# GCN_circulars

GRB_name: GRB161004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19986
SUBJECT: GRB 161004A: SAO RAS optical upper limit
DATE:    16/10/04 23:02:45 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO RAS), A. Volnova (IKI), and A. Pozanenko (IKI)
report on behalf of the larger GRB follow-up team.

We observed the field of GRB 161004A (Evans et al., GCN 19979)
with Zeiss-1000 - the 1-meter telescope of Special Astrophysical
Observatory of Russian Academy of Sciences. We obtain several
images with filter Rc starting on October, 4 (UT) 15:44:35.

In the refined XRT error circle (Beardmore et al., GCN 19983)
we do not detect the optical counterpart (Breeveld and Evans,
GCN 19984). Preliminary photometry of a combined image is following

Date       UT start   t-T0     Filter   Exp.   OT      UL
                   (mid, days)          (s)
2016-10-04 15:44:35   0.1396    Rc      12*300 n/d    22.4

Photometry is based on nearby SDSS-DR9 stars reported
by Mazaeva et al. (GCN 19980).


GRB_name: GRB161004B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19987
SUBJECT: GRB 161004B: Swift detection of a burst
DATE:    16/10/04 23:18:17 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf
of the Swift Team:

At 23:07:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161004B (trigger=715246).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 112.157, -39.895 which is 
   RA(J2000) = 07h 28m 38s
   Dec(J2000) = -39d 53' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single FRED peak
with substructure and  a duration of about 20 sec.  The peak count rate
was ~12000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 23:09:12.7 UT, 73.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 112.15290, -39.89858 which
is equivalent to:
   RA(J2000)  = 07h 28m 36.70s
   Dec(J2000) = -39d 53' 54.9"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 17 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 5.23e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 82 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.54. 

Burst Advocate for this burst is A. D'Ai (antonino.dai AT ifc.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.)


GRB_name: GRB161004B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19988
SUBJECT: GRB 161004B: Prompt enhanced Swift-XRT position
DATE:    16/10/04 23:53:05 GMT
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 161004B, we find an
enhanced XRT position of the afterglow: RA, Dec: 112.1514, -39.8976
which is equivalent to:
   RA (J2000)  = 07 28 36.34
   Dec (J2000) = -39 53 51.5
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/715246.

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.


GRB_name: GRB160915A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19989
SUBJECT: GRB 160915A: Lomonosov BDRG gamma ray detection
DATE:    16/10/05 09:16:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov,
A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, 
A.V.Bogomolov, A.F.Iyudin, V.V.Kalegaev, D.Nguen,  V.L. Petrov, 
I.V.Yashin, P.S.Kazarian
Physics Department, Skobel'tsyn Institute of Nuclear Physics, Moscow State

V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute

I. Park, J. Lee, S. Jeong
Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, 
Korea

At 22:51:12.00 UT on 15 Sep 2016, during the Lomonosov BDRG  Gamma-ray 
Burst Monitor data inspection 
(http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg ),
it was found GRB 160915A, which matches with INTEGRAL SPI-ACS Trigger 
event Sub Num 7564, http://gcn.gsfc.nasa.gov/integral_spiacs.html .
GRB 160915A has several peaks LC, three of them match with peaks of 
INTEGRAL SPI-ACS Trigger event Sub Num 7564 , total duration 12s duration, 
the energy range 120-1000 keV.
More information will be available at: 
http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts

This Notice was ground-generated.

The message may be cited.


GRB_name: GRB160917A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19990
SUBJECT: GRB 160917A: Lomonosov BDRG gamma ray detection 
DATE:    16/10/05 11:48:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov,
A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, 
V.V.Kalegaev, D.Nguen,  V.L. Petrov, I.V.Yashin, P.S.Kazarian
Physics Department, Skobel'tsyn Institute of Nuclear Physics, Moscow State

V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute

I. Park, J. Lee, S. Jeong
Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, 
Korea

At 11:30:20 UT on 17 Sep 2016, the Lomonosov BDRG  Gamma-ray Burst
Monitor  (http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg )
triggered GRB 160917A (J. L. Racusin, GCN 19962).
GRB 160917A has several peaks LC, total duration 25s,
the energy range 70-1000 keV.
More information will be available at:
http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts
This Notice was ground-generated.
The message may be cited.


GRB_name: GRB161004B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19991
SUBJECT: GRB 161004B: Enhanced Swift-XRT position
DATE:    16/10/05 11:55:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3535 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 161004B, 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 = 112.15126, -39.89791 which is equivalent
to:

RA (J2000): 07h 28m 36.30s
Dec (J2000): -39d 53' 52.5"

with an uncertainty of 1.4 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.


GRB_name: GRB160917B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19992
SUBJECT: GRB 160917B: Lomonosov BDRG gamma ray discovery
DATE:    16/10/05 12:06:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov,
A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, 
V.V.Kalegaev, D.Nguen,  V.L. Petrov, I.V.Yashin, P.S.Kazarian
Physics Department, Skobel'tsyn Institute of Nuclear Physics, Lomonosov 
Moscow State University

V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute

I. Park, J. Lee, S. Jeong
Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, 
Korea

At 10:56:12.00 UT on 17 Sep 2016, the Lomonosov BDRG  Gamma-ray
Burst Monitor
(http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg ),
triggered GRB 160917B.
GRB 160917B has one peak LC and matches with peak 
of Fermi Trigger event Num 495802575, total duration ~10s,
the energy range 200-1600 keV.
LC is available at:
http://master.sai.msu.ru/static/Lomonosov/GRB160917B.jpg

More information will be available at:
http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts
This Notice was ground-generated.

The message may be cited.


GRB_name: GRB161004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19993
SUBJECT: GRB 161004A: RATIR Optical and NIR Observations
DATE:    16/10/05 12:32:05 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB),
Antonino Cucchiara (UVI), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM), Leonid Georgiev
(UNAM), Jess Gonzlez (UNAM), Carlos Romn-Ziga (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 161004A (Evans, et al., GCN 19979) with 
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) 
on the 1.5m Harold Johnson Telescope at the Observatorio Astronmico 
Nacional on Sierra San Pedro Mrtir from 2016/10 5.10 to 2016/10 5.22 
UTC (13.49 to 16.23 hours after the BAT trigger), obtaining a total 
of 1.73 hours exposure in the r and i bands and 0.65 hours exposure in 
the Z, Y, J, and H bands.

For a source within the Swift-UVOT error circle (Breeveld & Evans, 
GCN 19984), in comparison with the USNO-B1 and 2MASS catalogs, we 
obtain the following upper limits (3-sigma):

  r > 23.3
  i > 23.2
  Z > 22.4
  Y > 21.8
  J > 21.3
  H > 19.4

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir. 


GRB_name: GRB161004B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19994
SUBJECT: GRB 161004B: Swift-XRT refined Analysis
DATE:    16/10/05 12:53:00 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), L.M.
McCauley (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester),
J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB) and A. D'Ai report
on behalf of the Swift-XRT team:

We have analysed 7.1 ks of XRT data for GRB 161004B (D'Ai et al. GCN
Circ. 19987), from 63 s to 28.2 ks after the  BAT trigger. The data
comprise 77 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 Evans et
al. (GCN Circ. 19988).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.89 (+/-0.05), followed by a break at T+2716 s to an
alpha of 1.44 (+0.30, -0.22).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.99 (+0.19, -0.18). The
best-fitting absorption column is  1.14 (+0.21, -0.19) x 10^22 cm^-2,
in excess of the Galactic value of 3.5 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 5.1 x 10^-11 (9.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.14 (+0.21, -0.19) x 10^22 cm^-2
Galactic foreground: 3.5 x 10^21 cm^-2
Excess significance: 7.1 sigma
Photon index:      1.99 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
1.44, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (2.0 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/00715246.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161004B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19995
SUBJECT: GRB 161004B: Swift-BAT refined analysis
DATE:    16/10/05 13:02:02 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
A. D'Ai (INAF-IASFPA), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161004B (trigger #715246)
(D'Ai, et al., GCN Circ. 19987).  The BAT ground-calculated position is
RA, Dec = 112.156, -39.896 deg which is
    RA(J2000)  =  07h 28m 37.4s
    Dec(J2000) = -39d 53' 47.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.

The mask-weighted light curve shows two overlapping peaks starting at T-10 sec,
peaking at T+1 sec and ending at T+40 sec.  T90 (15-350 keV) is
15.9 +- 0.7 sec (estimated error including systematics).

The time-averaged spectrum from T-5.16 to T+27.31 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.21 +- 0.13,
and Epeak of 177 +- 73 keV (chi squared 35.21 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 8.8 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.36 sec in the 15-150 keV band is
10.1 +- 0.4 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.47 +- 0.03 (chi squared 47.75 for 57 d.o.f.).  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/715246/BA/


GRB_name: GRB161004B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19996
SUBJECT: GRB161004B: AstroSat CZTI detection
DATE:    16/10/05 14:56:42 GMT
FROM:    Dipankar Bhattacharya at IUCAA  <dipankar@iucaa.in>

V. Kumar, V. Sharma, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed clear detection of GRB161004B (Swift BAT detection: D.Palmer et al., GCN Circ. 19987) in the 40-200 keV energy range. The light curve shows a single peak at 23:07:59.0 UT, coincident with the Swift Trigger. The measured peak count rate is 187.3 counts/sec above the background in combined data of four quadrants, with a total of 1393.0 counts. The local mean background count rate was 313.7 counts/sec. Using cumulative rates, we measure a T90 of 13.1 secs.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb.  CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB161004B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19997
SUBJECT: GRB 161004B: Swift/UVOT Upper Limits
DATE:    16/10/05 16:23:52 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161004B
82 s after the BAT trigger (D'Ai et al., GCN Circ. 19987).
No optical afterglow consistent with the XRT position
(Evans et al., GCN Circ. 19991) 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) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            82          232          147         >20.8
u_FC               294          544          246         >19.6
white               82         1886          431         >21.2
v                  624         1937          156         >19.5
b                  550         1862          136         >19.6
u                  294         1836          363         >19.6
w1                 674         1812          136         >18.9
m2                5622         5747          123         >18.8
w2                 600         1736          136         >18.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.54 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161004B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19998
SUBJECT: GRB 161004B: Fermi GBM detection
DATE:    16/10/05 16:51:33 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

R. Hamburg (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 23:07:54.79 UT on 04 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161004B (trigger 497315278 / 161004964)
which was also detected by the Swift BAT
(D'Ai et al. 2016, GCN 19987)
The GBM on-ground location is consistent with the Swift position.

The trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux
of the GRB. This ARR was accepted and the spacecraft slewed to the GBM
in-flight
location. The initial angle from the Fermi LAT boresight to
the Swift location is 69 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 14 s (50-300 keV).
The time-averaged spectrum from T0-0.0 s to T0+18.4 s is
best fit by a Band function with Epeak = 132 +/- 6 keV,
alpha = -0.75 +/- 0.04, and beta = -2.4 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(1.877 +/- 0.039)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.7 s in the 10-1000 keV band
is 15.4 +/- 0.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161001A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  19999
SUBJECT: GRB 161001A: IRSF upper limits
DATE:    16/10/06 04:48:24 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

K. L. Murata (Nagoya University),  K. Miyakawa (Tokyo Institute of
Technology), and T. Nagayama (Kagoshima University)

We observed the field of GRB 161001A ( Page et al., GCN Circular #19967)
with the near-infrared (J, H, Ks) simultaneous imaging camera SIRIUS
attached to 1.4 m telescope IRSF ( InfraRed Survey Facility) in Sutherland
observatory, South Africa.

The observations started on 2016-10-01 02:41:46 UT (~ 95 min. after the
burst). We could not detect  the afterglow within the enhanced XRT error
circle (Osborne et al., GCN Circular #19969) in the three bands. We have
obtained the following preliminary upper limits (Vega magnitude system):

 J > 14.61
 H >14.19
 Ks > 14.01

Given magnitudes were calibrated against 2MASS point sources in this field.
The upper limits were determined as the magnitudes of the fainter star
within 1 arcmin from the enhanced XRT position.

This observation was carried out by IRSF and OISTER collaboration.


GRB_name: GRB150302A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20000
SUBJECT: GRB 150302A: late-time imaging and optical afterglow confirmation
DATE:    16/10/06 06:03:14 GMT
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), and T. 
Kruehler (MPE), report on behalf of a larger collaboration:

We observed the field of GRB 150302A (Lien et al., GCN 17526) with the 
Nordic Optical Telescope (NOT) equipped with the ALFOSC imaging camera. 
Observations (4x300 s exposure) were carried out in the SDSS r filter, 
at a mean epoch 2016 Jun 23.94 UT (1.3 years after the GRB).

At the location of the optical afterglow candidate (Fynbo et al., GCN 
17527), we detect no source down to a limiting magnitude of r = 23.5, 
calibrated against nearby SDSS stars. By comparing with our early epoch, 
we conclude that the source has faded by more than 1 mag. Together with 
the positional consistency with the enhanced XRT location (Goad et al., 
GCN 17534), we can thus now confirm it as the optical afterglow of GRB 
150302A.

We acknowledge excellent support from the NOT observing staff, in 
particular John Telting.


GRB_name: GRB161004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20001
SUBJECT: GRB 161004A: Swift-BAT refined analysis
DATE:    16/10/06 09:03:15 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
P. A. Evans (U Leicester), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), J. P. Norris (BSU),
T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
  
Using the data set from T-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161004A (trigger #715084)
(Evans, et al., GCN Circ. 19979).  The BAT ground-calculated position is
RA, Dec = 263.127, -0.947 deg which is
    RA(J2000)  =  17h 32m 30.6s
    Dec(J2000) = -00d 56' 50.7"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
  
The mask-weighted light curve shows a single peak starting at T-0.1 sec,
peaking at T+0.5 sec and ending at T+5 sec.  T90 (15-350 keV) is 1.08 +- 0.21 sec
(estimated error including systematics).
  
The time-averaged spectrum from T-0.11 to T+1.06 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.26 +- 0.33.  The fluence in the 15-150 keV band is 9.5 +- 1.6 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T+0.06 sec in the 15-150 keV band
is 1.0 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Due to a low signal-to-noise of the data, the lag analysis is not possible.
Therefore, it is not clear whether this burst belongs to a short GRB or not.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/715084/BA/
  


GRB_name: GRB160927A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20002
SUBJECT: GRB 160927A: CALET Gamma-Ray Burst Monitor ground detection
DATE:    16/10/06 13:43:52 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Moriyama, A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Yamada (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka,
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The short-duration GRB 160927A (Gibson et al., GCN Circ. 19952) was
detected by the ground analysis of the CALET Gamma-ray Burst Monitor
(CGBM) data at 18:04:49.88 on 27 September 2016.  The highest signal-to-noise
based on the light curve data is 5.3 sigma.  The burst signal was seen
by the SGM instrument.

The light curve of the SGM shows a single peak starting at T0, peaking
at T+0.4 sec and ending at T+0.6 sec.  The T90 duration measured by
the SGM data is 0.35 +- 0.11 sec (40-1000 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1159034645/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB161004B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20003
SUBJECT: GRB 161004B: CALET Gamma-Ray Burst Monitor detection
DATE:    16/10/06 13:51:35 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Yamada, A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka,
S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 161004B (D'Ai et al., GCN Circ. 19987; Kumar et al.,
GCN Circ. 19996;  Hamburg et al., GCN Circ. 19998; INTEGRAL-SPI/ACS trigger #7590)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:07:52.64 on 4 October 2016.
The burst signal was seen by the SGM instrument.

The light curve of the SGM shows a single peak starting at T0, peaking at
T+7 sec and ending at T+15 sec.  The T90 duration measured by the SGM data
is 11.1 +- 0.9 sec (40-450 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1159657616/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB160927A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20004
SUBJECT: GRB 160927A: GTC observations
DATE:    16/10/06 15:58:07 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), L. Izzo (IAA-CSIC), 
D.A. Kann (TLS Tautenburg), C.C. Thoene (IAA-CSIC), Z. Cano 
(IAA-CSIC), D. Reverte-Paya (GRANTECAN, IAC, ULL) report on 
behalf of a larger collaboration:

We observed the afterglow of the short-hard GRB 160927A (Gibson 
et al., GCN 19952) with OSIRIS on the 10.4m GTC telescope. 
Observations consisted in 10x190s exposures in r-band, with a mean 
epoch on 28 September 2016 at 20:26 UT (26.52 hr after the burst). 
The optical counterpart (Tkachenko et al., GCN 19954; Dâ€™Avanzo et 
al., GCN 19956; Wiseman et al. GCN 1959; Xu et al., GCN 19960; 
Fong et al., GCN 19964) is detected at a magnitude of r_AB = 
25.3+/-0.2, as compared to several SDSS field stars.

Combining this observation with the rest of the available GCN data, 
the light curve indicates an early evolution with a shallow decay, 
followed by a faster decay (as already mentioned by Wiseman et al. 
GCN 1959 and Xu et al., GCN 19960), with the break at around the 
TNG epoch, after which we estimate a decay rate of with alpha = 
-1.03+/-0.08 (where F~t^alpha).This decay is significantly shallower 
than the one reported by (Xu et al., GCN 19960), indicating that the 
light curve may be flattening at the time of the GTC observation. This 
could be due to the contribution of an additional component (either 
the host galaxy, or more unlikely the contribution of a kilonova) or just 
due to the uncertainties of the different photometric measurements.


GRB_name: GRB161004B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20005
SUBJECT: Konus-Wind observation of GRB 161004B
DATE:    16/10/06 16:02:46 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 161004B (Swift-BAT trigger #715246:
D'Ai et al., GCN 19987; Sakamoto et al., GCN 19995;
Fermi GBM detection: Hamburg & Meegan, GCN 19998;
CALET Gamma-Ray Burst Monitor detection: Yamada et al., GCN 20003)
triggered Konus-Wind at T0=83274.317 s UT (23:07:54.317).

The burst light curve shows a single pulse with a total duration of ~18 s.
The emission is seen up to ~2 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.71(-0.07,+0.08)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+4.144 s,
of 3.43(-0.80,+0.80)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+15.616 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.05(-0.09,+0.09),
and Ep = 175(-12,+14) keV (chi2 = 56/58 dof).
Fitting by the GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -3.14 (chi2 = 56/57 dof).

The spectrum near the peak count rate
(measured from T0 to T0+7.424 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.71(-0.10,+0.11),
and Ep = 210(-13,+15) keV (chi2 = 67/58 dof).
Fitting by the GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index:
beta < -3.12 (chi2 = 67/57 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161004_T83274/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB160925A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20006
SUBJECT: GRB 160925A: Kottamia R-band observation
DATE:    16/10/06 23:05:13 GMT
FROM:    Gamal B. Ali at NRIAG  <gamalali@lycos.com>

G. B. Ali, Y. Hendy, A. Takey, N. Essam, and A. Essam (NRIAG, Egypt) 
report on behalf of the Kottamia collaboration:

We observed the field of the Fermi GRB 160925A (trigger #496473540) with
the 1.88m telescope of the KAO (Kottamia Astronomical Observatory),
Egypt. The observation was performed in the Rc-band at the Newtonian
camera (F4.8) and started at 2016-09-29 T19:58:17 UT (~4.08 day after
the burst). 

We obtained several exposures in the Rc-band each one with 300s exposure
time.  We clearly detected the optical transient (Lipunov et al., GCN
19938; Guidorzi et al., GCN  19939). 

The following accurate photometry is obtained for the transient: 

UT (Start)                            Rc           error*   

2016-09-29T19:58:17       17.260   0.011 

2016-09-29T20:03:31       17.232   0.011 

2016-09-29T20:08:42       17.252   0.012 

2016-09-29T20:13:53       17.326   0.013 

2016-09-29T20:19:04       17.267   0.012 

2016-09-29T20:24:15       17.223   0.011 

2016-09-29T20:29:26       17.305   0.011 

2016-09-29T20:34:37       17.281   0.012 

2016-09-29T20:39:48       17.239   0.011 

---------------------------------------------------- 

(*) Poisson noise error only. 

The Photometric calibration is based on nearby USNO-B1.0 stars

USNO-B1.0        R2 

0750-0813981 13.69 

0750-0813991 14.20 

0750-0813958 14.93 

0750-0813917 15.62

[GCN OPS NOTE(08oct16): Per author's request, the signigure block and the appended
copy of the 19947 circular have been removed.]


GRB_name: GRB160821A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20007
SUBJECT: GRB 160821A: Maisoncelles observatory optical observations
DATE:    16/10/06 23:05:54 GMT
FROM:    Alain Klotz at IRAP-CNRS-OMP  <Alain.Klotz@free.fr>

Soulier J.-F. (Observatoire de Maisoncelles, France) repports:

I imaged the field of GRB 160821A detected by SWIFT
(trigger 709351) with the Newtonian 30cm F/3.8 telescope
located at the Maisoncelles observatory, France (IAU C10).

I detected the optical transcient described by Gendre et al.
(GCNC 19832) at the following position (+/- 0.5 arcsec):

RA(J2000) = 11h 25m 01.83s
DEC(J2000) = +42d 20' 06.5"

Filter  T_start(d)   T_stop(d)  Exp(s)     R
None    0.992        1.008      1440       18.6
None    4.992        4.008      1440   >20

Taking account for the magnitude provided by Gendre et al.
(GCNC 19832) I derived an optical decay alpha=0.78 for the
first day.

Magnitudes were estimated with the nearby UCAC-4 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB161007A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20008
SUBJECT: GRB 161007A: Swift detection of a burst
DATE:    16/10/07 21:40:54 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), L. M. Z. Hagen (PSU), J. A. Kennea (PSU),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 21:25:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161007A (trigger=716127).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 103.390, +23.289 which is 
   RA(J2000) = 06h 53m 34s
   Dec(J2000) = +23d 17' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 60 sec.  The peak count rate
was ~600 counts/sec (15-350 keV), at ~30 sec after the trigger. 

The XRT began observing the field at 21:27:47.8 UT, 124.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 103.40706, 23.30639 which
is equivalent to:
   RA(J2000)  = 06h 53m 37.69s
   Dec(J2000) = +23d 18' 23.0"
with an uncertainty of 4.3 arcseconds (radius, 90% containment). This
location is 84 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 1.56e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 133 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.12. 

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.)


GRB_name: GRB161007A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20009
SUBJECT: GRB 161007A: MASTER-net early optical observations 
DATE:    16/10/07 21:45:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, N.Tyurina, N.Shatskiy, 
P.Balanutsa, A.Kuznetsov, V.V.Chazov
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Krushinsky, I.Zalozhnih,  A. Popov
Ural Federal University, Yekaterinburg, Kourovka


R.Podesta, C.Lopez, F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)

H. Levato, C. Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB161007A 38 sec after notice time 
and 114 sec after trigger time at 2016-10-07 21:27:42 UT in two 
polarizations. On our first (20s exposure)  set we haven't found optical 
transient  within SWIFT error-box (ra=06 53 33 dec=+23 17 20 r=0.050000).
The 5-sigma upper limit has been about 17.0 mag.
The observations made on zenit distance = 33 degrees, galaxy latitude b = 
11 degree. The moon (38 % bright part) below the horizon (The altitude of 
the Moon is -56 degree ).



MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB161007A 33 sec after notice 
time and 109 sec after trigger time at 2016-10-07 21:27:36 UT in two 
polarizations.. On our first (20s exposure)  set we haven't found optical 
transient  within SWIFT error-box.
The 5-sigma upper limit has been about 17.0 mag.
The observations made on zenit distance = 68 degrees, galaxy latitude b = 
11 degree. The moon (38 % bright part) below the horizon (The altitude of 
the Moon is -28 degree ).


The message may be cited.


GRB_name: GRB161007A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20010
SUBJECT: GRB 161007A: Prompt enhanced Swift-XRT position
DATE:    16/10/07 22:05:42 GMT
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 161007A, we find an
enhanced XRT position of the afterglow: RA, Dec: 103.4092, 23.3068
which is equivalent to:
   RA (J2000)  = 06 53 38.21
   Dec (J2000) = +23 18 24.6
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/716127.

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.


GRB_name: GRB161004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20011
SUBJECT: GRB 161004A: refined analysis of TSHAO optical observations
DATE:    16/10/07 23:58:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Kusakin 
(Fesenkov Astrophysical Institute),  A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We present a refined analysis of our observations (Mazaeva et al., GCN 
19980) of  the field of GRB 161004A  (Evans  et al., GCN 19979)  with 
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. 
We obtained several images in R filter starting on Oct. 04 (UT) 
13:36:52.  In a combined image of the first 30 minutes of our 
observations we detect the afterglow (Breeveld et al., GCN 19984). 
Preliminary photometry of a combined image is following

Date       UT start   t-T0   Filter   Exp.  OT     Err.  UL
                       (mid, days)     (s)
2016-10-04 13:36:52 0.03632  R       9*180  21.65  0.25  21.7

Photometry is based on nearby SDSS-DR9 stars used in GCN 19980.


GRB_name: GRB161004A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20012
SUBJECT: GRB 161004A: Maidanak optical observations
DATE:    16/10/08 00:26:58 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), B. Hafizov (UBAI), A. Volnova 
(IKI), O. Burhonov (UBAI) report on behalf of larger GRB follow-up 
collaboration:

We observed the field of GRB 161004A  (Evans  et al., GCN 19979) with 
AZT-22 telescope of Maidanak observatory equipped with SNUCAM in R 
filter starting on Oct. 04 (UT) 14:25:10. We  clearly detected optical 
afterglow  (Evans  et al., GCN 19979; Breeveld et al., GCN 19984; 
Mazaeva et al., GRB 20011). Preliminary photometry  of the afterglow in 
a combined image is following

Date         UT start   t-T0    Filter   Exp.     OT    Err.   UL
                        (mid, days)        (s)

2016-10-04   14:25:10  0.06981  R        15*120   22.0  0.15   22.7

Photometry is based on nearby SDSS-DR9 stars used in GCN 19980.


GRB_name: GRB161007A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20013
SUBJECT: GRB 161007A: Enhanced Swift-XRT position
DATE:    16/10/08 03:08:17 GMT
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 2452 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 161007A, 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 = 103.40903, +23.30704 which is equivalent
to:

RA (J2000): 06h 53m 38.17s
Dec (J2000): +23d 18' 25.4"

with an uncertainty of 2.2 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.


GRB_name: GRB161007A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20014
SUBJECT: GRB 161007A: GTC observations
DATE:    16/10/08 04:32:45 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC), D. A. Kann (TLS Tautenburg), 
L. Izzo, C. C. Thoene (both IAA-CSIC), N. Castro-Rodriguez, and 
G. Gomez Velarde (GRANTECAN/IAC/Universidad de La Laguna) 
report:

We observed the field of GRB 161007A (Swift 716127, D'Elia et al., 
GCN #20008), with the 10.4m GTC on La Palma, Canary Islands, 
Spain. We obtained four 30 sec images in the Sloan i' band at an 
airmass of 1.8. The midtime of our observations was 0.2228 days 
after the GRB trigger.

At the UVOT-enhanced Swift XRT position (Goad et al., GCN #20013), 
we detect a source at the edge of the error circle, at:

RA (J2000) =     06:53:38.10
Dec. (J2000) = +23:18:24.6

For this source, we measure:

iâ€™ (Vega) = 22.23 +/- 0.15 

The photometric calibration was done by comparing to USNOB-1.0 
stars in the I-band filter, therefore this is only a preliminary value.
 
No statement can be made about fading. We note that the X-ray 
spectrum of this GRB's afterglows shows evidence for excess 
absorption, therefore this may be a dark GRB, with this source being 
its host galaxy. The source looks extended in our image, which has a 
seeing of 1.2".


GRB_name: GRB161007A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20015
SUBJECT: GRB 161007A: Swift-XRT refined Analysis
DATE:    16/10/08 09:34:15 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

T.G.R. Roegiers (PSU), L.M. McCauley (PSU), J.A. Kennea (PSU), S.L.
Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB) and V. D'Elia report on behalf of the Swift-XRT team:

We have analysed 7.4 ks of XRT data for GRB 161007A (D'Elia et al. GCN
Circ. 20008), from 114 s to 24.7 ks after the  BAT trigger. The data
comprise 228 s in Windowed Timing (WT) mode (the first 8 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. 20010).

The late-time light curve (from T0+5.0 ks) can be modelled with a
power-law decay with a decay index of alpha=0.8 (+/-0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.69 (+/-0.09). The
best-fitting absorption column is  7.5 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 1.7 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.65 (+0.25, -0.23)
and a best-fitting absorption column of 5.5 (+1.9, -1.6) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.1 x 10^-11 (7.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.5 (+1.9, -1.6) x 10^21 cm^-2
Galactic foreground: 1.7 x 10^21 cm^-2
Excess significance: 4.0 sigma
Photon index:      1.65 (+0.25, -0.23)

If the light curve continues to decay with a power-law decay index of
0.8, the count rate at T+24 hours will be 3.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x
10^-13 (2.2 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/00716127.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161007A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20016
SUBJECT: GRB 161007A: Swift/UVOT Upper Limits
DATE:    16/10/08 17:29:28 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and V. D'Elia (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161007A
133 s after the BAT trigger (D'Elia et al., GCN Circ. 20008). No
optical afterglow consistent with the XRT position (Goad et al., GCN
Circ. 20013) or the possible GTC optical counterpart (de Ugarte
Postigo et al., GCN Circ. 20014) 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 early
exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white              133         1716          411         >20.79
v                  621         1593          116         >18.39
b                  547         1691          116         >19.26
u                  291         1666          343         >19.73
uvw1               671         1642          116         >18.69
uvm2               646         1617          116         >18.81
uvw2               596         1735          129         >19.04


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.12 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161007A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20017
SUBJECT: GRB 161007A: Swift-BAT refined analysis
DATE:    16/10/08 21:13:40 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
V. D'Elia (ASDC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161007A (trigger #716127)
(D'Elia, et al., GCN Circ. 20008).  The BAT ground-calculated position is
RA, Dec = 103.408, 23.289 deg which is
    RA(J2000)  =  06h 53m 37.9s
    Dec(J2000) = +23d 17' 18.8"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 87%.

The mask-weighted light curve shows a peak starting from T+20 sec,
peaking at T+40 sec and ending at T+100 sec.  There is a hint of an
extended emission up to T+250 sec.  T90 (15-350 keV) is 201.7 +- 40.3 sec
(estimated error including systematics).
  
The time-averaged spectrum from T+18.2 to T+105.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.46 +- 0.18.  The fluence in the 15-150 keV band is 1.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+33.81 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/716127/BA/


GRB_name: GRB161007A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20018
SUBJECT: GRB 161007A: Mondy optical observations
DATE:    16/10/08 21:35:58 GMT
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 the the GRB 161007A (D'Elia et al., GCN 20008) 
with  AZT-33IK telescope of Sayan observatory (Mondy) starting on 
October, 07 (UT) 21:51:45. We obtained several images in R-filter. 
Within XRT error circle (Goad et al., GCN 20013) we do not detected any 
source. Preliminary photometry  of the field  is following

Date        UT start   t-T0      Filter Exp.   OT   UpLim (3 sigma)
                       (mid, days)       (s)

2016-10-07  21:51:45   0.03025   R      35*60  n/d  21.5

Photometry is based on nearby USNO-B1.0 stars
USNO-B1         R2
1133-0144160    15.67
1133-0144193    15.95
1133-0144230    14.48


GRB_name: GRB161007A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20019
SUBJECT: GRB 161007A: AbAO optical observations
DATE:    16/10/08 21:58:20 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), R. Inasaridze (AbAO), 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 the GRB 161007A (D'Elia et al., GCN 20008) with 
AS-32 (0.7m) telescope of Abastumani Observatory  on October, 07 (UT) 
22:14:13. We obtained several unfiltered images of the field. Within XRT 
error circle (Goad et al., GCN 20013) we do not detected optical 
afterglow candidate (de Ugarte Postigo et al., GCN 20014). Preliminary 
photometry  of the field  is following

Date        UT start   t-T0      Filter Exp.   OT   UpLim (3 sigma)
                       (mid, days)       (s)

2016-10-07  22:14:13   0.05758   CR     37*60  n/d  22.4

Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id R2
1133-0144160    15.67
1133-0144193    15.95
1133-0144230    14.48
1133-0144267    15.92
1133-0144281    15.23


GRB_name: GRB161007A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20020
SUBJECT: GRB 161007A: NOT optical observations
DATE:    16/10/10 10:47:07 GMT
FROM:    Kasper Elm Heintz at Cen.for Astrophys Cosmo/Dark Cosmology Cen  <heintz@dark-cosmology.dk>

K. E. Heintz (Univ. of Iceland and DARK/NBI), D. Malesani (DARK/NBI and DTU Space), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI), T. Pursimo (NOT), T. Kruehler (MPE Garching), J. Telting (NOT) and J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:

We observed the field of GRB 161007A (D'Elia et al., GCN 20008) using the ALFOSC camera mounted at the 2.56m Nordic Optical Telescope (NOT). Observations started at 04:39:59 UT on 2016-10-09 (i.e., 31 hr after the trigger) and 6x300 s SDSS i-band frames were obtained under excellent seeing (0.6-0.7").

In our stacked i-band image, we clearly detect the object reported by de Ugarte Postigo et al. (GCN 20014). We confirm that this source is extended.

No significant variability is measured with respect to the GTC images (taken 5.3 hr after the GRB) down to ~0.2 mag. The extension, the lack of variability, and the low chance probability association for such a bright object all indicate that this is the host galaxy of GRB 161007A.


