# GCN_circulars

GRB_name: GRB191024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26067
SUBJECT: GRB 191024A: VLT/X-shooter optical observations
DATE:    19/10/24 13:48:45 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu (NAOC), J.T. Palmerio (CNRS - Obs. de Paris/GEPI), D. B. Malesani 
(DTU space), K. E. Heintz (Univ. of Iceland), N. R. Tanvir (Univ. 
Leicester), J. P. U. Fynbo (DAWN/NBI), A. J. Levan (Radboud Univ.), G. 
Pugliese (Univ. Amsterdam), C. Kouveliotou (GWU, APSIS), report on 
behalf of the Stargate collaboration:

We observed the field of GRB 191024A (Page et al., GCN 26063) using the 
ESO VLT UT2 (Kueyen) equipped with the X-shooter camera. Observations 
started at 06:14:13 UT on 2019-10-14 (i.e., 1.523 hr after the BAT 
trigger) and 3x40 s, 3x30 s , 3x60 s frames were obtained in the Sloan 
g- / r- / z- bands, respectively.

No optical source is detected in our stacked image within the enhanced 
XRT error circle (Beardmore et al., GCN 26064), down to a limiting 
magnitude of r ~ 24.3 AB mag.

However, there exist two sources just outside and south of the XRT error 
circle in all the stacked g-, r-, and z-band images. Their coordinates 
and magnitudes are as follows

S1
R.A.(J2000) = 0:40:27.360
Dec.(J2000) = -67:08:44.800
Distance from the XRT center: 2.8"
m(r) ~ 24.1 AB mag

S2
R.A.(J2000) = 00:40:27.480
Dec.(J2000) = -67:08:45.800
Distance from the XRT center: 3.6"
m(r) ~ 23.7 AB mag

Due to small FOV, the magnitudes are calculated using only one DSS-2 
reference star at R.A. (J2000) = 00:40:29.68 and Dec. (J2000) = 
-67:08:43.99 with R1=19.68.  And due to only one epoch of photometry, it 
is not clear if either of the two sources is related to the burst. 
Further observations are required to check for variability.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Trystyn Berg and Marcela Espinoza.

[GCN OPS NOTE(24oct19): Per author's request, "Marcela Espinoza"
was added to the last sentence.]


GRB_name: GRB191024A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26068
SUBJECT: GRB 191024A: Swift-XRT refined Analysis
DATE:    19/10/24 14:45:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), A. Tohuvavohu (U.
Toronto), J.A. Kennea (PSU), B. Sbarufatti (PSU), J.P. Osborne (U.
Leicester), A.P. Beardmore (U. Leicester), M.G. Bernardini (INAF-OAB)
and K.L. Page report on behalf of the Swift-XRT team:

We have analysed 6.6 ks of XRT data for GRB 191024A (Page et al. GCN
Circ. 26063), from 837 s to 31.5 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. 26064).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.87 (+0.22, -0.18).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+0.7, -0.6). The
best-fitting absorption column is  3.2 (+4.0, -2.6) x 10^21 cm^-2, in
excess of the Galactic value of 2.7 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 4.1 x 10^-11 (5.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+4.0, -2.6) x 10^21 cm^-2
Galactic foreground: 2.7 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      1.8 (+0.7, -0.6)

If the light curve continues to decay with a power-law decay index of
0.87, the count rate at T+24 hours will be 1.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.9 x
10^-14 (8.1 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/00931242.

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


GRB_name: GRB191024A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26069
SUBJECT: GRB 191024A: Afterglow Upper Limits with LCO
DATE:    19/10/24 15:13:12 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (U. of the Virgin Islands/College of Marin) report on behalf of a larger collaboration:

We observed Swift GRB 191024A (Palmer et al., GCN 26063) with the LCO 1-m Sinistro instrument at Las Cumbres, Chile site, on October 24, from 05:18 to 05:23 UT (corresponding to 0.13 to 0.22 hours from the GRB trigger time) with Bessel R filter.

We performed a series of 2x120s exposures in R-band. We do not detect any sources in the Swift 90% confidence region (Evans et al., GCN 26064).  Using the USNO-B.1 catalog as reference, we obtain the following 3-sigma upper limit:


R > 17.08

These observations were possible thanks to the USVI NASA-EPSCoR Research Infrastructure Development (RID) grant NNX16AL44A.


GRB_name: GRB191024A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26070
SUBJECT: GRB 191024A: Swift/UVOT Upper Limits
DATE:    19/10/24 16:21:03 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) 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 191024A 833 s after the BAT trigger
(Page et al., GCN Circ. 26063).
No optical afterglow consistent with the XRT position (Beardmore et al., GCN Circ. 26064) 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           833          982          147         >21.2
white              833        13531          360         >22.0
v                  989         6893          274         >19.9
b                 1087        13389         1043         >21.6
u                 1062        19531          716         >21.3
w1                1038        19072         1160         >21.1
m2                6898         7098          197         >20.2
w2                1137         1506           39         >19.7

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: GRB191024A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26071
SUBJECT: GRB 191024A: Swift-BAT refined analysis
DATE:    19/10/25 00:00:03 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
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 191024A (trigger #931242)
(Page et al., GCN Circ. 26063).  The BAT ground-calculated position is
RA, Dec = 10.129, -67.138 deg which is
   RA(J2000)  =  00h 40m 30.9s
   Dec(J2000) = -67d 08' 17.1"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.

The mask-weighted light curve shows a single-pulsed structure that starts
and peaks at ~T0, and ends at ~T+8 s. T90 (15-350 keV) is 7.08 +- 0.98 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.96 to T+7.45 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.78 +- 0.14.  The fluence in the 15-150 keV band is 4.7 +- 0.4 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T-0.31 sec in the 15-150 keV band
is 1.6 +- 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/931242/BA/


GRB_name: GRB191025A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26072
SUBJECT: Swift Trigger 931384: possible GRB 191025A
DATE:    19/10/25 03:23:10 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

A. P. Beardmore (U Leicester), J.D. Gropp (PSU), J. A. Kennea (PSU),
K. L. Page (U Leicester), B. Sbarufatti (PSU), M. H. Siegel (PSU) and
A. Tohuvavohu (Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 02:46:47 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191025A (trigger=931384).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 320.755, -48.330 which is 
   RA(J2000) = 21h 23m 01s
   Dec(J2000) = -48d 19' 46"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty). The significance is relatively low in both 
the rate and image domains. 

The XRT began observing the field at 02:48:08.9 UT, 82.0 seconds after
the BAT trigger. No source was detected in 1.5 ks of promptly
downlinked data. We are waiting for the full dataset to detect and
localise the XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 85 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 25% of  the BAT 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  BAT 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 0.03. 

Due to the low significance of the BAT trigger and the lack of immediate
counterpart detection in the XRT or UVOT, the Swift team will not be able to
confirm or deny whether this event is a GRB without further data. 

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/)


GRB_name: GRB191025A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26073
SUBJECT: Possible GRB 191025A: FRAM-Auger optical limit
DATE:    19/10/25 17:14:29 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ),
Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek,
Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza
(Institute of Physics, Prague, CZ)

report:

The 30cm robotic telescope FRAM-Auger in Malargue
(Argentina) reacted robotically to the Swift/BAT alert
of GRB191025A (Page et al., GCNC 26072), starting
with a series of 20s unfiltered images at 02:47:17 UT,
i.e. 30s post trigger.

We do not detect any new or strongly variable source at
or around the reported gamma-ray errorbox at single
frames or combined 10 x 20s exposures taken between 30s
and 585s after the initial trigger. The combined
images have a limiting magnitude r'(AB) = 19.1, as
calibrated against the APASS Catalogue.


GRB_name: GRB191023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26074
SUBJECT: GRB 191023A: MASTER optical observation
DATE:    19/10/25 17:37:47 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina,P.Balanutsa,A.Kuznetsov, V.Vladimirov, D. Vlasenko,
I.Gorbunov,D.Zimnukhov,V.Senik, T.Pogrosheva, K.Pozdnyakov,A.Chasovnikov, V.Topolev,D.Kuvshinov(Lomonosov Moscow State University, SAI,Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio AstronomicoFelixAguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova(Irkutsk State University, API),
A. Tlatov, D. Dormidontov(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University)

MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov etal.,2010,Advances in Astronomy, vol.2010, 30L)
started Fermi GRB 191023A / trigger 593536021 (GBM team GCN 26060, BALROG team Biltzinger et al. GCN 26061)
error box optical observation 596 sec after notice time (643 sec after trigger time)
at 2019-10-23 15:17:40 UT.

Real time updated cover map is available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1175192

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory)
started inspect of the FERMI GRB191023.63  errorbox 
596 sec after notice time (643 sec after trigger time) at 2019-10-23 15:17:40 UT,
with upper limit up to  19.0 mag.
Observations started at twilight.  The observations began at zenith distance = 37 deg. The sun  altitude  was -11.8 deg.

MASTER-Tavrida robotic telescope  located in Russia  started inspect of the FERMI GRB191023.63 
errorbox  1974 sec after notice time (2021 sec after trigger time at 2019-10-23 15:40:37 UT),
with upper limit up to  18.4 mag.
Observations started at twilight.  The observations began at zenith distance = 37 deg. The sun  altitude  was -10.2 deg.

MASTER-Tunka robotic telescope  located in Russia (Applied Physics Institute, Irkutsk State University)
started inspect of the FERMI GRB191023.63 errorbox  1974 sec after notice time (80330 sec after trigger time at 2019-10-24 13:25:47 UT),
with upper limit up to  18.0 mag. 
The observations began at zenith distance = 56 deg. The sun  altitude  was -32.8 deg.

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the FERMI GRB191023.63 errorbox
1974 sec after notice time and 1 days 9459 sec after trigger time at 2019-10-24 17:44:36 UT, with upper limit up to  16.4 mag. 
Observations started at twilight.  The observations began at zenith distance = 46 deg. The sun  altitude  is -10.4 deg.

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory) 
started inspect of the FERMI GRB191023.63 errorbox  1974 sec after notice time (1 days 14406 sec after trigger time) at 2019-10-24 19:07:03 UT, 
with upper limit up to  17.9 mag.
Observations started at twilight.  The observations began at zenith distance = 24 deg. The sun  altitude  is -9.8 deg.

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University)
started inspect of the FERMI GRB191023.63 errorbox  1974 sec after notice time (1 days 30856 sec after trigger time at 2019-10-24 23:41:13 UT),
with upper limit up to  17.3 mag. 
Observations started at twilight.  The observations began at zenith distance = 47 deg. The sun  altitude  is -10.9 deg.

MASTER-Amur robotic telescope  located in Russia (Blagoveshchensk State Pedagogical University)
started inspect of the FERMI GRB191023.63 errorbox  1974 sec after notice time (1 days 76356 sec after trigger time at 2019-10-25 12:19:32 UT),
with upper limit up to  16.9 mag.
The observations began at zenith distance = 62 deg. The sun  altitude  is -37.8 deg.

The galactic latitude b = -60 deg., longitude l = 98 deg.

Reduction will be continued, up to now there is no OT detected inside both error-boxes.
The message may be cited.


GRB_name: GRB191026A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26076
SUBJECT: GRB 191026A: Fermi GBM Final Real-time Localization
DATE:    19/10/26 08:34:54 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 08:23:44 UT on 26 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191026A (trigger 593771029.458568 / 191026350).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 37.2, Dec = -52.7 (J2000 degrees, equivalent to J2000 02h 28m, -52d 42'), with a statistical uncertainty of 5.0 degrees.

The angle from the Fermi LAT boresight is 114.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191026350/quicklook/glg_skymap_all_bn191026350.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191026350/quicklook/glg_healpix_all_bn191026350.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191026350/quicklook/glg_lc_medres34_bn191026350.gif


GRB_name: GRB191026B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26077
SUBJECT: GRB 191026B: AstroSat CZTI detection
DATE:    19/10/27 15:06:00 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

R. Gaikwad, S. Gupta, V. Sharma, D. Bhattacharya and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a GRB 191026B.

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 2019-10-26 10:15:24.0 UT. The measured peak count rate associated with the burst is 1412 cts/s above the background in the combined data of four quadrants, with a total of 11228 cts. The local mean background count rate was 582 cts/s. Using cumulative rates, we measure a T90 of 21.01 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191027A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26078
SUBJECT: GRB 191027A: Fermi GBM Final Real-time Localization
DATE:    19/10/27 15:29:32 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:19:07 UT on 27 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191027A (trigger 593882352.589944 / 191027638).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 185.5, Dec = 30.4 (J2000 degrees, equivalent to J2000 12h 22m, 30d 23'), with a statistical uncertainty of 2.6 degrees.

The angle from the Fermi LAT boresight is 33.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191027638/quicklook/glg_skymap_all_bn191027638.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191027638/quicklook/glg_healpix_all_bn191027638.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191027638/quicklook/glg_lc_medres34_bn191027638.gif


GRB_name: GRB191027A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26079
SUBJECT: GRB 191027A: BALROG localization (Fermi Trigger 593882352 / GRB 191027638)
DATE:    19/10/27 16:38:02 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
593882352 at 15:19:07 on 27 Oct. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 191.4+/-1.7 deg
Decl.(2000.0) = -11.0+/-2.4 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB191027638/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB191027638/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB191027638/json

                        


GRB_name: GRB191025A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26080
SUBJECT: Swift/BAT Trigger 931384 is not a GRB ( 191025A )
DATE:    19/10/27 21:40:55 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

Swift/BAT Trigger 931384 is not a GRB ( 191025A )

D. M. Palmer (LANL) reports on behalf of the Neil Gehrels Swift
Observatory Team:

After analysis of the complete data set, we have determined that Swift/BAT 
Trigger #931384 (tentatively labelled GRB 191025A in GCN #26072)
is a statistical fluctuation (noise peak) in the image plane and 
not an astrophysical source.


GRB_name: GRB191025B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26081
SUBJECT: GRB 191025B: Insight-HXMT/HE detection
DATE:    19/10/28 03:31:23 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, C. Cai, S. Xiao, Q. B. Yi, Y. G. Zheng, Y. Huang, 
C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-10-25T18:42:09.10 (T0), Insight-HXMT/HE detected 
GRB 191025A (trigger ID: HEB191025779) in a routine search of the data, 
which was also triggered by INTEGRAL/SPIACS (Trigger Number: 8394) and 
Konus-Wind. 

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 0.145 s measured from T0+0.03 s. 
The 1-ms peak rate, measured from T0+0.123 s, is 63021 cnts/sec. 
The total counts from this burst is 2544 counts. The data of 
Insight-HXMT/HE suffers saturation in the brightest part.
URL_LC: http://www.hxmt.org/images/GRB/HEB191025779_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191028A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26082
SUBJECT: GRB 191028A: Fermi GBM Final Real-time Localization
DATE:    19/10/28 04:20:19 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 04:10:01 UT on 28 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191028A (trigger 593928606.398038 / 191028174).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 319.2, Dec = -11.3 (J2000 degrees, equivalent to J2000 21h 16m, -11d 18'), with a statistical uncertainty of 8.8 degrees.

The angle from the Fermi LAT boresight is 89.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191028174/quicklook/glg_skymap_all_bn191028174.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191028174/quicklook/glg_healpix_all_bn191028174.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191028174/quicklook/glg_lc_medres34_bn191028174.gif


GRB_name: GRB191028B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26084
SUBJECT: GRB 191028B: Fermi GBM Final Real-time Localization
DATE:    19/10/28 14:18:19 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 14:08:04 UT on 28 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191028B (trigger 593964489.441812 / 191028589).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 276.9, Dec = 70.0 (J2000 degrees, equivalent to J2000 18h 27m, 70d 00'), with a statistical uncertainty of 7.7 degrees.

The angle from the Fermi LAT boresight is 48.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191028589/quicklook/glg_skymap_all_bn191028589.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191028589/quicklook/glg_healpix_all_bn191028589.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191028589/quicklook/glg_lc_medres34_bn191028589.gif


GRB_name: GRB191028B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26085
SUBJECT: GRB 191028B: BALROG localization (Fermi Trigger 593964489 / GRB 191028589)
DATE:    19/10/28 14:33:10 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
593964489 at 14:08:04 on 28 Oct. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 291.6+/-11.1 deg
Decl.(2000.0) = 69.8+/-3.8 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB191028589/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB191028589/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB191028589/json

                        


GRB_name: GRB191025B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26086
SUBJECT: IPN triangulation of GRB 191025B (short)
DATE:    19/10/28 20:30:41 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

K. Hurley, on behalf of the IPN,

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

Q. Luo, X. B. Li, Y. Huang, S. L. Xiong, and S. N. Zhang,
on behalf of the Insight-HXMT team, report:

The short-duration, very bright GRB 191025B
(Insight-HXMT detection: Luo et al., GCN Circ. 26081)
was detected by Konus-Wind, INTEGRAL (SPI-ACS), and Insight-HXMT,
at about 67329 s UT (18:42:09).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    60.104 (04h 00m 25s) +56.480 (+56d 28' 47")
  Corners:
    61.751 (04h 07m 00s) +54.782 (+54d 46' 54")
    60.165 (04h 00m 40s) +56.600 (+56d 36' 01")
    58.207 (03h 52m 50s) +58.177 (+58d 10' 36")
    60.041 (04h 00m 10s) +56.360 (+56d 21' 36")
  ---------------------------------------------
The error box area is 1261 sq. arcmin, and its maximum
dimension is 3.9 deg (the minimum one is 10.3 arcmin).
The Sun distance was about 130 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB191025_T67331/IPN/

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


GRB_name: GRB191027A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26087
SUBJECT: IPN triangulation of GRB 191027A
DATE:    19/10/29 07:12:56 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,

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

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

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

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

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

The long-duration GRB 191027A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 26078;
BALROG localization: Biltzinger et al., GCN Circ. 26079)
was detected by Fermi (GBM trigger 593882352), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND),
and Swift (BAT), at about 55148 s UT (15:19:08).
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:
    186.657 (12h 26m 38s) +30.957 (+30d 57' 25")
   Corners:
    166.009 (11h 04m 02s) +19.308 (+19d 18' 27")
    202.558 (13h 30m 14s) +30.844 (+30d 50' 39")
    206.169 (13h 44m 40s) +29.642 (+29d 38' 31")
    170.349 (11h 21m 24s) +23.297 (+23d 17' 48")
   ---------------------------------------------
The error box area is about 7.5 sq. deg, and its maximum
dimension is 37.7 deg (the minimum one is 13.0 arcmin).
The Sun distance was about 42 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM one.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB191027_T55143/IPN

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


GRB_name: GRB191029A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26088
SUBJECT: GRB 191029A: Swift detection of a burst
DATE:    19/10/29 11:40:59 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

P. A. Evans (U Leicester), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), K. L. Page (U Leicester) and
A. Tohuvavohu (Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 11:15:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191029A (trigger=932058).  Swift did not slew immediately 
because of an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 352.140, -40.464 which is 
   RA(J2000) = 23h 28m 34s
   Dec(J2000) = -40d 27' 49"
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 40 sec.  The peak count rate
was ~1080 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+48.5
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is P. A. Evans (pae9 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/)


GRB_name: GRB191025B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26089
SUBJECT: Konus-Wind observation of GRB 191025B
DATE:    19/10/29 12:34:07 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

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

The short-duration GRB 191025B
(Insight-HXMT detection: Luo et al., GCN Circ. 26081;
IPN triangulation: Svinkin et al., GCN Circ. 26086)
triggered Konus-Wind at T0=67331.034 s UT (18:42:11.034).

The burst light curve shows a single pulse
started at ~T0 with a total duration of ~0.2 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 8.41(-1.44,+1.52)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.006 s,
of 1.32(-0.32,+0.33)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+0.128 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.84(-0.11,+0.13)
and Ep = 2184(-608,+812) keV (chi2 = 23/26 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 =22/25 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191025_T67331/

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


GRB_name: GRB191029A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26090
SUBJECT: GRB 191029A: Swift-XRT observations
DATE:    19/10/29 13:00:49 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), D.N. Burrows (PSU), J.A. Kennea (PSU), G.
Cusumano (INAF-IASF PA), M. Perri (ASDC) and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 191029A at 12:06:55.2 UT,
3095.1 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 352.15967,
-40.50028 which is equivalent to:
   RA(J2000)  = 23h 28m 38.32s
   Dec(J2000) = -40d 30' 01.0"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 141 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 1.78
x 10^20 cm^-2 (Willingale et al. 2013). 


GRB_name: GRB191029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26091
SUBJECT: GRB 191029A: iTelescope optical upper limits
DATE:    19/10/29 17:39:05 GMT
FROM:    Filipp Dmitrievich Romanov at Amateur astronomer  <filipp.romanov.27.04.1997@gmail.com>

I observed the field of GRB 191029A (Evans et al., GCN #26088) with remote
telescope T30 (0.50-m f/6.8 reflector + CCD) of iTelescope.Net in Siding
Spring Observatory, Australia. Two images with a luminance filter were
obtained on 2019-10-29 13:16:48 UT (7288 seconds after trigger) with 60
seconds exposure time and on 13:18:46 UT (7406 seconds after trigger) with
120 seconds exposure time (the average time of each exposure). I did not
detect any optical transients (magnitude limit of about 19.2 G from Gaia
DR2 catalogue).


GRB_name: GRB191029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26092
SUBJECT: GRB 191029A: BOOTES-4/MET optical limit
DATE:    19/10/29 17:51:04 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), C. Perez 
del Pulgar, A. Castellon, I. Carrasco, A. Reina (Univ. de Malaga), S. 
Guziy (Univ. of Nikolaev), D. Xiong, Y. Fan, X. Zhao, J. Bai, C. Wang 
and Y. Xin (Yunnan Nacional Astronomical Observatory), on behalf of a 
larger collaboration, report:

Following the detection of GRB 191029A by Swift (Evans et al. GCNC 
26088), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical 
Observatory (China) automatic slewed to the GRB position and gathered 
g-band images starting at 11:31:27 UT (0.26 h after trigger, once the 
field became reachable). No optical afterglow is found down to 19.2 mag 
(at 0.9 h median time after trigger). Once the XRT position was 
available, we also took several images (clear filter) starting at 13:38 
UT. No optical afterglow was found down to 20.3 mag (at 2.5 h median 
time post trigger) at the enhaced XRT position (Osborne et al. GCNC 
26090). This is in agreement with Romanov et al. (GCNC 26091).

We thank the staff at Lijiang Observatory for their excellent support.


GRB_name: GRB191028B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26093
SUBJECT: GRB 191028B: MASTER optical observation
DATE:    19/10/29 18:41:50 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tiurina,P.Balanutsa,A.Kuznetsov, V.Vladimirov, D. Vlasenko, I.Gorbunov,
D.Zimnukhov,V.Senik (Lomonosov Moscow State University, SAI,Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova(Irkutsk State University, API),
A. Tlatov, D. Dormidontov(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University),
X.Wang (TSU),
H.Hongbo (IHEP CAS),
M.Panasyuk, I.Svertilov (SINP MSU)

MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)
started Fermi GRB 191028B (Trigger 593964489, Ttrig=2019-10-28 14:08:04UT, 
GBM localization GCN 26084, BALROG localization Biltzinger et al. GCN 26085)
  inspection 4270s after trigger time at 2019-10-28 15:19:14 UT
https://master.sai.msu.ru/site/master2/observ.php?id=1179604 .


MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory)
started inspect of the FERMI GRB191028.59 (trigger No 593964489) errorbox 
4270 sec after trigger time at 2019-10-28 15:19:14 UT, with upper limit up to  20.2 mag.
Observations started at twilight.  The observations began at zenith distance = 31 deg. The sun  altitude  is -13.3 deg.

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station)
started inspect of the FERMI GRB191028.59 errorbox  6020 sec after trigger time at 2019-10-28 15:48:24 UT
  with upper limit up to  19.3 mag. Observations started at twilight.
The observations began at zenith distance = 31 deg. The sun  altitude  is -12.9 deg.

MASTER-Tunka robotic telescope  located in Russia (Applied Physics Institute, Irkutsk State University)
started inspect of the FERMI GRB191028.59 errorbox  13498 sec after trigger time at 2019-10-28 17:53:02UT
with upper limit up to  15.9 mag.
The observations began at zenith distance = 55 deg. The sun  altitude  is -50.0 deg.

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory)
started inspect of the FERMI GRB191028.59 errorbox  26797 sec after trigger time at 2019-10-28 21:34:41 UT,
with upper limit up to  19.2 mag. 
The observations began at zenith distance = 54 deg. The sun  altitude  was -43.0 deg.

Error-box center's galactic latitude b = -60 deg., longitude l = 98 deg.

We obtained a following upper limits.

Tmid-T0  |      Date Time      |          Site       |             Coord (J2000)          |Filt.| Expt. | Limit|
_________|_____________________|_____________________|____________________________________|_____|_______|______|

     4300 | 2019-10-28 15:19:14 |   MASTER-Kislovodsk | (18h 18m 50.508s ,+68d 28m 45.13s) |   C |    60 | 19.3 |
     4300 | 2019-10-28 15:19:14 |   MASTER-Kislovodsk | (18h 41m 27.739s ,+68d 02m 33.99s) |   C |    60 | 18.9 |
     4395 | 2019-10-28 15:20:49 |   MASTER-Kislovodsk | (18h 54m 43.080s ,+70d 02m 03.07s) |   C |    60 | 19.1 |
     4395 | 2019-10-28 15:20:49 |   MASTER-Kislovodsk | (18h 29m 55.121s ,+70d 28m 22.79s) |   C |    60 | 19.5 |
     4495 | 2019-10-28 15:22:29 |   MASTER-Kislovodsk | (18h 20m 26.325s ,+72d 02m 07.00s) |   C |    60 | 19.0 |
     4495 | 2019-10-28 15:22:29 |   MASTER-Kislovodsk | (17h 53m 00.447s ,+72d 27m 59.24s) |   C |    60 | 19.5 |
     4602 | 2019-10-28 15:24:16 |   MASTER-Kislovodsk | (18h 07m 48.226s ,+70d 01m 28.67s) |   C |    60 | 19.2 |
     4602 | 2019-10-28 15:24:16 |   MASTER-Kislovodsk | (17h 43m 05.065s ,+70d 27m 11.44s) |   C |    60 | 19.5 |
     5708 | 2019-10-28 15:42:42 |   MASTER-Kislovodsk | (18h 41m 22.383s ,+68d 02m 13.56s) |   C |    60 | 19.2 |
     5708 | 2019-10-28 15:42:42 |   MASTER-Kislovodsk | (18h 18m 46.092s ,+68d 28m 02.67s) |   C |    60 | 19.5 |
     5807 | 2019-10-28 15:44:21 |   MASTER-Kislovodsk | (18h 54m 37.221s ,+70d 01m 41.42s) |   C |    60 | 19.3 |
     5807 | 2019-10-28 15:44:21 |   MASTER-Kislovodsk | (18h 29m 50.438s ,+70d 27m 39.37s) |   C |    60 | 19.5 | 
....

Real time updated cover map and discovered OT are available at:
https://master.sai.msu.ru/site/master2/observ.php?id=1179604

The reduction will be continued.
The message may be cited.
This work was suported by RFBR 17-52-80133


GRB_name: GRB191029A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26094
SUBJECT: GRB 191029A: Swift-XRT refined Analysis
DATE:    19/10/29 22:49:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), J.A. Kennea (PSU), B. Sbarufatti (PSU), D.N.
Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester),
M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA)  and P.A. Evans
report on behalf of the Swift-XRT team:

We have analysed 9.0 ks of XRT data for GRB 191029A (Evans et al. GCN
Circ. 26088), from 4.0 ks to 27.7 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The refined XRT position is
RA, Dec = 352.1492, -40.5661 which is equivalent to:

RA (J2000): 23 28 35.80
Dec(J2000): -40 33 58.0

with an uncertainty of 3.6 arcsec (radius, 90% confidence). The light
curve is consistent with a constant source of mean count rate 8.2e-02
ct/sec. A power-law fit gives an index of 0.08 (+0.12, -0.13).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.54 (+0.16, -0.10). The
best-fitting absorption column is  1.92 (+3.90, -0.14) x 10^20 cm^-2,
consistent with the Galactic value of 1.8 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 3.9 x 10^-11 (4.0 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.92 (+3.90, -0.14) x 10^20 cm^-2
Galactic foreground: 1.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.54 (+0.16, -0.10)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00932058.

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


GRB_name: GRB191029A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26095
SUBJECT: GRB 191029A: Enhanced Swift-XRT position
DATE:    19/10/29 23:31:08 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 6396 s of XRT Photon Counting mode data and 12 UVOT
images for GRB 191029A, 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 = 352.16141, -40.50108 which is equivalent
to:

RA (J2000): 23h 28m 38.74s
Dec (J2000): -40d 30' 03.9"

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: GRB191027A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26096
SUBJECT: Correction to GCN 26079 regarding GRB 191027A
DATE:    19/10/30 02:41:15 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

B. Biltzinger, J. Greiner (both MPE Garching) report:

The BALROG localization of GRB 191027A (Fermi Trigger 593882352 / GRB 191027638)  
(https://grb.mpe.mpg.de/grb/GRB191027638/?data_version=0)
published in Biltzinger et al. 2019 (GCN Circ. 26079) was sent by mistake, as
it suffered an obvious problem in the automatic background fit (e.g. n1, n5).
Corrected files have now been uploaded on 
https://grb.mpe.mpg.de/grb/GRB191027638/?data_version=zzz_bkg_corrected

The history of the original fits will remain on the page.
  
We apologize for any confusion this may have caused.


