GRB 060117
GCN Circular 4533
Subject
GRB 060117: Swift-BAT detection of a bright burst
Date
2006-01-17T07:22:11Z (19 years ago)
From
Scott Barthelmy at NASA/GSFC <Scott@lheamail.gsfc.nasa.gov>
S. Campana (INAF-OAB), S. Barthelmy (GSFC), N. Gehrels (GSFC),
C. Gronwall (PSU), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
K. Page (U Leicester), D. Palmer (LANL), M. Perri (ASDC)
on behalf of the Swift team:
At 06:50:01 UT, Swift-BAT triggered and located GRB 060117 (trigger=177666).
The spacecraft did not slew because of the Sun observing constraint.
It will come out of the Swift observing constraint on 07 Feb 2006.
The BAT on-board calculated location is RA,Dec 327.926d,-59.980d
{21h 51m 42s,-59d 58' 49"} (J2000), with an uncertainty of 3 arcmin
(radius, 90% containment, stat+sys). The BAT light curve shows
a bright multi-peak structure with a total duration of ~25 sec.
The peak count rate was ~40,000 counts/sec (15-350 keV), at ~12 seconds
after the trigger.
We note that this is within 3 arcmin of the bright (J=13.0 mag) galaxy
IRAS 21482-6015.
GCN Circular 4534
Subject
GRB 060117: nearby galaxy
Date
2006-01-17T07:39:54Z (19 years ago)
From
Nial Tanvir at IofA U.Cambridge <nrt@ast.cam.ac.uk>
N.R. Tanvir (U. Hertfordshire) notes:
The galaxy that is within 2.7 arcmin of the BAT position of GRB 060117
(GCN 4533) is at redshift z=0.042, and there are other galaxies visible
on DSS2 in the same field, which could well be at similar redshift.
Given the high luminosity of this burst, it is therefore a candidate
to be at low-redshift, and followup observations are encouraged, despite
the poor location on the sky.
GCN Circular 4535
Subject
GRB 060117: FRAM optical afterglow candidate
Date
2006-01-17T09:41:08Z (19 years ago)
From
Martin Jelinek at Inst.Astrophys.Andalucia,Granada <mates@iaa.es>
Petr Kubanek, (ASU Ondrejov, Czech Rep. and ISDC Versoix, Switzerland)
Martin Jelinek (IAA Greanada, Spain),
Michael Prouza (FZU Praha, Czech Rep.,
Martin Nekola and Rene Hudec (ASU Ondrejov, Czech Rep.)
Report:
The wide field camera of the telescope FRAM located at Pierre
Auger observatory in Malargue, Argentina, observed the field
of Swift trigger 177666 (Cmpana et al., GCN 4533) starting
123s after the GRB (10s after GCN). We detect an optical
source at coordinates:
21:51:36.1 -59:58:58 (J2000)
The object faded during few exposures from the reach of the
telescope.
Note that this object is within few arcseconds from the galaxy
LEDA 128172.
GCN Circular 4536
Subject
GRB 060117: FRAM refined analysis
Date
2006-01-17T10:50:00Z (19 years ago)
From
Martin Jelinek at Inst.Astrophys.Andalucia,Granada <mates@iaa.es>
Martin Jelinek (IAA Greanada, Spain),
Petr Kubanek, (ASU Ondrejov, Czech Rep. and ISDC Versoix, Switzerland)
Michael Prouza (FZU Praha, Czech Rep.,
Martin Nekola and Rene Hudec (ASU Ondrejov, Czech Rep.)
Report:
The observation of the GRB060117 (GCN 4533, 4534, 4535)
started with a 10s R-band exposure at 06:52:05.4 UT, i.e. 124s
after the GRB. The afterglow magnitude is 11.5+/-0.3
(calibration noise) and faded by 1.4mag during the first 120s
of observation.
The optical candidate is at a refined position:
21:51:36.13 -59:58:39.1 +/-1.5" (J2000)
We note that the originally reported position was wrong by 20"
in declination.
[GCN OPS NOTE(07apr10): As pointed out by F.Marshall, the missing
minus sign on the declination was added.]
GCN Circular 4538
Subject
GRB 060117: Refined analysis of the Swift-BAT burst
Date
2006-01-17T19:16:15Z (19 years ago)
From
Hans Krimm at NASA-GSFC <krimm@milkyway.gsfc.nasa.gov>
J. Cummings (GSFC/NRC), L. Barbier (GSFC), S. Barthelmy (GSFC)
E. Fenimore (LANL), N. Gehrels (GSFC), K. Gendreau (GSFC),
D. Hullinger (GSFC/UMD), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), P. Meszaros (PSU), J. Norris (GSFC),
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+120 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 060117 (trigger
#177666) (Campana, et al., GCN 4533). The BAT ground-calculated
position is RA,Dec = 327.917, -59.967 {21h 51m 40s, -59d 58' 1"}
(J2000) +- 1.0 arcmin, (radius, sys+stat, 90% containment). This
position includes a small correction for small BAT image distortions.
