# GCN_circulars

GRB_name: GRB200801C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28189
SUBJECT: GRB 200801C: BOOTES-1 and BOOTES-2 optical limits 
DATE:    20/08/02 01:51:10 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

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), R. Fernandez-Munoz (IHSM/UMA-CSIC) and F. Rendon (IAA-CSIC and INTA-CEDEA), on behalf of a larger collaboration, report:

Following the Swift trigger of GRB 200801C, a likely flare from AX J1846.4-0258 (Krimm et al., GCNC 28187), the 60cm BOOTES-2/TELMA robotic telescope at IHSM La Mayora (UMA-CSIC) in Algarrobo Costa (Malaga, Spain) automatically responded to this event. A series of images were taken starting 20:13:18.40UT (91 s after trigger, clear filter). In the co-added 10s exposure image, no soure is detected within the BAT 3' error box radius down to 17.7 mag.

Later on, the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, started gathering images at 20:31:01UT (19.2 min after trigger) after the twilight. In the co-added of 10 s exposure images (clear filter), no new source is detected down to 16.9 mag.

The images limiting magnitude were affected by the presence of the full moon 22 deg away. The above-mentioned non-detections are consistent with the limit reported by MASTER (Lipunov et al., GCNC 28186).

We thank the staff at INTA-CEDEA and at IHSM/UMA-CSIC La Mayora for their excellent support.


GRB_name: GRB200802A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28190
SUBJECT: GRB 200802A: Fermi GBM Final Real-time Localization
DATE:    20/08/02 11:57:10 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 11:46:46 UT on 2 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200802A (trigger 618061611.842764 / 200802491).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 329.8, Dec = 54.8 (J2000 degrees, equivalent to J2000 21h 59m, 54d 47'), with a statistical uncertainty of 2.1 degrees.

The angle from the Fermi LAT boresight is 99.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200802491/quicklook/glg_skymap_all_bn200802491.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/bn200802491/quicklook/glg_healpix_all_bn200802491.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200802491/quicklook/glg_lc_medres34_bn200802491.gif


GRB_name: GRB200802A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28191
SUBJECT: GRB 200802A: BALROG localization (Fermi Trigger 618061611 / GRB 200802491)
DATE:    20/08/02 12:16:09 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
618061611 at 11:46:46 on 02 Aug. 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) = 329.8+/-3.6 deg
Decl.(2000.0) = 52.1+/-3.1 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200802491/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200802491/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200802491/json

                        


GRB_name: GRB200729A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28192
SUBJECT: Konus-Wind detection of GRB 200729A
DATE:    20/08/02 16:38:02 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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 GRB 200729A (Swift trigger #984929:
Evans et al., GCN 28165, Krimm et al., GCN 28179;
Fermi-GBM Sub-Threshold  candidate: Malacaria et al., GCN 28174)
was detected by Konus-Wind in the waiting mode.

The burst light curve shows a single emission episode
with a duration of ~ 74 s.

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB200729A/

As observed by Konus-Wind, the burst had a fluence of
5.23(-1.00,+1.32)x10^-6 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(BAT)+5.8 s, of 2.18(-0.55,+0.66)x10^-7 erg/cm2/s
(both in the 20 - 1500 keV energy range).

The K-W 3-channel time-integrated spectrum
(from ~T0(BAT) s to ~T0(BAT)+73.5 s)
is well described by a cutoff power-law model
with alpha = -0.47(-0.3,+0.5) and Ep = 269(-65,+105) keV.

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


GRB_name: GRB200802A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28194
SUBJECT: Fermi GRB 200802A: Global MASTER-Net observations report 
DATE:    20/08/02 20:30:09 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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200802A ( Fermi GBM team, GCN 28190) errorbox  23912 sec after notice time and 23939 sec after trigger time at 2020-08-02 18:25:46 UT, with upper limit up to  18.4 mag. Observations started at twilight.  The observations began at zenith distance = 42 deg. The sun  altitude  is -12.9 deg. 

The galactic latitude b =  0 deg., longitude l = 101 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1412536

We obtain a following upper limits.  

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

   23969 | 2020-08-02 18:25:46 |      MASTER-Tavrida | (21h 53m 53.03s , +55d 48m 42.6s) |   C |    60 | 17.4 |        
   24050 | 2020-08-02 18:27:06 |      MASTER-Tavrida | (21h 44m 23.60s , +53d 47m 50.9s) |   C |    60 | 17.6 |        
   24130 | 2020-08-02 18:28:27 |      MASTER-Tavrida | (22h 11m 29.27s , +53d 47m 31.8s) |   C |    60 | 17.4 |        
   24211 | 2020-08-02 18:29:47 |      MASTER-Tavrida | (22h 03m 06.05s , +51d 48m 25.7s) |   C |    60 | 17.4 |        
   24292 | 2020-08-02 18:31:08 |      MASTER-Tavrida | (21h 53m 46.84s , +55d 49m 41.1s) |   C |    60 | 17.8 |        
   24372 | 2020-08-02 18:32:28 |      MASTER-Tavrida | (22h 08m 10.23s , +55d 48m 26.3s) |   C |    60 | 17.5 |        
   24453 | 2020-08-02 18:33:49 |      MASTER-Tavrida | (21h 44m 17.10s , +53d 47m 47.6s) |   C |    60 | 17.6 |        
   24533 | 2020-08-02 18:35:09 |      MASTER-Tavrida | (21h 57m 56.37s , +53d 47m 37.7s) |   C |    60 | 17.6 |        
   24613 | 2020-08-02 18:36:30 |      MASTER-Tavrida | (22h 11m 29.20s , +53d 48m 57.1s) |   C |    60 | 17.4 |        
   24694 | 2020-08-02 18:37:50 |      MASTER-Tavrida | (22h 25m 03.70s , +53d 47m 14.3s) |   C |    60 | 17.4 |        
   24774 | 2020-08-02 18:39:11 |      MASTER-Tavrida | (22h 03m 10.46s , +51d 49m 20.7s) |   C |    60 | 17.5 |        
   24855 | 2020-08-02 18:40:31 |      MASTER-Tavrida | (22h 16m 04.26s , +51d 48m 13.9s) |   C |    60 | 17.4 |        
   24935 | 2020-08-02 18:41:52 |      MASTER-Tavrida | (22h 08m 03.50s , +55d 49m 27.6s) |   C |    60 | 17.6 |        
   25016 | 2020-08-02 18:43:12 |      MASTER-Tavrida | (21h 57m 56.48s , +53d 48m 34.3s) |   C |    60 | 17.7 |        
   25097 | 2020-08-02 18:44:33 |      MASTER-Tavrida | (22h 25m 00.63s , +53d 47m 09.2s) |   C |    60 | 17.5 |        
   25177 | 2020-08-02 18:45:53 |      MASTER-Tavrida | (22h 16m 08.72s , +51d 47m 15.5s) |   C |    60 | 17.4 |        
   25257 | 2020-08-02 18:47:14 |      MASTER-Tavrida | (22h 06m 02.45s , +57d 47m 54.6s) |   C |    60 | 16.1 |        
   25338 | 2020-08-02 18:48:34 |      MASTER-Tavrida | (22h 22m 20.31s , +55d 48m 14.7s) |   C |    60 | 15.2 |        
   25499 | 2020-08-02 18:51:15 |      MASTER-Tavrida | (21h 35m 58.27s , +57d 48m 19.6s) |   C |    60 | 14.4 |        
   25579 | 2020-08-02 18:52:36 |      MASTER-Tavrida | (22h 06m 02.60s , +57d 49m 15.7s) |   C |    60 | 15.4 |        
   25660 | 2020-08-02 18:53:56 |      MASTER-Tavrida | (22h 21m 06.03s , +57d 47m 49.9s) |   C |    60 | 17.1 |        
   25982 | 2020-08-02 18:59:18 |      MASTER-Tavrida | (21h 50m 12.78s , +51d 48m 42.9s) |   C |    60 | 17.6 |        
   26062 | 2020-08-02 19:00:39 |      MASTER-Tavrida | (21h 35m 52.16s , +57d 48m 12.2s) |   C |    60 | 18.1 |        
   26143 | 2020-08-02 19:01:59 |      MASTER-Tavrida | (21h 51m 01.50s , +57d 48m 14.2s) |   C |    60 | 18.2 |        
   26224 | 2020-08-02 19:03:20 |      MASTER-Tavrida | (22h 21m 05.95s , +57d 48m 58.5s) |   C |    60 | 17.9 |        
   26385 | 2020-08-02 19:06:01 |      MASTER-Tavrida | (21h 50m 11.28s , +51d 49m 36.6s) |   C |    60 | 17.9 |        
   26465 | 2020-08-02 19:07:21 |      MASTER-Tavrida | (21h 50m 55.03s , +57d 48m 56.1s) |   C |    60 | 17.9 |        
   27704 | 2020-08-02 19:28:00 |      MASTER-Tavrida | (21h 36m 31.11s , +55d 55m 06.0s) |   C |    60 | 18.2 |        
   28469 | 2020-08-02 19:40:45 |      MASTER-Tavrida | (21h 36m 31.68s , +55d 55m 09.0s) |   C |    60 | 18.2 |        
   29195 | 2020-08-02 19:52:51 |      MASTER-Tavrida | (22h 02m 25.38s , +59d 54m 02.8s) |   C |    60 | 18.4 |        
   29598 | 2020-08-02 19:59:34 |      MASTER-Tavrida | (22h 02m 21.74s , +59d 53m 49.1s) |   C |    60 | 18.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200801B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28195
SUBJECT: Fermi GRB 200801B: Global MASTER-Net observations report 
DATE:    20/08/03 01:30:11 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) started inspect of the Fermi GRB 200801B ( Fermi GBM team, GCN 28184) errorbox  1 days 31237 sec after notice time and 1 days 31265 sec after trigger time at 2020-08-03 00:16:52 UT, with upper limit up to  17.8 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -64.7 deg. 

The galactic latitude b = -40 deg., longitude l = 235 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1412095

We obtain a following upper limits.  

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

  117695 | 2020-08-03 00:16:52 |         MASTER-SAAO | (04h 34m 14.12s , -34d 00m 12.6s) |   C |    60 | 17.2 |        
  117775 | 2020-08-03 00:18:11 |         MASTER-SAAO | (04h 40m 57.39s , -36d 00m 44.9s) |   C |    60 | 17.4 |        
  117855 | 2020-08-03 00:19:31 |         MASTER-SAAO | (04h 27m 58.81s , -31d 59m 52.9s) |   C |    60 | 16.7 |        
  118436 | 2020-08-03 00:29:13 |         MASTER-SAAO | (04h 34m 12.90s , -34d 00m 26.1s) |   C |    60 | 17.4 |        
  118516 | 2020-08-03 00:30:32 |         MASTER-SAAO | (04h 41m 02.38s , -36d 01m 46.2s) |   C |    60 | 17.6 |        
  118596 | 2020-08-03 00:31:52 |         MASTER-SAAO | (04h 28m 06.15s , -32d 00m 17.9s) |   C |    60 | 17.0 |        
  118755 | 2020-08-03 00:34:32 |         MASTER-SAAO | (04h 38m 34.73s , -32d 00m 30.4s) |   C |    60 | 17.0 |        
  118755 | 2020-08-03 00:34:32 |         MASTER-SAAO | (04h 46m 51.81s , -31d 59m 19.5s) |   C |    60 | 16.7 |        
  118835 | 2020-08-03 00:35:52 |         MASTER-SAAO | (04h 45m 06.92s , -34d 01m 26.8s) |   C |    60 | 17.6 |        
  118835 | 2020-08-03 00:35:52 |         MASTER-SAAO | (04h 53m 35.54s , -34d 00m 14.9s) |   C |    60 | 17.3 |        
  118915 | 2020-08-03 00:37:11 |         MASTER-SAAO | (04h 40m 53.02s , -30d 01m 20.5s) |   C |    60 | 16.9 |        
  119074 | 2020-08-03 00:39:51 |         MASTER-SAAO | (04h 38m 38.04s , -32d 00m 48.7s) |   C |    60 | 17.3 |        
  119074 | 2020-08-03 00:39:51 |         MASTER-SAAO | (04h 46m 55.19s , -31d 59m 37.1s) |   C |    60 | 16.9 |        
  119154 | 2020-08-03 00:41:10 |         MASTER-SAAO | (04h 45m 03.41s , -34d 01m 59.9s) |   C |    60 | 17.8 |        
  119154 | 2020-08-03 00:41:10 |         MASTER-SAAO | (04h 53m 32.11s , -34d 00m 47.6s) |   C |    60 | 17.5 |        
  119234 | 2020-08-03 00:42:30 |         MASTER-SAAO | (04h 40m 59.17s , -29d 59m 21.2s) |   C |    60 | 17.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200803A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28196
SUBJECT: GRB 200803A: Fermi GBM Final Real-time Localization
DATE:    20/08/03 03:44:43 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 LONG GRB

At 03:34:26 UT on 3 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200803A (trigger 618118471.567908 / 200803149).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 313.6, Dec = -62.0 (J2000 degrees, equivalent to J2000 20h 54m, -62d 00'), with a statistical uncertainty of 1.4 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/2020/bn200803149/quicklook/glg_skymap_all_bn200803149.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/bn200803149/quicklook/glg_healpix_all_bn200803149.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200803149/quicklook/glg_lc_medres34_bn200803149.gif


GRB_name: GRB200801B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28197
SUBJECT: GRB 200801B: AstroSat CZTI detection
DATE:    20/08/03 04:37:13 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed a weak detection of a long GRB 200716A, which was also detected by Fermi GBM (GCN #28184) and BALROG (Biltzinge B. et al., GCN #28185) and Global MASTER-Net (Lipunov V. et al., GCN #28195).

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 2020-08-01 15:35:48.939 UT. The measured peak count rate associated with the burst is 112 +/- 16 cts/s above the background in the combined data of four quadrants, with a total of 697 +/- 48 cts. The local mean background count rate was 420 +/- 2 cts/s. Using cumulative rates, we measure a T90 of 17.08 +/- 0.47 s. 

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-08-01 15:35:45.558 UT. The measured peak count rate is 327 +/- 37 cts/s above the background in the combined Veto data of four quadrants, with a total of 1598 +/- 87 cts. The local mean background count rate was 1709 +/- 4 cts/s.  We measure a T90 of 16.17 +/- 0.26 s from the cumulative Veto light curve.

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: GRB200803A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28198
SUBJECT: Fermi GRB 200803A: Global MASTER-Net observations report 
DATE:    20/08/03 05:30:08 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) started inspect of the Fermi GRB 200803A ( Fermi GBM team, GCN 28196) errorbox  47 sec after notice time and 74 sec after trigger time at 2020-08-03 03:35:40 UT, with upper limit up to  18.4 mag. The observations began at zenith distance = 50 deg. The sun  altitude  is -23.6 deg. 

The galactic latitude b = -37 deg., longitude l = 330 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1412844

We obtain a following upper limits.  

