GRB 161214B
GCN Circular 20453
Subject
GRB 161214B: 15 GHz upper limits from AMI
Date
2017-01-13T18:59:15Z (9 years ago)
From
Kunal Mooley at Oxford U <kunal.mooley@physics.ox.ac.uk>
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 robotically triggered on the Swift alert for GRB
161214B (D'Avanzo et al., GCN 20257) as part of the 4pisky program, and
subsequent follow up observations were obtained up to 10 days
post-burst. Our observations at 15 GHz on 2016 Dec 14.76, Dec 16.76, Dec
18.75 and Dec 21.74 (UT) do not reveal any radio source at the XRT
location (Goad et al., GCN 20264), with 3sigma upper limits of 96 uJy,
87 uJy, 85 uJy and 104 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/.
GCN Circular 20345
Subject
GRB 161214B: MASTER-Kislovodsk early optical observations
Date
2016-12-27T17:03:34Z (9 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
D.Vlasenko, V. Lipunov, E.Gorbovskoy, N.Tyurina, V.Kornilov,
O.Gress, P.Balanutsa, A.Kuznetsov, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute
R. Rebolo, M. Serra Ricart, N. Lodieu, G. Israelian
The Instituto de Astrofisica de Canarias
R.Podesta, C.Lopez, F.Podesta
Observatorio Astronomico Felix Aguilar (OAFA), San Juan Univerdity,
H. Levato, C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)
D.Buckley, S. Potter,
South African Astronomical Observatory
O.Gres, K.Ivanov, J.Rabinovich, N.M.Budnev,
Irkutsk State University
A. Tlatov, V.Senik, D. Dormidontov, A.Parkhomenko
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, A.Gabovich
Blagoveschensk Educational State University, Blagoveschensk
MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Kislovodsk was pointed to the GRB161214B 882 sec after notice
time and 900.34 sec after trigger time at 2016-12-14 17:35:11 UT. On our
first (180s exposure) set we haven`t found optical transient within
Swift error-box (ra=00 16 16 dec=+07 26 10 r=3.00) (D'Avanzo et al., GCN
20257). The 5-sigma upper limit set is about 16.5 mag(polaroid,
unfiltered).
The observations made on zenit distance = 49 degrees, galaxy latitude b =
-54 degree.
The moon (98 % bright part) is 29.5 degrees above the horizon. The
distance between moon and object is 87
The sun altitude is -40 degree.
The object can be observed till 2016-12-14 22:27:18
Maximal coadded limit ~18.7 m. No OT found.
The message may be cited.
GCN Circular 20319
Subject
GRB 161214B: optical spectroscopy of the foreground SDSS object
Date
2016-12-21T10:31:39Z (9 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI and DTU Space), J. P. U. Fynbo (DARK/NBI), B.
Milvang-Jensen (DARK/NBI), N. R. Tanvir (Univ. Leicester), M. I.
Andersen (DARK/NBI), H. Korhonen (DARK/NBI), D. A. Perley (DARK/NBI), T.
Kruehler (MPE), D. Xu (NAOC/CAS), G. Fedorets (NOT and Univ. Helsinki),
report on behalf of a larger collaboration:
We report on further analysis of our data (Malesani et al., GCN 20260)
taken at the Nordic Optical Telescope for GRB 161214B (D'Avanzo et al.,
GCN 20257). The best-seeing images (~0.9") clearly reveal two blended
objects within the XRT error circle, separated by <1 arcsec, with
comparable brightness (at ~2.2 hr after the GRB). As first suggested in
GCN 20260, the likely interpretation is the near-superposition of the
afterglow of GRB 161214B and an unrelated, foreground object.
Astrometric registration of our images with the SDSS frames shows that
the afterglow is slightly south of the SDSS source.