We note that this error circle formally excludes the position of IRAS
21482-6015 (GCN 4533, GCN4534). We also note that fading afterglow
discovered by the FRAM telescope group (Jelinek et al, GCN 4536) is
0.8 arc min from the center of the BAT 90% error circle. The partial
coding was 25%.
The light curve has multiple peaks, with the main peaks spanning the
time range T-1 to T+17. T90 (15-350 keV) is (16 +- 1) sec (estimated
error including systematics). There does appear to be weak emission
extending out to T+100 seconds.
The best fit to the spectral data for the time averaged period from
T-1.98 to T+26.99 seconds is a power law with an exponential cutoff.
This fit gives a photon index 1.51 +- 0.13, and Epeak of 71 +- 5 keV
(chi squared 40 for 59 d.o.f). For this model the total fluence in the
15-150 keV band is (2.04 +- 0.04) x 10^-05 erg/cm2 and the 1-sec peak
flux measured from T+11.12 sec is 48.9 +- 1.6 ph/cm2/sec. A fit to a
simple power law gives a photon index of 1.93 +- 0.03 (chi square 68
for 59 d.o.f.) All the quoted errors are at the 90% confidence level.
Using the lag-luminosity method of Norris et al. (2000),
and a lag measurement of 25 ms +- 5 ms (1 sigma; 100-350 keV
to 25-50 keV bands), yields a pseudo-redshift of z ~ 1.3 +- 0.3
(includes spectral uncertainties).
The remainder of the expected event data for this burst (from T-300 to T-60
sec and from T+120 to T+300) has not yet been received on the ground. If
we see evidence for emission after T+120 sec in these data, we will
issue another circular.
GCN Circular 4542
Subject
Konus-Wind observation of GRB 060117
Date
2006-01-18T16:24:43Z (19 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 long soft GRB 060117 (Swift-BAT trigger #177666;
Campana et al., GCN 4533; Cummings et al., GCN 4538)
triggered Konus-Wind at T0=24597.852 s UT (06:49:57.852).
The Konus-Wind light curve shows multiple peaks with a total duration of
~20 sec.
As observed by Konus-Wind the burst had
a fluence of (2.97+/-0.13)x10^-5 erg/cm2 and
peak flux measured from T+11.12 on 16 msec time scale
(1.28+/-0.18)x10^-5 erg/cm2/sec
(both in the 20 keV - 1 MeV energy range).
The time-integrated spectrum of the GRB (from T0 to T0+21.504 sec)
is well fitted (in the 20 keV - 1 MeV range)
by GRBM (Band) model for which:
the low-energy photon index is alpha = -1.519 (-0.070,+0.082),
the high energy photon index beta = -2.91(-0.50, +0.25),
the break energy E0 = 184(-30, +34) keV (chi2 = 53/59 dof).
The peak energy Ep = 89+/-5 keV.
All the quoted errors are at the 90% confidence level.
GCN Circular 4543
Subject
Correction to GCN 4542 on GRB 060117
Date
2006-01-18T16:54:51Z (19 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
V. Pal'shin on behalf of the Konus-Wind team:
The time of the measured peak flux quoted in GCN 4542 is wrong.
Actually, the peak flux was measured from T0+11.392 sec.
GCN Circular 4544
Subject
GRB 060117: pseudo-z from spectral parameters of the prompt emission
Date
2006-01-18T17:45:03Z (19 years ago)
From
Jean-Luc Atteia at Lab d Astrophys.,OMP,Toulouse <atteia@ast.obs-mip.fr>
A. Pelangeon & J-L. Atteia (LATT-OMP) report:
We have used the spectral parameters of GRB 060117
provided by Golenetskii et al. (GCNC 4542) to
compute the spectral pseudo-redshift of this burst
detected by SWIFT-BAT (Campana et al., GCNC 4533;
Cummings et al., GCNC 4538).
We find a pseudo-redshift pz= 0.45 +/- 0.2
This is significantly lower than the pseudo-redshift computed from
the lag-luminosity relation (pz=1.3, GCNC 4538, Cummings et al.).
This small pseudo-redshift suggests that the supernova associated
with GRB 060117 could be detectable.
We encourage observers to follow-up this GRB at various wavelengths
to look for the possible emergence of the supernova.
