Gamma-ray Burst 161109A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

none

Results of Observations

GCN Circular #20155
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.
GCN Circular #20156
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."
GCN Circular #20158
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.

GCN Notice

TITLE:          GCN/GRB_COUNTERPART POSITION NOTICE
NOTICE_DATE:    Thu 10 Nov 16 01:11:40 UT 
NOTICE_TYPE:    Other
TRIGGER_NUM:    20711
CNTRPART_RA:    157.9039d {+10h 31m 36.9s} (J2000),
                158.1854d {+10h 32m 44.5s} (current),
                157.0628d {+10h 28m 15.0s} (1950)
CNTRPART_DEC:   +61.8838d {+61d 53' 01.6"} (J2000),
                +61.7968d {+61d 47' 48.3"} (current),
                +62.1410d {+62d 08' 27.5"} (1950)
CNTRPART_ERROR: 6.1 [arcsec, radius]
GRB_DATE:       17701 TJD;   314 DOY;   16/11/09
GRB_TIME:       63133.00 SOD {17:32:13.00} UT 
OBS_DATE:       17701 TJD;   314 DOY;   16/11/09
OBS_TIME:       63133.0 SOD {17:32:13.00} UT
OBS_DUR:        1499.4 [sec]   
INTENSITY:      4.50e-13 +/- 1.90e-13 [erg/cm2/sec]
ENERGY:         0.3-10 [keV]   
TELESCOPE:      Swift-XRT
SUBMITTER:      Phil_Evans
SUN_POSTN:      225.61d {+15h 02m 27s}  -17.21d {-17d 12' 43"} 
SUN_DIST:        95.02 [deg]   Sun_angle= 4.5 [hr] (West of Sun)
MOON_POSTN:     347.00d {+23h 08m 00s}   -6.25d {-06d 14' 48"}  
MOON_DIST:      124.07 [deg]   
MOON_ILLUM:     73 [%]
GAL_COORDS:     146.85, 48.24 [deg] galactic lon,lat of the counterpart
ECL_COORDS:     130.38, 47.62 [deg] ecliptic lon,lat of the counterpart
COMMENTS:       GRB COUNTERPART Coordinates.
COMMENTS:       We cannot confirm whether this is the GRB or serendipitous.

GCN Notice

TITLE:          GCN/GRB_COUNTERPART POSITION NOTICE
NOTICE_DATE:    Thu 10 Nov 16 02:58:30 UT
NOTICE_TYPE:    Other
TRIGGER_NUM:    20711
CNTRPART_RA:    157.9735d {+10h 31m 53.6s} (J2000),
                158.2550d {+10h 33m 01.1s} (current), 
                157.1325d {+10h 28m 31.8s} (1950)
CNTRPART_DEC:   +61.9382d {+61d 56' 17.5"} (J2000),
                +61.8511d {+61d 51' 04.0"} (current),
                +62.1955d {+62d 11' 43.8"} (1950)
CNTRPART_ERROR: 5.8 [arcsec, radius]
GRB_DATE:       17701 TJD;   314 DOY;   16/11/09
GRB_TIME:       63133.00 SOD {17:32:13.00} UT
OBS_DATE:       17701 TJD;   314 DOY;   16/11/09
OBS_TIME:       63133.0 SOD {17:32:13.00} UT
OBS_DUR:        1529.5 [sec]   
INTENSITY:      3.60e-13 +/- 1.30e-13 [erg/cm2/sec]
ENERGY:         0.3-10 [keV]
TELESCOPE:      Swift-XRT
SUBMITTER:      Phil_Evans
SUN_POSTN:      225.69d {+15h 02m 45s}  -17.23d {-17d 13' 58"}
SUN_DIST:        95.06 [deg]   Sun_angle= 4.5 [hr] (West of Sun)
MOON_POSTN:     347.99d {+23h 11m 59s}   -5.93d {-05d 55' 46"} 
MOON_DIST:      123.61 [deg]
MOON_ILLUM:     74 [%]
GAL_COORDS:     146.75, 48.23 [deg] galactic lon,lat of the counterpart
ECL_COORDS:     130.37, 47.68 [deg] ecliptic lon,lat of the counterpart
COMMENTS:       GRB COUNTERPART Coordinates.
COMMENTS:       We cannot confirm whether this is the GRB or serendipitous.

GCN Notice

TITLE:          GCN/GRB_COUNTERPART POSITION NOTICE
NOTICE_DATE:    Thu 10 Nov 16 03:03:50 UT
NOTICE_TYPE:    Other
TRIGGER_NUM:    20711
CNTRPART_RA:    158.0652d {+10h 32m 15.6s} (J2000),
                158.3457d {+10h 33m 22.9s} (current), 
                157.2272d {+10h 28m 54.5s} (1950)
CNTRPART_DEC:   +61.6754d {+61d 40' 31.4"} (J2000),
                +61.5883d {+61d 35' 17.7"} (current),
                +61.9329d {+61d 55' 58.3"} (1950)
CNTRPART_ERROR: 6.8 [arcsec, radius]
GRB_DATE:       17701 TJD;   314 DOY;   16/11/09
GRB_TIME:       63544.00 SOD {17:39:04.00} UT
OBS_DATE:       17701 TJD;   314 DOY;   16/11/09
OBS_TIME:       63544.0 SOD {17:39:04.00} UT
OBS_DUR:        1579.6 [sec]   
INTENSITY:      2.40e-13 +/- 9.00e-14 [erg/cm2/sec]
ENERGY:         0.3-10 [keV]
TELESCOPE:      Swift-XRT
SUBMITTER:      Phil_Evans
SUN_POSTN:      225.69d {+15h 02m 45s}  -17.23d {-17d 14' 01"}
SUN_DIST:        94.91 [deg]   Sun_angle= 4.5 [hr] (West of Sun)
MOON_POSTN:     348.04d {+23h 12m 10s}   -5.91d {-05d 54' 49"} 
MOON_DIST:      123.86 [deg]
MOON_ILLUM:     74 [%]
GAL_COORDS:     147.01, 48.43 [deg] galactic lon,lat of the counterpart
ECL_COORDS:     130.64, 47.49 [deg] ecliptic lon,lat of the counterpart
COMMENTS:       GRB COUNTERPART Coordinates.
COMMENTS:       We cannot confirm whether this is the GRB or serendipitous.

GCN Circular #20164
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 (J2000.0):  157.9051  =  10:31:37.24
  Dec (J2000.0): +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 (J2000.0):  157.9726  =  10:31:53.43
  Dec (J2000.0): +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 (J2000.0):  158.0653  =  10:32:15.66
  Dec (J2000.0): +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.
GCN Circular #20165
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.
GCN Circular #20169
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).
GCN Circular #20171
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.

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Jochen Greiner, last update: 12-Nov-2016 [Disclaimer]