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

      79 | 2020-08-03 03:35:40 |         MASTER-SAAO | (21h 32m 06.21s , -63d 47m 40.4s) |   C |    10 | 17.1 |        
      79 | 2020-08-03 03:35:40 |         MASTER-SAAO | (21h 16m 08.66s , -63d 48m 22.1s) |   C |    10 | 17.0 |        
     117 | 2020-08-03 03:36:13 |         MASTER-SAAO | (20h 58m 19.87s , -62d 07m 21.8s) |   C |    20 | 17.4 |        
     117 | 2020-08-03 03:36:13 |         MASTER-SAAO | (20h 43m 15.94s , -62d 08m 01.9s) |   C |    20 | 17.3 |        
     161 | 2020-08-03 03:36:52 |         MASTER-SAAO | (20h 58m 19.46s , -62d 06m 21.5s) |   C |    30 | 17.7 |        
     161 | 2020-08-03 03:36:53 |         MASTER-SAAO | (20h 43m 16.07s , -62d 07m 01.3s) |   C |    30 | 17.5 |        
     216 | 2020-08-03 03:37:42 |         MASTER-SAAO | (20h 58m 25.16s , -62d 07m 20.7s) |   C |    40 | 17.7 |        
     216 | 2020-08-03 03:37:42 |         MASTER-SAAO | (20h 43m 21.25s , -62d 08m 01.0s) |   C |    40 | 17.7 |        
     281 | 2020-08-03 03:38:42 |         MASTER-SAAO | (20h 58m 18.78s , -62d 08m 20.2s) |   C |    50 | 17.3 |        
     281 | 2020-08-03 03:38:42 |         MASTER-SAAO | (20h 43m 14.45s , -62d 09m 00.3s) |   C |    50 | 17.4 |        
     355 | 2020-08-03 03:39:51 |         MASTER-SAAO | (20h 58m 23.73s , -62d 08m 19.8s) |   C |    60 | 18.0 |        
     355 | 2020-08-03 03:39:51 |         MASTER-SAAO | (20h 43m 19.42s , -62d 08m 59.6s) |   C |    60 | 17.8 |        
     639 | 2020-08-03 03:44:05 |         MASTER-SAAO | (20h 59m 38.80s , -62d 04m 25.4s) |   C |   120 | 18.4 |        
     639 | 2020-08-03 03:44:05 |         MASTER-SAAO | (20h 44m 36.50s , -62d 05m 05.2s) |   C |   120 | 18.1 |        
     788 | 2020-08-03 03:46:24 |         MASTER-SAAO | (20h 59m 38.20s , -62d 03m 23.4s) |   C |   140 | 18.2 |        
     788 | 2020-08-03 03:46:24 |         MASTER-SAAO | (20h 44m 36.56s , -62d 04m 02.7s) |   C |   140 | 18.1 |        
     963 | 2020-08-03 03:49:04 |         MASTER-SAAO | (20h 59m 44.87s , -62d 04m 22.3s) |   C |   170 | 18.3 |        
     963 | 2020-08-03 03:49:04 |         MASTER-SAAO | (20h 44m 42.77s , -62d 05m 01.8s) |   C |   170 | 18.1 |        
    1157 | 2020-08-03 03:52:14 |         MASTER-SAAO | (20h 59m 38.04s , -62d 05m 21.5s) |   C |   180 | 18.4 |        
    1157 | 2020-08-03 03:52:14 |         MASTER-SAAO | (20h 44m 35.46s , -62d 06m 00.8s) |   C |   180 | 18.2 |        
    1357 | 2020-08-03 03:55:33 |         MASTER-SAAO | (20h 59m 42.62s , -62d 05m 06.0s) |   C |   180 | 18.3 |        
    1357 | 2020-08-03 03:55:33 |         MASTER-SAAO | (20h 44m 40.17s , -62d 05m 44.4s) |   C |   180 | 18.2 |        
    1556 | 2020-08-03 03:58:52 |         MASTER-SAAO | (20h 59m 39.66s , -62d 03m 31.5s) |   C |   180 | 18.2 |        
    1556 | 2020-08-03 03:58:52 |         MASTER-SAAO | (20h 44m 38.10s , -62d 04m 09.5s) |   C |   180 | 18.1 |        
    1756 | 2020-08-03 04:02:12 |         MASTER-SAAO | (20h 59m 39.41s , -62d 05m 01.5s) |   C |   180 | 18.2 |        
    1756 | 2020-08-03 04:02:12 |         MASTER-SAAO | (20h 44m 37.33s , -62d 05m 39.6s) |   C |   180 | 18.1 |        
    1895 | 2020-08-03 04:05:32 |         MASTER-SAAO | (20h 46m 24.22s , -64d 02m 24.8s) |   C |    60 | 18.1 |        
    1895 | 2020-08-03 04:05:32 |         MASTER-SAAO | (20h 30m 19.82s , -64d 02m 58.5s) |   C |    60 | 18.0 |        
    2147 | 2020-08-03 04:09:43 |         MASTER-SAAO | (21h 06m 07.28s , -62d 03m 57.9s) |   C |    60 | 18.0 |        
    2147 | 2020-08-03 04:09:43 |         MASTER-SAAO | (20h 51m 06.05s , -62d 04m 36.1s) |   C |    60 | 17.7 |        
    2227 | 2020-08-03 04:11:03 |         MASTER-SAAO | (20h 46m 17.65s , -64d 04m 27.7s) |   C |    60 | 18.0 |        
    2227 | 2020-08-03 04:11:03 |         MASTER-SAAO | (20h 30m 12.34s , -64d 05m 00.7s) |   C |    60 | 17.9 |        
    2307 | 2020-08-03 04:12:23 |         MASTER-SAAO | (21h 23m 04.83s , -64d 05m 11.2s) |   C |    60 | 18.1 |        
    2307 | 2020-08-03 04:12:23 |         MASTER-SAAO | (21h 06m 58.62s , -64d 05m 49.1s) |   C |    60 | 17.9 |        
    2386 | 2020-08-03 04:13:42 |         MASTER-SAAO | (20h 31m 48.01s , -62d 02m 08.5s) |   C |    60 | 17.8 |        
    2386 | 2020-08-03 04:13:42 |         MASTER-SAAO | (20h 16m 48.47s , -62d 02m 41.6s) |   C |    60 | 17.7 |        
    2466 | 2020-08-03 04:15:02 |         MASTER-SAAO | (21h 04m 46.12s , -66d 04m 21.7s) |   C |    60 | 17.9 |        
    2466 | 2020-08-03 04:15:02 |         MASTER-SAAO | (20h 47m 25.31s , -66d 04m 53.5s) |   C |    60 | 17.9 |        
    2546 | 2020-08-03 04:16:22 |         MASTER-SAAO | (21h 12m 34.17s , -58d 03m 28.1s) |   C |    60 | 17.7 |        
    2546 | 2020-08-03 04:16:22 |         MASTER-SAAO | (20h 59m 16.32s , -58d 04m 09.5s) |   C |    60 | 17.5 |        
    2626 | 2020-08-03 04:17:42 |         MASTER-SAAO | (21h 22m 58.71s , -64d 04m 09.6s) |   C |    60 | 17.9 |        
    2626 | 2020-08-03 04:17:42 |         MASTER-SAAO | (21h 06m 53.08s , -64d 04m 46.3s) |   C |    60 | 17.7 |        
    2706 | 2020-08-03 04:19:02 |         MASTER-SAAO | (20h 31m 44.41s , -62d 02m 04.4s) |   C |    60 | 17.8 |        
    2706 | 2020-08-03 04:19:02 |         MASTER-SAAO | (20h 16m 44.79s , -62d 02m 36.9s) |   C |    60 | 17.7 |        
    2785 | 2020-08-03 04:20:21 |         MASTER-SAAO | (21h 04m 49.16s , -66d 03m 46.7s) |   C |    60 | 18.0 |        
    2785 | 2020-08-03 04:20:21 |         MASTER-SAAO | (20h 47m 28.61s , -66d 04m 17.9s) |   C |    60 | 18.0 |        
    3125 | 2020-08-03 04:26:01 |         MASTER-SAAO | (21h 12m 27.15s , -58d 04m 47.1s) |   C |    60 | 17.5 |        
    3125 | 2020-08-03 04:26:01 |         MASTER-SAAO | (20h 59m 21.24s , -58d 05m 36.2s) |   C |    60 | 17.3 |        
    3374 | 2020-08-03 04:30:10 |         MASTER-SAAO | (21h 40m 16.15s , -62d 03m 51.9s) |   C |    60 | 17.4 |        
    3374 | 2020-08-03 04:30:10 |         MASTER-SAAO | (21h 25m 21.18s , -62d 04m 45.3s) |   C |    60 | 17.2 |        
    3454 | 2020-08-03 04:31:30 |         MASTER-SAAO | (20h 25m 05.24s , -66d 02m 51.4s) |   C |    60 | 17.2 |        
    3454 | 2020-08-03 04:31:30 |         MASTER-SAAO | (20h 07m 53.31s , -66d 03m 26.9s) |   C |    60 | 17.1 |        
    3709 | 2020-08-03 04:35:45 |         MASTER-SAAO | (21h 40m 10.66s , -62d 05m 20.6s) |   C |    60 | 16.8 |        
    3709 | 2020-08-03 04:35:45 |         MASTER-SAAO | (21h 25m 14.14s , -62d 06m 15.2s) |   C |    60 | 16.9 |        
    3789 | 2020-08-03 04:37:05 |         MASTER-SAAO | (20h 25m 09.83s , -66d 03m 27.2s) |   C |    60 | 16.7 |        
    3789 | 2020-08-03 04:37:05 |         MASTER-SAAO | (20h 07m 57.18s , -66d 04m 03.3s) |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200803A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28200
SUBJECT: GRB 200803A: Tiled Swift observations
DATE:    20/08/03 13:40:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 200803A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00092

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

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

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


GRB_name: GRB200803B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28201
SUBJECT: GRB 200803B: Fermi GBM Final Real-time Localization
DATE:    20/08/03 17:03:05 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 16:52:43 UT on 3 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200803B (trigger 618166368.636552 / 200803703).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 198.5, Dec = -42.5 (J2000 degrees, equivalent to J2000 13h 13m, -42d 30'), with a statistical uncertainty of 4.7 degrees.

The angle from the Fermi LAT boresight is 139.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200803703/quicklook/glg_skymap_all_bn200803703.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/bn200803703/quicklook/glg_healpix_all_bn200803703.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200803703/quicklook/glg_lc_medres34_bn200803703.gif


GRB_name: GRB200803A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28202
SUBJECT: GRB 200803A: MASTER optical counterpart discovery
DATE:    20/08/03 17:12:31 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 StateUniversity)


MASTER Global Robotic Net inspected GRB 200803A
(MASTER Lipunov et al. GCN 28198, Fermi LAT GCN 28199)
The result is optical counterpart discovery with classical OT decay

MASTER OT J204422.34-625641.8 discovery

MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic 
Net", Advances in Astronomy, 2010, 30L ) discovered OT source at
(RA, Dec) = 20h 44m 22.34s -62d 56m 41.8s on 2020-08-03.15015 UT.

The OT unfiltered magnitude is 15.8m (mlim=17.7).

The OT is seen in 13 images. There is no minor planet at this place.

We have reference image on 2015-04-04.15164 UT with  unfiltered mlim= 19.9m.

Spectral observations are required.


GRB_name: GRB200803A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28203
SUBJECT: GRB 200803A:  Fermi-LAT detection
DATE:    20/08/03 17:37:42 GMT
FROM:    Sara Cutini at INFN  <sara.cutini@pg.infn.it>

S. Cutini (INFN Perugia), F. Longo (University & INFN Trieste), 
M. Axelsson (KTH & StockholmUniv.), M. Ohno (Hiroshima Univ. & Eotvos Univ.),  
F. Dirirsa (Univ. of Johannesburg), D.Kocesvki (NASA/MSFC), and N. Omodei (Stanford U.),
report on behalf of the Fermi-LAT team:

At 03:34:26.57 on August, 03, 2020 Fermi-LAT detected high-energy emission from GRB 200803A, 
which was also detected by Fermi-GBM (GCN 28196).

The best LAT on-ground location is found to be 

RA, Dec = 311.29, -63.08 (J2000)

with an error radius of 0.46 deg (90 % containment, statistical error only).

This was 39 deg from the LAT boresight at the time of the trigger, 
the Fermi-LAT entered  in the SAA at around 450 seconds after the trigger.

The data from the Fermi-LAT show a significant increase in the event rate
 that is spatially and temporally correlated with the trigger with high significance.

The photon flux above 100 MeV in the time interval 0-450 s after the GBM trigger is 8.0e-6 +/- 2.3e-6 ph/cm2/s.
The estimated photon index above 100 MeV is -2.4+/-0.3.

The highest-energy photon is ~650 MeV  event which is observed ~200 seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Sara Cutini (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: GRB200803B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28204
SUBJECT: Fermi GRB 200803B: Global MASTER-Net observations report 
DATE:    20/08/03 18:15:11 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) started inspect of the Fermi GRB 200803B ( Fermi GBM team, GCN 28201) errorbox  558 sec after notice time and 586 sec after trigger time at 2020-08-03 17:02:29 UT, with upper limit up to  18.9 mag. Observations started at twilight.  The observations began at zenith distance = 25 deg. The sun  altitude  is -12.7 deg. 

The galactic latitude b = 20 deg., longitude l = 308 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1413147

We obtain a following upper limits.  

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

     646 | 2020-08-03 17:02:29 |         MASTER-SAAO | (13h 17m 10.58s , -42d 23m 09.6s) |   C |   120 | 18.1 |        
     807 | 2020-08-03 17:04:55 |         MASTER-SAAO | (13h 17m 11.44s , -42d 22m 10.7s) |   C |   150 | 18.2 |        
     807 | 2020-08-03 17:04:55 |         MASTER-SAAO | (13h 07m 35.82s , -42d 23m 16.8s) |   C |   150 | 18.7 |        
     991 | 2020-08-03 17:07:45 |         MASTER-SAAO | (13h 17m 16.35s , -42d 23m 11.8s) |   C |   180 | 18.2 |        
     991 | 2020-08-03 17:07:45 |         MASTER-SAAO | (13h 07m 40.58s , -42d 24m 18.0s) |   C |   180 | 18.9 |        
    1191 | 2020-08-03 17:11:04 |         MASTER-SAAO | (13h 17m 11.97s , -42d 24m 13.2s) |   C |   180 | 18.1 |        
    1191 | 2020-08-03 17:11:04 |         MASTER-SAAO | (13h 07m 36.04s , -42d 25m 19.1s) |   C |   180 | 18.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200803A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28205
SUBJECT: GRB 200803A: Swift-XRT afterglow detection
DATE:    20/08/03 20:28:04 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), M.G. Bernardini
(INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA), B.
Sbarufatti (PSU), D.N. Burrows (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
Fermi/LAT-detected burst GRB 200803A (Cutini et al. GCN Circ. 28203) in
a series of observations tiled on the sky. The total exposure time is
3.5 ks, distributed over 4 tiles; the maximum exposure at a single sky
location was 1.6 ks. The data were collected between T0+36.3 ks and
T0+46.6 ks, and are entirely in Photon Counting (PC) mode. 

Five uncatalogued X-ray sources are detected, of which one ("Source 1")
is above the RASS limit, and is therefore likely the GRB afterglow.
Using 812 s of PC mode data and 2 UVOT images, we find an enhanced XRT
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 311.09390, -62.94478 which is
equivalent to:

RA (J2000): 20h 44m 22.54s
Dec(J2000): -62d 56' 41.2"

with an uncertainty of 2.8 arcsec (radius, 90% confidence). This
position is 9.7 arcmin from the Fermi/LAT position and 1.5 arcsec from
the MASTER optical counterpart reported by Lipunov et al. (GCN Circ.
28202). 

The light curve can be modelled with a power-law decay with a decay
index of alpha=3.30 (+0.06, -2.56).

If the light curve continues to decay with a power-law decay index of
3.30, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/xrt_products/TILED_GRB00092/Source1.php.

The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00092.

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


GRB_name: GRB200803A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28206
SUBJECT: GRB 200803A: Fermi GBM detection
DATE:    20/08/03 22:22:25 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 03:34:26.00 UT on 03 August 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200803A (trigger 618118471 / 200803149)
which was also detected by the Fermi/LAT (Cutini et al. 2020,
GCN 28203). The Fermi GBM Final Real-time Localization (GCN 28196) is
consistent with the LAT position. An x-ray afterglow candidate has
been detected by the Swift/XRT (GCN 28205), and a potential optical
counterpart has also been reported by MASTER (GCN 28202).

The angle from the Fermi LAT boresight at the GBM trigger time is ~39
degrees.

The GBM light curve consists of two main pulses
with a duration (T90) of about 119 s (50-300 keV).

The time-averaged spectrum of the first pulse, from T0-4 s to
T0+14 s is best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.67 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 302 +/- 13 keV.
The event fluence (10-1000 keV) in this time interval is
(1.12 +/- 0.03)E-05.

The time-averaged spectrum of the second pulse, from T0+85 s to
T0+118 s is also best fit by a power law function with an
exponential high-energy cutoff. The power law index is
-1.13 +/- 0.02 and the cutoff energy, parameterized as Epeak,
is 223 +/- 8 keV. The event fluence (10-1000 keV) in this time
interval is (1.84 +/- 0.03)E-05.

The 1-sec peak photon flux measured
starting from T0+112 s in the 10-1000 keV band
is 10.8 +/- 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: GRB200803A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28207
SUBJECT: GRB 200803A: AstroSat CZTI detection
DATE:    20/08/04 12:43:55 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

The AstroSat CZT Imager recorded a transient event in all four of its CsI anticoincidence (Veto) detectors in the 100-500 keV energy range, coincident with the GRB 200803A reported by Fermi GBM (GCN #28196), Global MASTER-Net (Lipunov V. et al., GCN #28198) Tiled Swift (Evans P. et al., GCN #29200), Fermi-LAT (Cutini S. et al., GCN #29203) and Swift-XRT (Osborne J. et al., GCN #29205). There was no significant detection in the main CZT detectors. 

The light curve showed multiple peaks of emission with the strongest peak at 2020-08-03 03:34:34.825 UT. The measured peak count rate is 444 +/- 46 cts/s above the background in the combined Veto data of four quadrants, with a total of 2872 +/- 42 cts. The local mean background count rate was 1740 +/- 2 cts/s.  We measure a T90 of 17.81 +/- 0.77 s from the cumulative Veto light curve.

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: GRB200803B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28208
SUBJECT: GRB 200803B: MASTER possibly OT discovery 
DATE:    20/08/06 14:09:02 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov,  E. Gorbovskoy, V.Kornilov, N.Tyurina, K.Zhirkov, P.Balanutsa,A.Kuznetsov,F.Balakin,
V.Vladimirov, A.Chasovnikov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Topolev, 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 (Irkutsk State University, API),
A. Gabovich, Yu. Sergienko, V.Yurkov (Blagoveschensk Educational State University)


MASTER Global Robotic Net started Fermi GRB 200803B( Fermi GBM team, GCN 28201)
  errorbox  27 sec after notice time (55 sec after trigger time) at 
2020-08-03 16:53:38 UT, with upper limit up to  18.6 mag. (GCN 28204)
Observations started at twilight at zenith distance = 10 deg, the sun  altitude  was -10.9 deg.
The cover map with discovered OT is  at alert page
https://master.sai.msu.ru/site/master2/event.php?id=1413139

MASTER OT J144603.45-413156.7 discovery (AT2020qvn)

During these alert observations (Fermi inspection, open mode for twin 
MASTER, and fast coverage of large error-box by 8 square deg.)
MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L )
  discovered OT source at
(RA, Dec) = 14h 46m 03.45s -41d 31m 56.7s on 2020-08-03.70644 UT.

The OT unfiltered magnitude is 17.9m (mlim=18.1).

The OT is seen in 5 images. There is no any known sources in VIZIER and minor planet at this place

We have reference image on 2017-05-28.87608 UT with unfiltered mlim=20.9m.

Spectral observations are required (it also can be MilkyWay's CV, PSN in 
52" from 6df galaxy (z=0.05128, B=16.96,R=15.97, too far for PSN but can 
be).

The discovery and reference images are available at:

http://master.sai.msu.ru/static/OT/144603.45-413156.7.png

Spectral observations and deep photometry are required.


GRB_name: GRB200806A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28211
SUBJECT: GRB 200806A: Swift detection of a burst
DATE:    20/08/06 15:57:43 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Ambrosi (INAF-IASFPA), D. N. Burrows (PSU), V. D'Elia (SSDC),
J.D. Gropp (PSU), H. A. Krimm (NSF), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), 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 15:28:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200806A (trigger=987016).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 52.905, +37.082 which is 
   RA(J2000) = 03h 31m 37s
   Dec(J2000) = +37d 04' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty). The BAT light curve showed a pulse 
that starts at ~T0 and lasts beyond the currently available data,
which ends at ~T+8 s. The peak count rate was ~4800 counts/sec (15-350 keV), 
at ~0 sec after the trigger. 

The XRT began observing the field at 15:30:07.6 UT, 77.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 52.93173, 37.07845
which is equivalent to:
   RA(J2000)  = 03h 31m 43.62s
   Dec(J2000) = +37d 04' 42.4"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 77 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 2.56
x 10^21 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 2.59e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 86 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image 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
0.42. 