GRB_name: GRB191029A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26097
SUBJECT: GRB 191029A: Swift/UVOT Upper Limits
DATE:    19/10/30 05:38:53 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (U.Warwick) and P. A. Evans (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191029A
4.3 ks after the BAT trigger (Evans et al., GCN Circ. 26088).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 26095)
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             4280        22783         1598         >22.1
v                 4691        15599         1082         >20.2
b                 5510        28520         2353         >21.7
u                 5305        21337         1082         >20.9
w1                5100        17046          723         >20.4
m2                4895        16504         1082         >20.6
w2                4486        11309          868         >20.7

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: GRB191019A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26098
SUBJECT: GRB 191019A: Zadko Telescope optical observations
DATE:    19/10/30 05:46:27 GMT
FROM:    Bruce Gendre at UVI  <bruce.gendre@gmail.com>

B. Gendre (OzGrav-UWA), H. Crisp (OzGrav-UWA), D. Coward (OzGrav-UWA), 
J. Zadko (Claire Energy), J. A. Moore (OzGrav-UWA), A. Burrell 
(OzGrav-UWA), A. Klotz (IRAP-OMP-UPS), P. Thierry (Auragne Observatory), 
E.J. Howell (OzGrav-UWA), A. Verveer (ASA), J. Kennewell (UWA, ASA)

report:

We observed GRB 191019A (Simpson et al., GCN 26031) with the Zadko 
Telescope (Coward et al. 2017), starting at 2019 October the 19th at
15:20:23 UT (7 minutes 50 seconds after the trigger) under fair conditions.

The object reported by Reva et al. (GCN 26036) is clearly visible in our 
images. However, we measure an R magnitude of 18.92 at the time reported 
by the GCN. Observations stopped one hour twenty three minutes after the 
burst, and during that time we do not see any variation on the light 
curve, similar to other teams (Perley et al., GCN 26039; Fynbo et al., 
GCN 26041; and Zhu et al., GCN 26059). At that position, the USNO 
catalog reports a source of magnitude R = 19.0, consistent with our 
findings. We conclude that this object is not the afterglow of GRB 
191019A, but the host galaxy, as reported by Perley et al. (GCN 26062).


The Zadko Telescope has been under refurbishment during the last year, 
and is still in recommissioning mode. This message can be cited.


-- 
L'absence de virus dans ce courrier Ã©lectronique a Ã©tÃ© vÃ©rifiÃ©e par le logiciel antivirus Avast.
https://www.avast.com/antivirus


GRB_name: GRB191029A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26099
SUBJECT: GRB 191029A: CORRECTED Swift-XRT refined analysis
DATE:    19/10/30 09:56:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans and K.L. Page (U. Leicester) report on behalf of the
Swift-XRT team:

The XRT refined analysis for GRB 191029A, given in GCN 26094 was
incorrect. There is an AGN within the BAT error circle and unfortunately
the automated light curve and spectral analysis had been performed for
this source, rather than the afterglow.

The correct refined analysis is below. We apologise for any
inconvenience.

We have analysed 13 ks of XRT data for GRB 191029A (Evans et al. GCN
Circ. 26088), from 3.1 ks to 62.0 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Evans et al. (GCN Circ. 26095).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.77 (+0.13, -0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.23, -0.19). The
best-fitting absorption column is  3.4 (+5.3, -1.6) x 10^20 cm^-2,
consistent with the Galactic value of 1.8 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 3.5 x 10^-11 (3.7 x
10^-11) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Total column:        3.4 (+5.3, -1.6) x 10^20 cm^-2
Galactic foreground: 1.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:        1.81 (+0.23, -0.19)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00932058.


GRB_name: GRB191027A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26100
SUBJECT: Konus-Wind observation of GRB 191027A
DATE:    19/10/30 20:03:53 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

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

The long-duration GRB 191027A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 26078;
IPN triangulation: Hurley et al., GCN Circ. 26087)
triggered Konus-Wind at T0=55143.905 s UT (15:19:03.905).

The burst light curve shows a single pulse
started at ~T0-0.1 s with a total duration of ~7.1 s.
The emission is seen up to ~4 MeV.

As observed by Konus-Wind, the burst
had a fluence of 5.24(-1.01,+1.84)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.002 s,
of 7.53(-2.28,+2.60)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+8.448 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 = -1.28(-0.22,+0.26)
and Ep = 443(-153,+468) keV (chi2 = 68/73 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 = 68/72 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+0.064 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model
with  alpha = -0.09(-0.61,+0.84)
and Ep = 444(-106,+210) keV (chi2 = 8/15 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 8/14 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191027_T55143/

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


GRB_name: GRB191031A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26101
SUBJECT: GRB 191031A: Swift detection of a burst
DATE:    19/10/31 00:45:49 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC),
J. A. Kennea (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 00:36:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191031A (trigger=932435).  Swift did not slew due to an 
observing constraint.  The BAT on-board calculated location is 
RA, Dec 233.470, +6.144 which is 
   RA(J2000) = 15h 33m 53s
   Dec(J2000) = +06d 08' 37"
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 50 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 23:18 UT on 2019 December 22. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB191031A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26102
SUBJECT: GRB 191031A: Fermi GBM Final Real-time Localization
DATE:    19/10/31 00:46:50 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 00:36:35 UT on 31 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191031A (trigger 594175000.608294 / 191031025).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 247.3, Dec = 22.1 (J2000 degrees, equivalent to J2000 16h 29m, 22d 06'), with a statistical uncertainty of 12.9 degrees.

The angle from the Fermi LAT boresight is 93.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031025/quicklook/glg_skymap_all_bn191031025.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031025/quicklook/glg_healpix_all_bn191031025.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031025/quicklook/glg_lc_medres34_bn191031025.gif


GRB_name: GRB191031A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26103
SUBJECT: GRB 191031A: COATLI Optical Observations 
DATE:    19/10/31 03:43:46 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM),  Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego GonzÃ¡lez
(UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita Pereyra
(UNAM), and Eleonora Troja (GSFC) report:

We observed the field of GRB 191031A (D'Ai et al., GCN Circ. 26101; Fermi GBM
Team, GCN Circ. 26102) with the COATLI 50-cm telescope and interim imager at the
Observatorio AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-10-31 02:14 UTC (1.63 hours after the
trigger) to 02:25, obtaining a total of 540 seconds of exposure in the w filter.
The observations were taken at airmasses between 6.4 and 8.3.

We do not detetect any uncataloged sources in the BAT error region to a 10-sigma
limit of w = 18.75.

Our w magnitudes are calibrated against the Pan-STARRS1 catalog, are on an
approximate AB system (Becerra et al., 2019, ApJ, 872, 118), and are not
corrected for Galactic extinction in the direction of the GRB.

We thank the COATLI technical team and the staff of the Observatorio AstronÃ³mico
Nacional.


GRB_name: GRB191031B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26104
SUBJECT: GRB 191031B: Fermi GBM Final Real-time Localization
DATE:    19/10/31 15:25:13 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:14:54 UT on 31 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191031B (trigger 594227699.816476 / 191031635).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 31.8, Dec = -14.2 (J2000 degrees, equivalent to J2000 02h 07m, -14d 11'), with a statistical uncertainty of 14.3 degrees.

The angle from the Fermi LAT boresight is 70.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031635/quicklook/glg_skymap_all_bn191031635.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031635/quicklook/glg_healpix_all_bn191031635.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031635/quicklook/glg_lc_medres34_bn191031635.gif


GRB_name: GRB191025B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26106
SUBJECT: GRB 191025B: AstroSat CZTI detection
DATE:    19/10/31 18:19:38 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 191025B, which was also detected by Insight-HXMT/HE (Luo Q. et al., GCN #26081), IPN triangulation (Svinkin D. et al., GCN #26086) and Konus-Wind (Kozlova et al., GCN #26089).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 2019-10-25 18:42:09.0 UT. The measured peak count rate associated with the burst is 449 cts/s above the background in the combined data of four quadrants, with a total of 567 cts. The local mean background count rate was 514 cts/s. Using cumulative rates, we measure a T90 of 6.9 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191031C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26107
SUBJECT: GRB 191031C: Fermi GBM Final Real-time Localization
DATE:    19/10/31 18:53:33 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 18:43:16 UT on 31 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191031C (trigger 594240201.70685 / 191031780).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 120.8, Dec = -59.6 (J2000 degrees, equivalent to J2000 08h 03m, -59d 36'), with a statistical uncertainty of 1.6 degrees.

The angle from the Fermi LAT boresight is 19.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031780/quicklook/glg_skymap_all_bn191031780.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031780/quicklook/glg_healpix_all_bn191031780.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031780/quicklook/glg_lc_medres34_bn191031780.gif


GRB_name: GRB191031C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26108
SUBJECT: GRB 191031C: Swift detection of a burst
DATE:    19/10/31 18:55:34 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), J.D. Gropp (PSU),
N. J. Klingler (PSU), H. A. Krimm (NSF), S Laha (GSFC/UMBC/CRESST),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 18:43:54 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191031C (trigger=932595).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 115.862, -62.335 which is 
   RA(J2000) = 07h 43m 27s
   Dec(J2000) = -62d 20' 04"
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 80 sec.  The peak count rate
was ~2400 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 18:45:16.2 UT, 81.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 115.8682, -62.3247 which is equivalent to:
   RA(J2000)  = 07h 43m 28.37s
   Dec(J2000) = -62d 19' 28.9"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 38 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 2.60e-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
0.17. 

Burst Advocate for this burst is E. Ambrosi (elena.ambrosi AT 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/)


GRB_name: GRB191031C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26109
SUBJECT: GRB 191031C: Prompt enhanced Swift-XRT position
DATE:    19/10/31 19:20:12 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 191031C, we find an
enhanced XRT position of the afterglow: RA, Dec: 115.8709, -62.3251
which is equivalent to:
   RA (J2000)  = 07 43 29.01
   Dec (J2000) = -62 19 30.5
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/932595.

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: GRB191029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26110
SUBJECT: GRB 191029A: Swift-BAT refined analysis
DATE:    19/10/31 19:46:10 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),  J. R. Cummings (CPI), 
P. A. Evans (U Leicester), H. A. Krimm (NSF), S. Laha (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+240 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 191029A (trigger #932058)
(Evans, et al., GCN Circ. 26088).  The BAT ground-calculated position is
RA, Dec = 352.140, -40.464 deg which is 
  RA(J2000)  =  23h 28m 33.6s 
  Dec(J2000) = -40d -27' -49.8" 
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.

The mask-weighted light curve shows a pair of weak pulses spanning the period 
from approximately T-5 to T+35 seconds. T90 (15-350 keV) is 39.5 +- 7.9 sec 
(estimated error including systematics).

The time-averaged spectrum from T-1.05 to T+45.85 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.77 +- 0.21.  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+1.90 sec in the 15-150 keV band
is 1.1 +- 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/932058/BA/


GRB_name: GRB191031C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26111
SUBJECT: GRB 191031C: Fermi GBM Final Real-time Localization
DATE:    19/10/31 21:33:56 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 21:23:31 UT on 31 Oct 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191031C (trigger 594249816.128134 / 191031891).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 282.8, Dec = 55.0 (J2000 degrees, equivalent to J2000 18h 51m, 55d 00'), with a statistical uncertainty of 2.4 degrees.

The angle from the Fermi LAT boresight is 58.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031891/quicklook/glg_skymap_all_bn191031891.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031891/quicklook/glg_healpix_all_bn191031891.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191031891/quicklook/glg_lc_medres34_bn191031891.gif


GRB_name: GRB191031D
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26112
SUBJECT: GRB 191031D: Swift detection of a short hard burst
DATE:    19/10/31 21:53:41 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

V. D'Elia (SSDC), E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
H. A. Krimm (NSF), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 21:23:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191031D (trigger=932608).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 283.275, +47.639 which is 
   RA(J2000) = 18h 53m 06s
   Dec(J2000) = +47d 38' 19"
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 0.4 sec.  The peak count rate
was ~18000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 21:24:59.8 UT, 88.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 283.2890,
47.6438 which is equivalent to:
   RA(J2000)  = 18h 53m 09.37s
   Dec(J2000) = +47d 38' 37.7"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 38 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. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 92 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
0.08. 

This GRB was also detected by Fermi/GBM (trignum=191031891, GCN
26111), and the INTEGRAL/SPIACS event (trignum=8402). We note that the
Fermi automated circular has misnamed this event GRB 191031C. 

Burst Advocate for this burst is V. D'Elia (delia AT ssdc.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/)


GRB_name: GRB191031D
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26114
SUBJECT: Correction in name: GRB 191031D (not GRB 191031C)
DATE:    19/10/31 22:21:14 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

B. Mailyan (UAH) reports on behalf of the Fermi GBM Team:

"The Fermi Gamma-ray Burst Monitor (GBM) trigger 594249816/191031891
at 21:23:31 UT on 31 Oct 2019, of GRB 191031C (GCN Circ. #26111) should be
GRB 191031D.
We apologize for any confusion caused.â€


GRB_name: GRB191031C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26115
SUBJECT: GRB 191031C: Enhanced Swift-XRT position
DATE:    19/10/31 22:53:20 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 1562 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 191031C, 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 = 115.87049, -62.32466 which is equivalent
to:

RA (J2000): 07h 43m 28.92s
Dec (J2000): -62d 19' 28.8"

with an uncertainty of 1.8 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: GRB191031A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26116
SUBJECT: GRB 191031A: Fermi GBM detection
DATE:    19/10/31 23:56:09 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

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

"At 00:36:35.61 UT on 31 October 2019, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 191031A (trigger 594175000 / 191031025)
which was also detected by the Swift/BAT (D'Ai et al. 2019, GCN 26101)
The Fermi GBM Final Real-time Localization (GCN 26102) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 106
degrees.

The GBM light curve shows two pulses with a duration (T90) of about 200 s
(50-300 keV). The time-averaged spectrum of the first pulse from T0-10.24 s
to T0+10.24 s is best fit by a power law with an exponential
high-energy cutoff. The power law index is -0.9 +/- 0.2 and the cutoff
energy, parameterized as Epeak, is 218 +/- 57 keV. The time-averaged
spectrum of the second pulse from T+174.08 to T0+197.64 is best fit
by the same function with an index of -1.1 +/- 0.1 and an Epeak of 242 +/-
48 keV.

The event fluence (10-1000 keV) in the time interval of the two pulses is
(6.6 +/- 0.6)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+175.56 s in the 10-1000 keV band
is 2.5 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB191031D
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26117
SUBJECT: GRB 191031D: Enhanced Swift-XRT position
DATE:    19/11/01 00:27:16 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 722 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 191031D, 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 = 283.28951, +47.64407 which is equivalent
to:

RA (J2000): 18h 53m 9.48s
Dec (J2000): +47d 38' 38.6"

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: GRB191031D
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26118
SUBJECT: GRB 191031D: Fermi GBM detection
DATE:    19/11/01 03:22:35 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

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

"At 21:23:31.13 UT on 31 October 2019, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 191031D (trigger 594249816/191031891)
which was also detected by the Swift BAT and XRT (D'Elia et al. 2019, GCN
26112)
The Fermi GBM Final Real-time Localization (GCN 26111) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 64
degrees.

The GBM light curve shows a short spike with a duration (T90) of about
0.256 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.32 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.42 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 856 +/- 53 keV

The event fluence (10-1000 keV) in this time interval is
(4.36 +/- 0.09)E-06 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.128 s in the 10-1000 keV band
is 48.7 +/- 1.59 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB191031C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26119
SUBJECT: GRB 191031C: Fermi GBM detection
DATE:    19/11/01 03:48:32 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

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

"At 18:43:16.71 UT on 31 October 2019, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 191031C (trigger 594240201 / 191031780)
which was also detected by the Swift BAT and XRT (Ambrosi et al. 2019, GCN 26108).
The Fermi GBM Final Real-time Localization (GCN 26107) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 20 degrees.

The GBM light curve shows a complex, multi-peaked structure
with a duration (T90) of about 78 s (50-300 keV).
The time-averaged spectrum from T0+3.3  s to T0+81.2 s is
best fit by a Band function with Epeak = 107 +/- 9 keV,
alpha = -0.5 +/- 0.1, and beta = -2.3 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(1.33 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+42.2 s in the 10-1000 keV band
is 7.3 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB191031D
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26120
SUBJECT: GRB 191031D: VLA 9.8 GHz upper limit
DATE:    19/11/01 04:14:06 GMT
FROM:    Wen-fai Fong at Northwestern U  <wfong@northwestern.edu>

T. Laskar (Bath), W. Fong, K. D. Alexander, G. Schroeder, K. Paterson (Northwestern) and E. Berger (Harvard) report:

"We observed the position of the short-duration GRB 191031D (Fermi-GBM et al., GCN 26111; D'Elia et al., GCN 26112; Mailyan et al., GCN 26118) with the Karl G. Jansky Very Large Array (VLA) under Program 19B-217 (PI: Fong) beginning on 2019 Oct 31.992 UT (2.4 hr post-burst) at a mean frequency of 9.8 GHz. Based on preliminary analysis, in 1 hour of observations we do not detect any radio emission at or near the position of the XRT afterglow (Osborne et al., GCN 26117) to a 3-sigma limit of 15 microJy. Additional, detailed analysis is ongoing.

We thank Amy Mioduszewski and the rest of the VLA staff for their assistance with rapidly approving and executing these observations. Further observations are planned."


GRB_name: GRB191031D
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26121
SUBJECT: GRB 191031D: RATIR Optical and NIR Observations 
DATE:    19/11/01 04:40:51 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

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), JesÃºs GonzÃ¡lez (UNAM), Carlos
RomÃ¡n-ZÃºÃ±iga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou
(U. Wash.), and Vicki Toy (UMD) report:

We observed the field of GRB 191031D (Fermi GBM Team, GCN Circ. 26111; D'Elia et
al., GCN Circ. 26112) 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 2019/11 1.09 to 2019/11
1.12 UTC (4.65 to 5.49 hours after the BAT trigger), obtaining a total of 0.56
hours exposure in the r and i bands, 0.23 hours exposure in the Z and Y
bands, and 0.06 hours exposures in the J 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 > 22.94
  i > 23.17
  Z > 21.50
  Y > 21.40
  J > 19.44
  H > 19.33

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: GRB191031D
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26122
SUBJECT: GRB 191031D: COATLI Optical Observations 
DATE:    19/11/01 05:13:02 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM),  Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego GonzÃ¡lez
(UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita Pereyra
(UNAM), and Eleonora Troja (GSFC) report:

We observed the field of GRB 191031A (D'Ai et al., GCN Circ. 26101; Fermi GBM
Team, GCN Circ. 26102) with the COATLI 50-cm telescope and interim imager at the
Observatorio AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-11-01 02:47 UTC to 04:49 UTC (5.4 to
7.4 hours after the trigger), obtaining a total of 4530 seconds of exposure in
the w filter.

We do not detetect any uncataloged sources in the enhanced XRT error region
(Osborne et al., GCN Circ. 26117) to a 3-sigma limit of w = 23.2.

Our w magnitudes are calibrated against the Pan-STARRS1 catalog, are on an
approximate AB system (Becerra et al., 2019, ApJ, 872, 118), and are not
corrected for Galactic extinction in the direction of the GRB.

We thank the COATLI technical team and the staff of the Observatorio AstronÃ³mico
Nacional.


GRB_name: GRB191031D
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26123
SUBJECT: GRB 191031D: AGILE/MCAL observations
DATE:    19/11/01 09:11:45 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G.
Piano (INAF/IAPS), F. Lucarelli, C. Pittori (SSDC, and INAF/OAR), A.
Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia, A.
Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), F. Longo (Univ. Trieste and
INFN Trieste), report on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected the short GRB 191031D at T0 =
2019-10-31 21:23:28.17 +/- 0.01 s (UTC), already detected by Fermi/GBM (GCN
#26111), Swift (D'Elia et al., 2019; GCN #26112), and INTEGRAL/SPIACS
(trignum=8402).

The event lasted about 0.2 s and released a total number of ~430 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 544 counts / s.

The light curve shows a single peak episode and can be found at
http://www.agilescienceapp.it/notices/GRB_064997_499641808.174626.png.

The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the
energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress.


GRB_name: GRB191031D
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26124
SUBJECT: GRB 191031D: Swift-XRT refined Analysis
DATE:    19/11/01 09:29:57 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

B. Sbarufatti (PSU), D.N. Burrows (PSU), J. D. Gropp (PSU), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi  (INAF-IASFPA) , M.
Capalbi (INAF-IASFPA) and V. D'Elia report on behalf of the Swift-XRT
team:

We have analysed 6.2 ks of XRT data for GRB 191031D (D'Elia et al. GCN
Circ. 26112), from 101 s to 17.5 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. 26117).

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.04 (+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 1.90 (+0.26, -0.16). The
best-fitting absorption column is  consistent with the Galactic value
of 6.6 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 3.3 x 10^-11 (3.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.6 (+/-2.1) x 10^20 cm^-2
Galactic foreground: 6.6 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.90 (+0.26, -0.16)

If the light curve continues to decay with a power-law decay index of
2.04, the count rate at T+24 hours will be 1.9 x 10^-6 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x
10^-17 (7.1 x 10^-17) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00932608.

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


GRB_name: GRB191031D
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26125
SUBJECT: GRB 191031D: MITSuME Akeno optical upper limits
DATE:    19/11/01 10:51:07 GMT
FROM:    Ogawa Futa at Tokyo Institute of Technology  <ogawa@hp.phys.titech.ac.jp>

F. Ogawa, R. Adachi, K. L. Murata, M. Oeda, K.Shiraishi, K. Iida, M. 
Niwano,
R. Hosokawa, S. Toma, Y. Yatsu, and N. Kawai (TokyoTech)
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 191031D (The Fermi GBM 
team, GCN Circular #26111, V. D'Elia et al., GCN Circular #26112, Bagrat 
Mailyan, #26114) 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 19/11/01 08:18:36 UT. We did not find any new 
point
sources within the XRT circle (J.P. Osborne et al., GCN Circular #26117)
in all three bands.
We obtained the following 5-sigma limits for the magnitudes.

T0+[hour]   MID-UT    T-EXP[sec]    5-sigma limits
------------------------------------------------------------------------------------------------ 

  ~11.5         09:12:34    1680              g'>18.3, Rc>18.2, Ic>17.3
------------------------------------------------------------------------------------------------ 

T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used UCAC4 catalog for flux calibration.
The magnitudes are expressed in the AB system.


GRB_name: GRB191031D
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26126
SUBJECT: Konus-Wind observation of GRB 191031D
DATE:    19/11/01 11:56:53 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The short-duration GRB 191031D
(Swift detection: D'Elia et al., GCN Circ. 26112;
Fermi GBM detection: Mailyan & Meegan, GCN Circ. 26118;
AGILE/MCAL observations: Ursi et al., GCN Circ. 26123)
triggered Konus-Wind at T0=77011.324 s UT (21:23:31.324).

The burst light curve shows a mult-peaked pulse
which started at ~T0-0.064 s and had a total duration of ~0.35 s.
The emission is seen up to ~5 MeV.

As observed by Konus-Wind, the burst
had a fluence of 2.72(-0.27, +0.31)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.016 s,
of 1.95(-0.32,+0.38)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 15 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.27(-0.17,+0.20)
and Ep = 370(-46,+58) keV (chi2 = 35/39 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 =35/38 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191031_T77011/

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


GRB_name: GRB191031C
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26127
SUBJECT: GRB 191031C: Swift/UVOT Detection
DATE:    19/11/01 16:22:13 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

GRB 191031C: Swift/UVOT Detection

J. D. Gropp (PSU) and Ambrosi (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191031C
91 s after the BAT trigger (Ambrosi et al., GCN Circ. 26108).
A source consistent with the XRT position
(Goad et al. GCN Circ. 26115)
is detected in the initial UVOT exposures.

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

u                        307           556            245          >19.71
white                   92            242            147            20.27+-0.32
white                 862          1011            147          >20.39


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.17 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB191031D
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26128
SUBJECT: GRB 191031D: Swift/UVOT Upper Limits
DATE:    19/11/01 17:00:34 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

GRB 191031D: Swift/UVOT Upper Limits

J. D. Gropp (PSU) and V. D'Elia (SSDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191031D
93 s after the BAT trigger (D'Elia et al., GCN Circ. 26112).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 26117)
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            93          242          147         >20.8
u_FC               306          555          246         >20.2
white               93         6694          575         >21.1
v                  636         5863          294         >19.9
b                  561         6683          471         >20.4
u                  306         6477          697         >20.3
w1                 686         6273          452         >19.8
m2                 661         6067          294         >19.6
w2                 612         5658          294         >19.9

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: GRB191031D
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26129
SUBJECT: GRB 191031D: AstroSat CZTI detection
DATE:    19/11/01 18:46:38 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 191031D, which was also detected by Fermi GBM Real-time Localization (GCN #26111), Swift (D'Elia et al., GCN #26112), Swift-XRT (Osborne et al., GCN #26117), Fermi GBM (Mailyan et al., GCN #26118), VLA (Laskar T. et al., GCN #26120), RATIR (Butler N. et al., GCN #26121), COATLI (Watson A. M. et al., GCN #26122), AGILE/MCAL (Ursi A. et al., GCN #26123), MITSuME Akeno (Ogawa F. et al., GCN #26125) and Konus-Wind (Frederiks D. et al., GCN #26126).

The source was clearly detected in the 40-200 keV energy range. The light curve showed single pulse of emission peaking at 2019-10-31 21:23:31.0 UT. The measured peak count rate associated with the burst is 628 cts/s above the background in the combined data of four quadrants, with a total of 393 cts. The local mean background count rate was 556 cts/s. Using cumulative rates, we measure a T90 of 0.35 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191031C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26130
SUBJECT: GRB 191031C: Swift-XRT refined Analysis
DATE:    19/11/01 18:56:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J. D. Gropp (PSU), P.A. Evans (U. Leicester), J.P.
Osborne (U. Leicester), K.L. Page (U. Leicester), M. Capalbi
(INAF-IASFPA), M. Perri (ASDC), A. Tohuvavohu (U. Toronto) and E.
Ambrosi report on behalf of the Swift-XRT team:

We have analysed 4.9 ks of XRT data for GRB 191031C (Ambrosi et al. GCN
Circ. 26108), from 87 s to 52.5 ks after the  BAT trigger. The data
comprise 1.6 ks in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN Circ. 26109).

The late-time light curve (from T0+6.6 ks) can be modelled with a
power-law decay with a decay index of alpha=1.06 (+0.17, -0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.99 (+0.08, -0.06). The
best-fitting absorption column is  1.87 (+0.28, -0.08) x 10^21 cm^-2,
consistent with the Galactic value of 1.8 x 10^21 cm^-2 (Willingale et
al. 2013). The PC mode spectrum has a photon index of 1.79 (+0.12,
-0.05) and a best-fitting absorption column consistent with the
Galactic value. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.9 x 10^-11 (4.9 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.8 (+0.4, -0.0) x 10^21 cm^-2
Galactic foreground: 1.8 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.79 (+0.12, -0.05)

If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 0.029 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 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/00932595.

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


GRB_name: GRB191031A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26131
SUBJECT: GRB 191031A: Swift-BAT refined analysis
DATE:    19/11/01 19:05:44 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), 
A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), 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-61 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 191031A (trigger #932435)
(D'Ai, et al., GCN Circ. 26101).  The BAT ground-calculated position is
RA, Dec = 233.490, 6.109 deg which is 
 RA(J2000)  =  15h 33m 57.7s 
 Dec(J2000) = +06d 06' 32.9" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.

The mask-weighted light curve shows a single pulse with some overlying 
structure.  The emission starts at ~T-8 sec, peaks at T+3 sec, and decays
to background by ~T+18 sec. A pre-planned spacecraft slew took the burst
location out of the field of view by T+95 sec. T90 (15-350 keV) is 19.1 +- 6.3 sec 
(estimated error including systematics).

The time-averaged spectrum from T-11.08 to T+16.87 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.38 +- 0.19.  The fluence in the 15-150 keV band is 9.0 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.48 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. 

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/932435/BA/


GRB_name: GRB191031C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26132
SUBJECT: GRB 191031C: Swift-BAT refined analysis
DATE:    19/11/01 19:06:54 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

D. M. Palmer (LANL), E. Ambrosi (INAF-IASFPA), S. D. Barthelmy (GSFC), 
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), 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-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 191031C (trigger #932595)
(Ambrosi, et al., GCN Circ. 26108).  The BAT ground-calculated position is
RA, Dec = 115.880, -62.322 deg which is 
  RA(J2000)  =  07h 43m 31.2s 
  Dec(J2000) = -62d 19' 20.1" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 24%.

The mask-weighted light curve shows several peaks.  The first begins around 
T-40 sec and runs until T-20 sec.  The second, brightest, peak begins immediately
after, peaks around T+5 sec, and decays to background by T+120 sec. There are
several weak peaks superimposed on this one, the largest coming around T+45 sec.  
T90 (15-350 keV) is 93.2 +- 19.0 sec (estimated error including systematics).

The time-averaged spectrum from T-37.98 to T+112.66 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.60 +- 0.07.  The fluence in the 15-150 keV band is 7.2 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.04 sec in the 15-150 keV band
is 4.6 +- 0.5 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/932595/BA/


GRB_name: GRB191031D
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26133
SUBJECT: GRB 191031D: Swift-BAT refined analysis
DATE:    19/11/01 19:07:47 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), V. D'Elia (SSDC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), J. P. Norris (BSU), D. M. Palmer (LANL), 
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 191031D (trigger #932608)
(D'Elia, et al., GCN Circ. 26112).  The BAT ground-calculated position is
RA, Dec = 283.269, 47.645 deg which is 
 RA(J2000)  =  18h 53m 04.5s 
 Dec(J2000) = +47d 38' 40.9" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 37%.

The mask-weighted light curve shows a multi-peak structure from T-0.05 sec to T+0.3 sec
with a harder first pulse and softer second pulse.  There is no sign of extended emission.
T90 (15-350 keV) is 0.29 +- 0.05 sec (estimated error including systematics).

The time-averaged spectrum from T-0.03 to T+0.31 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.80 +- 0.15.  The fluence in the 15-150 keV band is 4.1 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.36 sec in the 15-150 keV band
is 4.3 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The duration and hardness of GRB 191031D place it squarely within the distribution of
short, hard bursts detected by BAT.   Using the 4-ms binned light curve, the spectral lag 
of the burst is 0.2 ms +- 2 ms for the 50-100 keV to 15-25 keV bands, and 0.4 ms +- 3 ms
for the 100-350 keV to 25-50 keV bands. These values are consistent with a short GRB.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/932608/BA/


GRB_name: GRB191031D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26134
SUBJECT: GRB 191031D: MMT Binospec Optical Upper Limit
DATE:    19/11/01 20:39:58 GMT
FROM:    Kerry Paterson at Northwestern  <kerry.paterson@northwestern.edu>

K. Paterson, W. Fong, K. D. Alexander, G. Schroeder, A. Rouco Escorial (Northwestern) report:

â€œWe observed the field of the short-duration GRB 191031D (Fermi-GBM et al., GCN 26111; D'Elia et al., GCN 26112; Mailyan et al., GCN 26118) with Binospec mounted on the 6.5-m MMT on Mount Hopkins, Arizona, starting on 2019 November 1 at 01:44:13 UT, 4.31 hours after the burst. We obtained 15x120-sec of observations in the r-band in 1.05â€ seeing and clear conditions.