GRB_name: GRB161010A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20021
SUBJECT: GRB 161010A: a long GRB detected by INTEGRAL
DATE:    16/10/10 14:33:02 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro@iasf-milano.inaf.it>

S.Mereghetti (INAF, IASF-Milano), D.Gotz (CEA,Saclay), C.Ferrigno, 
E.Bozzo, M.Tuerler (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on 
behalf of the IBAS Localization Team report:

a gamma ray burst lasting about 30 s has been detected by IBAS in the 
IBIS/ISGRI data at 13:36:32 UT of 2016 October 10.

The refined coordinates (J2000) are:

R.A.=  275.2178 deg
DEC.=  -28.7868 deg

with an uncertainty of  1.5   arcmin (90% c.l.).

The burst had a peak flux larger than 6 ph/cm2/s (20-200 keV, 1-s 
integration time) and a fluence in the same energy range larger than 4e-6 
erg/cmq. Note that due to telemetry saturation we can give only lower 
limits on fluence and peak flux.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB161010A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20022
SUBJECT: GRB 161010A: Swift ToO observations
DATE:    16/10/10 16:52:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a ToO observation of the INTEGRAL GRB 161010A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020702

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the INTEGRAL event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161011A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20023
SUBJECT: GRB 161011A: Swift detection of a burst
DATE:    16/10/11 06:07:15 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Y. Lien (GSFC/UMBC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 05:54:54 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161011A (trigger=716876).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 245.710, +8.326 which is 
   RA(J2000) = 16h 22m 51s
   Dec(J2000) = +08d 19' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 5 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 05:56:44.4 UT, 110.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 245.72866, 8.31221
which is equivalent to:
   RA(J2000)  = 16h 22m 54.88s
   Dec(J2000) = +08d 18' 44.0"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 82 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 5.25
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 5.16e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 117 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.07. 

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.)


GRB_name: GRB161011A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20024
SUBJECT: GRB 161011A: Prompt enhanced Swift-XRT position
DATE:    16/10/11 06:26:50 GMT
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 161011A, we find an
enhanced XRT position of the afterglow: RA, Dec: 245.7285, 8.3113 which
is equivalent to:
   RA (J2000)  = 16 22 54.85
   Dec (J2000) = +08 18 40.6
with an uncertainty of 2.2 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/716876.

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.


GRB_name: GRB161010A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20025
SUBJECT: GRB 161010A: Swift-XRT afterglow detection
DATE:    16/10/11 07:31:55 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@ifc.inaf.it>

L.M. McCauley (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), B. Mingo (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), B. Sbarufatti
(INAF-OAB/PSU) and P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of the INTEGRAL-detected
burst GRB 161010A (Mereghetti et al. GCN Circ. 20021), collecting 5.0
ks of Photon Counting (PC) mode data between T0+12.0 ks and T0+30.3 ks.


An uncatalogued X-ray source is detected consistent with being within
148 arcsec of the INTEGRAL position and is above the RASS limit and
fading with 3-sigma significance, and is therefore likely the GRB
afterglow. Using 123 s of PC mode data and 1 UVOT image, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 275.21435, -28.78515
which is equivalent to:

RA (J2000): 18h 20m 51.44s
Dec(J2000): -28d 47' 06.6"

with an uncertainty of 2.9 arcsec (radius, 90% confidence). This
position is 12 arcsec from the INTEGRAL position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.36 (+0.22, -0.21).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.78 (+0.18, -0.17). The
best-fitting absorption column is  3.1 (+0.9, -0.6) x 10^21 cm^-2,
consistent with the Galactic value of 2.5 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.2 x 10^-11 (5.7 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+0.9, -0.6) x 10^21 cm^-2
Galactic foreground: 2.5 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.78 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
1.36, the count rate at T+24 hours will be 0.023 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.9 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis of the likely afterglow
are at http://www.swift.ac.uk/ToO_GRBs/00020702/index_18.php.
The results of the full analysis of the XRT observations are available
at http://www.swift.ac.uk/ToO_GRBs/00020702.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161011A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20026
SUBJECT: GRB 161011A: Enhanced Swift-XRT position
DATE:    16/10/11 12:11:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 985 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 161011A, 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 = 245.72859, +8.31105 which is equivalent
to:

RA (J2000): 16h 22m 54.86s
Dec (J2000): +08d 18' 39.8"

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.


GRB_name: GRB161010A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20027
SUBJECT: Konus-Wind observation of GRB 161010A
DATE:    16/10/11 14:32:00 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov,  A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 161010A
(INTEGRAL IBIS/ISGRI detection: Mereghetti et al., GCN Circ. 20021) 
triggered Konus-Wind at T0=48993.832 s UT (13:36:33.832).

The burst light curve shows a single multipeaked emission episode
started at T0-4.7 s with a total duration of ~22 s.
The emission is seen up to 3 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161010_T48993/
Note: 'dips' in the count rate are due
to the GRB source occultation by the s/c structure.

As observed by Konus-Wind, the burst
had a fluence of 3.36(-0.38,+0.40)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.008 s,
of 1.07(-0.26,+0.26)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.10(-0.19,+0.23),
the high energy photon index beta = -2.17(-0.21,+0.13),
the peak energy Ep = 205(-39,+56) keV
(chi2 = 62/68 dof)

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB161011A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20028
SUBJECT: GRB 161011A: Swift-XRT refined Analysis
DATE:    16/10/11 16:05:58 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), K.L. Page (U. Leicester), B. Mingo (U. Leicester),
A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), A. D'Ai
(INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU) and V.
D'Elia report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 161011A (D'Elia et al. GCN
Circ. 20023), from 100 s to 23.1 ks after the  BAT trigger. The data
comprise 41 s in Windowed Timing (WT) mode (the first 8 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 Osborne et
al. (GCN Circ. 20024).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.77 (+0.19, -0.17), followed by a break at T+443 s to
an alpha of 0.06 (+0.08, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.75 (+0.18, -0.17). The
best-fitting absorption column is  7.8 (+5.1, -2.6) x 10^20 cm^-2,
consistent with the Galactic value of 5.3 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.8 x 10^-11 (4.3 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.8 (+5.1, -2.6) x 10^20 cm^-2
Galactic foreground: 5.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.75 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
0.06, the count rate at T+24 hours will be 0.072 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.7 x
10^-12 (3.1 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00716876.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161011A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20029
SUBJECT: GRB 161011A: Swift/UVOT Upper Limits
DATE:    16/10/11 17:23:48 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

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 161011A
118 s after the BAT trigger (D'Elia et al., GCN Circ. 20023).
No optical afterglow consistent with the XRT position
(Osborne et al., GCN Circ. 20026) 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) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC           118          268          147         >20.7
u_FC               330          580          246         >20.0
white              118         1009          334         >21.1
v                  660         6564          255         >19.4
b                  586        11301          252         >20.3
u                  330        11089         1170         >20.6
w1                 709         6889          152         >20.4
m2                6569         6769          197         >20.3
w2                1015         6359          216         >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20030
SUBJECT: GRB 161011A: TSHAO afterglow candidate
DATE:    16/10/11 22:10:02 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute),  A. 
Volnova (IKI),  I. Reva (Fesenkov Astrophysical Institute), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 161011A  (D'Elia et al., GCN 20023)  with 
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. 
We obtained several images in R filter starting on Oct. 11 (UT) 
13:13:27.  In the enhanced XRT error circle (Osborne al., GCN 20026) we 
marginally detect an object which is absent in SDDS-DR9 catalog. 
Preliminary photometry of the object which we suggest as an afterglow 
candidate is following

Date       UT start   t-T0    Filter  Exp.   OT     Err.  UL
                       (mid, days)     (s)
2016-10-11 13:13:27   0.32098 R       21*120 20.6   0.3   20.8

Photometry is based on nearby SDSS-DR9 stars (Lupton transformations):
SDSS-DR9_id            R
J162253.68+081834.3    15.26
J162242.22+082241.1    14.18
J162312.65+081527.2    14.72
J162302.30+081614.7    14.96

A finding chart can be found at 
http://grb.rssi.ru/GRB161011A/GRB161011A_TSHAO_161011_fc.png


GRB_name: GRB161011A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20031
SUBJECT: GRB 161011A: Swift burst of interest
DATE:    16/10/11 22:22:59 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL-UCL), N. Gehrels (GSFC), J. Kennea (PSU).

The light-curve of Swift GRB 161011A X-ray afterglow shows strong
variability around a flux level of a few 10^{-12} / erg cm^2 s.
The Swift team decleares this GRB a "burst of interest". We
encourage ground based follow up observations.


GRB_name: GRB161011A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20032
SUBJECT: GRB 161011A, Swift-BAT refined analysis
DATE:    16/10/12 03:08:56 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), (i.e. the Swift-BAT team):

Using the data set from T-790 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161011A (trigger #716876)
(D'Elia, et al. GCN Circ. 20023).  The BAT ground-calculated position is
RA, Dec = 245.687, 8.313 deg which is
   RA(J2000)  =  16h 22m 44.9s
   Dec(J2000) = +08d 18' 47.3"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.

The mask-weighted light curve shows a weak single-pulse structure that
starts at ~T0, peaks at ~ T+1 s, and ends at ~T+5 s. T90 (15-350 keV) is
4.3 +- 1.3 sec (estimated error including systematics).

The time-averaged spectrum from T-0.3 to T+4.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.15 +- 0.35.  The fluence in the 15-150 keV band is 2.3 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.37 sec in the 15-150 keV band
is 0.9 +- 0.3 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/716876/BA/


GRB_name: GRB161010A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20033
SUBJECT: GRB 161010A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/10/13 00:11:55 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

K. Yamaoka (Nagoya U), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama,
Y. Yamada (AGU), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa,
S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 161010A (Mereghetti et al., GCN Circ. 20021; Svinkin et al.,
GCN Circ. 20027; McCauley et al., GCN Circ. 20025) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 13:36:31.69 on 10 October 2016.
The burst signal was seen by the SGM instrument.

The light curve of the SGM shows a single weak peak starting at T0, peaking at
T+3 sec and ending at T+8 sec.  The T90 duration measured by the SGM data
is 4.9 +- 0.5 sec (40-1000 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1160141725/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB161010A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20034
SUBJECT: GRB 161010A: Swift/UVOT Possible Detection
DATE:    16/10/13 12:53:23 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161010A
3.3 hours after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 20021).
A source consistent with the XRT position
(McCauley et al., GCN Circ. 20025) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
     RA  (J2000) =  18:20:51.27 = 275.21364 (deg.)
     Dec (J2000) = -28:47:06.7  = -28.78519 (deg.)
with an estimated uncertainty of about 1 arc sec. (radius, 90% confidence).

As shown in the table below, the source faded in the observations
using the U filter, suggesting that it could be the afterglow
of the GRB. However, the GRB is only 7.8 degrees from 
the direction of the Galactic Center, and this is a crowded
field for UVOT. Consequently, the association of the source
with the GRB is not certain.

Preliminary magnitudes using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag
u                12034        13628         1035         18.8 +/- 0.1
u                17802        19985          744         19.0 +/- 0.1
u                23563        25993          794         19.4 +/- 0.2
u                29338        30137          787         20.4 +/- 0.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.54 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161014A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20035
SUBJECT: GRB 161014A: Swift detection of a burst
DATE:    16/10/14 12:49:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. L. Racusin (NASA/GSFC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
A. Melandri (INAF-OAB), B. Mingo (U Leicester),
K. L. Page (U Leicester), T. Sakamoto (AGU) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 12:31:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161014A (trigger=717500).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 332.628, +7.486 which is 
   RA(J2000)  =  22h 10m 31s
   Dec(J2000) = +07d 29' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows any short peaks
with a total duration of about 35 sec.  The peak count rate
was ~3200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 12:33:24.5 UT, 121.8 seconds after
the BAT trigger. No source was detected in 574 s of promptly downlinked
data, which covered 0% of the BAT error circle. We are waiting for the
full dataset to detect and localise the XRT counterpart. 

No UVOT data is available at this time. 

We note that this BAT trigger time is within 7 sec of a Fermi-GBM trigger
(trigger= 498141079). 

Burst Advocate for this burst is J. L. Racusin (judith.racusin AT nasa.gov). 
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.)


GRB_name: GRB161014A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20036
SUBJECT: GRB 161014A: MITSuME-Akeno optical observation
DATE:    16/10/14 13:14:41 GMT
FROM:    Yoichi Yatsu at Tokyo Tech.  <yatsu@hp.phys.titech.ac.jp>

K.Morita,  Y. Saito, Y. Ono, T. Yoshii, H. Ohuchi, Y.Tachibana, Y. Yano,
T.Fujiwara, S. Harita, Y.Muraki,  K.Saisho, T.Ozawa, Y. Yatsu, and N. Kawai
(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 161014A (J. L. Racusin et
al., GCN Circular #20035) with the
optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50
cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2016-10-14 12:32:08 UT (46 sec after the burst).
We found a candidate afterglow in the BAT error circle (J. L. Racusin,
GCNCircular
#20035), at
RA(J2000) = 22:10:35.47
Dec(J2000) = +07:28:07.6
with an uncertainty of ~0.4 arcsec.

 We obtained the following magnitude in Rc band.

T0+[sec]    MID-UT    T-EXP[sec]    Rc    Rc_err
â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”
     46       12:32:23         30       ~14.52   0.06
â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”â€”
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20037
SUBJECT: GRB161014A: optical afterglow candidate with the LCOGT-FTS
DATE:    16/10/14 13:20:55 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), C.G. Mundell 
(U. Bath), A. Gomboc (U. Nova Gorica) on behalf of a large collaboration 
report:

The 2-m LCOGT Faulkes Telescope South began observing Swift GRB161014A 
(Racusin et al., GCN 20035) in the SDSS r and i filters on October 14, 
12:44:15 UT (~13 minutes since trigger). Within the BAT error circle we 
find an uncatalogued object at the following position:

RA(J2000)=  22:10:35.47
Dec(J2000)= +07:28:07.3

with a 1 arcsec error radius and a magnitude of i~18 as calibrated 
against nearby SDSS stars.


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20038
SUBJECT: GRB 161014A : Xinglong TNT optical observation
DATE:    16/10/14 15:18:07 GMT
FROM:    L.P. Xin at NAOC  <xlp@nao.cas.cn>

L. P. Xin,   M. Zhai,  J. Y. Wei,  Y. L. Qiu,  J. S. Deng, 
J. Wang,  X. H. Han, L. H. Li and C. Wu on behalf of EAFON report:
 
We began to observe GRB 161014A (Racusin et al., GCN 20035) 
with Xinglong  0.8-m TNT telescope at 2016-10-14, 12:33:03(UT),
about 100 sec after the Swift trigger time. 
 
The new source reported by  Morita et al., (GCN 20036) and 
Guidorzi et al., (GCN 20037) was clearly detected  in the white images.  
Preliminary analysis shows that  the brightness of the optical afterglow
in R band is about 15.02 mag, calibrated by a nearby USNO B1.0 object
(22:10:31.5, +07:28:47, J2000, R=13.78mag), 
at the mid time of 110 sec after the burst.

This message could be cited. 

We thank the excellent support of the Xinglong 80cm TNT staff, particularly S. Liu


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20039
SUBJECT: GRB 161014A: Kanata optical observation
DATE:    16/10/14 16:56:59 GMT
FROM:    Michitoshi Yoshida at HASC,Hiroshima U  <yoshidam@hiroshima-u.ac.jp>

Nakaoka, T., Kawahara, N., Yang, C., Nagashima, H, Yoshida, M.,
Kawabata, K. (Hiroshima Univ.) on behalf of the OISTER collaboration

We performed R band imaging observations around the error circle of
GRB 161014A (Racusin et al., GCN 20035) with the optical imager HOWPol
attached to Kanata telescope of Hiroshima University. The observation
was made at 2016-10-14 12:32:48 UT (mid time of the observation). We
detected the optical transient reported by Morita et al. (GCN 20036),
Guidorzi et al. (GCN 20037) and Xin et al. (GCN 20038) in our R-band
image. The detected magnitude and five sigma upper limit (in Vega
magnitude) of the OT are listed below.

# T0+   MID-UT     T-EXP    R mag.   R err   R limit
-------------------------------------------------------
   86    12:32:48   30       15.1     0.2     17.0
-------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]


GRB_name: GRB161014A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20040
SUBJECT: GRB 161014A: Swift-XRT and UVOT afterglow detection
DATE:    16/10/14 19:04:03 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

P. D'Avanzo, S. R. Oates (U. of Warwick), A. Melandri (INAF-OAB), P. A. Evans (U. Leicester), F. E. Marshall (NASA/GSFC), J. L. Racusin (NASA/GSFC) report on behalf of the Swift team: 

We have analysed 1.9 ks of XRT data for GRB 161014A (Racusin et al. GCN Circ. 20035), from 108 s to 5.8 ks after the  BAT trigger. The data comprise 48 s in Windowed Timing (WT) mode (the first 7 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. Using 1696 s of PC mode data and 4 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 332.64764, +7.46858 which is equivalent to:

RA (J2000): 22h 10m 35.43s
Dec(J2000): +07d 28' 06.9"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

UVOT took a settling exposure of 9.8 seconds with the v filter starting 109 seconds after the BAT trigger. We find a source consistent with the position of the afterglow  reported by MITSuME (Morita et al GCN Circ 20036) and LCOGT FTS (Guidorzi et al., GCN Circ. 20037). The estimated magnitude is 16.52. No correction has been made for the expected extinction corresponding to E(B-V) of 0.08 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB161011A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20041
SUBJECT: GRB 161011A: RATIR Optical and NIR Observations
DATE:    16/10/14 19:25:39 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G.
Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC),
Josh Bloom (UCB), Antonino Cucchiara (UVI), Owen Littlejohns
(ASU), Enrico Ramirez-Ruiz (UCSC), Jos A. de Diego (UNAM),
Leonid Georgiev (UNAM), Jess Gonzlez (UNAM), Carlos
Romn-Ziga (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 161011A (D'Elia, et al., GCN 20023) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astronmico Nacional on
Sierra San Pedro Mrtir from 2016/10 13.11 to 2016/10 13.15 UTC (44.66
to 45.69 hours after the BAT trigger), obtaining a total of 0.69 hours
exposure in the r and i bands and 0.27 hours exposure in the Z,
Y, J, and H bands.

We do not detect the optical source reported by Mazaeva, et al. (GCN 20030).
For a source within the Swift-XRT error circle (Osborne, et al., GCN 20026),
in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detections and upper limits (3-sigma):

  r > 23.4
  i > 22.7
  Z > 21.7
  Y > 21.4
  J > 21.0
  H > 20.7

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astronmico Nacional in San Pedro
Mrtir.


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20042
SUBJECT: GRB 161014A: TSHAO optical observations
DATE:    16/10/15 00:07:46 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute),  I. 
Reva (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 161014A  (Racusin et al., GCN 20035)  with 
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. 
We obtained several images in R filter starting on Oct. 14 (UT) 
13:48:35. We detected the afterglow of GRB 161014A (Morita et al., GCN 
20036; Guidorzi et al., GCN 20037; Xin et al., GCN 20038). Preliminary 
photometry of  of combined the first observational set is following

Date       UT start   t-T0   Filter   Exp.   OT   Err.  UL
                       (mid, days)     (s)
2016-10-14 13:48:35   0.07046  R      21*120 19.0 0.10  20.6

Photometry is based on nearby SDSS-DR9 stars (Lupton transformations):
SDSS-DR9_id         R(Lupton)

J221053.78+072643.3    14.88
J221018.77+072726.4    14.05
J221023.66+073006.3    15.49
J221024.28+072335.5    15.75
J221050.55+072341.7    17.10


GRB_name: GRB161014A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20043
SUBJECT: GRB 161014A: GTC spectroscopy
DATE:    16/10/15 00:26:17 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C. Thoene (IAA-CSIC),
L. Izzo (IAA-CSIC), D.A. Kann (TLS Tautenburg), P. Pessev 
(IAC, ULL, GRANTECAN), A. Tejero (GRANTECAN) report on behalf 
of a larger collaboration:

We observed the afterglow of GRB 161014A (Racusin et al., GCN 20035, 
Morita et al. GCN 20036, Guidorzi et al. GCN 20037, Xin et al. 
GCN 20038, Nakaoka et al. GCN 20039, Dâ€™Avanzo et al. GCN 20040, 
Mazaeva et al. GCN 20042) with OSIRIS at the 10.4m GTC telescope on 
La Palma (Spain). The observations started at 20:52 UT (with an average 
epoch at 8.8 hr after the burst) and consisted of 3 x 900 s spectra using 
grism R1000B, which covers the spectral region between 3700 and 7800 AA 
at a resolution of R ~ 1000.

The spectrum has a low signal to noise ratio, but the preliminary reduction 
with archive calibrations still reveals prominent features due to Ly-alpha, 
SiII, CII, SiIV, CIV, AlII, and AlIII at a common redshift of z=2.823, which 
we identify as the redshift of the GRB.


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20044
SUBJECT: GRB161014A: NOT optical observations
DATE:    16/10/15 00:35:17 GMT
FROM:    Kasper Elm Heintz at Univ. of Iceland and DARK/NBI  <heintz@dark-cosmology.dk>

K. E. Heintz (Univ. of Iceland and DARK/NBI), D. Xu (NAOC), D. Malesani (DARK/NBI and DTU Space), E. Poretti (INAF/OABr), J. Telting (NOT), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI) and J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:

We observed the field of GRB 161014A (Racusin et al., GCN 20035) using the ALFOSC camera mounted at the 2.56m Nordic Optical Telescope (NOT). Observations started at 21:22:59 UT on 2016-10-14 (i.e., 8.85 hr after the trigger) and SDSS g-/r-/i-filter frames were obtained with 4x300 s in each filter in a cloudy weather.

In the stacked r- and i-bands we clearly detect the optical afterglow of the burst (Morita et al., GCN 20036, Guidorzi et al., GCN 20037, Xin et al., GCN 20038, Nakaoka et al., GCN 20039 and Mazaeva et al., GCN 20042).

We measure a magnitude of m(r) = 21.60 +/- 0.06 AB mag at a median time of 9.44 hr post-burst, calibrated with nearby SDSS stars.


GRB_name: GRB161014A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20045
SUBJECT: GRB 161014A: Swift/UVOT Detection
DATE:    16/10/15 10:59:41 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (U. of Warwick) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161014A
4 ks after the BAT trigger (Racusin et al., GCN Circ. 20035).
A source consistent with the optical position reported by MITSuME (Morita et al GCN Circ 20036)
and LCOGT-FTS (Guidorzi et al., GCN Circ. 20037) is detected in the
initial UVOT exposures. The lack of detection in the u and UV bands
is consistent with the redshift of 2.823 reported by GTC
(de Ugarte Postigo et al., GCN Circ. 20043).

The preliminary UVOT position is:
    RA  (J2000) =  22:10:35.46 = 332.64775 (deg.)
    Dec (J2000) =   7:28:07.3  =   7.46869 (deg.)
with an estimated uncertainty of about 0.9 arc sec. (radius, 90% confidence).

Preliminary magnitudes using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag
wh       4491          4690          197       20.4 +/- 0.3
wh       5929          6129          197       > 20.85
v       4903          5103          197       19.1 +/- 0.4
b       4286          5924          393         20.3 +/- 0.3
u       4081          23870         1630        > 20.9
w1       5314          23503         1968        > 21.0
m2       5109          18128         1163        > 20.8
w2       4698          6335          393         > 20.2

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).


GRB_name: GRB161014A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20046
SUBJECT: GRB 161014A: Continued MITSuME Akeno Optical Observation 
DATE:    16/10/15 11:33:51 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

K.Morita, T.Fujiwara, Y. Saito, Y. Ono, T. Yoshii, H. Ohuchi, Y.Tachibana, Y. Yano, S. Harita, Y.Muraki,  K.Saisho, T.Ozawa, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We have been observing the optical counterpart of GRB 161014A (J. L. Racusin et al., GCN
Circular #20035) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2016-10-14 12:32:08 UT (46 sec after the burst) and
we detected the optical counterpart in all three bands.
The measured magnitudes were listed as follows.

We obtained following results for the magnitudes.

T0+[sec]    MID-UT      T-EXP[sec]         g'              Rc                      Ic
-------------------------------------------------------------------------------------------------------
46            12:34:48        270                  16.67 +/- 0.13         15.69 +/- 0.08      15.40 +/- 0.07
376           13:03:53        1380                 > 18.57                17.59 +/- 0.17      17.86 +/- 0.25
-------------------------------------------------------------------------------------------------------

T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20047
SUBJECT: GRB 161014A: AROMA-N Optical Observation
DATE:    16/10/15 11:38:58 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Kitaoka, T. Sakamoto, A. Yoshida (AGU)

We observed the field of GRB 161014A detected by Swift
(Racusin et al., GCN Circ. 20035) with the 12-inch AGU Robotic
Optical Monitor for Astrophysical object - Narrow (AROMA-N)
located at the Sagamihara campus of Aoyama Gakuin University.

20 images of 60 sec exposures were taken in the R filter starting
from October 14 12:47:48 (UT) about 1200 seconds after the trigger
and stopped on October 14 13:13:14 (UT).  We do not detect the optical
afterglow (Morita et al., GCN Circ. 20036; Guidorzi et al., GCN Circ. 20037;
Xin et al., GCN Circ. 20038; Nakaoka et al., GCN Circ. 20039;
D'Avanzo et al., GCN Circ. 20040; Mazaeva et al., GCN Circ. 20042;
de Ugarte Postigo et al., GCN CIrc. 20043) both in the individual
images and the stacked image.  The estimated five sigma upper limit
of the combined image (total exposure of 1200 sec) is ~15.9 mag
using the USNO-B1 catalog.


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20048
SUBJECT: GRB 161014A: TNG optical observations
DATE:    16/10/15 12:08:09 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri, P. D'Avanzo (INAF-OAB), V. D'Elia (INAF/OAR & ASI/ASDC), W. Boschin, D. Carosati (INAF-TNG) report on behalf of the CIBO collaboration: 

We observed the field of GRB 161014A (Racusin et al., GCN 20035) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped with DOLoRes. Observations were carried out in the r-sdss filter. Observations started on Oct 15 at 00:19:03 UT (~11.8 hours after the burst) and consist in a single image lasting 120 seconds. 

The optical afterglow (Morita et al., GCN 20036 and GCN 20046; Guidorzi et al., GCN 20037; Xin et al., GCN 20038; Nakaoka et al., GCN 20039; Mazaeva et al., GCN 20042; Heintz et al. GCN 20044; Kitaoka et al., GCN 20047) is detected with a magnitude r(AB) = 21.5 +/- 0.3 (calibrated against nearby SDSS stars).


GRB_name: GRB161014A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20049
SUBJECT: GRB 161014A: Swift-BAT refined analysis
DATE:    16/10/15 14:04:09 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC), 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 161014A (trigger #717500)
(Racusin, et al., GCN Circ. 20035).  The BAT ground-calculated position is
RA, Dec = 332.626, 7.467 deg which is
    RA(J2000)  =  22h 10m 30.1s
    Dec(J2000) = +07d 28' 01.9"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 13%.

The mask-weighted light curve shows a complex structure starting at T-10 sec
and ending at T+15 sec.  T90 (15-350 keV) is 18.3 +- 2.8 sec (estimated error
including systematics).

The time-averaged spectrum from T-9.1 to T+12.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.47 +- 0.15.  The fluence in the 15-150 keV band is 1.9 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.10 sec in the 15-150 keV band
is 2.9 +- 0.6 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/717500/BA/


GRB_name: GRB161014A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20050
SUBJECT: GRB 161014A: Swift-XRT refined Analysis
DATE:    16/10/15 14:31:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri
(INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R.
Roegiers (PSU) and J.L. Racusin report on behalf of the Swift-XRT team:

We have analysed 5.5 ks of XRT data for GRB 161014A (Racusin et al. GCN
Circ. 20035), from 108 s to 34.8 ks after the  BAT trigger. The data
comprise 48 s in Windowed Timing (WT) mode (the first 7 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. Using 5612 s of PC mode data and 8 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 332.64760, +7.46873
which is equivalent to:

RA (J2000): 22h 10m 35.42s
Dec(J2000): +07d 28' 07.4"

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.45 (+/-0.12), followed by a break at T+1757 s to an
alpha of 1.59 (+0.14, -0.13).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.83 (+0.11, -0.10). The
best-fitting absorption column is  1.5 (+0.9, -0.8) x 10^22 cm^-2, at a
redshift of 2.823, in addition to the Galactic value of 7.5 x 10^20
cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.7 x
10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 7.5 x 10^20 cm^-2
Intrinsic column:    1.5 (+0.9, -0.8) x 10^22 cm^-2 at z=2.823
Photon index:      1.83 (+0.11, -0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00717500.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161014A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20051
SUBJECT: GRB 161014A: Fermi GBM observation
DATE:    16/10/15 16:16:43 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (Politecnico & INFN Bari)
reports on behalf of the Fermi GBM Team:


"At 12:31:15.91 UT on 14 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161014A (trigger 498141079 / 161014522),
which was also detected by the Swift/BAT (Racusin et al. 2016, GCN 20035).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 69 degrees.

The GBM light curve shows multiple peaks with a duration (T90) of
about 37 s (50-300 keV).
The time-averaged spectrum from T0-6 s to T0+23 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.74 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 167 +/- 15 keV.
The event fluence (10-1000 keV) in this time interval is
(5.4 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7 s in the 10-1000 keV band
is 5.7 +/- 0.3 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161014A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20052
SUBJECT: GRB 161014A: RATIR Optical and NIR Observations
DATE:    16/10/15 23:51:01 GMT
FROM:    V. Zach Golkhou at ASU/RATIR  <golkhou@gmail.com>

V. Zach Golkhou (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), 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), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley
(GSFC), John Capone (UMD), and Vicki Toy (UMD) report:

We observed the field of GRB 161014A (Racusin, et al., GCN 20035) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2016/10 15.20 to 2016/10 15.39 UTC (16.17 to
20.80 hours after the BAT trigger), obtaining a total of 2.72 hours
exposure in the r and i bands and 1.22 hours exposure in the Z, Y, J, and H
bands.

For a source within the Swift-XRT error circle (Mingo, et al., GCN 20050),
in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detections and upper limits (3-sigma):

  r 22.89 +/- 0.12
  i 22.24 +/- 0.10
  Z 22.01 +/- 0.15
  Y > 21.60
  J 21.19 +/- 0.15
  H > 20.48

This source is consistent with the source reported in Morita  et al., (GCNs
20036, 20046), Guidorzi et al., (GCN 20037), Xin et al., (GCN
20038), Nakaoka et al., (GCN 20039),  Mazaeva et al., (GCN
20042), and Melandri et al., (GCN 20048). These magnitudes are in the AB
system and are not corrected for Galactic extinction in the direction of
the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161004A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20053
SUBJECT: GRB161004A: Further analysis of the burst nature
DATE:    16/10/16 00:06:51 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. D. Barthelmy (GSFC), P.A. Evans (U Leicester), N. Gehrels (GSFC),
A. Y. Lien (GSFC/UMBC), J. P. Norris (BSU), P. O'Brien (U Leicester),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
and H. Ziaeepour report on behalf of the Swift Team:

We performed further analysis of GRB161004A (trigger #715084;
Evans et al., GCN Circ. 19979), to explore the possibility to
clarify its short/long nature.

Using the full BAT event data set from T-240 to T+962 sec,
the updated T90 is 3 +/- 1.4 s (using the 1-s binned light curve).
This T90 is longer than the 1.08 +- 0.21 s originally reported
(Palmer et al, GCN Circ. 20001). However, we note that due to
the weakness of the burst, the standard pipeline finds a T90 that
varies from ~ 1.3 s to ~ 3 s when using light curves with different
bin sizes.

The image analysis with the BAT data in 15-150 keV finds no significant
detections for extended emission within several hundred seconds
after the trigger. However, the BAT image from T+250 s to T+350 s,
which is the time period around the peak of the XRT flare,
does show a slight increase of significance of 3.8 sigma (comparing
to ~ 1 to 2 sigma detections for other periods). Therefore, it is possible
that the XRT flare might be the second peak of the prompt emission, but
was close to the detection limit of the BAT.

The time averaged spectrum is best fit by a simple power-law model,
with an index of 1.3 +/- 0.33. This value is consistent with the average
value of the short GRB distribution, and slightly on the harder side of the
long burst distribution, but still within the majority (Lien & Sakamoto et al.
2016).

The lag analysis is still unavailable due to the weakness of the burst
(Palmer et al, GCN Circ. 20001).

The bright flare in the XRT light curve around T+300 s is unusual
for short GRBs. However, Swift have detected short GRBs with
flares before (e.g., GRB 070724A, GRB 100816A; Margutti et al., 2011,
MNRAS, 417, 2144), and thus we cannot rule out the short-burst
possibility base on this.

Therefore, we conclude that the burst nature remains ambiguous
with current information.


GRB_name: GRB161015A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20054
SUBJECT: GRB 161015A: Fermi-LAT detection
DATE:    16/10/16 02:25:49 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hep01.hepl.hiroshima-u.ac.jp>

Masanori Ohno (Hiroshima Univ.), E. Bissaldi (Politecnico & INFN Bari), J.
E. McEnery (NASA/GSFC), M. Arimoto (Tokyo Tech) and G. Vianello (Stanford)
report on behalf of the Fermi-LAT team:

At 17:03:07.04 on October, 15, 2016 Fermi-LAT detected high-energy emission
from GRB 161015A, which was also detected by Fermi-GBM (trigger 498243790 /
161015710).

