of approximately 19.0 at 09:20:58.48 UT. Combined with the
detection reported by ROTSE-III (GCN 4472), we find a power law decay
with an exponent, alpha, of about 0.7.
GCN Circular 4478
Subject
GRB 060110: Mitsume optical observations
Date
2006-01-11T04:30:40Z (20 years ago)
From
Nobuyuki Kawai at Tokyo Tech <nkawai@hp.phys.titech.ac.jp>
K. Yanagisawa (OAO/NAOJ), H. Toda and N. Kawai (Tokyo Tech) report
on behalf of the Mitsume collaboration:
"We have observed the field of GRB 060110 (Zane et al. GCN 4463,
Parsons et al. GCN 4477) with the three-color Mitsume 50 cm
telescopes at Okayama, Japan in g', Rc, and Ic bands starting at
9:58 UT (T_burst+2.0h) until 10:12 UT (T_burst+2.2h) for an effective
exposure of 10 min (60sec x 10). The observing condition was not good
due to clouds and the position near the moon.
In the co-added image, we could not confirm the OT candidate (Torii
GCN 4468; Bloom et al. GCN 4471, Rujopakarn et al. GCN 4472, Tanvir et
al. GCN 4473, Wozniak et al. GCN 4474) down to the following 3-sigma
magnutude limits:
g': 17.6
Rc: 18.0
Ic: 17.3
The images obtained at Okayama can be viewed at
http://bragi.oao.nao.ac.jp/support/telescope/grb50/images/GRB060110A.pdf"
GCN Circular 4477
Subject
GRB 060110: Swift-BAT refined analysis
Date
2006-01-11T02:57:21Z (20 years ago)
From
Takanori Sakamoto at NASA/GSFC <takanori@milkyway.gsfc.nasa.gov>
A. Parsons (GSFC), 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),
J. Nousek (PSU), D. Palmer (LANL), T. Sakamoto (GSFC/ORAU),
G. Sato (ISAS), M. Tripicco (GSFC-SSAI), J. Tueller (GSFC),
on behalf of the Swift-BAT team:
Using the data set from T-299.7 to T+95 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 060110
(trigger #176702) (Zane, et al., GCN 4463).
The BAT ground-calculated position
is (RA,Dec) = 72.738, 28.427 {4h 50m 57.2s, 28d 25' 35.7"} (deg; J2000)
+- 0.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
The mask-tagged lightcurve shows a single FRED like peak starting from
T-2 sec. T90 (15-350 keV) is (17 +- 2) sec
(estimated error including systematics).
Due to viewing constraints, Swift slewed away from this burst after
95 seconds, so no information on any possible later emission is
available. There is no sign of emission after the single FRED peak,
however.
Over the full burst interval (T-3.7 to T+20.4 sec),
the power law index of the time-averaged spectrum is 1.63 +- 0.08.
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 (1.9 +- 0.2) ph/cm2/sec. All the quoted errors are at the 90%
confidence level.
GCN Circular 4473
Subject
GRB 060110: UKIRT K-band observations
Date
2006-01-10T15:35:42Z (20 years ago)
From
Nial Tanvir at IofA U.Cambridge <nrt@ast.cam.ac.uk>
N.R. Tanvir, A.J Levan (U. Hertfordshire), F. Nakata (U. Durham)
and L. Fuhrman (JACH) report on behalf of a larger collaboration:
We observed the field of GRB 060110 with UKIRT/WFCAM. A 21 min K-band
exposure was made in ~1.1 arcsec seeing, starting Jan 10 08.47 UT
(ie. approximately 45 minutes post-burst).
The source reported by Bloom et al. (GCN 4465) is clearly detected
in our images, and provisional photometry relative to nearby 2MASS stars
gives K=13.75+/-0.10. Compared to the magnitudes reported by Bloom (GCN
4471), the source appears to have faded, although the errors are such
that a constant brightness is not strongly rejected.
Further observations are in progress.