A spectrum of the complex was secured using the AlFOSC spectrograph,
covering both objects. Observations started on 2016 Dec 14.82 UT (2.42
hr after the GRB) and consisted of 2x20 min exposures using grism #4,
covering the wavelength range 3500-9400 AA. A few absorption lines are
apparent, and there is a hint that their spatial extent on the trace is
offset to the North (consistent with the SDSS source location). The two
most prominent features can be identified as the Mg I b triplet and the
Na I D doublet at redshift ~0, confirming that the SDSS object is a
Galactic star (probably of K or early M type). One more feature is
observed at ~4238 AA, whose identification is unclear. One possibility
is the Ca I 4226 A resonant line at z = 0, sometimes observed in K
stars, which would however require an offset of the wavelength
calibration in the blue part of our spectrum.
No features which can be clearly attributed to the afterglow are
detected in our spectrum. Marshall & D'Avanzo (GCN 20268) report
detection of the afterglow in the UVOT UVW2 filter, at a flux level much
brighter than the SDSS object (u ~ 22.5). This allows to set an upper
limit to the redshift z <~ 1.2 from the absence of the Lyman limit dropout.
GCN Circular 20279
Subject
GRB 161214B: AbAO and ISON/Terskol optical observations
Date
2016-12-17T07:25:30Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), R. Inasaridze (AbAO), A. Mokhnatkin (KIAM), A. Pozanenko
(IKI), A. Volnova (IKI), V. Ayvazian (AbAO), V. Zhuzhunadze, (AbAO),
O.Kvaratskhelia (AbAO), G. Inasaridze (AbAO), I. Molotov (KIAM) report on
behalf of larger GRB follow-up collaboration:
We observed the field of GRB 161214B (D'Avanzoet al., GCN 20257) with
AS-32 (0.7m) telescope of Abastumani Observatory and with K-800 (0.8m)
telescope of ISON/Terskol observatory on December, 15. We obtained
several unfiltered images in each observatory. The source previously
reported (Malesani et al. GCN 20260; Marshall et al. GCN 20261) is clearly
visible. Preliminary photometry of the source is following
Date UT start t-T0 Filter Exp. OT Err. UL
(mid, days) (s)
2016-12-15 15:31:49 0.97738 CR 85*60 18.79 0.05 22.2 AS-32
2016-12-15 18:07:05 1.06047 CR 142*30 18.76 0.13 21.4 K-800
Photometry is based on R-magnitudes the same stars used in (Mazaeva et al.,
GCN 20275)
GCN Circular 20275
Subject
GRB 161214B: Mondy optical observations
Date
2016-12-16T18:12:42Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), A. Volnova
(IKI), I. Korobtsev (ISTP) report on behalf of larger GRB follow-up
collaboration:
We observed the field of GRB 161214B (D'Avanzoet al., GCN 20257) with
AZT-33IK telescope of Sayan observatory (Mondy) starting on December, 15
(UT) 13:22:26. We obtained several images in R-filter.
The source previously reported (Malesani et al. GCN 20260; Marshall et
al. GCN 20261) is clearly visible. Preliminary photometry of the source
is following
Date UT start t-T0 Filter Exp. OT Err. UL
(mid, days) (s)
2016-12-15 13:22:26 0.85579 R 120*30 18.69 0.03 21.9
The photometry includes a catalogued star SDSS J001524.26+072108.5
already mentioned by Malesani et al. (GCN 20260) and Marshall et al.
(GCN 20268). The R magnitude of the star obtained by Lupton
transformations is 18.83 +/- 0.03.
Photometry is based on nearby SDSS-DR9 stars
SDSS-DR9_id R(Lupton)
J001520.09+072300.5 17.01
J001517.29+072310.4 17.05
J001513.07+071914.3 17.28
J001511.86+071859.3 16.07
J001513.35+071841.1 15.26
J001525.83+072141.2 14.31
J001524.40+072156.0 17.79
J001530.21+072230.9 16.94
GCN Circular 20270
Subject
GRB 161214B: Swift-BAT refined analysis
Date
2016-12-15T17:35:50Z (9 years ago)
From
Hans Krimm at NSF/NASA-GSFC <hkrimm@nsf.gov>
H. A. Krimm (NSF/USRA), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
P. D'Avanzo (INAF-OAB), N. Gehrels (GSFC), A. Y. Lien (GSFC/UMBC),
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-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 161214B (trigger #726885) (D'Avanzo, et al., GCN Circ. 20257). The BAT ground-calculated position is RA, Dec = 3.857, 7.342 deg which is
RA(J2000) = 00h 15m 25.6s
Dec(J2000) = +07d 20' 30.7���
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 64%.