The best LAT on-ground location is found to be
RA, Dec = 269.15, 30.19 (J2000)
with an error radius of 0.21 deg (90 % containment, statistical error
only).
This was 50 deg from the LAT boresight at the time of the trigger and
triggered an autonomous repoint of the spacecraft.
The data from the Fermi-LAT show a significant increase in the event rate
that is spatially and temporally correlated with the trigger with high
significance.
The highest-energy photon is a 1.5 GeV event which is observed 72 seconds
after the GBM trigger.
A Swift ToO has been requested for this burst.
The Fermi-LAT point of contact for this burst is Masanori Ohno (
ohno@hep01.hepl.hiroshima-u.ac.jp)


The Fermi-LAT is a pair conversion telescope designed to cover the energy
band from 20 MeV to greater than 300 GeV. It is the product of an
international collaboration between NASA and DOE in the U.S. and many
scientific institutions across France, Italy, Japan and Sweden.


GRB_name: GRB161015A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20055
SUBJECT: GRB 161015A: Tiled Swift observations
DATE:    16/10/16 03:46:29 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 161015A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00059

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161015A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20056
SUBJECT: GRB 161015A: Fermi GBM detection
DATE:    16/10/16 04:08:41 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

M Stanbro (UAH) and C Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 17:03:07.03 UT on 15 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161015A (trigger 498243791 / 161015710),
which was also detected by the Fermi-LAT
(Masanori Ohno et al. 2016, GCN 20054)
The GBM on-ground location is consistent with the Fermi-LAT position.

The GBM light curve consists of 3 episodes
with a duration (T90) of about 15 s (50-300 keV).
The time-averaged spectrum from T0-0.003 s to T0+16.384 s is
best fit by a Band function with Epeak = 151 +/- 9 keV,
alpha = -0.82 +/- 0.05, and beta = -2.32 +/- 0.11.

The event fluence (10-1000 keV) in this time interval is
(1.17 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.24 s in the 10-1000 keV band
is 10.58 +/- 0.30 ph/s/cm^2.

A power law function with an exponential
high-energy cutoff fits the spectrum equally well
with Epeak= 183 +/- 7 keV, alpha = -0.93 +/- 0.03.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."

-- 
Matthew C. Stanbro
Fermi GBM Graduate Research Assistant
University of Alabama in Huntsville


GRB_name: GRB161015A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20057
SUBJECT: GRB 161015A: Swift-XRT observations
DATE:    16/10/16 15:11:23 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, A. Melandri (INAF-OAB), P. A. Evans (U. Leicester), 
report on behalf of the Swift-XRT team: 

Swift-XRT has performed follow-up observations of the Fermi/LAT-detected 
burst GRB 161015A (Masanori Ohno et al., GCN 20054; Stanbro & Meegan, 
GCN Circ. 20056) in a series of observations tiled on the sky. The total 
exposure time is 5 ks, distributed over 4 tiles. The data were collected 
between T0+38.2 ks and T0+45.8 ks, and are entirely in Photon Counting 
(PC) mode. 

An uncatalogued X-ray source is detected within the Fermi/LAT error circle. 
The position of this source is RA, Dec=269.2518, +30.37356 which is 
equivalent to:

RA (J2000): 17:57:00.43
Dec(J2000): +30:22:24.8

with an uncertainty of 2.7 arcsec (radius, 90% confidence). This
position is 12.2 arcmin from the Fermi/LAT position. The source has a 
0.3-10 keV count rate of about 0.03 ct/sec. We cannot determine fading 
at this time.

[GCN OPS NOTE(17oct16): Per author's request, the GRB name in the first sentence
was corrected from 16A to 15A.]


GRB_name: GRB161014A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20058
SUBJECT: GRB 161014A: refined analysis of TSHAO optical observations
DATE:    16/10/16 15:59:49 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute),  I. 
Reva (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 161014A  (Racusin et al., GCN 20035)  with 
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. 
We obtained several images in R filter starting on Oct. 14 (UT) 
13:48:35. Preliminary light curve of the afterglow  (Morita et al., GCN 
20036; Guidorzi et al., GCN 20037; Xin et al., GCN 20038;  Nakaoka et 
al., GCN 20039; Mazaeva et al., GCN 20042; Heintz et al., GCN 20044) can 
be found at http://grb.rssi.ru/GRB161014A/GRB161014A_TSHAO_LC.png

Photometry is based on nearby SDSS-DR9 stars used in GCN 20042 (Mazaeva 
et al.)


GRB_name: GRB161014A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20059
SUBJECT: Konus-Wind observation of GRB 161014A
DATE:    16/10/16 18:14:06 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 161014A (Swift/BAT observation:
Racusin et al., GCN 20035; Barthelmy et al., GCN 20049;
Fermi GBM observation: Bissaldi, GCN 20051)
triggered Konus-Wind at T0=45088.321 s UT (12:31:28.321).

The light curve shows a multi-peaked pulse with a duration
of ~25 s. A weak, soft pulse is also seen in the burst light
curve around ~T0+95 s, which KW ecliptic latitude response is
consistent with the position of GRB 161014A.
The emission is seen up to ~3 MeV.

As observed by Konus-Wind, the burst had a fluence of
(4.7 Â± 0.7)x10^-6 erg/cm2 and a 64-ms peak energy flux,
measured from T0-0.032, of (1.3 Â± 0.4)x10^-6 erg/cm2
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 5 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -1.15(-0.48,+0.73),
and the peak energy Ep = 226(-79,+267) keV,
chi2 = 92/78 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -1.8,
chi2 = 92/71 dof.

Assuming the redshift z=2.823 (de Ugarte Postigo et al., GCN 20043)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.3, and Omega_Lambda = 0.7,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~8.2x10^52 erg,
the peak luminosity L_iso is ~8.7x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~860 keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161014_T45088/

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB161015A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20060
SUBJECT: GRB161015A: AstroSat CZTI detection
DATE:    16/10/17 07:03:29 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.in>

V. Kumar, V. Sharma, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed clear detection of a bright GRB161015A (Fermi LAT detection: Masanori Ohno et al., GCN Circ. 20054) in the 40-200 keV energy range. The light curve shows a complex structure with peak at 17:03:08.04 UT after 1 second of the Fermi Trigger at 17:03:07.04 UT. The measured peak count rate is 660.0 counts/sec above the background in combined data of four quadrants, with a total of 2942.0 counts. The local mean background count rate was 320.0 counts/sec. Using cumulative rates, we measure a T90 of 22.0 secs.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb.  CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB161014A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20061
SUBJECT: GRB 161014A: VLT/X-shooter redshift confirmation 
DATE:    16/10/17 12:23:39 GMT
FROM:    Jonatan Selsing at DARK/NBI  <jselsing@dark-cosmology.dk>

J. Selsing (DARK/NBI), K. E. Heintz (Univ. of Iceland and DARK/NBI), D. Malesani
(DARK/NBI and DTU Space), D. Xu (NAOC), A. de Ugarte Postigo (IAA-CSIC and
DARK/NBI), N. R. Tanvir (Univ. Leicester), K. Wiersema (Univ. Leicester) and 
J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:

We have observed the optical afterglow of GRB 161014A (Racusin et al., GCN
20035; Morita et al. GCN 20036; Guidorzi et al., GCN 20037; D'Avanzo et al., GCN
20040), with the cross-dispersed echelle spectrograph, X-shooter, mounted at
VLT/UT2. Observations started 11.6 hours after the BAT trigger and consist of 4
x 1200 s integration time in the three spectral arms of X-shooter, covering 3000
- 21000 AA.

The afterglow continuum is detected in all arms at high significance. A broad
absorption trough from Lyman alpha is visible at 4650 AA, along with a number of
absorption lines spread across the rest of the afterglow continuum, among which
we identity absorption features due to Mg II, Si II, C II, C IV, Al II, Al III,
Fe II, all at a consistent redshift of z = 2.823, confirming the redshift
reported by de Ugarte Postigo et al. (GCN 20043).

We acknowledge excellent support from the ESO observing staff in Paranal, in
particular Jonathan Smoker, Thomas Rivinius, Marcela Espinoza and Dimitri Gadotti


GRB_name: GRB161015A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20062
SUBJECT: Konus-Wind observation of GRB 161015A
DATE:    16/10/17 13:30:12 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 161015A
(Fermi-LAT detection: Masanori Ohno et al., GCN Circ. 20054;
Fermi-GBM detection: Stanbro and Meegan, GCN Circ. 20056;
AstroSat-CZTI detection: Kumar et al., GCN Circ. 20060)
triggered Konus-Wind at T0=61386.899 s UT (17:03:06.899).

The burst light curve shows multipeaked structure
starting at ~T0-0.5 s and having a total duration of ~16 s.
The emission is seen up to 3 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161015_T61386/

As observed by Konus-Wind, the burst
had a fluence of 1.11(-0.08,+0.09)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.888 s,
of 4.01(-0.84,+0.85)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.12(-0.12,+0.13)
and Ep = 215(-26,+34) keV (chi2 = 60/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 60/72 dof)

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+8.448 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model:
with  alpha = -0.68(-0.14,+0.16)
and Ep = 256(-26,+32) keV (chi2 = 73/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -3.2
(chi2 = 73/72 dof)

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB161017A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20064
SUBJECT: GRB 161017A: Swift detection of a burst with a bright optical afterglow
DATE:    16/10/17 18:04:12 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/UMCP), D. N. Burrows (PSU),
P. D'Avanzo (INAF-OAB), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), K. L. Page (U Leicester), D. M. Palmer (LANL)
and T. N. Ukwatta (LANL) report on behalf of the Swift Team:

At 17:51:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161017A (trigger=718023).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 142.765, +43.142 which is 
   RA(J2000) = 09h 31m 04s
   Dec(J2000) = +43d 08' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 160 sec.  The peak count rate
was ~2100 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 17:52:48.8 UT, 57.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 142.7681, 43.1300 which is equivalent to:
   RA(J2000)  = +09h 31m 4.34s
   Dec(J2000) = +43d 07' 48.0"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 43 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 3.24e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of nominal 150.000 seconds with the White
filter starting 67 seconds after the BAT trigger. There is a candidate
afterglow in the list of sources generated on-board at
  RA(J2000)  = 09:31:04.58 = 142.76910
  DEC(J2000) = +43:07:36.3  =  43.12675
with a 90%-confidence error radius of about 1.10 arc sec. This position is 12.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
13.86. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.02. 

Burst Advocate for this burst is E. Troja (eleonora.troja AT nasa.gov). 
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.)


GRB_name: GRB161015A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20065
SUBJECT: GRB 161015A: Swift/UVOT observations
DATE:    16/10/17 19:48:19 GMT
FROM:    Massimiliano de Pasquale at IASF-Palermo  <m.depasquale@ucl.ac.uk>

M. De Pasquale (MSSL-UCL) and J. Cannizzo (NASA/UMBC) report on
behalf of the Swift/UVOT team:

The Swift/UVOT report started to observe the field of the putative X-ray
afterglow of GRB 161015A, the Fermi/LAT burst (Ohno et al. GCN
Circ. 20054, D'Avanzo et al. GCN Circ. 20057), 38 ks after the
LAT trigger.

No optical counterpart to this source is found. The 3 sigma upper limit
is given in the table below.

  T_start (s)  T_end (s)  Exposure Time (s)  filter   3s UL

   37991        45608         1210             u      >20.35

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).

-- 

Dr. Massimiliano De Pasquale
Research associate - Swift UVOT scientist
Mullard Space Science Laboratory, University College London


GRB_name: GRB161014A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20066
SUBJECT: GRB 161014A: Continued RATIR Optical and NIR Observations
DATE:    16/10/17 23:23:29 GMT
FROM:    V. Zach Golkhou at ASU/RATIR  <golkhou@gmail.com>

V. Zach Golkhou (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), 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), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley
(GSFC), John Capone (UMD), and Vicki Toy (UMD) report:

We observed the field of GRB 161014A (Racusin, et al., GCN 20035) with
the Reionization
and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold
Johnson Telescope at the Observatorio AstronÃ³mico Nacional on Sierra San
Pedro MÃ¡rtir from 2016/10 16.16 to 2016/10 16.26 UTC (39.29 to 41.69 hours
after the BAT trigger), obtaining a total of 1.78 hours exposure in the r
and i bands and 0.75 hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (Mingo, et al., GCN 20050)
and reported in Golkhou, et al. (GCN 20052), in comparison with the SDSS
DR9 and 2MASS catalogs, we obtain the following detection and upper limits
(3-sigma):

  r > 23.79
  i 23.57 +/- 0.32
  Z > 22.72
  Y > 22.57
  J > 22.20
  H > 21.91

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161017A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20067
SUBJECT: GRB 161017A: Enhanced Swift-XRT position
DATE:    16/10/18 04:38:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2929 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 161017A, 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 = 142.76888, +43.12633 which is equivalent
to:

RA (J2000): 09h 31m 4.53s
Dec (J2000): +43d 07' 34.8"

with an uncertainty of 1.4 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.


GRB_name: GRB161017A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20068
SUBJECT: GRB 161017A: Fermi GBM observation 
DATE:    16/10/18 05:00:56 GMT
FROM:    C. Michelle Hui at MSFC/Fermi-GBM  <c.m.hui@nasa.gov>

C. M. Hui (NASA/MSFC) and C Meegan (UAH)
report on behalf of the Fermi GBM Team:

At 17:52:08.26 UT on 17 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161017A (trigger 498419532/161017745), 
which was also detected by Swift (Troja et al., GCN 20064).  
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 125 degrees.

The GBM light curve shows two peaks with a duration (T90) 
of about 32 s (50-300 keV).  The time-averaged spectrum 
from T0-22.1 s to T0+8.6 s is adequately fit by a power law function 
with an exponential high-energy cutoff.  
The power law index is -1.04 +/- 0.09 and the cutoff energy, 
parameterized as Epeak, is 298.50 +/- 45.00 keV

The event fluence (10-1000 keV) in this time interval is
 (7.02 +/- 0.43)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.3 s in the 10-1000keV band is 5.6 +/- 0.5 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.


GRB_name: GRB161017A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20069
SUBJECT: GRB 161017A: Redshift from GTC
DATE:    16/10/18 06:22:19 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. A. Kann (TLS Tautenburg), 
C. Thoene (IAA-CSIC), L. Izzo (IAA-CSIC), R. Sanchez-Ramirez (IAA-CSIC), 
Z. Cano (IAA-CSIC), K. Bensch (IAA-CSIC), D. Garcia-Alvarez (IAC, ULL, 
GRANTECAN) and D. Perez Valladares (GRANTECAN) report :

We observed the afterglow of GRB 161017A (Yurkov et al., GCN 20063, 
Troja et al. GCN 20064) with OSIRIS at the 10.4m GTC telescope on 
La Palma (Spain). The observations started at 04:38:44 UT (10.78 hr after 
the burst) and consist of 3 x 900 s spectra using grism R1000B, which 
covers the spectral region between 3700 and 7800 AA at a resolution of 
R ~ 1000.

The r-band acquisition image shows the afterglow at a magnitude of r(AB) = 
18.24+/-0.07, as compared to several SDSS stars.

The spectrum shows a strong continuum with weak features of SiII, CIV, AlII, 
and FeII at a common redshift of 2.013, which we identify as the redshift of the 
GRB. Additionally, we detect two intervening systems at z=0.916 and z=1.370, 
both with MgII features.


GRB_name: GRB161017A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20070
SUBJECT: GRB 161017A: MITSuME Akeno Optical Observation 
DATE:    16/10/18 07:08:21 GMT
FROM:    Taketoshi Yoshii at Tokyo Tech  <yoshii.t.ac@m.titech.ac.jp>

T.Fujiwara, Y.Saito, Y. Tachibana, T. Yoshii, Y. Yano,
Y.Ono, S.Harita, Y.Muraki, K.Morita, T.Ozawa, K.Saisho,Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 161017A (E. Troja et al., GCN
Circular #20064) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2016-10-17 17:52:42 UT (51 sec after the burst) and
we detected the optical counterpart in g', Rc and Ic band.
The measured magnitudes were listed as follows.

We obtained following results for the magnitudes.

T0+[sec]    MID-UT      T-EXP[sec]         g'              Rc                      Ic
-------------------------------------------------------------------------------------------------------
51            17:52:57        30          14.55 +/- 0.06        13.78 +/- 0.05      13.38 +/- 0.06
87            17:55:41        240         14.35 +/- 0.05        13.61 +/- 0.04      13.25 +/- 0.04
331          18:03:41        600         15.50 +/- 0.05        14.73 +/- 0.04      14.42 +/- 0.04
996          18:28:35        2100       16.58 +/- 0.05        15.89 +/- 0.05      15.63 +/- 0.04
3320        19:15:35        2040       16.76 +/- 0.06        16.03 +/- 0.05      15.77 +/- 0.05
-------------------------------------------------------------------------------------------------------

T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20071
SUBJECT: GRB 161017A: TNG optical observations
DATE:    16/10/18 10:14:06 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri, P. D'Avanzo (INAF-OAB), V. D'Elia (INAF/OAR & ASI/ASDC), V. Lorenzi, Hristo Stoev (INAF-TNG) report on behalf of the CIBO collaboration: 

We observed the field of GRB 161017A (Troja et al., GCN 20064) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped with DOLoRes. Observations were carried out in the r-sdss filter. Observations started on Oct 18 at 03:51:18 UT (~10 hours after the burst) and consist in a single image lasting 120 seconds. 

The optical afterglow (Yurkov et al. GCN 20063; Troja et al. GCN 20064; de Ugarte Postigo et al. GCN 20069; Fujiwara et al. GCN 20070) is detected with a magnitude r(AB) = 17.9 +/- 0.1 (calibrated against nearby SDSS stars).


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20072
SUBJECT: GRB161017A: optical observations with 1-m LCOGT McDonald
DATE:    16/10/18 11:18:07 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), C.G. Mundell 
(U. Bath), A. Gomboc (U. Nova Gorica) on behalf of a large collaboration 
report:

The 1-m LCOGT McDonald telescope began observing Swift GRB161017A (Troja 
et al., GCN 20064) in the SDSS r filter on October 18, 10:03 UT (~0.67 
days since the GRB). We detect the optical afterglow (Yurkov et al. GCN 
20063; Troja et al. GCN 20064; de Ugarte-Postigo et al. GCN 20069; 
Fujiwara et al GCN 20070; Melandri et al. GCN 20071) with r=18.95 +- 
0.10 mag at 0.68 days mid epoch, as calibrated against nearby SDSS stars.


GRB_name: GRB161017A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20073
SUBJECT: GRB 161017A: Swift-XRT refined Analysis
DATE:    16/10/18 11:27:12 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), T.G.R. Roegiers (PSU), L.M. McCauley
(PSU), J.A. Kennea (PSU), S.L. Gibson (U. Leicester), J.P. Osborne (U.
Leicester) and E. Troja report on behalf of the Swift-XRT team:

We have analysed 7.6 ks of XRT data for GRB 161017A (Troja et al. GCN
Circ. 20064), from 51 s to 46.2 ks after the  BAT trigger. The data
comprise 595 s in Windowed Timing (WT) mode (the first 5 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 Beardmore
et al. (GCN Circ. 20067).

The late-time light curve (from T0+4.5 ks) can be modelled with a
power-law decay with a decay index of alpha=1.04 (+/-0.06).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.656 (+/-0.019). The
best-fitting absorption column is  7.5 (+/-0.7) x 10^21 cm^-2, at a
redshift of 2.013, in addition to the Galactic value of 1.8 x 10^20
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.99 (+0.10, -0.07) and a best-fitting absorption column of 4 (+20,
-4) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.2 x 10^-11 (3.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.8 x 10^20 cm^-2
Intrinsic column:    4 (+20, -4) x 10^20 cm^-2 at z=2.013
Photon index:      1.99 (+0.10, -0.07)

If the light curve continues to decay with a power-law decay index of
1.04, the count rate at T+24 hours will be 0.042 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.3 x
10^-12 (1.4 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00718023.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161017A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20074
SUBJECT: GRB 161017A: Swift/UVOT Detection
DATE:    16/10/18 12:34:01 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161017A
68 s after the BAT trigger (Troja et al., GCN Circ. 20064, Yurkov et 
al., GCN Circ. 20063).
The UVOT source described in Troja et al., GCN Circ. 20064, is at a 
position consistent with the enhanced XRT position (Beardmore et al., 
GCN Circ. 20067) and is found to be fading.

The preliminary UVOT position is:
     RA  (J2000) =  09:31:04.60 = 142.76915 (deg.)
     Dec (J2000) = +43:07:36.3  =  43.12676 (deg.)
with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).

Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early 
exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white               68          217          147         14.08 Â± 0.02
v                  609          629           20         15.14 Â± 0.09
b                  535          555           20         15.60 Â± 0.06
u                  280          529          246         14.56 Â± 0.02
uvw1               658          661          2.7         15.5  Â± 0.3

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.02 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20075
SUBJECT: GRB 161017A: Lomonosov Gamma Ray and MASTER Optical  prompt observations
DATE:    16/10/18 16:23:33 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V.A.Sadovnichy,
Lomonosov Moscow State University

M.I.Panasyuk,  S.I.Svertilov, A.V.Bogomolov, 
V.V.Bogomolov, N.L.Dzhioeva, A.M.Amelushkin, V.O.Barinova, A.F.Iyudin, 
V.V.Kalegaev, D.Nguen,  V.L. Petrov, I.V.Yashin, P.S.Kazarian
Physics Department, Skobel'tsyn Institute of Nuclear Physics, Moscow State

V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov, M.Panchenko, 
A.Kuznetsov, V.G.Kornilov, P. Balanutsa, E.Popova 
Lomonosov Moscow State University, Sternberg Astronomical Institute

V.Yurkov, A.Gabovich, Yu.Sergienko 
Blagoveschensk Educational State University, Blagoveschensk

N.M.Budnev, K.Ivanov, O.Gres, O.Chuvalaev, V.A.Poleshchuk, S.Yazev
Irkutsk State University

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

I. Park, J. Lee, S. Jeong
Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, 
Korea

At 17:52:17 UT on 17 Sep 2016, the Lomonosov BDRG  Gamma-ray Burst
Monitor  (http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg )
triggered GRB 161017A (E. Troja et al.,, GCN 20064).
GRB 161017A has several peaks LC, total duration ~100s,the energy range
70-300 keV.

The light curve is available at
http://master.sai.msu.ru/static/Lomonosov/GRB161017A_BDRG2.png

More information will be available at:
http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts

MASTER-Amur  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Blagoveschensk was pointed to the  GRB161017A 21 sec after 
notice time and 47 sec after Swift trigger time at 2016-10-17 17:52:38 UT 
in two polarizations. 
On  our first (10s exposure)  set we  marginally found  optical transient 
at  Yurkov et al. (GCN 20063) and Troja et al. (GCN 20064) position.
The 5-sigma upper limit has been about 14.5 mag .
The OT was became brighter up to maximum at 3-4  set .

The observations made on zenit distance = 53 degrees, galaxy latitude b = 
47 degree.
The moon (96 % bright part) is 50 degrees above the horizon. The distance 
between  moon and  object is 87
The sun  altitude  is -37.8 degree.


MASTER-Tunka  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka (Baykal lake) was pointed to the  GRB161017.74 75 sec 
after notice time 
and 103 sec after trigger time at 2016-10-17 17:53:34 UT. On our second 
(20s exposure)  set we haven't found optical transient  within SWIFT 
error-box (ra=09 31 03 dec=+43 08 31 r=0.050000).
The 5-sigma upper limit has been about 12.5 mag.

The observations made on zenit distance = 65 degrees, galaxy latitude b = 
47 degree.
The moon (96 % bright part) is 50 degrees above the horizon. The distance 
between  moon and  object is 87 degrees.
The sun  altitude  is -45.9 degrees.
The low mahnitude limit because dense fog due to Irkut (Famost Sibirian 
river) evaporation.

We imaged OT late.

MASTER-IAC  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located at Teide Observatory (Tenerife, Canary, Spain) was pointed to the 
GRB161017A  32942 sec after trigger time at 2016-10-18 03:00:53 UT. On our 
first (180s exposure)  set we found optical transient  on coaded images.
The 5-sigma upper limit has been about 17.8 mag

The observations made on zenit distance = 69 degrees, galaxy latitude b = 
47 degrees. The moon (94 % bright part) is 75 degrees above the horizon. 
The distance  between  moon and  object is 82 degrees.
The sun  altitude  is -54.1 degree.

Our preliminary photometry is next:

Time     Tstart  Tmid Expt    Site      Filter  Mag   eMag Filter  Mag   eMag

17:52:38    47    52   10   MASTER-Amur   P/   15.69   1.0  P\   15.46   1.0
17:53:07    71    76   10   MASTER-Amur   P/   14.05   0.3  P\   13.99   0.3
17:53:03    96   106   20   MASTER-Amur   P/   13.87   0.2  P\   13.63   0.2
17:54:03   131   146   30   MASTER-Amur   P/   13.90   0.3  P\   13.80   0.3
17:54:46   175   195   40   MASTER-Amur   P/   14.34   0.3  P\   14.34   0.3
17:55:41   229   254   50   MASTER-Amur   P/   15.03   0.4  P\
17:56:46   295   325   60   MASTER-Amur   P/   14.91   0.4  P\   14.91   0.4
17:58:12   381   540  240   MASTER-Amur   P/   15.88   0.4  P\   16.03   0.4
18:05:20   809   889  160   MASTER-Tunka  P|   15.64   0.2
03:00:53 32942 33464  900   MASTER-IAC    C    18.62   0.2
03:19:17 34046 34587  900   MASTER-IAC    C    18.60   0.2
03:38:01 35170 35726  900   MASTER-IAC    C    18.62   0.2
03:57:26 36335 36885  900   MASTER-IAC    C    18.68   0.2

Preliminary OT light curve is available at
http://master.sai.msu.ru/static/GRB161017A.png


The message may be cited.


GRB_name: GRB161017A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20076
SUBJECT: GRB 161017A: Swift-BAT refined analysis
DATE:    16/10/18 17:08:51 GMT
FROM:    Tilan Ukwatta at LANL  <tilan.ukwatta@gmail.com>

J. R. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP),
T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+833 sec from the recent
telemetry downlink, we report further analysis of BAT
GRB 161017A (trigger #718023) (Troja, et al., GCN Circ. 20064).
The BAT ground-calculated position is
RA, Dec = 142.770, 43.125 deg which is
   RA(J2000)  =  09h 31m 04.8s
   Dec(J2000) = +43d 07' 29.0"
with an uncertainty of 1.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 100%.

The mask-weighted light curve shows two main
episodes. The first multi-peak episode starts around T-5 sec,
and ends at ~T+50 sec. The second relatively weaker episode
starts at ~T+60 sec and ends around T+250 sec. T90 (15-350 keV)
is 216.3 +- 6.9 sec (estimated error including systematics).

The time-averaged spectrum from T-4.88 to T+233.42 sec is best
fit by a simple power-law model.  The power law index of the
time-averaged spectrum is 1.55 +- 0.06.  The fluence in the
15-150 keV band is 5.3 +- 0.2 x 10^-06 erg/cm2. The 1-sec peak
photon flux measured from T+17.78 sec in the 15-150 keV band
is 2.8 +- 0.2 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/718023/BA/


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20077
SUBJECT: GRB 161017A: GTC additional spectroscopy and refined redshift
DATE:    16/10/18 18:18:16 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC), A. F. Valeev (SAO-RAS), V. V. Sokolov (SAO-RAS), P. Ferrero (IAA-CSIC), J. C. Tello (IAA-CSIC), Y. Hu (IAA-CSIC), B.-B. Zhang (IAA-CSIC), S. Jeong (SKKU and IAA-CSIC), J. Cepa (IAC), S. R. Oates (U. of Warwick), D. Garcia-Alvarez (IAC, ULL, GRANTECAN), D. Perez Valladares (GRANTECAN), N. Castro-Rodriguez (GRANTECAN) and S. Fernandez (GRANTECAN) on behalf of a larger collaboration, report:

Following the detection of GRB 161017A by Swift (Troja et al. GCNC 20064), Fermi (Hui and Meegan, GCNC 20068)
and Lomonosov (Sadovnichy et al. GCNC 20075), we observed the optical afterglow (Yurkov et al. GCNC 20063; Breeveld and Troja, GCNC 20074) with the 10.4m Gran Telescopio Canarias (GTC) at the Spanish island of La Palma, starting at 05:59 UT on Oct 18 (i.e. 12.1 hr post-burst), with both the R1000B and R2500I OSIRIS grisms, covering a combined range of 3800-10000 A. The reddest spectrum (convering the range between 7350 and 10000 A at a resolution of 2500) shows the strong Mg II doublet at a redshift z = 2.0127, consistent with the value reported by de Ugarte Postigo et al. (GCNC 20069). We also identify, in the bluest spectrum, other absorption lines (eg. SiII, FeII) and the two intervening systems reported on their GTC (+OSIRIS) R1000B spectrum taken 1.3 hr earlier than us.

We acknowledge excellent support from the GTC staff.


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20078
SUBJECT: GRB 161017A: TNG spectroscopy and redshift confirmation
DATE:    16/10/18 20:02:16 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), D. Malesani (DARK/NBI and DTU Space), 
V. D'Elia (INAF/OAR & ASI/ASDC), A. Melandri (INAF-OAB), V. Lorenzi, 
H. Stoev (INAF-TNG) report on behalf of the CIBO collaboration: 

We observed the optical afterglow of GRB 161017A (Yurkov et al. GCN 20063; 
Troja et al. GCN 20064; de Ugarte Postigo et al. GCN 20069; Fujiwara et al. 
GCN 20070; Guidorzi et al. GCN 20072; Breeveld & Troja, GCN 20074; Sadovnichy 
et al. GCN 20075) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped 
with the DOLoRes camera in spectroscopic mode. Observations were carried out 
with the LR-B filter, covering the range 3500-8000 AA. The observations consisted of 
two spectra, each one lasting 1200 s, carried out at a mean time of Oct 18.1852 UT 
(~10.58 hours after the burst). 

The spectrum shows a clear continuum. We detect absorption features consistent 
with Li-alpha, Si II, C IV and Fe II lines at a common redshift of z = 2.01, together
with MgII intervening systems at z=0.92 and z=1.37, in agreement with the results 
reported by de Ugarte Postigo et al. (GCN 20069) and Castro-Tirado et al. (GCN 20077). 


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20079
SUBJECT: GRB161017A optical R band observations with SARA-RM
DATE:    16/10/18 21:59:31 GMT
FROM:    Dieter Hartmann at Clemson.U  <hdieter@clemson.edu>

A. Kaur (Clemson U.), G. Henson (ETSU), and D. H. Hartmann (Clemson U.)

report optical observations of GRB161017A discovered by Swift (Yurkov et al.,
GCN Circ. 20063;Troja et al., GCN Circ. 20064).



The UVOT source described in Troja et al., GCN Circ. 20064, is at a
position consistent with the enhanced XRT position (Beardmore et al.,GCN
Circ. 20067) and is  fading (Breeveld & Troja, GCN Circ. 20074) at the
preliminary UVOT position:

     RA  (J2000) =  09:31:04.60 = 142.76915 (deg.)

     Dec (J2000) = +43:07:36.3  =  43.12676 (deg.)

with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).



We observed the field on 2016-10-18.17 UT centered at 09:31:4.65
+43:07:36.34 (J2000), imaging for 20 minutes in the Cousins R filter with
the 1.0m JKT telescope (SARA-RM) located on La Palma, Canary Isles, Spain.
We detect the fading source at an R magnitude of 17.606 +/- 0.017 using the
Andor IkonL 2048 x 2048 CCD (11.6 x 11.6 arc min). The photometric standard
GD71 was utilized for calibration.



SARA is described at http://saraobservatory.org


GRB_name: GRB161017A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20080
SUBJECT: GRB 161017A: LT optical observations
DATE:    16/10/19 08:29:40 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), C.G. Mundell 
(U. Bath), A. Gomboc (U. Nova Gorica), N.R. Tanvir (U. Leicester) on 
behalf of a large collaboration report:

The 2-m Liverpool Telescope observed Swift GRB161017A (Troja et al., GCN 
20064) in the SDSS r and i filters on October 19, from 03:45 to 05:37 UT 
(mid time~1.45 days since the GRB). We clearly detect the optical 
afterglow (Yurkov et al. GCN 20063; Troja et al. GCN 20064; de 
Ugarte-Postigo et al. GCN 20069; Fujiwara et al GCN 20070; Melandri et 
al. GCN 20071) with the following values, as calibrated against nearby 
SDSS stars:

Mid Time      Exposure       Filter       Magnitude
(days)           (s)
-------------------------------------------------------
1.42            5x120         SDSS-R      20.02 +- 0.03
1.42            5x120         SDSS-I      19.80 +- 0.03
-------------------------------------------------------

Compared with our previous report (Guidorzi et al. GCN 20072), we 
estimate an average power-law decay index alpha~1.3 between 0.68 and 
1.45 days post burst.