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: GRB200806A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28212
SUBJECT: Swift GRB 200806A: Global MASTER-Net observations report 
DATE:    20/08/06 21:40:17 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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 200806A ( E. Ambrosi et al., GCN 28211) errorbox  17964 sec after notice time and 17986 sec after trigger time at 2020-08-06 20:28:36 UT, with upper limit up to  17.5 mag. The observations began at zenith distance = 80 deg. The sun  altitude  is -26.8 deg. 

The galactic latitude b = -15 deg., longitude l = 156 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1414905

We obtain a following upper limits.  

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

   18076 |      MASTER-Tavrida |   C |   180 | 16.8 |        
   21887 |      MASTER-Tavrida |   C |   180 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200806A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28214
SUBJECT: GRB 200806A: Enhanced Swift-XRT position
DATE:    20/08/07 02:48:55 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 619 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200806A, 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 = 52.93214, +37.07876 which is equivalent
to:

RA (J2000): 03h 31m 43.71s
Dec (J2000): +37d 04' 43.5"

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: GRB200806A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28215
SUBJECT: GRB 200806A: MITSuME Akeno optical upper limits
DATE:    20/08/07 05:56:59 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

K. L. Murata, R. Adachi, R. Hosokawa, M. Niwano, F. Ogawa, N. Nakamura, N.
Ito, S. Ogata, H. Takamatsu, H. Hara, Y. Yatsu, and N. Kawai (TokyoTech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 200806A (Ambrosi et al., GCN 28211; Beardmore
et al., GCN 28214) 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 with a series of 60 sec exposures started on 2020-08âˆ’06
15:30:34 UT. The first 15 images were heavily affected by the presence of
the moon. We stacked the images excluding the 15 images and did not find
any new point sources within the enhanced Swift/XRT error circle (Beardmore
et al., GCN 28214) of the stacked images. We obtained the 5-sigma limits as
follows.

T0+[min] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
19 2020-08-06T15:57:10 960 g'>16.7, Rc>16.7, Ic>16.9
------------------------------------------------------------------------------------------------
T0+: Elapsed time after the burst
T-EXP: Total Exposure time

We used the PS1 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., submitted;
https://github.com/MNiwano/Eclaire)


GRB_name: GRB200806A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28216
SUBJECT: GRB 200806A: AstroSat CZTI detection
DATE:    20/08/07 07:50:04 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 200806A, which was also detected by Swift (Ambrosi E. et al., GCN #28211), Global MASTER-Net (Lipunov V. et al., GCN #28212) and Swift-XRT (Beardmore A. et al., GCN #28214).

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 2020-08-06 15:29:11.500 UT. The measured peak count rate associated with the burst is 665 +/- 33 cts/s above the background in the combined data of four quadrants, with a total of 5023 +/- 36 cts. The local mean background count rate was 402 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 33.93 +/- 0.05 s. In the preliminary analysis, we find that 636 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. The light curve showed multiple peaks of emission with the strongest peak at 2020-08-06 15:29:10.000 UT. The measured peak count rate is 987 +/- 50 cts/s above the background in the combined Veto data of four quadrants, with a total of 6708 +/- 67 cts. The local mean background count rate was 1506 +/- 1 cts/s.  We measure a T90 of 33.68 +/- 0.13 s from the cumulative Veto light curve.

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: GRB200805A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28217
SUBJECT: GRB 200805A: CALET Gamma-Ray Burst Monitor detection of a short burst
DATE:    20/08/07 11:31:11 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 (ICRR), 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:

At 13:31:12.629 UTC on 5 August 2020, the CALET Gamma-ray Burst Monitor
(CGBM) triggered on short GRB 200805A. The burst signal was seen
by the SGM detector only.
Because of a problem in one of the ground alert processing script,
the GCN notice was not distributed automatically for this event.

This short GRB is also clearly seen by the publicly available
INTEGRAL SPI-ACS light curve and was detected by Konus-Wind
(see the GCN IPN_RAW Notices).

The burst light curve shows a short pulse which starts at T-0.192 sec,
peaks at -0.144 sec and ends at T-0.032 sec. The T90 and T50 durations
measured by the SGM data are 0.144 +- 0.045 sec and 0.064 +- 0.036 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1280669472/

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


GRB_name: GRB200806A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28218
SUBJECT: GRB 200806A: AbAO optical upper limit
DATE:    20/08/07 12:55:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), R.Ya. Inasaridze (AbAO),  N. Pankov 
(HSE), K. Kamyshnikov (HSE),  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 Swift GRB 200806A (Ambrosi et al., GCN 28211) 
also registered by AstroSat CZTI (Gupta et al., GCN 28216)  with AS-32 
(0.7m) telescope of Abastumani Observatory starting on 2020-08-06 (UT) 
23:42:53.  We do not detect any object  within the enhanced XRT position 
error circle (Beardmore et al., GCN 28214).  Preliminary photometry of 
the field is following.

Date       UT start  t-T0    Filter Exp.  OT    Err. UL
                     (mid, days)     (s)
2020-08-06 23:42:53  0.36498 R      63*60 n/d   n/d  21.0

The photometry is based on nearby USNO-B1.0 stars

USNO-B1.0_id R2
1270-0058216 15.48
1270-0058260 14.22
1270-0058260 14.98
1271-0065622 15.31


GRB_name: GRB200805A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28219
SUBJECT: CGBM-SPI-ACS triangulation of short GRB 200805A
DATE:    20/08/07 13:03:48 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 (ICRR), 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:


Using the CALET Gamma-Ray Burst Monitor (CGBM) event data and
publicly available INTEGRAl-SPI-ACS light curve data we have triangulated
the short GRB 200805A (Shimizu et al., GCN Circ. 28217)
to a preliminary CGBM-SPI-ACS annulus centered at
RA(J2000)=57.359 deg (03h 49m 26s) Dec(J2000)=-49.453 deg (-49d 27' 10"),
whose radius is 37.65(-5.06,+4.54) deg (3 sigma).

The portion of the annulus within 69.8 deg from
RA, Dec(J2000) = 315.5 deg, -33.3 deg was below the horizon for CALET.

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

The INTEGRAL public data used for this analysis provided by
INTEGRAL Science Data Centre through
http://isdc.unige.ch/~savchenk/spiacs-online/
maintained by Volodymir Savchenko.


GRB_name: GRB200806A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28221
SUBJECT: GRB 200806A: Swift-XRT refined Analysis
DATE:    20/08/07 15:57:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 5.9 ks of XRT data for GRB 200806A (Ambrosi et al. GCN
Circ. 28211), from 84 s to 22.1 ks after the  BAT trigger. The data
comprise 372 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN Circ. 28214).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.01 (+/-0.04).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.58 (+/-0.07). The
best-fitting absorption column is  3.6 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 2.6 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.85 (+/-0.14) and a
best-fitting absorption column of 4.8 (+0.9, -0.8) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 4.4 x 10^-11 (6.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.8 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 2.6 x 10^21 cm^-2
Excess significance: 4.5 sigma
Photon index:      1.85 (+/-0.14)

If the light curve continues to decay with a power-law decay index of
1.01, the count rate at T+24 hours will be 0.023 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.9 x
10^-13 (1.5 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/00987016.

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


GRB_name: GRB200806A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28222
SUBJECT: GRB 200806A: Swift/UVOT Possible Detection
DATE:    20/08/07 17:37:59 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

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

The Swift/UVOT began settled observations of the field of GRB 200806A
86 s after the BAT trigger (Ambrosi et al., GCN Circ. 28211).
A source consistent with the enhanced XRT position
(Beardmore et al. GCN Circ. 28214)
is marginally detected in the initial UVOT exposures.

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               86          236          147         20.26 +/- 0.28
v                  629          821           39        >17.9
b                  555          747           39        >19.3
u                  300          722          265        >19.5
w1                 678          870           39        >18.8
m2                 653          845           39        >19.4
w2                 604         1052           58        >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.42 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200806A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28223
SUBJECT: GRB 200806A: Swift-BAT refined analysis 
DATE:    20/08/07 18:10:15 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

A. Y. Lien (GSFC/UMBC), 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), 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 200806A (trigger #987016)
(Ambrosi, et al., GCN Circ. 28211).  The BAT ground-calculated position is
RA, Dec = 52.933, 37.076 deg which is 
  RA(J2000)  =  03h 31m 43.9s 
  Dec(J2000) = +37d 04' 33.5" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 57%.

The mask-weighted light curve shows a multi-peaked structure, with a sharp 
rise close to T+0 sec.  The emission peaked at T+22 sec and declined to 
background by T+50 sec. T90 (15-350 keV) is 38.8 +- 1.1 sec (estimated error 
including systematics).

The time-averaged spectrum from T-0.13 to T+61.22 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.72 +- 0.12, 
and Epeak of 148.1 +- 18.6 keV (chi squared 40.06 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.6 +- 0.02 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+22.24 sec in the 15-150 keV band is
14.1 +- 0.4 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.27 +- 0.03 (chi squared 111.98 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/987016/BA/


GRB_name: GRB200806A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28224
SUBJECT: GRB 200806A: VIRT optical observations
DATE:    20/08/07 18:21:00 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

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

We observed the field of GRB200806A (Ambrosi et al, GCN 28211) with the
0.5m Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 08-06-2020 starting at 06:22:50 UT (T+15
hrs). We performed a series of exposures in R filter with a total exposure
of 5810 s. The weather conditions were clear during the hours of
observation with an average airmass of 1.6.

We find no new source within the enhanced XRT position error circle
(Beardmore et al., GCN 28214) and report the following 3-sigma upper limit:

T_mid       ||Exposure     ||Filter      ||Limit
T+16 hrs   ||5810s          ||R             ||19.6

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.

This work is supported by NASA-MUREP-MIRO grant NNX15AP95A, NSF EiR AST
Award 1901296, and NSF HBCU-UP AST Award 1831682. This message can be cited.


GRB_name: GRB200803A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28226
SUBJECT: GRB 200803A: Chilescope optical upper limit
DATE:    20/08/07 22:07:23 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), M. Krugov (AFIF),  A. Volnova 
(IKI), E. Mazaeva (IKI) report on behalf of IKI-FuN follow-up collaboration:

We observed  the GRB 200803A (Fermi GBM Team, GCN 28196; Hamburg et al., 
GCN 28206)  with Chilescope RC-1000 starting on 2020-08-05 (UT) 03:53:45 
in r'-filter. We did not detect optical afterglow (Lipunov et al., GCN 
28202).

Preliminary photometry is following.


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

2020-08-05 03:53:45 2.03425     r'  6*600 n/d n/d  21.5

The photometry is based on nearby USNO-B1.0 stars
Ref.stars
USNO-B1.0_id R2
0270-0863045 16.4
0270-0862955 15.5
0271-0884796 15.0


GRB_name: GRB200806A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28227
SUBJECT: GRB 200806A: CAHA optical afterglow confirmation
DATE:    20/08/07 22:19:18 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), C. C. Thoene, M. Blazek, J. F. Agui Fernandez (all 
HETH/IAA-CSIC), and L. Montoya (CAHA) report:

We observed the afterglow position (Beardmore et al., GCN #28214; 
Marshall et al., GCN #28222) of the bright Swift GRB 200806A (Ambrosi et 
al., GCN #28211; Lien et al., GCN #28223) with CAFOS at the 2.2m 
telescope at Calar Alto, Almeria, Spain, in the SDSS i' band. We 
obtained 20 x 180 s exposures, centered at 0.49185 days after the GRB, 
under good conditions but moonlight.

At the position of the potential UVOT afterglow (Marshall et al., GCN 
#28222), we detect a faint source not visible in PanSTARRS archival 
imaging, at position (J2000) RA = 03:31:43.76, Dec. = +37:04:43.90, with 
an estimated error of 0".75.

Photometry is made complicated by an uneven background, but measured 
against two nearby SDSS stars, we derive i' = 22.95 +/- 0.25 mag.

As this is significantly fainter than the UVOT detection, we consider 
this to be the afterglow of GRB 200806A. We note foreground extinction 
is rather high (E(B-V)=0.3564 mag according to the maps of Schlafly & 
Finkbeiner 2011), and there is additional hydrogen column density along 
the line-of-sight (Page et al., GCN #28221), implying this is likely a 
dark GRB.


GRB_name: GRB200805A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28228
SUBJECT: IPN triangulation of GRB 200805A (short)
DATE:    20/08/07 23:50:34 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

K. Hurley, on behalf of the IPN,

and

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

The short-duration GRB 200521A
(CALET-CGBM detection: Shimizu et al., GCN Circ. 28217;
CGBM-SPI-ACS triangulation: Tamura et al., GCN Circ. 28219)
was detected by CALET (CGBM), Konus-Wind, and
INTEGRAL (SPI-ACS) at about 48670 s UT (13:31:10).

We have triangulated it to a preliminary, 3 sigma error arc whose
coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
  97.601 (06h 30m 24s) -31.467 (-31d 28' 01")
  Corners:
  97.403 (06h 29m 37s)  -31.623 (-31d 37' 23")
  121.103 (08h 04m 25s) -44.012 (-44d 00' 43")
  120.592 (08h 02m 22s) -43.397 (-43d 23' 49")
  97.798 (06h 31m 11s)  -31.310 (-31d 18' 36")
  84.870 (05h 39m 29s)  -13.195 (-13d 11' 43")
  84.208 (05h 36m 50s)  -12.881 (-12d 52' 52")
  ---------------------------------------------
The error arc area is 20.3 sq. deg, and its maximum
dimension is ~43.7 deg (the minimum one is ~27.6 arcmin).
The Sun distance was ~58 deg.

This arc may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200805_T48670/IPN/

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


GRB_name: GRB200806A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28229
SUBJECT: GRB 200806A: Nanshan/NEXT optical upper limit
DATE:    20/08/08 06:35:51 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

S.Y. Fu, Z.P. Zhu, X. Liu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High 
School), X. Zhang, J.Z. Liu (XAO) report:

We observed the field of GRB 200806A (Ambrosiet al., GCN 28211) using 
the NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We obtained 
8x100s frames in the Sloan r-band, starting at 19:42:36 UT on 
2020-08-07, i.e., 28.22 hr after the burst.

No optical source is detected in our stacked image at the enhanced XRT 
position (Beardmore et al., GCN 28214), down to a limiting magnitude of 
r~20.2, calibrated with the nearby PanSTARRS field.


GRB_name: GRB200808A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28230
SUBJECT: GRB 200808A: Fermi GBM Final Real-time Localization
DATE:    20/08/08 11:26:13 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 11:15:57 UT on 8 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200808A (trigger 618578162.404866 / 200808469).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 20.1, Dec = 55.5 (J2000 degrees, equivalent to J2000 01h 20m, 55d 30'), with a statistical uncertainty of 5.3 degrees.

The angle from the Fermi LAT boresight is 38.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200808469/quicklook/glg_skymap_all_bn200808469.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/bn200808469/quicklook/glg_healpix_all_bn200808469.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200808469/quicklook/glg_lc_medres34_bn200808469.gif


GRB_name: GRB200808A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28231
SUBJECT: Fermi GRB 200808A: Global MASTER-Net observations report 
DATE:    20/08/08 15:45:09 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-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200808A ( Fermi GBM team, GCN 28230) errorbox  15558 sec after notice time and 15585 sec after trigger time at 2020-08-08 15:35:43 UT, with upper limit up to  15.1 mag. The observations began at zenith distance = 48 deg. The sun  altitude  is -19.8 deg. 

The galactic latitude b =  2 deg., longitude l = 125 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1415866

We obtain a following upper limits.  

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

   15616 | 2020-08-08 15:35:43 |        MASTER-Tunka | (01h 17m 33.52s , +55d 38m 40.5s) |   C |    60 | 15.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200809A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28232
SUBJECT: GRB 200809A: Fermi GBM Final Real-time Localization
DATE:    20/08/09 05:14:46 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 05:04:31 UT on 9 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200809A (trigger 618642276.564984 / 200809211).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 205.1, Dec = -26.4 (J2000 degrees, equivalent to J2000 13h 40m, -26d 23'), with a statistical uncertainty of 5.2 degrees.

The angle from the Fermi LAT boresight is 17.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200809211/quicklook/glg_skymap_all_bn200809211.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/bn200809211/quicklook/glg_healpix_all_bn200809211.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200809211/quicklook/glg_lc_medres34_bn200809211.gif


GRB_name: GRB200806A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28234
SUBJECT: GRB 200806A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/08/09 12:42:57 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 (ICRR), S. Torii, Y. Akaike, K. Kobayashi (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 long GRB 200806A (Swift detection: Ambrosi et al., GCN Circ. 28211,
Lien et al., GCN Circ. 28223; AstroSat CZTI detection: Gupta et al.,
GCN Circ. 28216; https://gcn.gsfc.nasa.gov/other/200806A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 15:28:52.289 UTC
on 6 August 2020. 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-peaked structure which starts
at T-2.7 sec, peaks at T+20.0 sec and ends at T+40.9 sec.
The T90 and T50 durations measured by the SGM data are 33.4 +- 3.1 sec
and 14.5 +- 2.0 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1280762930/

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


GRB_name: GRB200808A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28235
SUBJECT: GRB 200808A: AGILE detection
DATE:    20/08/09 13:27:57 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected emission most likely associated with the long
burst GRB 200808A reported by Fermi-GBM (GCN #28230). The event is visible
in the scientific ratemeters of the SuperAGILE detector (SA; 18-60 keV),
starting at T0 = 2020-08-08 11:15:05 (UT). The SA light curve shows two
separate emission episodes about 250 s apart. The first episode lasted
about 27 s and released ~4350 counts; the second episode lasted about 50 s
and released ~7900 counts in the detector, above a background rate of 60
Hz. The event has an off-axis angle of about 40 degrees. The SA light curve
can be found at:
http://www.agilescienceapp.it/notices/GRB200808A_AGILE_RMs.png .

No detection is visible in the scientific ratemeters of the MiniCALorimeter
(MCAL; 0.4-100 MeV).

Additional analysis of AGILE data is in progress.