We do not detect any optical source in or around the enhanced XRT position (Osborne et al. GCN 26117).

We obtain a 3-sigma upper limit of r > 23.5 AB mag on the afterglow or any coincident host galaxy, not corrected for Galactic extinction. Photometry is calibrated to the USNO-B1.0 catalog. This limit is consistent with, and slightly deeper than the limit found by Butler et al. (GCN 26121). We note that the closest, clearly-extended source is 5.48 arcsec to the southwest.

Further observations are planned. We thank the MMT staff, and in particular observer Michael Calkins, for their assistance with these observations.â€


GRB_name: GRB191101A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26135
SUBJECT: GRB 191101A: Swift detection of a burst
DATE:    19/11/01 21:33:39 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC),
J. A. Kennea (PSU), N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 21:08:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191101A (trigger=932742).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 251.844, +43.754 which is 
   RA(J2000) = 16h 47m 23s
   Dec(J2000) = +43d 45' 15"
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 20 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 21:09:42.4 UT, 99.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 251.83474, 43.74103 which
is equivalent to:
   RA(J2000)  = 16h 47m 20.34s
   Dec(J2000) = +43d 44' 27.7"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 52 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 8.42e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 109 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.01. 

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


GRB_name: GRB191101B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26136
SUBJECT: GRB 191101B: Fermi GBM Final Real-time Localization
DATE:    19/11/01 21:39:07 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 21:28:50 UT on 1 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191101B (trigger 594336535.522754 / 191101895).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 153.7, Dec = 19.0 (J2000 degrees, equivalent to J2000 10h 14m, 19d 00'), with a statistical uncertainty of 7.8 degrees.

The angle from the Fermi LAT boresight is 118.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191101895/quicklook/glg_skymap_all_bn191101895.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191101895/quicklook/glg_healpix_all_bn191101895.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191101895/quicklook/glg_lc_medres34_bn191101895.gif


GRB_name: GRB191101A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26137
SUBJECT: GRB 191101A: Prompt enhanced Swift-XRT position
DATE:    19/11/01 21:48:45 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 191101A, we find an
enhanced XRT position of the afterglow: RA, Dec: 251.8374, 43.7406
which is equivalent to:
   RA (J2000)  = 16 47 20.97
   Dec (J2000) = +43 44 26.3
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/932742.

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: GRB191101A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26140
SUBJECT: GRB 191101A: Enhanced Swift-XRT position
DATE:    19/11/01 23:49:51 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 1298 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 191101A, 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 = 251.83723, +43.74096 which is equivalent
to:

RA (J2000): 16h 47m 20.94s
Dec (J2000): +43d 44' 27.5"

with an uncertainty of 1.8 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: GRB191101A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26142
SUBJECT: GRB 191101A: VIRT Optical Upper Limits
DATE:    19/11/02 01:51:43 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

P. Gokuldass (UVI), D. Morris (UVI), N. Orange (OrangeWave Innovative
Science, LLC), A. Cucchiara (College of Marin), R. Strausbaugh (UVI) report:



We observed the field of GRB 191101A (A.P. Beardmore et al., GCN 26140;
P.A. Evans et al., GCN 26137, D'Ai et al., GCN 26135) with the 0.5m Virgin
Island Robotic Telescope (VIRT) on 11-01-2019 starting at 23:03:18 UT
(T+115m). We report on an initial series of exposures in Clear filter
totaling 110s with an observation midpoint of T+117m. The weather
conditions were very good during the hours of observation and the zenith
angle at the start of the observation was 63 degrees. We observed the Swift
XRT position with a 20'x20' field of view.



We find no new source at the Swift-XRT position and report a 3-sigma upper
limit of approximately V=17.0. The limit is estimated from comparison to
nearby USNO B1 stars and is not corrected for Galactic extinction. The VIRT
is still in the commissioning phase.



Observations and analysis are ongoing. This message can be cited.


GRB_name: GRB191101A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26144
SUBJECT: GRB 191101A: Swift-XRT refined Analysis
DATE:    19/11/02 06:34:50 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), M. Capalbi (INAF-IASFPA), M.
Perri (ASDC), V. D'Elia (ASDC), A. Tohuvavohu (U. Toronto), J.A. Kennea
(PSU) and A. D'Ai report on behalf of the Swift-XRT team:

We have analysed 7.9 ks of XRT data for GRB 191101A (D'Ai et al. GCN
Circ. 26135), from 92 s to 24.5 ks after the  BAT trigger. The data
comprise 190 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. 26137). The late-time light curve (from T0+4.8 ks) is
consistent with a constant source of mean count rate 4.8e+00 ct/sec. A
power-law fit gives an index of 0.18 (+0.22, -0.21).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.28 (+/-0.05). The
best-fitting absorption column is  9.9 (+1.2, -1.1) x 10^20 cm^-2, in
excess of the Galactic value of 1.3 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.08 (+0.15, -0.14)
and a best-fitting absorption column of 6.2 (+3.2, -2.9) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.1 x 10^-11 (3.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.2 (+3.2, -2.9) x 10^20 cm^-2
Galactic foreground: 1.3 x 10^20 cm^-2
Excess significance: 2.8 sigma
Photon index:      2.08 (+0.15, -0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00932742.

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


GRB_name: GRB191101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26145
SUBJECT: GRB 191101A: iTelescope optical limit
DATE:    19/11/02 10:01:01 GMT
FROM:    Albert Kong at NTHU  <akhkong@gmail.com>

A.K.H. Kong (NTHU, Taiwan) reports

We observed the field of GRB 191101A (D'Ai et al. GCN 26135) with the
T11 0.5m telescope of iTelescope.Net in New Mexico. The observation
was done with a luminance filter (400-700 nm) beginning at 2019-11-02
02:08:44 UT (5 hours after the trigger) for 300 sec. At the position
of the enhanced X-ray afterglow (Evans et al. GCN 26137), we do not
detect any optical emission with a detection limit of about 19.5 mag
by comparing with the Gaia DR2 catalogue.


GRB_name: GRB191031C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26146
SUBJECT: GRB 191031C: Insight-HXMT/HE detection
DATE:    19/11/02 15:20:49 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, C. Cai, S. Xiao, Q. B. Yi, Y. G. Zheng, Y. Huang, 
C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-10-31T18:43:16.00 (T0), Insight-HXMT/HE detected 
GRB 191031C (trigger ID: HEB191031780) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #26107) and 
Swift-BAT (GCN #26108). 

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 47.315 s measured from T0+0.74 s. 
The 1-ms peak rate, measured from T0+42.703 s, is 848 cnts/sec. 
The total counts from this burst is 11529 counts. The data of 
Insight-HXMT/HE suffers saturation in the brightest part.
URL_LC: http://www.hxmt.org/images/GRB/HEB191031780_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191031D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26147
SUBJECT: GRB 191031D: Gemini optical upper limit
DATE:    19/11/02 19:25:43 GMT
FROM:    Eleonora Troja at NASA/GSFC/UMD  <eleonora@umd.edu>

S.Dichiara (UMD, NASA-GSFC) and E. Troja (UMD, NASA-GSFC) report on behalf
of a larger collaboration:

We observed the field of the short duration GRB 191031D (Fermi GBM Team,
GCN Circ. 26111; D'Elia et al., GCN Circ. 26112) with the Gemini North
8-meter telescope located on Mauna Kea, beginning on 2019-11-02  04:43:08
UT, approximately 1.3 d post-burst. We obtained a series of 6x120s r-band
images using the Gemini Multi-Object Spectrograph (GMOS).

No credible counterpart is detected within the enhanced X-ray position
(Osborne el al., GCN 26117) down to r > 25 AB mag, not corrected for
Galactic extinction.

We thank S. Stewart and the Gemini North staff for executing these
observations.


GRB_name: GRB191031E
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26148
SUBJECT: GRB 191031E: Insight-HXMT/HE detection
DATE:    19/11/03 01:11:20 GMT
FROM:    QiBin Yi at IHEP, HXMT  <yiqb@ihep.ac.cn>

Q. B. Yi, S. Xiao, Q. Luo, C. Cai, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:

At 2019-10-31T07:39:03.00 (T0), Insight-HXMT/HE detected 
GRB 191031E (trigger ID: HEB191031318) in a routine search of the data, 
which was also triggered by INTEGRAL/SPI-ACS (Num #8401) and KONUS/WIND. 

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 9.83 s measured from T0-6.60 s. 
The 1-ms peak rate, measured from T0+0.03 s, is 1045 cnts/sec. 
The total counts from this burst is 6357 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB191031318_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191031D
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26149
SUBJECT: Konus-Wind observation of GRB 191031D: correction to GCN 26126
DATE:    19/11/03 11:15:05 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, on behalf of the Konus-Wind team:

Reported in Frederiks et al. 2019 (GCN Circ. 26126),
the KW spectral parameters and fluxes of short/hard GRB 191031D
are incorrect due to wrong instrument calibrations used.
The correct values are given below.

As observed by Konus-Wind, the burst had a fluence
of 5.72(-0.63,+0.69)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.016 s,
of 4.12(-0.72,+0.80)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst (measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 15 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.12(-0.18,+0.20)
and Ep = 735(-92,+112) keV (chi2 = 32/39 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.9
(chi2 =32/38 dof).

I apologize for possible inconvenience this may have caused.


GRB_name: GRB191031D
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26150
SUBJECT: GRB 191031D: Zwicky Transient Facility Follow-Up of a Swift Short GRB (Trigger 594249816/191031891)
DATE:    19/11/03 19:13:26 GMT
FROM:    Tomas Ahumada at U. of Maryland  <tahumada@astro.umd.edu>

TomÃ¡s Ahumada (UMD), Shreya Anand (Caltech), Michael W. Coughlin (Caltech),
S. Bradley Cenko (NASA GSFC), Eric C. Bellm (UW), Leo P. Singer (NASA
GSFC), Mansi M. Kasliwal (Caltech) on behalf of the ZTF and GROWTH
collaborations

We observed the localization region of the short GRB 191031D (trigger
594249816/191031891) detected by the Swift XRT, BAT and the Gamma-Ray Burst
Monitor (GBM) on the Fermi satellite with the Palomar 48 inch telescope
equipped with the 47 square degree Zwicky Transient Facility (ZTF) camera.
These observations are part of the ZTF public survey and serendipitously
covered the GRB localization. We obtained a series of g-band images
beginning at 02:48:56.6 UT on 2019 Nov 01 (5.4 hours after the burst
trigger time). This corresponds to ~68% of the probability enclosed in the
GBM localization region and the totality of the Swift region.

The images were processed through the ZTF reduction and image subtraction
pipelines at IPAC to search for potential counterparts. No
high-significance transients were identified by our pipeline in the area
observed.

The median 5 sigma upper limit for an isolated point source in our images
was g > 20.8 mag for these observations.

ZTF is a project led by PI S. R. Kulkarni at Caltech (see ATEL #11266
<http://www.astronomerstelegram.org/?read=11266>), and includes IPAC; WIS,
Israel; OKC, Sweden; JSI/UMd, USA; UW, USA; DESY, Germany; NRC, Taiwan; UW
Milwaukee, USA and LANL USA. ZTF acknowledges the generous support of the
NSF under AST MSIP Grant No 1440341. Alert distribution service provided by
DIRAC@UW. Alert filtering is being undertaken by the GROWTH marshal system,
supported by NSF PIRE grant 1545949.


GRB_name: GRB191101A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26164
SUBJECT: GRB 191101A: Swift/UVOT Upper Limits
DATE:    19/11/04 19:01:00 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

GRB 191101A: Swift/UVOT Upper Limits

S. J. LaPorte (PSU) 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 191101A
110 s after the BAT trigger (D'Ai et al., GCN Circ. 26135).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 26140)
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           110          259          147         >21.1
u_FC               268          517          246         >20.3
white              110         5863          589         >21.6
v                  597         1588          110         >19.6
b                  523         5658          294         >21.2
u                  268         5453          540         >20.9
w1                 646         5248          294         >19.3
m2                 622         5043          300         >19.8
w2                 573         1564          117         >19.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB191101A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26167
SUBJECT: GRB 191101A: Swift-BAT refined analysis
DATE:    19/11/04 21:44:54 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),  A. D'Ai (INAF-IASFPA),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), 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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 191101A (trigger #932742)
(D'Ai, et al., GCN Circ. 26135).  The BAT ground-calculated position is
RA, Dec = 251.845, 43.740 deg which is 
  RA(J2000)  =  16h 47m 22.8s 
  Dec(J2000) = +43d 44' 24.5" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 47%.

The mask-weighted light curve shows a single, rather weak pulse, extending from
~T-20 sec, peaking at T+0 sec, dropping sharply at T+25 sec, followed by low-level
extended emission out to ~T+140 sec.  T90 (15-350 keV) is 137.95 +- 22.83 sec 
(estimated error including systematics).

The time-averaged spectrum from T-20.97 to T+143.53 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.78 +- 0.18.  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-1.00 sec in the 15-150 keV band
is 1.3 +- 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/932742/BA/


GRB_name: GRB191031D
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26175
SUBJECT: GRB 191031D: Chandra upper limit 
DATE:    19/11/05 14:50:39 GMT
FROM:    Wen-fai Fong at Northwestern U  <wfong@northwestern.edu>

A. Rouco Escorial, W. Fong, (Northwestern), E. Berger (Harvard), and R. Margutti (Northwestern) report:

"We initiated observations of the location of the short-duration GRB191031D (Fermi-GBM et al., GCN 26111; D'Elia et al., GCN 26112; Mailyan et al., GCN 26118) with the Chandra X-ray Observatory on 2019 Nov 3.694 UT (mid-time of 16:39:42 UT), 2.8 days post-burst under Program 20500021 (ObsID 21302; PI: Berger). The effective exposure time is 19.8 ksec.

We do not detect an X-ray source within the enhanced XRT position (Osborne et al., GCN 26117), and calculate a 3-sigma limit of <4.5e-4 cps in the 0.5-10 keV energy range using the method described by Gehrels (1986). Applying the best-fit XRT spectral parameters, we calculate an unabsorbed flux limit of <6.0e-15 erg/s/cm^2 in the 0.3-10 keV energy range. 

Relative to the XRT light curve starting from t~900 sec post-burst, this constrains the late-time X-ray power-law decline to be alpha<-0.75 (where F~t^alpha).

We thank the Chandra staff for the rapid scheduling and execution of these observations."


GRB_name: GRB191016A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26176
SUBJECT: GRB191016A GROND observations
DATE:    19/11/05 15:45:33 GMT
FROM:    Patricia Schady at Swift  <p.schady@bath.ac.uk>

P. Schady (Univ. of Bath) and J. Bolmer (MPE Garching) report:


We observed the field of GRB 161019A (Swift trigger 929744; Gropp et al., GCN #26008) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).


Observations started at 04:19 UT on 2019-10-16, 10 min after the GRB trigger. They were performed at an average seeing of 1.7" and at an average airmass of 1.7.


We detect a bright point source in all optical and near-infrared filters consistent with the reported optical afterglow position (Watson et al., GCN #26010; Siegel et al., GCN #26024). Based on the first 3.3 min of total exposures in g'r'i'z'JHK, we estimate preliminary AB magnitudes of


g' = 16.81 +/- 0.03
r' = 16.33 +/- 0.03
i' = 15.84 +/- 0.04
z' = 15.51 +/- 0.04
J = 15.28 +/- 0.05
H = 14.80 +/- 0.05
K = 14.83 +/- 0.08


Given magnitudes are calibrated against SDSS and 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.09 in the direction of the burst (Schlafly & Finkbeiner 2011).

We acknowledge the excellent support provided by the telescope operator at La Silla.


GRB_name: GRB191106A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26177
SUBJECT: GRB 191106A: Swift detection of a burst
DATE:    19/11/06 14:27:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), M. G. Bernardini (INAF-OAB),
D. N. Burrows (PSU), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC),
P. A. Evans (U Leicester), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), S. J. LaPorte (PSU), A. Melandri (INAF-OAB),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 14:15:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191106A (trigger=933515).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 269.350, +46.052, which is 
   RA(J2000)c =  17h 57m 24s
   Dec(J2000) = +46d 03' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a few peaks
with a total duration of about 5 sec.  The peak count rate
was ~2800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 14:16:34.2 UT, 70.3 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 269.3349,
46.0346 which is equivalent to:
   RA(J2000)  = 17h 57m 20.38s
   Dec(J2000) = +46d 02' 04.7"
with an uncertainty of 2.4 arcseconds (radius, 90% containment). This
location is 73 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 (4.38 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4
(+4.05/-3.32) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
130 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 19.2 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 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.06. 

Burst Advocate for this burst is F. E. Marshall (marshall 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/)


GRB_name: GRB191106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26178
SUBJECT: GRB 191106A: MASTER optical observation 
DATE:    19/11/06 15:10:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tiurina,P.Balanutsa,A.Kuznetsov,V.Vladimirov, D. Vlasenko, I.Gorbunov,
D.Zimnukhov, A.Pozdnyakov, E.Minkina, V.Senik (Lomonosov Moscow State University, SAI,Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix Aguilar OAFA),
H. Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova(Irkutsk State University, API),
A. Tlatov, D. Dormidontov(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University),

MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)
started Swift GRB 191106A (Marshall et al. GCN 26177) alert observation 19 sec after at 2019-11-06 14:16:03 UT.

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory)
was pointed to the  GRB191106.59 19 sec after notice time (39 sec after trigger time)
  at 2019-11-06 14:16:03 UT at sunset (sun  altitude  is -8.5 deg.).

There is no OT with 5-sigma upper limit  14.0 mag at  2019-11-06 14:38:00UT.

Error-box galactic latitude b = 28 deg., longitude l = 73 deg.
The observations made on zenith distance = 27 deg.The moon (70 % bright part) is 26 deg. above the horizon.
The distance between  moon and  object is 87 deg.
The error-box can be observed till sunrise at 2019-11-07 03:49:40

MASTER-Amur was pointed to GRB 191106A 20 sec after notice time (41s after trigger time) 
at 2019-11-06 14:16:05 UT, but there are clouds.

The message may be cited.


GRB_name: GRB191106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26179
SUBJECT: GRB 191106A: BOOTES-4/MET optical limit
DATE:    19/11/06 15:57:20 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), C. Perez 
del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga), S. Guziy (Univ. 
of Nikolaev) and D. Xiong, Y. Fan, X. Zhao, J. Bai, C. Wang, Y. Xin 
(Yunnan National Astronomical Observatory) on behalf of a larger 
collaboration, report:

Following the detection of GRB 191106A by Swift (Marshall et al. GCNC 
26177), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical 
Observatory (China) gathered images starting at 14:21 UT (~5.7 min after 
trigger). No optical afterglow is found down to 20.7 mag (unfiltered 
images) within the Swift/XRT error box, consistent with the 
non-detections by Swift/UVOT (Marshall et al. GCNC 26177) and MASTER 
(Lipunov et al. GCNC 26178). Observations are ongoing.

We thank the staff at Lijiang Astronomical Observatory for their 
excellent support.


GRB_name: GRB191106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26180
SUBJECT: GRB 191106A: Mondy optical upper limit
DATE:    19/11/06 16:15:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), E. Klunko (ISTP), A. Pozanenko (IKI), E. Mazaeva (IKI), 
A. Volnova    report   on behalf of IKI-GRB-FuN:

We observed the field of  GRB 191106A (Marshall et al.  GCN 26177) with 
AZT-33IK telescope of Sayan observatory (Mondy) starting on Nov. 06 (UT) 
  14:24:30, i.e. ~11 minutes after GRB trigger.   We  do not detect any 
optical object in the XRT error circle  (Marshall et al.  GCN 26177). 
Preliminary photometry of the field  is following.

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

2019-11-06 14:24:30    0.03688    R      22*120  n/d      22.0


Photometry is based on the USNO-B2.0 nearby stars.


GRB_name: GRB191106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26190
SUBJECT: GRB 191106A: Swift-XRT refined Analysis
DATE:    19/11/06 21:28:30 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA),
A. Tohuvavohu (U. Toronto), J.A. Kennea (PSU), B. Sbarufatti (PSU) and
F.E. Marshall report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 191106A (Marshall et al.
GCN Circ. 26177), from 106 s to 13.2 ks after the  BAT trigger. The
data are entirely 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 = 269.3356, 46.0353 which is equivalent to:

RA (J2000): 17 57 20.55
Dec(J2000): +46 02 06.9

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=3.37 (+0.33, -0.30).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.6). The
best-fitting absorption column is  3.1 (+3.1, -2.1) x 10^21 cm^-2, in
excess of the Galactic value of 4.4 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 (5.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+3.1, -2.1) x 10^21 cm^-2
Galactic foreground: 4.4 x 10^20 cm^-2
Excess significance: 2.1 sigma
Photon index:      2.1 (+/-0.6)

If the light curve continues to decay with a power-law decay index of
3.37, the count rate at T+24 hours will be 7.4 x 10^-10 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.7 x
10^-20 (4.1 x 10^-20) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00933515.

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


GRB_name: GRB191106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26191
SUBJECT: GRB 191106A: NOT optical upper limit
DATE:    19/11/07 01:08:39 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu, D. Xu (NAOC), J. Viuho (NOT) report on behalf of a larger 
collaboration:

We observed the field of GRB 191106A (Marshall et al., GCN 26177) using 
the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. 
Observations started at 19:35:51 UT on 2019-11-06 (i.e., 3.35 hr after 
the BAT trigger), and 16x200s Sloan z-band frames were obtained.

No optical source is detected in our stacked image at the XRT position 
(Page et al., GCN 26190), down to a limiting magnitude of z > 22.0 at a 
mean time of 4.0 hr post-burst, calibrated with the nearby SDSS field.


GRB_name: GRB191106A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26198
SUBJECT: GRB 191106A: Swift-BAT refined analysis
DATE:    19/11/07 13:20:21 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. D. Barthelmy (GSFC), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), F. E. Marshall (NASA/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-61 to T+242 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 191106A (trigger #933515)
(Marshall et al., GCN Circ. 26177).  The BAT ground-calculated position is
RA, Dec = 269.356, 46.046 deg which is
   RA(J2000)  =  17h 57m 25.4s
   Dec(J2000) = +46d 02' 44.7"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 95%.

The mask-weighted light curve shows many overlapping pulses. The burst
emission
starts at ~T-1.3 s and ends at ~T+2.4 s. T90 (15-350 keV) is 3.42 +- 0.35
sec
(estimated error including systematics).

The time-averaged spectrum from T-1.31 to T+2.38 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.89 +- 0.17.  The fluence in the 15-150 keV band is 3.2 +- 0.3 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T-0.02 sec in the 15-150 keV band
is 1.1 +- 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/933515/BA/


GRB_name: GRB191106A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26199
SUBJECT: GRB 191106A: Swift/UVOT Upper Limits
DATE:    19/11/07 14:14:44 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S. R. Oates (U.Warwick) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191106A
132 s after the BAT trigger (Marshall et al., GCN Circ. 26177).
No optical afterglow consistent with the XRT position
(Page et al., GCN Circ. 26190) 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          4987         5137          147         >20.0
u_FC               132          381          246         >20.1
white             4987         6775          541         >21.0
v                  437         7186          549         >19.9
b                  387        12533         1264         >21.3
u                  132        11621         1631         >20.8
w1                 486         7510          464         >20.0
m2                 461         7391          510         >20.0
w2                 412        13245         1223         >20.6

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: GRB191108A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26200
SUBJECT: GRB 191108A: Fermi GBM Final Real-time Localization
DATE:    19/11/08 00:14:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 00:04:37 UT on 8 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191108A (trigger 594864282.595766 / 191108003).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 232.9, Dec = 10.8 (J2000 degrees, equivalent to J2000 15h 31m, 10d 48'), with a statistical uncertainty of 17.4 degrees.

The angle from the Fermi LAT boresight is 62.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191108003/quicklook/glg_skymap_all_bn191108003.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191108003/quicklook/glg_healpix_all_bn191108003.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191108003/quicklook/glg_lc_medres34_bn191108003.gif


GRB_name: GRB191106A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26201
SUBJECT: GRB 191106A: AstroSat CZTI detection
DATE:    19/11/08 12:52:56 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

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

Analysis of AstroSat CZTI data showed a weak detection of a GRB 191106A, which was also detected by Swift (Marshall F. E. et al., GCN # 26177), MASTER (Lipunov V. et al., GCN # 26178), BOOTES-4/MET (Hu Y.-D. et al., GCN # 26179), Mondy (Belkin S. et al., GCN # 26180), Swift-XRT (Page K. L. et al., GCN # 26190), NOT (Zhu Z. P. et al., GCN # 26191), Swift/BAT (Barthelmy S. D. et al., GCN # 26198) and Swift/UVOT (Oates S. R. et al., GCN # 26199).

The source was detected in the 40-200 keV energy range. The light curve showed single pulse of emission peaking at 2019-11-06 14:15:23.0 UT. The measured peak count rate associated with the burst is 134 cts/s above the background in the combined data of four quadrants, with a total of 408 cts. The local mean background count rate was 502 cts/s. Using cumulative rates, we measure a T90 of 3.6 s.

It was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191110A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26214
SUBJECT: GRB 191110A: Fermi GBM Final Real-time Localization
DATE:    19/11/10 14:16:45 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 14:05:34 UT on 10 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191110A (trigger 595087539.99285 / 191110587).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 260.2, Dec = 43.5 (J2000 degrees, equivalent to J2000 17h 20m, 43d 30'), with a statistical uncertainty of 9.5 degrees.

The angle from the Fermi LAT boresight is 25.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191110587/quicklook/glg_skymap_all_bn191110587.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191110587/quicklook/glg_healpix_all_bn191110587.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191110587/quicklook/glg_lc_medres34_bn191110587.gif


GRB_name: GRB191111A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26226
SUBJECT: GRB 191111A: Fermi GBM Final Real-time Localization
DATE:    19/11/11 08:54:44 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 08:44:29 UT on 11 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191111A (trigger 595154674.947684 / 191111364).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 189.3, Dec = -32.1 (J2000 degrees, equivalent to J2000 12h 37m, -32d 06'), with a statistical uncertainty of 3.7 degrees.

The angle from the Fermi LAT boresight is 72.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191111364/quicklook/glg_skymap_all_bn191111364.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191111364/quicklook/glg_healpix_all_bn191111364.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191111364/quicklook/glg_lc_medres34_bn191111364.gif


GRB_name: GRB191111B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26231
SUBJECT: GRB 191111B: Fermi GBM Final Real-time Localization
DATE:    19/11/11 13:17:30 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 13:07:10 UT on 11 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191111B (trigger 595170435.791792 / 191111547).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 239.4, Dec = -70.4 (J2000 degrees, equivalent to J2000 15h 57m, -70d 24'), with a statistical uncertainty of 4.0 degrees.

The angle from the Fermi LAT boresight is 34.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191111547/quicklook/glg_skymap_all_bn191111547.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191111547/quicklook/glg_healpix_all_bn191111547.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191111547/quicklook/glg_lc_medres34_bn191111547.gif


GRB_name: GRB191111B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26233
SUBJECT: GRB 191111B: BALROG localization (Fermi Trigger 595170435 / GRB 191111547)
DATE:    19/11/11 13:32:43 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
595170435 at 13:07:10 on 11 Nov. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 239.4+/-3.3 deg
Decl.(2000.0) = -68.8+/-1.4 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB191111547/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB191111547/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB191111547/json

                        


GRB_name: GRB191112A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26239
SUBJECT: GRB 191112A: Fermi GBM Final Real-time Localization
DATE:    19/11/12 09:01:31 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 08:51:18 UT on 12 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191112A (trigger 595241483.192484 / 191112369).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 164.4, Dec = -72.3 (J2000 degrees, equivalent to J2000 10h 57m, -72d 17'), with a statistical uncertainty of 5.5 degrees.

The angle from the Fermi LAT boresight is 150.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191112369/quicklook/glg_skymap_all_bn191112369.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191112369/quicklook/glg_healpix_all_bn191112369.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191112369/quicklook/glg_lc_medres34_bn191112369.gif


GRB_name: GRB191031D
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26240
SUBJECT: GRB 191031D: CALET Gamma-Ray Burst Monitor detection
DATE:    19/11/13 03:39:09 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

Y. Shimizu (Kanagawa U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (Waseda U), T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The short bright GRB 191031D (Swift detection: Ambrosi et al.,
GCN Circ. 26112, Sakamoto et al., GCN Circ. 26133;
Fermi GBM detection: Mailyan and Meegan, GCN Circ. 26118;
AGILE/MCAL observations: Ursi et al., GCN Circ. 26123;
Konus-Wind observation: Frederiks et al., GCN Circ. 26126, 26149;
AstroSat CZTI detection: Gaikwad et al., GCN Circ. 26129;
https://gcn.gsfc.nasa.gov/other/191031D.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 21:23:31.261 UTC
on 31 October 2019. The burst signal was seen by all CGBM detectors.
No real-time CGBM GCN notice was distributed about this trigger because
the real-time communication from the ISS was off (loss of signal).

The burst light curve shows a multi-peak structure which starts at T-0.168
sec, peaks at 0.008 sec and ends at T+0.192 sec. The T90 and T50 durations
measured by the SGM data are 0.240 +- 0.079 sec and 0.104 +- 0.008 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1256592147/

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


GRB_name: GRB191113A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26241
SUBJECT: GRB 191113A: Fermi GBM Final Real-time Localization
DATE:    19/11/13 14:02:49 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 13:52:44 UT on 13 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191113A (trigger 595345969.522208 / 191113578).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 298.1, Dec = 20.9 (J2000 degrees, equivalent to J2000 19h 52m, 20d 53'), with a statistical uncertainty of 5.8 degrees.

