GRB 060111B
GCN Circular 4487
Subject
GRB 060111B: Swift detection of a burst
Date
2006-01-11T20:53:53Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
M. Perri (ASDC), S. Barthelmy (GSFC), P. Boyd (GSFC), D. Burrows (PSU),
J. Cummings (GSFC/NRC), N. Gehrels (GSFC), C. Gronwall (PSU),
J. Kennea (PSU), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
F. Marshall (GSFC), D. Palmer (LANL), T. Sakamoto (GSFC)
on behalf of the Swift team:
At 20:15:43 UT, Swift-BAT triggered and located GRB 060111B (trigger=176918).
The spacecraft slewed immediately. The BAT on-board calculated location is
RA,Dec 286.337d,+70.360d {19h 05m 21s,+70d 21' 35"} (J2000), with an
uncertainty of 3 arcmin (radius, 90% containment, stat+sys).
The BAT light curve shows a main peak with a total duration of at least 25 sec.
There is a possible second peak at T+55 sec. The peak count rate was
~2000 counts/sec (15-350 keV), at ~2 seconds after the trigger.
XRT began observing the field at 20:17:02 UT, 79 seconds after the BAT trigger.
On-board centroiding found a previously uncatalogued fading X-ray source
in the field of view at the following coordinates:
RA(J2000) = 19 05 42.3
Dec(J2000)= 70 22 37
This location is 124 arcseconds from the BAT position. The estimated
uncertainty is 8 arcseconds (90% confidence radius), including
a systematic error of about 5 arcseconds due to an XRT boresight offset not
currently corrected on-board. The initial flux was 1.7e-09 ergs/cm2/s (0.2-10 keV).
UVOT took a finding chart exposure of 200 seconds with the B filter
starting 84 seconds after the BAT trigger. There is a candidate
afterglow in the list of sources generated on-board at (RA,DEC) (J2000)
of (286.4270,70.3760) or (19h 05m 42.48s,+70d 22' 33.6") with a 1-sigma
error radius of about 0.5 arc sec. This position is 3.6 arc sec. from
the center of the XRT error circle. The estimated V magnitude is 17.2
with a 1-sigma error of about 0.5 mag. No correction has been made for
the expected visual extinction of about 0.4 magnitudes. This source
was detected in a 200 sec B finding chart image taken beginning at
20:20:34 UT with a B magnitude of 19.55. We did not receive the V finding
chart through TDRSS, so are unable to confirm the V magnitude from the
V parameterized source list.
GCN Circular 4488
Subject
GRB 060111B: ROTSE-III Detection of Optical Counterpart Flare
Date
2006-01-11T21:25:14Z (19 years ago)
From
Sarah Yost at U.Michigan <sayost@umich.edu>
S.A. Yost, F. Yuan, H. Swan, C. Akerlof (U Mich), report on behalf of
the ROTSE collaboration:
ROTSE-IIId, located at the Turkish National Observatory at Bakirlitepe,
Turkey, responded to GRB 060111B (Swift trigger 176918). The first image
was at 20:16:12 UT, 29 s after the burst (9 s after the GCN notice
time). The unfiltered images are calibrated relative to USNO A2.0.
We detect an optical flare at the position of the UVOT optical
counterpart (GCN 4487). It was observed initially at 13.0 mag, fading at
least as rapidly as ~ t^-2.6. We detect it in 3 5-sec images and it has
faded to or below the limiting magnitude of 15.5 in the 4th image at 69
sec post-burst.
start UT mag mlim(of image)
----------------------------------
20:16:12 13.0 15.2
20:16:52 >~15.5 15.5
A jpeg image is available at
http://www.rotse.net/images/gsb176918_3d00_img.jpg
GCN Circular 4489
Subject
GRB 060111B: Gualba observatory limit
Date
2006-01-11T23:36:38Z (19 years ago)
From
Martin Jelinek at Inst.Astrophys.Andalucia,Granada <mates@iaa.es>
Albert Sanchez Caso (Gualba observatory, Spain),
Martin Jelinek and Alberto J. Castro-Tirado
(IAA CSIC Granada) on behalf of a larger colaboration
report:
We have observed the field of GRB060111B (Perri et al., GCN
4487) with a 12" telescope at Gualba observatory in Spain. We
do not detect the afterglow seen by Yost et al. (GCN 4488) on
our 30x30s R-band combined image with mid-exposure time
21:59:40 UT (i.e. ~1.75h after the GRB) and 3-sigma limit 19.2.