GRB_name: GRB200809B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28236
SUBJECT: GRB 200809B: Fermi GBM Final Real-time Localization
DATE:    20/08/09 15:51:48 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 15:41:27 UT on 9 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200809B (trigger 618680492.129862 / 200809654).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 359.8, Dec = -76.9 (J2000 degrees, equivalent to J2000 23h 59m, -76d 54'), with a statistical uncertainty of 3.4 degrees.

The angle from the Fermi LAT boresight is 116.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200809654/quicklook/glg_skymap_all_bn200809654.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/bn200809654/quicklook/glg_healpix_all_bn200809654.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200809654/quicklook/glg_lc_medres34_bn200809654.gif


GRB_name: GRB200809B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28237
SUBJECT: GRB 200809B: Swift/BAT-GUANO detection and arcminute localization
DATE:    20/08/09 18:57:54 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), James DeLaunay (PSU), Jamie Kennea (PSU) report:

Swift/BAT did not trigger on GRB 200809B (T0: 2020-08-09 15:41:27 UTC,
Fermi/GBM Team GCN 28236).

The Fermi/GBM notice, distributed at T0+7 seconds triggered the Swift
Mission Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, arXiv: 2005.01751).

Upon trigger by this notice, GUANO sent a command to the Swift Burst
Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from
[-50,+150] seconds around the time of the burst. All the requested
event mode data was delivered to the ground.

Using the normal BAT imaging technique, we find the location of the
GRB with an SNR of 10.4.

The BAT ground-calculated position is
RA, Dec = 15.9406, -73.8459 deg which is
   RA(J2000)  = 01h 3m 45.7s
   Dec(J2000) =  -73d 50â€™ 45.24â€
with an uncertainty of 4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 28.9%.

This position is consistent with the Fermi GBM localization (GCN 28236).

XRT and UVOT follow-up has been triggered. Results of follow-up
observations will be reported in future circulars.

GUANO is a fully autonomous, extremely low latency, spacecraft
commanding pipeline designed for targeted recovery of BAT event mode
data around the times of compelling astrophysical events to enable
more sensitive GRB searches.

A live reporting of Swift/BAT event data recovered by GUANO can be
found at: https://www.swift.psu.edu/guano/


GRB_name: GRB200809B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28238
SUBJECT: GRB 200809B: AstroSat CZTI detection
DATE:    20/08/09 19:31:34 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 200809B, which was also detected by Fermi GBM (GCN #28236) and Swift/BAT-GUANO (Tohuvavohu A. et al., GCN #28237).

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 2020-08-09 15:41:26.500 UT. The measured peak count rate associated with the burst is 371 +/- 30 cts/s above the background in the combined data of four quadrants, with a total of 706 +/- 7 cts. The local mean background count rate was 537 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 5.44 +/- 0.01 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-08-09 15:41:25.000 UT. The measured peak count rate is 583 +/- 48 cts/s above the background in the combined Veto data of four quadrants, with a total of 785 +/- 19 cts. The local mean background count rate was 1637 +/- 2 cts/s.  We measure a T90 of 5.72 +/- 0.45 s from the cumulative Veto light curve.

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: GRB200809B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28239
SUBJECT: GRB 200809B: Swift ToO observations
DATE:    20/08/09 19:32:22 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 200809B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021026

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: GRB200809B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28240
SUBJECT: GRB 200809B: MAXI/GSC detection
DATE:    20/08/10 03:27:53 GMT
FROM:    Satoshi Sugita at Aoyama Gakuin U.  <sugita@phys.aoyama.ac.jp>

S. Sugita (AGU), H. Negoro, M. Nakajima, M. Aoki,
K. Kobayashi, R. Takagi, K, Asakura, K, Seino (Nihon U.),
T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.),
M. Shidatsu (Ehime U.), N. Kawai, R. Adachi, M. Niwano (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M.
Tominaga, T. Nagatsuka (JAXA),
Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi, K. Miike (Miyazaki U.),
Y. Kawakubo (LSU), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), 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 15:41:27 UT on 2020 Aug 9.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (15.369 deg, -73.867 deg) = (01 01 28, -73 52 01) (J2000)
with a 90% C.L. statistical error of 0.38 deg and an additional
systematic uncertainty of 0.1 deg (90% containment radius).
The position was consistent with GRB200809B (Fermi GBM: GCN 28236,
Swift BAT: 28237).
The X-ray flux averaged over the scan was 94 +- 17 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the next transit at 8/9
17:14 UT with an upper limit of 20 mCrab.


GRB_name: GRB200809B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28241
SUBJECT: GRB 200809B: Swift-XRT afterglow detection
DATE:    20/08/10 09:24:54 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@inaf.it>

M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea
(PSU), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), A.P. Beardmore
(U. Leicester), J.P. Osborne (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 GRB 200809B
(detected by Fermi/GBM, GCN 28236, Swift/BAT, GCN 28237, and MAXI/GSC,
GCN 28240), collecting 3.1 ks of Photon Counting (PC) mode data between
T0+14.0 ks and T0+41.4 ks. 

Two uncatalogued X-ray sources are detected, of which one ("Source 1")
is  believed to be the afterglow. Using 1323 s of PC mode data and 2
UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 15.82953, -73.84557 which is equivalent to:

RA (J2000): 01h 03m 19.09s
Dec(J2000): -73d 50' 44.1"

with an uncertainty of 4.5 arcsec (radius, 90% confidence). This
position is 111 arcsec from the Swift/BAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.7 (+2.0, -1.2).

If the light curve continues to decay with a power-law decay index of
1.7, the count rate at T+24 hours will be 1.1 x 10^-3 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021026.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021026.

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


GRB_name: GRB200809B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28242
SUBJECT: GRB 200809B: BOOTES-3/YA optical upper limit
DATE:    20/08/10 12:36:13 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), I. Carrasco and C. Perez del Pulgar (Univ. de Malaga), M. D. Caballero-Garcia (ASU-CAS, CZ) and R. Querel (NIWA), on behalf of a larger collaboration report:

The 60cm BOOTES-3/YA robotic telescope at NIWA Lauder in Otago (New Zealand) gathered images covering the position of the position of the Swift/XRT X-ray afterglow of Fermi GRB 200809B (Fermi team. GCNC 28236). The first image (clear filter) was obtained starting at 09:58:18.81 UT 10th Aug (~ 18.4 hr after trigger). In the co-added image (5 exposures 60s each), no source is found at the position reported by Swift/XRT (Perri et al. GCNC 28241) down to 19.8 mag. Further observations are ongoing.

We thank the staff at NIWA for its excellent support.


GRB_name: GRB200809B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28243
SUBJECT: Fermi GRB 200809B: Global MASTER-Net observations report 
DATE:    20/08/10 17:15:10 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-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) started inspect of the Fermi GRB 200809B ( Fermi GBM team, GCN 28236) errorbox  27196 sec after notice time and 27226 sec after trigger time at 2020-08-09 23:15:13 UT, with upper limit up to  18.3 mag. Observations started at twilight.  The observations began at zenith distance = 71 deg. The sun  altitude  is -15.3 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200809B errorbox  1 days 4224 sec after notice time and 1 days 4253 sec after trigger time at 2020-08-10 16:52:21 UT, with upper limit up to  17.9 mag. Observations started at twilight.  The observations began at zenith distance = 65 deg. The sun  altitude  is -9.8 deg. 

The galactic latitude b = -40 deg., longitude l = 307 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1416521

We obtain a following upper limits.  

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

   27316 | 2020-08-09 23:15:13 |         MASTER-OAFA | (01h 02m 46.23s , -74d 39m 11.1s) |   C |   180 | 18.0 |        
   27749 | 2020-08-09 23:22:26 |         MASTER-OAFA | (01h 02m 47.91s , -74d 41m 22.8s) |   C |   180 | 18.1 |        
   28173 | 2020-08-09 23:29:29 |         MASTER-OAFA | (01h 02m 50.85s , -74d 39m 24.3s) |   C |   180 | 18.2 |        
   28598 | 2020-08-09 23:36:34 |         MASTER-OAFA | (01h 02m 54.25s , -74d 39m 46.9s) |   C |   180 | 18.2 |        
   29023 | 2020-08-09 23:43:40 |         MASTER-OAFA | (01h 02m 49.90s , -74d 39m 21.1s) |   C |   180 | 18.0 |        
   29448 | 2020-08-09 23:50:44 |         MASTER-OAFA | (01h 02m 50.04s , -74d 41m 20.6s) |   C |   180 | 18.0 |        
   31197 | 2020-08-10 00:19:53 |         MASTER-OAFA | (01h 02m 59.48s , -74d 39m 21.9s) |   C |   180 | 18.3 |        
   31618 | 2020-08-10 00:26:55 |         MASTER-OAFA | (01h 02m 53.37s , -74d 39m 10.0s) |   C |   180 | 18.3 |        
   57541 | 2020-08-10 07:38:58 |         MASTER-OAFA | (01h 02m 58.89s , -74d 41m 01.4s) |   C |   180 | 16.8 |        
   57741 | 2020-08-10 07:42:17 |         MASTER-OAFA | (01h 02m 56.20s , -74d 39m 38.4s) |   C |   180 | 17.1 |        
   57940 | 2020-08-10 07:45:37 |         MASTER-OAFA | (01h 02m 56.15s , -74d 41m 07.6s) |   C |   180 | 17.4 |        
   58140 | 2020-08-10 07:48:57 |         MASTER-OAFA | (01h 02m 59.81s , -74d 39m 27.4s) |   C |   180 | 17.2 |        
   58340 | 2020-08-10 07:52:16 |         MASTER-OAFA | (01h 02m 53.24s , -74d 40m 19.7s) |   C |   180 | 16.6 |        
   58539 | 2020-08-10 07:55:36 |         MASTER-OAFA | (01h 02m 53.57s , -74d 39m 21.4s) |   C |   180 | 16.5 |        
   90684 | 2020-08-10 16:52:21 |         MASTER-SAAO | (23h 43m 25.70s , -78d 04m 51.2s) |   C |    60 | 17.5 |        
   90684 | 2020-08-10 16:52:21 |         MASTER-SAAO | (00h 17m 44.42s , -78d 03m 55.8s) |   C |    60 | 17.4 |        
   90763 | 2020-08-10 16:53:40 |         MASTER-SAAO | (23h 43m 26.71s , -78d 04m 49.1s) |   C |    60 | 17.6 |        
   90763 | 2020-08-10 16:53:40 |         MASTER-SAAO | (00h 17m 45.09s , -78d 03m 53.9s) |   C |    60 | 17.5 |        
   90843 | 2020-08-10 16:55:00 |         MASTER-SAAO | (23h 40m 17.20s , -80d 05m 50.2s) |   C |    60 | 17.7 |        
   90843 | 2020-08-10 16:55:00 |         MASTER-SAAO | (00h 21m 30.38s , -80d 04m 52.9s) |   C |    60 | 17.6 |        
   90923 | 2020-08-10 16:56:20 |         MASTER-SAAO | (00h 15m 05.09s , -76d 03m 10.0s) |   C |    60 | 17.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200809B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28244
SUBJECT: GRB 200809B: Fermi GBM detection
DATE:    20/08/10 17:48:07 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

"At 15:41:27.13 UT on 09 August 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200809B (trigger 618680492 / 200809654)
which was also detected by the Swift/BAT-GUANO (Tohuvavohu et al. 2020, GCN
28237)
The Fermi GBM Final Real-time Localization (GCN 28236) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 111
degrees.

This burst was also independently detected by MAXI/GSC (GCN 28240)
and AstroSat CZTI (GCN 28238).

The GBM light curve consists of a single peak
with a duration (T90) of about 17 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+17.6 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.5 +/- 0.3 and
the cutoff energy, parameterized as Epeak, is 682 +/- 246 keV.


The event fluence (10-1000 keV) in this time interval is
(3.717 +/- 0.387)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.13 s in the 10-1000 keV band
is 4.7 +/- 0.3 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
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: GRB200811A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28245
SUBJECT: GRB 200811A: BALROG localization (Fermi Trigger 618851447 / GRB 200811632)
DATE:    20/08/11 15:35:30 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
618851447 at 15:10:42 on 11 Aug. 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) = 122.2+/-1.8 deg
Decl.(2000.0) = -4.9+/-1.8 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200811632/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200811632/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200811632/json

                        


GRB_name: GRB200811A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28246
SUBJECT: GRB 200811A: Fermi GBM Final Real-time Localization
DATE:    20/08/11 17:38:58 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

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

At 15:10:42 UT on 11 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200811A (trigger 618851447 / 200811632).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 120.2, Dec = -4.80 (J2000 degrees, equivalent to J2000 8h 1m, -4d 48'), with a statistical uncertainty of 1.7 degrees.

The angle from the Fermi LAT boresight is 60.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200811632/quicklook/glg_skymap_all_bn200811632.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/bn200811632/quicklook/glg_healpix_all_bn200811632.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200811632/quicklook/glg_lc_medres34_bn200811632.gif


GRB_name: GRB200817A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28254
SUBJECT: GRB 200817A: Fermi GBM Final Real-time Localization
DATE:    20/08/17 09:36:37 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 09:25:20 UT on 17 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200817A (trigger 619349125.224034 / 200817393).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 194.5, Dec = 51.8 (J2000 degrees, equivalent to J2000 12h 58m, 51d 47'), with a statistical uncertainty of 16.5 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/2020/bn200817393/quicklook/glg_skymap_all_bn200817393.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/bn200817393/quicklook/glg_healpix_all_bn200817393.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200817393/quicklook/glg_lc_medres34_bn200817393.gif


GRB_name: GRB200815A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28255
SUBJECT: GRB 200815A: CALET Gamma-Ray Burst Monitor detection of a short burst
DATE:    20/08/17 12:01:19 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

K. Kobayashi (Waseda U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), S. Torii, Y. Akaike (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:

At 21:02:43.555 UTC on 15 August 2020, the CALET Gamma-ray Burst Monitor
(CGBM) triggered on short GRB 200815A. The burst signal was seen mainly by
the SGM detector.
Because of a problem in one of the ground alert processing script, the GCN
notice was not distributed automatically for this event.

This short GRB is also clearly seen by the publicly available
INTEGRAL SPI-ACS light curve.

The burst light curve shows a short pulse which starts at T-0.056 sec,
peaks at T-0.040 sec and ends at T+0.064 sec. The T90 and T50 durations
measured by the SGM data are 0.104 +- 0.025 sec and 0.056 +- 0.008 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1281560544/

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


GRB_name: GRB200817A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28256
SUBJECT: Fermi GRB 200817A: Global MASTER-Net observations report 
DATE:    20/08/17 14:00:19 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-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200817A ( Fermi GBM team, GCN 28254) errorbox  14716 sec after notice time and 14749 sec after trigger time at 2020-08-17 13:31:09 UT, with upper limit up to  18.3 mag. Observations started at twilight.  The observations began at zenith distance = 43 deg. The sun  altitude  is -10.0 deg. 

The galactic latitude b = 66 deg., longitude l = 120 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1421422

We obtain a following upper limits.  

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

   14780 | 2020-08-17 13:31:09 |        MASTER-Tunka | (12h 57m 56.42s , +58d 23m 36.8s) |   C |    60 | 16.9 |        
   14859 | 2020-08-17 13:32:29 |        MASTER-Tunka | (13h 14m 28.63s , +56d 23m 12.7s) |   C |    60 | 17.1 |        
   14939 | 2020-08-17 13:33:49 |        MASTER-Tunka | (12h 45m 43.50s , +56d 22m 38.3s) |   C |    60 | 17.2 |        
   15018 | 2020-08-17 13:35:08 |        MASTER-Tunka | (13h 02m 54.40s , +54d 23m 36.1s) |   C |    60 | 17.4 |        
   15098 | 2020-08-17 13:36:27 |        MASTER-Tunka | (12h 57m 48.21s , +58d 24m 27.1s) |   C |    60 | 17.3 |        
   15177 | 2020-08-17 13:37:47 |        MASTER-Tunka | (13h 13m 04.06s , +58d 23m 38.4s) |   C |    60 | 17.5 |        
   15257 | 2020-08-17 13:39:07 |        MASTER-Tunka | (13h 14m 22.85s , +56d 22m 39.2s) |   C |    60 | 17.7 |        
   15337 | 2020-08-17 13:40:26 |        MASTER-Tunka | (13h 28m 48.70s , +56d 22m 54.9s) |   C |    60 | 17.7 |        
   15416 | 2020-08-17 13:41:46 |        MASTER-Tunka | (12h 45m 42.90s , +56d 23m 42.2s) |   C |    60 | 17.7 |        
   15496 | 2020-08-17 13:43:06 |        MASTER-Tunka | (13h 00m 03.48s , +56d 22m 46.0s) |   C |    60 | 17.8 |        
   15577 | 2020-08-17 13:44:27 |        MASTER-Tunka | (13h 03m 00.68s , +54d 24m 04.9s) |   C |    60 | 18.0 |        
   15657 | 2020-08-17 13:45:47 |        MASTER-Tunka | (13h 16m 32.39s , +54d 23m 33.9s) |   C |    60 | 18.2 |        
   15737 | 2020-08-17 13:47:06 |        MASTER-Tunka | (13h 12m 57.57s , +58d 24m 26.9s) |   C |    60 | 18.1 |        
   15816 | 2020-08-17 13:48:26 |        MASTER-Tunka | (13h 28m 47.54s , +56d 23m 39.4s) |   C |    60 | 18.1 |        
   15895 | 2020-08-17 13:49:45 |        MASTER-Tunka | (12h 59m 59.01s , +56d 22m 13.0s) |   C |    60 | 18.2 |        
   15975 | 2020-08-17 13:51:05 |        MASTER-Tunka | (13h 16m 37.84s , +54d 22m 52.0s) |   C |    60 | 18.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200818A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28261
SUBJECT: GRB 200818A: Fermi GBM Final Localization
DATE:    20/08/19 01:10:59 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

The Fermi GBM team reports the detection of a likely long GRB.

At 23:57:18.34 UT on 18 August 2020, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 200818A (trigger 619487843 / 200818889).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 207.6, Dec = +22.1(J2000 degrees, equivalent to J2000 +13h 50m, +22d
07'), with a statistical uncertainty of 12 degrees.