GRB_name: GRB161017A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20081
SUBJECT: GRB161017A: NOEMA detection of the millimetre afterglow
DATE:    16/10/19 16:15:03 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (Weizmann Institute), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), M. Bremer, E. Chapillon, J. M. Winters (IRAM) and S. Martin (JAO) report on behalf a larger collaboration:

We conducted millimetre observations of GRB 161017A (Troja et al. GCN 20064) with the NOrthern Extended Millimeter Array (NOEMA; Plateau de Bure, France) at 93 and 133 GHz. Observations started at 6:51 UT on October 19 (i.e. 1.54 day after the burst).

We detect the afterglow at both frequencies. A preliminary analysis of the 93 GHz data reveals a flux density of 1.50 +/- 0.06 mJy. Further observations are scheduled.

We encourage follow-up observations at all frequencies.


GRB_name: GRB161017A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20082
SUBJECT: Konus-Wind observation of GRB 161017A
DATE:    16/10/19 17:42:56 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 161017A (Swift-BAT trigger #718023:
Troja et al., GCN 20064, T0(BAT)=17:51:51 UT;
Fermi-GBM observation: Hui & Meegan, GCN 20068;
Lomonosov observation: Sadovnichy et al., GCN 20075)
was detected by Konus-Wind in the waiting mode.

The light curve shows an emission pulse which starts
~10 s before the BAT trigger, peaks at ~T0(BAT)+7 s,
and lasts till ~T0(BAT)+28 s.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB161017_T64311/

As observed by Konus-Wind, the burst had a fluence of
(8.5 Â± 1.1)x10^-6 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+7 s, of (8.7 Â± 0.2)x10^-7 erg/cm2
(both in the 20 - 10000 keV energy range).

Modeling the KW 3-channel time-integrated spectrum
(from T0(BAT)-10 s to T0(BAT)+28 s) by a power law
with exponential cutoff (CPL) model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.25 Â± 0.16, and Ep = 289 Â± 73 keV.

Modeling the KW 3-channel spectrum near the peak count rate with
the CPL model yields alpha = -1.17 Â± 0.20, and Ep = 404 Â± 136 keV.

Assuming the redshift z=2.013 (de Ugarte Postigo et al., GCN 20069)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.3, and Omega_Lambda = 0.7,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~8.3x10^52 erg,
the peak luminosity L_iso is ~2.5x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~870 keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB161007A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20083
SUBJECT: GRB 161007A: 15 GHz upper limits from AMI
DATE:    16/10/20 10:33:59 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley (Hintze Fellow, Oxford), 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 
161007A (D'Elia et al., GCN 20008) 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 Oct 08.05, Oct 09.25, Oct 
11.25 and Oct 15.25 (UT) do not reveal any radio source at the XRT 
location (Goad et al., GCN 20013), with 3sigma upper limits of 372 uJy, 
273 uJy, 333 uJy and 222 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/.


GRB_name: GRB161011A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20084
SUBJECT: GRB 161011A: 15 GHz upper limits from AMI
DATE:    16/10/20 10:38:44 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley (Hintze Fellow, Oxford), 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 the 
burst of interest GRB 161011A (D'Elia et al., GCN 20023; Pasquale et 
al., GCN 20031) 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 Oct 11.44, Oct 13.66, Oct 14.60 and Oct 18.56 (UT) do not 
reveal any radio source at the XRT location (Osborne et al., GCN 20026), 
with 3sigma upper limits of 171 uJy, 117 uJy, 108 uJy and 147 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/.


GRB_name: GRB161015A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20085
SUBJECT: GRB 161015A: further Swift-XRT follow-up observations
DATE:    16/10/20 14:41:03 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

A. Melandri, P. D'Avanzo (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU) and J. Cannizzo (NASA/UMBC) report on behalf of the Swift team:

Swift-XRT carried out further observations of the field of the Fermi GRB 161015A (Ohno et al., GCN Circ. 20054; Stanbro & Meegan, GCN 20056) between T0+371.3 ks and T0+395.9 ks. The total exposure time is 5.0 ks, entirely in Photon Counting (PC) mode.

The source reported in D'Avanzo et al. (GCN Circ. 20057) as an X-ray afterglow candidate is no longer detected. The 3sigma u.l. is about 3.4e-3 ct/sec (corresponding to a 0.3-10 keV observed flux of 1.7e-13 erg cm^-2 s^-1, assuming a typical GRB spectrum). We thus confirm it as the X-ray afterglow associated with GRB 161015A.

This is an official product of the Swift-XRT team.


GRB_name: GRB161020A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20086
SUBJECT: GRB 161020A: A long GRB detected by INTEGRAL
DATE:    16/10/20 20:35:50 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro@iasf-milano.inaf.it>

S.Mereghetti (IASF-Milano), V. Savchenko (APC, Paris), D.Gotz (CEA, 
Saclay), C.Ferrigno (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on 
behalf of the IBAS Localization Team report:

a gamma ray burst lasting about 15 s has been detected by IBAS in the 
IBIS/ISGRI data at 00:34:40 UT of 2016 October 20. This burst was also 
detected by Fermi/GBM (trigger num. 498616490).

The burst occurred immediately after the end of a slew of the INTEGRAL 
satellite. For this reason the corresponding IBAS Alert was not 
distributed in real time.

From an offline analysis we derived the burst coordinates (J2000):

R.A.=  161.0309 deg
DEC.=  -54.7687 deg

with an uncertainty of about 2 arcmin (90% c.l.).

The burst had a peak flux of 0.8 counts/cm2/s (20-200 keV, 1-s integration 
time) and a fluence in the same energy range of about 4e-7 erg/cmq.

A plot of the light curve will be posted at 
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB161022A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20087
SUBJECT: GRB 161022A: Swift detection of a burst
DATE:    16/10/22 03:03:37 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. Stamatikos (OSU/NASA/GSFC), S. D. Barthelmy (GSFC),
J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and T. N. Ukwatta (LANL)
report on behalf of the Swift Team:

At 02:43:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161022A (trigger=718655).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 128.967, +54.365 which is 
   RA(J2000)  =  08h 35m 52s
   Dec(J2000) = +54d 21' 54"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 20 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 02:45:53.4 UT, 133.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 129.00074, 54.34876 which is equivalent
to:
   RA(J2000)  = 08h 36m 00.18s
   Dec(J2000) = +54d 20' 55.5"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 91 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.13 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 1.2
(+1.30/-1.19) x 10^21 cm^-2 (90% confidence). 

No UVOT data are available at this time. 

Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). 
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.)


GRB_name: GRB161022A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20088
SUBJECT: GRB 161022A: Prompt enhanced Swift-XRT position
DATE:    16/10/22 03:20:24 GMT
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 161022A, we find an
enhanced XRT position of the afterglow: RA, Dec: 129.0018, 54.3490
which is equivalent to:
   RA (J2000)  = 08 36 00.44
   Dec (J2000) = +54 20 56.3
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/718655.

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.


GRB_name: GRB161022A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20089
SUBJECT: GRB 161022A: TAROT Calern observatory optical observations
DATE:    16/10/22 08:01:15 GMT
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 161022A detected by SWIFT
(trigger 718655) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 71s after the GRB trigger
(17s after the notice). The elevation of the field increased
from 56 degrees above horizon and weather conditions
were excellents.

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+71.2s to t0+131.2s : Rlim = 17.4

The second image is 30.0s exposure in tracking mode:
t0+146.3s to t0+176.3s : Rlim = 18.5

We co-added a series of exposures:
t0+146.3s to t0+442.9s : Rlim = 19.0

No more OT detection until t0+6800s at Rlim = 19.0.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB161022A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20090
SUBJECT: GRB 161022A: LT observations
DATE:    16/10/22 09:04:32 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), C.G. Mundell (U. Bath), S. Kobayashi, I.A. 
Steele (LJMU), A. Gomboc (U. Nova Gorica) on behalf of a large 
collaboration report:

The 2-m Liverpool Telescope began observing Swift GRB161022A (Stamatikos 
et al., GCN 20087) with the RINGO3 polarimeter on October 22, 02:46:59 
UT (199 s since trigger). Within the prompt enhanced XRT error circle 
(Evans et al. GCN 20088) we found nothing brighter than 20.5 mag in the 
SDSS-R filter at a mid time of 35 minutes post burst.


GRB_name: GRB161020B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20091
SUBJECT: IPN Triangulation of GRB 161020B
DATE:    16/10/22 11:22:49 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa,
and A. Goldstein, on behalf of the Fermi GBM team,

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

A long-duration GRB 161020B has been detected by Fermi (GBM),
Konus-Wind, INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and Swift (BAT)
at about 65597 s UT (18:13:17). The burst was outside the coded
field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose
coordinates are:
---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
   63.105 (04h 12m 25s) -75.580 (-75d 34' 49")
 Corners:
   68.180 (04h 32m 43s) -76.773 (-76d 46' 23")
   68.921 (04h 35m 41s) -76.461 (-76d 27' 38")
   58.787 (03h 55m 09s) -74.305 (-74d 18' 18")
   57.959 (03h 51m 50s) -74.583 (-74d 35' 00")
 ---------------------------------------------
The error box area is 4250 sq. arcmin, and its maximum
dimension is 3.4 deg (the minimum one is 21 arcmin).
The Sun distance was about 90 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB161020_T65597/IPN/

The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.


GRB_name: GRB161022A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20092
SUBJECT: GRB 161022A: Swift-XRT refined Analysis
DATE:    16/10/22 12:26:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), B. Mingo (U. Leicester), A.
Melandri (INAF-OAB) and M. Stamatikos report on behalf of the Swift-XRT
team:

We have analysed 8.7 ks of XRT data for GRB 161022A (Stamatikos et al.
GCN Circ. 20087), from 118 s to 22.5 ks after the  BAT trigger. The
data comprise 7 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The best
available XRT position (using the promptly downlinked event data, the
XRT-UVOT alignment and matching UVOT field sources to the USNO-B1
catalogue) is RA, Dec = 129.0017, 54.3486 which is equivalent to:

RA (J2000): 08 36 00.40
Dec(J2000): +54 20 55.0

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.46 (+0.13, -0.11).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.70 (+0.16, -0.07). The
best-fitting absorption column is  consistent with the Galactic value
of 4.1 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.8 x 10^-11 (4.0 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.1 (+/-2.0) x 10^20 cm^-2
Galactic foreground: 4.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.70 (+0.16, -0.07)

If the light curve continues to decay with a power-law decay index of
1.46, the count rate at T+24 hours will be 1.5 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.6 x
10^-15 (5.9 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00718655.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161020B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20093
SUBJECT: Konus-Wind observation of GRB 161020B
DATE:    16/10/22 12:28:12 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A.Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 161020B
(IPN triangulation: Hurley et al., GCN Circ. 20091)
triggered Konus-Wind at T0=65597.4 s UT (18:13:17.400).

The burst light curve shows a multipeaked structure
started at ~T0-9 s with a total duration of ~45.6 s.
The emission is seen up to 3 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161020_T65597/

As observed by Konus-Wind, the burst
had a fluence of 5.12(-0.48,+0.54)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.136 s,
of 6.42(-1.29,+1.33)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+37.888 s)
is best fit in the 20 keV - 3 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.03(-0.10,+0.11),
the high energy photon index beta = -2.63(-0.59,+0.26),
the peak energy Ep = 186(-19,+21) keV
(chi2 = 69/64 dof)

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+5.120 s)
is best fit in the 20 keV - 3 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.51(-0.10,+0.11),
the high energy photon index beta = -2.72(-0.32,+0.21),
the peak energy Ep = 224(-16,+17) keV
(chi2 = 58/61 dof)

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB161022A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20094
SUBJECT: GRB 161022A: Enhanced Swift-XRT position
DATE:    16/10/22 14:29:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1530 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 161022A, 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 = 129.00148, +54.34828 which is equivalent
to:

RA (J2000): 08h 36m 0.35s
Dec (J2000): +54d 20' 53.8"

with an uncertainty of 1.4 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.


GRB_name: GRB161022A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20095
SUBJECT: GRB 161022A: NOT optical observations
DATE:    16/10/22 15:40:02 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI and DTU Space) and J. Prieto-Arranz (IAC) report 
on behalf of a larger collaboration:

We observed the field of GRB 161022A (Stamatikos et al., GCN 20087) 
using the Nordic Optical Telescope (NOT) equipped with the AlFOSC 
imaging camera. Observations started on 2016 Oct 22.161 UT, 68.5 min 
after the GRB, and consisted of 2x300 s exposures in the SDSS r band. 
Observations were affected by adverse weather conditions.

Within or in the proximity of the XRT error circle (Evans, GCN 20088), 
at a mid time of 73.9 min after the GRB trigger, we detect no new 
sources down to a limiting magnitude r > 22 (AB), calibrated against 
nearby SDSS stars.


GRB_name: GRB161022A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20096
SUBJECT: GRB 161022A: Fermi GBM observation
DATE:    16/10/22 16:33:18 GMT
FROM:    Oliver Roberts at UCD/Fermi  <oliver.roberts@ucd.ie>

O.J. Roberts (UCD) reports on behalf of the Fermi GBM Team:

At 02:43:45.92 UT on October 22nd, 2016, the Fermi Gamma-Ray
Burst Monitor triggered and located GRB 161022A
(trigger 498797029/161022114), which was also detected by Swift
(Stamatikos et al., GCN 20087). The GBM on-ground location is
consistent with the Swift position. The angle from the Fermi LAT
boresight is 131 degrees.

The GBM light curve shows a weak, FRED-like peak with a duration
(T90) of about 19 s (50-300 keV). The time-averaged spectrum
from T0-6.1 s to T0+11.3 s is adequately fit by a power law function
with an exponential high-energy cutoff. The power law index is
-0.59 +/- 0.37 and the cutoff energy, parameterized as Epeak,
is 155.7 +/- 33.2 keV

The event fluence (10-1000 keV) in this time interval is
(1.65 +/- 0.24)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.3 s in the 10-1000keV band is 2.5 +/- 0.4 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.


GRB_name: GRB161022A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20097
SUBJECT: GRB 161022A: Swift/UVOT Upper Limits
DATE:    16/10/22 16:48:34 GMT
FROM:    Lea Hagen at PSU  <lea.zernow.hagen@gmail.com>

L. M. Z. Hagen (PSU) and M. Stamatikos (OSU/NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161022A
137 s after the BAT trigger (Stamatikos et al., GCN Circ. 20087). No
optical afterglow consistent with the XRT position (Evans et al. GCN
Circ. 20094) 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 early exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white              137         1544          539         >21.25
u                  296         1668          333         >19.90
b                  551         1692           99         >19.27
v                  627         1421           97         >18.34
uvw1               676         1644          116         >18.86
uvm2               824         1272           38         >17.99
uvw2               602         1570          116         >19.10


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161022A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20098
SUBJECT: GRB 161022A: RATIR Optical and NIR Observations 
DATE:    16/10/22 17:26:16 GMT
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), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±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 161022A (Stamatikos et al., GCN Circ.
20087) with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from 2016/10 22.37 to
2016/10 22.53 UTC (6.23 to 9.89 hours after the BAT trigger), obtaining
a total of 2.49 hours exposure in the r and i bands and 1.04 hours
exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (D'Elia et al., GCN Circ.
20092), in comparison with the SDSS DR9 and 2MASS catalogs, we obtain
the following 3-sigma upper limits:

  r > 24.24
  i > 24.04
  Z > 22.96
  Y > 22.50
  J > 22.18
  H > 21.87

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161022A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20100
SUBJECT: GRB 161022A: Swift-BAT refined analysis
DATE:    16/10/22 22:02:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
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-239 to T+737 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 161022A (trigger #718655)
(Stamatikos, et al., GCN Circ. 20087).  The BAT ground-calculated position is
RA, Dec = 128.988, 54.366 deg, which is 
   RA(J2000)  =  08h 35m 57.2s 
   Dec(J2000) = +54d 21' 57.8" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 14%.
 
The mask-weighted light curve shows a few overlapping peaks starting at ~T-1 sec,
peaking at ~T+2 sec, an ending at ~T+15 sec.
T90 (15-350 keV) is 7.3 +- 1.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.53 to T+8.24 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.14 +- 0.21.  The fluence in the 15-150 keV band is 7.5 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+2.13 sec in the 15-150 keV band
is 1.6 +- 0.4 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/718655/BA/


GRB_name: GRB161023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20102
SUBJECT: GRB 161023A (Integral trigger 7613) MASTER-Net bright OT detection
DATE:    16/10/23 23:06:38 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

E. Gorbovskoy, V. Lipunov,  N.Tyurina, V.Kornilov, P.Balanutsa, 
A.Kuznetsov, D.Kuvshinov,
Lomonosov Moscow State University, Sternberg Astronomical Institute

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik
Kislovodsk Solar Station of the Pulkovo Observatory

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov, A. Gabovich
Blagoveschensk Educational State University, Blagoveschensk


V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in SAAO was pointed to the  GRB161023.94 24 sec after notice time 
and 33 sec after trigger time at 2016-10-23 22:39:24 UT in two 
polarization.
On our first (10s exposure)  and consequent images we  found optical 
bright transient   within INTEGRAL  error-box (ra=20 45 08 dec=-47 37 08 
r=0.054667) at following position:
RA                  Dec
20h 44m 05.21s , -47d 39m 48s.5

OT rise up to  maximum magnituge about  12.5 (~ 3 minutes after the 
trigger).


The 5-sigma upper limit at first  has been about 16.11mag
The message may be cited.


GRB_name: GRB161023A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20103
SUBJECT: GRB 161023A: A long GRB detected by INTEGRAL
DATE:    16/10/23 23:45:13 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro@iasf-milano.inaf.it>

S.Mereghetti (IASF-Milano), D.Gotz (CEA, Saclay), C.Ferrigno, 
S.Fotopoulou(ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of 
the IBAS Localization Team report:

a gamma ray burst lasting about 45 s has been detected by IBAS in the 
IBIS/ISGRI data at 22:38:40 UT of 2016 October 23.

The refined coordinates (J2000) are:
R.A.=  311.0342 deg
DEC.=  -47.6614  deg

with an uncertainty of  1   arcmin (90% c.l.).

The burst had a peak flux greater than 5 counts/cm2/s (20-200 keV, 1-s 
integration time) and a fluence in the same energy range greater than 5e-6 
erg/cmq. These are lower limits because this bright burst caused ISGRI 
telemetry saturation.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB161023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20104
SUBJECT: GRB 161023A VLT/X-shooter redshift
DATE:    16/10/24 03:17:06 GMT
FROM:    Nial Tanvir at U.Leicester  <nrt3@star.le.ac.uk>

N. R. Tanvir (U. Leicester), T. Kruehler (MPE), A. De Cia (ESO),
K. Wiersema (U. Leicester), D. Xu (NAOC), D. Malesani (DARK/NBI),
report on behalf of a larger collaboration:

We observed the optical counterpart of the bright INTEGRAL
GRB 161023A (Mereghetti et al. GCN 20103; Gorbovskoy et al.
GCN 20102) with the ESO Very Large Telescope UT 2 (Kueyen)
equipped with the X-shooter spectrograph, covering the wavelength
range 3500-20000 AA.  Observations started on October 24.05 UT
(approx 3.0 hr after the GRB) and consisted of 2 exposures of
600 s each.

The spectrum exhibits numerous absorption features including the
hydrogen Lyman series, and lines of SII, SiII, SiIV, CIV, AlII, FeII, OI,
several of which are fine structure lines, at a redshift of z=2.708. We
conclude this is the redshift of the GRB.

We acknowledge the generosity of the visiting observer, Chris D'Andrea,
who approved the override, and expert support from the ESO observing
staff, particularly Linda Schmidtobreick and Luca Sbordone, in obtaining
these observations.

[GCN OPS NOTE(24oct16):  L.Sbordone was added to the last paragraph.]


GRB_name: GRB161011A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20105
SUBJECT: Radio upper limit on the GRB 161011A with the GMRT
DATE:    16/10/24 07:00:22 GMT
FROM:    Nayana A J at NCRA-TIFR  <nayan89deva@gmail.com>

A. J. Nayana (NCRA-TIFR), Vikas Chand (TIFR), Poonam Chandra (NCRA-TIFR) and A.R. Rao
(TIFR)  report:

We carried out the Giant Metrewave Radio Telescope (GMRT) observations of GRB 161011A
(GCN Circ 20023) in the 1390 MHz band on 2016 October 21.71 UT. We do not detect radio
afterglow of the GRB in this frequency band. The 3-sigma upper limit at the GRB position
(GCN Circ. 20026) is 120 uJy.

We thank GMRT staff for making these observations possible. 


GRB_name: GRB161023A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20106
SUBJECT: GRB 161023A: Swift ToO observations
DATE:    16/10/24 07:55:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a ToO observation of the INTEGRAL GRB 161023A. 
Automated analysis of the XRT data will be presented online at
http://www.swift.ac.uk/ToO_GRBs/00020709

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the INTEGRAL event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20107
SUBJECT: GRB 161023A: LCOGT-FTS optical observations
DATE:    16/10/24 10:30:23 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), C.G. Mundell 
(U. Bath), A. Gomboc (U. Nova Gorica) on behalf of a large collaboration 
report:

The 2-m LCOGT Faulkes Telescope South began observing INTEGRAL GRB 
161023A (Mereghetti et al., GCN 20103) in the SDSS ri filters on October 
24, 09:17 UT (~0.44 days since the GRB). We clearly detect the optical 
afterglow (Gorbovskoy et al. GCN 20102; Tanvir al. GCN 20104) at the 
position RA(J2000)= 20:44:05.17, DEC(J2000)= -47:39:47.8 (error radius 
of 1 arcsec) with the following values:

Mid time from GRB     Exposure     Filter       Magnitude
(days)                  (s)
-------------------------------------------------------------
0.44                   5x60        SDSS-R       18.57 +- 0.03
0.45                   5x60        SDSS-I       18.38 +- 0.03
-------------------------------------------------------------

Calibration is done against nearby USNOB-1 star 20:44:08.421, 
-47:39:34.63 assuming r=17.27, i=17.20 mag.


GRB_name: GRB161023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20108
SUBJECT: GRB 161023A: Watcher optical observations
DATE:    16/10/24 14:27:48 GMT
FROM:    Antonio Martin-Carrillo at UCD,Space Science Group  <antonio.martin-carrillo@ucd.ie>

A. Martin-Carrillo (UCD), D. Murphy (UCD), L. Hanlon (UCD), H. J. van Heerden (UFS), B. van Soelen (UFS) and P. J. Meintjes (UFS)

We observed the field of GRB 161023A (Mereghetti et al, GCN 20103) using the 40cm UCD Watcher telescope at Boyden Observatory in South Africa.

Observations started at 22:39:23 UT, 43.7 seconds after the burst trigger (T0=22:38:40 UT) when the source was just 21.9 degrees above the horizon. A series of 5 second exposures was taken in the SDSS râ€™ filter using an Andor EMCCD camera for the first 600 seconds, followed by 60 second exposures until the source was below our observation limit at 22:53:33 UT (T0+893 seconds).

A bright transient source is clearly detected in all individual frames consistent with the location reported by Gorbovskoy et al. (GCN 20102). The source shows a fast rise up to ~T0+200 seconds where it peaks at m(râ€™) ~12.8, followed by a slow decay. On our last measurement at T0+893 seconds, the source had faded to m(râ€™)~14.4.

Magnitudes were calibrated using several nearby APASS stars and are shown in the Vega system. No correction for Galactic extinction in the direction of the GRB has been applied.


GRB_name: GRB161023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20109
SUBJECT: GRB 161023A: Zadko observatory - Gingin optical observations
DATE:    16/10/24 14:28:37 GMT
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.),
Coward, D. McPherson, D. Williams A., Martin R.,
Moore J., Dodson R. (UWA) report:
report:

We imaged the field of GRB 161023A detected by Integral
(trigger 7613, Mereghetti et al., GCN 20103)
with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 0.55 day after the GRB trigger.
The elevation of the field decreased from
72 degrees above horizon and weather conditions
were good.

We detected the candidate couterpart mentioned by Gorbovskoy
et al. (GCNC 20102) and Tanvir al. (GCN 20104). We used the same
calibration star than Guidorzi et al. (GCNC 20107):

t0+0.55d to t0+0.63d : R = 19.09 +/- 0.05

Magnitudes are not corrected for galactic dust extinction.


GRB_name: GRB161023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20110
SUBJECT: GRB 161023A: TAROT La Silla observatory optical observations
DATE:    16/10/24 14:52:46 GMT
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 161023A detected by Integral
(trigger 7613, Mereghetti et al., GCN 20103)
with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 64 min after the GRB trigger
(just after the dusk).
The elevation of the field decreased from
71 degrees above horizon and weather conditions
were cloudy so only few images can be measured.

We detected the couterpart mentioned by Gorbovskoy
et al. (GCNC 20102) and Tanvir al. (GCN 20104).

t0 +64 min to t0 +87 min : R    = 15.2 +/-0.2
t0 +96 min to t0+116 min : R    = 15.8 +/-0.4
t0+143 min to t0+149 min : Rlim = 15.8

Magnitudes were estimated with the nearby star
NOMAD-1 0423-1044399 ra=311.0274867 dec=-47.6493169
R=12.37.

Magnitudes are not corrected for galactic dust extinction.


GRB_name: GRB161023A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20111
SUBJECT: Konus-Wind observation of GRB 161023A
DATE:    16/10/24 17:04:57 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

The long GRB 161023A (INTEGRAL detection: Mereghetti et al., GCN 20103)
triggered Konus-Wind at T0=81552.321 s UT (22:39:12.321).

The light curve shows a broad emission pulse with a duration
of ~50 s. The emission is seen up to ~6 MeV.

As observed by Konus-Wind, the burst had a fluence of
(4.2 Â± 0.6)x10^-5 erg/cm2 and a 64-ms peak energy flux,
measured from T0-8.320, of (5.3 Â± 0.8)x10^-6 erg/cm2
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.11 (-0.18,+0.22),
the high energy photon index beta = -2.27 (-0.32,+0.16),
the peak energy Ep = 163 (-28,+37) keV,
chi2 = 81/97 dof.

The spectrum near the peak count rate (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.55 (-0.28,+0.34),
the high energy photon index beta = -2.16 (-0.24,+0.14),
the peak energy Ep = 172 (-28,+43) keV,
chi2 = 89/97 dof.


Assuming the redshift z=2.708 (Tanvir et al., GCN 20104)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.3, and Omega_Lambda = 0.7,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~6.8x10^53 erg,
the peak luminosity L_iso is ~3.2x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~640 keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161023_T81552/

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB161023A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20112
SUBJECT: GRB 161023A: Swift-XRT afterglow detection
DATE:    16/10/24 17:39:57 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. D'Ai (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows
(PSU), T.G.R. Roegiers (PSU), K.L. Page (U. Leicester), B. Mingo (U.
Leicester), A.P. Beardmore (U. Leicester), A. Melandri (INAF-OAB), P.
D'Avanzo (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf of
the Swift-XRT team:

Swift-XRT has performed follow-up observations of the INTEGRAL-detected
burst GRB 161023A (Gorbovskoy et al. GCN Circ. 20102), collecting 1.1
ks of Photon Counting (PC) mode data between T0+34.8 ks and T0+53.2 ks.


A fading, uncatalogued X-ray source is detected consistent with the
MASTER position (Gorbovskoy et al., GCN Circ. 20102) and is therefore
believed to be the afterglow. Using 3643 s of PC mode data and 4 UVOT
images, we find an enhanced XRT position (using the XRT-UVOT alignment
and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
311.02161, -47.66348 which is equivalent to:

RA (J2000): 20h 44m 05.19s
Dec(J2000): -47d 39' 48.5"

with an uncertainty of 1.5 arcsec (radius, 90% confidence). This
position is 0.2 arcsec from the MASTER position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.3 (+0.9, -1.0).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.09 (+0.30, -0.16). The
best-fitting absorption column is  consistent with the Galactic value
of 3.2 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.1 x 10^-11 (3.4 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+/-5.6) x 10^20 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.09 (+0.30, -0.16)

If the light curve continues to decay with a power-law decay index of
2.3, the count rate at T+24 hours will be 9.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.8 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/00020709.
The results of the full analysis of the XRT observations are available
at http://www.swift.ac.uk/ToO_GRBs/00020709.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161023A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20113
SUBJECT: GRB 161023A: GROND Observations
DATE:    16/10/25 06:37:38 GMT
FROM:    Thomas Kruehler at MPE Garching  <kruehler@mpe.mpg.de>

T. Kruehler and J. Greiner (both MPE Garching) report on behalf
of the GROND team:

We observed the field of GRB 161023A (INTEGRAL trigger 7613;
Mereghetti et al., GCN #20103) simultaneously in g'r'i'z'JHK with
GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG
telescope at the ESO La Silla Observatory (Chile).

Observations started at 23:52 UT on 2016-10-24, 25.2 hr after the GRB
trigger. They were performed at an average seeing of 1".6, and at an
average airmass of 1.1.

Based on combined images with 9.7 min of total exposures in g'r'i'z'
and 10.0 min in JHK at a mid-time of 00:12 UT on 2016-10-25,
we derive the following preliminary magnitudes (all in AB system) for
the optical/NIR afterglow (Gorbovskoy et al. GCN 20102, Tanvir et al.,
GCN 20104, Guidorzi et al., GCN 20107).

g' = 19.7 +- 0.1 mag
r' = 19.4 +- 0.1 mag
i' = 19.2 +- 0.1 mag
z' = 19.1 +- 0.1 mag
J = 18.7 +- 0.1 mag
H = 18.4 +- 0.1 mag
K = 18.2 +- 0.1 mag

Given magnitudes are calibrated against GROND zeropoints as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V) = 0.03 mag
in the direction of the burst (Schlafly & Finkbeiner 2011).


GRB_name: GRB161023A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20114
SUBJECT: GRB161023A: AstroSat CZTI detection
DATE:    16/10/25 07:05:27 GMT
FROM:    Varun Bhalerao at IUCAA  <varunb@iucaa.in>

V. Sharma, V. Kumar, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed clear detection of a long duration GRB161023A (INTEGRAL detection: Sandro Mereghetti et al., GCN Circ.  20103) in the 40-200 keV energy range. The light curve shows a single peak at 22:39:10.00 UT, 30 seconds after the INTREGAL trigger at 22:38:40 UT. The measured peak count rate is 132.10 counts/sec above the background in combined data of four quadrants, with a total of 2846 counts. The local mean background count rate was 367.10 counts/sec.  Using cumulative rates, we measure a T90 of 44 sec.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB161014A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20115
SUBJECT: GRB 161014A: 15 GHz upper limits from AMI
DATE:    16/10/27 21:35:51 GMT
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 
161014A (Racusin et al., GCN 20035) 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 Oct 14.67, Oct 15.85, Oct 
17.85, and Oct 20.85 (UT) do not reveal any radio source at the XRT 
location (Mingo et al., GCN 20050), with 3sigma upper limits of 225 uJy, 
285 uJy, 129 uJy, and 228 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/.


GRB_name: GRB161015A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20116
SUBJECT: GRB 161015A: 15 GHz upper limits from AMI
DATE:    16/10/27 21:38:30 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley (Hintze Fellow, Oxford), 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)

We observed the Fermi/LAT GRB 161015A (Ohno et al., GCN 20054) with the 
AMI Large Array at 15 GHz on 2016 Oct 17.75, Oct 18.73, Oct 20.70, and 
Oct 24.65 (UT) as part of the 4pisky program. We do not detect any radio 
source at the XRT location (D'Avanzo et al., GCN 20057), with 3sigma 
upper limits of 105 uJy, 96 uJy, 147 uJy, and 78 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/.


GRB_name: GRB161020A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20118
SUBJECT: GRB 161020A: Fermi GBM observation 
DATE:    16/11/01 22:16:18 GMT
FROM:    C. Michelle Hui at MSFC/Fermi-GBM  <c.m.hui@nasa.gov>

C. M. Hui (NASA/MSFC), C Meegan (UAH), and P. Jenke (UAH)
report on behalf of the Fermi GBM Team:

At 00:34:46.95 UT on 20 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161020A (trigger 498616490/161020024),
which was also detected by INTEGRAL (Mereghetti et al., GCN 20086).
The GBM on-ground location is consistent with the INTEGRAL position.
The angle from the Fermi LAT boresight is 117 degrees.

The GBM light curve shows a single peak
with a duration (T90) of about 12.3 s (50-300 keV).
The time-averaged spectrum from T0-6.1 s to T0+3.1 s is adequately
fit by a simple power law function with index -1.74 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(1.49 +/- 0.14)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.1s in the 10-1000 keV band is 2.3 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog.


GRB_name: GRB161104A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20123
SUBJECT: GRB 161104A: Swift detection of a short burst
DATE:    16/11/04 10:00:19 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

B. Mingo (U Leicester), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), P.A. Evans (U Leicester),
K. L. Page (U Leicester) and T. N. Ukwatta (LANL) report on behalf of
the Swift Team:

At 09:42:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161104A (trigger=720568).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 77.881, -51.452 which is 
   RA(J2000) = 05h 11m 31s
   Dec(J2000) = -51d 27' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 0.3 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~0.1 sec after the trigger. 

The XRT began observing the field at 09:43:24.9 UT, 58.3 seconds after
the BAT trigger. The position determined from promptly downlinked data
is incorrect because the XRT centroided on a cosmic ray. 
Using promptly downlinked data we find an uncatalogued X-ray source 
located at RA, Dec 77.89236, -51.45898 which is equivalent to:
   RA(J2000)  = 05h 11m 34.17s
   Dec(J2000) = -51d 27' 32.3"
with an uncertainty of 4.5 arcseconds (radius, 90% containment). This
location is 35 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 101 seconds with the White filter
starting 67 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 0.02. 