No further observations are expected from spanish ground-based
telescopes due to technical and weather constraints.
This message may be cited.
GCN Circular 4492
Subject
GRB 060111B: Refined analysis of the Swift-BAT burst
Date
2006-01-12T03:10:05Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
J. Tueller (GSFC), L. Barbier (GSFC), S. Barthelmy (GSFC),
J. Cannizzo (GSFC-UMBC), L. Cominsky (Sonoma State U.),
J. Cummings (GSFC/NRC), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Hullinger (GSFC/UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/NRC),
G. Sato (ISAS)
on behalf of the Swift-BAT team:
Using the partial data set (T-60.2 to T+122.9 sec) from the recent telemetry
downlink, we report further analysis of BAT GRB 060111 (trigger #176918)
(Perri, et al., GCN 4487). The BAT ground-calculated position is
RA,Dec = 286.460,+70.382 deg {19h 5m 50.4s,+70d 22' 54.0"} (J2000)
+- 1.6 arcmin, (radius, sys+stat, 90% containment). The partial coding was 29%.
The mast-weighted lightcurve shows two peaks. The first one starts at T-4 sec,
peaks at T+1, and extends out to T+28 sec. The second, smaller peak starts
at T+53, peaks at T+55, and is over by T+62 sec. T90 (15-350 keV) is
59 +- 1) sec (estimated error including systematics).
The power law index of the time-averaged spectrum (T-2 to T+63 sec)
is 1.04 +- 0.17. The fluence in the 15-150 keV band is
(1.6 +- 0.1) x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+0.36 sec in the 15-150 keV band is 1.4 +- 0.3 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
GCN Circular 4493
Subject
GRB060111B: RTT150, possible host galaxy
Date
2006-01-12T06:10:18Z (19 years ago)
From
Irek Khamitov at TUG <irekk@tug.tug.tubitak.gov.tr>
I. Khamitov, K. Uluc, Z. Aslan (TUG), U. Kiziloglu (METU),
E. Gogus (Sabanci Uni.), T. Saygac, O. Onal (Ist. Uni.),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Bikmaev, N. Sakhibullin (KSU/AST)
report:
We observed field around position of optical counterpart (Perri et
al., GCN4487, Yost et al, GCN4488) of GRB060111B (Swift trigger 176918)
with Russian-Turkish 1.5-m telescope (RTT150, Bakyrlytepe, TUBITAK
National Observatory, Turkey), starting at Jan. 12, 02:11UT, i.e.
~5.9 hours after the burst.
A series of frames (13*300s exposures in R bands) were taken. We did
not detect OT, but detect an extended source on about 5 arcsec NW from OT
position with coordinates:
RA= 19h05m43.0s (J2000.0)
DEC=+70d22'29."8 (J2000.0)
Using USNO-B1 stars we estimate the following magnitude for this
source: R=20.52+/-0.03, and limiting magnitude of combined image as:
R~22.6
The finding chart can be found at:
http://www.tug.tubitak.gov.tr/~irekk/grb/grb060111b/grb060111B.JPG
This message may be cited.
[GCN OPS NOTE(12jan06): See correction in Circular 4494.]
GCN Circular 4495
Subject
GRB 060111B: TAROT optical observation
Date
2006-01-12T14:22:29Z (19 years ago)
From
Alain Klotz at CESR-CNRS <Alain.Klotz@free.fr>
Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report:
We imaged the field of GRB 060111B detected by SWIFT
(trigger 176918) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.
First image was acquired 28s after the GCN trigger
(8s after the notice). The field elevation decreased
from 28 degrees above horizon and weather conditions
were good.