The mask-weighted light curve shows a single, FRED-shaped peak, beginning at
T-2 sec, peaking at T+0 sec and fading to background by T+30 sec. There is a
soft precursor at T-74 sec, which was detected on board at too low significance
to trigger. T90 (15-350 keV) is 24.8 +- 3.1 sec (estimated error including systematics).
The time-averaged spectrum from T-0.42 to T+30.75 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.76 +- 0.09. The fluence in the 15-150 keV band is 2.1 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+0.11 sec in the 15-150 keV band is 2.2 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level.
GCN Circular 20268
Subject
GRB 161214B: Swift/UVOT Afterglow Confirmation
Date
2016-12-15T14:57:31Z (9 years ago)
From
Frank Marshall at GSFC <femarsha@khamseen.gsfc.nasa.gov>
F. E. Marshall (NASA/GSFC) and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:
Continuing Swift/UVOT observations of the field of GRB 161214B
(D'Avanzo et al., GCN Circ. 20257) show that the single source
consistent with the XRT position (Goad et al. GCN Circ. 20264)
reported by Marshall and D'Avanzo (GCN Circ. 20261) brightened
to 17.89 mag in white and then subsequently dimmed by more than
1 magnitude. This confirms the detection of the afterglow
reported by Kugel (GCN Circ. 20262), Klotz et al. (GCN Circ. 20263),
and Watson et al. (GCN Circ. 20266) following the suggestion
by Malesani et al. (GCN Circ. 20260). Detection of the afterglow
in the w2 filter indicates that the redshift is < 1.5.
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures
are given in the following table. The magnitudes include contributions
from both the afterglow and the catalogued star SDSS J001524.26+072108.5.
Filter T_start(s) T_stop(s) Exp(s) Mag
white 84 234 147 19.3 +/- 0.1
white 748 768 18 17.9 +/- 0.1
white 27988 28895 841 19.5 +/- 0.1
u 296 546 246 18.4 +/- 0.1
u 17963 18176 208 19.1 +/- 0.2
w2 5119 5319 197 18.8 +/- 0.2
w2 28903 29657 742 20.4 +/- 0.2
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 20266
Subject
GRB 161214B: RATIR Optical and Near-Infrared Observations
Date
2016-12-15T05:21:07Z (9 years ago)
From
Alan M. Watson at Instituto de Astronomia UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz
(UCSC), Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s Gonz��lez
(UNAM), Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley
(GSFC), John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD)
report:
We observed the field of GRB 161214B (D'Avanzo et al., GCN Circ. 20257)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
Astron��mico Nacional on Sierra San Pedro M��rtir from 2016/12 15.08 to
2016/12 15.10 UTC (8.60 to 9.05 hours after the BAT trigger), obtaining
a total of 0.26 hours exposure in the r and i bands and 0.15 hours
exposure in the Z, Y, J, and H bands.
We detect a source within the Swift-XRT enhanced error circle (Evans,
GCN Circ 20259. In comparison with the SDSS DR9 and 2MASS catalogs, we
obtain the following magnitudes:
r 18.87 +/- 0.01
i 18.56 +/- 0.01
Z 18.34 +/- 0.01
Y 18.23 +/- 0.03
J 18.23 +/- 0.03
H 18.05 +/- 0.04
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
The fading from r = 18.35 reported at 2.2 hours by Malesani et al. (GCN
Circ. 20260) to our observation of r = 18.87 at 8.8 hours confirms the
behavior reported by Kugel (GCN Circ. 20262). Our image quality is about
1.7 arcsec FWHM, so we are not able to separate this source from the
nearly coincident r = 19.09 SDSS source J001524.26+072108.5 mentioned by
Malesani et al.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 20265
Subject
GRB 161214B: Swift-XRT refined Analysis
Date
2016-12-15T05:10:40Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
D.N. Burrows (PSU), T.G.R. Roegiers (PSU), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), B. Mingo (U. Leicester), V. D'Elia (ASDC), A.