GCN Circular 4472
Subject
GRB 060110: ROTSE-III Confirmation of Optical Counterpart
Date
2006-01-10T14:31:47Z (20 years ago)
From
Wiphu Rujopakarn at U Michigan/ROTSE <wiphu@umich.edu>
W. Rujopakarn (U Mich), T.A. McKay (U Mich), F. Yuan (U Mich), H. Swan
(U Mich), D.A. Smith (Guilford), S. A. Yost (U Mich) report on behalf
of the ROTSE collaboration:
ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
060110 (Zane al. GCN 4463). The first image was at 08:01:44.8 UT, 27.1
s after the burst (9 s after the GCN notice time). Imaging is shallow
due to the brightness of the Moon. The unfiltered images are calibrated
relative to USNO A2.0 R-band. We detect the source reported by Bloom
(GCN 4471) near the limiting magnitude of the early coadded exposures.
It was ~15.5 mag at about 50 s post-trigger, in an image at limiting
magnitude 16.0
Further data analyses are in progress.
GCN Circular 4471
Subject
GRB 060110: IR Candidate Afterglow
Date
2006-01-10T12:29:54Z (20 years ago)
From
Josh Bloom at UC Berkeley <jbloom@astron.berkeley.edu>
J. S. Bloom (UC Berkeley) reports:
"We have conducted further analysis on the source noted in GCNs
4465/4467 and suggest that, while the source is formally outside of
the 90% containment BAT error circle (e.g. Torii GCN 4468), there is
evidence this is the (bright) afterglow of GRB 060110 (Zane al. GCN
4463). This follows from a few lines of evidence:
[1] evidence for fading. We created two mosaic epochs (1: 08:06:52
-- 08:11:32; 2: 08:12:46 -- 08:30:36) and found that the average
brightness decreased by ~0.12 mag in JHKs. We believe that this
fading is significant but photometry is complicated by large
background gradients owing to the proximity to the Moon.
[2] no bright minor planets are nearby this position (see GCN 4467).
[3] no evidence for apparent motion between the epochs (~<1"/hr)
and point-like PSF.
All the other minor planets in the field have significant
motions, particularly in RA (>10"/hr)
Our current astrometric solution gives a position of the afterglow
(in both epochs) to be:
04:50:57.85 +28:25:55.7
(J2000; 200 mas uncertainty). This is close to the position noted by
Torii (GCN 4468) and lends credence to their tentative R-band
detection. Photometry in the second epoch yields magnitudes J =
15.23, H = 14.25, Ks = 13.57 (absolute zp uncertainty of ~0.04 mag)."
Follow on observations are urged.
GCN Circular 4470
Subject
GRB060110, optical observation
Date
2006-01-10T11:38:20Z (20 years ago)
From
Shouta Maeno at U.of Miyazaki <shouta@astro.miyazaki-u.ac.jp>
S.Maeno,E.Sonoda,S.Masuda,Y.Nakamura,M.Yamauchi
(University of Miyazaki)
"We have observed the field covering the error circle of
GRB060110 (GCN 4463) with the unfiltered CCD camera on
the 30-cm telescope at University of Miyazaki.
The observation was started 09:32:57 UT on Jan.10.
After co-adding a set of 13 images (09:32:57 - 09:53:51 UT)
of 30 sec exposures, we have compared with the USNO A2.0 catalog.
Preliminary analysis shows there is no new source brighter
than 17.3mag."
GCN Circular 4469
Subject
GRB 060110: Super-LOTIS observations
Date
2006-01-10T10:48:03Z (20 years ago)
From
Peter A. Milne at Super-LOTIS <pmilne@as.arizona.edu>
P.A.Milne (Steward Obs),
on behalf of the Super-LOTIS GRB team reports:
The error region of GRB 060110 (Zane et al. GCN 4463) was
observed by the 60cm Super-LOTIS telescope at Kitt Peak, AZ..
Starting at 08:01:55 UT (38 s after the burst), 5 ten second
exposure images, 5 twenty second exposure images and 30 sixty second
exposure images were obtained. All images were obtained in the
R band.
