| Summary table |
|---|
| Variable |
Value |
Source |
| T0 |
1:27:34 UTC |
GCN_circulars,Swift Det |
| ra |
150.6510° |
Swift |
| decl |
52.3590° |
Swift |
| pos_error |
1.94e-04° |
Swift |
| T90 |
18.2 s |
Swift |
| T90_start |
1:27:34 UTC |
Swift |
| fluence |
1.90e-07 erg/cm² |
Swift |
| T100 |
18.2 s |
|
| GBM_located |
False |
|
| mjd |
57739.06081018518 |
GCN_circulars,Swift Det |
| IPN table |
|---|
| GRB_name |
GRB161217A |
| ra |
150.6375° |
| decl |
52.3833° |
| pos_error |
5.00e-02° |
| Swift table |
|---|
| GRB_name |
GRB161217A |
| t_trigger |
1:27:34 UTC |
| ra |
150.6510° |
| decl |
52.3590° |
| pos_error |
1.94e-04° |
| T90 |
18.2 s |
| fluence |
1.90e-07 erg/cm² |
| GCN 20276 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20276 |
| Detection_method |
Swift Det |
| t_trigger |
1:27:34 UTC |
| ra |
150.6370° |
| decl |
52.3890° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20276
SUBJECT: GRB 161217A: Swift detection of a burst
DATE: 16/12/17 01:54:47 GMT
FROM: David Palmer at LANL
V. D'Elia (ASDC), J. A. Kennea (PSU), H. A. Krimm (CRESST/NSF/USRA),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and T. Sakamoto (AGU) report on behalf of the
Swift Team:
At 01:27:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161217A (trigger=727167). Swift slewed immediately to the burst.
The BAT on-board calculated location is RA, Dec 150.637, +52.389 which is
RA(J2000) = 10h 02m 33s
Dec(J2000) = +52d 23' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a peak starting
around T+35s and lasting about 15 seconds. (Because this was
an image trigger, the 'trigger time' is not tightly synchronized to
the time of the rate increase.) The peak count rate
was ~600 counts/sec (15-350 keV), at ~35 sec after the trigger.
The XRT began observing the field at 01:30:15.5 UT, 160.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 150.6517, 52.3592 which
is equivalent to:
RA(J2000) = 10h 02m 36.40s
Dec(J2000) = +52d 21' 33.1"
with an uncertainty of 2.4 arcseconds (radius, 90% containment). This
location is 112 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
http://www.swift.ac.uk/sper. We cannot determine whether the source is
fading at the present time. No spectrum from the promptly downlinked
event data is yet available to determine the column density.
UVOT took a finding chart exposure of 144 seconds with the White filter
starting 163 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. 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 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.01.
Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
|
| GCN 20278 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20278 |
| Detection_method |
Swift-XRT Det |
| ra |
150.6513° |
| decl |
52.3589° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20278
SUBJECT: GRB 161217A: Enhanced Swift-XRT position
DATE: 16/12/17 05:27:58 GMT
FROM: Phil Evans at U of Leicester
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1529 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 161217A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 150.65129, +52.35891 which is equivalent
to:
RA (J2000): 10h 02m 36.31s
Dec (J2000): +52d 21' 32.1"
with an uncertainty of 1.9 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
|
| GCN 20280 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20280 |
| Detection_method |
Swift-XRT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20280
SUBJECT: GRB 161217A: Swift-XRT refined Analysis
DATE: 16/12/17 10:10:04 GMT
FROM: Phil Evans at U of Leicester
T.G.R. Roegiers (PSU), K.L. Page (U. Leicester), B. Mingo (U.
Leicester), A.P. Beardmore (U. Leicester), A. D'Ai (INAF-IASFPA), A.
Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), L.M. McCauley (PSU), J.A.
Kennea (PSU) and V. D'Elia report on behalf of the Swift-XRT team:
We have analysed 6.5 ks of XRT data for GRB 161217A (D'Elia et al. GCN
Circ. 20276), from 171 s to 16.8 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Osborne et al. (GCN Circ. 20278).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.69 (+/-0.06).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.67 (+0.20, -0.11). The
best-fitting absorption column is consistent with the Galactic value
of 7.7 x 10^19 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum is 3.9 x 10^-11 (3.9 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 7 (+/-37) x 10^19 cm^-2
Galactic foreground: 7.7 x 10^19 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.67 (+0.20, -0.11)
If the light curve continues to decay with a power-law decay index of
0.69, the count rate at T+24 hours will be 7.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x
10^-13 (3.1 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00727167.
