- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Tue 17 Jan 06 06:50:20 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 177666, Seg_Num: 0
GRB_RA: 327.926d {+21h 51m 42s} (J2000),
328.035d {+21h 52m 08s} (current),
327.026d {+21h 48m 06s} (1950)
GRB_DEC: -59.980d {-59d 58' 49"} (J2000),
-59.952d {-59d 57' 06"} (current),
-60.215d {-60d 12' 54"} (1950)
GRB_ERROR: 3.00 [arcmin radius, statistical only]
GRB_INTEN: 17055 [cnts] Image_Peak=2776 [image_cnts]
TRIGGER_DUR: 1.024 [sec]
TRIGGER_INDEX: 150 E_range: 25-100 keV
BKG_INTEN: 30248 [cnts]
BKG_TIME: 24583.03 SOD {06:49:43.03} UT
BKG_DUR: 8 [sec]
GRB_DATE: 13752 TJD; 17 DOY; 06/01/17
GRB_TIME: 24601.59 SOD {06:50:01.59} UT
GRB_PHI: -159.03 [deg]
GRB_THETA: 50.11 [deg]
SOLN_STATUS: 0x3
RATE_SIGNIF: 217.57 [sigma]
IMAGE_SIGNIF: 24.66 [sigma]
MERIT_PARAMS: +1 +0 +0 +0 +2 +30 -100 +0 -71 +1
SUN_POSTN: 299.06d {+19h 56m 15s} -20.75d {-20d 45' 14"}
SUN_DIST: 44.24 [deg]
MOON_POSTN: 151.77d {+10h 07m 06s} +14.87d {+14d 52' 02"}
MOON_DIST: 134.83 [deg]
MOON_ILLUM: 93 [%]
GAL_COORDS: 333.05,-45.24 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 305.78,-43.53 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Coordinates.
COMMENTS: This is a rate trigger.
COMMENTS: A point_source was found.
COMMENTS: This does not match any source in the on-board catalog.
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 148.98,-18.85 [deg].
- red DSS finding chart
ps-file
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Tue 17 Jan 06 06:53:41 UT
NOTICE_TYPE: Swift-BAT GRB Lightcurve
TRIGGER_NUM: 177666, Seg_Num: 0
GRB_RA: 327.926d {+21h 51m 42s} (J2000),
328.035d {+21h 52m 08s} (current),
327.026d {+21h 48m 06s} (1950)
GRB_DEC: -59.980d {-59d 58' 49"} (J2000),
-59.952d {-59d 57' 06"} (current),
-60.215d {-60d 12' 54"} (1950)
GRB_DATE: 13752 TJD; 17 DOY; 06/01/17
GRB_TIME: 24601.59 SOD {06:50:01.59} UT
TRIGGER_INDEX: 150
GRB_PHI: -159.03 [deg]
GRB_THETA: 50.11 [deg]
DELTA_TIME: 64.00 [sec]
TRIGGER_DUR: 1.024 [sec]
LC_URL: sw00177666000msb.lc
SUN_POSTN: 299.06d {+19h 56m 15s} -20.75d {-20d 45' 12"}
SUN_DIST: 44.24 [deg]
MOON_POSTN: 151.80d {+10h 07m 12s} +14.86d {+14d 51' 21"}
MOON_DIST: 134.82 [deg]
MOON_ILLUM: 93 [%]
GAL_COORDS: 333.05,-45.24 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 305.78,-43.53 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Lightcurve.
COMMENTS:
COMMENTS: The next comments were copied from the BAT_POS Notice:
COMMENTS: This is a rate trigger.
COMMENTS: A point_source was found.
COMMENTS: This does not match any source in the on-board catalog.
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 148.98,-18.85 [deg].
- GCN Circular #4533
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
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
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
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 Circular #4538
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
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
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
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
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
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
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
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.
- astro-ph/0606004 from
Jelinek: The bright optical flash from GRB 060117
We present a discovery and observation of an extraordinarily bright prompt
optical emission of the GRB 060117 obtained by a wide-field camera atop the
robotic telescope FRAM of the Pierre Auger Observatory from 2 to 10 minutes
after the GRB. We found rapid average temporal flux decay of alpha = -1.7 +-
0.1 and a peak brightness R = 10.1 mag. Later observations by other instruments
set a strong limit on the optical and radio transient fluxes, unveiling an
unexpectedly rapid further decay. We present an interpretation featuring a
relatively steep electron-distribution parameter p ~ 3.0 and providing a
straightforward solution for the overall fast decay of this optical transient
as a transition between reverse and forward shock.
- astro-ph/0702197 from 7 Feb 2007
Jelinek: GRB 060117: Reverse + forward shock solution
We present a discovery and observation of an extraordinarily bright prompt
optical emission of the GRB 060117 obtained by a wide-field camera atop the
robotic telescope FRAM of the Pierre Auger Observatory from 2 to 10 minutes
after the GRB.
We found rapid average temporal flux decay of alpha = -1.7 +/- 0.1 and a peak
brightness R = 10.1 mag.
We interpret the shape of the lightcurve as a transition between reverse and
forward shock emission.
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