We detected the OT source mentioned by Yost et al.
(GCNC 4488) at the position (+/- 0.6 arcsec):
RA(J2000.0) = 19 05 42.46
DEC(J2000.0) +70 22 32.3
OT was R~13.8 at 28s after GRB with a fading rate
t^-1.74 (+/-0.1) until 200s.
Magnitudes were estimated with the nearby USNO-B1
star: 1603-125792 (R=15.00).
This message may be cited.
GCN Circular 4496
Subject
GRB 060111B: MITSuME detection of optical afterglow
Date
2006-01-12T14:55:54Z (19 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 060111B (Perri et al. GCN 4487,
Tueller et al. GCN 4492) with the three-color MITSuME 50 cm telescope
at Okayama, Japan starting at 20:26:18 UT (T_burst+10.6 min) for an
effective exposure of 45 min (60sec x 45).
Comparison of the two stacked images
at midtime 20:28:56 UT (T_burst+13.2min, exp=60sec x5) and
at midtime 20:56:26 UT (T_burst+40.7min, exp=60sec x5)
revealed a fading object at the same location in the Rc and Ic band
images. The coordinates of the fading object are:
RA 19:05:42.47, DEC +70:22:33.1 (error = 0.3 arcsec)
We identify this object as the optical afterglow of GRB 05111B for the
following reasons:
1) these coordinates are consistent with those of the UVOT afterglow
candidate by Perri et al. (GCN 4487), and
2) while we do not confirm the possible host galaxy noted by Khamitov
et al. (GCN 4493) in our images, it is not likely to confuse our
identification as it is 4.2 arcsec away.
The magnitudes of the OT at midtime 20:28:56 UT (T_burst+13.2min) were
following:
$B!!(Bg': > 19.1 (3 sigma detection limit)
Rc: 18.9 +/- 0.4
Ic: 18.3 +/- 0.4
The Rc and Ic magnitudes were calibrated with the R2 and I2 magnitudes
of the USNO-B1.0 stars. The g' magnitudes was derived from the NOMAD
B, V magnitudes using the formula by Smith et al. (2002).
The images obtained at Okayama can be viewed at
http://bragi.oao.nao.ac.jp/support/telescope/grb50/images/GRB060111B.pdf"
GCN Circular 4498
Subject
GRB 060111B: Swift XRT refined analysis
Date
2006-01-12T18:37:21Z (19 years ago)
From
Matteo Perri at ISAC/ASDC <perri@asdc.asi.it>
M. Perri (ASDC), A. Moretti (OAB), D. N. Burrows (PSU), R. Fink (GSFC),
M. Ajello (MPE) report on behalf of the Swift XRT team:
We have analyzed the first 6 orbits of XRT data from GRB 060111B (trigger
176918, GCN 4487). A ~13 ks Photon Counting mode image provides a refined
XRT position:
RA(J2000) = 19h 05m 42.23s,
Dec(J2000) = +70d 22m 35.8s
with an uncertainty of 3.6 arcsec (90% containment). This position is 1.1
arcsec away from the on-board XRT position (GCN 4487) and includes the
latest
XRT boresight correction. This position is 45 arcsec from the refined BAT
position (Tueller et al., GCN 4492) and 3.0 arcsec from the optical
afterglow
reported by Yanagisawa et al. (GCN 4496).
The X-ray light curve can be fit with a broken power-law with an initial
decay slope of -4.0+/-0.4, a break at T+139+/-7 s, and a post-break slope
of -1.1+/-0.1.
A power-law fit to the X-ray spectrum from T+88s to T+425s gave a photon
index of 2.1+/-0.3 and a column density of (2.0+/-0.9)e21 cm**-2. We note
the Galactic hydrogen column density in the direction of the burst is
7.1e20cm**-2.
If the burst continues decaying at the current rate we estimate an XRT
count rate of 0.004 counts/s at T+24hr, which corresponds to an
observed 0.3-10.keV flux of 2e-13 ergs cm**-2 s**-1.