The angle from the Fermi LAT boresight is 67 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200818889/quicklook/glg_skymap_all_bn200818889.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/bn200818889/quicklook/glg_healpix_all_bn200818889.fit


GRB_name: GRB200819A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28263
SUBJECT: GRB 200819A: Swift detection of a burst
DATE:    20/08/19 16:04:22 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Dichiara (NASA/GSFC/UMCP), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), P. A. Evans (U Leicester), C. Gronwall (PSU),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), 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 15:43:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200819A (trigger=992099).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 21.428, +63.048 which is 
   RA(J2000) = 01h 25m 43s
   Dec(J2000) = +63d 02' 52"
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 10 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 15:45:17.4 UT, 84.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 21.4240, 63.0614 which
is equivalent to:
   RA(J2000)  = 01h 25m 41.76s
   Dec(J2000) = +63d 03' 40.9"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 48 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 9.84
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 88 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 large, but uncertain, extinction expected. 

We note that this source is near the Galactic plane (lat=0.45, lon=126.8 
degrees) which raises the possibility that this is a new Galactic transient. 
The source is somewhat soft (visible above 50 keV but not above 100 keV). 
The lightcurve is consistent with either a GRB or a Galactic transient. 
The complete dataset from this event and further observations of
the source will determine the nature of this source. 
If it is a Galactic transient we would name it Swift J0125.7+6303 . 

Burst Advocate for this burst is S. Dichiara (dichiara AT umd.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: GRB200819A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28264
SUBJECT: Swift GRB 200819A: Global MASTER-Net observations report 
DATE:    20/08/19 16:58:19 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-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Swift GRB 200819A ( S. Dichiara et al., GCN 28263) errorbox  80 sec after notice time and 149 sec after trigger time at 2020-08-19 15:46:22 UT, with upper limit up to  17.7 mag. The observations began at zenith distance = 39 deg. The sun  altitude  is -23.8 deg. 

The galactic latitude b =  1 deg., longitude l = 127 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1422693

We obtain a following upper limits.  

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

     165 |        MASTER-Tunka |  P| |    30 | 16.3 |        
     465 |        MASTER-Tunka |  P| |   630 | 17.7 |  Coadd 
     219 |        MASTER-Tunka |  P| |    40 | 16.5 |        
     284 |        MASTER-Tunka |  P| |    50 | 16.7 |        
     358 |        MASTER-Tunka |  P| |    60 | 16.9 |        
     448 |        MASTER-Tunka |  P| |    80 | 17.0 |        
     557 |        MASTER-Tunka |  P| |   100 | 16.8 |        
     687 |        MASTER-Tunka |  P| |   120 | 16.6 |        
     841 |        MASTER-Tunka |  P| |   150 | 16.1 |        
    1026 |        MASTER-Tunka |  P| |   180 | 16.1 |        


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


GRB_name: GRB200819A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28265
SUBJECT: GRB 200819A: Enhanced Swift-XRT position
DATE:    20/08/19 18:22:27 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 493 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200819A, 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 = 21.42421, +63.06092 which is equivalent
to:

RA (J2000): 01h 25m 41.81s
Dec (J2000): +63d 03' 39.3"

with an uncertainty of 2.2 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB200819A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28266
SUBJECT: GRB 200819A: Kitab, TSHAO optical upper limit
DATE:    20/08/19 21:04:51 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Kusakin (FAPHI),  A. Novichonok (KIAM), A. Pozanenko 
(IKI), I. Reva (FAPHI), E. Mazaeva (IKI),  A. Volnova (IKI) report on 
behalf of larger GRB follow-up collaboration:

We observed the field of GRB 200819A (Dichiara  et al., GCN 28263) with 
Zeiss-1000 telescope of Tien Shan Astronomical observatory starting on 
August 19 (UT) 18:03:47 and with RC-36 of Kitab observatory on (UT) 
16:30:50.   We do not detect any optical object within enhanced XRT 
position (Evans et al., GCN 28265). Preliminary photometry of the field 
is following.

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

2020-08-19  16:30:50 0.05345   CR     3600  n/d  n/d    20.0 RC-36
2020-08-19  18:03:47 0.10289   R      990   n/d  n/d    21.2 Zeiss-1000


The photometry is based on nearby USNO-B1.0 stars.

Ref.stars
USNO-B1.0_id R2
1530-0056474 15.45
1530-0056771 15.06


GRB_name: GRB200819A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28267
SUBJECT: GRB 200819A / Swift J0125.7+6303: Ondrejov Perek-2m optical limit
DATE:    20/08/19 21:25:18 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek, Jan Strobl and Ludek Rezba
(ASU CAS Ondrejov, CZ), report:

We observed the location of the GRB 200819A / Swift
J0125.7+6303 (Dichiara et al, GCNC 28263), with the
photometric camera of the 2m Perek telescope of Ondrejov
observatory in the Czech Republic.

The observations consisted of 20 x 120s dithered SDSS-z'
exposures, starting at 20:30:19 UT, with observation mean
time 5.08h after the initial trigger. There is no source
detected within the XRT errorbox (Evans et al, GCN28265), we
estimate the magnitude limit of our combined image as
z'>22.0


GRB_name: GRB200819A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28269
SUBJECT: GRB 200819A: MITSuME Akeno optical upper limits
DATE:    20/08/19 23:59:46 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

K. L. Murata, R. Hosokawa, R. Adachi, M. Niwano, F. Ogawa, N.
Nakamura, N. Ito, S. Ogata, H. Takamatsu, H. Hara, Y. Yatsu, and N.
Kawai (Tokyo Tech), Takashi Horiuchi, Hidekazu Hanayama (NAOJ) report
on behalf of the MITSuME collaboration:

We observed the field of GRB 200819A (Dichiara et al., GCN 28263;
Evans et al., GCN 28265) 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 with a series of 60 sec exposures started on
2020-08âˆ’19 15:45:44 UT. Some images were heavily affected by bad
weather conditions. We stacked the images with good weather
conditions. We did not find any new point sources within the enhanced
Swift/XRT error circle (Evans et al., GCN 28265) of the stacked
images. We obtained the 5-sigma limits as follows.

T0+[sec] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
~290 2020-08-19T17:36:48 5640 gâ€™>18.4, Rc>19.0, Ic>19.3
------------------------------------------------------------------------------------------------
T0+: Elapsed time after the burst
T-EXP: Total Exposure time

We used the PS1 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., submitted;
https://github.com/MNiwano/Eclaire)


GRB_name: GRB200729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28270
SUBJECT: GRB 200729A: Lowell Discovery Telescope observations
DATE:    20/08/20 02:43:52 GMT
FROM:    Simone Dichiara at UMCP/NASA/GSFC  <dichiara@umd.edu>

S.Dichiara (UMD, NASA-GSFC), P. Gatkine (UMD), J. Durbak (UMD),
S.B. Cenko (NASA-GSFC), E. Troja (UMD, NASA-GSFC), A. Kutyrev (UMD,
NASA-GSFC), S. Veilleux (UMD), report on behalf of a larger
collaboration:

We observed the field of GRB 200729A (Evans et al., GCN Circ. 28165)
using the Large Monolithic Imager (LMI) on the 4.3m Lowell Discovery
Telescope (LDT) at Happy Jack, AZ. Observations started on August 17,
03:52:06 UT (18.34 days after the Swift trigger) taking 6 exposures of
150 s each with SDSS i filter. Observations were taken at an airmass of
about 2.4 and seeing of 1.9".
We do not find any source inside the enhanced XRT position  (Osborne et
al., GCN Circ. 28168) down to a 3-sigma limiting magnitude of i>21.8
AB mag.

Magnitudes are calibrated against the SDSS catalog and not corrected for
Galactic extinction.

The time of our observation corresponds to the typical peak time for an
associated supernova. Therefore, our upper limit on the supernova
component strengthens the hypothesis of a chance alignment of the GRB
with the foreground galaxy NGC 4242, which is at a distance of ~ 7.5 Mpc
(Anand et al., GCN Circ. 28175). In particular we note that our limit is
about 11.6 magnitudes deeper than the one expected from a SN1998bw-like
supernova at the same distance (without correcting for the large but
uncertain extinction; Tohuvavohu et al., GCN Circ. 28176).

We thank the staff of the Lowell Discovery Telescope for assistance with
these observations.


GRB_name: GRB200819A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28271
SUBJECT: GRB 200819A: MITSuME Ishigaki optical upper limits
DATE:    20/08/20 04:43:13 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

Takashi Horiuchi, Hidekazu Hanayama (NAOJ), Katsuhiro L. Murata,
Yoichi Yatsu, Nobuyuki Kawai (Tokyo Tech) report on behalf of the
MITSuME collaboration:

We observed the field of GRB 200819A (Dichiara et al., GCN 28263;
Evans et al., GCN 28265) with the optical three color (g', Rc, and Ic)
CCD cameras attached to the 105 cm Murikabushi telescope of
Ishigakijima Astronomical Observatory, Okinawa, Japan.

The observation with a series of 60 sec exposures started on
2020-08âˆ’19 16:35:33 UT. Throughout, the images were terribly extended
by the altitude oscillation of the Murikabushi Telescope. We stacked
the 79 images and did not find any new point sources other than the
USNO-B1.0 sources from the stacked images. We obtained the SN = 10
limits as follows.

T0+[min] MID-UT T-EXP[sec] SN=10 limits
------------------------------------------------------------------------------------------------
52 2020-08-19T17:21:38 960 g'>18.7, Rc>19.0, Ic>17.8
------------------------------------------------------------------------------------------------


GRB_name: GRB200819A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28272
SUBJECT: GRB 200819A: Swift-XRT refined Analysis
DATE:    20/08/20 08:08:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.3 ks of XRT data for GRB 200819A (Dichiara et al.
GCN Circ. 28263), from 94 s to 40.7 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. 28265).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.83 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+/-0.5). The
best-fitting absorption column is  2.2 (+1.1, -0.9) x 10^22 cm^-2, in
excess of the Galactic value of 9.8 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 7.6 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+1.1, -0.9) x 10^22 cm^-2
Galactic foreground: 9.8 x 10^21 cm^-2
Excess significance: 2.3 sigma
Photon index:      1.6 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
0.83, the count rate at T+24 hours will be 2.3 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (2.9 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/00992099.

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


GRB_name: GRB200819A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28273
SUBJECT: GRB 200819A: Optical Observations from HCT
DATE:    20/08/20 16:13:01 GMT
FROM:    Anirban Dutta at Indian Inst. of Astrophysics  <anirban.dutta@iiap.res.in>

Anirban Dutta(IIA, Bengaluru), Brajesh Kumar(ARIES, Nainital), Avinash
Singh, G. C. 
Anupama, D. K. Sahu and Pramod Kumar (IIA, Bengaluru)

 We observed the field of GRB 200819A (Dichiara et
 al., GCN #28263;  Evans et al., GCN #28265) with the Himalaya Faint
Object
 Spectrograph and Camera  (HFOSC) mounted on the 2-m Himalayan Chandra
Telescope (IAO, Hanle, India). Multiple frames (each 300 sec) of the GRB
field in Bessell R and I bands were obtained with an average airmass of
1.3
and a seeing of  2''. Preliminary PSF photometry on the stacked
images was performed and calibrated against  USNO-B1 catalogue. We do
not
detect any OT within the enhanced XRT position (Belkin et al., GCN
#28266;  Jelinek et al., GCN #28267).

The estimated limiting magnitude is as under -
 Date          |       UT (mean)     | Filter |  Exp time x no. of
frames |  Upper limit (mag)
 2020-08-19        19:16:23          R                300 sec x 4       
               21.5
 2020-08-19        19:32:37          I                 300 sec X 4      
                20.3 

We thank the staff at IAO and CREST for helping with the observations.


GRB_name: GRB200815A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28274
SUBJECT: IPN triangulation of GRB 200815A (short)
DATE:    20/08/20 18:29:49 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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. 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 short-duration 200815A
(CALET-GBM detection: Kobayashi et al., GCN Circ. 28255)
has been detected by Konus-Wind, INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND), and Swift (BAT), so far,
at about 75764 s UT (21:02:44).
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:
   356.686 (23h 46m 45s) -27.798 (-27d 47' 54")
  Corners:
   356.902 (23h 47m 36s) -27.811 (-27d 48' 41")
   356.836 (23h 47m 21s) -28.066 (-28d 03' 58")
   356.471 (23h 45m 53s) -27.785 (-27d 47' 05")
   356.536 (23h 46m 09s) -27.528 (-27d 31' 39")
  ---------------------------------------------
The error box area is 357 sq. arcmin, and its maximum
dimension is 36 arcmin (the minimum one is 7 arcmin).
The Sun distance was 148 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200815_T75768/IPN

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


GRB_name: GRB200815A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28275
SUBJECT: GRB 200815A: MASTER optical observations
DATE:    20/08/20 20:09:03 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov,  E. Gorbovskoy, V.Kornilov, N.Tyurina, K.Zhirkov,P.Balanutsa,A.Kuznetsov,F.Balakin,
V.Vladimirov, A.Chasovnikov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Topolev, 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 (Irkutsk State University, API),
A. Gabovich, Yu. Sergienko, V.Yurkov (Blagoveschensk Educational State University)


MASTER Global Robotic Net  (Lipunov et al., 2010, Advances in Astronomy, vol. 2010, p.30L)
started  GRB 2008015A (IPN triangulation, Hurley et al. GCN 28274) errorbox observations
22881 sec after notice time (1 days 3261 sec after trigger time) at 
2020-08-16 21:57:09 UT in MASTER-Tavrida, with upper limit up to  19.0 mag.
The observations began at zenith distance = 76 deg. The sun  altitude  was -32.5 deg.

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory) 
started inspect of the IPN GRB200815.88 errorbox  26435 sec after notice 
time and 1 days 6815 sec after trigger time at 2020-08-16 22:56:23 UT, 
with upper limit up to  17.4 mag. The observations began at zenith 
distance = 82 deg. The sun  altitude  is -37.9 deg.

The galactic latitude b = -60 deg., longitude l = 98 deg.
We didn't find OT.

Real time updated cover map is available here:
https://master.sai.msu.ru/site/master2/ligo_1.php?id=11510

We obtained the following upper limits.

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

    89752 | 2020-08-16 21:57:09 |      MASTER-Tavrida | (23h 39m 20.64s , -28d 07m 25.9s) |   C |   180 | 19.0 |
    89952 | 2020-08-16 22:00:30 |      MASTER-Tavrida | (23h 48m 25.29s , -28d 08m 52.4s) |   C |   180 | 18.8 |
    90803 | 2020-08-16 22:14:41 |      MASTER-Tavrida | (23h 48m 28.58s , -28d 07m 39.8s) |   C |   180 | 18.9 |
    93305 | 2020-08-16 22:56:23 |          MASTER-IAC | (23h 45m 32.32s , -28d 00m 54.2s) |   C |   180 | 17.1 |
    93915 | 2020-08-16 23:06:33 |          MASTER-IAC | (23h 45m 29.43s , -28d 00m 38.4s) |   C |   180 | 17.4 |
Filter C is a clear (unfiltred) band.

Cover map is available at
     http://master.sai.msu.ru/static/images/MASTERGRB200815Acmap.png

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


GRB_name: GRB200819A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28276
SUBJECT: GRB 200819A: Swift-BAT refined analysis
DATE:    20/08/21 02:37:04 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), S. Dichiara (NASA/GSFC/UMCP),
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-60 to T+243 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 200819A (trigger #992099)
(Dichiara et al., GCN Circ. 28263).  The BAT ground-calculated position is
RA, Dec = 21.527, 63.061 deg which is
   RA(J2000)  =  01h 26m 06.4s
   Dec(J2000) = +63d 03' 39.3"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The mask-weighted light curve shows a double-peaked structure that starts
at ~T0 and ends at ~T+7 s, followed by some tail emission that
lasts until ~T+27 s. T90 (15-350 keV) is 23.62 +- 6.74 sec (estimated
error including systematics).

The time-averaged spectrum from T-0.72 to T+27.12 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 2.08 +- 0.31.  The fluence in the 15-150 keV band is
3.2 +- 0.6 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from
T+0.31 sec in the 15-150 keV band is 0.6 +- 0.1 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/992099/BA/


GRB_name: GRB200815A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28277
SUBJECT: Konus-Wind observation of GRB 200815A
DATE:    20/08/21 13:06:17 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

Konus-Wind observation of GRB 200815A

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 200815A
(CALET-GBM detection: Kobayashi et al., GCN Circ. 28255;
IPN triangulation: Hurley et al., GCN Circ. 28274)
triggered Konus-Wind at T0=75768.265 s UT (21:02:48.265).

The burst light curve shows a single pulse
which starts at ~T0-0.03 s and has a total duration of ~0.2 s.
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200815_T75768/

As observed by Konus-Wind, the burst
had a fluence of 3.04(-0.39,+0.43)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.038 s,
of 3.33(-0.73,+0.77)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 a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.37(-0.23,+0.27)
and Ep = 516(-89,+116) keV (chi2 = 35/45 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.3
(chi2 = 35/44 dof).

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


GRB_name: GRB200821A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28278
SUBJECT: Swift Trigger 992444: a possible GRB 200821A
DATE:    20/08/21 14:04:25 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Dichiara (NASA/GSFC/UMCP), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), P. A. Evans (U Leicester), C. Gronwall (PSU),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
N. P. M. Kuin (UCL-MSSL), S. Laha (GSFC/UMBC/CRESST),
K. L. Page (U Leicester), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 13:15:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located a possible GRB 200821A (trigger=992444).  Swift slewed 
immediately to the location. 
The BAT on-board calculated location is 
RA, Dec 353.570, -48.277 which is 
   RA(J2000) = 23h 34m 17s
   Dec(J2000) = -48d 16' 37"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a sequence of
short peaks covering about 20 seconds.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~9 sec after the trigger. 