Burst Advocate for this burst is B. Mingo (bm188 AT le.ac.uk). 
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.)


GRB_name: GRB161104A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20124
SUBJECT: GRB 161104A: Enhanced Swift-XRT position
DATE:    16/11/04 12:32:51 GMT
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 95 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 161104A, 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 = 77.89359, -51.46011 which is equivalent
to:

RA (J2000): 05h 11m 34.46s
Dec (J2000): -51d 27' 36.4"

with an uncertainty of 3.2 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.


GRB_name: GRB160928A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20126
SUBJECT: GRB 160928A: The first GRB detected by POLAR
DATE:    16/11/04 15:30:06 GMT
FROM:    Shaolin Xiong at IHEP  <xiongsl@ihep.ac.cn>

S. L. Xiong (IHEP), N. Produit (UniGe), T. W. Bao (IHEP), T. Batsch (NCBJ),
T. Bernasconi, F. Cadoux, I. Cernuda (UniGe), J. Y. Chai, Y. W. Dong, M.  Z. Feng (IHEP),
N. Gauvin (UniGe), M. Y. Ge (IHEP), W. Hajdas (PSI), J. J. He, Y. Huang (IHEP),
M. R. Kole (UniGe), M. N. Kong (IHEP), C. Lechanoine-Leluc (UniGe), H.  C. Li,
L. Li, Z. H. Li, J. T. Liu, X. Liu, F. J. Lu (IHEP), R. Marcinkowski (PSI), S. Orsi, M. Pohl,
D. Rapin (UniGe), A. Rutczynska, D. Rybka (NCBJ), H. L. Shi, L. M. Song, J. C. Sun (IHEP),
J. Szabelski (NCBJ), R. J. Wang, Y. H. Wang, X. Wen, B. B. Wu (IHEP), X.  Wu (UniGe),
H. L. Xiao (PSI), H. H. Xu, M. Xu, J. Zhang, L. Zhang, L. Y. Zhang (IHEP), P. Zhang (PSI),
S. N. Zhang, X. F. Zhang, Y. J. Zhang, Y. Zhao, S. J. Zheng (IHEP), A. 
Zwolinska (NCBJ)
(i.e. the POLAR team):

POLAR, a dedicated Gamma-Ray Burst polarimeter, has been launched successfully
on-board the Chinese space laboratory Tiangong-2 (TG-2) on Sep 15, 2016.

During the commissioning operation phase, at 19:48:05.00 UT on 28 
September 2016 (T0),
POLAR detected the GRB160928A in a routine ground search of the data,
which was also observed by the Fermi/GBM (trigger 496784887/160928825),
INTEGRAL/SPI-ACS (trigger #7579) and Konus-WIND (trig #4385).

POLAR can localize bursts within its FOV (~ half sky) to an accuracy of degrees
(Suarez-Garcia et al., NIM A, 2010, 624). However, since this burst is 
not very bright and
falls on the edge of the FOV, the localization is difficult and still on-going.

Using the best location from the Fermi/GBM, which is (J2000):
RA:   130.39    [deg]
Dec:    8.14    [deg]
Err:    3.19    [deg]

the incident angle at T0 in POLAR detector coordinate is:
theta:   94.7   [deg]
phi:    -26.8   [deg]

The distribution of the GRB signal among its 25 detector modules is 
consistent with this incident geometry.

In addition, the timing and structures in the POLAR light curve is well 
consistent with that of other instruments mentioned above.
Thus we conclude that this event is the first confirmed GRB which POLAR detected,
and that POLAR works as expected.

The POLAR light curve consists of multiple peaks
with a duration (T90) of 5.1 s measured from T0-1.7 s.
The 50-ms peak flux, measured from T0+0.55 s, is 1406.7 cnts/sec.
The above measurements are in the energy range of about 80-500 keV.

The analysis results presented above are preliminary;
final results will be published in the POLAR paper.

The POLAR mission is a joint effort of the international collaboration 
between the Institute of High Energy Physics (IHEP) in China, the University of 
Geneva (UniGe) and the Paul Scherrer Institute (PSI) in Switzerland, and the National 
Center for Nuclear Research (NCBJ) in Poland. More information about POLAR could be 
found at http://polar.ihep.ac.cn/en/.

[GCN OPS NOTE(05nov16):  Per author's request, the affiliation in the FROM:-line
was changed from "POLAR" to "IHEP".  And some line-wrapping was fixed.


GRB_name: GRB161104A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20128
SUBJECT: GRB 161104A: Swift-XRT refined Analysis
DATE:    16/11/04 21:00:38 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

D.N. Burrows (PSU), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), B.
Mingo (U. Leicester), A.P. Beardmore (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC) and B. Mingo (U
Leicester) report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 161104A (Mingo et al. GCN
Circ. 20123), from 68 s to 23.6 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Goad et al. (GCN Circ. 20124).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.37 (+0.17, -0.16).

If the light curve continues to decay with a power-law decay index of
0.37, the count rate at T+24 hours will be 1.6 x 10^-3 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00720568.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161104A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20129
SUBJECT: GRB 161104A, Swift-BAT refined analysis
DATE:    16/11/05 02:14:12 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
B. Mingo (U Leicester), J. P. Norris (BSU), 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+150 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161104A (trigger #720568)
(Mingo, et al., GCN Circ. 20123). The BAT ground-calculated position is
RA, Dec = 77.906, -51.447 deg which is
   RA(J2000)  =  05h 11m 37.3s
   Dec(J2000) = -51d 26' 49.7"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.

The mask-weighted light curve shows a single spike that starts at at ~T-0.02,
peaks at ~T+0.02, and ends at~T+0.1. T90 (15-350 keV) is 0.1 +- 0.02 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.0 to T+0.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.57 +- 0.20.  The fluence in the 15-150 keV band is 3.1 +- 0.5 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.46 sec in the 15-150 keV band
is 0.6 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Using a 4-ms binned light curve, the lag analysis finds a lag of
2.0 +/- 8.0 ms for the 100-350 keV to 25-50 keV band,
and -3.5 +/- 8.0 ms for the 50-100 keV to 15-25 keV band.
These values are consistent with those of a short GRB.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/720568/BA/

[GCN OPS NOTE05nov16):  Per author's request, JN as was added
to the author list.]


GRB_name: GRB161104A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20130
SUBJECT: GRB 161104A: Swift/UVOT Upper Limits 
DATE:    16/11/05 03:28:35 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and B. Mingo (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161104A
69 s after the BAT trigger (Mingo et al., GCN Circ. 20123).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 20124)
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 initial exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white               69          170           99         >20.8
w1                4984         5184          197         >19.9
m2                4779         4979          197         >21.7
w2                5805         6005          197         >19.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161105A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20131
SUBJECT: GRB 161105A: Swift detection of a burst
DATE:    16/11/05 05:14:04 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K. L. Page (U Leicester), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL)
and M. H. Siegel (PSU) report on behalf of the Swift Team:

At 04:53:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161105A (trigger=720697).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 120.163, -44.780 which is 
   RA(J2000) = 08h 00m 39s
   Dec(J2000) = -44d 46' 46"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 140 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~8 sec after the trigger. 

The XRT began observing the field at 04:54:10.1 UT, 67.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 120.1839,
-44.7753 which is equivalent to:
   RA(J2000)  = 08h 00m 44.14s
   Dec(J2000) = -44d 46' 31.1"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 56 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.15
x 10^21 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 3.12e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 586 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.32. 

Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). 
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.)


GRB_name: GRB161104A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20132
SUBJECT: GRB 161104A: GROND observations
DATE:    16/11/05 07:37:21 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Schmidl (both TLS Tautenburg) and J. Greiner
(MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 161104A (Swift trigger 720568; Mingo et
al., GCN 20123) simultaneously in g'r'i'z'JHK with GROND (Greiner et
al. 2008, PASP 120, 405) mounted at the 2.2m MPG telescope at the ESO
La Silla Observatory (Chile).

Observations started at 04:00 UT on 2016-11-05, 18 hours after the GRB
trigger. They were performed at an average seeing of 1" and at an
average airmass of 1.2.  Inside the enhanced 3.2" XRT position (GCN
20124, Goad et al.) we find a single source at coordinates:

Source A
RA (J2000) = 05:11:34.46
DEC (J2000) = -51:27:36.3
with an uncertainty of 0.5" in each coordinate.

At the border of the XRT error circle lie two more sources  at coordinates:

Source B
RA (J2000) = 05:11:34.31
DEC (J2000) = -51:27:33.6

Source C
RA (J2000) = 05:11:34.73
DEC (J2000) = -51:27:34.2

Their r'-band AB magnitudes are:

Source A
r' = 24.1 +- 0.1 mag,
Source B
r' = 24.3 +- 0.1 mag,
Source C
r' = 25.1 +- 0.3 mag,

For the moment no evidence for a fading of any of these objects can be
stated.

Given magnitudes are calibrated against GROND zeropoints and are not
corrected for the Galactic foreground extinction corresponding to a
reddening of E_(B-V) = 0.01 mag in the direction of the burst
(Schlafly & Finkbeiner 2011).

We thank Angela Hempel, La Silla, for performing the observations.


GRB_name: GRB161105A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20133
SUBJECT: GRB 161105A: MASTER-IAC early optical observations
DATE:    16/11/05 10:56:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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 IAC was pointed to the  GRB161105A  27 sec after notice time 
and 42 sec after trigger time at 2016-11-05 04:53:44 UT. On our first (10s 
exposure)  set we haven't found optical transient  within SWIFT error-box 
(ra=120.163 dec=-44.7794 r=0.05) (Page et al., GCN 20131).
The 5-sigma upper limit has been about  16.4 mag (polaroid, 
unfiltered).

The observations made on zenit distance = 75 degrees, galaxy latitude b = 
-7 degree. The moon (25 % bright part) below the horizon (The altitude of 
the Moon is  -80 degree ).
The sun  altitude  is -32.4 degree.
The object can be observed till sunrise at 2016-11-05 07:20:31

Maximal coadded limit ~19.5 m. No OT found.

The message may be cited.


GRB_name: GRB161105A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20135
SUBJECT: GRB 161105A: Enhanced Swift-XRT position
DATE:    16/11/05 16:45:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2913 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 161105A, 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 = 120.18375, -44.77529 which is equivalent
to:

RA (J2000): 08h 00m 44.10s
Dec (J2000): -44d 46' 31.0"

with an uncertainty of 1.7 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.


GRB_name: GRB161105A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20136
SUBJECT: GRB 161105A: Swift-BAT refined analysis
DATE:    16/11/05 17:50:26 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
D. M. Palmer (LANL), K. L. Page (U Leicester),
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 161105A (trigger #720697)
(Page  et al. GCN Circ. 20131).  The BAT ground-calculated position is
RA, Dec = 120.198, -44.763 deg which is
  RA(J2000)  =  08h 00m 47.5s
  Dec(J2000) = -44d 45' 47.6"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~T-90 s and ends at ~T+160 s. There are roughly two main pulses
in the structure. The first one contains two obvious peaks at ~T0 and ~T+10s,
and the second one peaks at ~T+50 s. T90 (15-350 keV) is 177.3 +- 25.8 sec
(estimated error including systematics).

The time-averaged spectrum from T-88.00 to T+164.81 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.02 +- 0.24,
and Epeak of 159.1 +- 135.3 keV (chi squared 55.64 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.1 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.63 sec in the 15-150 keV band is
1.4 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.35 +- 0.06 (chi squared 61.67 for 57 d.o.f.).  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/720697/BA/


GRB_name: GRB161104A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20137
SUBJECT: GRB 161104A: Gemini South optical observations
DATE:    16/11/05 22:12:41 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

E. Troja (UMD/GSFC), A. Watson (UNAM), S. Covino (INAF), W. H. Lee
(UNAM), N. Butler (ASU), J. Becerra-Gonzalez (UMD/GSFC), A. Lien
(UMBC), T. Sakamoto (AGU) and N. Gehrels (NASA/GSFC) report:

We observed the field of the short GRB 161104A (Mingo et al., GCN 20123)
with the Gemini Multi-Object Spectrograph (GMOS) on the 8m Gemini South
telescope. We acquired 6x120s exposures in the r-band beginning at
02:53 UT on 05 November 2016 (~17 hours after the Swift trigger) and
under good observing conditions.

The three sources reported by Nicuesa Guelbenzu et al. (GCN 20132) are
detected with similar magnitudes, showing no significant variability
between our observations and the GROND exposures taken 1 hour later.
Within the enhanced XRT position (Goad et al., GCN 20124) we detect an
additional faint, point-like source not reported by Nicuesa Guelbenzu
et al. (GCN 20132). The position of this source is RA, Dec = 05:11:34.5,
-51:27:33.90 (J2000), accurate to about 0.5" in each coordinate. We
measure a preliminary magnitude of r~24.6 (AB).

The lack of detection in the subsequent GROND observations suggests that
the source significantly faded, however such rapid decay rate is unusual
for a GRB optical afterglow.

We thank the Gemini staff and observers for rapidly scheduling and executing
these observations.


GRB_name: GRB161105A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20138
SUBJECT: GRB 161105A: Swift-XRT refined Analysis
DATE:    16/11/06 05:13:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

T.G.R. Roegiers (PSU), L.M. McCauley (PSU), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), P.
D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A.
Kennea (PSU) and K.L. Page report on behalf of the Swift-XRT team:

We have analysed 5.0 ks of XRT data for GRB 161105A (Page et al. GCN
Circ. 20131), from 560 s to 23.3 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. 20135).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.6 (+/-1.2), followed by a break at T+909 s to an alpha
of 0.86 (+0.14, -0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.90 (+0.28, -0.15). The
best-fitting absorption column is  consistent with the Galactic value
of 4.1 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.1 x 10^-11 (5.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.1 (+/-1.1) x 10^21 cm^-2
Galactic foreground: 4.1 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.90 (+0.28, -0.15)

If the light curve continues to decay with a power-law decay index of
0.86, the count rate at T+24 hours will be 4.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-13 (2.6 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/00720697.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161106A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20140
SUBJECT: GRB 161106A: Fermi GBM detection
DATE:    16/11/06 20:37:05 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

R. Hamburg(UAH), C. Meegan (UAH), and A von Kienlin (MPE)
report on behalf of the Fermi GBM Team:

"At 11:57:53.62 UT on 06 November 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161106A (trigger 500126277 / 161106499).

The on-ground calculated location, using the GBM trigger
data, is RA = 202.1, DEC = +64.9, with an uncertainty
of 1.5 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error [Connaughton et al. 2015, ApJS, 216, 32].

The trigger resulted in an Autonomous Repoint Request (ARR)
by the GBM Flight Software owing to the high peak flux
of the GRB. This ARR was accepted and the spacecraft slewed to the GBM
in-flight
location. The initial angle from the Fermi LAT boresight to
the GBM ground location is 52 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 11 s (50-300 keV).
The time-averaged spectrum from T0-0.00 s to T0+16 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.61 +/- 0.02 and
the cutoff energy, parameterized as Epeak, is 125 +/- 2 keV.

The event fluence (10-1000 keV) in this time interval is
(1.34 +/- 0.01)E-05 (erg/cm^2). The 1-sec peak photon flux measured
starting from T0+2.6 s in the 10-1000 keV band
is 16.3 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161103A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20141
SUBJECT: GRB 161103A: an ultra-long GRB detected by Konus-Wind
DATE:    16/11/07 18:23:34 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:

A very long-duration GRB 161103A has been detected
by Konus-Wind in the waiting mode starting from ~T0=82000 UT
(22:46:40) on November 3, 2016.

The burst was seen almost equally well in both KW detectors,
so its source is close to the ecliptic plane.
We note, that the location of the IceCube event 161103 (GCN 20119),
which occurred ~ 14 hours before GRB 161103 is also at low
ecliptic latitude (~ -3.1 deg). According to the GOES data,
there was no prominent solar X-ray activity at the time of the burst.

The event light curve shows several peaks in the interval
from ~T0-300 s to ~T0+4400 s. The total burst duration,
~4700 s, makes this event an ultra-long GRB candidate.
The spectral hardness of the emission is rather high at
the beginning of the event and decreases with the development
of the burst.

As observed by Konus-Wind, the burst had a fluence of
(3.0 Â± 0.15)x10^-4 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0+160 s, of (8.6 Â± 4.6)x10^-7 erg/cm2
(both in the 20 - 1500 keV energy range).

The time-integrated 3-channel spectrum of the burst, measured from
T0-310 s to T0+4400 s, is well described by a simple power law
function with the PL index of 1.72 Â± 0.04.
The spectrum near the peak count rate, measured from T0+110s
to T0+174 s, can be modeled by a power law with exponential
cutoff (CPL) with alpha = -0.41 Â± 0.45, and Ep = 925 Â± 345 keV.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB161103A/

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB161017A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20142
SUBJECT: GRB 161017A: 15 GHz upper limits from AMI
DATE:    16/11/07 19:25:56 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley (Hintze Fellow, Oxford), 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 
161017A (Troja et al., GCN 20064) 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 Oct 18.14, Oct 19.33, Oct 
21.30 and Oct 25.31 (UT) do not reveal any radio source at the XRT 
location (Beardmore et al., GCN 20067), with 3sigma upper limits of 132 
uJy, 84 uJy, 63 uJy and 78 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/.


GRB_name: GRB161022A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20143
SUBJECT: GRB 161022A: 15 GHz upper limits from AMI
DATE:    16/11/07 19:29:05 GMT
FROM:    Kunal Mooley at Oxford U  <kunal.mooley@physics.ox.ac.uk>

K. P. Mooley (Hintze Fellow, Oxford), 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 
161022A (Stamatikos et al., GCN 20087) 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 Oct 22.15, Oct 23.26, Oct 
26.22 and Oct 29.31 (UT) do not reveal any radio source at the XRT 
location (Evans et al., GCN 20094), with 3sigma upper limits of 135 uJy, 
93 uJy, 105 uJy and 105 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/.


GRB_name: GRB161108A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20145
SUBJECT: GRB 161108A: Swift detection of a burst
DATE:    16/11/08 03:49:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), N. Gehrels (NASA/GSFC),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 03:32:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161108A (trigger=721234).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 180.784, +24.869 which is 
   RA(J2000) = 12h 03m 08s
   Dec(J2000) = +24d 52' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 30 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 03:33:53.5 UT, 80.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 180.78748,
24.86801 which is equivalent to:
   RA(J2000)  = 12h 03m 09.00s
   Dec(J2000) = +24d 52' 04.8"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 11 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.79
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 8.63e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 90 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.02. 

Burst Advocate for this burst is A. P. Beardmore (apb AT star.le.ac.uk). 
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.)


GRB_name: GRB161108A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20146
SUBJECT: GRB 161108A: NOT candidate afterglow
DATE:    16/11/08 06:08:47 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI and DTU Space), A. de Ugarte Postigo (IAA-CSIC and 
DARK/NBI), A. Somero (UTU), E. Gafton (NOT, SU, OKC), S. Damsted (Univ. 
Helsinki), G. Erfanianfar (MPE), A. Finoguenov (Univ. Helsinki), C. 
Gibson (Univ. Helsinki), F. Kiefer (MPE), C. Kirkpatrick (Univ. 
Helsinki), M. Lumme (Univ. Helsinki), V. Oja (Univ. Helsinki), J. 
Rantakyla (Univ. Helsinki), I. Salmenpera (Univ. Helsinki), and M. 
Seppala (Univ. Helsinki), report on behalf of a larger collaboration:

We observed the field of GRB 161108A (Beardmore et al., GCN 20145) with 
the Nordic Optical Telescope (NOT) equipped with the AlFOSC imager and 
spectrograph. Observations started on Nov 8.2132 UT (94.4 min after the 
GRB trigger) and were carried out in the r and z filters.

Within the currently available XRT position (Beardmore et al., GCN 
20145), we detect a single object, at coordinates (J2000):

RA = 12:03:09.11
Dec = +24:52:04.9

This source has a magnitude r = 20.82 +- 0.05 AB, calibrated against 
nearby SDSS stars. The same object is visible in the SDSS archival 
images, at a significantly fainter magnitude r = 22.69 +- 0.20. It is 
classified as a galaxy with a photometric redshift of 0.50 +- 0.12. The 
most likely interpretation is that the object seen in the NOT images is 
the superposition of afterglow and host galaxy, so we consider the 
association with GRB 161108A secure.


GRB_name: GRB161108A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20147
SUBJECT: GRB 161108A: Enhanced Swift-XRT position
DATE:    16/11/08 11:23:14 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 3332 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 161108A, 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 = 180.78794, +24.86815 which is equivalent
to:

RA (J2000): 12h 03m 9.11s
Dec (J2000): +24d 52' 05.3"

with an uncertainty of 1.6 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.


GRB_name: GRB161108A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20148
SUBJECT: GRB 161108A: Swift-XRT refined Analysis
DATE:    16/11/08 14:19:15 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

L.M. McCauley (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U.
Leicester), J.P. Osborne (U. Leicester), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU), B. Sbarufatti
(INAF-OAB/PSU) and A.P. Beardmore report on behalf of the Swift-XRT
team:

We have analysed 6.5 ks of XRT data for GRB 161108A (Beardmore et al.
GCN Circ. 20145), from 73 s to 27.1 ks after the  BAT trigger. The data
comprise 263 s in Windowed Timing (WT) mode (the first 6 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 Beardmore
et al. (GCN Circ. 20147).Considering only the late-time light curve
(from T0+4.5 ks), the source is fading with alpha >1.2.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.20 (+/-0.04). The
best-fitting absorption column is  2.20 (+0.15, -0.14) x 10^21 cm^-2,
in excess of the Galactic value of 1.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.09 (+0.24, -0.22)
and a best-fitting absorption column of 1.5 (+0.7, -0.6) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (4.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.5 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 1.8 x 10^20 cm^-2
Excess significance: 3.7 sigma
Photon index:      2.09 (+0.24, -0.22)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00721234.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161108A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20149
SUBJECT: GRB 161108A: RATIR Afterglow Confirmation
DATE:    16/11/08 14:29:23 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), 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), JosÃ© A.
de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos
RomÃ¡n-ZÃºÃ±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 161108A (Beardmore, et al., GCN 20145) with
the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on
the 1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional
on Sierra San Pedro MÃ¡rtir from 2016/11 8.48 to 2016/11 8.54 UTC (7.87 to
9.34 hours after the BAT trigger), obtaining a total of 1.03 hours exposure
in the r and i bands and 0.40 hours exposure in the Z, Y, J, and H bands.

The afterglow candidate reported by Malesani et al. (GCN 20146) is well
detected.  In comparison with the SDSS DR9 and 2MASS catalogs, we obtain
the following detections and upper limits (3-sigma):

  r = 21.97 +/- 0.12
  i = 21.36 +/- 0.06
  Z = 20.88 +/- 0.11
  Y = 20.57 +/- 0.14
  J = 20.05 +/- 0.27
  H > 18.12

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.  The source appears to have faded
in r by about 1 magnitude as compared to Malesani et al. (GCN 20146).

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161108A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20150
SUBJECT: GRB 161108A: NOT redshift
DATE:    16/11/08 15:00:18 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (IAA-CSIC and DARK/NBI), D. Malesani (DARK/NBI 
and DTU Space), D.A. Perley (DARK/NBI), J.P.U. Fynbo (DARK/NBI), 
K.E. Heintz (Univ. of Iceland and DARK/NBI), A. Somero (UTU), E. Gafton 
(NOT, SU, OKC), S. Damsted (Univ. Helsinki), G. Erfanianfar (MPE), 
A. Finoguenov (Univ. Helsinki), C. Gibson (Univ. Helsinki), F. Kiefer (MPE), 
C. Kirkpatrick (Univ. Helsinki), M. Lumme (Univ. Helsinki), V. Oja (Univ. 
Helsinki), J. Rantakyla (Univ. Helsinki), I. Salmenpera (Univ. Helsinki), and 
M. Seppala (Univ. Helsinki), report on behalf of a larger collaboration:

Continuing with the observations of GRB 161108A (Beardmore et al., 
GCN 20145) reported by Malesani et al. (GCN 20146) we performed 
spectroscopy of the afterglow (see also Butler et al. GCN 20149) and host 
galaxy using the Nordic Optical Telescope (NOT) equipped with AlFOSC. 
The observation consisted of 2x1200s+1x600s exposures using grism 4, 
starting at 5:47 UT (2.25 hr after the burst).

The spectrum shows continuum from 3900 to 9300 AA, with a single 
emission line at 8048 AA, consistent with being due to the [O II] doublet 
at z=1.159. Additionally we detect low SNR absorption features consistent 
with Mg II, Mg I, and Fe II at the same redshift, which we identify as the 
redshift of the GRB.


GRB_name: GRB161108A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20151
SUBJECT: GRB 161108A, Swift-BAT refined analysis
DATE:    16/11/08 22:14:28 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
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 161108A (trigger #721234)
(Beardmore, et al., GCN Circ. 20145).  The BAT ground-calculated position is
RA, Dec = 180.776, 24.905 deg which is
  RA(J2000)  =  12h 03m 06.1s
  Dec(J2000) = +24d 54' 19.4"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 95%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~ T-5 s and ends at ~ T+ 130 s. The main peak occurs at ~T0.
T90 (15-350 keV) is 105.1 +- 11.9 sec (estimated error including systematics).

The time-averaged spectrum from T-1.9 to T+126.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.85 +- 0.17.  The fluence in the 15-150 keV band is 1.1 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-1.80 sec in the 15-150 keV band
is 0.6 +- 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/721234/BA/


GRB_name: GRB161105A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20152
SUBJECT: GRB 161105A: TAROT La Silla observatory optical observations
DATE:    16/11/08 22:25:29 GMT
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 161105A detected by SWIFT
(trigger 720697) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 27.4s after the GRB trigger
(14.8s after the notice). The elevation of the field increased from
31 degrees above horizon and weather conditions
were excellent.

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 (in the XRT error box provided by
Page et al. GCNC 20131) with a limiting magnitude of:

t0+27.4s to t0+87.4s : Rlim = 16.5

Due to technical problems the second image was taken only
743 seconds after the GRB:

t0+743.2s to t0+833.2s : Rlim = 19.8

No more candidate were found in the next images taken
until 2000 seconds after the GRB at the same limiting
magnitude.

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB161108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20153
SUBJECT: GRB 161108A: TAROT Calern observatory optical observations
DATE:    16/11/08 22:57:10 GMT
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 161108A detected by SWIFT
(trigger 721234) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 449s after the GRB trigger
The elevation of the field increased from 28 degrees
above horizon and weather conditions were good.

We co-added a series of exposures but we did not detect the
afterglow candidate of Malesani et al. (GCNC 20146).
TAROT limiting magnitudes are:

t0+ 449s to t0+ 539s : Rlim = 18.5
t0+1271s to t0+1941s : Rlim = 19.5
t0+1952s to t0+3694s : Rlim = 19.5
t0+3705s to t0+6041s : Rlim = 19.5

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB161106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20154
SUBJECT: GRB 161106A: Lomonosov BDRG gamma ray discovery
DATE:    16/11/09 12:46:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov,
A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, 
V.V.Kalegaev, D.Nguen,  V.L. Petrov, I.V.Yashin, P.S.Kazarian
Physics Department, Skobel'tsyn Institute of Nuclear Physics, Lomonosov Moscow 
State University

V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute

I. Park, J. Lee, S. Jeong
Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, 
Korea


At 11:57:55.12 UT on 06 Nov 2016, the Lomonosov BDRG  Gamma-ray
Burst Monitor (http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg ),
triggered GRB 161106A.
GRB 161106A (R. Hamburg(UAH), GCN 20140) has one peak LC
and matches with peak of Fermi Trigger event Num 495802575,
total duration ~10s,
the energy range 340-1100 keV.
LC is available at:
http://master.sai.msu.ru/static/OT/0611.jpg

More information will be available at:
http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts
This Notice was ground-generated.

The message may be cited.


GRB_name: GRB161109A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20155
SUBJECT: GRB 161109A: Fermi-LAT detection
DATE:    16/11/09 14:56:49 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

R. Desiante (INFN Torino), E. Bissaldi (Politecnico & INFN Bari),
F. Longo (University & INFN Trieste), M. Negro (University and INFN Torino),
and J. Racusin (NASA/GSFC) report on behalf of the Fermi-LAT team:
  

At 06:18:45.66 UT on November 09, 2016, Fermi-LAT detected
high-energy emission from GRB 161109A,
which was also detected by Fermi-GBM (trigger 500365129).
The best LAT on-ground location is found to be

RA, Dec: 157.86, 61.80 (degrees, J2000)

with an error radius of 0.26 deg (90% containment, statistical error only).
This was 75 deg from the LAT boresight at the time of the trigger.

The data from the Fermi-LAT show a significant increase
in the event rate that is spatially and temporally correlated
with the GBM emission with high significance.
More than 60 photons above 100 MeV and about 4 photons
above 1 GeV are observed between T0+400 s and T0+1800 s.
The highest-energy photon is a 3.5 GeV event which is
observed 600 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is
Francesco Longo (francesco.longo@ts.infn.it).


The Fermi-LAT is a pair conversion telescope designed to cover
the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.


GRB_name: GRB161109A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20156
SUBJECT: GRB 161109A: Fermi GBM observation
DATE:    16/11/09 15:45:37 GMT
FROM:    Elisabetta Bissaldi at U.Innsbruk/IAPP  <Elisabetta.Bissaldi@uibk.ac.at>

E. Bissaldi (Politecnico & INFN Bari)
reports on behalf of the Fermi GBM Team:


"At 06:18:45.66 UT on 9 November 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161109A (trigger 50036512 / 161109263),
which was also detected by the Fermi/LAT
(Desiante et al. 2008, GCN 20155).
The GBM on-ground location is consistent with the LAT position.
The angle from the Fermi LAT boresight at the GBM trigger time is 77 degrees.

The GBM light curve consists of three peaks
with a duration (T90) of about 24 s (50-300 keV).
The time-averaged spectrum from T0 to T0+30 s is
best fit by a Band function with Epeak = 250 +/- 16 keV,
alpha = -0.73 +/- 0.04, and beta = -2.06 +/- 0.06.

The event fluence (10-1000 keV) in this time interval is
(2.30 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+17 s in the 10-1000 keV band
is 16.7 +/- 0.3 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161105A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20157
SUBJECT: GRB 161105A: Swift/UVOT Upper Limits
DATE:    16/11/09 17:08:21 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and K. L. Page (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161105A
586 s after the BAT trigger (Page et al., GCN Circ. 20131).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 20135)
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 initial exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white (fc)         586          735          147         >20.44
white              586         5286          549         >21.11
v                 1046         7179          274         >18.86
b                  841         5081          274         >20.07
u                  816         1652           86         >18.62
uvw1               792        11242          713         >19.91
uvm2               767         7384          293         >19.12
uvw2              1022         6974          290         >19.24

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.33 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161109A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20158
SUBJECT: GRB 161109A: Tiled Swift observations
DATE:    16/11/09 17:34:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 161109A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00060

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161108A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20159
SUBJECT: GRB 161108A: Swift/UVOT Upper Limits
DATE:    16/11/09 18:46:33 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and A. P. Beardmore (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161108A
90 s after the BAT trigger (Beardmore et al., GCN Circ. 20131).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 20147) or the NOT position (Malesani et al.,
GCN Cir., 20146) 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 initial exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white (fc)         90          239          147         >20.08
white              90         5617          344         >20.62
v                 578         6029          235         >18.61
b                5212         5412          196         >19.76
u                 248          498          245         >19.24
u                 248        10794          652         >19.88
uvw1              628         6439          412         >19.66
uvm2              603         6234          412         >19.89
uvw2              554         5823          235         >19.59

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20160
SUBJECT: GRB 161108A: TSHAO optical observations
DATE:    16/11/09 21:29:59 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute),  I. 
Reva (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 161108A  (Beardmore et al., GCN 20145) 
with Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical 
Observatory. We obtained several images in R filter starting on Nov. 08 
(UT) 23:06:16. Within enhanced XRT position (Beardmore et al., GCN 
20147) we detected a source coinciding with the afterglow of GRB 161014A 
(Malesani et al., GCN 20146; Butler et al., GCN 20149). Preliminary 
photometry of the source is following

Date       UT start   t-T0   Filter   Exp.   OT   Err.  UL
                       (mid, days)     (s)
2016-11-08 23:06:16   0.83869  R      28*120 21.8 0.20  22.0

Our photometry of the afterglow might be  affected by nearby galaxy 
mentioned in GCN 20149 (Malesani et al.)

Photometry is based on nearby SDSS-DR9 stars (Lupton transformations):
SDSS-DR9_id         R(Lupton)
J120315.88+245217.4 18.37
J120326.17+245228.7 18.71
J120318.05+245356.7 18.52
J120250.21+245354.3 18.35
J120258.81+245024.2 16.90
J120314.67+244944.0 17.06
J120321.43+244829.2 16.79


GRB_name: GRB161106A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20161
SUBJECT: GRB 161106A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/11/09 23:58:14 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

S. Nakahira (JAXA), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada (AGU),
K. Yamaoka (Nagoya U), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 161106A (Hamburg et al., GCN Circ. 20140;
Konus-Wind trigger time on 11:57:52.938) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 11:57:50.79 on 6 November 2016.
The burst signal was seen by all CGBM instruments.