GCN Circular 4571
Subject
GRB 060111B: Suzaku WAM observation of the prompt emission
Date
2006-01-24T17:36:05Z (19 years ago)
From
Kazutaka Yamaoka at Aoyama Gakuin U <yamaoka@phys.aoyama.ac.jp>
G.Sato, K.Nakazawa, T.Takahashi (ISAS/JAXA),
K.Yamaoka, S.Sugita (Aoyama Gakuin U.), Y.Terada (RIKEN),
M.Ohno, T.Takahashi, Y.Fukazawa (Hiroshima U.),
K.Abe, Y.Endo, S. Hong, K.Onda, M.Tashiro (Saitama U.),
R.Miyawaki, M.Kokubun, K.Makishima (Univ. of Tokyo)
and the HXD-II team
The long burst, GRB 060111B (Swift-BAT trigger #176918;
Perri et al., GCN 4487), triggered the Suzaku Wide-band
All-sky Monitor (WAM) which is sensitive to an energy band
of 50 keV - 5 MeV at 20:15:41 (UT).
The WAM light curve exhibits a double peak structure
with a duration (T90) of 25 seconds.
The fluence in 100 - 1000 keV was (5.6 +/- 0.8)X10^-6 erg/cm2.
The 1-s peak flux was 1.0 +/- 0.2 photons/cm2/s
in the same energy range.
Preliminary result shows that the time-averaged spectrum
is well fitted by a single power law with a photon index
of 1.5 +/- 0.3.
All the quoted errors are at statistical 90% confidence level.
The WAM in-flight calibration is still under way, and systematic
errors, such as the flux calibration uncertainties of about 20%,
are not included in the errors.
The WAM light curve of this event is available at
http://www.astro.isas.ac.jp/suzaku/research/HXD-WAM/WAM-GRB/grb/grb_table.html
Further detailed analysis and the refinement are in progress.
GCN Circular 5820
Subject
GRB 060111B: Swift UVOT Refined Magnitudes
Date
2006-11-13T14:13:58Z (19 years ago)
From
Stephen Holland at USRA/NASA/GSFC/SSC <sholland@milkyway.gsfc.nasa.gov>
S. T. Holland (NASA/GSFC & USRA) reports on behalf of the UVOT team:
The UVOT data for GRB 060111B (Perri, et al. 2006, GCN
Circ. 4487) on January 11, 2006 has been reanalysed. We find the
following magnitudes and 3-sigma upper limits in the early UVOT
exposures. The start and stop times are relative to the BAT trigger
time, 20:15:43 UT.
Filter Start Stop Exposure Mag Err
(s) (s) (s)
Early Exposures
V 83 282 197 17.4 0.1
V 542 562 19 18.0 3-sigma upper limit
V 831 1031 197 19.4 3-sigma upper limit
B 289 489 197 20.5 3-sigma upper limit
B 638 658 19 18.9 3-sigma upper limit
U 614 633 19 18.4 3-sigma upper limit
UVW1 590 610 19 18.0 3-sigma upper limit
UVM2 6017 6217 197 20.0 3-sigma upper limit
UVW2 518 538 19 17.5 3-sigma upper limit
White 494 514 19 19.4 3-sigma upper limit
Coadded Esposures
V 542 52472 2435 21.0 3-sigma upper limit
B 638 70515 5861 22.4 3-sigma upper limit
U 614 69818 6008 22.0 3-sigma upper limit
UVW1 590 68905 4089 22.2 3-sigma upper limit
UVM2 566 53170 3663 22.2 3-sigma upper limit
UVW2 519 58952 3662 22.4 3-sigma upper limit
White 494 64734 3696 22.2 3-sigma upper limit
The values quoted above are not corrected for the expected Galactic
extinction of E_{B-V} = 0.11 mag (Schlegel et al. 1998).
These data supercede those reported in GCN Circ. 4487. We note
that the B-band detection reported in GCN Circ. 4487 is not real, and
the initial finding chart was taken with the V filter, not the B
filter as previously reported. The UVOT team apologizes for these
errors.