The angle from the Fermi LAT boresight is 72.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191113578/quicklook/glg_skymap_all_bn191113578.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191113578/quicklook/glg_healpix_all_bn191113578.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191113578/quicklook/glg_lc_medres34_bn191113578.gif


GRB_name: GRB191027A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26246
SUBJECT: GRB 191027A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/11/14 01:02:06 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

T. Tamura (Kanagawa U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (Waseda U), Y. Shimizu (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

GRB 191027A (Fermi GBM Final Real-time Localization: Fermi GBM Team,
GCN Circ. 26078; BALROG localization: Biltzinger et al., GCN Circ. 26079,
26096; IPN triangulation: Hurley et al., GCN Circ. 26087; Konus-Wind
observation: Ridnaia et al., GCN Circ. 26100;
https://gcn.gsfc.nasa.gov/other/191027A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 15:19:06.826 UTC
on 27 October 2019. The burst signal was seen by all CGBM detectors.

The burst light curve shows a FRED-like pulse which starts at T+0.6 sec,
peaks at T+0.9 sec and ends at T+3.0 sec. The T90 and T50 durations
measured by the SGM data are 1.9 +- 0.6 sec and 0.6 +- 0.3 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1256224690/

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


GRB_name: GRB191111A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26247
SUBJECT: GRB 191111A: Insight-HXMT/HE detection
DATE:    19/11/14 01:51:09 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, Q. Luo, C. Cai, Q. B. Yi, Y. G. Zheng, Y. Huang, 
C. K. Li, X. B. Li, G. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-11-11T08:44:29.95 (T0), Insight-HXMT/HE detected 
GRB 191111A (trigger ID: HEB191111364) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #26226). 

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 93.09 s measured from T0+0.24 s. 
The 1-ms peak rate, measured from T0+57.973 s, is 905 cnts/sec. 
The total counts from this burst is 22029 counts. The data of 
Insight-HXMT/HE suffers saturation in the brightest part.
URL_LC: http://www.hxmt.org/images/GRB/HEB191111364_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
normal mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191115A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26251
SUBJECT: Swift GRB191115A: Global MASTER-Net observations report
DATE:    19/11/15 11:39:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, 
A.Kuznetsov, F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva, 
D.Kuvshinov
(Lomonosov Moscow State University, SAI, Physics Department),

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

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

R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),

D. Buckley
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev, O.Ershova
(Irkutsk State University, API),

A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),

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




MASTER-Amur robotic telescope  (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical 
University) was pointed to the Swift GRB191115.48 (trigger No 937114,19h 
28m 42.96s , +38d 43m 48.0s, R=0.05) errorbox  43 sec after trigger time 
at 2019-11-15 11:27:04 UT, with upper limit up to  16.2 mag. The 
observations began at zenith distance = 44 deg. The sun  altitude  is 
-35.0 deg.

The galactic latitude b = 10 deg., longitude l = 72 deg.


Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1196549

We obtain a following upper limits.

Tmid-T0  |          Site       |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________

       49 |         MASTER-Amur |  P/ |    10 | 15.5 |
       67 |         MASTER-Amur |  P/ |    10 | 15.5 |
       90 |         MASTER-Amur |  P/ |    20 | 15.5 |
      118 |         MASTER-Amur |  P/ |    20 | 15.5 |
      152 |         MASTER-Amur |  P/ |    30 | 16.2 |


The observation and reduction will continue.
The message may be cited.


GRB_name: GRB191117A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26253
SUBJECT: GRB 191117A: Fermi GBM Final Real-time Localization
DATE:    19/11/17 00:19:41 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 00:08:28 UT on 17 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191117A (trigger 595642113.724042 / 191117006).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 297.9, Dec = 76.4 (J2000 degrees, equivalent to J2000 19h 51m, 76d 24'), with a statistical uncertainty of 9.1 degrees.

The angle from the Fermi LAT boresight is 39.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191117006/quicklook/glg_skymap_all_bn191117006.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191117006/quicklook/glg_healpix_all_bn191117006.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191117006/quicklook/glg_lc_medres34_bn191117006.gif


GRB_name: GRB191117B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26255
SUBJECT: GRB 191117B: Fermi GBM Final Real-time Localization
DATE:    19/11/17 15:28:00 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:17:38 UT on 17 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191117B (trigger 595696663.360798 / 191117637).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 156.1, Dec = 11.7 (J2000 degrees, equivalent to J2000 10h 24m, 11d 41'), with a statistical uncertainty of 7.4 degrees.

The angle from the Fermi LAT boresight is 54.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191117637/quicklook/glg_skymap_all_bn191117637.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191117637/quicklook/glg_healpix_all_bn191117637.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191117637/quicklook/glg_lc_medres34_bn191117637.gif


GRB_name: GRB191118A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26256
SUBJECT: GRB 191118A: Fermi GBM Final Real-time Localization
DATE:    19/11/18 22:19:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 22:12:01 UT on 18 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191118A (trigger 595807926.820754 / 191118925).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 214.0, Dec = -48.4 (J2000 degrees, equivalent to J2000 14h 16m, -48d 23'), with a statistical uncertainty of 2.2 degrees.

The angle from the Fermi LAT boresight is 105.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191118925/quicklook/glg_skymap_all_bn191118925.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191118925/quicklook/glg_healpix_all_bn191118925.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191118925/quicklook/glg_lc_medres34_bn191118925.gif


GRB_name: GRB191118A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26257
SUBJECT: GRB 191118A: BALROG localization (Fermi Trigger 595807926 / GRB 191118925)
DATE:    19/11/18 22:33:53 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
595807926 at 22:12:01 on 18 Nov. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 218.5+/-6.0 deg
Decl.(2000.0) = -49.3+/-3.3 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB191118925/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB191118925/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB191118925/json

                        


GRB_name: GRB191116A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26268
SUBJECT: GRB191116A: AstroSat CZTI detection of a short GRB
DATE:    19/11/22 09:11:41 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

V. Shenoy (IITB), Y. Sharma (Caltech), V. Bhalerao (IITB), 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 a strong detection of a short GRB 191119A.

The source was clearly detected in the 40-200 keV energy range. The light curve showed single pulse of emission peaking at 2019-11-19 10:41:04.0 UT. The measured peak count rate associated with the burst is 1798 cts/s above the background in the combined data of four quadrants, with a total of 338 cts. The local mean background count rate was 469 cts/s. Using cumulative rates, we measure a T90 of 0.23 s.

It was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

There is no event reported at this time in Fermi sub-threshold triggers list.

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: GRB191122A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26269
SUBJECT: GRB 191122A: Swift detection of a burst
DATE:    19/11/22 13:45:34 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

B. Sbarufatti (PSU), A. P. Beardmore (U Leicester), J.D. Gropp (PSU),
J. A. Kennea (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL),
S Laha (GSFC/UMBC/CRESST) and A. Tohuvavohu (U Toronto) report on
behalf of the Neil Gehrels Swift Observatory Team:

At 13:32:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191122A (trigger=938899).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 54.296, -32.176 which is 
   RA(J2000) = 03h 37m 11s
   Dec(J2000) = -32d 10' 32"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 50 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 13:34:31.1 UT, 94.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 54.26926,
-32.18602 which is equivalent to:
   RA(J2000)  = 03h 37m 04.62s
   Dec(J2000) = -32d 11' 09.7"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 89 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. 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 1.89e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 103 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
0.01. 

Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu). 
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/)


GRB_name: GRB191122A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26270
SUBJECT: GRB 191122A: Prompt enhanced Swift-XRT position
DATE:    19/11/22 14:05:22 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 191122A, we find an
enhanced XRT position of the afterglow: RA, Dec: 54.2703, -32.1864
which is equivalent to:
   RA (J2000)  = 03 37 04.86
   Dec (J2000) = -32 11 10.9
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/938899.

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: GRB191122A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26271
SUBJECT: GRB 191122A: CHES Optical Observations 
DATE:    19/11/22 16:50:23 GMT
FROM:    Tianrui Sun at Purple Mountain Obs,CAS  <trsun@pmo.ac.cn>

Tianrui Sun, Chen Zhang, Yiding Ping, Xuefeng Wu (PMO).

We report the observations for the GRB191122A (B. Sbarufatti et al., GCN Circ 26269).
We use the 80cm telescope of CHanging Event Survey at the YaoAn observation station(101.1811E, 25.528N) in Yunnan Province, China. 

Our observation starts at  13:48:57 UT and ends at 13:54:24 UT Nov 22, 2019, with five exposure 60 seconds in white filter.
We do not detect any candidate sources in the combined image in the enhanced XRT position error region to a 5 sigma limit at 18.31 generated from G band magnitude in Gaia DR2 .


GRB_name: GRB191122A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26272
SUBJECT: GRB 191122A: Enhanced Swift-XRT position
DATE:    19/11/22 21:05:05 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 4899 s of XRT Photon Counting mode data and 11 UVOT
images for GRB 191122A, 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 = 54.26986, -32.18665 which is equivalent
to:

RA (J2000): 03h 37m 4.77s
Dec (J2000): -32d 11' 11.9"

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: GRB191122A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26273
SUBJECT: GRB 191122A: BOOTES-4/MET optical limit
DATE:    19/11/22 21:54:26 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), C. Perez 
del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga),  S. Guziy 
(Univ. of Nikolaev) and D. Xiong, Y. Fan, X. Zhao, J. Bai, C. Wang, Y. 
Xin (Yunnan Nacional Astronomical Observatory) on behalf of a larger 
collaboration, report:

Following the detection of GRB 191122A by Swift (Sbarufatti et al. GCNC 
26269), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical 
Observatory (China) started to gather images at 13:34 UT (~94s after 
trigger). No optical afterglow is found down to 20.3 mag (unfiltered 
images) at the enhaced Swift/XRT position (Evans et al. GCNC 26270), 
consistent with the non-detections by Swift/UVOT (Sbarufatti et al. GCNC 
26269) and CHES (Sun et al. GCNC 26271). Observations are ongoing."

We thank the staff at Lijiang Astronomical Observatory for their 
excellent support.


GRB_name: GRB191122A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26274
SUBJECT: GRB 191122A: Swift-XRT refined Analysis
DATE:    19/11/22 22:21:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.8 ks of XRT data for GRB 191122A (Sbarufatti et al.
GCN Circ. 26269), from 301 s to 23.9 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN Circ. 26270).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.97 (+0.26, -0.31). At T+746 s  the decay
steepens to an alpha of 1.94 (+0.26, -0.10) before breaking again at
T+6109 s to a final decay with index alpha=-0.1 (+/-0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.06 (+0.04, -0.03). The
best-fitting absorption column is  consistent with the Galactic value
of 1.0 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.12 (+0.08, -0.07) and a best-fitting absorption
column consistent with the Galactic value. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 5.6 x 10^-11 (5.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      10.0 (+15.8, -0.0) x 10^19 cm^-2
Galactic foreground: 1.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.12 (+0.08, -0.07)

If the light curve continues to decay with a power-law decay index of
-0.1, the count rate at T+24 hours will be 0.067 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.8 x
10^-12 (3.8 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/00938899.

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


GRB_name: GRB191122A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26275
SUBJECT: GRB 191122A: Swift-BAT refined analysis
DATE:    19/11/22 23:46:51 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),  S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), B. Sbarufatti (PSU), 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 191122A (trigger #938899)
(Sbarufatti, et al., GCN Circ. 26269).  The BAT ground-calculated position is
RA, Dec = 54.290, -32.176 deg which is 
   RA(J2000)  =  03h 37m 09.7s 
   Dec(J2000) = -32d 10' 35.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 26%.

The mask-weighted light curve shows a single FRED-shaped pulse rising from 
T-20 sec to T+0 sec, then decaying out to roughly T+250 sec.
T90 (15-350 keV) is 153.3 +- 38.3 sec (estimated error including systematics).

The time-averaged spectrum from -11.2 to 245.4 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.24 +- 0.28, 
and Epeak of 89.2 +- 41.9 keV (chi squared 69.11 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.6 +- 0.3 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+6.44 sec in the 15-150 keV band is
3.1 +- 0.4 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.67 +- 0.07 (chi squared 76.48 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/938899/BA/


GRB_name: GRB191122A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26277
SUBJECT: GRB 191122A: Swift/UVOT Upper Limits
DATE:    19/11/23 01:05:16 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and B. Sbarufatti (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191122A
104 s after the BAT trigger (Sbarufatti et al., GCN Circ. 26269).
No optical afterglow consistent with the XRT position
(Evans GCN Circ. 26270,26272)
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           104          253          147         >21.1
u_FC               316          566          246         >20.4
white              104        11801         1305         >22.0
v                  647         6097          432         >20.2
b                  572        10938         1121         >21.9
u                  316         6696          642         >20.5
w1                 696         6508          413         >20.1
m2                 846         6303          413         >21.2
w2                 797         5893          413         >20.1

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: GRB191118A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26278
SUBJECT: GRB 191118A: Insight-HXMT/HE detection
DATE:    19/11/23 02:46:16 GMT
FROM:    YaoGuang Zheng at IHEP  <zhengyg@ihep.ac.cn>

Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-11-18T22:12:01.82 (T0), Insight-HXMT/HE detected 
GRB 191118A (trigger ID: HEB191118925) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #26256).

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 15.71 s measured from T0+0.12 s. 
The 1-ms peak rate, measured from T0+7.85 s, is 928 cnts/sec. 
The total counts from this burst is 7570 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB191118925_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191123A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26279
SUBJECT: GRB 191123A: Swift detection of a burst with an optical counterpart
DATE:    19/11/23 11:05:32 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaronb@swift.psu.edu>

A. Tohuvavohu (U Toronto), J.D. Gropp (PSU), A. Y. Lien (GSFC/UMBC),
K. L. Page (U Leicester) and B. Sbarufatti (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 10:38:44 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191123A (trigger=939079).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 215.261, +22.842 which is 
   RA(J2000) = 14h 21m 03s
   Dec(J2000) = +22d 50' 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 150 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 10:39:54.1 UT, 69.8 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find an uncatalogued X-ray source with an enhanced position: RA, Dec
215.2619, 22.8600 which is equivalent to:
   RA(J2000)  = 14h 21m 02.87s
   Dec(J2000) = +22d 51' 36.0"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 64 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 (3.01 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.9
(+2.28/-2.01) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 78 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 14:21:02.87 = 215.26196
  DEC(J2000) = +22:51:36.3  =  22.86008
with a 90%-confidence error radius of about 0.75 arc sec. This position is 9.7
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.13 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.04. 

Burst Advocate for this burst is A. Tohuvavohu (aaronb AT swift.psu.edu). 
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/)


GRB_name: GRB191123A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26282
SUBJECT: GRB 191123A: Swift/UVOT detection
DATE:    19/11/23 16:12:05 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and A. Tohuvavohu (U Toronto)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of
GRB 191123A  78 s after the BAT trigger (Tohuvavohu et al.,
GCN Circ. 26279). A candidate optical afterglow was
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         78          228          147     18.26+-0.07
u_FC            290          540          246    >19.89
white           869         1019          147     19.28+-0.13

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: GRB191123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26283
SUBJECT: GRB 191123A: iTelescope optical upper limits
DATE:    19/11/23 16:55:37 GMT
FROM:    Filipp Dmitrievich Romanov at Amateur astronomer  <filipp.romanov.27.04.1997@gmail.com>

I observed the field of GRB 191123A (Tohuvavohu et al., GCN Circular 26279)
with remote telescope T21 (0.43-m f/6.8 reflector + CCD + f/4.5 focal
reducer) of iTelescope.Net in New Mexico Observatory. Two images with a
luminance filter and with 120 seconds exposure time were obtained on
2019-11-23. Average time of images: 12:13:54 UT (5710 seconds after
trigger; Binx1) and 12:16:38 UT (5874 seconds after trigger; Binx2). I did
not detect any optical transients (magnitude limit of about 19.0 G from
Gaia DR2 catalogue).


GRB_name: GRB191123A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26284
SUBJECT: GRB 191123A: Enhanced Swift-XRT position
DATE:    19/11/23 18:35:33 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 1802 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 191123A, 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 = 215.26186, +22.85991 which is equivalent
to:

RA (J2000): 14h 21m 2.85s
Dec (J2000): +22d 51' 35.7"

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: GRB191123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26285
SUBJECT: GRB 191123A: Swift-XRT refined Analysis
DATE:    19/11/23 20:52:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), A. D'Ai (INAF-IASFPA), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), B. Sbarufatti (PSU), D.N. Burrows
(PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester) and A. Tohuvavohu report on behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 191123A (Tohuvavohu et al.
GCN Circ. 26279), from 76 s to 18.5 ks after the  BAT trigger. The data
comprise 540 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN Circ. 26284).

The late-time light curve (from T0+5.6 ks) can be modelled with a
power-law decay with a decay index of alpha=1.00 (+/-0.15).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.52 (+/-0.05). The
best-fitting absorption column is  6.7 (+1.6, -1.5) x 10^20 cm^-2, in
excess of the Galactic value of 3.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.98 (+0.12, -0.11)
and a best-fitting absorption column of 4.8 (+2.6, -1.8) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (3.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.8 (+2.6, -1.8) x 10^20 cm^-2
Galactic foreground: 3.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.98 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
1.00, the count rate at T+24 hours will be 0.022 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.2 x
10^-13 (8.1 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/00939079.

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


GRB_name: GRB191123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26286
SUBJECT: GRB 191123A: Swift-BAT refined analysis
DATE:    19/11/23 22:52:53 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),  
A. Tohuvavohu (U Toronto), 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 191123A (trigger #939079)
(Tohuvavohu, et al., GCN Circ. 26279).  The BAT ground-calculated position is
RA, Dec = 215.289, 22.823 deg which is 
  RA(J2000)  =  14h 21m 09.3s 
  Dec(J2000) = +22d 49' 23.5" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-weighted light curve shows a pair of pulses, each with some sub-
structure.  The first starts at ~T-10 sec, peaks at T+0 and decays by T+40 sec.
The second pulse starts at T+110 sec, peaks soon afterward and decays by 
T+180 sec.  T90 (15-350 keV) is 275.1 +- 102.4 sec (estimated error including 
systematics).

The time-averaged spectrum from -2.1 to 288.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.67 +- 0.25.  The fluence in the 15-150 keV band is 1.2 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+111.77 sec in the 15-150 keV band
is 1.2 +- 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/939079/BA/


GRB_name: GRB191123A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26287
SUBJECT: GRB 191123A: Swift/UVOT further analysis
DATE:    19/11/24 00:57:25 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and A. Tohuvavohu (U. Toronto)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191123A
78 s after the BAT trigger (Tohuvavohu et al., GCN Circ. 26279).
A source consistent with the XRT position (Goad et al. GCN Circ. 26284)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  14:21:02.88 = 215.26200 (deg.)
    Dec (J2000) = +22:51:36.1  =  22.86002 (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:

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

white               78          228          147         18.25 +/- 0.05
v                  620         2111          175         18.28 +/- 0.19
b                  546         1168           58         19.18 +/- 0.25
u                  290         6376          501        >20.4
w1                 669         6171          372        >19.9
m2                1074         5966          216        >19.8
w2                 595        12186          944        >20.9

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: GRB191125A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26292
SUBJECT: GRB 191125A: Fermi GBM Final Real-time Localization
DATE:    19/11/25 05:07:00 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 04:56:43 UT on 25 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191125A (trigger 596350608.13565 / 191125206).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 243.1, Dec = -13.1 (J2000 degrees, equivalent to J2000 16h 12m, -13d 05'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 71.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191125206/quicklook/glg_skymap_all_bn191125206.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191125206/quicklook/glg_healpix_all_bn191125206.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191125206/quicklook/glg_lc_medres34_bn191125206.gif


GRB_name: GRB191125B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26293
SUBJECT: GRB 191125B: Fermi GBM Final Real-time Localization
DATE:    19/11/25 15:23:58 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:12:45 UT on 25 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191125B (trigger 596387570.686402 / 191125634).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 353.5, Dec = 18.2 (J2000 degrees, equivalent to J2000 23h 33m, 18d 11'), with a statistical uncertainty of 4.1 degrees.

The angle from the Fermi LAT boresight is 66.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191125634/quicklook/glg_skymap_all_bn191125634.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191125634/quicklook/glg_healpix_all_bn191125634.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191125634/quicklook/glg_lc_medres34_bn191125634.gif


GRB_name: GRB191125B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26299
SUBJECT: GRB 191125B: MASTER-VWFC synchronous observation 
DATE:    19/11/27 18:43:59 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, K.Zhirkov, F.Balakin, V.Vladimirov,
A.Kuznetsov, N.Tiurina, P.Balanutsa,A.Kuznetsov,V.Vladimirov, D. Vlasenko, I.Gorbunov,
D.Zimnukhov, A.Pozdnyakov, E.Minkina, V.Senik (Lomonosov Moscow State University, SAI,Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix Aguilar OAFA),
H. Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova(Irkutsk State University, API),
A. Tlatov, D. Dormidontov(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University),

MASTER Global Robotic Net (http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)
consists of 8 robotic telescopes with identical equipment (MASTER-Amur, 
-Tunka,-Ural, -Kislovodsk, -Tavrida, -SAAO, -IAC, -OAFA),
including wide field (twin MASTER telescopes with 2x8sq.deg. field of view)
and very wide field optical channels.

MASTER-Amur very wide field cameras(d=60 mm, FOV = 2x384 sq. degree) 
synchronously observed Fermi GRB191125B (GCN 26293) position before, 
during and after trigger time.
The synchronous images are available here:
http://master.sai.msu.ru/static/MASTER_FERMI_GRB191125B.gif
where 
Fermi team (GCN 26293) localization with systematical uncertainty
and
  BALROG localization (ApJ, 873,60, 2019) of GRB 191125B are at MASTER wide field cameras image.

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station)
started inspect of the Fermi GRB191125.63 
errorbox  321 sec after notice time and 473 sec after trigger time at 
2019-11-25 15:20:39 UT.

No optical transients were found (Lipunov et al. GCN 26294).

Real time updated cover map and OT discovered available here:
http://master.sai.msu.ru/site/master2/observ.php?id=1206143

The message may be cited.


GRB_name: GRB191129A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26301
SUBJECT: GRB 191129A: Fermi GBM Final Real-time Localization
DATE:    19/11/29 03:32:46 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 03:22:27 UT on 29 Nov 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191129A (trigger 596690552.12649 / 191129141).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 8.9, Dec = 5.4 (J2000 degrees, equivalent to J2000 00h 35m, 5d 24'), with a statistical uncertainty of 2.5 degrees.

The angle from the Fermi LAT boresight is 110.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191129141/quicklook/glg_skymap_all_bn191129141.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191129141/quicklook/glg_healpix_all_bn191129141.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191129141/quicklook/glg_lc_medres34_bn191129141.gif


GRB_name: GRB191129A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26316
SUBJECT: GRB 191129A: AstroSat CZTI detection
DATE:    19/11/30 10:35:03 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 191129A, which was also detected by Fermi GBM Real-time Localization (GCN # 26301)and Global MASTER-Net (Lipunov V. et al., GCN # 26302).

The source was clearly detected in the 40-200 keV energy range. The light curve showed single peak of emission peaking at 2019-11-29 03:22:27.0 UT. The measured peak count rate associated with the burst is 640 cts/s above the background in the combined data of four quadrants, with a total of 8062 cts. The local mean background count rate was 412 cts/s. Using cumulative rates, we measure a T90 of 26.6 s. In preliminary analysis, we find that 538 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191201A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26322
SUBJECT: GRB 191201A: AstroSat CZTI detection
DATE:    19/12/02 09:08:53 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

R. Gaikwad, S. Gupta, V. Sharma, A. Vibhute and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a GRB 191201A.

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with strongest peak at 2019-12-01 14:54:37.0 UT. The measured peak count rate associated with the burst is 444 cts/s above the background in the combined data of four quadrants, with a total of 5986 cts. The local mean background count rate was 645 cts/s. Using cumulative rates, we measure a T90 of 26.85 s. In preliminary analysis, we find that 491 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191202A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26323
SUBJECT: GRB 191202A: Fermi GBM Final Real-time Localization
DATE:    19/12/02 20:59:08 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 20:48:51 UT on 2 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191202A (trigger 597012536.229574 / 191202867).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 245.3, Dec = 16.8 (J2000 degrees, equivalent to J2000 16h 21m, 16d 48'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 15.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191202867/quicklook/glg_skymap_all_bn191202867.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191202867/quicklook/glg_healpix_all_bn191202867.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191202867/quicklook/glg_lc_medres34_bn191202867.gif


GRB_name: GRB191004A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26324
SUBJECT: GRB 191004A: correction to reported GROND upper limits
DATE:    19/12/02 22:48:59 GMT
FROM:    Patricia Schady at Swift  <p.schady@bath.ac.uk>

P. Schady (Univ. of Bath) reports:

I would like to correct a mistake in the GROND g'r'i'z' upper limits reported in Schady et al. (GCN #25959). The reported afterglow position (Osborne et al., GCN #25950; Lipunov et al., GCN #25944) lay at the edge of the g'r'i'z' field of view, where the exposure coverage is not complete. Taking into account the exposure map reduces the optical band 3 sigma upper limits reported in GCN #25959 by around 0.5 mag. The correct 3 sigma upper limits (AB system) are as follows:

g > 23.3
r > 23.7
i > 23.1
z > 22.7

I would like to thank Jochen Greiner for bringing this mistake to my attention.


GRB_name: GRB191203A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26325
SUBJECT: GRB 191203A: Fermi GBM Final Real-time Localization
DATE:    19/12/03 07:07:43 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 06:57:19 UT on 3 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191203A (trigger 597049044.076016 / 191203290).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 332.4, Dec = 51.8 (J2000 degrees, equivalent to J2000 22h 09m, 51d 47'), with a statistical uncertainty of 34.2 degrees.

The angle from the Fermi LAT boresight is 15.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191203290/quicklook/glg_skymap_all_bn191203290.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191203290/quicklook/glg_healpix_all_bn191203290.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191203290/quicklook/glg_lc_medres34_bn191203290.gif


GRB_name: GRB191202A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26326
SUBJECT: GRB 191202A: AstroSat CZTI detection
DATE:    19/12/03 07:19:56 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 191202A, which was also detected by Fermi GBM Final Real-time Localization (GCN #26323).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with strongest peak at 2019-12-02 20:48:51 UT. The measured peak count rate associated with the burst is 829 cts/s above the background in the combined data of four quadrants, with a total of 3809 cts. The local mean background count rate was 499 cts/s. Using cumulative rates, we measure a T90 of 11.92 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191130A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26327
SUBJECT: GRB 191130A, a long burst detected in Swift-BAT ground analysis
DATE:    19/12/03 15:22:09 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

At 13:05:02 UT on 2019-11-30, GRB 191130A occurred during a
preplanned slew of the Neil Gehrels Swift Observatory and was
later found in the Swift/BAT ground analysis.

Using the data set from T-139 to T+106 sec from the recent telemetry
downlink (observation ID: 03110538005),
the BAT ground-calculated position is
RA, Dec = 133.137, 5.017 deg which is
   RA(J2000)  =  08h 52m 32.9s
   Dec(J2000) = +05d 01' 02.1"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).

The mask-weighted light curve shows a single-pulse structure that starts
at ~T0, peaks at ~T+7 s, and ends at ~T+22 s. T90 (15-350 keV)
is 17.6 +- 2.9 sec (estimated error including systematics).

The time-averaged spectrum from T-0.0 to T+22.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.13.  The fluence in the 15-150 keV band is 6.86 +- 0.6 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+6.18 sec in the 15-150 keV band
is 1.1 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
https://swift.gsfc.nasa.gov/results/BATbursts/GRB191130A/03110538005/bascript/top.html


GRB_name: GRB191202A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26329
SUBJECT: GRB 191202A: Fermi GBM observation
DATE:    19/12/03 17:48:19 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres and C. Meegan (both UAH)
report on behalf of the Fermi GBM Team:

"At 20:48:51.23 UT on 2 December 2019, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 191202A (trigger 597012536 / 191202867)
which was also detected by the Fermi-LAT.
The GBM on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger time is 12
degrees.

The GBM light curve shows two pulses
with a duration (T90) of about 30.7 s (50-300 keV).
The time-averaged spectrum from T0-1.0 s to T0+18.4 s is
best fit by a Band function with Epeak = 190 +/- 19 keV,
alpha = -1.20 +/- 0.04, and beta = -2.05 +/- 0.08.

The event fluence (10-1000 keV) in this time interval is
(1.95 +/- 0.04)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+9.0 s in the 10-1000 keV band
is 23.5 +/- 0.4 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB191202A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26330
SUBJECT: GRB 191202A: Fermi-LAT detection
DATE:    19/12/03 20:04:05 GMT
FROM:    Lorenzo Scotton at CNRS/IN2P3/LUPM  <lorenzoscotton@live.it>

D. Kocevski (NASA/GSFC), R. Angioni (ASI/SSDC and INFN, Roma2), F. Longo (University and INFN, Trieste),

N. Omodei (Stanford University), E. Bissaldi (Politecnico and INFN, Bari) and L. Scotton (CNRS/IN2P3/LUPM, Montpellier)

report on behalf of the Fermi-LAT Collaboration:


On December 2nd, 2019, Fermi-LAT detected high-energy emission from

GRB 191202A, which was also detected by Fermi-GBM (trigger 597012536/191202867) (Veres et al. 2019, GCN 26329).


The best LAT on-ground location is found to be


RA, Dec = 249.54, 17.56 (degrees, J2000)


with an error radius of 0.24 deg (90% containment, statistical error only).

This was 11.4 deg from the LAT boresight at the time of the GBM trigger:


T0 = 20:48:51.23 UT.


The data from the Fermi-LAT show a significant increase
in the event rate after the GBM trigger that is spatially correlated with the
GBM emission with high significance.
The photon flux above 100 MeV in the time interval 0-1000s after the
GBM trigger is 2.6e-06 +/- 8.8e-07 ph/cm2/s.



The estimated photon index above 100 MeV is -1.6 +/- 0.2.




The highest-energy photon is a 1.8 GeV event which is observed 393 seconds

after the GBM trigger.