The light curve of the SGM shows a FRED-like structure with possible overlapping pulses.
The emission starts at T0, peaks at T0+5 sec and ends at T+15 sec.
The T90 duration measured by the SGM data is 9.1 +- 0.5 sec (40-1000 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1162468560/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB161108A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20163
SUBJECT: GRB 161108A: MITSuME Okayama upper limits
DATE:    16/11/10 01:15:17 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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 161108A (Beardmore et al., GCNC 20145)
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 2016-11-08 17:48:36 UT (~14.3 h after
the burst). We could not detect the previously reported afterglow
(Malesani et al., GCNC 20146; Butler et al., GCNC 20149)
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
-----------------------------------------------------
0.63016    18:39:58    5940.0   >19.9  >19.6  >19.2
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB161109A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20164
SUBJECT: GRB 161109A: Swift-XRT observations
DATE:    16/11/10 08:00:39 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@ifc.inaf.it>

S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N.
Burrows (PSU) and P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 161109A (Desiante et al. GCN Circ. 20155)
in a series of observations tiled on the sky. The total exposure time
is 4.1 ks, distributed over 5 tiles; the maximum exposure at a single
sky location was 2.9 ks. The data were collected between T0+40.4 ks and
T0+63.6 ks, and are entirely in Photon Counting (PC) mode. 

Three uncatalogued X-ray sources have been detected, however none of
them is above the RASS limit or shows definitive signs of fading.
Therefore, at the present time we cannot identify which, if any, is the
afterglow. Details of these sources are given below:

Source 2:
  RA (J2000):  157.9051  =  10:31:37.24
  Dec (J2000): +61.8845  =  +61:53:04.4
  Error: 3.7 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (6.1 [+3.2, -2.4])e-3 ct s^-1   
  Distance: 244 arcsec from Fermi/LAT position.

Source 5:
  RA (J2000):  157.9726  =  10:31:53.43
  Dec (J2000): +61.9393  =  +61:56:21.6
  Error: 6.4 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (6.6 [+2.6, -2.1])e-3 ct s^-1   
  Distance: 471 arcsec from Fermi/LAT position.

Source 6:
  RA (J2000):  158.0653  =  10:32:15.66
  Dec (J2000): +61.6754  =  +61:40:31.5
  Error: 6.9 arcsec (radius, 90% conf.)
  Count-rate: (6.8 [+3.1, -2.4])e-3 ct s^-1   
  Distance: 635 arcsec from Fermi/LAT position.
  Flux: (2.01 [+0.91, -0.70])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Three catalogued sources were also detected.

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00060.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161109A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20165
SUBJECT: GRB 161109A: Lomonosov BDRG gamma ray discovery
DATE:    16/11/10 14:42:02 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.L.Dzhioeva,V.V.Bogomolov, S.I.Svertilov,
A.M.Amelushkin, V.O.Barinova, M.I.Panasyuk, A.V.Bogomolov, A.F.Iyudin, 
V.V.Kalegaev, D.Nguen,  V.L. Petrov, I.V.Yashin, P.S.Kazarian
Physics Department, Skobel'tsyn Institute of Nuclear Physics, Lomonosov Moscow 
State University

V. Lipunov, E.S. Gorbovskoy, N.Tyurina, D.Kuvshinov
Lomonosov Moscow State University, Sternberg Astronomical Institute

I. Park, J. Lee, S. Jeong
Department of Physics, Sungkyunkwan University, Seobu-ro, Jangangu, Suwonsi, 
Korea


At 06:11:45 UT on 09 Nov 2016,
the Lomonosov BDRG  Gamma-ray Burst Monitor 
(http://lomonosov.sinp.msu.ru/en/scientific-equipment-2/bdrg),
triggered GRB 161109A.
GRB 161106A (R. Desiante (INFN Torino), GCN 20155),
total duration ~25s,
the energy range 35-300 keV.
LC is available at:
http://master.sai.msu.ru/static/OT/0911.jpg

More information will be available at:
http://lomonosov.sinp.msu.ru/category/results/observation-gamma-ray-bursts
This Notice was ground-generated.

The message may be cited.


GRB_name: GRB161104A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20166
SUBJECT: GRB 161104A: Chandra X-ray observations
DATE:    16/11/10 17:27:14 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

R. Margutti (Northwestern U.), E. Berger (Harvard U.), and W. Fong (U.
Arizona) report:

"We observed the location of the short GRB161104A with the Chandra X-ray
Observatory (CXO) on 2016 Nov 8th, 14:41:45 UT, 364 ks after trigger (Mingo
et al., GCN 20123) under a pre-approved guest observer program (PI Berger).
No X-ray source is detected within the enhanced XRT position (Goad et al.,
GCN 20124). In particular, we do not find evidence for statistically
significant X-ray emission at the location of the optical source reported
by Troja  et al., GCN 20137 at RA, Dec = 05:11:34.5, -51:27:33.90.   Using
19.8 ks of CXO observations we infer a 3 sigma count-rate limit of  3.0E-4
c/s in the 0.5-8 keV energy range. The neutral hydrogen absorption in the
direction of the transient is 1.4E+20 cm-2 (Kalberla et al., 2005).
Assuming the spectral parameters that best fit the Swift-XRT observations
(power-law photon index Gamma=1.36  and no evidence for intrinsic neutral
hydrogen absorption, Burrows et al., GCN 20128) the inferred absorbed
(unabsorbed) flux limit is Fx< 4.4E-15 erg/s/cm2  (Fx<4.5E-15 erg/s/cm2) in
the 0.3-10 keV energy range. Our observations indicate a steepening of the
X-ray afterglow temporal decay. Starting from 20 ks after trigger, the
X-ray afterglow decays as t^-alpha with alpha>1.3.

We thank the CXO team for rapid scheduling of our observations."


GRB_name: GRB161108A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20167
SUBJECT: GRB 161108A: continued TSHAO optical observations
DATE:    16/11/10 20:53:57 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute),  I. 
Reva (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 161108A  (Beardmore et al., GCN 20145) with 
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. 
We obtained several images in R filter starting on Nov. 09 (UT) 
22:52:14. Within enhanced XRT position (Beardmore et al., GCN 20147) we 
detected the afterglow of GRB 161014A (Malesani et al., GCN 20146; 
Butler et al., GCN 20149). Preliminary photometry of the afterglow is 
following

Date       UT start   t-T0   Filter   Exp.   OT   Err.  UL
                       (mid, days)     (s)
2016-11-09 22:52:14   1.83762  R      41*120 22.0 0.24  22.2

The photometry of the afterglow might be  affected by nearby galaxy 
mentioned in GCN 20149 (Malesani et al.)

Photometry is based on nearby SDSS-DR9 stars (Mazaeva et al., GCN 20160).


GRB_name: GRB161104A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20168
SUBJECT: GRB 161104A: Magellan imaging and spectroscopy
DATE:    16/11/11 02:15:11 GMT
FROM:    Wen-fai Fong at U of Arizona  <wfong@email.arizona.edu>

W. Fong (University of Arizona) and R. Chornock (Ohio University) report:

We imaged the location of the short-duration GRB 161104A (Mingo et al., GCN
20213) with the Inamori-Magellan Areal Camera and Spectrograph (IMACS)
mounted on the Magellan/Baade 6.5-m telescope at a mid-time of 2016 Nov
7.170 UT (2.77 days post-burst). We obtained 6x360-sec of r-band exposures
in 1.0" seeing at an airmass of 1.3. We clearly detect the four optical
sources reported from GROND (Nicuesa Guelbenzu et al.; GCN 20132) and
Gemini (Troja et al.; GCN 20137) imaging. Given the relatively poor seeing,
accurate photometry of the individual sources is challenging. However, the
sources appear to have similar relative flux levels as previously reported,
suggesting a lack of significant variability in any of these sources. We
note that Source A (Nicuesa Guelbenzu et al.; GCN 20132) is fully
coincident with the latest XRT position*, while the three remaining sources
are on the outskirts of the position.

In addition, we obtained 3x1800-sec of spectroscopy with Magellan/IMACS on
2016 Nov 8 UT in 0.6" seeing at an airmass of 1.1.  We used the 200 line
grism and the f/2 camera to cover 4000-10000 Angstroms. The slit was
aligned through Sources A and B (Nicuesa Guelbenzu et al.; GCN 20132) and
also serendipitously passed through a nearby extended source 6.1" from the
center of the XRT position (Source X; RA=5:11:34.77, Dec=-51:27:41.8). The
spectrum of Source A exhibits a red continuum indicative of an early-type
galaxy with prominent Ca II H+K stellar absorption lines at z=0.793. Source
B has a faint trace with a single possible emission line of unknown
identification near 9780 Angs. The spectrum of Source X is also that of an
early-type galaxy at z=0.788. We note that both Sources A and X lack
prominent emission lines of either [O II] 3727 or H-beta.  The similarity
in the redshifts of Sources A and X, their early-type galaxy spectra, and
the abundance of extended sources in the vicinity of the XRT position may
signify an origin from a cluster or group.

We thank Magellan telescope operators Hernan, Jorge and Mauricio for their
assistance with these observations.

*http://www.swift.ac.uk/xrt_positions/


GRB_name: GRB161109A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20169
SUBJECT: GRB 161109A: Swift/UVOT Upper Limits
DATE:    16/11/11 15:34:35 GMT
FROM:    Sam Emery at MSSL-UCL  <samuel.emery.15@ucl.ac.uk>

S. W. K Emery (MSSL-UCL) and A. D'Ai (INAF-IASFPA) report on behalf
of the Swift/UVOT team:

Swift-UVOT performed follow-up observations of the Fermi/LAT-detected
burst GRB 161109A (Desiante et al. GCN Circ. 20155) in a series of
observations tiled on the sky. Observations were taken in the u band
filter between T0+40.4 ks and T0+63.3 ks after the Fermi trigger.

Swift/UVOT did not find any new optical counterpart. The 3 sigma
upper limits at the position of each of the uncatalogued X-ray sources (Gibson et
al. GCN Circ. 20164) are:

Source  T_start (s)  T_end (s)  Exposure Time (s)  filter   3s UL

Source 2     40425     57980     1152     u     20.11
Source 3     40425     57980     1152     u     20.08 
Source 6     41245     63272     1121     u     19.22

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).


GRB_name: GRB161109A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20171
SUBJECT: GRB 161109A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/11/11 23:29:43 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

I. Takahashi (IPMU), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, Y. Yamada (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 161109A (Desiante et al., GCN Circ. 20155;
Bissaldi et al., GCN Circ. 20156; Konus-Wind trigger time on 6:18:43.284)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 6:18:40.56 on
9 November 2016.  The burst signal was seen by all CGBM instruments.

The light curve of the SGM shows at least four peaks.  The first three peaks
are rather weak, and they peak at T+5 sec, T+10 sec and T+15 sec, respectively.
The forth peak is the brightest, and it starts at T+20 sec, peaks at T+22 sec
and ends at T+32 sec.  The T90 duration measured by the SGM data is
24.8 +- 2.3 sec (40-1000 keV).

The light curve is available at

http://yoshidalab.mydns.jp/cgbm_trigger/flight/1162707406/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB161113A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20172
SUBJECT: GRB 161113A: Swift detection of a burst
DATE:    16/11/13 17:51:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

P. D'Avanzo (INAF-OAB), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
J. A. Kennea (PSU), H. A. Krimm (CRESST/NSF/USRA),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:

At 17:30:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161113A (trigger=722063).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 179.834, -5.347, which is 
   RA(J2000)  =  11h 59m 20s
   Dec(J2000) = -05d 20' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two overlapping peaks
with a total duration of about 45 sec.  The peak count rate
was ~2400 counts/sec (15-350 keV), at ~15 sec after the trigger. 

The XRT began observing the field at 17:31:18.5 UT, 51.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 179.79351,
-5.30848 which is equivalent to:
   RA(J2000)  = 11h 59m 10.44s
   Dec(J2000) = -05d 18' 30.5"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 200 arcseconds from the BAT onboard position. This position
may be improved as more data are received; the latest position is
available at http://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.11 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 6.5
(+6.17/-4.70) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.07e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 78 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.02. 

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.)


GRB_name: GRB161113A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20173
SUBJECT: GRB 161113A: RATIR Optical and NIR Observations
DATE:    16/11/14 17:56:08 GMT
FROM:    Nat Butler at Az State U  <natbutler@asu.edu>

Nat Butler (ASU), Alan M. Watson (UNAM), 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), JosÃ© A.
de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez (UNAM), Carlos
RomÃ¡n-ZÃºÃ±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 161113A (D'Avanzo, et al., GCN 20172) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro MÃ¡rtir from 2016/11 14.48 to 2016/11 14.52 UTC (17.94 to
19.01 hours after the BAT trigger), obtaining a total of 0.71 hours
exposure in the r and i bands and 0.14 hours exposure in the Z, Y, and H
bands.

For a source within the Swift-XRT error circle, in comparison with the
USNO-B1 and 2MASS catalogs, we obtain the following upper limits (3-sigma):

  r > 22.41
  i > 22.18
  Z > 21.21
  Y > 20.72
  H > 18.83

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161113A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20174
SUBJECT: GRB 161113A: Enhanced Swift-XRT position
DATE:    16/11/14 18:34:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2998 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 161113A, 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 = 179.79452, -5.30897 which is equivalent
to:

RA (J2000): 11h 59m 10.68s
Dec (J2000): -05d 18' 32.3"

with an uncertainty of 2.2 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.


GRB_name: GRB161113A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20175
SUBJECT: GRB 161113A: Kuban State University optical upper limit
DATE:    16/11/14 19:08:55 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), A. Ivanov (KubSU), V. Ivanov (KubSU), V. Lysenko 
(KubSU), D. Ivanova (KubSU), A. Volnova (IKI), A. Pozanenko (IKI) report 
on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 161113A (D'Avanzo, et al., GCN 20172) with 
the RC510 telescope (0.51-m f/8) of Kuban State University Astrophysical 
Observatory. We obtained several unfiltered  images   starting on Nov. 
14 (UT) 02:02:08. Within enhanced XRT position (Evans et al., GCN 20174) 
we do not detect any source. Preliminary photometry of the field is 
following

   Date       UT start   t-T0    Filter  Exp.  OT   Err. UL(3 sigma)
                        (mid, days)      (s)
2016-11-14   02:02:08   0.37062 CR      52*30 n/d  n/d  18.9

Photometry is based on nearby USNO-B1.0 stars (R2 magnitudes).


GRB_name: GRB161113A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20176
SUBJECT: GRB 161113A: Swift-XRT refined Analysis
DATE:    16/11/15 08:12:35 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), B. Sbarufatti
(INAF-OAB/PSU), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), B. Mingo (U.
Leicester) report on behalf of the Swift-XRT team:

We have analysed 23 ks of XRT data for GRB 161113A (D'Avanzo et al. GCN
Circ. 20172), from 42 s to 74.9 ks after the  BAT trigger. The data
comprise 118 s in Windowed Timing (WT) mode (the first 8 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 Evans et
al. (GCN Circ. 20174).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.52 (+0.25, -0.28). At T+109 s  the decay
steepens to an alpha of 6.0 (+0.5, -0.4) before breaking again at T+272
s to a final decay with index alpha=0.45 (+0.04, -0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.82 (+/-0.09). The
best-fitting absorption column is  3.63 (+0.29, -0.27) x 10^21 cm^-2,
in excess of the Galactic value of 2.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.03 (+0.22, -0.21)
and a best-fitting absorption column of 1.2 (+0.6, -0.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (4.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.2 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 2.1 x 10^20 cm^-2
Excess significance: 3.0 sigma
Photon index:      2.03 (+0.22, -0.21)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00722063.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161113A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20177
SUBJECT: GRB 161113A: Swift/UVOT Upper Limits
DATE:    16/11/15 13:15:18 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL), P. D'Avanzo (INAF-OAB) and S. W. K. Emery 
(UCL-MSSL) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161113A 61 
s after the BAT trigger (D'Avanzo et al., GCN Circ. 20172).
No optical afterglow consistent with the XRT position (Evans et al. GCN 
Circ. 20174) 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            61          211          147         >19.8
u_FC               274          483          206         >18.8
white              555         6332          369         >21.0
v                 5152         5352          197         >19.2
b                 4537         6171          393         >20.1
u                  274         5966          599         >19.6
w1                4126         5762          393         >20.1

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.02 in the direction of the 
burst (Schlegel et al. 1998).


GRB_name: GRB161113A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20178
SUBJECT: GRB 161113A: Swift-BAT refined analysis
DATE:    16/11/15 14:49:29 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

S. D. Barthelmy (GSFC),  J. R. Cummings (GSFC/UMBC), P. D'Avanzo (INAF-OAB),
N. Gehrels (GSFC), H. A. Krimm (NSF/USRA), 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+499 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161113A (trigger #722063)
(D'Avanzo, et al., GCN Circ. 20172).  The BAT ground-calculated position is
RA, Dec = 179.794, -5.316 deg which is 
   RA(J2000)  =  11h 59m 10.6s 
   Dec(J2000) = -05d 18' 57.3" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a pair of overlapping peaks, both containing 
substructure.  The first peak begins at T-3 sec and peaks at T+5 sec.  The second
peaks at T+15 sec and continues until about T+60 sec.
T90 (15-350 keV) is 42.60 +- 11.10 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.12 to T+64.88 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.73 +- 0.10.  The fluence in the 15-150 keV band is 1.5 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+15.28 sec in the 15-150 keV band
is 1.4 +- 0.2 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/722063/BA/


GRB_name: GRB161117A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20179
SUBJECT: GRB 161117A: Swift detection of a burst with an optical counterpart
DATE:    16/11/17 01:46:55 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), V. D'Elia (ASDC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/NSF/USRA), F. E. Marshall (NASA/GSFC) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 01:35:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161117A (trigger=722604).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 322.070, -29.629 which is 
   RA(J2000)  =  21h 28m 17s
   Dec(J2000) = -29d 37' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several bright peaks
with a total duration of about 160 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~110 sec after the trigger. 

The XRT began observing the field at 01:36:37.5 UT, 60.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 322.0530, -29.6119 which is equivalent to:
   RA(J2000)  = +21h 28m 12.72s
   Dec(J2000) = -29d 36' 42.8"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 81 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 8.04e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 69 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 21:28:12.53 = 322.05219
  DEC(J2000) = -29:36:48.9  = -29.61358
with a 90%-confidence error radius of about 0.62 arc sec. This position is 6.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.40 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.06. 

Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
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.)


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20180
SUBJECT: GRB 161117A: VLT/X-shooter spectroscopy and redshift
DATE:    16/11/17 08:32:11 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

Daniele Malesani (DARK/NBI and DTU Space), Thomas Kruehler (MPE), Kasper 
E. Heintz (Univ. Iceland and DARK/NBI), and Johan P. U. Fynbo (DARK/NBI) 
report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 161117A (Cummings et al., GCN 
20179) with the ESO VLT Kueyen equipped with the X-shooter spectrograph. 
In the acquisition image, taken on 2016 Nov 17.097 UT (0.73 hr after the 
GRB), the optical afterglow is clearly detected with a magnitude R ~ 19 
(assuming R = 18.10 for the USNO star at RA = 21:28:14.70, Dec = 
-29:37:08.8). The seeing was very poor, around 2.5", and the sky 
conditions were partially cloudy.

Four spectra by 600 s each were collected covering the full X-shooter 
wavelength range 3000-25,000 AA. A faint trace is detected, down to at 
least 3800 Ã…. Superimposed on it, we are able to identify a number of 
absorption features which we interpret as due to Mg I, Mg II, and Fe II, 
all at a common redshift z = 1.549.

We acknowledge excellent support from the ESO observing staff in Paranal,
in particular Elizabeth Bartlett, Eleonora Sani, Steffen Mieske, and Jose
Velasquez, and the visiting astronomers Gerard Gilmore, Amelia Bayo, and
Aurora Aguayo.

[GCN OPS NOTE(17nov16):  Per author's request, the last paragraph was modified.]


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20181
SUBJECT: GRB161117A: REM optical and NIR afterglow detection
DATE:    16/11/17 08:52:18 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza, S. Covino, A. Melandri (INAF/OAB) report on behalf of the REM team:

We observed the field of GRB 161117A (Cummings et al., GCN 20179) with the 60-cm robotic telescope REM 
located at the La Silla Observatory (Chile). The observations started at 01:37:05 UT, 89 seconds after the burst, 
and were carried out simultaneously in the g, r, i, z and H bands.

A preliminary photometry indicates that the optical and NIR afterglow (Cummings et al., GCN 20179; Malesani 
et al. GCN 20180) is detected with a magnitude H = 16.4 +/- 0.3 at t-t0 = 233 s, and r = 18.3 +/- 0.3 at t-t0 = 808 s. 
Magnitudes are in the AB system and have been calibrated with respect to the 2MASS (H-band) and APASS 
(r-band) catalogues.


GRB_name: GRB161117B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20182
SUBJECT: GRB 161117B: Swift detection of a burst
DATE:    16/11/17 10:04:47 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

E. Troja (NASA/GSFC/UMCP), A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC),
P.A. Evans (U Leicester), H. A. Krimm (CRESST/NSF/USRA),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 09:49:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161117B (trigger=722642).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 298.855, -67.707 which is 
   RA(J2000) = 19h 55m 25s
   Dec(J2000) = -67d 42' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed am initial weak peak
near the trigger time followed by stronger emission starting about 100
seconds later.  The total duration is about 150 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~135 sec after the trigger. 

The XRT began observing the field at 09:50:58.0 UT, 74.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
298.8244, -67.7029 which is equivalent to:
   RA(J2000)  = 19h 55m 17.85s
   Dec(J2000) = -67d 42' 10.6"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 44 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.49 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 5.3
(+2.89/-2.47) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.69e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 82 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.10. 

Burst Advocate for this burst is E. Troja (eleonora.troja AT nasa.gov). 
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.)


GRB_name: GRB161117B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20183
SUBJECT: GRB 161117B: LCO optical observations
DATE:    16/11/17 11:30:18 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), C.G. Mundell 
(U. Bath), A. Gomboc (U. Nova Gorica) on behalf of a large collaboration 
report:

One of the LCO 1-m telescope units in Siding Springs began observing 
Swift GRB 161117B (Troja et al., GCN 20182) in the SDSS r filter on 
November 17, 10:28:49 UT (39 minutes since the GRB trigger time). We do 
not find any object within the XRT error circle down to the following limit:

Mid time from GRB     Exposure     Filter       Magnitude
(min)                  (s)
----------------------------------------------------------
45                    5x120        SDSS-R       > 21.2
----------------------------------------------------------

Calibration is done against nearby USNOB-1 stars.


GRB_name: GRB161117A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20184
SUBJECT: GRB 161117A: Enhanced Swift-XRT position
DATE:    16/11/17 11:45:40 GMT
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 7318 s of XRT Photon Counting mode data and 11 UVOT
images for GRB 161117A, 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 = 322.05243, -29.61401 which is equivalent
to:

RA (J2000): 21h 28m 12.58s
Dec (J2000): -29d 36' 50.4"

with an uncertainty of 1.4 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.


GRB_name: GRB161117A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20185
SUBJECT: GRB 161117A: Swift-XRT refined Analysis
DATE:    16/11/17 12:10:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

K.L. Page (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A.
D'Ai (INAF-IASFPA), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), L.M.
McCauley (PSU), B. Mingo (U. Leicester), A.P. Beardmore (U. Leicester)
and J.R. Cummings report on behalf of the Swift-XRT team:

We have analysed 7.7 ks of XRT data for GRB 161117A (Cummings et al.
GCN Circ. 20179), from 52 s to 19.0 ks after the  BAT trigger. The data
comprise 384 s in Windowed Timing (WT) mode (the first 7 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. 20184).

The late-time light curve (from T0+5.1 ks) can be modelled with a
power-law decay with a decay index of alpha=0.92 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.322 (+/-0.028). The
best-fitting absorption column is  2.9 (+/-0.8) x 10^21 cm^-2, at a
redshift of 1.549, in addition to the Galactic value of 4.4 x 10^20
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.94 (+/-0.08) and a best-fitting absorption column of 7.4 (+1.9,
-1.8) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum  is 3.5 x 10^-11 (4.4
x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 4.4 x 10^20 cm^-2
Intrinsic column:    7.4 (+1.9, -1.8) x 10^21 cm^-2 at z=1.549
Photon index:      1.94 (+/-0.08)

If the light curve continues to decay with a power-law decay index of
0.92, the count rate at T+24 hours will be 0.050 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-12 (2.2 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00722604.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161117B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20186
SUBJECT: GRB 161117B: Enhanced Swift-XRT position
DATE:    16/11/17 14:13:23 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 787 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 161117B, 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 = 298.82508, -67.70256 which is equivalent
to:

RA (J2000): 19h 55m 18.02s
Dec (J2000): -67d 42' 09.2"

with an uncertainty of 1.7 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.


GRB_name: GRB161117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20188
SUBJECT: GRB 161117A: Swift-BAT refined analysis
DATE:    16/11/17 18:35:49 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
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 161117A (trigger #722604)
(Cummings, et al., GCN Circ. 20179).  The BAT ground-calculated position is
RA, Dec = 322.053, -29.612 deg which is
  RA(J2000)  =  21h 28m 12.8s
  Dec(J2000) = -29d 36' 41.7"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows three main overlapping peaks, of increasing
amplitude. The tops of the peaks are at T+3, T+35 and T+112 s, respectively.
The burst faded to baseline by about 160 seconds.
T90 (15-350 keV) is 125.7 +- 1.1 sec (estimated error including systematics).

The time-averaged spectrum from T-6.00 to T+154.44 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.19 +- 0.12,
and Epeak of 73.9 +- 4.3 keV (chi squared 33.82 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.0 +- 0.0 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+111.35 sec in the 15-150 keV band is
6.8 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.82 +- 0.00 (chi squared 122.02 for 57 d.o.f.).  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/722604/BA/


GRB_name: GRB161117B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20189
SUBJECT: GRB 161117B: Swift-BAT refined analysis
DATE:    16/11/17 18:40:10 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),  J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), 
(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 161117B (trigger #722642)
(Troja, et al., GCN Circ. 20182).  The BAT ground-calculated position is
RA, Dec = 298.830, -67.681 deg which is 
   RA(J2000)  =  19h 55m 19.1s 
   Dec(J2000) = -67d 40' 51.8" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.

The mask-weighted light curve shows a complex structure.  The first set of peaks
begins around T-10 sec, peaks at T+2 and fades by T+10 sec.  The second set 
of peaks begins around T+92 sec, peaks at T+102 sec and fades nearly to 
background by T+115 sec.  This is when the third set of peaks begins to rise,
which peaks at T+T+135 sec and fades by T+160 sec.  All of these peak 
structures have multiple sub-peaks. T90 (15-350 keV) is 152.51 +- 3.37 sec 
(estimated error including systematics).

The time-averaged spectrum from T-8.32 to T+157.44 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.39 +- 0.28, 
and Epeak of 37.5 +- 5.5 keV (chi squared 39.62 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.0 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+133.80 sec in the 15-150 keV band is
6.0 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.14 +- 0.06 (chi squared 64.42 for 57 d.o.f.).  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/722642/BA/


GRB_name: GRB161117A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20190
SUBJECT: GRB 161117A: Swift/UVOT Detection
DATE:    16/11/17 23:04:40 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and J. R. Cummings (NASA/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161117A
69 s after the BAT trigger (Cummings et al., GCN Circ. 20179).
A source consistent with the XRT position
(Goad et al., GCN Circ. 20184)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  21:28:12.55 = 322.05230 (deg.)
    Dec (J2000) = -29:36:49.1  = -29.61365 (deg.)
with an estimated uncertainty of 0.44 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are
in the table below. The lack of detections in the m2 and w2 filters
is consistent with the redshift of 1.549 reported by
Malesani et al. (GCN Circ. 20180).

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white               69          219          147         18.26 +/- 0.05
v                  611         6146          255         18.77 +/- 0.19
b                  536         5531          236         19.42 +/- 0.17
u                  281          531          246         19.48 +/- 0.20
w1                 660         6556          255         19.48 +/- 0.25
m2                1064        13173          712        >20.2
w2                 586        11751         1141        >20.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.06 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161117B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20191
SUBJECT: GRB 161117B: Swift/UVOT Upper Limits
DATE:    16/11/17 23:07:40 GMT
FROM:    Frank Marshall at GSFC  <femarsha@khamseen.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161117B
84 s after the BAT trigger (Troja et al., GCN Circ. 20182).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 20186)
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) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            84          234          147         >21.1
u_FC               296          546          246         >20.3
white               84         1026          334         >21.4
v                  626          820           39         >18.1
b                  552          745           39         >19.6
u                  296          720          265         >20.3
w1                 676          870           39         >18.9
m2                 651          844           39         >19.9
w2                 602         1050           57         >19.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161117A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20192
SUBJECT: GRB 161117A: Fermi GBM detection/observation
DATE:    16/11/18 01:16:45 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

B. Mailyan (UAH) and A. Goldstein (USRA) report on behalf of the Fermi GBM Team:

"At 01:35:31.36 UT on 17 November 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161117A (trigger 501039335/161117066),
which was also detected by Swift (Cummings et al., GCN 20179).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight is 94 degrees.

The GBM light curve shows bright, multiple peaks with a duration (T90)
of about 122 s (50-300 keV).  The time-averaged spectrum
from T0-4.7 s to T0+129.4 s is adequately fit by a Band function with
Epeak = 68.04 +/- 2.66 keV, alpha = -0.43 +/- 0.07, and beta = -2.27 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
 (3.93 +/- 0.079)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+116 s in the 10-1000keV band is 10.3 +/- 0.5 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20193
SUBJECT: GRB 161117A: GMG observation limit
DATE:    16/11/18 05:31:04 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, X. Yu, and J.-M. Bai (YNAO) report:


We observed the field of GRB 161117A (Cummings et al., GCN 20179) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG)
station of Yunnan Observatories. Observations began from 11:07:21 UT, Nov. 17th, 2016, about 9.5 hours after the trigger. 
We did not detect any source at the afterglow position down to a limit of R~20.6 mag.


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20194
SUBJECT: GRB 161117A: TAROT La Silla observatory optical observations
DATE:    16/11/18 11:25:16 GMT
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 161117A detected by SWIFT
(trigger 722604) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 26s after the GRB trigger
(14s after the notice). The elevation of the field decreased from
48 degrees above horizon and weather conditions
were good.

A difficulty is the presence of the bright star
NOMAD1 0603-1050209 (ra=322.0444192 dec=-29.6163561)
of magnitude R=11.060 located at 25 arcsec from the
the GRB provided at by Marshall et al. (GCNC 20190).

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+26s to t0+86s : Rlim = 16.8

Magnitudes were estimated with the nearby NOMAD1 stars
and are not corrected for galactic dust extinction.


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20195
SUBJECT: GRB 161117A: MASTER-OAFA (Argentina) prompt OT observations
DATE:    16/11/18 12:54:01 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

R.Podesta, C.Lopez, F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA) , National University of San 
Juan, Argentina

H. Levato, C. Saffe
Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE),
San Juan, Argentina

V. Lipunov, E. Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina,
A.V.Krylov, I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov
Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik
Kislovodsk Solar Station of the Pulkovo Observatory

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

MASTER-OAFA  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in OAFA was pointed to the  GRB161117A 22 sec after notice time 
and 31 sec after trigger time at 2016-11-17 01:36:13 UT. On our first (10s 
exposure)  set we  found optical transient  within SWIFT error box 
(Cummings et al., 20179) at the Swift UVOT position (Cummings et al., 
20179; Daniele Malesani et al. GCN 20180;).
The OT magnitude ~17.0 .
The 5-sigma upper limit has been about 17.5 mag

After several minutes OT disapear and apear against around 01 35 56 UT
  with unfiltered (red) magnirude ~ 18.0 
(cf  D'Avanzo et al., GCN 20181;).

The observations started at
zenit distance = 42 degrees,
galaxy latitude b = -46 degree.
The moon (91 % bright part) below the horizon (The altitude of 
the Moon is -1 degree ).
The sun  altitude  is -25.6 degree.
The object can be observed till 2016-11-17 05:44:35 UT.

The message may be cited.


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20196
SUBJECT: GRB 161117A iTelescope observation
DATE:    16/11/18 13:07:22 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Kitaoka, T. Sakamoto, A. Yoshida (AGU)

We observed the field of GRB 161117A detected by Swift
(Cummings et al., GCN Circ. 20179) with the iTelescope.Net
(http://www.itelescope.net) T11 (20" Plane wave ) telescope
located at the AstroCamp Observatory (Mayhill, New Mexico, USA).
20 images of 60 sec exposures were taken in the R filter
starting from November 17 02:02:56 (UT) about 27 minutes
after the trigger and stopped on November 17 02:45:49 (UT).
We do not detect the optical afterglow both in the individual
images and the stacked image at the optical afterglow position
(Marshall et al., GCN Circ. 20190).  The estimated five sigma
upper limit of the combined image (total exposure of 1200 sec)
is ~16.9 using the USNO-B1 catalog.


GRB_name: GRB161117A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20197
SUBJECT: Konus-Wind observation of GRB 161117A
DATE:    16/11/18 13:12:24 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 161117A
(Swift-BAT observation: Cummings et al., GCN Circ. 20179;
Fermi-GBM detection: Mailyan & Goldstein, GCN Circ. 20192)
triggered Konus-Wind at T0=5738.426 s UT (01:35:38.426).