The XRT began observing the field at 13:17:33.3 UT, 147.9 seconds after
the BAT trigger. No source was detected in 1.3 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 250 seconds with the U filter
starting  310 seconds after the BAT trigger. There is a candidate
afterglow in the  rapidly available 2.7'x2.7' sub-image at 
  RA(J2000)  = 23:34:24.51 = 353.60212 
  DEC(J2000) = -48:16:28.4  = -48.27456  with a 90%-confidence error
radius of about 0.83 arc sec. This position is 77.5  arc sec. from the
center of the BAT error circle. The estimated magnitude is  19.92 with
a 1-sigma error of about  0.23. No correction has been made for the 
expected extinction corresponding to E(B-V) of 0.01.  We note there is
a known faint source at this position in the DSS. 

This source lies within the current (Sector 28) field-of-view of TESS camera 2. 

This event has a highly unusual lightcurve for a GRB in BAT. 
The XRT data is dominated by a single hot pixel, which is preventing
rapid analysis of the data to find a counterpart.  The UVOT
detection may be due to the known DSS source. 

For these reasons we cannot confidently say whether this is an instrumental
artifact or an astrophysical source.  Further analysis will require the
downlinked data set. 

Burst Advocate for this burst is S. Dichiara (dichiara AT umd.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: GRB200819A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28281
SUBJECT: GRB 200819A: Swift/UVOT Upper Limits
DATE:    20/08/21 20:55:50 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) and S. Dichiara (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200819A
89 s after the BAT trigger (Dichiara et al., GCN Circ. 28263).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 28265)
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            89          239          147         >20.4
u_FC               301          551          246         >19.0
white               89          601          167         >20.3
b                  557          577           19         >17.7
u                  301          551          246         >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 1.59 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200824A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28283
SUBJECT: GRB 200824A: Fermi GBM Final Real-time Localization
DATE:    20/08/24 14:25:59 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 14:15:38 UT on 24 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200824A (trigger 619971343.818026 / 200824594).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 117.7, Dec = 10.5 (J2000 degrees, equivalent to J2000 07h 50m, 10d 30'), with a statistical uncertainty of 15.4 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/2020/bn200824594/quicklook/glg_skymap_all_bn200824594.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/bn200824594/quicklook/glg_healpix_all_bn200824594.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200824594/quicklook/glg_lc_medres34_bn200824594.gif


GRB_name: GRB200826A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28284
SUBJECT: GRB 200826A: Fermi GBM Final Real-time Localization
DATE:    20/08/26 04:40:17 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 04:29:52 UT on 26 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200826A (trigger 620108997.570644 / 200826187).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 4.7, Dec = 35.3 (J2000 degrees, equivalent to J2000 00h 18m, 35d 17'), with a statistical uncertainty of 1.7 degrees.

The angle from the Fermi LAT boresight is 73.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200826187/quicklook/glg_skymap_all_bn200826187.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/bn200826187/quicklook/glg_healpix_all_bn200826187.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200826187/quicklook/glg_lc_medres34_bn200826187.gif


GRB_name: GRB200826A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28285
SUBJECT: Fermi GRB 200826A: Global MASTER-Net observations report 
DATE:    20/08/26 05:00:17 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),

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-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) started inspect of the Fermi GRB 200826A ( Fermi GBM team, GCN 28284) errorbox  18 sec after notice time and 46 sec after trigger time at 2020-08-26 04:30:38 UT, with upper limit up to  18.3 mag. The observations began at zenith distance = 76 deg. The sun  altitude  is -69.3 deg. 

The galactic latitude b = -24 deg., longitude l = 116 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1427181

We obtain a following upper limits.  

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

      51 | 2020-08-26 04:30:38 |         MASTER-OAFA | (00h 16m 30.99s , +38d 58m 23.2s) |   C |    10 | 16.5 |        
     102 | 2020-08-26 04:31:24 |         MASTER-OAFA | (00h 16m 59.22s , +35d 52m 18.4s) |   C |    20 | 17.0 |        
     159 | 2020-08-26 04:32:16 |         MASTER-OAFA | (00h 18m 21.45s , +36d 49m 55.4s) |   C |    30 | 17.2 |        
     214 | 2020-08-26 04:33:06 |         MASTER-OAFA | (00h 18m 17.46s , +36d 48m 57.2s) |   C |    40 | 17.5 |        
     278 | 2020-08-26 04:34:05 |         MASTER-OAFA | (00h 18m 22.91s , +36d 49m 03.8s) |   C |    50 | 17.6 |        
     353 | 2020-08-26 04:35:15 |         MASTER-OAFA | (00h 18m 20.27s , +36d 50m 58.1s) |   C |    60 | 17.8 |        
     442 | 2020-08-26 04:36:34 |         MASTER-OAFA | (00h 18m 20.68s , +36d 49m 32.1s) |   C |    80 | 17.9 |        
     552 | 2020-08-26 04:38:14 |         MASTER-OAFA | (00h 18m 23.06s , +36d 50m 57.8s) |   C |   100 | 17.8 |        
     683 | 2020-08-26 04:40:15 |         MASTER-OAFA | (00h 17m 00.73s , +35d 50m 57.2s) |   C |   120 | 18.1 |        
     837 | 2020-08-26 04:42:34 |         MASTER-OAFA | (00h 17m 02.07s , +35d 51m 59.4s) |   C |   150 | 18.2 |        
    1022 | 2020-08-26 04:45:24 |         MASTER-OAFA | (00h 17m 08.96s , +35d 51m 02.3s) |   C |   180 | 18.3 |        
    1221 | 2020-08-26 04:48:43 |         MASTER-OAFA | (00h 17m 02.21s , +35d 50m 06.3s) |   C |   180 | 18.3 |        
    1421 | 2020-08-26 04:52:03 |         MASTER-OAFA | (00h 17m 08.56s , +35d 50m 36.7s) |   C |   180 | 18.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200826A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28286
SUBJECT: GRB 200826A: BALROG localization (Fermi Trigger 620108997 / GRB 200826187)
DATE:    20/08/26 05:19:26 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
620108997 at 04:29:52 on 26 Aug. 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) = 7.0+/-2.1 deg
Decl.(2000.0) = 36.1+/-2.4 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200826187/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200826187/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200826187/json

                        


GRB_name: GRB200826A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28287
SUBJECT: GRB 200826A: Fermi GBM observation
DATE:    20/08/26 17:18:41 GMT
FROM:    Joe Mangan at UCD  <joseph.mangan@ucdconnect.ie>

J.Mangan (UCD), R.Dunwoody (UCD) and C.Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 04:29:52.57 UT on 26 August 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200826A (trigger 620108997 / 200826187).

The on-ground calculated location, using the GBM trigger
data, was reported in GCN 28284.

The GBM light curve shows an exceptionally bright short GRB
with a duration (T90) of about 1.14 s (50-300 keV).
The time-averaged spectrum from T0-0.29 s to T0+1.76 s is
best fit by a Band function with Epeak = 89.8 +/- 3.7 keV,
alpha = -0.41 +/- 0.07, and beta = -2.4 +/- 0.1

The event fluence (10-1000 keV) in this time interval is
(4.8 +/- 0.1)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0 s in the 10-1000 keV band
is 39.06 +/- 0.42 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: GRB200826A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28288
SUBJECT: GRB 200826A: AstroSat CZTI detection
DATE:    20/08/26 19:40:25 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a bright short GRB 200826A, which was also detected by Fermi GBM (GCN #28284), Global MASTER-Net (Lipunov V. et al., GCN #28285) and BALROG (Kunzweiler F. et al., GCN #28286).

The source was clearly detected in the 40-200 keV energy range. The light curve showed a single peak of emission peaking at 2020-08-26 04:29:51.529 UT. The measured peak count rate associated with the burst is 686 +/- 34 cts/s above the background in the combined data of four quadrants, with a total of 1383 +/- 10 cts. The local mean background count rate was 537 +/- 2 cts/s. Using cumulative rates, we measure a T90 of 1.95 +/- 0.01 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed a single peak of emission peaking at 2020-08-26 04:29:51.000 UT. The measured peak count rate is 735 +/- 53 cts/s above the background in the combined Veto data of four quadrants, with a total of 1043 +/- 42 cts. The local mean background count rate was 1870 +/- 16 cts/s.  We measure a T90 of 2.17 +/- 0.23 s from the cumulative Veto light curve.

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: GRB200826A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28289
SUBJECT: GRB 200826A: AGILE detection
DATE:    20/08/26 20:30:44 GMT
FROM:    Francesco Verrecchia at SSDC,INAF-OAR  <francesco.verrecchia@ssdc.asi.it>

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

The AGILE satellite detected the short burst GRB 200826A at T0=2020-08-26
04:29:52 (UTC), reported by Fermi-GBM (GCN #28284, trigger 620108997.570644
/ 200826187).

The event was detected by the scientific ratemeters of the Super-AGILE (SA;
18-60 keV) detector. The light curve shows a single peak profile, 
lasting 0.5
s and releasing ~84 counts above an average background rate of about 40
counts/s. The short burst was observed at an off-axis angle of about 54
degrees. The Super-AGILE light curve can be found here:
https://tools.ssdc.asi.it/ImgView/Agile/SA-TOT_GRB200826A_lcr28

Additional analysis of AGILE data is in progress.


GRB_name: GRB200826A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28290
SUBJECT: GRB 200826A: Tiled Swift observations
DATE:    20/08/26 20:46:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/GBM GRB 200826A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00093

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

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

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


GRB_name: GRB200826A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28291
SUBJECT: IPN triangulation of GRB 200826A (short/bright)
DATE:    20/08/26 21:28:52 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,

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

and

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

The short-duration, bright GRB 200826A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 28284;
Mangan et al., GCN Circ. 28287;
BALROG localization: Kunzweiler et al., GCN Circ. 28286;
AstroSat-CZTI detection: Gupta et al.,  GCN Circ. 28288;
AGILE detection: Pittori et al.,  GCN Circ. 28289)
has been detected by Fermi (GBM trigger 620108997),
Konus-Wind, INTEGRAL (SPI-ACS), AstroSat (CZTI),
AGILE (SA), and Mars-Odyssey (HEND),
so far, at about 16193 s UT (04:29:53).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
     6.817 (00h 27m 16s) +34.038 (+34d 02' 18")
  Corners:
     7.081 (00h 28m 19s) +34.000 (+34d 00' 00")
     6.808 (00h 27m 14s) +34.222 (+34d 13' 21")
     6.553 (00h 26m 13s) +34.075 (+34d 04' 31")
     6.826 (00h 27m 18s) +33.854 (+33d 51' 14")
  ---------------------------------------------
The error box area is 288 sq. arcmin, and its maximum
dimension is 27 arcmin (the minimum one is 15 arcmin).
The Sun distance was 126 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the Fermi 
RoboBA and BALROG localizations (GCN Circ. 28284 and 28286).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200826_T16195/IPN

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


GRB_name: GRB200826B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28292
SUBJECT: GRB 200826B: Fermi GBM Final Real-time Localization
DATE:    20/08/26 22:19:50 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 22:09:42 UT on 26 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200826B (trigger 620172587.721156 / 200826923).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 151.3, Dec = 51.7 (J2000 degrees, equivalent to J2000 10h 05m, 51d 42'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 96.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200826923/quicklook/glg_skymap_all_bn200826923.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/bn200826923/quicklook/glg_healpix_all_bn200826923.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200826923/quicklook/glg_lc_medres34_bn200826923.gif


GRB_name: GRB200826A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28293
SUBJECT: GRB200826A: Zwicky Transient Facility Follow-Up of a Fermi Short GRB (Trigger 620108997)
DATE:    20/08/26 22:32:02 GMT
FROM:    Tomas Ahumada at U. of Maryland  <tahumada@astro.umd.edu>

Ana Sagues Carracedo (OKC), Harsh Kumar (IITB), Tomas Ahumada (UMD), Igor
Andreoni (Caltech), Shreya Anand (Caltech),  Robert Stein (DESY), Michael
Coughlin (UMN), Leo Singer (NASA/GSFC) on behalf of the Zwicky Transient
Facility (ZTF) and Global Relay of Observatories Watching Transients Happen
(GROWTH) collaborations


We observed the localization region of the short GRB200826A (trigger
620108997) detected by 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.
We obtained a series of g- and r-band images covering 185.5 square degrees
beginning at 09:22:55 UT on 2020 Aug 26 (about 5 hours after the burst
trigger time). This corresponds to ~77.5% of the probability enclosed in
the GRB localization map (GCN 28284). Each exposure was 300s, reaching a
g-band median depth of 22.3 mag and r-band median depth of 22.1 mag. The
median limiting magnitude of the last 5 survey-mode nights (30 sec
exposures) was g ~ 20.6 mag and r ~ 20.0 mag, limiting our capability to
temporally constrain some of our faintest transients. The images were
processed in real-time through the ZTF reduction and image subtraction
pipelines at IPAC (Masci et al. 2019).

We queried the ZTF alert stream using Kowalski (Duev et al. 2019) and AMPEL
(Nordin et al. 2019). We required at least 2 detections separated by at
least 15 minutes to select against moving objects. Furthermore, we
cross-matched our candidates with the Minor Planet Center to flag known
asteroids, reject stellar sources (Tachibana and Miller 2018), and apply
machine learning algorithms (Duev et al. 2019, Mahabal et al. 2019). We
require no spatially coincident ZTF alert to be issued before the detection
time of the GBM trigger. The candidates within the 95% probability contour
of the GRB localization map that passed the automatic selection criteria
and human vetting are presented in the table below.


+----------------------------------------------------------------------------------------------------+
| ZTF Name      | IAU Name  | RA (deg)  | DEC (deg)  | Filter | Mag   |
MagErr | g-r |MJD      | Notes |
+----------------------------------------------------------------------------------------------------+
| ZTF20abwyple  | AT2020sbi | 1.3824038 | 37.3638915 | r | 21.2 | 0.11 |
0.13 | 2459087.9109491 | (a) |
| ZTF20abwyueq  | AT2020sbn | 9.2615748 | 39.6340049 | r | 21.8 | 0.13 |
0.08 | 2459087.9219444 | (a) |
| ZTF20abwyzdb  | AT2020sbp | 9.2046817 | 43.6712369 | r | 21.7 | 0.17 |
0.4  | 2459087.9219444 | (b) |
| ZTF20abwytgj  | AT2020sbc | 5.7051754 | 29.8539268 | r | 22.0 | 0.19 |
0.09 | 2459087.9181366 | (a) |
| ZTF20abwysgz  | AT2020sbm | 8.2746333 | 30.7142518 | r | 20.2 | 0.05 |
0.1  | 2459087.9181366 | (a) |
| ZTF20abwywiz  | AT2020sbv | 1.4094587 | 36.2573281 | r | 21.9 | 0.21 |
0.45 | 2459087.9145486 | (b) |
| ZTF20abwyrop  | AT2020sbd | 359.33861 | 31.1190224 | r | 21.5 | 0.12 |
0.22 | 2459087.9145486 | (c) |
| ZTF20abwyxpj  | AT2020sbs | 12.411974 | 31.7868639 | r | 21.8 | 0.16 |
0.35 | 2459087.9181366 | (c)(d) |
| ZTF20abwypor  | AT2020sbk | 6.8956443 | 37.2409844 | r | 21.5 | 0.13 |
0.15 | 2459087.9109491 | (c) |
| ZTF20abwyvrl  | AT2020sbj | 2.7749043 | 37.6768649 | r | 21.9 | 0.21 |
0.34 | 2459087.9109491 | (a) |
| ZTF20abwypqf  | AT2020sbl | 5.1321015 | 39.4099175 | r | 21.8 | 0.21 |
0.0  | 2459087.9109491 | (a) |
| ZTF20abwyrzs  | AT2020sbo | 359.79701 | 32.1773094 | r | 21.6 | 0.17 |
0.09 | 2459087.9145486 | (a)(d)(e) |
| ZTF20abwzabz  | AT2020sbr | 12.580528 | 42.6494866 | r | 21.9 | 0.16 |
0.02 | 2459087.9219444 | (b)(e) |
| ZTF20abwysmm  | AT2020sbt | 11.333202 | 33.4189371 | r | 21.5 | 0.14 |
0.0  | 2459087.9181366 | (d)(e) |
+----------------------------------------------------------------------------------------------------+
Notes:
(a) offset from a galaxy
(b) nuclear
(c) hostless
(d) PS1 detection at source position
(e) possible point-like source underneath


We checked for galaxies in the GLADE catalog (Dalya et al. 2018) around 100
arcsec of each candidate in the table above. We found crossmatches for
ZTF20abwysgz, which is 25.8 arcsec or 81.7 kpc away from a GLADE galaxy,
and ZTF20abwyrzs, 35.9 arcsec or 163.1 kpc offset. However, there are
several ZTF sources closer in the image to both candidates, which makes an
association between the ZTF candidates and GLADE galaxies improbable. In
fact, many candidates (including ZTF20abwysgz and ZTF20abwyrzs) appear to
be a few arcseconds offset from their possible host galaxies:

name         | separation  |
-------------+--------------
ZTF20abwyple | ~2.7 arcsec |
ZTF20abwypqf | ~1.1 arcsec |
ZTF20abwyple | ~2.6 arcsec |
ZTF20abwyueq | ~1.9 arcsec |
ZTF20abwytgj | ~2.0 arcsec |
ZTF20abwysgz | ~1.6 arcsec |
ZTF20abwyvrl | ~2.3 arcsec |
ZTF20abwypqf | ~5.3 arcsec |
ZTF20abwyrzs | ~5.0 arcsec |

Follow-up observations of these candidates is encouraged.

ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC,
USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY,
Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan;
IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia.
ZTF acknowledges the generous support of the NSF under AST MSIP Grant No
1440341.
GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949.
Alert distribution service provided by DIRAC@UW (Patterson et al. 2019).
Alert database searches are done by AMPEL (Nordin et al. 2019) and Kowalski
(Duev et al. 2019).


GRB_name: GRB200826A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28294
SUBJECT: Konus-Wind detection of GRB 200826A
DATE:    20/08/27 13:29:13 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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 200826A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 28284;
Mangan et al., GCN Circ. 28287;
BALROG localization: Kunzweiler et al., GCN Circ. 28286;
AstroSat-CZTI detection: Gupta et al.,  GCN Circ. 28288;
AGILE detection: Pittori et al.,  GCN Circ. 28289;
IPN triangulation: Hurley et al., GCN Circ. 28291)
triggered Konus-Wind at T0=16195.106 s UT (04:29:55.106).