The Fermi-LAT point of contact for this burst is

Lorenzo Scotton (lorenzo.scotton@lupm.in2p3.fr).



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: GRB191130A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26331
SUBJECT: GRB 191130A: Swift ToO observations
DATE:    19/12/04 08:16:15 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 Swift/BAT GRB 191130A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00020950

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 Swift/BAT 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: GRB191202A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26344
SUBJECT: Konus-Wind observation of GRB191202A
DATE:    19/12/05 16:23:17 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration GRB191202A (AstroSat CZTI detection: Gaikwad et al., 
GCN 26326;
Fermi GBM observation: Veres & Meegan, GCN 26329;
Fermi-LAT detection: Kocevski et al., GCN 26330)
triggered Konus-Wind at T0=74930.521 s UT (20:48:50.521).

The burst light curve shows a multi-peaked structure
which starts at ~T0-3.9 s and has a total duration of~17.6 s.
The emission is seen up to ~1.3 MeV.

As observed by Konus-Wind, the burst
had a fluence of 2.78(-0.68,+0.76)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+7.024 s,
of 8.80(-2.80,+3.04)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+15.872 s)
is best fit in the 20 keV - 1.3 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.22(-0.12,+0.22),
the high energy photon index beta = -2.17(-1.00,+0.26),
the peak energy Ep = 265(-87,+91) keV,
chi2 = 46/59 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191202_T74930/

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


GRB_name: GRB191130A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26346
SUBJECT: GRB 191130A: Swift-XRT observations
DATE:    19/12/05 17:22:42 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

B. Sbarufatti (PSU) ), J. D. Gropp (PSU) and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the
Swift/BAT-detected burst GRB 191130A (Palmer et al. GCN Circ. 26327),
collecting 5.0 ks of Photon Counting (PC) mode data between T0+310.0 ks
and T0+343.5 ks. 

Three uncatalogued sources were detected, all of them too far from the
GRB position to be likely afterglow candidates.

The 3-sigma upper limit at the BAT position is 1.19e-3 ct s^-1,
corresponding to a 0.3-10 keV observed flux of 6.0e-14 erg cm^-2 s^-1
(assuming a typical GRB spectrum).

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00020950.

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


GRB_name: GRB191205A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26347
SUBJECT: GRB 191205A: Fermi GBM Final Real-time Localization
DATE:    19/12/05 17:56:26 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 17:46:20 UT on 5 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191205A (trigger 597260785.441392 / 191205741).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 14.0, Dec = -34.2 (J2000 degrees, equivalent to J2000 00h 56m, -34d 12'), with a statistical uncertainty of 21.4 degrees.

The angle from the Fermi LAT boresight is 42.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191205741/quicklook/glg_skymap_all_bn191205741.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191205741/quicklook/glg_healpix_all_bn191205741.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191205741/quicklook/glg_lc_medres34_bn191205741.gif


GRB_name: GRB191202A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26370
SUBJECT: GRB 191202A: Insight-HXMT/HE detection
DATE:    19/12/07 01:58:48 GMT
FROM:    YaoGuang Zheng at IHEP  <zhengyg@ihep.ac.cn>

Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-12-02T20:48:59.55 (T0), Insight-HXMT/HE detected 
GRB 191202A (trigger ID: HEB191202867) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #26323), 
AstroSat CZTI (GCN #26326) and Konus-Wind (GCN #26344).

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 11.09 s measured from T0-5.67 s. 
The 1-ms peak rate, measured from T0-0.08 s, is 2101 cnts/sec. 
The total counts from this burst is 5960 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB191202867_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191203A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26371
SUBJECT: GRB 191203A: Insight-HXMT/HE detection
DATE:    19/12/07 02:00:51 GMT
FROM:    YaoGuang Zheng at IHEP  <zhengyg@ihep.ac.cn>

Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-12-03T06:57:19.08 (T0), Insight-HXMT/HE detected 
GRB 191203A (trigger ID: HEB191203289) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #26325).

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 0.27 s measured from T0-0.30 s. 
The 1-ms peak rate, measured from T0-0.10 s, is 2238 cnts/sec. 
The total counts from this burst is 339 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB191203289_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191105B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26376
SUBJECT: GRB191105B: AstroSat CZTI detection
DATE:    19/12/07 06:51:58 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 191105B.

The source was detected in the 40-200 keV energy range. The light curve showed multiple pulses of emission with the strongest peak at 2019-11-05 06:16:40 UT. The measured peak count rate associated with the burst is 497 cts/s above the background in the combined data of four quadrants, with a total of 3491 cts. The local mean background count rate was 755 cts/s. Using cumulative rates, we measure a T90 of 19.0 s.

It was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191102A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26378
SUBJECT: GRB191102A: AstroSat CZTI discovery of a burst
DATE:    19/12/07 06:56:21 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

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

Analysis of AstroSat CZTI data showed detection of a GRB 191102A.

The source was detected in the 40-200 keV energy range. The light curve showed single pulse of emission peaking at 2019-11-02 12:18:21 UT. The measured peak count rate associated with the burst is 198 cts/s above the background in the combined data of four quadrants, with a total of 634 cts. The local mean background count rate was 573 cts/s. Using cumulative rates, we measure a T90 of 4.4 s.

It was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191207A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26385
SUBJECT: GRB 191207A: Possible GRB detected in Fermi-LAT blind search
DATE:    19/12/09 16:46:27 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

G. Vianello (Stanford Univ.), M. Axelsson (KTH & Stockholm Univ.), N. Omodei (Stanford Univ.), M. Arimoto (Kanazawa Univ.), D. Kocevski (NASA/MSFC), J. McEnery (NASA/GSFC), J. Racusin (NASA/GSFC), P. Veres (UAH), F. Longo (University & INFN, Trieste), E. Bissaldi (Politecnico and INFN Bari) and S. Cutini (INFN Perugia) report on behalf of the Fermi-LAT team:

A blind search of Fermi-LAT data from December 7, 2019, discovered a potential GRB at time T0 = 2019-12-07 16:19:01 UT. The transient is detected slightly above the 5 sigma threshold during an interval from T0 to T0 + 50s.

The best LAT on-ground location is found to be

RA, Dec =  237.1, -55.5 (degrees, J2000)

with an error radius of 0.52 deg (90% containment, statistical error only).

The position is in the Galactic plane, and was 52 deg from the LAT boresight at the time of the trigger time, and 65 degrees from the spacecraft zenith.

A power-law fit gives a spectral index of -2.0 +/- 0.3, and the highest-energy photon is a 1.3 GeV event, which is observed at T0 + 49s.

Further analysis is ongoing.

The Fermi-LAT point of contact for this burst is Sara Cutini (sara.cutini@pg.infn.it<mailto:sara.cutini@pg.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: GRB191210A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26389
SUBJECT: Possible HAWC-detected GRB 191210A: Swift-XRT observations
DATE:    19/12/11 16:46:56 GMT
FROM:    Valerio D'Elia at ASDC  <valerio.delia@ssdc.asi.it>

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

Swift-XRT has performed follow-up observations of the possible
HAWC-detected burst GRB 191210A
(https://gcn.gsfc.nasa.gov/notices_amon_hawc/9066_1171.amon) in a
series of observations tiled on the sky. The total exposure time is 8.1
ks, distributed over 20 tiles; the maximum exposure at a single sky
location was 948 s. The data were collected between T0+7.0 ks and
T0+30.1 ks, and are entirely in Photon Counting (PC) mode. 

Four 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 1:
  RA (J2000):  210.3973  =  14:01:35.35
  Dec (J2000): -0.7503  =  -00:45:01.1
  Error: 10.2 arcsec (radius, 90% conf.)
  Count-rate: (3.8 [+6.0, -2.9])e-3 ct s^-1   
  Distance: 3115 arcsec from HAWC position.

Source 2:
  RA (J2000):  210.1243  =  14:00:29.84
  Dec (J2000): -1.3003  =  -01:18:01.1
  Error: 10.5 arcsec (radius, 90% conf.)
  Count-rate: 0.019 [+0.017, -0.011] ct s^-1   
  Distance: 2561 arcsec from HAWC position.

Source 4:
  RA (J2000):  211.3249  =  14:05:17.98
  Dec (J2000): -1.9738  =  -01:58:25.8
  Error: 6.0 arcsec (radius, 90% conf.)
  Count-rate: 0.0139 [+0.0102, -0.0069] ct s^-1   
  Distance: 2502 arcsec from HAWC position.

Source 5:
  RA (J2000):  210.6745  =  14:02:41.89
  Dec (J2000): -1.9321  =  -01:55:55.6
  Error: 8.4 arcsec (radius, 90% conf.)
  Count-rate: 0.0110 [+0.0081, -0.0054] ct s^-1   
  Distance: 1572 arcsec from HAWC position.

A catalogued source was 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 https://www.swift.ac.uk/xrt_products/TILED_GRB00087.

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


GRB_name: GRB191210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26391
SUBJECT: Possible HAWC-detected GRB 191210A: no neutrino counterpart candidate in ANTARES search
DATE:    19/12/11 20:43:08 GMT
FROM:    Antoine Kouchner at ANTARES Collaboration  <kouchner@apc.in2p3.fr>

Alexis Coleiro (APC/Univ de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration. 
Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported HAWC alert (https://gcn.gsfc.nasa.gov/notices_amon_hawc/9066_1171.amon <https://gcn.gsfc.nasa.gov/notices_amon_hawc/9066_1171.amon>). 

No up-going muon neutrino candidate events were detected within 3 degrees from the event coordinates over a time window of +/-1h during which the potential source remained visible in the up-going field of view of ANTARES. A search over an extended time window of +/-1 day has also yielded no detection (50.5% visibility). 

This leads to a preliminary 90% confidence level upper limit on the muon-neutrino radiant fluence from a point source of about 17 GeV.cm^-2 over the energy range 3 TeV - 3 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 69 GeV.cm^-2 (600 GeV - 3 TeV) for an E^-2.5 spectrum, computed for the time of the alert. 

ANTARES is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.


GRB_name: GRB191210A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26392
SUBJECT: Possible HAWC-detected GRB 191210A: Fermi-LAT Upper Limits
DATE:    19/12/11 21:41:53 GMT
FROM:    Nicola Omodei at Stanford U.  <nicola.omodei@slac.stanford.edu>

N. Omodei (Stanford U.), S. Cutini (INFN Perugia), and F.Longo (University and INFN, Trieste) 

report on behalf of the Fermi-LAT Collaboration:

Fermi-LAT has performed follow-up observations of the possible HAWC-detected burst GRB 191210A: https://gcn.gsfc.nasa.gov/notices_amon_hawc/9066_1171.amon

At the time of the HAWC trigger (T0), the location of the candidate transient was outside the LAT field of view, at an inclination angle of 145 degrees.

The region of Interest entered in LAT field of view at about T0+2.5 ks and exited again at 4.5 ks.

During this time window we performed a search for a transient counterpart, and no significant new sources are found. 

The flux upper bounds in the 100 MeV - 10 GeV (90% CL), assuming a E^-2 power law spectrum, are:

Energy flux < 8.76e-10 [erg/cm2/s]
Photon flux < 1.18e-06 [ph./cm2/s]

We also searched for late time emission (until T0+100 ks seconds) and no significant excess is found. 

The Fermi-LAT point of contact for this event is:
Nicola Omodei (nicola.omodei@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: GRB191213A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26398
SUBJECT: GRB 191213A: Swift detection of a burst
DATE:    19/12/13 04:16:19 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. B. Cenko (GSFC), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 04:06:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191213A (trigger=944091).  Due to a Sun constraint,
Swift did not slew to this burst. 
The BAT on-board calculated location is 
RA, Dec 224.507, -9.726 which is 
   RA(J2000) = 14h 58m 02s
   Dec(J2000) = -09d 43' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is typical for an image trigger, there is
no obvious variation in the immediately-available lightcurve. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 16:25 UT on 2019 December 23. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is S. B. Cenko (brad.cenko 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/)


GRB_name: GRB191213B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26414
SUBJECT: GRB 191213B: Fermi GBM Final Real-time Localization
DATE:    19/12/13 18:59:22 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 18:49:07 UT on 13 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191213B (trigger 597955752.969344 / 191213784).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 331.1, Dec = -13.9 (J2000 degrees, equivalent to J2000 22h 04m, -13d 54'), with a statistical uncertainty of 6.7 degrees.

The angle from the Fermi LAT boresight is 29.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191213784/quicklook/glg_skymap_all_bn191213784.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191213784/quicklook/glg_healpix_all_bn191213784.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191213784/quicklook/glg_lc_medres34_bn191213784.gif


GRB_name: GRB191213A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26418
SUBJECT: GRB 191213A: Swift-BAT refined analysis
DATE:    19/12/14 03:08:22 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
S. B. Cenko (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF), S. Laha (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 191213A (trigger #944091)
(Cenko et al., GCN Circ. 26398).  The BAT ground-calculated position is
RA, Dec = 224.530, -9.745 deg which is
   RA(J2000)  =  14h 58m 07.2s
   Dec(J2000) = -09d 44' 41.9"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.

The mask-weighted light curve shows some weak emission that starts at ~T-30
s
and remains detectable until the burst went out of the BAT FOV at T+139 s.
It is likely that the emission continues beyond T+139 s. The burst did not
come
back into the BAT FOV within the next ~ 2 hours.

The time-averaged spectrum from T-33.52 to T+104.01 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.49 +- 0.16.  The fluence in the 15-150 keV band is 2.1 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+99.95 sec in the 15-150 keV band
is 0.5 +- 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/944091/BA/


GRB_name: GRB191213A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26420
SUBJECT: GRB 191213A: BOOTES-5/JGT optical limit
DATE:    19/12/14 08:38:06 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

I. Carrasco (UMA), Y.-D. Hu, E. Fernandez-Garcia, M. A. Castro Tirado 
and A. J. Castro-Tirado (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), S. 
Jeong and I. H. Park (SKKU) and M. D. Caballero-Garcia (ASU-CAS, CZ) on 
behalf of a larger collaboration, report:

The 60cm BOOTES-5/JGT robotic telescope at Observatorio Astronomico 
Nacional in San Pedro Martir (Mexico) observed GRB 191213A ( Cenko et 
al., GCNC 26398 ) starting at 13:16 UT (~9.17 hr after trigger) at high 
airmass. Within the refined Swift/BAT error position ( Lien et al., GCNC 
26418 ), no optical afterglow is found down to 18.6 mag in the clear 
filter on the co-added 15 images (60s each).

We thank the staff at Observatorio Astronomico Nacional in San Pedro 
Martir for its excellent support.


GRB_name: GRB191218A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26480
SUBJECT: GRB 191218A: Swift detection of a burst
DATE:    19/12/18 02:51:29 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/UMCP), N. J. Klingler (PSU),
A. Y. Lien (GSFC/UMBC), M. J. Moss (GWU), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 02:42:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191218A (trigger=944916).  Swift did not slew to this burst due
to a Sun constraint. 
The BAT on-board calculated location is 
RA, Dec 301.078, -40.274 which is 
   RA(J2000) = 20h 04m 19s
   Dec(J2000) = -40d 16' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 60 sec.  The peak count rate
was ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 12:12 UT on 2020 February 27. There will thus be no XRT
or UVOT data for this trigger before this time. 

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/)


GRB_name: GRB191218A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26482
SUBJECT: GRB 191218A: AstroSat CZTI detection
DATE:    19/12/18 10:02:28 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

R. Gaikwad, S.Gupta, V. Sharma, A. Vibhute and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a GRB 191218A, which was also detected by Swift (Troja E. et al., GCN #26480).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 2019-12-18 02:42:43.0 UT. The measured peak count rate associated with the burst is 348 cts/s above the background in the combined data of four quadrants, with a total of 3669 cts. The local mean background count rate was 507 cts/s. Using cumulative rates, we measure a T90 of 51.03 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191213A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26484
SUBJECT: Konus-Wind observation of GRB 191213A (ulong)
DATE:    19/12/18 12:51:10 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

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

The ultra-long GRB 191213A (Swift-BAT trigger #944091:
Cenko et al., GCN 26398; Lien et al., GCN 26418)
was detected by Konus-Wind (KW) in the waiting mode.

The burst light curve shows the main multipeaked episode of emission
started at ~T0(BAT)-25 s and lasted until ~T0(BAT)+1815 s (the
duration is ~1790 s; T0(BAT)=14781.499 s UT (04:06:21.499)).
There is also a weaker broad pulse of emission seen before the main
pulse from ~T0(BAT)-834 s to ~T0(BAT)-772 s. It might be related to
GRB 191213A (it was detected by the same KW detector, and the KW
ecliptic latitude response for it is consistent with the common
origin with the main episode).

As observed by KW, the burst (main episode) had a fluence of
1.12(-0.06,+0.07)x10^-4 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(BAT)+676.012s, of 2.5(-0.41,+0.41)x10^-7 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The emission shows no signs of strong spectral variability.
Modeling the KW 3-channel time-integrated spectrum
(from ~T0(BAT)-24.660 s to ~T0(BAT)+1815.340 s)
by a power law with exponential cutoff model
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.16 (-0.12,+0.14), and Ep = 409 (-71,+110) keV.

Thus, the prompt gamma-ray emission properties of this GRB:
fluence, peak flux, Ep, and duration are similar to those
observed in other ultra-long GRBs.

The KW light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB191213A/

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


GRB_name: GRB191218A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26495
SUBJECT: GRB 191218A: Swift-BAT refined analysis
DATE:    19/12/19 03:53:53 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), E. Troja (GSFC/UMD),
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 191218A (trigger #944916)
(Troja et al., GCN Circ. 26480).  The BAT ground-calculated position is
RA, Dec = 301.070, -40.277 deg which is
   RA(J2000)  =  20h 04m 16.7s
   Dec(J2000) = -40d 16' 38.8"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 9%.

The mask weighted light curve shows two peaks at ~T+4 s and ~T+45 s. The
overall structure starts at ~T-2 s and lasts till ~T+58 s.
T90 (15-350 keV) is 44.67 +- 0.73 sec (estimated error including systematics).

The time-averaged spectrum from T-0.23 to T+46.03 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.12 +- 0.10.  The fluence in the 15-150 keV band is 7.8 +- 0.4 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.66 sec in the 15-150 keV band
is 6.3 +- 0.9 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/944916/BA/


GRB_name: GRB191218A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26506
SUBJECT: Konus-Wind observation of GRB 191218A
DATE:    19/12/19 19:58:46 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

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

The long-duration GRB 191218A (Swift-BAT trigger #944916:
Troja et al., GCN 26480; Markwardt et al., GCN 26495;
AstroSat CZTI detection: Gaikwad et al., GCN 26482)
triggered Konus-Wind at T0=9758.735 s UT (02:42:38.735).

The burst light curve shows a double-peaked structure
which starts at ~T0-0.5 s and has a total duration of ~78.8 s.
The emission is seen up to ~4 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.92(-0.37,+0.45)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.440 s,
of 4.08(-1.07,+1.07)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+81.664 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 = -0.76(-0.18,+0.20)
and Ep = 330(-44,+61) keV (chi2 = 54/69 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 53/68 dof).

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+7.936 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model
with  alpha = -0.27(-0.15,+0.17)
and Ep = 322(-24,+28) keV (chi2 = 74/69 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.7
(chi2 = 73/68 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191218_T09758/

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


GRB_name: GRB191220A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26515
SUBJECT: GRB 191220A: Prompt enhanced Swift-XRT position
DATE:    19/12/20 14:02:07 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 191220A, we find an
enhanced XRT position of the afterglow: RA, Dec: 281.3800, 26.6558
which is equivalent to:
   RA (J2000)  = 18 45 31.19
   Dec (J2000) = +26 39 20.9
with an uncertainty of 2.3 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/945344.

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: GRB191220A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26516
SUBJECT: GRB 191220A: Swift detection of a burst
DATE:    19/12/20 14:13:01 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

S. Laha (GSFC/UMBC/CRESST), D. N. Burrows (PSU), J.D. Gropp (PSU), N. P.
M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester), D.
M. Palmer (LANL) and A. Tohuvavohu (U Toronto) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 13:29:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191220A (trigger=945344).  Swift slewed immediately to the
burst. The BAT on-board calculated location is
RA, Dec 281.391, +26.667 which is
   RA(J2000) = 18h 45m 34s
   Dec(J2000) = +26d 40' 02"
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 20 sec.  The peak count rate
was ~200 counts/sec (15-350 keV), at ~1 sec after the trigger.

The XRT began observing the field at 13:31:50.2 UT, 132.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 281.37924,
26.65599 which is equivalent to:
   RA(J2000)  = 18h 45m 31.02s
   Dec(J2000) = +26d 39' 21.6"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 54 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 https://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 1.53
x 10^21 cm^-2 (Willingale et al. 2013).

The initial flux in the 2.5 s image was 4.03e-10 erg cm^-2 s^-1 (0.2-10
keV).

UVOT took a finding chart exposure of 250 seconds with the U filter
starting 137 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 19.2 mag. The 8'x8' region for the list of sources
generated on-board covers 0.00% of the XRT error circle. No correction has
been made for the expected extinction corresponding to E(B-V) of 0.14.

Burst Advocate for this burst is S Laha (sib.laha 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/)


GRB_name: GRB191220A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26519
SUBJECT: GRB 191220A: SAO RAS possible OT detection
DATE:    19/12/20 17:32:49 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin on behalf of larger GRB follow-up team report.

We observed the field of the GRB 191220A with the SAO RAS
Zeiss-1000 telescope equipped with the MMPP (Multi-Mode
Photometer-Polarimeter). The observations were started since
1.419 hours after the trigger (Laha et al., GCNC #26516).
We obtained 8 x 300 sec. frames in Rc band (14:54:44 -- 15:39:44 UT).

Within the enhanced XRT error circle (Evans, GCNC #26515)
we detect single object, possible OT, with the coordinates
R. A. = 18:45:31.10, Decl. = +26:39:20.8, +/- 0".3, Epoch = 2000.
ftp://ftp.sao.ru/pub/grb/GRB191220A/GRB_possibleOT.jpg

Preliminary brightness of the object is R = 20.46 +/- 0.08
(T_mid - T0 = 1.794 h). Photometry were made against the R2
magnitudes of nearby USNO-B1 stars.


GRB_name: GRB191220A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26522
SUBJECT: GRB 191220A: Enhanced Swift-XRT position
DATE:    19/12/20 21:43:50 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 2496 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 191220A, 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 = 281.37980, +26.65588 which is equivalent
to:

RA (J2000): 18h 45m 31.15s
Dec (J2000): +26d 39' 21.2"

with an uncertainty of 2.3 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: GRB191220A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26524
SUBJECT: GRB 191220A: Swift-XRT refined Analysis
DATE:    19/12/20 22:52:47 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), B. Sbarufatti (PSU),
D.N. Burrows (PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M.G.
Bernardini (INAF-OAB) and S. Laha report on behalf of the Swift-XRT
team:

We have analysed 8.0 ks of XRT data for GRB 191220A (Laha et al. GCN
Circ. 26516), from 138 s to 23.9 ks after the  BAT trigger. The data
comprise 38 s in Windowed Timing (WT) mode with the remainder in Photon
Counting (PC) mode. The enhanced XRT position for this burst was given
by Osborne et al. (GCN Circ. 26515).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.2 (+0.7, -1.5), followed by a break at T+349 s to an
alpha of 0.51 (+0.14, -0.30).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+0.18, -0.14). The
best-fitting absorption column is  consistent with the Galactic value
of 1.5 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 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:      1.53 (+/-0.25) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.01 (+0.18, -0.14)

If the light curve continues to decay with a power-law decay index of
0.51, the count rate at T+24 hours will be 9.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.3 x
10^-13 (4.0 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/00945344.

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


GRB_name: GRB191220A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26525
SUBJECT: GRB 191220A: AbAO optical observations
DATE:    19/12/20 23:38:38 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), R. Ya. Inasaridze (AbAO), V.R. 
Ayvazian (AbAO),    G. V.  Kapanadze (AbAO),   E. Mazaeva (IKI), A. 
Volnova  (IKI),  I. Molotov (KIAM) report on behalf of  GRB IKI FuN:

We observed the field of GRB 191220A (Evans et al., GCN 26515; Laha et 
al., GCN 26516) with AS-32 (0.7m) telescope of Abastumani Observatory 
starting on Dec. 20 (UT) 14:40:39.  We do no detect any source within 
enhanced Swift-XRT position (Osborne et al., GCN 26522). In particular 
we do not detect the candidate in the OT (Moskvitin, GCN 26519). 
Preliminary photometry of the field is following.

Date       UT start  t-T0    Filter Exp.  OT    Err. UL
                     (mid, days)     (s)
2019-12-20 14:40:39  0.05037 R      23*60 n/d   n/d  19.8

The photometry is based on nearby USNO-B1.0 stars
UUSNO-B1.0_id R2
1166-0338499  14.74
1166-0338587  15.40
1166-0338614  15.08


GRB_name: GRB191220A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26526
SUBJECT: GRB 191220A: Swift/UVOT Upper Limits
DATE:    19/12/21 02:45:24 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and S. L. Laha (GSFC/UMBC/CRESST)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191220A
138 s after the BAT trigger (Laha et al., GCN Circ. 26516).  No optical
afterglow consistent with the XRT position (Laha et al. GCN Circ. 26516)
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

u_FC               138          387          246         >19.8
u                  138         6726         1061         >20.0
w1                 446         6521          687         >19.6
m2                 420         6316          687         >19.9
w2                 396         6766          719         >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.14 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB191221A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26532
SUBJECT: GRB 191221A: Fermi GBM Final Real-time Localization
DATE:    19/12/21 19:24:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 19:14:28 UT on 21 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191221A (trigger 598648473.844298 / 191221802).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 40.8, Dec = -43.0 (J2000 degrees, equivalent to J2000 02h 43m, -43d 00'), with a statistical uncertainty of 5.9 degrees.

The angle from the Fermi LAT boresight is 21.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191221802/quicklook/glg_skymap_all_bn191221802.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191221802/quicklook/glg_healpix_all_bn191221802.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191221802/quicklook/glg_lc_medres34_bn191221802.gif


GRB_name: GRB191221B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26534
SUBJECT: GRB 191221B: Swift detection of a burst and a very bright optical candidate
DATE:    19/12/21 21:00:24 GMT
FROM:    Sibasish Laha at GSFC  <sib.laha@gmail.com>

S Laha (GSFC/UMBC/CRESST), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and
K. K. Simpson (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 20:39:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191221B (trigger=945521).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 154.832, -38.141 which is 
   RA(J2000) = 10h 19m 20s
   Dec(J2000) = -38d 08' 28"
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 15 sec.  The peak count rate
was ~17000 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 20:40:39.3 UT, 86.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 154.8286, -38.1579 which is equivalent to:
   RA(J2000)  = 10h 19m 18.86s
   Dec(J2000) = -38d 09' 28.4"
with an uncertainty of 6.8 arcseconds (radius, 90% containment). This
location is 61 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. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 91 seconds after the BAT trigger. A very bright afterglow candidate has
been found at the XRT position in the initial data products. Because of 
coincidence loss we cannot calculate the magnitude accurately at this time. 
No correction has been made for the expected extinction corresponding to E(B-V) of 0.08. 

Burst Advocate for this burst is S Laha (sib.laha 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/)


GRB_name: GRB191220A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26535
SUBJECT: GRB 191220A: Swift-BAT refined analysis
DATE:    19/12/21 21:19:35 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), 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-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 191220A (trigger #945344)
(Laha et al., GCN Circ. 26516).  The BAT ground-calculated position is
RA, Dec = 281.335, 26.679 deg which is
   RA(J2000)  =  18h 45m 20.3s
   Dec(J2000) = +26d 40' 43.1"
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.


The mask weighted light curve shows complex structures with a duration of ~50 sec, with a hint of some weak emission lasting till ~ T+ 240 s.
The overall structure starts at ~ T-2 sec and lasts till ~ T+60 sec.
T90 (15-350 keV) is 175.55 +- 125.93 sec (estimated error including systematics).

The time-averaged spectrum from T-2.46 to T+248.42 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.12 +- 0.40.  The fluence in the 15-150 keV band is 1.1 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+6.69 sec in the 15-150 keV band
is 1.1 +- 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/945344/BA/


GRB_name: GRB191221B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26536
SUBJECT: Swift GRB 191221B: Global MASTER-Net observations report 
DATE:    19/12/21 21:27:29 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

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

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev, O.Ershova 
(Irkutsk State University, API),

A. Tlatov, D. Dormidontov 
(Kislovodsk Solar Station of the Pulkovo Observatory),

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 191221B ( S Laha et al., GCN 26534) errorbox  1677 sec after notice time and 1700 sec after trigger time at 2019-12-21 21:07:33 UT, with upper limit up to  17.0 mag. The observations began at zenith distance = 69 deg. The sun  altitude  is -30.6 deg. 

The galactic latitude b = 16 deg., longitude l = 273 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1234924

We obtain a following upper limits.  

Tmid-T0  |          Site       |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________

    1790 |         MASTER-SAAO |  P\ |   180 | 16.0 |        
    1991 |         MASTER-SAAO |  P\ |   180 | 16.7 |        
    2192 |         MASTER-SAAO |  P\ |   180 | 16.6 |        
    2394 |         MASTER-SAAO |  P\ |   180 | 17.0 |        


The observation and reduction will continue. 
The message may be cited.


GRB_name: GRB191221B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26537
SUBJECT: GRB 191221B: MASTER OT detection
DATE:    19/12/21 21:44:15 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov,  E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa,A.Kuznetsov,F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix
Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State
University)

MASTER auto-detection system discovered OT in Swift GRB 191221B (Laha et 
al GCN 26534) error-box
at coordinates

RA,Dec(2000)=10h 19m 19.24s , -38d 09m 28s.7

with quick decay  with m_OT=14.4 at 2019-12-21 21:07:33 UT



The observation and reduction will be continued. The message may be cited.


GRB_name: GRB191221B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26538
SUBJECT: GRB 191221B: Swift/UVOT redshift
DATE:    19/12/22 01:33:28 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT obtained a 49s grism spectrum of GRB 191221B
242 s after the BAT trigger (Laha et al., GCN Circ. 26534).
The spectrum shows a clear break at 2008 Angstrom, suggesting
a redshift of z=1.19. At that redshift, the line of He II 1640A is well
defined
and N II 2143A is present, as well as possibly N V at 1243 A.