D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), L.M. McCauley (PSU) and P.
D'Avanzo report on behalf of the Swift-XRT team:
We have analysed 9.1 ks of XRT data for GRB 161214B (D'Avanzo et al.
GCN Circ. 20257), from 64 s to 29.6 ks after the BAT trigger. The data
comprise 234 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 20259).
The late-time light curve (from T0+5.1 ks) can be modelled with a
power-law decay with a decay index of alpha=0.63 (+/-0.09).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.54 (+0.16, -0.15). The
best-fitting absorption column is 1.22 (+0.33, -0.30) x 10^21 cm^-2,
in excess of the Galactic value of 7.2 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.94 (+0.15, -0.14)
and a best-fitting absorption column of 9.3 (+3.9, -2.0) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.4 x 10^-11 (4.1 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 9.3 (+3.9, -2.0) x 10^20 cm^-2
Galactic foreground: 7.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.94 (+0.15, -0.14)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00726885.
This circular is an official product of the Swift-XRT team.
[GCN OPS NOTE(15dec16): Per author's request, the value for alpha
was added in the second paragraph.]
GCN Circular 20264
Subject
GRB 161214B: Enhanced Swift-XRT position
Date
2016-12-15T00:12:53Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 3923 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 161214B, 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 = 3.85122, +7.35236 which is equivalent
to:
RA (J2000): 00h 15m 24.29s
Dec (J2000): +07d 21' 08.5"
with an uncertainty of 1.5 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 Circular 20263
Subject
GRB 161214B: TAROT Calern observatory optical observations
Date
2016-12-14T23:43:16Z (9 years ago)
From
Alain Klotz at IRAP-CNRS-OMP <Alain.Klotz@free.fr>
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 161214B detected by SWIFT
(trigger 726885) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.
The observations started 32.4s after the GRB trigger
(17.7s after the notice). The elevation of the field increased from
51 degrees above horizon and weather conditions
were good with the moon.
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+32.4s to t0+92.4s : Rlim = 17.3
Later images show the star at the following magnitudes:
t0+ 1046 sec to t0+ 1496 sec : 17.6 +/- 0.5
t0+ 1561 sec to t0+ 2371 sec : 17.8 +/- 0.5
t0+ 3681 sec to t0+ 4581 sec : 18.2 +/- 0.7
Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.
GCN Circular 20262
Subject
GRB 161214B: Chante-perdrix observatory optical observations
Date
2016-12-14T23:41:41Z (9 years ago)
From
Alain Klotz at IRAP-CNRS-OMP <Alain.Klotz@free.fr>
Kugel F. (Chante-perdrix observatory) report:
We imaged the field of GRB 161214B detected by SWIFT
(trigger 726885) with a 400 mm telescope (F/D=3)
located at the Chante-perdrix observatory, France (IAU A77).
The CCD camera is an Atik 460EX unfiltered.
We detect the same star as Malesani et al. (GCNC 20260).
A first series images show the star 0.7 magnitude
brighter than measured in later images:
t0 + 8.1 min to t0 + 20.1 min : R = 17.2 +/- 0.3
t0 + 106.6 min to t0 + 128.6 min : R = 17.9 +/- 0.3
t0 + 131.1 min to t0 + 153.1 min : R = 17.9 +/- 0.3
Magnitudes were estimated with the nearby USNO-SA stars
and are not corrected for galactic dust extinction.