The burst light curve shows a multipeaked pulse
which starts at ~T0-0.1 s with a total duration of ~1.6 s.
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200826_T16195/

As observed by Konus-Wind, the burst
had a fluence of 3.30(-0.42,+0.47)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.560 s,
of 9.04(-2.49,+2.63)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 - 2 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = 1.27(-1.78,+4.03),
the high-energy photon index beta = -2.32(-0.25,+0.19),
the peak energy Ep = 67(-17,+31) keV
(chi2 = 50/59 dof).

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


GRB_name: GRB200826A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28295
SUBJECT: GRB200826A: Zwicky Transient Facility Identifies Optical Afterglow Candidate of a Fermi Short GRB (Trigger 620108997)
DATE:    20/08/27 16:42:00 GMT
FROM:    Tomas Ahumada at U. of Maryland  <tahumada@astro.umd.edu>

Tomas Ahumada (UMD), Shreya Anand (Caltech), Robert Stein (DESY), Harsh
Kumar (IITB), Ana Sagues Carracedo (OKC), Igor Andreoni (Caltech), Michael
Coughlin (UMN), Leo Singer (NASA/GSFC), Mansi Kasliwal (Caltech), Daniel
Perley (LJMU), Brad Cenko (NASA/GSFC), Varun Bhalerao (IITB), David Kaplan
(UWM) on behalf of the Zwicky Transient Facility (ZTF) and Global Relay of
Observatories Watching Transients Happen (GROWTH) collaborations

We continued a second night of monitoring the localization region of the
short GRB200826A (Fermi trigger 620108997; GCN 28284, 28287) with the
Zwicky Transient Facility (first night summary in Sagues Carracedo et al.
GCN 28293). Each exposure was 600s, reaching a g-band median depth of 22.3
mag and r-band median depth of 22.3 mag. IPN also triangulated this GRB
(Hurley et al. GCN 28291). Our total coverage was >99% of the joint
Fermi-IPN localization.

We followed standard candidate vetting procedures. We identify the
following compelling candidate for the optical afterglow:

+-------------------------------------------------------------------------------------------------+
| ZTF Name      | IAU Name  | RA (deg)  | DEC (deg)   | Filter | Mag   |
MagErr |MJD              |
+---------------+-----------+-----------+-------------+--------+-------+--------+-----------------+
| ZTF20abwysqy  | AT2020scz | 6.7855741 | +34.0273043 |   g    | 20.86 |
0.04   | 2459087.9181366 |
+---------------+-----------+-----------+-------------+--------+-------+--------+-----------------+

ZTF20abwysqy faded by >1.7 mag in 22.5 hours in the g-band. We ran forced
photometry and we obtained the following light curve:

+----------+--------+-------+--------+--------+
Time (Hrs) | Filter | Mag   | MagErr | Limmag |
+----------+--------+-------+--------+--------+
|    5.07  | g      | 20.86 | 0.048  | 22.50  |
|    5.53  | r      | 20.70 | 0.050  | 22.28  |
|    6.67  | g      | 20.96 | 0.168  | 21.24  |
|    27.5  | g      | -     | -      | 22.53  |
|    29.1  | r      | -     | -      | 21.31  |
|    30.9  | g      | -     | -      | 21.21  |
+----------+--------+-------+--------+--------+

ZTF20abwysqy is spatially coincident with X-ray Source 3 reported by the
Neil Gehrels Swift Observatory (GCN 28290,
https://www.swift.ac.uk/xrt_products/TILED_GRB00093/) with a separation of
2" from the XRT position that has an uncertainty of 2.7". It also has a
faint underlying galaxy counterpart within 0.35" (Legacy Survey (LS) DR8
photometric redshift z = 0.714 +- 0.137 and LS DR8 r-mag = 22.55). We
strongly encourage multi-wavelength follow-up.


ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC,
USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY,
Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan;
IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia.
ZTF acknowledges the generous support of the NSF under AST MSIP Grant No
1440341.
GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949.
Alert distribution service provided by DIRAC@UW (Patterson et al. 2019).
Alert database searches are done by AMPEL (Nordin et al. 2019) and Kowalski
(Duev et al. 2019).


-- 
TomÃ¡s Ahumada (he/his)
Ph.D. Student
Department of Astronomy
University of Maryland, College Park
NASA <tomas.f.ahumdamena@nasa.gov> Goddard Space Flight Center, Code 661
B.Sc. Astronomy, Pontificia Universidad CatÃ³lica de Chile


GRB_name: GRB200824A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28296
SUBJECT: Fermi GRB 200824A: Global MASTER-Net observations report 
DATE:    20/08/27 19:09:07 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200824A ( Fermi GBM team, GCN 28283) errorbox  2 days 40217 sec after notice time and 2 days 40245 sec after trigger time at 2020-08-27 01:26:24 UT, with upper limit up to  16.4 mag. Observations started at twilight.  The observations began at zenith distance = 64 deg. The sun  altitude  is -16.3 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200824A errorbox  2 days 68646 sec after notice time and 2 days 68673 sec after trigger time at 2020-08-27 09:20:12 UT, with upper limit up to  17.7 mag. The observations began at zenith distance = 66 deg. The sun  altitude  is -21.4 deg. 

The galactic latitude b = 18 deg., longitude l = 211 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1425935

We obtain a following upper limits.  

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

  213075 | 2020-08-27 01:26:24 |      MASTER-Tavrida | (07h 12m 38.47s , +24d 02m 24.8s) |   C |    60 | 14.7 |        
  214850 | 2020-08-27 01:55:58 |      MASTER-Tavrida | (07h 19m 46.57s , +26d 02m 10.0s) |   C |    60 | 16.4 |        
  214931 | 2020-08-27 01:57:19 |      MASTER-Tavrida | (07h 17m 32.19s , +20d 00m 58.9s) |   C |    60 | 15.2 |        
  215011 | 2020-08-27 01:58:40 |      MASTER-Tavrida | (07h 07m 36.58s , +16d 00m 47.4s) |   C |    60 | 14.0 |        
  215418 | 2020-08-27 02:05:26 |      MASTER-Tavrida | (06h 47m 06.52s , +14d 01m 43.5s) |   C |    60 | 15.4 |        
  215579 | 2020-08-27 02:08:08 |      MASTER-Tavrida | (06h 50m 54.44s , +16d 02m 17.9s) |   C |    60 | 15.3 |        
  241503 | 2020-08-27 09:20:12 |         MASTER-OAFA | (07h 22m 58.21s , -02d 39m 33.4s) |   C |    60 | 17.7 |        
  244022 | 2020-08-27 10:02:11 |         MASTER-OAFA | (07h 22m 58.79s , -02d 38m 33.0s) |   C |    60 | 17.4 |        
  244102 | 2020-08-27 10:03:30 |         MASTER-OAFA | (07h 30m 54.12s , -02d 39m 18.0s) |   C |    60 | 17.4 |        
  244397 | 2020-08-27 10:08:26 |         MASTER-OAFA | (06h 46m 38.15s , +13d 20m 22.5s) |   C |    60 | 17.2 |        
  244477 | 2020-08-27 10:09:45 |         MASTER-OAFA | (07h 03m 11.85s , +13d 20m 43.8s) |   C |    60 | 16.7 |        
  244558 | 2020-08-27 10:11:06 |         MASTER-OAFA | (06h 54m 48.45s , +17d 20m 41.9s) |   C |    60 | 16.7 |        
  244638 | 2020-08-27 10:12:26 |         MASTER-OAFA | (07h 07m 02.70s , +15d 19m 02.3s) |   C |    60 | 16.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200826B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28297
SUBJECT: Fermi GRB 200826B: Global MASTER-Net observations report 
DATE:    20/08/27 19:18:52 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200826B ( Fermi GBM team, GCN 28292) errorbox  640 sec after notice time and 669 sec after trigger time at 2020-08-26 22:20:51 UT, with upper limit up to  16.4 mag. The observations began at zenith distance = 83 deg. The sun  altitude  is -35.3 deg. 

The galactic latitude b = 51 deg., longitude l = 163 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1427827

We obtain a following upper limits.  

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

     734 | 2020-08-26 22:20:51 |      MASTER-Tavrida | (10h 05m 19.01s , +51d 55m 00.9s) |   C |   130 | 14.7 |        
    1129 | 2020-08-26 22:27:01 |      MASTER-Tavrida | (10h 05m 18.37s , +51d 52m 53.7s) |   C |   180 | 14.8 |        
    1558 | 2020-08-26 22:34:11 |      MASTER-Tavrida | (10h 05m 22.98s , +51d 54m 35.8s) |   C |   180 | 14.6 |        
    5955 | 2020-08-26 23:48:27 |      MASTER-Tavrida | (10h 17m 44.99s , +52d 12m 40.0s) |   C |    60 | 13.0 |        
    6197 | 2020-08-26 23:52:29 |      MASTER-Tavrida | (09h 51m 23.97s , +50d 11m 34.2s) |   C |    60 | 14.8 |        
    9451 | 2020-08-27 00:46:43 |      MASTER-Tavrida | (10h 16m 17.78s , +50d 10m 53.5s) |   C |    60 | 15.0 |        
   13932 | 2020-08-27 02:01:24 |      MASTER-Tavrida | (10h 06m 27.15s , +54d 08m 38.9s) |   C |    60 | 16.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200826B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28298
SUBJECT: GRB 200826B: Fermi GBM detection
DATE:    20/08/27 21:10:30 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

C. Malacaria (NASA-MSFC/USRA) and C.Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 22:09:42.72 UT on 26 August 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200826B (trigger 620172587 / 200826923).

The on-ground calculated location, using the GBM trigger
data, was reported in GCN 28292.

The GBM light curve shows an exceptionally bright long GRB
with a duration (T90) of about 7.4 s (50-300 keV).
The time-averaged spectrum from T0-0.003 s to T0+ 12.544 s is
best fit by a Band function with Epeak = 410.3 +/- 5.6  keV,
alpha = -0.64 +/- 0.01, and beta = -2.52 +/- 0.04
The event fluence (10-1000 keV) in this time interval is
(1.414 +/- 0.006)E-04 erg/cm^2. 
The 1.024-sec peak photon flux measured starting from T0+5.1 s in 
the 10-1000 keV band is 110.1 +/- 0.7 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: GRB200824A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28299
SUBJECT: GRB 200824A: Insight-HXMT/HE detection
DATE:    20/08/28 15:39:30 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, C. Cai, 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 2020-08-24T14:15:38.82 (T0), Insight-HXMT/HE detected 
GRB 200824A (trigger ID: HEB200824594) in a routine search of the data, 
which also triggered Fermi-GBM (Fermi GBM team, GCN 28283).

The Insight-HXMT/HE light curve mainly consists of a single 
pulse with a duration (T90) of 1.56 s measured from T0-0.84 s. 
The 1-ms peak rate, measured from T0-0.445 s, is 754 cnts/sec. 
The total counts from this burst is 569 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200824594_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: GRB200826A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28300
SUBJECT: GRB 200826A: Swift-XRT afterglow detection
DATE:    20/08/28 15:55:28 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

A. D'Ai (INAF-IASFPA), B. Sbarufatti (PSU), S. R. Oates (U.
Birmingham), D.N. Burrows (PSU), J. D. Gropp (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), A.
Melandri (INAF-OAB), T. Sbarrato (INAF-OAB) and P.A. Evans (U.
Leicester) report on behalf of the Swift team:

Swift-XRT has performed follow-up observations of theFermi/GBM and IPN
detected burst GRB 200826A (Gupta et al. GCN Circ. 28288, Hurley et
al., GCN Circ. 28291) in a series of observations tiled on the sky. The
total exposure time is 7.4 ks, distributed over 4 tiles; the maximum
exposure at a single sky location was 5.2 ks. The data were collected
between T0+59.9 ks and T0+169.6 ks, and are entirely in Photon Counting
(PC) mode. 

Seven uncatalogued X-ray sources are detected, of which one ("Source
3") is consistent with ZTF20abwysqy, reported by ZTF (Ahumada et al.
GCN Circ. 28293 and 28295). 
Source 3 is fading with 3-sigma significance, and is therefore likely
the GRB afterglow. Using 1504 s of PC mode data and 1 UVOT image, we
find an enhanced XRT position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue): RA, Dec =
6.78466, +34.02670 which is equivalent to:

RA (J2000): 00h 27m 08.32s
Dec(J2000): +34d 01' 36.1"

with an uncertainty of 3.3 arcsec (radius, 90% confidence). This
position is 104 arcsec from the Fermi/GBM position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.3 (+0.7, -0.5).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+0.6, -0.5). The
best-fitting absorption column is  2.2 (+2.5, -1.6) x 10^21 cm^-2,
consistent with the Galactic value of 6.0 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 (4.6 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+2.5, -1.6) x 10^21 cm^-2
Galactic foreground: 6.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.8 (+0.6, -0.5)

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/xrt_products/TILED_GRB00093/Source3.php.

The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00093.

The Swift/UVOT began observations of the optical counterpart
ZTF20abwysqy, 140ks after the Fermi/GBM trigger (Fermi GBM Team, GCN
Circ. 28284). A source consistent with ZTF20abwysqy is detected in the
UVOT summed exposures. ZTF20abwysqy is consistent with XRT source 3,
however no earlier UVOT photometry is avaliable since XRT source 3 is
outside of the field of view for all earlier tiles. The UVOT detection
is possibly explained by the underlying galaxy emission. 

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  140782    169578 5032        21.86 +/- 0.13

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

This circular is an official product of the Swift-XRT and Swift-UVOT
teams.


GRB_name: GRB200826A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28301
SUBJECT: GRB 200826A: further analysis of the Konus-Wind data and classification
DATE:    20/08/28 18:29:11 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, D. Frederiks, A. Ridnaia, and A. Tsvetkova,
on behalf of the Konus-Wind team, report:

Following the X-ray afterglow detection (GCN 28300) and
the identification of possible optical transient (GCN 28295)
spatially coincident with the X-ray source,
we present a further analysis of the KW detection of
the short-duration, soft-spectrum, bright GRB 200826A
(GCNs 28284, 28287, 28288, 28289, 28294).

As observed by KW the burst duration is T50=0.286+/-0.029 s
(T90 = 0.772+/-0.188 s). The position of the GRB 200826A in
the hardness-duration diagram (logT50-logHR32) of 1610 KW bright GRBs
(Svinkin et al., JPhCS 1400, 2, 022010, 2019)
suggests that the burst comes from the long/soft GRB population.
The figure showing the hardness-duration diagram is available at
http://www.ioffe.ru/LEA/GRBs/GRB200826_T16195/GRB200826A_HRT50.png
The contours denote the 1 and 3 sigma confidence regions for
two-dimensional Gaussian distributions. The HR32 is the ratio of counts
in the 200-760 keV and 50-200 keV bands accumulated during burst
duration. The vertical dashed line at T50=0.7 s marks the boundary used
by Svinkin et al. 2019 to distinguish between short and long KW GRBs.

Assuming the redshift of an underlying galaxy z=0.714 (GCN 28295)
and a standard cosmology model 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 is ~4.7x10^51 erg,
the peak luminosity L_iso is ~1.6x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~115 keV.

With these values, GRB 200826A is within the 1 sigma prediction band of
both 'Amati' and 'Yonetoku' relations built for 138 Type II (long/soft) 
GRBs with known z (Tsvetkova et al., ApJ 850 161, 2017).
Meanwile, in both Eiso-Ep,z and Liso-Ep,z planes,
the GRB 200826A position is inconsistent with
short-hard (Type I) GRB population,
see http://www.ioffe.ru/LEA/GRBs/GRB200826_T16195/GRB200826A.pdf

Thus, from the analysis of the KW detection, we conclude, that,
GRB 200826A may be classified as Type II (long/soft, core-collapse origin).


GRB_name: GRB200826A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28302
SUBJECT: GRB 200826A: VLA Detection at 6 GHz
DATE:    20/08/28 19:27:02 GMT
FROM:    Kate Alexander at Northwestern U  <kate.alexander@northwestern.edu>

K. D. Alexander, W. Fong, K. Paterson, and J. Rastinejad (Northwestern)
report on behalf of a larger collaboration:

We observed the Fermi GRB 200826A (Fermi GBM Team GCN 28284; Mangan et al.
GCN 28287) at a mean frequency of 6 GHz with the Karl G. Jansky Very Large
Array (VLA; Program 19B-217) beginning 2020 August 28.47 UT (2.28 days
after the burst). We detect a radio source with a preliminary flux density
of ~40 microJy at:

RA (J2000) = 00:27:08.54
Dec (J2000) = +34:01:38.37

with an uncertainty of 0.3 arcsec in each coordinate. This position is
fully consistent with the position of the optical afterglow candidate
ZTF20abwysqy (Ahumada et al. GCN 28295) and the catalogued galaxy. The
position is also on the outskirts of the Swift/XRT afterglow position (D'Ai
et al. GCN 28300; 90% confidence). Follow-up observations are planned.

We thank the VLA staff for rapidly executing these observations.


GRB_name: GRB200826B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28303
SUBJECT: IPN triangulation of GRB 200826B
DATE:    20/08/28 19:31:31 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,

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

and

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

The long-duration GRB 200826B
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 28292;
Malacaria and Meegan, GCN Circ. 28298)
has been detected by Fermi (GBM trigger 620172587),
Konus-Wind, INTEGRAL (SPI-ACS), and Mars-Odyssey (HEND),
so far, at about 79779 s UT (22:09:39).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
    ---------------------------------------------
     RA(2000), deg                 Dec(2000), deg
    ---------------------------------------------
    Center:
     153.175 (10h 12m 42s) +57.580 (+57d 34' 48")
    Corners:
     154.647 (10h 18m 35s) +58.181 (+58d 10' 52")
     153.503 (10h 14m 01s) +58.301 (+58d 18' 03")
     151.749 (10h 07m 00s) +56.954 (+56d 57' 14")
     152.864 (10h 11m 27s) +56.858 (+56d 51' 28")
    ---------------------------------------------
The error box area is 3280 sq. arcmin, and its maximum
dimension is 2.0 deg (the minimum one is 33.4 arcmin).
The Sun distance was 47 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi RoboBA localization (GCN Circ. 28292).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200826_T79779/IPN

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


GRB_name: GRB200826B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28304
SUBJECT: Konus-Wind detection of GRB 200826B
DATE:    20/08/28 20:46:49 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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, very bright GRB 200826B
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 28292;
Malacaria & Meegan, GCN Circ. 28298;
IPN triangulation: Hurley et al., GCN Circ. 28303)
triggered Konus-Wind at T0=79779.087 s UT (22:09:39.087).