GRB_name: GRB191221B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26540
SUBJECT: GRB 191221B: Enhanced Swift-XRT position
DATE:    19/12/22 03:10:37 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 1950 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 191221B, 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 = 154.82992, -38.15759 which is equivalent
to:

RA (J2000): 10h 19m 19.18s
Dec (J2000): -38d 09' 27.3"

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: GRB191221B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26549
SUBJECT: GRB 191221B: AGILE/MCAL observations
DATE:    19/12/22 09:23:58 GMT
FROM:    Francesco Longo at U of Trieste,INFN Trieste  <franzlongo1969@gmail.com>

F. Longo (UniTS and INFN Trieste),  M. Pilia (INAF/OA-Cagliari),
F. Verrecchia (SSDC, and INAF/OAR) , A. Ursi (INAF/IAPS),
M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata),
A. Argan, M. Cardillo, C. Casentini, Y. Evangelista, G. Piano
(INAF/IAPS), F. Lucarelli, C. Pittori (SSDC, and INAF/OAR),
A. Bulgarelli, V. Fioretti, F. Fuschino, N. Parmiggiani (INAF/OAS-Bologna),
M. Marisaldi (INAF/OAS-Bologna, and Bergen University),
A. Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), A. Giuliani (INAF/IASF-Mi),
report on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected the long GRB191221B at
T0 = 2019-12-21 20:39:11.42 (+/- 0.01 s) already detected by Swift
(Laha et al., 2019; GCN #26534).

In the MCAL energy range (0.4-100 MeV), the burst lasted about ~15 s
and released a total number of ~12000 counts over a background rate of 650 Hz.

The light curve shows several peaks and can be found at
http://www.agilescienceapp.it/notices/GRB_065726_504045551.415264.png.

The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive
in the energy range 0.4-100 MeV. Additional analysis of AGILE data is
in progress.


GRB_name: GRB191221B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26551
SUBJECT: GRB 191221B: VIRT Optical Upper Limits
DATE:    19/12/22 10:12:13 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

P. Gokuldass (UVI), D. Morris (UVI), N. Orange (OrangeWave Innovative
Science, LLC), A. Cucchiara (College of Marin), R. Strausbaugh (UVI) report:

We observed the field of GRB191221B (Laha et al, GCN 26534) with the 0.5m
Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 12-22-2019 starting at 07:16:00 UT
(T+10.6hrs). We performed a series of 50x10s exposures in R-band filter.
The weather conditions were clear during the hours of observation and the
zenith angle at the start of observations was 60 degrees and rising. We
observed the enhanced Swift-XRT position with a 20'x20' field of view.

We clearly detect the uncatalogued source within the enhanced Swift-XRT
error radius that was reported by Lipunov et al (GCN 26537). We measure the
source with a magnitude:

R = 16.7 Â± 0.1

The magnitude is estimated from comparison to nearby USNO B1 stars and is
not corrected for Galactic extinction. The VIRT is still in the
commissioning phase.

Observations and data analysis are ongoing.

This work is supported by NASA-MUREP-MIRO grant NNX15AP95A and NSF-EiR
grant 1901296. This message can be cited.


GRB_name: GRB191221B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26552
SUBJECT: GRB 191221B: Correction to GCN26551 - VIRT OT observation
DATE:    19/12/22 10:39:57 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

P. Gokuldass (UVI), D. Morris (UVI), N. Orange (OrangeWave Innovative
Science, LLC), A. Cucchiara (College of Marin), R. Strausbaugh (UVI)
report:

We observed the field of GRB191221B (Laha et al, GCN 26534) with the
0.5m Virgin Island Robotic Telescope (VIRT) at the University of the
Virgin Islands' Etelman Observatory on 12-22-2019 starting at 07:16:00
UT (T+10.6hrs). We performed a series of 50x10s exposures in R-band
filter. The weather conditions were clear during the hours of
observation and the
zenith angle at the start of observations was 60 degrees and rising.
We observed the enhanced Swift-XRT position with a 20'x20' field of
view.

We clearly detect the uncatalogued source within the enhanced
Swift-XRT error radius that was reported by Lipunov et al (GCN 26537).
We measure the source with a magnitude:

R = 16.7 + / - 0.1

The magnitude is estimated from comparison to nearby USNO B1 stars and
is not corrected for Galactic extinction. The VIRT is still in the
commissioning phase.

Observations and data analysis are ongoing.

This work is supported by NASA-MUREP-MIRO grant NNX15AP95A and NSF-EiR
grant 1901296. This message can be cited.


GRB_name: GRB191221B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26553
SUBJECT: GRB 191221B: VLT/X-shooter redshift
DATE:    19/12/22 10:58:41 GMT
FROM:    Maryam Arabsalmani at University of Melbourne  <mar.arabsalmani@gmail.com>

Title: GRB 191221B: VLT/X-shooter redshift

J.-B. Vielfaure (CNRS, Paris Obs.), M. Arabsalmani (ICRAR/UWA), K. E.
Heintz (Univ. Iceland), N. R. Tanvir (Univ. Leicester), A. de Ugarte
Postigo (HETH/IAA-CSIC), D. B. Malesani (DTU Space), J. P. U. Fynbo
(DAWN/NBI), K. Wiersema (Univ. Warwick), S. D. Vergani (CNRS, Paris Obs.),
D. Xu (NAO/CAS), G. Pugliese (Univ. Amsteram), S. Schulze (WIS), D.
Burgarella (AMU, CNRS, CNES, LAM), report on behalf of the Stargate
collaboration:

We observed the optical afterglow of GRB 191221B (Laha et al., GCN 26534;
Longo et al., GCN 26549; Lipunov et al., GCN 26537). using the ESO VLT UT2
(Kueyen) equipped with the X-shooter spectrograph. Our spectra cover the
wavelength range 3000-21000 AA, and consist of 2 exposures by 600 s each.
The observation mid time was 2019 Dec 22.2707 UT (9.843 hr after the GRB).

In a 15 s image taken with the acquisition camera on Dec 22.2592 UT, we
detect the optical afterglow, for which we measure a magnitude r = 17.13 +-
0.01 AB (calibrated against nearby stars from the Skymapper catalog; Wolf
et al. 2018, PASA, 35, 010; https:doi.org/10.4225/41/593620ad5b574).

We detect several absorption profiles in the GRB spectrum including MgII,
MgI, SiII, CIV, AlII, NiII, and FeII lines. From these metal lines we infer
a redshift z=1.148 for the GRB, consistent with the redshift reported by
Swift/UVOT tram (GCN 26538). We also detect the MgII absorption profile
corresponding to an intervening system at z=0.961.

We acknowledge excellent support from the ESO observing staff in Paranal,
in particular Pascale Hibon, Francisco Belmar, and Trystyn Berg.


GRB_name: GRB191221B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26555
SUBJECT: GRB 191221B: MASTER VWFC OT yearly detection 
DATE:    19/12/22 14:31:51 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov,  E. Gorbovskoy, V.Kornilov, N.Tyurina,
P.Balanutsa,A.Kuznetsov,F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
D. Buckley(South African Astronomical Observatory),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix
Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State
University)

We found first image with error box at 2019-12-21 20:40:15  (62 sec after 
trigger time).


MASTER-OAFA Very Wide Field Camera  detected OT in Swift GRB 191221B
(Laha et al GCN 26534; Lipunov et al.,  GCN 26537; Kuin, GCN 26538;
Gokuldass et al., GCN 26551; Vielfaure et al., GCN 26553;) error-box
at coordinates at 2019-12-21 20:41:35 UT  (142 s after trigger time).
with m_OT~10.5 mag.



The observation and reduction will be continued. The message may be cited.


GRB_name: GRB191221B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26559
SUBJECT: GRB 191221B: Swift-XRT refined Analysis
DATE:    19/12/22 17:57:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. D'Avanzo (INAF-OAB), D.N. Burrows (PSU), J. D. Gropp (PSU), A.
Tohuvavohu (U. Toronto), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), M.G. Bernardini (INAF-OAB), E.
Ambrosi  (INAF-IASFPA) and S Laha report on behalf of the Swift-XRT
team:

We have analysed 7.8 ks of XRT data for GRB 191221B (S Laha et al. GCN
Circ. 26534), from 74 s to 58.6 ks after the  BAT trigger. The data
comprise 1.3 ks 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 Beardmore
et al. (GCN Circ. 26540).

The late-time light curve (from T0+4.9 ks) can be modelled with a
power-law decay with a decay index of alpha=1.03 (+0.09, -0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.097 (+/-0.014). The
best-fitting absorption column is  consistent with the Galactic value
of 8.6 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.86 (+0.07, -0.06) and a best-fitting absorption
column consistent with the Galactic value. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.6 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 8.6 x 10^20 cm^-2
Intrinsic column:    8.6 (+5.8, -0.0) x 10^20 cm^-2 at z=1.148
Photon index:      1.86 (+0.07, -0.06)

If the light curve continues to decay with a power-law decay index of
1.03, the count rate at T+24 hours will be 0.087 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-12 (3.6 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/00945521.

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


GRB_name: GRB191221B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26560
SUBJECT: GRB 191221B: LCO Optical Detection
DATE:    19/12/22 18:20:35 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (U. of the Virgin Islands/College of Marin) report on behalf of a larger collaboration:

We observed Swift GRB 191221B (Laha et al., GCN 26534) with the LCO 1-m Sinistro instrument at the Sutherland South African Astronomical Observatory site on December 22, from 00:30 to 01:11 UT (corresponding to 3.5 to 4.2 hours after the GRB trigger time) with the Bessel R and I filters.

We performed a series of 10x90s exposures in each band. We detect a bright source in the Swift-BAT refined error region (Laha et al., GCN 26536) that is not present in either USNO-B1.0 or 2MASS  surveys with the following  magnitudes:

R = 16.50 +/- 0.01

I = 15.86 +/- 0.01

This flux measurement is calibrated against several USNO-B1.0 objects near the GRB location and is not corrected for Galactic Extinction.


GRB_name: GRB191221B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26561
SUBJECT: GRB 191221B: Zadko observatory - Gingin optical observations
DATE:    19/12/22 19:43:01 GMT
FROM:    Bruce Gendre at UVI  <bruce.gendre@gmail.com>

B. Gendre (OzGrav-UWA), H. Crisp (OzGrav-UWA), J. Moore (OzGrav-UWA), 
D. Coward (OzGrav-UWA), A. Klotz (IRAP-CNRS-OMP), P. Thierry (Aragne 
Observatory), A. Burrell (OzGrav-UWA), J. Zadko (Claire Energy), 
M. Boer, (UNS-CNRS-OCA)
report:

We imaged the field of GRB 191221B detected by Swift (trigger 945521, 
Laha et al. GCN 26534) with the Zadko robotic telescope (D=100cm)
located at the Zadko observatory - Gingin, Australia.

The observations started 19 hours after the GRB trigger. The elevation 
of the field was at 32 degrees above horizon and weather conditions
were good. We performed 6 long exposures of 180s in Clear filter.

We detected the candidate couterpart mentioned by Lipunov et al. (GCNC 
26537) in each of the images.

OT was R~17.6+/-0.2 at that time. Further analysis and observations are 
ongoing.

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

This message may be cited.


GRB_name: GRB191221B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26562
SUBJECT: GRB 191221B: Swift-BAT refined analysis
DATE:    19/12/22 21:07:26 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), 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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 191221B (trigger #945521)
(Laha et al., GCN Circ. 26534).  The BAT ground-calculated position is
RA, Dec = 154.831, -38.152 deg which is
   RA(J2000)  =  10h 19m 19.3s
   Dec(J2000) = -38d 09' 07.1"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 12%.

The mask weighted light curve shows complex structures with a duration of ~30 s.
The overall structure starts at ~T-10 s and lasts till ~T+20s.
There is some hint of weak emission extending up to ~ T+60 s.
T90 (15-350 keV) is 48.00 +- 16.00 sec (estimated error including systematics).

The time-averaged spectrum from T-15.28 to T+96.72 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.24 +- 0.05.  The fluence in the 15-150 keV band is 1.9 +- 0.1 x 10^-05 erg/cm2.
the fluence of this burst is among the brightest ~3% of all BAT-detected GRBs
(based on fluences from the BAT GRB catalog https://swift.gsfc.nasa.gov/results/batgrbcat/).
The 1-sec peak photon flux measured from T+8.22 sec in the 15-150 keV band
is 4.8 +- 0.7 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/945521/BA/


GRB_name: GRB191221B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26564
SUBJECT: GRB 191221B: ALMA detection
DATE:    19/12/22 22:36:28 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (University of Bath), W. Fong (Northwestern), K. D. Alexander
(Northwestern), E. Berger (Harvard), S. Bhandari (CSIRO), G. Hosseinzadeh
(Harvard), R. Margutti (Northwestern), C. G. Mundell (University of Bath),
and P. Schady (University of Bath) report on behalf of a larger
collaboration:

"We observed GRB 191221B (Laha et al. GCN 26534) with the Atacama Large
Millimeter/Submillimeter Array (ALMA) beginning on 2019 December 22 at
07:43:55 UT (11.1 hr after the burst) at 97.5 GHz under good weather
conditions. Preliminary analysis reveals a bright (S/N > 300) mm source at
position:

10:19:19.225 (+/- 0.005), -38:09:27.45 (+/- 0.01)

consistent with the X-ray position (Beardmore et al. GCN 26540) and optical
position (Lipunov et al., GCN 26537). Follow-up observations are planned.

We thank the JAO staff, AoD, P2G, and the entire ALMA team for their help
with these observations."


GRB_name: GRB191221B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26565
SUBJECT: GRB 191221B: iTelescope optical observations
DATE:    19/12/23 00:21:24 GMT
FROM:    Filipp Dmitrievich Romanov at Amateur astronomer  <filipp.romanov.27.04.1997@gmail.com>

I observed the optical afterglow of GRB 191221B (Laha et al., GCN Circ.
26534) with remote telescope T32 (0.43-m f/6.8 reflector + FLI Proline
16803 CCD) of iTelescope.Net in Siding Spring Observatory (Australia) on
2019-12-22 since 13:28:52 UT (~16.8 hours after the trigger). Two images
were obtained in each band with Astrodon luminance filter and
Johnson/Cousins V filter for 180 and 120 seconds (Binx2). I detected the
optical afterglow in three images in the enhanced Swift-XRT position
(Beardmore et al., GCN Circ. 26540); it not present in images from DSS
Plate Finder.

The following magnitudes (mag. error ~ 0.2) were measured from comparison
to nearby stars from APASS DR9 catalogue (Henden et al., 2016):

Time of start  Exp.time  Mag.   Comp.star band  Filter
----------------------------------------------------------
13:28:52 UT    180 s     18.1        r'         Luminance
13:32:58 UT    180 s     18.3        V          V
13:36:51 UT    120 s     18.3        r'         Luminance
13:39:46 UT    120 s     <17.9       V          V
----------------------------------------------------------

Magnitudes were not corrected for Galactic extinction.


GRB_name: GRB191221B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26566
SUBJECT: GRB 191221B: iTelescope T17 detection
DATE:    19/12/23 02:27:04 GMT
FROM:    Albert Kong at NTHU  <akhkong@gmail.com>

A.K.H. Kong (NTHU, Taiwan) reports

We observed the field of GRB 191221B (Laha et al., GCN 26534) with the
T17 0.43m telescope of iTelescope.Net in Siding Spring, Australia. The
observation was done with a SDSS r filter beginning at 2019-12-22
14:56:51 UT (about 18 hours after the trigger) for 300 sec. The
optical counterpart (Laha et al., GCN 26534) was detected with
r=18.4+/-0.1 (AB) by calibrating with the SkyMapper Southern Sky
Survey.


GRB_name: GRB191221B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26567
SUBJECT: GRB 191221B: AstroSat CZTI detection
DATE:    19/12/23 10:16:07 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

R. Gaikwad, S. Gupta, V. Sharma, A. Vibhute and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a GRB 191221B, which was also detected by Swift (Laha S. et al., GCN #26534), Global MASTER-Net (Lipunov V. et al., GCN #26536), Swift/UVOT (Kuin N. et al., GCN #26538), Swift-XRT (Beardmore A. et al., GCN #26540), AGILE/MCAL (Longo F. et al., GCN #26549), VIRT (Gokuldass P. et al., GCN #26551), VLT/X-shooter (Vielfaure J. et al., GCN #26553), MASTER VWFC (Lipunov V. et al., GCN #26555), LCO (Strausbaugh R. et al., GCN #26560), Zadko (Gendre B. et al., GCN #26561), ALMA (Laskar T. et al., GCN #26564) and iTelescope (Romanov F. et al., GCN #26565).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 2019-12-21 20:39:12.0 UT. The measured peak count rate associated with the burst is 708 cts/s above the background in the combined data of four quadrants, with a total of 4829 cts. The local mean background count rate was 515 cts/s. Using cumulative rates, we measure a T90 of 11.16 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB191221B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26573
SUBJECT: GRB 191221B: Insight-HXMT/HE detection
DATE:    19/12/24 08:16:39 GMT
FROM:    Wangchen Xue at IHEP  <xuewc@ihep.ac.cn>

W. C. Xue, Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-12-21T20:39:10.70 (T0), Insight-HXMT/HE detected 
GRB 191221B (trigger ID: HEB191221860) in a routine search of the data, 
which was also triggered by Swift/BAT (GCN #26534).

The Insight-HXMT/HE light curve mainly consists of multiple  
pulses with a duration (T90) of 8.85 s measured from T0-0.62 s. 
The 1-ms peak rate, measured from T0+5.37 s, is 8262 cnts/sec. 
The total counts from this burst is 38429 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB191221860_LC.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191221B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26574
SUBJECT: GRB 191221B: Swift/UVOT Detection
DATE:    19/12/24 12:08:39 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and S. L. Laha (GSFC/UMBC/CRESST)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191221B
92 s after the BAT trigger (Laha et al., GCN Circ. 26534).
A source consistent with the XRT position (Beardmore et al. GCN Circ. 26540)
and ALMA position (Laskar et al., GCN Circ. 26564)  was detected in the
initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  10:19:19.24 = 154.83017 (deg.)
    Dec (J2000) = -38:09:27.64 = -38.15768 (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               92          241          147         see below
u                  304          554          246         12.30 +/- 0.02
b                  560          579           20         13.54 +/- 0.04
uvw2               610          630           20         13.20 +/- 0.06
v                  635          655           20         13.42 +/- 0.05
uvm2               659          679           20         12.79 +/- 0.06
uvw1               684          704           20         12.82 +/- 0.05

Aperture photometry shows initially a completely saturated detector,
leading
to wh < 13.8 mag. The first exposure in the white filter (tstart=T0+92s)
shows a readout streak but the readout streak traverses also another
relatively bright star which leads to a saturated readout streak
and precludes using that method of determining the magnitude (Page
et al, 2013 MNRAS 436, 1684).   Analysis continues.

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: GRB191221B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26576
SUBJECT: Konus-Wind observation of GRB 191221B
DATE:    19/12/24 15:30:57 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 191221B (Swift detection:  Laha et al., GCN 26534;
AGILE/MCAL detection: Longo et al., GCN 26549;
AstroSat CZTI detection: Gaikwad et al., GCN 26567)
triggered Konus-Wind (KW) at T0=74349.647 s UT (20:39:09.647).

The burst light curve shows a bright pulse with a complex, multi-peaked structure.
The total duration of the burst is ~35 s.
The emission is seen up to ~15 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191221_T74349/

As observed by Konus-Wind, the burst had
a fluence of (1.0 Â± 0.1)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0+8.064,
of (1.9 Â± 0.2)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+21.760 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.81 (-0.06,+0.06),
the high energy photon index beta = -2.47 (-0.24,+0.16),
the peak energy Ep = 377 (-29,+30) keV,
chi2 = 99/97 dof.

The spectrum near the peak count rate (measured from T0+6.912 s
to T0+8.448 s) is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.51 (-0.11,+0.13),
the high energy photon index beta = -2.72 (-0.50,+0.26),
the peak energy Ep = 338 (-36,+38) keV,
chi2 = 64/66 dof.

Assuming the redshift z=1.148 (Vielfaure et al., GCN 26553)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso = (3.6 Â± 0.4)x10^53 erg,
the peak luminosity L_iso = (1.5 Â± 0.16)x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum Ep,z=(810 Â± 65) keV.
With these values, GRB 191221B is within 68% prediction bands
for both 'Amati' and 'Yonetoku' relations built for the sample
of 138 long KW GRBs with known redshifts (Tsvetkova et al., ApJ 850 161, 2017),
see http://www.ioffe.ru/LEA/GRBs/GRB191221_T74349/GRB191221B.pdf

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


GRB_name: GRB191225A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26579
SUBJECT: GRB 191225A: Fermi GBM Final Real-time Localization
DATE:    19/12/25 07:35:21 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 07:25:16 UT on 25 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191225A (trigger 598951521.49675 / 191225309).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 95.5, Dec = -17.4 (J2000 degrees, equivalent to J2000 06h 21m, -17d 23'), with a statistical uncertainty of 6.7 degrees.

The angle from the Fermi LAT boresight is 66.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191225309/quicklook/glg_skymap_all_bn191225309.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191225309/quicklook/glg_healpix_all_bn191225309.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191225309/quicklook/glg_lc_medres34_bn191225309.gif


GRB_name: GRB191221B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26580
SUBJECT: GRB 191221B: ATCA detection of the radio afterglow
DATE:    19/12/25 16:43:35 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (University of Bath), S. Bhandari (CSIRO), K. D.
Alexander (Northwestern), E. Berger (Harvard), R. Chornock (Ohio U.), D.
Coppejans (Northwestern), M. Drout (U. Toronto), H. van Eerten (University
of Bath), Wen-fai Fong (Northwestern), C. Guidorzi (U. Ferrara), G.
Hosseinzadeh (Harvard), R. Margutti (Northwestern), C. G. Mundell
(University of Bath), and P. Schady (University of Bath) report:

"We observed GRB 191221B (Laha et al., GCN 26534) with the Australia
Telescope Compact Array (ATCA) at multiple frequencies and multiple epochs
beginning on 2019 December 22 14:17 UT (0.73 days after the burst). We
detect a varying radio counterpart at 5.5, 9.0, 16.7, and 21.2 GHz at a
position consistent with the X-ray position (Beardmore et al., GCN 26540)
and optical position (Lipunov et al., GCN 26537). We identify this source
as the radio afterglow of GRB 191221B.

Further analysis and observations are on-going.

We thank the CSIRO staff for approving these observations."


GRB_name: GRB191225B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26581
SUBJECT: GRB 191225B: Fermi GBM Final Real-time Localization
DATE:    19/12/25 17:47:56 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 17:37:51 UT on 25 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191225B (trigger 598988276.867438 / 191225735).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 145.8, Dec = -7.2 (J2000 degrees, equivalent to J2000 09h 43m, -7d 12'), with a statistical uncertainty of 2.8 degrees.

The angle from the Fermi LAT boresight is 61.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191225735/quicklook/glg_skymap_all_bn191225735.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191225735/quicklook/glg_healpix_all_bn191225735.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191225735/quicklook/glg_lc_medres34_bn191225735.gif


GRB_name: GRB191225B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26583
SUBJECT: GRB 191225B: BALROG localization (Fermi Trigger 598988276 / GRB 191225735)
DATE:    19/12/25 18:02:04 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
598988276 at 17:37:51 on 25 Dec. 2019 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 144.1+/-1.7 deg
Decl.(2000.0) = -7.2+/-0.8 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB191225735/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB191225735/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB191225735/json

                        


GRB_name: GRB191227A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26593
SUBJECT: GRB 191227A: Fermi GBM Final Real-time Localization
DATE:    19/12/27 01:49:48 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 01:39:24 UT on 27 Dec 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 191227A (trigger 599103569.720864 / 191227069).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 319.7, Dec = -13.2 (J2000 degrees, equivalent to J2000 21h 18m, -13d 11'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 93.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191227069/quicklook/glg_skymap_all_bn191227069.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191227069/quicklook/glg_healpix_all_bn191227069.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn191227069/quicklook/glg_lc_medres34_bn191227069.gif


GRB_name: GRB191227A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26595
SUBJECT: GRB 191227A: Swift detection of a burst
DATE:    19/12/27 01:52:07 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), N. J. Klingler (PSU),
S Laha (GSFC/UMBC/CRESST), A. Y. Lien (GSFC/UMBC) and M. J. Moss (GWU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 01:39:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191227A (trigger=946344).  Swift did not slew immediately
due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 319.170, -16.704 which is 
   RA(J2000) = 21h 16m 41s
   Dec(J2000) = -16d 42' 15"
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 30 sec.  The peak count rate
was ~12000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 15:10 UT on 2020 March 23. There will thus be no XRT or
UVOT data for this trigger before this time. 

Burst Advocate for this burst is A. Melandri (andrea.melandri 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/)


GRB_name: GRB191227A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26596
SUBJECT: Swift GRB191227A: Global MASTER-Net OT detection
DATE:    19/12/27 02:46:31 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

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

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

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

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

MASTER-OAFA robotic telescope (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan 
National University) was pointed to the  GRB191227.07 31 sec after notice 
time and 51 sec after trigger time at 2019-12-27 01:40:28 UT. On our first 
(10s exposure)  set we  found 1 optical transient within Swift error-box 
(ra=319.167 dec=-16.7033 r=0.05) brighter than  15.3.


  T-Tmid      Date      Time       Expt.        Ra                Dec           Mag
---------|---------------------|-------|-----------------|-----------------|-------
       56   2019-12-27 01:40:28      10   (21h 16m 37.28s , -16d 43m 33.5s)     14.4

The 5-sigma upper limit has been about  15.3mag
The message may be cited.



The OT has irregular early time  behaviour since 51.1 till 501.5 seconds 
after the trigger.


The galactic latitude b = -40 deg., longitude l = 34 deg.
The observations made on zenith distance = 83 deg.The moon ( 1 % bright 
part) below the horizon (The altitude of the Moon is -14 deg. ).
The sun  altitude  is -20.6 deg.


GRB_name: GRB191227A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26597
SUBJECT: GRB 191227A: MITSuME Akeno optical upper limits
DATE:    19/12/27 10:31:08 GMT
FROM:    Adachi Ryo at Tokyo Institute of Tech  <adachi@hp.phys.titech.ac.jp>

R. Adachi, K. L. Murata, M. Oeda, K.Shiraishi, K. Iida, M. Niwano, F.
Ogawa, R. Hosokawa, S. Toma, N. Nakamura, Y. Yatsu, and N. Kawai
(TokyoTech) report on behalf of the MITSuME collaboration:

We observed the field of the optical counterpart (V. Lipunov et al.
#26596) of GRB 191227A (The Fermi GBM team #26593, A. Melandri et al.
#26595) with the optical three color (gâ€™, Rc, and Ic) CCD cameras
attached to the MITSuME 50 cm telescope of Akeno Observatory,
Yamanashi, Japan.

The observation started on 19/12/27 08:08:42.73 UT. We did not detect
the optical counterpart in all three bands. We obtained the following
5-sigma limits for the magnitudes.

T0+[hour]    MID-UT T-EXP[sec]   5-sigma limits
-----------------------------------------------------------------------------------------------------
~6.75        08:57:46.67 3360         gâ€™>17.4, Rc>16.9, Ic>16.2
-----------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used UCAC4 catalog for flux calibration.
The magnitudes are expressed in the AB system.


GRB_name: GRB191227A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26598
SUBJECT: GRB 191227A: Marginal detection by Fermi-LAT
DATE:    19/12/27 17:15:42 GMT
FROM:    Francesco Longo at U of Trieste,INFN Trieste  <franzlongo1969@gmail.com>

F. Fana Dirirsa (Univ. of Johannesburg), F. Longo (University & INFN,
Trieste), M. Axelsson (KTH & Stockholm Univ.),
D. Kocevski (NASA/MSFC) and J. Racusin (NASA/GSFC) report on behalf of
the Fermi-LAT team:

On December 27, 2019, Fermi-LAT marginally detected high-energy emission from
GRB 191227A, which was also detected by Fermi-GBM (GCN 26593) and
Swift/BAT (Melandri et al, GCN 26595).
The best LAT on-ground location is found to be

RA, Dec 318.0, -16.9 (degrees, J2000)

with an error radius of 0.33 deg (90% containment, statistical error only).

This was 96 deg from the LAT boresight at the time of the GBM trigger
and entered in the LAT field of view around
1 ks later. The localisation is consistent with the Swift/BAT position.

The detection significance lies just below the 5-sigma threshold, but
more than 3 photons with >90% probability to
be associated with the GRB are found in the time interval up to 10ks
after the GBM trigger. The photon flux above
100 MeV in this time interval is (9 +/- 4) e-7 ph/cm2/s.

The estimated photon index above 100 MeV is -2.0 +/- 0.3.

Further analysis is ongoing.

The Fermi-LAT point of contact for this burst is Feraol Fana Dirirsa
(fdirirsa@uj.ac.za)

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: GRB191227A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26599
SUBJECT: GRB 191227A: Fermi GBM detection
DATE:    19/12/27 22:44:34 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

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

"At 01:39:24.72 UT on 27 December 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 191227A(trigger 599103569 / 191227069),
which was also detected by the Swift/BAT (Melandri et al. 2019, GCN 26595)
and Fermi LAT (Fana Dirirsa et al. 2019, GCN 26598).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 96
degrees.

The GBM light curve consists of multiple overlapping pulses
with a duration (T90) of about 25 s (50-300 keV).
The time-averaged spectrum from T0+8.19 s to T0+37.88 s is
best fit by a Band function with Epeak = 362 +/- 10 keV,
alpha = -0.93 +/- 0.01 and beta = -2.36 +/- 0.07.

The event fluence (10-1000 keV) in this time interval is
(7.30 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+15.8 s in the 10-1000 keV band
is 38.0 +/- 0.5 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB191228A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26601
SUBJECT: GRB 191228A: Swift detection of a burst
DATE:    19/12/28 00:18:33 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. G. Bernardini (INAF-OAB), S. D. Barthelmy (GSFC),
P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), S Laha (GSFC/UMBC/CRESST),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), M. J. Moss (GWU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 00:01:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191228A (trigger=946476).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 5.339, -8.670, which is 
   RA(J2000)  =  00h 21m 21s
   Dec(J2000) = -08d 40' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve is typically plain for an image trigger. 