GCN Circular 20261
Subject
GRB 161214B: Swift/UVOT Observations
Date
2016-12-14T21:55:35Z (9 years ago)
From
Frank Marshall at GSFC <femarsha@khamseen.gsfc.nasa.gov>
F. E. Marshall (NASA/GSFC) and P. D'Avanzo (INAF-OAB)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 161214B
295 s after the BAT trigger (D'Avanzo et al., GCN Circ. 20257).
A single source is detected within the enhanced XRT error region
(Evans, GCN Circ. 20259) in the initial UVOT exposures.
The source position is consistent with that of SDSS J001524.26+072108.5
and also with that of an entry in the USNO-B1.0 catalog.
Since the two UVOT exposures were taken with different filters, it is
not yet possible to report on variability.
It is possible that some of the flux is due to an optical afterglow
(as suggested for NOT observations by Malesani et al. GCN Circ. 20260).
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
u_FC 295 545 246 18.4 +/- 0.2
white_FC 872 955 82 18.1 +/- 0.2
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 20260
Subject
GRB 161214B: NOT optical observations, possible counterpart
Date
2016-12-14T21:15:24Z (9 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI and DTU Space), D. A. Perley (DARK/NBI), D. Xu
(NAOC/CAS), N. R. Tanvir (Univ. Leicester), G. Fedorets (NOT and Univ.
Helsinki), report on behalf of a larger collaboration:
We observed the field of GRB 161214B (D'Avanzo et al., GCN 20257) with
the Nordic Optical Telescope equipped with the AlFOSC camera. Seeing
conditions were modest (1.2").
In a 300-s image taken in the SDSS r band (mean time 2016 Dec 14.815 UT,
that is 2.2 hr after the GRB), we detect a single object within the
updated XRT error circle (Evans, GCN 20259), which is visible in
archival images (e.g. from the DSS and SDSS). No other objects are
visible within or close to the XRT position (though, the glare of this
object affects negatively the search for such objects). As this field is
covered from the SDSS, we can compute accurate photometry of this
object, r = 18.35 +- 0.02 (AB).
The brightness of this object is 0.76 +- 0.03 mag brighter then its
archival value from the SDSS, and it shows hint of extension in our
images. One possibility is that the detected source is actually the
blending of two very nearby objects, possibly the optical afterglow of
GRB 161214B and an unrelated, foreground star. However, given the modest
seeing of our images, we cannot exclude a real physical association
between the SDSS object and the GRB.
[GCN OPS NOTE(14dec16): Per author's request, the GRB name in the last
paragraph was changed from "161014B" to "161214B".]
GCN Circular 20259
Subject
GRB 161214B: Prompt enhanced Swift-XRT position
Date
2016-12-14T17:51:22Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Using promptly downlinked XRT event data for GRB 161214B, we find an
enhanced XRT position of the afterglow: RA, Dec: 3.8510, 7.3522 which
is equivalent to:
RA (J2000) = 00 15 24.23
Dec (J2000) = +07 21 08.0
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/726885.
Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
GCN Circular 20257
Subject
GRB 161214B: Swift detection of a burst
Date
2016-12-14T17:32:35Z (9 years ago)
From
David Burrows at PSU/Swift <burrows@astro.psu.edu>
P. D'Avanzo (INAF-OAB), D. N. Burrows (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/NSF/USRA), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (GSFC/UMBC), A. Melandri (INAF-OAB),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:
At 17:20:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161214B (trigger=726885). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 3.850, +7.342 which is
RA(J2000) = 00h 15m 24s
Dec(J2000) = +07d 20' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single FRED-shaped
structure with a duration of about 20 sec. The peak count rate
was ~2900 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 17:21:25.5 UT, 74.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 3.85151, 7.35291 which is
equivalent to:
RA(J2000) = 00h 15m 24.36s
Dec(J2000) = +07d 21' 10.5"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 39 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.
The initial flux in the 2.5 s image was 1.29e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT data are unavailable at this time.
Burst Advocate for this burst is P. D'Avanzo (paolo.davanzo AT brera.inaf.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.)