GCN Circular 4546
Subject
GRB060117 - ATCA 3/6cm radio limits
Date
2006-01-18T22:43:28Z (19 years ago)
From
Brian Schmidt at RSAA, ANU (MSSSO) <brian@mso.anu.edu.au>
Brian Schmidt (ANU), Mark Wieringa (ATNF),
Dale A. Frail (NRAO), and Alicia Soderberg (CalTech)
report on behalf of a larger collaboration
"We observed the field of GRB 061117 (GCN 4519) with the Australia
Telescope Compact Array at 4.8 and 8.6GHz beginning January 18.4 UT. We
detect no sources in a 20" box around the XRT/OT position (GCN
4522,4536) to an approximate 4 sigma limit of 0.6 mJy at both frequencies. "
We would like to thank the Director and Staff of the Australia Telescope
National Facility for obtaining these observations as part of a Target
of Opportunity Program.
GCN Circular 4547
Subject
GRB060117 - ATCA 3/6cm radio limits - correction
Date
2006-01-18T23:06:53Z (19 years ago)
From
Brian Schmidt at RSAA, ANU (MSSSO) <brian@mso.anu.edu.au>
Brian Schmidt (ANU), Mark Wieringa (ATNF),
Dale A. Frail (NRAO), and Alicia Soderberg (CalTech)
report on behalf of a larger collaboration
"We observed the field of GRB 061117 (GCN 4533, GCN 4538) with the
Australia Telescope Compact Array at 4.8 and 8.6GHz beginning January
18.4 UT. We detect no sources in a 20" box around the OT position (GCN
4536) of 21:51:36.13 -59:58:39.1 (J2000) to an approximate 4 sigma
limit of 0.6 mJy at both frequencies. "
We would like to thank the Director and Staff of the Australia Telescope
National Facility for obtaining these observations as part of a Target
of Opportunity Program.
GCN Circular 4548
Subject
GRB 060117: PROMPT Observations
Date
2006-01-19T17:49:26Z (19 years ago)
From
Melissa Nysewander at UNC,Chapel Hill <mnysewan@physics.unc.edu>
M. Nysewander, A. LaCluyze, D. Reichart, J.A. Crain, A. Foster, K. Ivarson
report on behalf of the UNC team of the FUN GRB collaboration:
We observed the error region of GRB 060117 (Campana et al., GCN 4533) with
four of the PROMPT telescopes simultaneously in Ur'Iz' beginning 18.0 hours
after the burst under the automated control of SkyNet at very high airmass.
Each exposure is 80 s long; the table below gives details of the
observations:
Filter Telescope Start (UT) Stop (UT) # Exp Total (hr)
U P2 00:47:39 02:17:47 61 1.36
r' P4 00:47:39 02:18:44 63 1.40
I P1 00:47:36 02:13:03 59 1.31
z' P5 00:47:38 02:14:16 61 1.36
We do not see the afterglow reported by Jelinek et al. (GCN 4536) in r'Iz'
to r' > 20.2, I > 21.2, and z' > 20.2 (3-sigma). The magnitudes have been
calibrated to 5 USNO NOMAD catalogue stars using the transformation
equations of Smith et al. 2002.
PROMPT is currently being built and commissioned at CTIO.
GCN Circular 4573
Subject
GRB 060117: Suzaku WAM observation of the prompt emission
Date
2006-01-24T17:45:26Z (19 years ago)
From
Kazutaka Yamaoka at Aoyama Gakuin U <yamaoka@phys.aoyama.ac.jp>
Y.Terada (RIKEN), K.Yamaoka, S.Sugita (Aoyama Gakuin U.),
M.Ohno, T.Takahashi, Y.Fukazawa (Hiroshima U.),
K.Abe, Y.Endo, S. Hong, K.Onda, M.Tashiro (Saitama U.),
G.Sato, K.Nakazawa, T.Takahashi (ISAS/JAXA), R.Miyawaki,
M.Kokubun, K.Makishima (Univ. of Tokyo) and the HXD-II team
The bright and long burst, GRB 060117 (Swift-BAT trigger
#177666; Campana et al., GCN 4533), triggered the Suzaku
Wide-band All-sky Monitor (WAM) which is sensitive to an
energy band of 50 keV - 5 MeV at 06:50:00 (UT).
The observed light curve shows multi-peak structures
with a duration (T90) of 16 seconds.
The fluence in 100 - 1000 keV was (1.5 +/- 0.1)X10^-5 erg/cm2.
The 1-s peak flux was 9.2 +/- 0.4 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 2.5 +/- 0.2.
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.