Comparisons between permutations of these images do not reveal a
fading source in any image. The proximity of the moon led to very
poor image quality, particularly in the portion of the image that
contains the location of the candidate NIR counterpart
(Bloom GCN 4465). A preliminary upper limit of about 16.0 for an
object at that location, is based upon USNO-B magnitudes for two
nearby stars that were not detected.
Further analysis of these images will be performed.
GCN Circular 4468
Subject
GRB 060110: Optical observation
Date
2006-01-10T10:36:04Z (20 years ago)
From
Ken ichi Torii at RIKEN <torii@ess.sci.osaka-u.ac.jp>
K. Torii (Osaka U.) reports:
We investigated our early Ic band frames for the IR afterglow
candidate (Bloom, GCN 4465; Bloom and Li, GCN 4467).
In our stacked frame, we identify a low significance enhancement at
the position (J2000)
04:50:57.9 +28:25:56
with 2" uncertainty. There is no corresponding object in DSS2 red.
The Ic band magnitude in our frame corresponds to ~16.3 mag. As of
this writing, we are not confident if this is an astrophysical source
or a noise, due to its low SN.
We note that this position is about 7" north of that given in GCN
4467. We also note that the position given in GCN 4467 is very close
to, but formally outside of, the BAT 3' error radius.
===
GCN Circular 4467
Subject
GRB 060110: Correction
Date
2006-01-10T09:46:58Z (20 years ago)
From
Josh Bloom at UC Berkeley <jbloom@astron.berkeley.edu>
J. S. Bloom and W. Li (UC Berkeley) report:
The correct position from GCN 4465 should be (J2000)
04:50:57.9
+28:25:49
We thank P. Milne for pointing out the 10 hour error in RA.
We further report that a check of Minor Planets (1) in the vicinity
of GRB 060110 shows no known bright (V < 19) sources in the field at
the time of the IR observations.
A comparison of the JHK imaging with the DSS is now posted (2).
(1) http://scully.harvard.edu/~cgi/CheckSN.COM
(2) http://astro.berkeley.edu/~jbloom/grb060110.png
(green = 2MASS sources; white box = candidate afterglow)
GCN Circular 4464
Subject
GRB 060110: Optical limit
Date
2006-01-10T09:18:38Z (20 years ago)
From
Ken ichi Torii at RIKEN <torii@ess.sci.osaka-u.ac.jp>
K. Torii (Osaka U.) reports:
The error region of GRB 060110 (Zane et al. GCN 4463) was observed by
a 0.3 m telescope in the New Mexico Skies Observatory. Starting at
08:03:39 UT (142 s after the burst), several 120 s exposures in Ic and
Rc bands were obtained.
Preliminary analysis of the two Ic frames does not reveal an
afterglow candidate brighter than about 16 mag (USNO B1.0 I mag)
within the BAT error region.
===
GCN Circular 4463
Subject
GRB 060110: Swift-BAT detection of a burst
Date
2006-01-10T08:42:15Z (20 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
S. Zane (UCL-MSSL), S. Barthelmy (GSFC), A. J. Blustin (UCL-MSSL),
N. Gehrels (GSFC), C. Markwardt (GSFC/UMD), J. Norris (GSFC),
K. Page (U Leicester), D. Palmer (LANL)
on behalf of the Swift team:
At 08:01:17 UT, Swift-BAT triggered and located GRB 060110 (trigger=176702).
The spacecraft did not slew because of the Moon observing constraint.
The BAT on-board calculated location is RA,Dec 72.741d,+28.380d
{04h 50m 58s,+28d 22' 48"} (J2000), with an uncertainty of 3 arcmin
(radius, 90% containment, stat+sys). The BAT light curve shows a single
FRED-like peak structure with a total duration of 15 sec. The peak count rate
was ~5000 counts/sec (15-350 keV), at ~2 seconds after the trigger.
We are currently in the Malindi downlink gap, so it will be at least 5 hours
before we get the full data set on this burst. This burst will remain
in the Moon observing constriant for 2.8 days.