The burst light curve shows  three bright emission peaks in the interval 
from ~T0-7 s to ~T0+130 s.
The emission is seen up to ~1 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161117_T05738/

As observed by Konus-Wind, the burst
had a fluence of 2.41(-0.14,+0.15)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0-0.342 s,
of 1.94(-0.77,+0.78)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+123.136 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.86(-0.33,+0.36)
and Ep = 69(-7,+6) keV (chi2 = 40/47 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta <-3.5
(chi2 =40/46 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
with  alpha = -0.56(-0.42,+0.52)
and Ep = 139(-20,+27) keV (chi2 = 49/47 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 49/46 dof).

Assuming the redshift z=1.549 (Malesani et al., GCN 20180)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~1.3x10^53 erg,
the peak luminosity L_iso is ~3.0x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~176 keV.

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB161117B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20198
SUBJECT: GRB 161117B: Swift-XRT refined Analysis
DATE:    16/11/20 13:16:42 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@ifc.inaf.it>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), T.G.R.
Roegiers (PSU), L.M. McCauley (PSU), J.A. Kennea (PSU), B. Mingo (U.
Leicester), A.P. Beardmore (U. Leicester) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift-XRT team:

We have analysed 5.9 ks of XRT data for GRB 161117B (Troja et al. GCN
Circ. 20182), from 65 s to 206.7 ks after the  BAT trigger. The data
comprise 178 s in Windowed Timing (WT) mode (the first 7 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 Osborne et
al. (GCN Circ. 20186).

The light curve shows an initial bright flare that is part of 
the prompt GRB emission. At T+95.1 s the decay can be modelled with 
a power-law of index alpha of 0.43 (+0.09, -0.07) before breaking at
T+101 ks to a final decay with index alpha=6.7 (+1.3, -5.2).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.10 (+/-0.05). The
best-fitting absorption column is  3.8 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 6.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.98 (+0.24, -0.23)
and a best-fitting absorption column of 5.3 (+1.5, -1.3) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.2 x 10^-11 (6.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.3 (+1.5, -1.3) x 10^21 cm^-2
Galactic foreground: 6.5 x 10^20 cm^-2
Excess significance: 5.9 sigma
Photon index:      1.98 (+0.24, -0.23)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00722642.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161108A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20200
SUBJECT: GRB 161108A: 15 GHz upper limits from AMI
DATE:    16/11/21 18:19:57 GMT
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 
161108A (Beardmore et al., GCN 20145) 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 Nov 08.19, Nov 09.40, Nov 
12.35 and Nov 15.36 (UT) do not reveal any radio source at the XRT 
location (Beardmore et al., GCN 20147), with 3sigma upper limits of 378 
uJy, 284 uJy, 190 uJy and 93 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/.


GRB_name: GRB161119A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20201
SUBJECT: GRB 161119A: MASTER-SAAO possible OT detection during Fermi Alert 
DATE:    16/11/21 19:49:43 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V.M. Lipunov, E.Popova, E.Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina,
A.V.Krylov, I.Gorbunov, P.Balanutsa, A.Kuznetsov, V.V.Chazov
Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

R.Podesta, C.Lopez, F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA) , National University of San 
Juan, Argentina

H. Levato, C. Saffe
Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE),
San Juan, Argentina

K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk
Irkutsk State University

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Senik
Kislovodsk Solar Station of the Pulkovo Observatory

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

MASTER OT J032252.81-482912.8 discovery

MASTER-SAAO  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in SAAO was starting survey on the FERMI  GRB161119.63 error-box 
(ra=03 08 45 dec=-47 12 35 r=3.27)  8795 sec after notice time and 11978 
sec after trigger time at 2016-11-19 18:30:45 UT. The 5-sigma upper limit 
on our first (60s exposure)  set is about 18.9 mag

During inspection of Fermi trigger 501261070 ( RaDec=47.190;-47.210, 
GRB_ERROR=3.27deg, GRB_TIME=2016/11/19 15:11:06.40UT 
http://gcn.gsfc.nasa.gov/other/501261070.fermi  , at alert time the 
GRB_altitude= MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER 
Global Robotic 
Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) 
= 03h 22m 52.70s -48d 29m 10.9s  on
  2016-11-19 21:17:17.878UT with unfiltered m_OT=17.8 (mlim=19.7).

This OT is seen on 6 sequential images ( 180s expositions), from 
2016-11-19 21:07:11 to 2016-11-19 21:20:34 with m_lim=19.8 on single and 
20.7 on summary images with m_OT=17.8

There is no OT on 2016-11-18 21:14:00UT with unfiltered mlim=20.3 and on 
2016-11-20 22:48:44UT with mlim=19.8

There is no any sources in VIZIER database outside.

Spectral observations are required.
The discovery and reference images are available at:

http://master.sai.msu.ru/static/OT/032252.81-482912.8.png

The observations made on zenit distance = 40 degrees, galaxy latitude b = 
-56 degree.
The moon (67 % bright part) below the horizon (The altitude of the Moon is 
-44 degree ).
Observations started at twilight.
The sun  altitude  is -14.2 degree.
The object can be observed till sunrise at 2016-11-20 03:24:39

The message may be cited.


GRB_name: GRB161117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20202
SUBJECT: GRB 161117A: SMARTS optical/IR afterglow observations
DATE:    16/11/22 01:11:47 GMT
FROM:    Bethany Cobb at GWU  <bcobb@gwu.edu>

B. E. Cobb (GWU), reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 161117A
(GCN 20179, Cummings et al.) at two epochs (with mid-exposure times of
2016-11-17 02:38 UT & 2016-11-18 01:47 UT). For each epoch, several
dithered images were obtained with total summed exposure times of
15 min in V and I and 12 min in J and K.

The fading afterglow of GRB 161117A (e.g. GCN 20179, Cummings et al.;
GCN 20180, Malesani et al.; GCN 20181, D'Avanzo et al.) was detected
with the following preliminary magnitudes (or 3-sigma limits):

mid-exposure
time post-burst
(hours)            V mag            I mag             J mag             K
mag
1.03333          19.42+/-0.10  18.69+/-0.07  18.40+/-0.15  16.49+/-0.11

24.19361        >22.3              >21.1             >18.5             >16.7

(Optical photometry is calibrated against Landolt standard stars
and IR photometry is calibrated against 2MASS stars in the field.)


GRB_name: GRB161123A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20203
SUBJECT: GRB 161123A: MAXI/GSC detection
DATE:    16/11/23 04:51:45 GMT
FROM:    Motoko Suzuki at RIKEN  <motoko@crab.riken.jp>

C. Hanyu (Miyazaki U.), S. Nakahira (JAXA), H. Negoro (Nihon U.),
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara (JAXA), 
Y. E. Nakagawa (JAMSTEC),
T. Mihara, M. Sugizaki, M. Serino, W. Iwakiri,  M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), 
N. Kawai, N.Isobe, S.Sugita, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara, S. Harita, Y. Muraki (Tokyo Tech), 
A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), 
H. Tsunemi, R. Shomura (Osaka U.), 
M. Nakajima, K. Tanaka, T. Masumitsu, T. Kawase (Nihon U.), 
Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto, S. Oda (Kyoto U.), 
Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), 
M. Yamauchi, K. Furuya (Miyazaki U.), 
K. Yamaoka (Nagoya U.)
report on behalf of the MAXI team:
 
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source 
at  03:05:58 UT on 2016 November 23.
The X-ray flux averaged over the scan was 149 +- 26 mCrab(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (32.229, -40.884) deg = (02 08 54, -40 53 02) (J2000)
(R.A., Dec) = (31.566, -40.860) deg = (02 06 15, -40 51 36) (J2000)
(R.A., Dec) = (32.268, -38.340) deg = (02 09 04, -38 20 24) (J2000)
(R.A., Dec) = (32.905, -38.394) deg = (02 11 37, -38 23 39) (J2000)
There was no significant excess flux in the previous transit at UT 01:33 
and in the next transit at 04:38 UT with an upper limit of 20 mCrab for each.

[GCN OPS NOTE(23nov16): Per author's request, the Subject was corrected
from 151123A to 161123A.]


GRB_name: GRB161123A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20204
SUBJECT: GRB 161123A: Tiled Swift observations
DATE:    16/11/23 09:15:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 161123A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00061

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20206
SUBJECT: GRB 161123A: Swift-XRT observations
DATE:    16/11/23 16:12:34 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), L.M. McCauley (PSU),
J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), A.P. Beardmore (U.
Leicester), S.L. Gibson (U. Leicester), P. D'Avanzo (INAF-OAB) and P.A.
Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 161123A (Hanyu et al. GCN Circ. 20203) in a series of
observations tiled on the sky. The total exposure time is 2.6 ks,
distributed over 7 tiles; the maximum exposure at a single sky location
was 825 s. The data were collected between T0+21.8 ks and T0+28.0 ks,
and are entirely in Photon Counting (PC) mode. 

No X-ray sources have been detected. The 3-sigma upper limit in the
field (not including the regions where the tiles overlap) ranges from
~0.02 to ~0.05 ct s^-1, corresponding to a 0.3-10 keV observed flux of
8.2e-13 to 1.9e-12 erg cm^-2 s^-1 (assuming a typical GRB spectrum).

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00061.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161129A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20210
SUBJECT: GRB 161129A: Swift detection of a burst
DATE:    16/11/29 07:32:25 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

D. Kocevski (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
J. R. Cummings (NASA/UMBC), B. Mingo (U Leicester),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and
M. H. Siegel (PSU) report on behalf of the Swift Team:

At 07:11:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161129A (trigger=724438).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 316.193, +32.125 which is 
   RA(J2000)  =  21h 04m 46s
   Dec(J2000) = +32d 07' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a duration of about 50 sec.  The peak count rate
was ~4400 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 07:13:01.8 UT, 82.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 316.22890, 32.13574 which is equivalent
to:
   RA(J2000)  = 21h 04m 54.94s
   Dec(J2000) = +32d 08' 08.7"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 116 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.50 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 2.5
(+2.84/-2.37) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White 
filter  starting 86 seconds after the BAT trigger. No credible 
afterglow candidate has  been found in the initial data products. The 
2.7'x2.7' sub-image does not cover 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 0.21. 

Burst Advocate for this burst is D. Kocevski (dankocevski AT gmail.com). 
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.)


GRB_name: GRB161129A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20211
SUBJECT: GRB 161129A: Enhanced Swift-XRT position
DATE:    16/11/29 12:54:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 2977 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 161129A, 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 = 316.22770, +32.13488 which is equivalent
to:

RA (J2000): 21h 04m 54.65s
Dec (J2000): +32d 08' 05.6"

with an uncertainty of 1.7 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.


GRB_name: GRB161129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20212
SUBJECT: GRB 161129A: Swift-XRT refined Analysis
DATE:    16/11/29 15:15:12 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), J.A. Kennea (PSU), B. Sbarufatti
(INAF-OAB/PSU), D.N. Burrows (PSU), P.A. Evans (U. Leicester), S.L.
Gibson (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC) and D. Kocevski report on behalf of the
Swift-XRT team:

We have analysed 7.8 ks of XRT data for GRB 161129A (Kocevski et al.
GCN Circ. 20210), from 90 s to 17.8 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN Circ. 20211).

The late-time light curve (from T0+3.9 ks) can be modelled with a
power-law decay with a decay index of alpha=2.21 (+0.15, -0.14).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.74 (+0.13, -0.12). The
best-fitting absorption column is  3.2 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 2.5 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.4 x 10^-11 (5.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 2.5 x 10^21 cm^-2
Excess significance: 2.0 sigma
Photon index:      1.74 (+0.13, -0.12)

If the light curve continues to decay with a power-law decay index of
2.21, the count rate at T+24 hours will be 7.1 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-14 (4.1 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00724438.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161129A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20213
SUBJECT: GRB161129A : Astrosat CZTI detection
DATE:    16/11/29 15:51:31 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

Kindly find the attachment of detection of GRB161129A by Astrosat CZTI.

-------------------------
Vidushi
JRF
IUCAA, Pune
E-mail: vidushi@iucaa.in
-------------------------


GRB_name: GRB161129A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20214
SUBJECT: GRB161129A : Astrosat CZTI detection
DATE:    16/11/29 15:56:22 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

V. Sharma, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed clear detection of GRB161129A (Swift BAT detection: S. Barthelmy et al., GCN Circ. 20210) in the 40-200 keV energy 
range. The light curve shows multiple peak structure at 07:12:06.0 UT, after 27 secs of the Swift Trigger. The measured peak count rate is 170.205 counts/sec 
above the background in combined data of four quadrants, with a total of 2160.0 counts. The local mean background count rate was 377.79 counts/sec. Using 
cumulative rates, we measure a T90 of 34.06 secs.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb.  CZTI is built by a TIFR-led consortium of institutes
across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.

-------------------------
Vidushi
JRF
IUCAA, Pune
E-mail: vidushi@iucaa.in
-------------------------


GRB_name: GRB161129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20215
SUBJECT: GRB 161129A: TSHAO optical observations / possible afterglow+host galaxy
DATE:    16/11/29 16:41:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Kusakin 
(Fesenkov Astrophysical Institute),  A. Volnova (IKI), A. Pozanenko 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed the field of 161129A  (Kocevski et al., GCN 20210)  with 
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory. 
We obtained several images in R filter starting on 2016-11-29 (UT) 
12:51:12.  Within enhanced XRT position (Beardmore et al. GCN 20211)  we 
detected  optical source which is absent in USNO-B1.0 but barely visible 
in DSS2 (red). At the moment we can not say anything about the source 
variability. The source might be a superposition of the afterglow and a 
host galaxy.  Preliminary photometry of the source  is following

Date       UT start   t-T0   Filter  Exp.   OT     Err.  UL
                       (mid, days)    (s)

2016-11-29 12:51:12 0.25949  R       13*300 20.60  0.06  22.4

Photometry is based on nearby USNO-B1.0 stars
USNO-B1.0_id    R2
1221-0612083 17.30
1221-0612140 19.02


GRB_name: GRB161129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20216
SUBJECT: GRB 161129A: Tautenburg Ic-band observations
DATE:    16/11/29 17:57:04 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose and B. Stecklum (both Thueringer Landessternwarte Tautenburg) 
report:

We imaged the field of GRB 161129A (Kocevski et al., GCN 20210) with the 
Tautenburg Schmidt telescope equipped with the prime focus CCD camera. 
Observations were performed at a midtime of 16:41 UT (November 29).

Inside the enhanced XRT error circle (radius 1.7 arcsec; Beardmore et al., 
GCN 20211) we find a faint source at coordinates RA, Decl. (J2000) = 
21:04:54.53, 32:08:05.9 (+/- 0.5 arcsec). Using the USNO B2 star at 
coordinates RA, Decl. (J2000) = 21:04:54.65, 32:08:05.6 as a photometric 
reference (Ic = 18.38), we measure for this source a preliminary (Vega) 
magnitude of Ic = 20.3 +/- 0.2 mag.

We note, however, that the DSS2 red shows a faint source at the central 
position of the enhanced XRT error circle at roughly the same coordinates. 
Given that the seeing in our images is about 2 arcsec, and given that our 
images are not substantially deeper than the DSS2 red, we cannot decide 
whether we see this faint source or a faint transient on top of it. In any 
case, at the time of our observations any optical transient was fainter 
than about Ic=20.


GRB_name: GRB161129A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20217
SUBJECT: GRB 161129A: Swift/UVOT Detection
DATE:    16/11/29 21:20:05 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and D. Kocevski (NASA/GSFC/ORAU) report on
behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161129A
86 s after the BAT trigger (Kocevski et al., GCN Circ. 20210).
A source consistent with the XRT position (Beardmore et al. GCN Circ.
20211) is detected in the initial UVOT exposures.

The source is detected in UVOT images at position:
RA =  21h 04m 54.6s (J2000)
Dec = 32d 08' 05.52" (J2000)
with an uncertainty of 0.6" (90% confidence)

Preliminary detections and 3-sigma upper limits using the UVOT
photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white               86         6356          400         20.61 +/- 0.20
v                 3858         5493          393        >19.0
b                  554         6314          413        >20.0
u                  298         6109          639        >19.8
w1                4268         5903          393        >19.4
m2                4063         5698          393        >19.6
w2                 604         5288          208        >19.5

There are low-significance signs of the source in all other filters. Though
the source seems to reach peak brightness around 500s the photometric
errors are also consistent with a constant source brightness up to 10ks.

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.21 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161129A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20218
SUBJECT: GRB 161129A: MITSuME Okayama Optical Observation
DATE:    16/11/30 00:35:47 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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 161129A (Kocevski et al., GCNC 20210)
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 2016-11-29 08:54:33 UT (~1.7 h after
the burst). We detected the previously reported source (Mazaeva
et al., GCNC 20215; Klose and Stecklum, GCNC 20216) in Rc and Ic
bands.

Photometric results and three sigma upper limit of the OT are
listed below. We used GSC2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'    Rc  Rc_err  Ic  Ic_err
------------------------------------------------------------------
0.11332    09:54:50    6120.0   >20.2   19.2 0.2    18.6 0.2
------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB161129A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20219
SUBJECT: GRB 161129A: Fermi GBM Detection
DATE:    16/11/30 01:21:31 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

O.J. Roberts (UCD), C. Meegan (UAH), and R. Hamburg (UAH)
report on behalf of the Fermi GBM Team:

"At 07:11:39.96 UT on the 29th of November 2016, the Fermi
Gamma-Ray Burst Monitor triggered and located GRB 161129A
(trigger 502096303/161129300), which was also detected by
Swift (Kocevski et al., GCN 20210). The GBM on-ground location
is consistent with the Swift position. The angle from the Fermi
LAT boresight is 87 degrees using the Swift position.

The GBM light curve shows a bright burst, with multiple peaks
over a duration (T90) of about 36 s (50-300 keV).
The time-averaged spectrum from T0+4.8 s to T0+45.7 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.13 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 197 +/- 21 keV.

The event fluence (10-1000 keV) in this time interval is
(8.4 +/- 0.4)E-06  erg/cm^2. The 1-sec peak photon flux measured
starting from T0+26 s in the 10-1000 keV band is 5.6 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20220
SUBJECT: GRB 161129A: Swift-BAT refined analysis
DATE:    16/11/30 02:02:40 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. D. Barthelmy (GSFC), J. R. Cummings (CPI),

N. Gehrels (GSFC), H. A. Krimm (NSF/USRA),

D. Kocevski (NASA/MSFC), A. Y. Lien (GSFC/UMBC),

C. B. Markwardt (GSFC), J. P. Norris (BSU),

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 161129A (trigger #724438)

(Kocevski, et al., GCN Circ. 20210).  The BAT ground-calculated position is

RA, Dec = 316.221, 32.137 deg which is

  RA(J2000)  =  21h 04m 53.1s

  Dec(J2000) = +32d 08' 11.9"

with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).

The partial coding was 69%.


The mask-weighted light curve shows a short spike from ~T0 to ~T+0.2 s,

followed by several overlapping pulses that last until ~T+45 s.

T90 (15-350 keV) is 35.53 +- 2.09 sec (estimated error including systematics).


The time-averaged spectrum from T+0.06 to T+44.58 sec is best fit by a simple

power-law model.  The power law index of the time-averaged spectrum is

1.57 +- 0.06.  The fluence in the 15-150 keV band is 3.6 +- 0.1 x 10^-6 erg/cm2.

The 1-sec peak photon flux measured from T+26.64 sec in the 15-150 keV band

is 3.4 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence

level.


Because the light curve seems to resemble that of a short GRB with

extended emission (Norris et al. 2010), we perform further analysis of the

short spike. Using a 4-ms binned light curve, the lag analysis finds a lag of

4 +/- 3 ms for the 50-100 keV to 15-25 keV band, which is consistent with

that of a short GRB. However, the spectral fit of the short spike

using a simple power-law model gives a power-law index of 1.9 +/- 0.3.

This value is on the softer end of short GRBs, and also softer than all the

initial pulses of those short GRBs with extended emission (Lien et al. 2016).

The power-law index of the spectrum for the rest of the light curve

is 1.53 +/- 0.06, which is harder than the initial spike and thus

unexpected from a short GRB with extended emission.


The results of the batgrbproduct analysis are available at

http://gcn.gsfc.nasa.gov/notices_s/724438/BA/


GRB_name: GRB160821B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20222
SUBJECT: GRB 160821B: HST detection of the optical and IR counterpart
DATE:    16/12/01 02:36:37 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

E. Troja (UMD/GSFC), N. Tanvir (U. Leicester), S. B. Cenko (NASA/GSFC),
A. Levan (U. Warwick), J. Barnes (U. Berkeley), A. Castro-Tirado (IAA-
CSIC), A. S. Fruchter (STScI), N. Gehrels (NASA/GSFC), J. Greiner (MPE),
N. Kawai (Tokyo Tech), R. Hounsell (UCSC), J. Hjorth (DARK/NBI), A. Lien
(NASA/GSFC), B. Metzger (Columbia),  D. Perley  (DARK/NBI), S. Rosswog
(U. Stockholm), T. Sakamoto (AGU), C. Thoene (IAA-CSIC), A. de Ugarte
Postigo (IAA-CSIC), and D. Watson (DARK/NBI) report:

We monitored the location of the short GRB 160821B (Siegel et al. GCN
19833; Xu et al. GCN 19834) with the Hubble Space Telescope under our
approved guest observer programs (GO14237 PI: Tanvir; GO14087 PI: Troja).
Observations were carried out with the Wide Field Camera (WFC3) in three
filters, F606W, F110W and F160W, at epochs 3.6, 10.4 and 23.2 days post-
burst. The GRB counterpart is clearly detected in all filters during the
first two epochs, and fades from a magnitude of F606W~25.8 (AB) in the
first epoch to become undetectable in the third epoch.

Assuming a redshift of z=0.162 from the nearby galaxy identified as the
likely host (Levan et al. GCN 19846), our observations rule out the
presence of an emerging supernova comparable to SN1998bw or to other SNe
associated to long GRBs. The observed fluxes constrain the contribution
of any r-process kilonova/macronova component to be at least a
factor ~5 fainter in the IR than that seen in GRB 130603B. The lack of
a bright supernova and the moderate-to-low ejecta mass implied by our
observations are consistent with this event being produced by the merger
of two neutron stars.

However, the current dataset cannot firmly exclude the presence of an
underlying, higher redshift host galaxy. Deeper HST observations aimed
at placing better constraints on the GRB redshift are on-going.

We thank the STScI staff, in particular Tricia Royle, for assistance
with rapidly scheduling our observations.


GRB_name: GRB161129A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20223
SUBJECT: GRB 161129A: MITSuME Okayama Ks-band Observation
DATE:    16/12/01 05:38:35 GMT
FROM:    Kenshi Yanagisawa at OAO/NAOJ  <yanagi@oao.nao.ac.jp>

K. Yanagisawa, D. Kuroda, Y. Shimizu, H. Izumiura (OAO/NAOJ),
M. Yoshida (Hiroshima), K. Ohta(Kyoto), and N. Kawai(Tokyo Tech.)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 161129A (Kocevski et al., GCNC 20210)
in Ks-band with a wide-field NIR camera at Okayama Astrophysical
Observatory (Japan). The camera has an effective aperture of 0.91m.

Observations started from 08:44 UT on 29th November, 93 min after
the BAT trigger, to 09:29 UT. The total exposure of 17.3 min was
successfully obtained.

In our co-add image, we found a faint source at coordinates
   R.A.(J2000) = 21:04:54.59
   DEC (J2000) = +32:08:05.2,
close to the position reported by Beardmore et al.(GCNC 20211),
and Klose & Stecklum (GCNC 20216).

We measured the source magnitude of Ks = 15.95 +/- 0.14 (Vega).
The calibration was made against 2MASS field stars.

T0+[min]    MID-UT     T-EXP[min]    Ks
------------------------------------------------------------
  +115       09:06       17.3         15.95 +/- 0.14 (Vega)
------------------------------------------------------------
T0+ : Elapsed time after the burst [min]
T-EXP: Total Exposure time [min]


GRB_name: GRB161129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20224
SUBJECT: GRB 161129A: ISON/UAFO optical observations
DATE:    16/12/01 09:40:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),  E. Chornaya (UAFO, ISON), A. Cochergin (UAFO), I. Molotov 
(KIAM), A. Pozanenko (IKI) report on behalf of  larger GRB  follow-up 
collaboration:

We observed the field of  GRB 161129A  (Kocevski et al., GCN 20210) with 
SANTEL-650 (0.65m)  telescope  of UAFO/ISON-Ussuriysk observatory. We 
obtained several unfiltered images starting on  November 29 (UT) 11:47:34. 
We detected  optical afterglow (Mazaeva et al. GCN 20215; Klose et al. GCN 
20216; Kuin et al. GCN 20217). Preliminary photometry of a combined image is 
following

Date             UT start      t-T0        Filter  Exp.     OT     Err.  UL
                                       (mid, days)         (s)

2016-11-29 10:46:15  0.16055  CR      27*60 19.90  0.08  22.5
2016-11-29 11:19:35  0.18449  CR      30*60 19.95  0.09  22.5


Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id    R2
1221-0612083 17.30
1221-0612140 19.02


GRB_name: GRB161129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20226
SUBJECT: GRB 161129A: Mondy optical observations
DATE:    16/12/01 17:04:15 GMT
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 161129A  (Kocevski et al., GCN 20210) with 
  AZT-33IK telescope of Sayan observatory (Mondy) starting on November, 
30 (UT) 11:19:53. We obtained several images in R-filter.
We detected  a source coinsiding with optical afterglow (Mazaeva et al. 
GCN 20215; Klose et al. GCN 20216; Kuin et al. GCN 20217; Kuroda et al. 
GCN 20218; Yanagisawa et al. GCN 20223). Preliminary photometry of a 
combined image is following

Date       UT start   t-T0    Filter  Exp.     OT     Err.  UL
                      (mid, days)      (s)

2016-11-30 11:19:53  1.19324  R      29*120    21.60  0.17  22.8

Photometry is based on nearby USNO-B1.0 stars
USNO-B.1_id    R2
1221-0612083 17.30
1221-0612140 19.02


GRB_name: GRB161202A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20227
SUBJECT: GRB 161202A: Swift detection of a burst
DATE:    16/12/02 23:29:05 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. Sbarufatti (INAF-OAB/PSU), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), S. B. Cenko (GSFC), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC) and M. H. Siegel (PSU) report on behalf of
the Swift Team:

At 23:12:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161202A (trigger=725036).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 356.895, +19.640, which is 
   RA(J2000)  =  23h 47m 35s
   Dec(J2000) = +19d 38' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows many peaks
with a total duration of about 70 sec.  The peak count rate
was ~10,000 counts/sec (15-350 keV), at ~7 sec after the trigger. 

The XRT began observing the field at 23:14:06.7 UT, 74.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
356.9031, 19.6477 which is equivalent to:
   RA(J2000)  = 23h 47m 36.74s
   Dec(J2000) = +19d 38' 51.7"
with an uncertainty of 2.4 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (6.00 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 9.9
(+6.04/-4.79) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 2.18e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 82 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 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
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
0.09. 

Burst Advocate for this burst is B. Sbarufatti (boris.sbarufatti 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.)


GRB_name: GRB161202A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20228
SUBJECT: GRB 161202A: Enhanced Swift-XRT position
DATE:    16/12/03 06:58:32 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 4140 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 161202A, 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 = 356.90269, +19.64648 which is equivalent
to:

RA (J2000): 23h 47m 36.65s
Dec (J2000): +19d 38' 47.3"

with an uncertainty of 1.6 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.


GRB_name: GRB161202A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20229
SUBJECT: GRB 161202A: Fermi-LAT detection
DATE:    16/12/03 09:38:30 GMT
FROM:    Giacomo Vianello at SLAC  <giacomov@slac.stanford.edu>

G.Vianello (Stanford), F.Longo (University and INFN, Trieste)

report on behalf of the Fermi-LAT team:


On December, 02, 2016 Fermi-LAT detected high-energy emission from GRB
161202A, which was also detected by Swift (GCN 20227).

The best LAT on-ground location is found to be

RA, Dec = 356.95, 19.49 (J2000)

with an error radius of 0.13 deg (90 % containment, statistical error
only), which is fully compatible with the enhanced Swift/XRT position
reported in GCN 20228.

This was outside the field of view of the LAT at the time of the
trigger t0 =  23:12:52.7. The location of the GRB was observed however
between t0 + 1680 s and t0 + 3500 s. During this time interval, the
data from the Fermi-LAT show a significant increase in the event rate
correlated with the trigger with high significance.

5 photons were detected above 100 MeV. The highest-energy photon is a
4 GeV event which is observed 2000 seconds after the GBM trigger.

The Fermi-LAT point of contact for this burst is Giacomo Vianello
(giacomov@stanford.edu).

The Fermi-LAT is a pair conversion telescope designed to cover the
energy band from 20 MeV to greater than 300 GeV. It is the product of
an international collaboration between NASA and DOE in the U.S. and
many scientific institutions across France, Italy, Japan and Sweden.


GRB_name: GRB161202A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20230
SUBJECT: GRB 161202A: MITSuME Okayama upper limits
DATE:    16/12/03 16:14:06 GMT
FROM:    Daisuke Kuroda at OAO/NAOJ  <dikuroda@oao.nao.ac.jp>

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 161202A (Sbarufatti et al., GCNC 20227)
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 2016-12-03 09:13:55 UT (~10.0 h after
the burst). We did not find any new point source within the
enhanced XRT circle (Evans et al., GCNC 20228) 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
-----------------------------------------------------
0.53482    12:03:00   11580.0   >20.6  >20.2  >19.8
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]


GRB_name: GRB161202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20231
SUBJECT: GRB 161202A: Swift-XRT refined Analysis
DATE:    16/12/03 16:46:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), T.G.R. Roegiers (PSU), S.L. Gibson (U. Leicester),
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA) and B. Sbarufatti
report on behalf of the Swift-XRT team:

We have analysed 8.5 ks of XRT data for GRB 161202A (Sbarufatti et al.
GCN Circ. 20227), from 66 s to 52.1 ks after the  BAT trigger. The data
comprise 160 s in Windowed Timing (WT) mode (the first 5 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 Evans et
al. (GCN Circ. 20228).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.53 (+0.41, -0.24). At T+217 s  the decay
flattens to an alpha of 0.83 (+/-0.09) before breaking again at T+8090
s to a final decay with index alpha=1.44 (+0.35, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.79 (+0.18, -0.17). The
best-fitting absorption column is  9.4 (+1.9, -1.7) x 10^21 cm^-2, in
excess of the Galactic value of 6.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.79 (+0.24, -0.23)
and a best-fitting absorption column of 1.39 (+0.22, -0.20) x 10^22
cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.7 x 10^-11 (1.7 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.39 (+0.22, -0.20) x 10^22 cm^-2
Galactic foreground: 6.0 x 10^20 cm^-2
Excess significance: 11.1 sigma
Photon index:      2.79 (+0.24, -0.23)

If the light curve continues to decay with a power-law decay index of
1.44, the count rate at T+24 hours will be 7.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.7 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00725036.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB161202A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20232
SUBJECT: GRB 161202A: Swift/UVOT Upper Limits
DATE:    16/12/03 19:45:55 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. H. Siegel (PSU) and B. Sbarufatti (INAF-OAB/PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 161202A
83 s after the BAT trigger (Sbarufatti et al., GCN Circ. 20227).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 20228)
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) exposure and subsequent exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)         Mag

white_FC            83          232          147         >21.2
white               83         4066          344         >21.5
v                 4277         4477          197         >19.4
b                 3661        11907          862         >20.8
u                  295        10303         1027         >20.5
w1                4688         6144          217         >19.6
w2                4071         4271          197         >19.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.09 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB161202A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20233
SUBJECT: GRB 161202A: Swift-BAT refined analysis
DATE:    16/12/04 02:10:37 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

J. R. Cummings (CPI), S. D. Barthelmy (GSFC),
N. Gehrels (GSFC), H. A. Krimm (NSF/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (INAF-OAB/PSU), 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 161202A (trigger #725036)
(Sbarufatti, et al., GCN Circ. 20227).  The BAT ground-calculated position is
RA, Dec = 356.904, 19.652 deg which is
  RA(J2000)  =  23h 47m 36.9s
  Dec(J2000) = +19d 39' 06.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 86%.

The first peaks of the burst occurred before it came into the BAT field of view
at ~T-67 s. The mask-weighted light curve shows more than ten pulses that
last till ~T+80 s.

The time-averaged spectrum from T-63.41 to T+65.79 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.55 +- 0.05.  The fluence in the 15-150 keV band is 8.6 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.11 sec in the 15-150 keV band
is 5.9 +- 0.3 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/725036/BA/


GRB_name: GRB161202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20234
SUBJECT: GRB 161202A: RATIR Optical and NIR Observations
DATE:    16/12/04 17:03:08 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer
(UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB),
Antonino Cucchiara (UVI), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz
(UCSC), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±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 161202A (Sbarufatti, et al., GCN 20227;
Vianello & Longo, GCN 20229) with the Reionization and Transients
Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson
Telescope at the Observatorio AstronÃ³mico Nacional on Sierra San Pedro
MÃ¡rtir from 2016/12 4.08 to 2016/12 4.31 UTC (26.70 to 32.11 hours after
the BAT trigger), obtaining a total of 3.34 hours exposure in the r and i
bands and 1.45 hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle (Burrows, et al., GCN 20231)
in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
upper limits (3-sigma):

   r    > 24.0
   i    > 23.9
   Z    > 23.1
   Y    > 22.8
   J    > 22.4
   H    > 22.0

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161202A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20235
SUBJECT: GRB 161202A: Astrosat CZTI detection
DATE:    16/12/05 07:58:12 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

V. Sharma, V. Bhalerao and D. Bhattacharya (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed clear detection of a long duration GRB161202A (Swift detection: B. Sbarufatti et al., GCN Circ. 20227) 
in the 40-200 keV energy range. The light curve shows a multiple peak structure with main peak at 23:11:50 UT, 62 secs before the Swift BAT 
trigger(consistent with GCN 20233). The measured peak count rate is 230.75 counts/sec above the background in combined data of four quadrants, 
with a total of 1432.98 counts. The local mean background count rate was 345.25 counts/sec. Using cumulative rates, we measure a T90 of 75.25 
sec.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium
of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated 
the project.