The XRT began observing the field at 00:03:23.2 UT, 123.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 5.34755, -8.68313 which is
equivalent to:
   RA(J2000)  = 00h 21m 23.41s
   Dec(J2000) = -08d 40' 59.3"
with an uncertainty of 3.7 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 https://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 in excess of the Galactic value (3.80 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.4
(+5.17/-3.93) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 0.1 s image was 1.26e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 131 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
0.04. 

Burst Advocate for this burst is M. G. Bernardini (grazia.bernardini 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/)


GRB_name: GRB191228A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26603
SUBJECT: GRB 191228A: UKIRT NIR upper limit
DATE:    19/12/28 07:36:11 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu, Z.P. Zhu, B.Y. Yu, H.J. Wang, L. Ge (NAOC) report:

We observed the field of GRB 191228A (Bernardini et al., GCN 26601) 
using the 3.8-m United Kingdom Infra-Red Telescope (UKIRT). Observations 
started at 04:38:02 UT on 2019-12-28 (i.e., 4.612 hr after the BAT 
trigger), and 3600 s H-band imagining was obtained in a seeing of ~1.0".

No NIR afterglow is detected in the stacked image at the XRT position 
(Bernardini et al., GCN 26601), down to a limiting magnitude of H ~ 
20.1, calibrated with nearby 2MASS stars.

We thank the great support of the UKIRT staff/observer, in particular 
Michael Pohlen and Watson Varricatt.


GRB_name: GRB191228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26604
SUBJECT: GRB 191228A: ePESSTO+ NTT optical upper limit
DATE:    19/12/28 10:11:51 GMT
FROM:    Daniele B Malesani at DTU Space  <malesani@space.dtu.dk>

Tomas Mueller (Southampton), Juanita Antilen (Universidad de Chile), 
Daniele B. Malesani (DTU Space), Paolo D'Avanzo (INAF/Brera), Joe 
Anderson (ESO), Mariusz Gromadzki (Warsaw), Cosimo Inserra (Cardiff), 
Erkki Kankare (Turku), Matt Nicholl (Birmingham), Ofer Yaron (Weizmann), 
David Young (QUB), Roberta Carini (INAF/Roma), Regis Cartier (CTIO), 
Ting-Wan Chen (Stockholm), Matt Grayling, Mat Smith, Phil Wiseman 
(Southampton), Chris Frohmaier (ICG Portsmouth), report:

We observed GRB 191228A (Bernardini et al., GCN 26601) under the the 
extended Public ESO Spectroscopic Survey for Transient Objects 
(ePESSTO+; see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ). 
The observations were performed on the ESO New Technology Telescope at 
La Silla with the EFOSC2 instrument in imaging mode, starting on 2019 
Dec 28 at 01:22:23 UT (i.e. 1.35 hr after the burst).

In a 2-minute image taken using the r filter, we detect no objects 
consistent with the XRT position, down to a 3-sigma limiting magnitude 
of r = 22.6 AB (calibrated against stars from the Pan-STARRS catalog).


GRB_name: GRB191228A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26606
SUBJECT: GRB 191228A: Enhanced Swift-XRT position
DATE:    19/12/28 17:21:03 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 2775 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 191228A, 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 = 5.34686, -8.68275 which is equivalent
to:

RA (J2000): 00h 21m 23.25s
Dec (J2000): -08d 40' 57.9"

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: GRB191228A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26607
SUBJECT: GRB 191228A: Swift-BAT refined analysis
DATE:    19/12/28 17:38:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

T. N. Ukwatta (LANL) S. D. Barthelmy (GSFC), M. G. Bernardini (INAF-OAB),
J. R. Cummings (CPI), H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
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-60 to T+243 sec from the recent telemetry downlinks,
we report further analysis of BAT GRB 191228A (trigger #946476)
(Bernardini, et al., GCN Circ. 26601).  The BAT ground-calculated position is
RA, Dec = 5.341, -8.650 deg, which is 
   RA(J2000)  =  00h 21m 21.9s 
   Dec(J2000) = -08d 38' 58.3" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 90%.
 
The mask-weighted light curve] shows 3 broad peaks starting at T-50 sec
with peaks at ~T+5, ~T+55, and ~T+130 sec, and ending at T+190 sec.
T90 (15-350 keV) is 166.9 +- 10.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-39.2 to T+138.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.06 +- 0.14.  The fluence in the 15-150 keV band is 2.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+54.59 sec in the 15-150 keV band
is 0.6 +- 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/946476/BA/


GRB_name: GRB191227A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26608
SUBJECT: GRB 191227A: Swift-BAT refined analysis
DATE:    19/12/28 17:57:54 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), A. Melandri (INAF-OAB),
D. M. Palmer (LANL), T. Sakamoto (AGU),
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 191227A (trigger #946344)
(Melandri et al., GCN Circ. 26595).  The BAT ground-calculated position is
RA, Dec = 319.172, -16.717 deg which is
   RA(J2000)  =  21h 16m 41.4s
   Dec(J2000) = -16d 43' 02.5"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 13%.

The mask-weighted light curve shows many overlapping pulses
that starts from ~T-30 s and ends at ~T+105 s. Several obvious peaks
can be seen at ~T0, ~T+3 s, ~T+5 s, and ~T+11 s, respectively.
T90 (15-350 keV) is 58.5 +- 14.4 sec (estimated error including
systematics).

The time-averaged spectrum from T-30.55 to T+105.93 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.30 +- 0.05.  The fluence in the 15-150 keV band is 2.5 +- 0.1 x 10^-5
erg/cm2.
The 1-sec peak photon flux measured from T+5.28 sec in the 15-150 keV band
is 21.8 +- 1.3 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/946344/BA/


GRB_name: GRB191228A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26609
SUBJECT: GRB 191228A: Swift-XRT refined Analysis
DATE:    19/12/28 19:22:36 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J. D. Gropp (PSU), A. Tohuvavohu (U. Toronto), J.A. Kennea (PSU), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA) and
M.G. Bernardini report on behalf of the Swift-XRT team:

We have analysed 7.7 ks of XRT data for GRB 191228A (Bernardini et al.
GCN Circ. 26601), from 127 s to 48.0 ks after the  BAT trigger. The
data comprise 216 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN Circ. 26606).

The late-time light curve (from T0+5.4 ks) can be modelled with a
power-law decay with a decay index of alpha=1.58 (+0.13, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.96 (+/-0.05). The
best-fitting absorption column is  3.09 (+0.24, -0.23) x 10^21 cm^-2,
in excess of the Galactic value of 3.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.14 (+0.16, -0.15)
and a best-fitting absorption column of 4.0 (+/-0.7) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (6.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.0 (+/-0.7) x 10^21 cm^-2
Galactic foreground: 3.8 x 10^20 cm^-2
Excess significance: 8.7 sigma
Photon index:      2.14 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.58, the count rate at T+24 hours will be 8.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.9 x
10^-13 (5.0 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/00946476.

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


GRB_name: GRB191225A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26610
SUBJECT: GRB 191225A : AstroSat CZTI detection
DATE:    19/12/29 09:13:02 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 191225A, which was also detected by Fermi GBM Final Real-time Localization ( GCN #26579).

The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak of emission  peaking at 2019-12-25 07:25:16.0 UT. The measured peak count rate associated with the burst is 241 cts/s above the background in the combined data of four quadrants, with a total of 435 cts. The local mean background count rate was 545 cts/s. Using cumulative rates, we measure a T90 of 6.9 s.

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: GRB191228A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26611
SUBJECT: GRB 191228A: Swift/UVOT Upper Limits
DATE:    19/12/29 21:38:22 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

 GRB 191228A: Swift/UVOT Upper Limits

J. D. Gropp (PSU) and M. G. Bernardini (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 191228A
131 s after the BAT trigger (Bernardini et al., GCN Circ. 26601).
No optical afterglow consistent with the XRT position
(Bernardini et al. GCN Circ. 26601)
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           131          281          147         >20.3
u_FC               289          539          246         >19.6
white              131         1009          327         >20.6
v                  619          811           39         >18.2
b                  545          737           39         >19.2
u                  289          712          265         >19.6
w1                 668          860           39         >18.4

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: GRB191227B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26612
SUBJECT: IPN triangulation of GRB 191227B (short)
DATE:    19/12/30 12:40:46 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

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

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

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

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

The very bright, short-duration GRB 191227B was detected by
Fermi (GBM trigger 599160109), Mars-Odyssey (HEND), Konus-Wind,
and Swift (BAT) at about 62504 s UT (17:21:44).
The burst was outside the coded field of view of the BAT.

We have triangulated it to two preliminary, 3 sigma error boxes
whose coordinates are:
Box 1:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   256.466 (17h 05m 52s) -26.739 (-26d 44' 19")
  Corners:
   256.590 (17h 06m 22s) -26.856 (-26d 51' 20")
   256.273 (17h 05m 05s) -27.785 (-27d 47' 06")
   256.342 (17h 05m 22s) -26.619 (-26d 37' 09")
   256.724 (17h 06m 54s) -25.195 (-25d 11' 40")
  ---------------------------------------------

  Box 2:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   257.405 (17h 09m 37s) -19.765 (-19d 45' 52")
  Corners:
   257.550 (17h 10m 12s) -19.678 (-19d 40' 41")
   257.500 (17h 10m 00s) -18.708 (-18d 42' 29")
   257.260 (17h 09m 02s) -19.853 (-19d 51' 12")
   257.244 (17h 08m 59s) -21.319 (-21d 19' 08")
  ---------------------------------------------
The area of each error box is 1162 sq. arcmin,
and their maximum dimension is 2.62 deg
(the minimum one is 14.16 arcmin).
The Sun distance for each box was ~18 deg.

These error boxes are both consistent with the GBM localization.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB191227_T62500/IPN

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB191227B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26613
SUBJECT: Konus-Wind observation of GRB 191227B
DATE:    19/12/30 12:56:09 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The short-duration GRB 191227B
(IPN triangulation: Hurley et al., GCN Circ. 26612)
triggered Konus-Wind at T0=62500.487 s UT (17:21:40.487).

The burst light curve shows a multi-peaked structure
which starts at ~T0 s and has a total duration of ~0.2 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191227_T62500/

As observed by Konus-Wind, the burst
had a fluence of 8.80(-1.42,+1.40)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.030 s,
of 8.83(-2.12,+2.10)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+0.192 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.56(-0.21,+0.31),
the high energy photon index beta = -2.35(-1.19,+0.38),
the peak energy Ep = 985(-323,+373) keV
(chi2 = 49/49 dof).

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


GRB_name: GRB191227A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26614
SUBJECT: Konus-Wind observation of GRB 191227A
DATE:    19/12/30 13:13:35 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long-duration GRB 191227A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 26593;
Swift-BAT detection: Melandri et al., GCN Circ. 26595;
Stamatikos et al., GCN Circ. 26608;
Fermi-LAT detection: Fana Dirirsa et al., GCN Circ. 26598)
triggered Konus-Wind at T0=5970.414 s UT (01:39:30.414).

The burst light curve shows a multi-peaked structure
which starts at ~T0-27 s and has a total duration of ~52 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB191227_T05970/

As observed by Konus-Wind, the burst
had a fluence of 1.02(-0.08,+0.09)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+8.096 s,
of 1.86(-0.35,+0.36)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+29.440 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.70(-0.12,+0.13),
the high energy photon index beta = -2.28(-0.16,+0.12),
the peak energy Ep = 275(-26,+30) keV
(chi2 = 102/97 dof).

The spectrum near the maximum count rate
(measured from T0+6.400 to T0+13.056 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.65(-0.18,+0.22),
the high energy photon index beta = -2.25(-0.22,+0.15),
the peak energy Ep = 266(-40,+46) keV
(chi2 = 82/97 dof).

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


GRB_name: GRB191228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26615
SUBJECT: GRB 191228A: Mondy optical upper limit
DATE:    19/12/30 15:53:01 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov (HSE), K. Kamyshnikov 
(HSE), E. Mazaeva (IKI), A. Volnova (IKI) report   on behalf of IKI-GRB-FuN:

We observed the field of  GRB 191228A (Bernardini et al.  GCN 26601) 
with AZT-33IK telescope of Sayan observatory (Mondy) starting on Dec. 28 
(UT)  11:15:09.   We  do not detect any optical object in the Enhanced 
Swift-XRT position  (Evans et al.  GCN 26606). Preliminary photometry of 
the field  is following.

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

2019-12-28 11:15:09    0.48923    R     30*120  n/d      20.1

Photometry is based on the USNO-B2.0 nearby stars.


GRB_name: GRB191221B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26616
SUBJECT: GRB 191221B: CALET Gamma-Ray Burst Monitor detection
DATE:    19/12/31 02:44:42 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

S. Sugita, A. Yoshida, T. Sakamoto, V. Pal'shin (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 191221B (Swift detection: Barthelmy et al., GCN Circ. 26534,
Sakamoto et al., GCN Circ. 26562; AGILE/MCAL observations: Longo et al.,
GCN Circ. 26549; AstroSat CZTI detection: Gaikwad et al., GCN Circ. 26567;
Insight-HXMT/HE detection: Xue et al., GCN Circ. 26573;
Konus-Wind observation: Frederiks et al., GCN Circ. 26576;
https://gcn.gsfc.nasa.gov/other/191221B.gcn3) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 20:39:04.868 UTC on 21 December 2019.
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked pulse which starts
at T+1.8 sec, peaks at T+11.3 sec and ends at T+23.4 sec.
The T90 and T50 durations measured by the SGM data are
13.0 +- 1.6 sec and 4.4 +- 0.4 sec (40-1000 keV), respectively.

The ground processed light curve will be available at

http://cgbm.calet.jp/cgbm_trigger/ground/1260995788/

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


GRB_name: GRB191227B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26617
SUBJECT: GRB 191227B: Insight-HXMT/HE observation
DATE:    19/12/31 03:43:14 GMT
FROM:    Yunfei Du at IHEP  <duyunfei@ihep.ac.cn>

Y. F. Du, Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-12-27T17:21:44.14 (T0), Insight-HXMT/HE detected 
GRB 191227B (trigger ID: HEB191227723) in a routine search of the data, 
which was also triggered by Fermi/GBM, IPN and Konus-Wind (GCN #26612).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 0.161 s measured from T0+0.010 s. 
The 1-ms peak rate, measured from T0+0.045 s, is 50,544 cnts/sec. 
The total counts from this burst is 4123 counts. But it should be
noted that the Insight-HXMT/HE detection suffers from saturation 
when the count rate exceeds ~20,000 cnts/sec. The uncorrected 
light curve can be found at:
URL_LC: http://www.hxmt.org/images/GRB/HEB191227723_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB191227A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26618
SUBJECT: GRB 191227A: Insight-HXMT/HE observation
DATE:    19/12/31 09:06:03 GMT
FROM:    Yunfei Du at IHEP  <duyunfei@ihep.ac.cn>

Y. F. Du, Y. G. Zheng, C. Cai, Q. Luo, S. Xiao, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2019-12-27T01:39:34.400 (T0), Insight-HXMT/HE detected 
GRB 191227A (trigger ID: HEB191227069) in a routine search of the data, 
which was also triggered by Fermi/GBM, Swift/BAT and Konus-Wind (GCN #26593).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 20.65 s measured from T0+0.40 s. 
The 1-ms peak rate, measured from T0+6.72 s, is 18,542 cnts/sec. 
The total counts from this burst is 118,722 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB191227069_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200101A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26624
SUBJECT: GRB 200101A: Fermi GBM Final Real-time Localization
DATE:    20/01/01 20:49:47 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 20:39:26 UT on 1 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200101A (trigger 599603971.45143 / 200101861).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 257.4, Dec = -35.1 (J2000 degrees, equivalent to J2000 17h 09m, -35d 06'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 61.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200101861/quicklook/glg_skymap_all_bn200101861.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200101861/quicklook/glg_healpix_all_bn200101861.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200101861/quicklook/glg_lc_medres34_bn200101861.gif


GRB_name: GRB200101A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26625
SUBJECT: GRB 200101A: BALROG localization (Fermi Trigger 599603971 / GRB 200101861)
DATE:    20/01/01 21:03:40 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
599603971 at 20:39:26 on 01 Jan. 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 259.1+/-0.4 deg
Decl.(2000.0) = -32.7+/-0.4 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200101861/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200101861/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200101861/json

                        


GRB_name: GRB200101A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26627
SUBJECT: GRB 200101A: Fermi GBM detection
DATE:    20/01/02 03:23:50 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres and C. Meegan (both UAH)
report on behalf of the Fermi GBM Team:

"At 20:39:26.45 UT on 1 January 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200101A (trigger 599603971 / 200101861).

The location for this GRB was reported in the Fermi GBM Final Real-time
Localization GCN (GCN 26624).

The GBM light curve shows of multiple pulses
with a duration (T90) of about 10 s (50-300 keV).
The time-averaged spectrum from T0+3.3 s to T0+19.8 s is
best fit by a Band function with Epeak = 595 +/- 13 keV,
alpha = -0.82 +/- 0.01, and beta = -2.15 +/- 0.03.

The event fluence (10-1000 keV) in this time interval is
(9.38 +/- 0.05)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+11.5 s in the 10-1000 keV band
is 124.8 +/- 0.6 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB191228A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26630
SUBJECT: GRB 191228A: Early Optical Upper Limits from LCO
DATE:    20/01/02 12:22:34 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (U. of the Virgin Islands/College of Marin) report on behalf of a larger collaboration:

We observed Swift GRB 191228A (Barthelmy et al., GCN 26601) with the LCO 1-m Sinistro instrument at the McDonald Observatory, Texas, USA site, on December 28, from 00:59 to 01:31 UT (corresponding to 0.66 to 1.22 hours from the GRB trigger time) with Bessel R and I filters.

We performed a series of 5x180s exposures in both bands. We do not detect any sources in the individual frames (nor in 5 stacked images in each band) in the enhanced Swift error region (Barthelmy et al., GCN 26607).  Using the USNO-B.1 catalog as reference, we obtain the following 3-sigma upper limits:

R > 14.69
I > 14.79

The low limiting magnitudes are most likely due to high sky background in the images in both bands.


GRB_name: GRB200101A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26632
SUBJECT: GRB 200101A : AstroSat CZTI detection
DATE:    20/01/02 17:58:05 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 200101A, which was also detected by Fermi GBM Final Real-time Localization (GCN #26624), Global MASTER-Net (Lipunov V. et al., GCN #26626), BALROG localization (Kunzweiler F. et al., GCN #26625) and Fermi GBM (Veres P. et al., GCN #26627).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peak of emission with strongest peak at 2020-01-01 20:39:27.0 UT. The measured peak count rate associated with the burst is 1588 cts/s above the background in the combined data of four quadrants, with a total of 6659 cts. The local mean background count rate was 570 cts/s. Using cumulative rates, we measure a T90 of 16.69 s. In preliminary analysis, we find that 497 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB200103A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26634
SUBJECT: GRB 200103A: Fermi GBM Final Real-time Localization
DATE:    20/01/03 16:27:12 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely SHORT GRB

At 16:16:50 UT on 3 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200103A (trigger 599761015.018562 / 200103678).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 355.4, Dec = -38.4 (J2000 degrees, equivalent to J2000 23h 41m, -38d 23'), with a statistical uncertainty of 16.7 degrees.

The angle from the Fermi LAT boresight is 86.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200103678/quicklook/glg_skymap_all_bn200103678.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200103678/quicklook/glg_healpix_all_bn200103678.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200103678/quicklook/glg_lc_medres34_bn200103678.gif


GRB_name: GRB200101A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26635
SUBJECT: IPN triangulation of GRB 200101A
DATE:    20/01/03 17:19:30 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

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

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team, and

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

The long-duration, extremely bright GRB 200101A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 26624;
Veres and Meegan, GCN Circ. 26627;
BALROG localization: Kunzweiler et al., GCN Circ. 26625;
AstroSat CZTI detection: Gaikwad et al., GCN Circ. 26632)
was detected by Konus-Wind, Fermi (GBM trigger 599603971),
Mars-Odyssey (HEND), and AstroSat(CZTI) at about 74366 s UT (20:39:26).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  258.995 (17h 15m 59s) -32.304 (-32d 18' 14")
 Corners:
  259.549 (17h 18m 12s) -31.755 (-31d 45' 20")
  258.488 (17h 13m 57s) -33.470 (-33d 28' 11")
  258.436 (17h 13m 45s) -32.806 (-32d 48' 22")
  259.506 (17h 18m 01s) -30.953 (-30d 57' 11")
 ---------------------------------------------
The error box area is about 2611 sq. arcmin, and its maximum
dimension is 2.7 deg (the minimum one is 21.8 arcmin).
The Sun distance was about 21 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM one.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200101_T74367/IPN/

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


GRB_name: GRB200101A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26637
SUBJECT: Konus-Wind observation of GRB200101A
DATE:    20/01/05 21:44:21 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration, hard-spectrum, very bright GRB200101A
(Fermi GBM detection: Veres & Meegan, GCN 26627;
AstroSat CZTI detection: Gaikwad et al., GCN 26632;
IPN triangulation: Hurley et al., GCN 26635)
triggered Konus-Wind at T0=74367.095 s UT (20:39:27.095).

The burst light curve shows a a double-peaked structure
which starts at ~T0-8.3 s and has a total duration of~81.8 s
The emission is seen up to ~20 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.43(-0.09,+0.09)x10^-4 erg/cm2,
and a 64-ms peak energy flux, measured from T0+7.776 s,
of 1.12(-0.12,+0.12)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+17.408 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.74(-0.06,+0.07),
the high energy photon index beta = -2.45(-0.23,+0.16),
the peak energy Ep = 552(-46,+49) keV,
chi2 = 103/97 dof.

The spectrum near the peak count rate
(measured from T0+7.680 to T0+7.936 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.43(-0.15,+0.18),
the high energy photon index beta = -2.06(-0.15,+0.11),
the peak energy Ep = 610(-105,+124) keV,
chi2 = 50/55 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200101_T74367/

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


GRB_name: GRB200105A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26638
SUBJECT: GRB 200105A: MAXI/GSC detection
DATE:    20/01/06 00:53:30 GMT
FROM:    Satoshi Sugita at Aoyama Gakuin U.  <sugita@phys.aoyama.ac.jp>

S. Sugita, M. Serino (AGU),
H. Negoro, M. Nakajima, W. Maruyama, M. Aoki, K. Kobayashi, R. Takagi
(Nihon U.),
T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, M. Oeda, K. Shiraishi (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, R.
Shimomukai, M. Tominaga (JAXA),
Y. Ueda, A. Tanimoto, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake
(Kyoto U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, S. Iwahori, Y. Kurihara, K. Kurogi, K. Miike (Miyazaki U.),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU),
M. Sugizaki (NAOC)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray
transient source at 21:55:28 UT on 2020 January 05.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (319.281 deg, -35.846 deg) = (21 17 07, -35 50 45) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.11 deg and 0.1 deg, respectively.
The roll angle of long axis from the north direction is 27.0 deg
counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90%
containment radius).

Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(318.473, -35.441) deg = (21 13 53, -35 26 27) (J2000)
(318.374, -35.646) deg = (21 13 29, -35 38 45) (J2000)
(320.376, -36.262) deg = (21 21 30, -36 15 43) (J2000)
(320.470, -36.054) deg = (21 21 52, -36 03 14) (J2000)

The X-ray flux averaged over the scan was 710 +- 50 mCrab
(4.0-10.0keV, 1 sigma error).

There was no significant excess flux in the previous transit at 20:42 UT
with an upper limit of 20 mCrab.


GRB_name: GRB191228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26653
SUBJECT: GRB 191228A: FRAM-ORM optical limit
DATE:    20/01/07 11:00:43 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek (ASU CAS Ondrejov, CZ), Sergey Karpov, Martin
Masek, Petr Janecek, Jakub Jurysek, Jan Ebr, Ronan Cunniffe,
Petr Travnicek, Michael Prouza (Institute of Physics, Prague,
CZ) and Jan Strobl (ASU CAS Ondrejov, CZ)

report:

The 25cm robotic telescope FRAM-CTA at La Palma (Spain) reacted
robotically under inferior weather conditions to the alert of
GRB 191228A (Bernardini et al., GCN Circular 26601) and obtained
a set of 20s unfiltered images starting at 00:03:11.1 UT, i.e.
112s after the initial BAT trigger.

We do not detect any new source in comparison to USNO-B1.0
catalog neither in single images nor in a combined 20x20s frame
(mean exp time 363s post trigger, 3-sigma limit R>~17.7).


GRB_name: GRB200107B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26659
SUBJECT: GRB 200107B: Fermi GBM Final Real-time Localization
DATE:    20/01/07 19:36:52 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 19:26:22 UT on 7 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200107B (trigger 600117987.8063 / 200107810).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 356.9, Dec = -80.1 (J2000 degrees, equivalent to J2000 23h 47m, -80d 05'), with a statistical uncertainty of 8.3 degrees.

The angle from the Fermi LAT boresight is 61.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200107810/quicklook/glg_skymap_all_bn200107810.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200107810/quicklook/glg_healpix_all_bn200107810.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200107810/quicklook/glg_lc_medres34_bn200107810.gif


GRB_name: GRB200107B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26661
SUBJECT: GRB 200107B: Swift detection of a burst
DATE:    20/01/07 20:32:11 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <siegel@swift.psu.edu>

M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB),
J. A. Kennea (PSU), N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL),
S. J. LaPorte (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), M. J. Moss (GWU),
K. L. Page (U Leicester), D. M. Palmer (LANL), B. Sbarufatti (PSU),
M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 19:26:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200107B (trigger=948219).  Swift did not slew immediately 
due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 107.066, -83.716 which is 
   RA(J2000) = 07h 08m 16s
   Dec(J2000) = -83d 42' 56"
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 80 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~35 sec after the trigger. 

The XRT began observing the field at 19:41:27.6 UT, 899.0 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 106.92567, -83.7189 which is
equivalent to:
   RA(J2000)  = 07h 07m 42.16s
   Dec(J2000) = -83d 43' 08.0"
with an uncertainty of 21.3 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 https://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 1.49
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 902 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image processing
FAILED because of no aspect solution. Results from the list of sources
generated on-board are not available at this time. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.19. 

The "B" burst name is based on the Fermi/GBM detection 
circular of this burst (GCN Circ. 26659). 

Burst Advocate for this burst is M. G. Bernardini (grazia.bernardini 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/)


GRB_name: GRB200101A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26663
SUBJECT: GRB 200101A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/01/08 02:32:40 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

Y. Kawakubo (LSU),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long bright GRB 200101A (Fermi-GBM detection: The Fermi GBM team,
GCN Circ. 26624, Veres and Meegan, GCN Circ. 26627; BALROG localization:
Kunzweiler et al., GCN Circ. 26625; AstroSat CZTI detection:
Gaikwad et al., GCN Circ. 26632; IPN triangulation: Hurley, GCN Circ. 26635;
Konus-Wind observation: Tsvetkova et al., GCN Circ. 26637;
https://gcn.gsfc.nasa.gov/other/200101A.gcn3) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 20:39:30.398 UTC on 1 January 2020.
The burst signal was seen by all CGBM detectors.
Because of a server problem no CGBM GCN notice was automatically
distributed for this event.

The burst light curve shows the main emission episode with two
multi-peaked pulses which starts at T-8.0 sec, peaks at T+8.0 sec and ends
at T+16.8 sec, followed by a weak pulse at ~T0+75 sec.The T90 and T50
durations measured by the SGM data are 15.4 +- 12.0 sec and 1.5 +- 0.1 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1261946195/

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


GRB_name: GRB200107B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26670
SUBJECT: GRB 200107B: Swift-BAT refined analysis
DATE:    20/01/08 16:50:49 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

S. D. Barthelmy(GSFC), M.G. Bernardini(INAF-OAB), J. R. Cummings(CPI),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
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 200107B (trigger #948219)
(M. G. Bernardini et al., GCN Circ. 26661).  The BAT ground-calculated position is
RA, Dec = 107.067, -83.716 deg which is
   RA(J2000)  =  07h 08m 16.0s
   Dec(J2000) = -83d 42' 56.5"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.


The mask weighted light curve shows complex multi-peak structures with a duration of ~100 s.
The overall structure starts at ~T-40 s and lasts till ~T+80s.
T90 (15-350 keV) is 86.68 +- 11.64 sec (estimated error including systematics).

The time-averaged spectrum from T-29.86 to T+77.04 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.41 +- 0.10.  The fluence in the 15-150 keV band is 3.0 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+36.09 sec in the 15-150 keV band
is 1.9 +- 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/948219/BA/


GRB_name: GRB200107B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26671
SUBJECT: GRB 200107B: Fermi GBM observation
DATE:    20/01/08 17:47:34 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

GRB 200107B: Fermi GBM observation

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

"At 19:26:22.81 UT on 07 January 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200107B (trigger 600117987 / 200107810),
which was also detected by the Swift/BAT (Bernardini et al. 2020, GCN
26661).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 47
degrees.

The GBM light curve shows a complex, multi-peaked structure
with a duration (T90) of about 81 s (50-300 keV).
The time-averaged spectrum from T0+4 s to T0+44 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.1 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 412 +/- 138 keV.

The event fluence (10-1000 keV) in this time interval is
(1.29 +/- 0.15)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+41.0 s in the 10-1000 keV band is 3.3 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB200107B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26672
SUBJECT: Swift GRB 200107B: Global MASTER-Net observations report 
DATE:    20/01/08 19:28:40 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

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

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev, O.Ershova 
(Irkutsk State University, API),

A. Tlatov, D. Dormidontov 
(Kislovodsk Solar Station of the Pulkovo Observatory),

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 200107B ( M. G. Bernardini et al., GCN 26661) errorbox  891 sec after notice time and 29 sec after trigger time at 2020-01-07 19:42:11 UT, with upper limit up to  18.7 mag. The observations began at zenith distance = 54 deg. The sun  altitude  is -20.2 deg. 