This circular is an official product of the Swift-XRT team.
|
| GCN 20282 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20282 |
| Detection_method |
Swift-UVOT Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20282
SUBJECT: GRB 161217A: Swift/UVOT Upper Limits
DATE: 16/12/17 17:26:54 GMT
FROM: Frank Marshall at GSFC
F. E. Marshall (NASA/GSFC) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 161217A
163 s after the BAT trigger (D'Elia et al., GCN Circ. 20276).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al., GCN Circ. 20278)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 163 308 142 >21.0
u_FC 314 564 246 >21.0
white 163 1713 406 >21.2
v 644 1589 117 >18.8
b 576 1689 111 >19.8
u 314 1664 343 >20.4
w1 693 1639 97 >20.3
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).
|
| GCN 20284 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20284 |
| Detection_method |
Swift-BAT Det |
| ra |
150.6580° |
| decl |
52.3440° |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20284
SUBJECT: GRB 161217A: Swift-BAT refined analysis
DATE: 16/12/18 04:08:49 GMT
FROM: Hans Krimm at NASA-GSFC/NSF
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
V. D'Elia (ASDC), N. Gehrels (GSFC), H. A. Krimm (NSF/USRA),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161217A (trigger #727167)
(D'Elia, et al., GCN Circ. 20276). The BAT ground-calculated position is
RA, Dec = 150.658, 52.344 deg which is
RA(J2000) = 10h 02m 38.0s
Dec(J2000) = +52d 20' 38.9"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows an initial soft, weak peak from T-20 to T+20
sec, followed by a stronger peak from T+32 to T+48 sec. T90 (15-350 keV) is 1
8.2 +- 5.8 sec (estimated error including systematics).
The time-averaged spectrum from T+33.77 to T+53.86 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.70 +- 0.35. The fluence in the 15-150 keV band is 1.9 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+42.64 sec in the 15-150 keV band
is 0.4 +- 0.1 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/727167/BA/
|
| GCN 20285 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20285 |
| Detection_method |
MITSuME |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20285
SUBJECT: GRB 161217A: MITSuME Okayama upper limits
DATE: 16/12/18 15:22:08 GMT
FROM: Daisuke Kuroda at OAO/NAOJ
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of MITSuME and OISTER collaboration:
We observed the field of GRB 161217A (D'Elia et al., GCNC 20276)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2016-12-17 12:40:15 UT (~11.2 h after
the burst). We did not find any new point source within the
Enhanced XRT circle (Osborne et al., GCNC 20278) in all the three
bands.
Three sigma upper limits of the OT are listed below.
We used SDSS-DR8 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' Rc Ic
-----------------------------------------------------
0.51298 13:46:16 5760.0 >19.1 >19.1 >18.4
0.76490 19:49:01 6180.0 >20.1 >19.9 >19.1
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
|
| GCN 20289 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20289 |
| Detection_method |
Optical |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20289
SUBJECT: GRB 161217A: TAROT Calern observatory optical observations
DATE: 16/12/18 20:41:58 GMT
FROM: Alain Klotz at IRAP-CNRS-OMP
Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.) report:
We imaged the field of GRB 161217A detected by SWIFT
(trigger 727167) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.
The observations started 133.3s after the GRB trigger
(18.3s after the notice). The elevation of the field increased from
65 degrees above horizon and weather conditions
were good.
The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT with a limiting magnitude of:
t0+133.3s to t0+193.3s : Rlim = 16.3
The second image is 30.0s exposure in tracking mode:
t0+208.6s to t0+238.6s : Rlim = 16.9
We co-added a series of exposures:
t0+208.6s to t0+611.7s : Rlim = 18.1
Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.
|
| GCN 20447 table |
|---|
| GRB_name |
GRB161217A |
| GCN_number |
20447 |
| Detection_method |
Swift Other |
| Circular_text |
TITLE: GCN CIRCULAR
NUMBER: 20447
SUBJECT: GRB 161217A: 15 GHz upper limits from AMI
DATE: 17/01/13 12:17:33 GMT
FROM: Kunal Mooley at Oxford U
K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson
(Curtin), T. Cantwell (Manchester), D. Titterington, S. H. Carey, J.
Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K.
Grainge, A. Scaife (Manchester)
The AMI Large Array triggered on the Swift alert for GRB 161217A (D'Elia
et al., GCN 20276) as part of the 4pisky program, and follow up
observations were obtained up to 10 days post-burst. Our observations at
15 GHz on 2016 Dec 23.16, Dec 24.15 and Dec 27.17 (UT) do not reveal any
radio source at the XRT location (Osborne et al., GCN 20278), with
3sigma upper limits of 84 uJy, 66 uJy and 77 uJy respectively.
We thank the AMI staff for scheduling these observations. The AMI-GRB
database is a log of all GRB follow up observations with the AMI, and is
available at http://4pisky.org/ami-grb/.
|