GRB_name: GRB161129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20236
SUBJECT: GRB 161129A: POLAR Detection
DATE:    16/12/05 14:22:18 GMT
FROM:    Shaolin Xiong at IHEP  <xiongsl@ihep.ac.cn>

J. C. Sun (IHEP), M. R. Kole (DPNC/UniGe), Y. H. Wang (IHEP),

S. L. Xiong (IHEP),Z. H. Li (IHEP),H. C. Li (IHEP),

Y. Zhao (IHEP), T. Batsch(NCBJ),T. Bernasconi (ISDC/UniGe),

  F. Cadoux (DPNC/UniGe), Y. W. Dong (IHEP),M. Z. Feng

(IHEP), M. Y. Ge (IHEP), W.Hajdas (PSI),Y. Huang (IHEP),

Karol Jedrzejczak (NCBJ), F. J. Lu (IHEP), R. Marcinkowski

(PSI), M. Pohl (DPNC/UniGe),N. Produit (ISDC/UniGe),

A. Rutczynska (NCBJ), D. Rybka (NCBJ),L. M. Song (IHEP),

J. Szabelski (NCBJ), X. Wen (IHEP), B. B. Wu (IHEP),X. Wu

(DPNC/UniGe), H. L. Xiao (PSI), M. Xu (IHEP), J. Zhang

(IHEP),L. Y. Zhang (IHEP), P. Zhang (PSI), S. N. Zhang

(IHEP),Y. J. Zhang (IHEP), A. Zwolinska (NCBJ)

report on behalf of the POLAR team:

At 2016-11-29T07:11:40.00 UT(T0), during a routine

on-ground search of data, POLAR detected the GRB 161129A,

which was also observed by the Swift/BAT (trigger

#724438), Fermi/GBM (trigger 502096303/161129300), and

Astrosat/CZTI (V. Sharma et al., GCN Circ. 20214). The

detection of this GRB happened on the tail of a big Solar Flare.

The POLAR light curve consists of multiple peaks

with a duration (T90) of 41.5 s measured from T0+3.75 s.

The 500-ms peak flux, measured from T0+27.25 s, is 705.7

cnts/sec. The above measurements are in the preliminary

calculated energy range of about 80 â€“ 500 keV.

LC_URL:

http://www.isdc.unige.ch/polar/lc/161129A/lcr.png

The incident angle at T0 in POLAR detector coordinate is:

theta:  42.6   [deg]

phi:    52.3   [deg]

These direction is computed using the best location from

the Swift/BAT, which is (J2000):

RA:   316.221  [deg]

Dec:  32.137   [deg]

Err:  1.8      [arcmin]

The distribution of the GRB signal among its 25 detector

modules is also consistent with this incident geometry.

Preliminary calculations of the MDP show that a

polarimetric measurement of this burst can be attempted.


The analysis results presented above are preliminary. The

calibration work is ongoing.


POLAR is a dedicated Gamma-Ray Burst polarimeter which was

launchedon-board the Chinese space laboratory Tiangong-2

(TG-2) on Sep 15, 2016.The energy detection range of POLAR

is ~ 50-500 keV.More information about POLAR can be found

at _http://polar.ihep.ac.cn/en/_.


GRB_name: GRB161202A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20238
SUBJECT: Konus-Wind observation of GRB 161202A
DATE:    16/12/06 16:44:29 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A.Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 161202A
(Swift-BAT detection and observation: Sbarufatti et al.,
GCN Circ. 20227, Cummings et al., GCN Circ. 20233;
Fermi-LAT detection: Vianello & Longo, GCN Circ. 20229)
triggered Konus-Wind at T0=83508.822 s UT (23:11:48.822).

The burst light curve shows a multipeaked structure
started at ~T0-57.1 s with a total duration of ~181.0 s.
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161202_T83508/

As observed by Konus-Wind, the burst
had a fluence of 2.90(-0.40,+0.73)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.920 s,
of 3.03(-0.80,+0.80)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+139.520 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.43(-0.25,+0.30)
and Ep = 222(-63,+201) keV (chi2 = 65/62 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high-energy photon index: beta < -1.9
(chi2 = 65/61 dof)

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+8.448 s)
is best fit in the 20 keV - 2 MeV range
by the power law with exponential cutoff model:
with  alpha = -0.67(-0.21,+0.24)
and Ep = 203(-20,+26) keV (chi2 = 76/62 dof).
Fitting by the GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high-energy photon index: beta < -2.5
(chi2 = 76/61 dof)

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB161206A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20239
SUBJECT: GRB 161206A: Fermi GBM detection
DATE:    16/12/06 17:33:13 GMT
FROM:    Matthew Stanbro at UAH/Fermi  <mcs0001@uah.edu>

M. Stanbro (UAH) and E. Bissaldi (Politecnico & INFN Bari)
report on behalf of the Fermi GBM Team:

"At 01:32:28.08 UT on 06 December 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161206A (trigger 502680752/161206064).
The on-ground calculated location, using the GBM trigger
data, is RA = 0.94, DEC = -34.02 (J2000 degrees),
with an uncertainty of 1 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error [Connaughton et al. 2015, ApJS, 216, 32]).

The angle from the Fermi LAT boresight at the GBM trigger time is 63
degrees.

The GBM light curve shows multiple peaks
with a duration (T90) of about 34 s (50-300 keV).
The time-averaged spectrum from T0-9 s to T0+25 s is
best fit by a Band function with Epeak = 309 +/- 15 keV,
alpha = -0.85 +/- 0.02, and beta = -2.11 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(3.92 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+9.6 s in the 10-1000 keV band
is 13.5 +/- 0.3 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB161203A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20240
SUBJECT: GRB 161203A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/12/07 02:58:46 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Asaoka (Waseda U), A. Yoshida, T. Sakamoto, Y. Kawakubo,
M. Moriyama, Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA),
I. Takahashi (IPMU), S. Ozawa, S. Torii (Waseda U), Y. Shimizu,
T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 161203A (Konus-Wind trigger time on 18:41:06.318;
INTEGRAL-SPI/ACS trigger #7641) triggered the CALET Gamma-ray Burst
Monitor (CGBM) at 18:41:07.71 on 3 December 2016.  The burst signal was
seen by all CGBM instruments.  Because of a problem in one of the ground
alert processing script, the GCN notice was not distributed automatically
for this event.

The light curve of the SGM shows at least two overlapping peaks.  The first
peak starts at T-1 sec, peaks at T+0.5 sec and ends at T+2 sec.  The second
peak, which is the brightest peak, starts at T+2 sec, peaks at T+3.5 sec and
ends at T+6 sec.  The T90 duration measured by the SGM data is
5.4 +- 0.8 sec (40-1000 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1164825510/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB161203A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20241
SUBJECT: GRB 161203A: Astrosat CZTI (Veto) detection
DATE:    16/12/07 13:29:30 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

V. Sharma, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed clear detection of GRB161203A (CALET detection: T. Sakamoto et al., GCN Circ. 20240) in the 40-200 keV 
energy range. The light curve shows a single peak structure with main peak at 18:41:10.32 UT, ~3 secs after the CALET trigger at 18:41:07.71 
UT. The measured peak count rate is 334.36 counts/sec above the background in combined data of four quadrants, with a total of 942.45 counts. 
The local mean background count rate was 322.63 counts/sec. Using cumulative rates, we measure a T90 of 8.6 secs.

CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium
of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated 
the project.


GRB_name: GRB161129A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20242
SUBJECT: GRB 161129A: KWFC z-band photometry
DATE:    16/12/08 09:21:59 GMT
FROM:    Tomoki Morokuma at U of Tokyo  <tmorokuma@ioa.s.u-tokyo.ac.jp>

Tomoki Morokuma and Yuki Sarugaku (Univ. of Tokyo) report on behalf 
ofã€€the OISTER collaboration:

We observed the field of GRB 161129A (Kocevski et al. GCN 20210) 
withã€€the 1.05-m Schmidt telescope and KWFC (Sako et al. 2012, Proc. 
SPIEã€€8446, 84466L) at Kiso Observatory in Japan. The observations were 
madeã€€in z-band at 2016-11-29 08:15-08:36 (UT; about 1 hour after the 
burst). The flux is calibrated with z-band imaging data for a nearby 
SDSS field taken at almost the same airmass as that of the GRB field.

We do not detect any new source within the XRT error circle or at the 
position with Swift/UVOT and other telescopes' detections (e.g., Kuin et 
al. GCN 20217) and the upper limits are as follows.

# ------------------------------------------------
# MID-MJD    MID-UT   t_exp  z_lim
# ------------------------------------------------
57721.3442  08:15:36   60.0   16.9
57721.3477  08:20:44  120.0   17.7
57721.3513  08:25:50  180.0   18.3
57721.3542  08:30:08  180.0   18.6
57721.3573  08:34:25  180.0   18.7
# ------------------------------------------------
MID-MJD [day] : MJD in the middle of exposure
MID-UT        : UT in the middle of exposure
t_exp [sec]   : Exposure time
z_lim         : 5-sigma limiting magnitude (AB)


GRB_name: GRB161203A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20243
SUBJECT: GRB 161203A: POLAR Detection
DATE:    16/12/08 15:21:23 GMT
FROM:    Merlin Kole at U of GenevaPOLAR  <merlin.kole@unige.ch>

M. Kole (DPNC/UniGe), N. Produit (ISDC/UniGe),  T. Bernasconi (ISDC/UniGe),
J. C. Sun (IHEP), Y. H. Wang (IHEP), S. L. Xiong (IHEP), Z. H. Li (IHEP),
H. C. Li (IHEP), Y. Zhao (IHEP), T. Batsch(NCBJ), F. Cadoux (DPNC/UniGe),
Y. W. Dong (IHEP), M. Z. Feng (IHEP), M. Y. Ge (IHEP), W. Hajdas (PSI),
Y. Huang (IHEP), Karol Jedrzejczak (NCBJ), F. J. Lu (IHEP), R. Marcinkowski
(PSI), M. Pohl (DPNC/UniGe), A. Rutczynska (NCBJ), D. Rybka (NCBJ),
L. M. Song (IHEP), J. Szabelski (NCBJ), X. Wen (IHEP), B. B. Wu (IHEP),
X. Wu (DPNC/UniGe), H. L. Xiao (PSI), M. Xu (IHEP), J. Zhang
(IHEP), L. Y. Zhang (IHEP), P. Zhang (PSI), S. N. Zhang
(IHEP), Y. J. Zhang (IHEP), A. Zwolinska (NCBJ)
report for he POLAR team:

During a routine on-ground search of data POLAR detected the GRB 161203A,

at 2016-12-03T18:41:07.75 UT(T0). This GRB was also observed by Konus-Wind,

INTEGRAL SPI/ACS (trigger #7641), CALET (GCN #20240) and Astrosat CZTI (GCN #20241).

The POLAR light curve consists two peaks with a total duration (T90)

of 4.75 +- 0.25 s measured from T0-0.5 s. The 250-ms peak flux of the

first peak, measured at T0+0.5 s is 1509 cnts/sec. The second stronger

peak measured at T0+3.0 s has a peak flux of 2821 cnts/sec. The

above measurements are in the preliminary calculated energy range

of about 80 - 500 keV.

LC_URL: http://www.isdc.unige.ch/polar/lc/161203A/lcr.png


The analysis results presented above are preliminary as the
instrument calibration is still ongoing.

Preliminary calculations of the MDP show that a
polarimetric measurement of this burst can be attempted.

POLAR is a dedicated Gamma-Ray Burst polarimeter which was
launched on-board the Chinese space laboratory Tiangong-2
(TG-2) on Sep 15, 2016. The energy detection range of POLAR
is ~ 50-500 keV. More information about POLAR can be found
at http://isdc.unige.ch/polar/

This message is quotable in publications.


GRB_name: GRB161129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20244
SUBJECT: GRB 161129A: NOT optical observations and candidate host galaxy
DATE:    16/12/09 14:58:08 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

K. E. Heintz (Univ. Iceland and DARK/NBI), D. Malesani (DARK/NBI and DTU 
Space), Z. Cano (IAA-CSIC), A. De Ugarte Postigo (IAA-CSIC and 
DARK/NBI), G. Fedorets (NOT and Univ. Helsinki), R. Tronsgaard Rasmussen 
(NOT), A. A. Djupvik (NOT), I. R. Losada (NOT and Stockholm Univ.), I. 
Svardh (NOT), J. Clasen (NOT), S. Armas Perez (NOT), report on behalf of 
a larger collaboration:

We observed the optical counterpart of GRB 161129A (Kocevski et al., GCN 
20210; Mazaeva et al., GCN 20215) with the Nordic Optical Telescope 
(NOT) equipped with the AlFOSC imager. Observations were carried out in 
the R band (3x200 s), with a mid time 2016 Dec 4.83 UT (5.6 days after 
the GRB). Observing conditions were good with a seeing of 0.8".

Two objects are detected within the XRT error region (Beardmore et al. 
2016, GCN Circ. 20211), at the following coordinates (calibrated against 
the USNO-B1.0 catalog):

source A: RA = 21:04:54.69, Dec = +32:08:04.7
source B: RA = 21:04:54.63, Dec = +32:08:05.9

A finding chart is posted at this URL: 
http://www.astro.ku.dk/~malesani/GRB/161129A/GRB161129A.png

Given their small separation (1.4"), these objects may be blended in 
images with coarser spatial resolution. Source A (with a magnitude R = 
21.6) is consistent in flux and position with the faint smudge visible 
in the DSS red, previously noted by Mazaeva et al. (GCN 20215) and Klose 
& Stecklum (GCN 20216).

Source B is extended, and is consistent with the position reported for 
the optical afterglow by Kuin et al. (GCN 20217) and Kuroda et al. (GCN 
20218). We propose that source B is (dominated by) the host galaxy of 
GRB 161129A. We further note that the cumulative magnitude of the 
complex (objects A+B) is R ~ 21.2, which is significantly fainter than 
previous reports (e.g. Kuroda et al., GCN 20218; Mazaeva et al., GCN 
20224), thus firmly establishing the presence of a fading optical 
afterglow for GRB 161129A. Photometry was computed against the values of 
the two USNO-B1.0 stars as listed by Mazaeva et al. (GCN 20215).


GRB_name: GRB161129A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20245
SUBJECT: GRB 161129A: GTC redshift of the likely host galaxy
DATE:    16/12/09 15:31:37 GMT
FROM:    Zach Cano at U of Iceland  <zewcano@gmail.com>

â€‹Z. Cano (IAA-CSIC), D. Malesani (DARK/NBI and DTU Space), A. de Ugarte
Postigo (IAA-CSIC, DARK/NBI), L. Izzo, C. C. Thoene (IAA-CSIC) and N.
Castro-Rodriguez (GRANTECAN/IAC/Universidad de La Laguna) report:

We observed the field of GRB 161129A (Kocevski et al., GCN Circ. 20210)
with OSIRIS on the 10.4 m GTC telescope on La Palma (Spain).  The
observations started at 19:46:40.9 UT on 05-December-2016 (6.52 days after
the burst), which consisted of 4 x 1200 s spectra using grism R1000B, which
covers the wavelength range 3700-7800 angstroms, with a resolution of
R~1000.

Within the enhanced XRT error region (Beardmore et al. 2016, GCN Circ.
20211) we note the presence of sources A & B detected by Heintz et al. (GCN
Circ. 20244).  The spectrum of the extended object (source B) shows a
continuum with a strong emission line that we attribute to the [OII]
3727/3729 doublet at z=0.645, as well as weaker emission lines consistent
with being H-gamma and H-delta at the same redshift. We propose this
star-forming galaxy to be the host of GRB 161129A. The spectrum of source A
displays absorption features of Ca II K and H, Mg I and MgH at z~0,
confirming it is a foreground star and not related to GRB 161129A.


GRB_name: GRB161207A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20246
SUBJECT: GRB 161207A: CALET Gamma-Ray Burst Monitor detection
DATE:    16/12/10 04:54:09 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

S. Ozawa (Waseda U), A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama,
Y. Yamada (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU),
Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena)
and the CALET collaboration:

The long-duration GRB 161207A (Fermi-GBM trigger #502836132) triggered
the CALET Gamma-ray Burst Monitor (CGBM) at 20:43:00.39 on 7 December 2016.
The burst signal was seen by all CGBM instruments.

The light curve of the SGM shows several overlapping peaks.  The entire
burst episode starts at T-20 sec, peaks at T+5 sec and ends at T+30 sec.
The T90 duration measured by the SGM data is 32.8 +- 1.7 sec (40-1000 keV).

The light curve is available at

http://cgbm.calet.jp/cgbm_trigger/flight/1165178415/

The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.


GRB_name: GRB161214A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20251
SUBJECT: GRB 161214A: A long GRB detected by INTEGRAL
DATE:    16/12/14 06:25:13 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro@iasf-milano.inaf.it>

S.Mereghetti (IASF-Milano), D.Gotz (CEA, Saclay), C.Ferrigno, E.Bozzo, 
J.G.Victor (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the 
IBAS Localization Team report:

a long gamma ray burst has been detected by IBAS in the IBIS/ISGRI data at 
4:46:07 UT of 2016 December 14

The refined coordinates (J2000) are:
R.A.= 190.757 deg
DEC.=  6.853 deg
with an uncertainty of  2.5   arcmin (90% c.l.).

The burst had an initial peak lasting about 7 s with peak flux of about 
0.3 counts/cm2/s (20-200 keV, 1-s integration time) and fluence of 1.5e-7 
erg/cmq, followed by fainter emission lasting about one minute.

The relatively low significance of the trigger was due to the fact that 
one of the eight modules composing the ISGRI detector was temporarily off 
during the burst.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html

[GCN OPS NOTE(14dec16): Per author's request, the date in the first
sentence was corrected from Dec 12 to Dec 14.]


GRB_name: GRB161214A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20252
SUBJECT: GRB 161214A: fading optical afterglow candidate with the LT
DATE:    16/12/14 07:46:37 GMT
FROM:    Cristiano Guidorzi at Ferrara U,Italy  <guidorzi@fe.infn.it>

C. Guidorzi (U. Ferrara), C.G. Mundell (Bath), S. Kobayashi, I.A. Steele 
(LJMU), A. Gomboc (U. Nova Gorica) on behalf of a large collaboration 
report:

The 2-m Liverpool Telescope automatically began observing INTEGRAL GRB 
161214A (Mereghetti et al., GCN 20251) in the SDSS r. Within the 
INTEGRAL error circle we find an uncatalogued fading object at the 
following position:

RA(J2000)=  12:43:00.36
Dec(J2000)= +06:51:50.1

with a 1 arcsec error radius and magnitudes of r=19.66 +- 0.07 at 35 
minutes, and r=19.95 +- 0.07 at 61 minutes post GRB trigger as 
calibrated against nearby SDSS stars.


GRB_name: GRB161214A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20254
SUBJECT: GRB 161214A: TAROT Calern observatory optical observations
DATE:    16/12/14 12:17:29 GMT
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 161214A detected by INTEGRAL
(trigger 7644) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 24.6s after the GRB trigger
(17.7s after the notice). The elevation of the field increased from
45 degrees above horizon and weather conditions
were good until the end of the night.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).

We detected the couterpart mentioned by Guidorzi
et al. (GCNC 20252). The optical afterglow reached flux peak
at t0+240s (+/- 15s). The early light curve:

t0 +  25 s to t0 +   85s  : Rlim = 16.6 (trailed image)
t0 +  99 s to t0 +  211s  : Rlim = 17.1
t0 + 222 s to t0 +  293s  : R    = 16.9 +/- 0.3
t0 + 304 s to t0 +  899s  : R    = 17.4 +/- 0.3
t0 + 910 s to t0 + 2180s  : R    = 18.7 +/- 0.4

Magnitudes were estimated with the nearby star
NOMAD-1 0968-0244492 ra=190.7246097 dec=+06.8741839
R=15.04.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=296.86 lat=+69.60
and the galactic extinction in R band is about 0.1 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.


GRB_name: GRB161214A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20255
SUBJECT: GRB 161214A: GROND afterglow observations
DATE:    16/12/14 12:45:02 GMT
FROM:    Thomas Kruehler at MPE Garching  <kruehler@mpe.mpg.de>

T. Kruehler and J. Greiner (both MPE Garching) report on behalf
of the GROND team:

We observed the field of GRB 161214A (INTEGRAL trigger 7644;
Mereghetti et al., GCN #20251) simultaneously in g'r'i'z'JHK with
GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG
telescope at the ESO La Silla Observatory (Chile).

Observations started at 08:39 UT on 2016-12-14, 3.9 hr after the GRB
trigger. They were performed at an average seeing of 1".3, and at an
average airmass of 1.8.

Based on combined images with 9.7 min of total exposures in g'r'i'z'
and 10.0 min in JHK at a mid-time of 08:45 UT on 2016-12-14,
we derive the following preliminary magnitudes (all in AB system)
for the optical/NIR afterglow (Guidorzi et al., GCN 20252).

g' = 21.7 +- 0.2 mag
r' = 21.0 +- 0.1 mag
i' = 20.6 +- 0.1 mag
z' = 20.4 +- 0.1 mag
J = 20.2 +- 0.2 mag
H = 20.2 +- 0.3 mag

Given magnitudes are calibrated against SDSS/2MASS field stars and
are not corrected for the expected Galactic foreground extinction
corresponding to a reddening of E_(B-V) = 0.02 mag in the direction of
the burst (Schlafly & Finkbeiner 2011).


GRB_name: GRB161214B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20257
SUBJECT: GRB 161214B: Swift detection of a burst
DATE:    16/12/14 17:32:35 GMT
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.)


GRB_name: GRB161214A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20258
SUBJECT: GRB 161214A: NOT observations of the afterglow
DATE:    16/12/14 17:47:41 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DARK/NBI and DTU Space), D. Xu (NAOC/CAS), J. Telting 
(NOT), E. Gafton, report on behalf of a larger collaboration:

We observed the field of the INTEGRAL GRB 161214A (Mereghetti et al., 
GCN 20251) with the Nordic Optical Telescope (NOT) equipped with the 
AlFOSC imaging camera. Observations were carried out at the very end of 
the night, starting about 40 min after the morning twilight, and only a 
single 200 s exposure taken with the SDSS r filter was useful.

The optical afterglow (Guidorzi et al., GCN 20252; Klotz et al., GCN 
20254; Kruehler & Greiner, GCN 20255) is faintly detected in our images. 
By comparison with nearby SDSS stars, we measure for the afterglow r = 
20.9 +- 0.3 (AB) at a mean epoch 2016 Dec 14.303, that is 2.50 hr after 
the GRB.


GRB_name: GRB161214B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20259
SUBJECT: GRB 161214B: Prompt enhanced Swift-XRT position
DATE:    16/12/14 17:51:22 GMT
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.


GRB_name: GRB161214B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20260
SUBJECT: GRB 161214B: NOT optical observations, possible counterpart
DATE:    16/12/14 21:15:24 GMT
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".]


GRB_name: GRB161214B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20261
SUBJECT: GRB 161214B: Swift/UVOT Observations
DATE:    16/12/14 21:55:35 GMT
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).


GRB_name: GRB161214B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20262
SUBJECT: GRB 161214B: Chante-perdrix observatory optical observations
DATE:    16/12/14 23:41:41 GMT
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.


GRB_name: GRB161214B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20263
SUBJECT: GRB 161214B: TAROT Calern observatory optical observations
DATE:    16/12/14 23:43:16 GMT
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.


GRB_name: GRB161214B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20264
SUBJECT: GRB 161214B: Enhanced Swift-XRT position
DATE:    16/12/15 00:12:53 GMT
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.


GRB_name: GRB161214B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20265
SUBJECT: GRB 161214B: Swift-XRT refined Analysis
DATE:    16/12/15 05:10:40 GMT
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.]


GRB_name: GRB161214B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20266
SUBJECT: GRB 161214B: RATIR Optical and Near-Infrared Observations
DATE:    16/12/15 05:21:07 GMT
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), JosÃ© A. de Diego (UNAM), Leonid Georgiev (UNAM), JesÃºs GonzÃ¡lez
(UNAM), Carlos RomÃ¡n-ZÃºÃ±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
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡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 AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB161214B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20268
SUBJECT: GRB 161214B: Swift/UVOT Afterglow Confirmation
DATE:    16/12/15 14:57:31 GMT
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).


GRB_name: GRB161214B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20270
SUBJECT: GRB 161214B: Swift-BAT refined analysis
DATE:    16/12/15 17:35:50 GMT
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' 30.7â€ 
 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. 


GRB_name: GRB161210A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20271
SUBJECT: GRB 161210A: POLAR observation
DATE:    16/12/16 06:21:33 GMT
FROM:    Zhengheng Li at POLAR  <lizhengheng@ihep.ac.cn>

Z. H. Li (IHEP), Y. H. Wang (IHEP), Y. Zhao (IHEP), M. Z. Feng(IHEP),
J. C. Sun (IHEP), H. C. Li (IHEP), S. L. Xiong (IHEP), T. Batsch(NCBJ),
T. Bernasconi (ISDC/UniGe), F. Cadoux (DPNC/UniGe), Y. W. Dong (IHEP),
M. Y. Ge (IHEP),W.Hajdas (PSI),Y. Huang (IHEP), Karol Jedrzejczak (NCBJ),
M. R. Kole (DPNC/UniGe), F. J. Lu (IHEP), R. Marcinkowski(PSI), 
M. Pohl (DPNC/UniGe), N. Produit (ISDC/UniGe),A. Rutczynska (NCBJ),
D. Rybka (NCBJ),L. M. Song (IHEP), J. Szabelski (NCBJ), X. Wen (IHEP),
 B. B. Wu (IHEP),X. Wu (DPNC/UniGe), H. L. Xiao (PSI), M. Xu (IHEP),
J. Zhang (IHEP),L. Y. Zhang (IHEP), P. Zhang (PSI), S. N. Zhang (IHEP),
Y. J. Zhang (IHEP), A. Zwolinska (NCBJ)
report for the POLAR collaboration:

At 2016-12-10T12:33:54 UT (T0), during a routine on-ground 
search of data, POLAR detected the GRB 161210A, 
which was also detected by the Fermi/GBM (trigger 503066038/161210523).

The POLAR light curve consists of a single peak,
with a duration (T90) of 11.76 s measured from T0-0.10 s .
The 1s peak rate measured from T0+0.00 s is 199.3 cnts/s,
The total counts is about 1318 cnts.  The above measurements are
in the energy range of about 80-500 keV.

LC_URL:
http://polar.ihep.ac.cn/grb/2016/GRB161210A/lc/POLAR_lc_grb161210523.jpg

Using the best location from the Fermi/GBM, which is (J2000):
RA:      283.120   [deg]
Dec:     +63.050   [deg]
Err:     10.11     [deg]

the incident angle in POLAR coordinate at T0 is:
theta:  75.9  [deg]
phi:   -23.6  [deg]

The analysis results presented above are preliminary.

POLAR is a dedicated Gamma-Ray Burst polarimeter (50-500 keV) on-board 
the Chinese space laboratory Tiangong-2 launched on Sep 15, 2016. More
information about POLAR can be found at http://polar.ihep.ac.cn/en/
, http://isdc.unige.ch/polar/ and http://polar.psi.ch/html/


GRB_name: GRB161205A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20272
SUBJECT: GRB 161205A: POLAR observation
DATE:    16/12/16 12:30:18 GMT
FROM:    Zhao Yi at POLAR  <yizhao@ihep.ac.cn>

Y. Zhao (IHEP), M. Z. Feng(IHEP), Z. H. Li (IHEP), Y. H. Wang (IHEP),
J. C. Sun (IHEP), H. C. Li (IHEP), S. L. Xiong (IHEP), T. Batsch(NCBJ),
T. Bernasconi (ISDC/UniGe), F. Cadoux (DPNC/UniGe), Y. W. Dong (IHEP),
M. Y. Ge (IHEP),W.Hajdas (PSI),Y. Huang (IHEP), Karol Jedrzejczak (NCBJ),
M. R. Kole (DPNC/UniGe), F. J. Lu (IHEP), R. Marcinkowski(PSI), 
M. Pohl (DPNC/UniGe), N. Produit (ISDC/UniGe),A. Rutczynska (NCBJ),
D. Rybka (NCBJ),L. M. Song (IHEP), J. Szabelski (NCBJ), X. Wen (IHEP),
 B. B. Wu (IHEP),X. Wu (DPNC/UniGe), H. L. Xiao (PSI), M. Xu (IHEP),
J. Zhang (IHEP),L. Y. Zhang (IHEP), P. Zhang (PSI), S. N. Zhang (IHEP),
Y. J. Zhang (IHEP), A. Zwolinska (NCBJ)
report for the POLAR collaboration:

At 2016-12-05T13:27:18UT(T0), during a routine 
on-ground search of data, POLAR detected the GRB 161205A, 
which was also observed by the Fermi/GBM (trigger502637242/161205561).

The POLAR light curve consists of multiple peaks
with a duration (T90) of 26.6s measured from T0-0.66s.
The 1s peak flux, measured from T0+7.00s, is 271.8cnts/s.
The total counts is about 1416cnts. The above measurements
are in the energy range of about 80-500 keV.

LC_URL: http://polar.ihep.ac.cn/grb/2016/GRB161205A/lc/POLAR_lc_grb161205560.jpg

Using the best location from the Fermi/GBM, which is (J2000):
RA:   318.980 [deg]
Dec:  +47.650 [deg]
Err:  5.42    [deg]

the incident angle at T0 in POLAR detector coordinate is:
theta:  63.7 [deg]
phi:    -3.7 [deg]

The analysis results presented above are preliminary.

POLAR is a dedicated Gamma-Ray Burst polarimeter (50-500 keV) on-board 
the Chinese space laboratory Tiangong-2 launched on Sep 15, 2016. More
information about POLAR can be found at http://polar.ihep.ac.cn/en/
, http://isdc.unige.ch/polar/ and http://polar.psi.ch/html/


GRB_name: GRB161207B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  20273
SUBJECT: GRB 161207B: POLAR observation
DATE:    16/12/16 12:51:22 GMT
FROM:    Feng Minzi at POLAR  <fengmz@ihep.ac.cn>

M. Z. Feng (IHEP), Y. Zhao (IHEP), Y. H. Wang (IHEP), J. C. Sun (IHEP),
Z. H. Li (IHEP), H. C. Li (IHEP), S. L. Xiong (IHEP), T. Batsch(NCBJ),
T. Bernasconi (ISDC/UniGe), F. Cadoux (DPNC/UniGe),Y. W. Dong(IHEP),
M. Y. Ge (IHEP),W.Hajdas (PSI),Y. Huang(IHEP),Karol Jedrzejczak(NCBJ),
M. R. Kole (DPNC/UniGe), F. J. Lu (IHEP),R. Marcinkowski(PSI),
M. Pohl (DPNC/UniGe),N. Produit (ISDC/UniGe),A. Rutczynska (NCBJ),
D. Rybka (NCBJ),L. M. Song (IHEP),J. Szabelski (NCBJ), X. Wen (IHEP),
B. B. Wu (IHEP),X. Wu(DPNC/UniGe), H. L. Xiao (PSI), M. Xu (IHEP),
J. Zhang(IHEP),L. Y. Zhang (IHEP), P. Zhang (PSI), S. N. Zhang(IHEP),
Y. J. Zhang (IHEP), A. Zwolinska (NCBJ)
report for the POLAR collaboration:

At 2016-12-07T05:22:44 UT (T0), during a routine on-ground 
search of data, POLAR detected the GRB 161207B, 
which was also detected by the Fermi/GBM (trigger 502780971/161207224).

The POLAR light curve consists of a single peak,
with a duration (T90) of 12.5 s measured from T0-0.94 s .
The 1s peak rate measured from T0+4.00 s is 151.3 cnts/s,
The total counts is about 713 cnts. The above measurements are
in the energy range of about 80-500 keV.

LC_URL: 
http://polar.ihep.ac.cn/grb/2016/GRB161207B/lc/POLAR_lc_grb161207224.jpg

Using the best location from the Fermi/GBM, which is (J2000):
RA:    294.810     [deg]
Dec:    -9.930     [deg]
Err:     18.01     [deg]

the incident angle in POLAR coordinate at T0 is:
theta:  60.7  [deg]
phi:   -66.0  [deg]

The analysis results presented above are preliminary.

POLAR is a dedicated Gamma-Ray Burst polarimeter (50-500 keV) on-board
the Chinese space laboratory Tiangong-2 launched on Sep 15, 2016. More
information about POLAR can be found at http://polar.ihep.ac.cn/en/,
http://isdc.unige.ch/polar/ and http://polar.psi.ch/pub/.



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