The galactic latitude b = -27 deg., longitude l = 296 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1253675

We obtain a following upper limits.  

Tmid-T0  |          Site       |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________

     119 |         MASTER-SAAO |  P\ |   180 | 17.1 |        
     415 |         MASTER-SAAO |  P\ |   180 | 17.4 |        
     616 |         MASTER-SAAO |  P\ |   180 | 17.4 |        
     818 |         MASTER-SAAO |  P\ |   180 | 16.6 |        
    1231 |         MASTER-SAAO |   C |   180 | 18.3 |        
    1348 |         MASTER-SAAO |  P\ |   180 | 17.4 |        
    1550 |         MASTER-SAAO |  P\ |   180 | 17.4 |        
    1751 |         MASTER-SAAO |  P\ |   180 | 17.5 |        
    1953 |         MASTER-SAAO |  P\ |   180 | 17.3 |        
    2161 |         MASTER-SAAO |   C |   180 | 18.6 |        
    2371 |         MASTER-SAAO |   C |   180 | 18.5 |        
    2582 |         MASTER-SAAO |   C |   180 | 18.5 |        
    2792 |         MASTER-SAAO |   C |   180 | 18.5 |        
    3001 |         MASTER-SAAO |   C |   180 | 18.6 |        
    3211 |         MASTER-SAAO |   C |   180 | 18.6 |        
    3421 |         MASTER-SAAO |   C |   180 | 18.7 |        
    3632 |         MASTER-SAAO |   C |   180 | 18.5 |        
    3843 |         MASTER-SAAO |   C |   180 | 18.7 |        
    4052 |         MASTER-SAAO |   C |   180 | 18.6 |        
    4261 |         MASTER-SAAO |   C |   180 | 18.6 |        
    4480 |         MASTER-SAAO |   C |   180 | 18.7 |        
    5034 |         MASTER-SAAO |   C |   180 | 17.6 |        
    5247 |         MASTER-SAAO |   C |   180 | 18.6 |        
    5459 |         MASTER-SAAO |   C |   180 | 18.6 |        
    5671 |         MASTER-SAAO |   C |   180 | 18.6 |        
    5884 |         MASTER-SAAO |   C |   180 | 18.6 |        
    6098 |         MASTER-SAAO |   C |   180 | 18.5 |        
    6310 |         MASTER-SAAO |   C |   180 | 18.6 |        
    6523 |         MASTER-SAAO |   C |   180 | 18.5 |        
    6735 |         MASTER-SAAO |   C |   180 | 18.5 |        
    6948 |         MASTER-SAAO |   C |   180 | 18.4 |        
    7160 |         MASTER-SAAO |   C |   180 | 18.4 |        
    7373 |         MASTER-SAAO |   C |   180 | 18.5 |        
    7585 |         MASTER-SAAO |   C |   180 | 18.5 |        
    7799 |         MASTER-SAAO |   C |   180 | 18.6 |        
    8010 |         MASTER-SAAO |   C |   180 | 18.5 |        
    8224 |         MASTER-SAAO |   C |   180 | 18.5 |        
    8471 |         MASTER-SAAO |   C |   180 | 18.6 |        
    8684 |         MASTER-SAAO |   C |   180 | 18.5 |        
    8896 |         MASTER-SAAO |   C |   180 | 18.5 |        
    9109 |         MASTER-SAAO |   C |   180 | 18.5 |        
    9321 |         MASTER-SAAO |   C |   180 | 18.4 |        
    9538 |         MASTER-SAAO |   C |   180 | 18.4 |        
    9752 |         MASTER-SAAO |   C |   180 | 18.5 |        
    9963 |         MASTER-SAAO |   C |   180 | 18.3 |        
   10176 |         MASTER-SAAO |   C |   180 | 18.3 |        
   10389 |         MASTER-SAAO |   C |   180 | 18.3 |        
   10601 |         MASTER-SAAO |   C |   180 | 18.3 |        
Filter C is a clear (unfiltred) band. 


The observation and reduction will continue. 
The message may be cited.


GRB_name: GRB200109A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26677
SUBJECT: GRB 200109A: Fermi GBM Final Real-time Localization
DATE:    20/01/09 01:56:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 01:45:51 UT on 9 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200109A (trigger 600227156.894404 / 200109074).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 284.7, Dec = 68.9 (J2000 degrees, equivalent to J2000 18h 58m, 68d 54'), with a statistical uncertainty of 10.4 degrees.

The angle from the Fermi LAT boresight is 40.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200109074/quicklook/glg_skymap_all_bn200109074.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200109074/quicklook/glg_healpix_all_bn200109074.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200109074/quicklook/glg_lc_medres34_bn200109074.gif


GRB_name: GRB200109A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26678
SUBJECT: GRB 200109A: Swift detection of a burst
DATE:    20/01/09 02:00:28 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU), N. J. Klingler (PSU),
S Laha (GSFC/UMBC/CRESST), D. M. Palmer (LANL), M. H. Siegel (PSU),
K. K. Simpson (PSU) and A. Tohuvavohu (U Toronto) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 01:46:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200109A (trigger=948361).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 307.171, +53.003 which is 
   RA(J2000) = 20h 28m 41s
   Dec(J2000) = +53d 00' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of 70 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 01:47:59.1 UT, 102.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
307.1258, 52.9932 which is equivalent to:
   RA(J2000)  = 20h 28m 30.19s
   Dec(J2000) = +52d 59' 35.5"
with an uncertainty of 2.2 arcseconds (radius, 90% containment). This
location is 104 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
https://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 3.98
x 10^21 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 1.12e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 109 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. Because of the density of catalogued stars, further
analysis is required to report an upper limit for any afterglow in the
sub-image. 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 0.29. 

Burst Advocate for this burst is A. Melandri (andrea.melandri 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/)


GRB_name: GRB200109A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26681
SUBJECT: GRB 200109A: Enhanced Swift-XRT position
DATE:    20/01/09 10:09:58 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 406 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200109A, 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 = 307.12462, +52.99363 which is equivalent
to:

RA (J2000): 20h 28m 29.91s
Dec (J2000): +52d 59' 37.1"

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: GRB200109A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26682
SUBJECT: GRB 200109A: Swift-XRT refined Analysis
DATE:    20/01/09 10:55:47 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), D.N. Burrows (PSU), J. D. Gropp (PSU), A. Tohuvavohu
(U. Toronto), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester),
J.P. Osborne (U. Leicester), A. D'Ai (INAF-IASFPA) and A. Melandri
report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 200109A (Melandri et al.
GCN Circ. 26678), from 91 s to 24.1 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. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 26681).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.9 (+/-0.3). At T+216 s  the decay
steepens to an alpha of 8.0 (+0.0, -3.2) before breaking again at T+262
s to a final decay with index alpha=1.50 (+0.28, -0.38).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.70 (+0.32, -0.30). The
best-fitting absorption column is  6.9 (+2.7, -2.2) x 10^21 cm^-2, in
excess of the Galactic value of 4.0 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 5.2 x 10^-11 (7.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.9 (+2.7, -2.2) x 10^21 cm^-2
Galactic foreground: 4.0 x 10^21 cm^-2
Excess significance: 2.2 sigma
Photon index:      1.70 (+0.32, -0.30)

If the light curve continues to decay with a power-law decay index of
1.50, the count rate at T+24 hours will be 1.3 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.0 x
10^-15 (1.0 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/00948361.

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


GRB_name: GRB200107B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26685
SUBJECT: GRB 200107B: Swift-XRT refined Analysis
DATE:    20/01/09 14:15:43 GMT
FROM:    Paolo D'Avanzo at INAF - OAB  <paolo.davanzo@inaf.it>

M. Perri (ASDC), V. D'Elia (ASDC), B. Sbarufatti (PSU), D.N. Burrows
(PSU), J. D. Gropp (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), A. D'Ai (INAF-IASFPA) and M. G. Bernardini (INAF-OAB)
report on behalf of the Swift-XRT team:

We have analysed 3.4 ks of XRT data for GRB 200107B (Bernardini et al.
GCN Circ. 26661), from 908 s to 139.6 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The refined XRT
position is RA, Dec = 106.9086, -83.7162 which is equivalent to:

RA (J2000): 07 07 38.07
Dec(J2000): -83 42 58.3

with an uncertainty of 4.0 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.0 (+0.3, -0.4).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.5, -0.4). The
best-fitting absorption column is  2.8 (+2.4, -1.3) x 10^21 cm^-2,
consistent with the Galactic value of 1.5 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 3.9 x 10^-11 (5.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.8 (+2.4, -1.3) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.9 (+0.5, -0.4)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00948219.

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


GRB_name: GRB200109A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26689
SUBJECT: GRB 200109A: Fermi GBM observation
DATE:    20/01/09 19:22:09 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 01:45:51.89 UT on 9 January 2020, the Fermi Gamma-Ray Burst Monitor
(GBM) triggered and located GRB 200109A (trigger 600227156 / 200109074),
which also triggered the Swift/BAT approximately 25 s later
(Melandri et al. 2019, GCN 26678). The Fermi GBM Final Real-time
Localization (GCN 26677) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 57
degrees.

The GBM light curve shows a complex structure with a duration (T90) of
about 41 s (50-300 keV). The time-averaged spectrum from T0-0.8 s to
T0+41.2 s is best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.98 +/- 0.08 and the
cutoff energy, parameterized as Epeak, is 449 +/- 109 keV.

The event fluence (10-1000 keV) in this time interval is
(6.9 +/- 0.6)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.7 s 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:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB200109A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26690
SUBJECT: GRB 200109A: Swift/UVOT Upper Limits
DATE:    20/01/09 19:26:41 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 200109A: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and A. Melandri (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200109A
110 s after the BAT trigger (Melandri et al., GCN Circ. 26678).
No optical afterglow consistent with the XRT position
(Melandri et al. GCN Circ. 26678)
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           110          259          147         >20.5
u_FC               268          518          246         >19.0
white              110         1023          295         >20.9
u                  268          518          246         >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.29 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200109A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26692
SUBJECT: GRB 200109A: Swift-BAT refined analysis
DATE:    20/01/09 21:24:27 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
A. Melandri (INAF-OAB), 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 200109A (trigger #948361)
(Melandri et al., GCN Circ. 26678).  The BAT ground-calculated position is
RA, Dec = 307.116, 52.988 deg which is
   RA(J2000)  =  20h 28m 27.7s
   Dec(J2000) = +52d 59' 17.7"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a weak structure with several
overlapping
pulses that start at ~T-30 s to ~T+20 s, followed by a weaker tail
emission that lasts till ~T+100 s. T90 (15-350 keV) is 112.0 +- 32.0 sec
(estimated error including systematics).

The time-averaged spectrum from T-31.45 to T+112.55 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.31 +- 0.14.  The fluence in the 15-150 keV band is 2.1 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+8.05 sec in the 15-150 keV band
is 0.7 +- 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/948361/BA/


GRB_name: GRB200107B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26693
SUBJECT: GRB 200107B: Swift/UVOT Observations
DATE:    20/01/09 22:28:12 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and M. G. Bernardini (INAF-OAB)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200107B
903 s after the BAT trigger (Bernardini et al., GCN Circ. 26661).
Some of the exposures are affected by poor attitude control,
but we have selected observing times for which this is not
a significant issue. A source consistent with the position of the optical  
source reported by Lipunov (GCN Circ. 26660) is weakly detected (2.6 sigma)
in the initial UVOT exposure.

The preliminary detection 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_FC           903         1052           55         19.3 (+0.5/-0.4)
v                 1059         1079           19        >18.6
b                 1157         1177           19        >18.6
u                 1133         3144          179        >19.7
w1                2777         2976          197        >19.5
w2                1208         1228           19        >18.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.19 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200109A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26699
SUBJECT: ANTARES 200108A: No detection by Swift-XRT
DATE:    20/01/10 16:19:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), A. Tohuvavohu (U. Toronto), J.A. Kennea (PSU)
and S.B. Cenko (GSFC) report on behalf of the Swift/XRT team:

Swift performed a series of 19 observations tiling the sky area of the 
Fermi-LAT / ANTARES coincident event ANTARES 200108A (Turley et al., GCN 
Circ. 26674). The observations were centred on RA=02h 49m 56.5s, 
Dec=-18d 05' 17", with a radius of ~50', and were carried out between 
22:53:41 UT on Jan 8 until 00:37:14 UT on Jan 9; the detection of GRB 
200109A subsequently interrupted the campaign. We gathered between 30 s 
and 150 s of exposure per tile, with the typical exposure being 110 s.

No X-ray sources were found, with a typical upper limit of 0.06 ct/sec 
(0.3-10 keV).

Assuming a standard AGN spectrum (NH=3e20, Gamma=1.7) this corresponds 
to a 0.3-10 keV observed flux of 2.6 x 10^-12 erg/cm^-2 s^-1.


GRB_name: GRB200111A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26705
SUBJECT: GRB 200111A: Fermi GBM Final Real-time Localization
DATE:    20/01/11 15:21:25 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 15:11:08 UT on 11 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200111A (trigger 600448273.105796 / 200111633).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 104.5, Dec = 31.7 (J2000 degrees, equivalent to J2000 06h 58m, 31d 41'), with a statistical uncertainty of 3.5 degrees.

The angle from the Fermi LAT boresight is 86.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200111633/quicklook/glg_skymap_all_bn200111633.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200111633/quicklook/glg_healpix_all_bn200111633.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200111633/quicklook/glg_lc_medres34_bn200111633.gif


GRB_name: GRB200109A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26710
SUBJECT: GRB 200109A: Insight-HXMT/HE detection
DATE:    20/01/12 03:04:57 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, Y. F. Du, Y. G. Zheng, C. Cai, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-01-09T01:45:51.89 (T0), Insight-HXMT/HE detected 
GRB 200109A (trigger ID: HEB200109073) in a routine search of the data, 
which also triggered Fermi/GBM (GCN #26689), and Swift (GCN #26678).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 36.405 s measured from T0-0.650 s. 
The 1-ms peak rate, measured from T0+ 9.281 s, is 595 cnts/sec. 
The total counts from this burst is 6014 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB200109073_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200112A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26711
SUBJECT: GRB 200112A: Fermi GBM Final Real-time Localization
DATE:    20/01/12 12:44:39 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 12:36:31 UT on 12 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200112A (trigger 600525396.101104 / 200112525).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 150.1, Dec = 64.4 (J2000 degrees, equivalent to J2000 10h 00m, 64d 24'), with a statistical uncertainty of 2.0 degrees.

The angle from the Fermi LAT boresight is 118.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200112525/quicklook/glg_skymap_all_bn200112525.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200112525/quicklook/glg_healpix_all_bn200112525.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200112525/quicklook/glg_lc_medres34_bn200112525.gif


GRB_name: GRB200112A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26713
SUBJECT: GRB 200112A: BALROG localization (Fermi Trigger 600525396 / GRB 200112525)
DATE:    20/01/12 13:11:45 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
600525396 at 12:36:31 on 12 Jan. 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 147.7+/-6.8 deg
Decl.(2000.0) = 66.5+/-1.4 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200112525/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200112525/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200112525/json

                        


GRB_name: GRB200111A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26714
SUBJECT: GRB 200111A: Insight-HXMT/HE detection
DATE:    20/01/12 13:51:48 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, Y. F. Du, Y. G. Zheng, C. Cai, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-01-11T15:11:07.61 (T0), Insight-HXMT/HE detected 
GRB 200111A (trigger ID: HEB200111632) in a routine search of the data, 
which also triggered Fermi/GBM (GCN #26705).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 8.474 s measured from T0-0.030 s. 
The 1-ms peak rate, measured from T0+5.459 s, is 1355 cnts/sec. 
The total counts from this burst is 2111 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB200111632_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200112A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26729
SUBJECT: GRB 200112A: AstroSat CZTI detection
DATE:    20/01/13 12:11:04 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 200112A, which was also detected by Fermi GBM Final Real-time Localization (GCN #26711) and BALROG localization (Biltzinger B. et al., GCN #26713).

The source was clearly detected in the 40-200 keV energy range. The light curve showed a single peak of emission peaking at 2020-01-12 12:36:31.0 UT. The measured peak count rate associated with the burst is 688 cts/s above the background in the combined data of four quadrants, with a total of 2590 cts. The local mean background count rate was 536 cts/s. Using cumulative rates, we measure a T90 of 11.9 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB200114A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26735
SUBJECT: GRB 200114A: Fermi GBM Final Real-time Localization
DATE:    20/01/14 03:51:01 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

The Fermi GBM team reports the detection of a likely LONG GRB

At 03:40:43 UT on 14 Jan 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200114A (trigger 600666048.723634 / 200114153).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 199.4, Dec = -0.3 (J2000 degrees, equivalent to J2000 13h 17m, 0d 18'), with a statistical uncertainty of 2.6 degrees.

The angle from the Fermi LAT boresight is 72.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200114153/quicklook/glg_skymap_all_bn200114153.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200114153/quicklook/glg_healpix_all_bn200114153.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200114153/quicklook/glg_lc_medres34_bn200114153.gif


GRB_name: GRB200114A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26736
SUBJECT: GRB 200114A: BALROG localization (Fermi Trigger 600666048 / GRB 200114153)
DATE:    20/01/14 04:10:04 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
600666048 at 03:40:43 on 14 Jan. 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 203.7+/-1.8 deg
Decl.(2000.0) = -2.4+/-1.7 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200114153/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200114153/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200114153/json

                        


GRB_name: GRB200114A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26746
SUBJECT: GRB 200114A: AstroSat CZTI detection
DATE:    20/01/14 13:17:48 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 200114A, which was also detected by Fermi GBM Final Real-time Localization (GCN #26735), BALROG localization (Kunzweiler F. et al., GCN #26736) and Global MASTER-Net (Lipunov V. et al., GCN #26737).

The source was clearly detected in the 40-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-01-14 03:40:45.0 UT. The measured peak count rate associated with the burst is 267 cts/s above the background in the combined data of four quadrants, with a total of 2222 cts. The local mean background count rate was 487 cts/s. Using cumulative rates, we measure a T90 of 38.4 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB200114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26754
SUBJECT: GRB 200114A: DDOTI/OAN optical observations report
DATE:    20/01/15 03:17:26 GMT
FROM:    Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada  <mpereyra@astro.unam.mx>

Margarita Pereyra (UNAM), Eleonora Troja (GSFC/UMD),  Alan M. Watson
(UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego Gonzalez (UNAM),
Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), and Tanner Wolfram
(ASU), Simone Dichiara (GSFC/UMD) report:

We observed the field of GRB 200114A detected by Fermi/GBM and AstroSat
CZTI (Fermi GBM Team, GCN Circ. 26735; Gaikwad et al., GCN Circ. 26746),
with the DDOTI/OAN wide-field imager at the Observatorio AstronÃ³mico
Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) from
2020-01-14 09:27 to 2020-01-14 13:18 UTC (5.78 to 9.63 hours after the
event).

We observed a region of 13.6 degrees in RA by 10.2 degrees in declination
centered on the peak of the Fermi GBM on-ground localization at 13:17:31
-00:19:12 J2000 (Fermi GBM Team, GCN Circ. 26735). This region contains
about 140 square degrees. We obtained about 30 to 36 minutes total exposure
across the region. We calibrated our images against the APASS catalog. Our
10-sigma limiting magnitude are typically between w = 18.70 and w = 18.80.

We found only one source with significant fading above our 10-sigma limit.
This source is at 12:55:26.84 -00:21:23.8 J2000 and fades from w =  17.0 to
w = 19.5 during our observations. However, the Pan-STARRS DR1 shows a 19
mag star at the source position, which rules it out as a GRB optical
counterpart.

Comparing to the USNO-B1 and Pan-STARRS DR1 catalogs, we detected no
uncatalogued sources to our 10-sigma limit.

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

-- 
*Dr. Margarita Pereyra *

*FFTF, Schlumberger Foundation Alumnae*
----------------------------------------------------------------------------------------------------------------

*CatedrÃ¡tico Conacyt*

*Instituto de AstronomÃ­a de la UNAM,*

*Km. 107 Carretera Tijua**na-Ensenada, *

*Ensenada Baja California, MÃ©xico. C.P. 22860*

Oficina: 405

Skype: margarita-pereyra


GRB_name: GRB200115A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26771
SUBJECT: GRB 200115A: Swift detection of a burst
DATE:    20/01/15 12:10:54 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

S. B. Cenko (GSFC), E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA),
V. D'Elia (SSDC), J.D. Gropp (PSU), N. J. Klingler (PSU) and
K. L. Page (U Leicester) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 11:50:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200115A (trigger=949361).  Swift did not slew to the burst. 
The BAT on-board calculated location is RA, Dec 56.454, +5.613 which is 
   RA(J2000) = 03h 45m 49s
   Dec(J2000) = +05d 36' 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 300 sec.  The peak count rate
was ~2600 counts/sec (15-350 keV), at ~101 sec after the trigger. 

Due to observations at a higher merit related to the follow-up 
of the GW event S200115j, Swift will not slew to the BAT position. 
There will thus be no XRT or UVOT data for this trigger. 

Burst Advocate for this burst is S. B. Cenko (brad.cenko 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/)


GRB_name: GRB200115A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26772
SUBJECT: GRB 200115A: Nanshan-0.6m optical upper limit
DATE:    20/01/15 12:56:33 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu, D. Xu, X. Liu, B.Y. Yu, Y. Ma (NAOC), X. Gao (Urumqi No.1 
Senior High School) report:

We observed the field of GRB 200115A (Cenko et al., GCN 26771) using the 
0.6m NEXT telescope located at Nanshan, Xinjiang, China. Observations 
started at 12:11:17 UT on 2020-01-15 (i.e., 20.9 min after the BAT 
trigger), and a series of 300 s R-band frames have been obtained. 
Observations are ongoing.

No optical transient is detected in the Swift BAT's error circle from 
initial frames, down to a limiting magnitude of m(R) ~ 20.0, calibrated 
with the nearby SDSS field.


GRB_name: GRB200114A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26773
SUBJECT: GRB 200114A: Insight-HXMT/HE detection
DATE:    20/01/15 13:02:23 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, S. Xiao, Y. F. Du, Y. G. Zheng, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-01-14T03:40:45.50 (T0), Insight-HXMT/HE detected 
GRB 200114A (trigger ID: HEB200114153) in a routine search of the data, 
which also triggered Fermi/GBM (GCN #26735).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 30.02 s measured from T0-2.72 s. 
The 1-ms peak rate, measured from T0-0.57 s, is 1112 cnts/sec. 
The total counts from this burst is 6070 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB200114153_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200115A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26776
SUBJECT: GRB 200115A: MITSuME Okayama optical upper limits
DATE:    20/01/15 15:01:10 GMT
FROM:    Masafumi Niwano at Tokyo Institute of Tech  <niwano@hp.phys.titech.ac.jp>

M. Niwano, K. L. Murata, M. Oeda, K. Shiraishi, K. Iida, R. Adachi, F. 
Ogawa, S. Toma, R. Hosokawa, N. Nakamura, Y. Yatsu, and N. 
Kawai(TokyoTech) report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 200115A (S. B. Cenko et 
al.,GCN Circular #26771) with the optical three color (g', Rc, and Ic) 
CCD cameras attached to the MITSuME 50 cm telescope of Okayama 
Astrophysical Observatory, Okayama, Japan.
The observation started on 11:52:38.68 UT. We did not find any new point 
sources within the Swift/BAT circle (S. B. Cenko et al., GCN Circular 
#26771) in all three bands.
We obtained the 5-sigma limits as follows.

T0+[sec]   MID-UT    T-EXP[sec]    5-sigma limits
------------------------------------------------------------------------------------------------
135   12:23:04.98   3060   g'>18.3, Rc>17.6, Ic>17.2
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used UCAC4 catalog for flux calibration.
The magnitudes are expressed in the AB system.
The images were processed in real-time through the MITSuME GPU reduction 
pipeline (Niwano et al. ,in prep; https://github.com/MNiwano/Eclair)


GRB_name: GRB200111A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26778
SUBJECT: IPN triangulation of GRB 200111A
DATE:    20/01/15 18:10:59 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

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

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

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

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

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

The long-duration GRB 200111A (The Fermi GBM team, GCN Circ. 26705;
Insight-HXMT/HE detection: Xiao et al., GCN Circ. 26714)
was detected by Konus-Wind, Fermi (GBM trigger 600448273),
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), Insight (HXMT/HE),
and Swift (BAT) at about 54668 s UT (15:11:08).
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:
  107.869 (07h 11m 29s) +32.551 (+32d 33' 03")
 Corners:
  107.545 (07h 10m 11s) +34.162 (+34d 09' 42")
  107.747 (07h 10m 59s) +34.483 (+34d 28' 58")
  108.134 (07h 12m 32s) +30.686 (+30d 41' 10")
  107.920 (07h 11m 41s) +30.214 (+30d 12' 52")
 ---------------------------------------------
The error box area is about 2864 sq. arcmin, and its maximum
dimension is 4.3 deg (the minimum one is 12.2 arcmin).
The Sun distance was about 167 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM one.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200111_T54677/IPN/

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


GRB_name: GRB200115A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26780
SUBJECT: GRB 200115A: Swift-BAT refined analysis
DATE:    20/01/16 00:41:51 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
K. Page (UL), 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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 200115A (trigger #949361)
(Page, et al., GCN Circ. 26771).  The BAT ground-calculated position is
RA, Dec = 56.453, 5.607 deg, which is
   RA(J2000)  =  03h 45m 48.7s
   Dec(J2000) = +05d 36' 26.0"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.

The mask-weighted light curve starts before T-50 sec, picking up at T-30 sec,
continued increasing until the peak at T+100 sec, a couple weak following peaks,
and having weak and flat emission out past the end of data at T+240 sec.
T90 (15-350 keV) is 158.4 +- 32.6 sec (estimated error including systematics).

The time-averaged spectrum from T-40.29 to T+233.12 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.29 +- 0.24,   
and Epeak of 75.0 +- 17.5 keV (chi squared 40.88 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.0 +- 0.0 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+99.75 sec in the 15-150 keV band is
3.6 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index  
of 1.77 +- 0.06 (chi squared 53.76 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/949361/BA/


GRB_name: GRB200111A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26783
SUBJECT: GRB 200111A: AstroSat CZTI detection
DATE:    20/01/16 10:01:06 GMT
FROM:    Ramkrishna Gaikwad at IUCAA/AstroSat  <ramkrishna@iucaa.in>

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

Analysis of AstroSat CZTI data showed the detection of a GRB 200111A, which was also detected by Fermi GBM Final Real-time Localization (GCN #26705) and Insight-HXMT/HE (Xiao S. et al., GCN #26714).

The source was clearly detected in the 40-200 keV energy range. The light curve showed multiple peaks of emission peaking at 2020-01-11 15:11:09.0 UT. The measured peak count rate associated with the burst is 421 cts/s above the background in the combined data of four quadrants, with a total of 1251 cts. The local mean background count rate was 548 cts/s. Using cumulative rates, we measure a T90 of 8.6 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB200115A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26790
SUBJECT: GRB 200115A: Mondy optical afterglow candidate
DATE:    20/01/16 18:22:00 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Volnova (IKI),  E. Klunko (ISTP), K. Kamyshnikov 
(HSE), N. Pankov (HSE),  E. Mazaeva (IKI), S. Belkin (IKI)  report   on 
behalf of GRB IKI FuN:

We observed the field of  GRB 200115A (Cenko et al.  GCN 26771) with 
AZT-33IK telescope of Sayan observatory (Mondy) starting on Jan. 15 (UT) 
  11:55:00, i.e. 4.6 minutes after GRB trigger.  Within  BAT 
ground-calculated position (Laha et al. GCN 26780) we   detected the 
only one unidentified object at the coordinates (J2000) 03:45:46.58 
+05:36:36 with uncertainty of 0.5 arcsec in both coordinates. The object 
is absent in SDSS DR12. At this time we cannot confirm variability of 
the object.   We suggest the object is the optical afterglow  of GRB 
200115A. Preliminary photometry of the afterglow candidate is following.

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

2020-01-15 11:55:00   0.02455    R      30*120  20.9  0.2   22.1

The photometry is based on the nearby SDSS DR12 stars
SDSS                 R_Lupton
J034551.63+053704.5  17.138  0.016
J034547.51+053555.6  18.214  0.029
J034543.70+053549.4  17.851  0.022


GRB_name: GRB200115A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  26792
SUBJECT: GRB 200115A: DDOTI/OAN  optical observations report
DATE:    20/01/16 20:59:20 GMT
FROM:    Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada  <mpereyra@astro.unam.mx>

Rosa L. Becerra (UNAM), Margarita Pereyra (UNAM), Nat Butler (ASU), Alan M.
Watson (UNAM),  Eleonora Troja (GSFC/UMD),  Diego Gonzalez (UNAM),
Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), and Tanner Wolfram
(ASU), Simone Dichiara (GSFC/UMD) report:

We observed the field of GRB 200115A detected by BAT/Swift (Cenko, GCN
Circ. 26771), with the DDOTI/OAN wide-field imager at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir (
http://ddoti.astroscu.unam.mx) from 2020-01-16 02:01 to 2020-01-16 02:19
UTC (14.2 to 14.48 hours after the event).

We observed a region of 6.8 degrees in RA by 10.2 degrees in declination
centered on the peak of the Swift-BAT on-board calculated location
03:45:48.7 +05:36:26.0 J2000. This region contains about 70 square degrees.
We obtained about 16 minutes total exposure across the region.

We calibrated our images against the APASS catalog. Our 3-sigma limiting
magnitude is w = 19.80 for the enhanced Swift-BAT error region (Laha et
al., GCN Circ. 26780). Comparing to the USNO-B1 and SDSS DR9 catalogs we do
not detect any uncataloged source  to our 3-sigma limit.

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


-- 
*Dr. Margarita Pereyra *

*FFTF, Schlumberger Foundation Alumnae*
----------------------------------------------------------------------------------------------------------------

*CatedrÃ¡tico Conacyt*

*Instituto de AstronomÃ­a de la UNAM,*

*Km. 107 Carretera Tijua**na-Ensenada, *

*Ensenada Baja California, MÃ©xico. C.P. 22860*

Oficina: 405

Skype: margarita-pereyra