The burst light curve shows a bright, multi-peaked pulse
which started at ~T0-3 s and had a total duration of ~23 s.
A weak post-burst emission is visible in the 18-70 keV band
up to the end of the KW trigger record at ~T0+250 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/GRB200826_T79779/

As observed by Konus-Wind, the burst had
a fluence of (2.0 Â± 0.1)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0+4.922,
of (4.8 Â± 0.4)x10^-5 erg/cm^2/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)
can be described, in the 20 keV - 15 MeV range,
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.54 (-0.04,+0.04),
the high energy photon index beta = -2.38 (-0.07,+0.06),
the peak energy Ep = 337 (-14,+15) keV,
chi2 = 169/96 dof.

The spectrum near the peak count rate
(measured from T0+4.864 to T0+5.120 s)
is best fit in the 20 keV - 15 MeV range by the GRB (Band)
function with the following model parameters:
the low-energy photon index alpha = -0.18 (-0.18,+0.22),
the high energy photon index beta = -2.42 (-0.23,+0.17),
the peak energy Ep = 320 (-45,+48) keV,
chi2 = 58/48 dof.

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


GRB_name: GRB200817A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28305
SUBJECT: Zwicky Transient Facility discovery of ZTF20abtxwfx/AT2020sev, a fast optical transient and candidate afterglow
DATE:    20/08/29 02:48:17 GMT
FROM:    Igor Andreoni at Caltech  <igor.andreoni@gmail.com>

Igor Andreoni (Caltech), Anna Ho (UCB), Michael Coughlin (UMN), Mansi
Kasliwal (Caltech), Eric Burns (LSU), Dmitry Svinkin (Ioffe
Institute), Tomas Ahumada (UM), Yuhan Yao (Caltech), Daniel Perley
(LJMU), Shreya Anand (Caltech), Erik Kool (OKC), Ana Sagues Carracedo
(OKC)
on behalf of the Zwicky Transient Facility (ZTF) and Global Relay of
Observatories Watching Transients Happen (GROWTH) collaborations

We report the discovery of the fast optical transient
ZTF20abtxwfx/AT2020sev with the Zwicky Transient Facility (ZTF, Bellm
et al. 2019, Graham et al. 2019) at coordinates:

RAJ2000 = 16:41:21.21 (250.338384d)
DecJ2000 = +57:08:20.5 (+57.139027d)

ZTF20abtxwfx was found during the science validation of the new "ZTF
Realtime Search and Triggering" (ZTF-ReST) project. ZTF-ReST will aim
at near real-time identification of kilonova candidates in ZTF data
using the methods described in Andreoni et al. (2020d), independently
of gravitational-wave or gamma-ray triggers.

ZTF20abtxwfx was first detected on 2020-08-18 05:20 UT, heareafter
labelled T_det. ZTF20abtxwfx faded by ~1.3 mag in r-band in the first
2 days since T_det. The transient was last detected on 2020-08-23
04:51 UT at r = 20.98 +- 0.24 mag. Stringent upper limits constrain
the transient onset time to be within ~1 day from T_det. The color of
the transient appears to be red, with g-r~0.1 and g-i~0.3 one day
after T_det. The Galactic extinction on the line of sight is low, with
E(B-V)=0.015 mag (Planck Collaboration et al., 2015).

In the table below, we report forced photometry obtained with
ForcePhotZTF (Yao et al., 2019) on images processed in real-time
through the ZTF reduction and image subtraction pipelines at IPAC
(Masci et al. 2019).

-----------------+--------+------+------
    Date (UT)    |  mag   | emag | band
-----------------+--------+------+------
2020-08-17 06:45 | > 21.0 |      |  r
2020-08-18 05:20 | 19.22  | 0.04 |  r
2020-08-19 04:19 | 20.03  | 0.11 |  r
2020-08-19 05:23 | 20.16  | 0.09 |  g
2020-08-19 05:53 | 19.83  | 0.14 |  i
2020-08-20 04:47 | 20.54  | 0.15 |  r
2020-08-20 05:46 | 20.66  | 0.16 |  g
2020-08-21 04:25 | 20.71  | 0.17 |  r
2020-08-21 06:54 | > 20.8 |      |  g
2020-08-23 04:12 | > 21.0 |      |  g
2020-08-23 04:51 | 20.98  | 0.24 |  r
2020-08-24 04:26 | > 20.5 |      |  r
-----------------+--------+------+------


ZTF20abtxwfx is located at high Galactic latitude b_Gal = 40.0 deg.
Deep Legacy Survey, Pan-STARRS1, and CFHT images of the field do not
reveal any permanent source at the transient location. The spatially
closest source reported in the Legacy Survey DR8 catalog (RA, Dec =
250.3368d, 57.1377d) has a separation of 5.7 arcsec from ZTF20abtxwfx,
is extended (not point-like), has photometric redshift of z = 0.73 +-
0.2, and has reported magnitudes of g=23.37 mag, r=22.63 mag, and
z=21.86 mag.

We searched the GCN archives, the Fermi GBM catalog, the Fermi GBM
subthreshold catalog, and the Konus-Wind triggered and waiting mode
data for any possible gamma-ray burst (GRB) counterpart. We found one
possible counterpart, GRB 200817A (Fermi GBM Team, GCN #28254). The
trigger time of GRB 200817A was on 2020-08-17 09:25:20 UT, which lies
in the time interval between our last optical non-detection and T_det.
ZTF20abtxwfx is located in the 93rd percentile of the localization
region, at an angular distance of about 32 degrees from the central
GRB position. We confirm that the position of ZTF20abtxwfx was within
the GBM field-of-view at the time of the GRB.

Multi-wavelength follow-up of ZTF20abtxwfx is encouraged.


ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC,
USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY,
Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan;
IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia.
ZTF acknowledges the generous support of the NSF under AST MSIP Grant No
1440341. GROWTH acknowledges generous support of the NSF under PIRE
Grant No 1545949. Alert distribution service provided by DIRAC@UW
(Patterson et al. 2019). Alert database searches are done with
Kowalski (Duev et al. 2019).


GRB_name: GRB200826A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28306
SUBJECT: GRB 200826A: Kitab optical observations
DATE:    20/08/29 10:22:06 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Zhornichenko (KIAM), A. Pozanenko (IKI),  N. Pankov 
(HSE), E. Mazaeva  (IKI), A. Volnova (IKI), Sh. Ehgamberdiev (UBAI) 
report on behalf of IKI-GRB-FuN:

We observed the field of a Fermi short GRB 200826A  (Fermi GBM team, GCN 
28284; Kunzweileret al., GCN 28286; Manganal., GCN 28287) with 
Kitab-ISON RC-36  telescope in Clear filter. In particular we cover a 
whole region of IPN  localization (Hurley et al., GCN 28291). The 
optical afterglow ZTF20abwysqy/AT2020scz (Carracedo et al., GCN 28293; 
Ahumada et al., GCN 28295) is not detected. Preliminary photometry of 
the filed is following

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

2020-08-26  22:22:17 0.76626  3720   CR      n/d    n/d   20.2
2020-08-27  22:08:30 1.73515  5520   CR      n/d    n/d   20.4

The photometry is based on nearby USNO-B1.0 stars, R2 magnitudes
USNO-B1.0_id R2
1238-0009330 16.37
1239-0009591 16.56


GRB_name: GRB200829A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28307
SUBJECT: GRB 200829A: Swift detection of a burst with an optical afterglow
DATE:    20/08/29 14:18:33 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

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

At 13:59:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200829A (trigger=993768).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 251.212, +72.335 which is 
   RA(J2000) = 16h 44m 51s
   Dec(J2000) = +72d 20' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 30 sec.  The peak count rate
was ~1335 counts/sec (15-350 keV), at ~6 sec after the trigger. 

The XRT began observing the field at 14:01:43.1 UT, 128.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 251.2096, 72.3273 which is equivalent to:
   RA(J2000)  = 16h 44m 50.30s
   Dec(J2000) = +72d 19' 38.3"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 27 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 9.30e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 138 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 16:44:49.05 = 251.20439
  DEC(J2000) = +72:19:45.3  =  72.32924
with a 90%-confidence error radius of about 0.61 arc sec. This position is 9.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.28 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.04. 

Burst Advocate for this burst is M. H. Siegel (siegel 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: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28308
SUBJECT: GRB 200829A: TSHAO optical observations
DATE:    20/08/29 17:02:07 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), I. Reva (FAPHI), A. Serebryanskiy (FAPHI),  S. 
Belkin (IKI), M. Krugov (FAPHI), E. Mazaeva (IKI), A. Volnova (IKI) 
report on behalf of IKI-GRB-FuN:

We are observing the afterglow of GRB 200829A (Siegel et al.  GCN 28307) 
with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory 
starting on Aug. 29 (UT) 14:49:05.   The afterglow is clearly visible in 
single images of 60 s exposure.  Preliminary photometry of the afterglow 
is R=16.8 +/- 0.1 at mid time (UT) 15:00:41.

Observations is continuing.


GRB_name: GRB200829A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28309
SUBJECT: Swift GRB 200829A: Global MASTER-Net observations report 
DATE:    20/08/29 17:36:30 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 200829A ( M. H. Siegel et al., GCN 28307) errorbox  12423 sec after notice time and 12502 sec after trigger time at 2020-08-29 17:27:56 UT, with upper limit up to  18.5 mag. Observations started at twilight.  The observations began at zenith distance = 30 deg. The sun  altitude  is -11.7 deg. 

The galactic latitude b = 35 deg., longitude l = 104 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1429750

We obtain a following upper limits.  

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

   12592 |      MASTER-Tavrida |   C |   180 | 18.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200829A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28311
SUBJECT: GRB 200829A: Swift/UVOT Detection
DATE:    20/08/29 19:10:29 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 200829A
138 s after the BAT trigger (Siegel et al., GCN Circ. 28307).
The UV-optical source position is RA=251.204709, Dec=72.329356 deg
(J2000) which is in sexagesimal:
RA(J2000) = 16h 44m 49.14s
Dec(J2000) = 72d 19' 45.63"
with a positional uncertainty of 0.35" 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              138          288          147         14.29 +/- 0.02
white              576          596           19         15.43 +/- 0.04
white             1527         1547           19         16.38 +/- 0.06
v                  626          646           19         15.50 +/- 0.10
b                  552          572           19         15.68 +/- 0.07
u                  296          546          246         14.54 +/- 0.03
u                  700          720           19         15.12 +/- 0.07
w1                 675          696           19         15.19 +/- 0.12
m2                1080         1100           19         16.25 +/- 0.25
w2                1032         1398           39         17.64 +/- 0.30

Note that the times are since the BAT trigger time. The main burst took
place around 60s earlier during a Swift Slew.

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: GRB200826A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28312
SUBJECT: GRB 200826A: Lowell Discovery Telescope observations of ZTF20abwysqy
DATE:    20/08/29 19:16:00 GMT
FROM:    Simone Dichiara at UMCP/NASA/GSFC  <dichiara@umd.edu>

S.Dichiara (UMD, NASA-GSFC), S.B. Cenko (NASA-GSFC), E. Troja
(UMD, NASA-GSFC), P. Gatkine (UMD), J.M. Durbak (UMD), A. Kutyrev (UMD,
NASA-GSFC), S. Veilleux (UMD), report on behalf of a larger
collaboration:

We observed at the position of the optical transient ZTF20abwysqy reported
by Ahumada el al. (GCN Circ. 28287) as a possible afterglow candidate for
GRB 200826A (Fermi GBM team, GCN 28284, Mangan et al., GCN Circ. 28287)
and coincident with the X-ray Source 3 reported by D'Ai et al. (GCN Circ.
28300). We use the Large Monolithic Imager (LMI) on the 4.3m Lowell
Discovery Telescope (LDT) at Happy Jack, AZ. Observations started on
August 29, 10:04:56 UT (3.23 days after the Fermi trigger) taking 8
exposures of 180 s each with SDSS r filter. Observations were taken at an
airmass of about 1 and seeing of 1.4".

We detect the underlying galaxy reported by Ahumada el al. (GCN Circ.
28287) with magnitude r=22.60 +/- 0.03 AB mag. We do not find any other
source at the reported position down to a 3-sigma field limit of r>24.5
AB mag.

Magnitudes are calibrated against the SDSS catalog and not corrected for
Galactic extinction.

We thank the staff of the Lowell Discovery Telescope for assistance with
these observations.


GRB_name: GRB200829A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28313
SUBJECT: GRB 200829A: Enhanced Swift-XRT position
DATE:    20/08/29 19:22:47 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 1810 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 200829A, 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 = 251.20605, +72.32921 which is equivalent
to:

RA (J2000): 16h 44m 49.45s
Dec (J2000): +72d 19' 45.2"

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

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB200829A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28314
SUBJECT: GRB 200829A: AGILE/MCAL detection
DATE:    20/08/29 19:23:40 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE Mini-CALorimeter (MCAL) detected GRB 200829A at T0 = 2020-08-29
13:58:30.90 +/- 0.01 s (UTC), reported by Swift-BAT (Siegel et al., GCN
#28307) and Swift-UVOT (Kuin et al., GCN #28311).

The event lasted about 5.6 s and it released a total number of ~15550
counts in the detector (in the 0.4-100 MeV energy range), above an average
background rate of 570 Hz.

The time-integrated spectrum of the burst can be fitted in the energy range
0.4-20 MeV with a single power-law with ph.ind. = 2.26 -0.03/+0.03,
resulting in a reduced chi-squared of 1.67 (62 d.o.f.) and a fluence of
6.2e-05 ergs/cm^2 (90% confidence level), in the same energy range.

The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB_069336_525794310.907011.png .

The event is also clearly visible in the scientific ratemeters (RMs) of the
SuperAGILE (18-60 keV), MCAL (0.4-100 MeV), and Anti-Coincidence (50-200
keV) detectors. Their light curves can be found at
http://www.agilescienceapp.it/notices/GRB200829A_AGILE_RMs.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.
Automatic MCAL GRB alert Notices can be found at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.


GRB_name: GRB200829A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28315
SUBJECT: GRB 200829A: Global MASTER-Net OT detection
DATE:    20/08/29 19:50:58 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, N.Tyurina, E. Gorbovskoy, V.Kornilov, 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),

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-Tavrida robotic telescope  (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical 
station) was pointed to the Swift GRB 200829A ( M. H. Siegel et al., GCN 
28307) errorbox  12423 sec after notice time and 12502 sec after trigger 
time at 2020-08-29 17:27:56 UT, with upper limit up to  18.5 mag.

We see OT at Swift/UVOT  position (Kuin et al GCN 28311).

Datetime:  2020-08-29 17:36:40
Coord:     16h 44m 48.88s , +72d 19m 45s.8
Mag:       18.1

Observations started at twilight.
The observations began at zenith 
distance = 30 deg. The sun  altitude  is -11.7 deg.


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28316
SUBJECT: GRB200829A: optical afterglow detection
DATE:    20/08/29 21:05:19 GMT
FROM:    Jozsef Vinko at Konkoly Observatory  <vinko@konkoly.hu>

GRB200829A: optical afterglow detection from Konkoly Observatory 

J. Vinko, K. Vida, A. Pal, L. Kriskovics, R. Szakats, A. Ordasi and K. Sarneczky
(Konkoly Observatory, Hungary) report:

The optical afterglow of GRB 200829A (Siegel et al. GCN 28307) is detected with the 
0.8m RC80 robotic telescope at Piszkesteto Station of Konkoly Observatory starting on 
Aug 29 19:22:00 UT, 19346 s after the Swift/BAT trigger. The afterglow 
is measured on stacked Sloan r'- and i'-band frames of 3x300 s exposure. 

Photometry, tied to nearby comparison stars with PS1 magnitudes, gives. 
r' = 18.45 +/- 0.09 and i' = 18.49 +/- 0.11 mag, in accord with previous optical 
detections (Pozanenko et al. GCN 28308; Kuin et al. GCN 28311; Ursi et al. GCN 28314; 
Lipunov et al. GCN 28315)..


GRB_name: GRB200829A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28317
SUBJECT: GRB 200829A: Swift-XRT refined Analysis
DATE:    20/08/30 02:47:18 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J. D. Gropp (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), T. Sbarrato
(INAF-OAB), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), A.
Tohuvavohu (U. Toronto) and M.H. Siegel report on behalf of the
Swift-XRT team:

We have analysed 6.8 ks of XRT data for GRB 200829A (Siegel et al. GCN
Circ. 28307), from 135 s to 24.2 ks after the  BAT trigger. The data
comprise 1.7 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. 28313).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=0.62 (+0.09, -0.10). At T+279 s  the decay
steepens to an alpha of 8.0 (+0.0, -6.9). The light curve breaks again
at T+283 s to a decay with alpha=0.885 (+0.016, -0.017),  before a
final break at T+1174 s s after which the decay index is 1.19
(+/-0.04).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.700 (+/-0.014). The
best-fitting absorption column is  9.9 (+/-0.4) x 10^20 cm^-2, in
excess of the Galactic value of 4.7 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.89 (+/-0.09) and a
best-fitting absorption column of 1.36 (+0.28, -0.26) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.7 x 10^-11 (4.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.36 (+0.28, -0.26) x 10^21 cm^-2
Galactic foreground: 4.7 x 10^20 cm^-2
Excess significance: 5.6 sigma
Photon index:      1.89 (+/-0.09)

If the light curve continues to decay with a power-law decay index of
1.19, the count rate at T+24 hours will be 0.23 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.4 x
10^-12 (1.0 x 10^-11) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00993768.

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


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28318
SUBJECT: GRB 200829A: THO optical observatios
DATE:    20/08/30 06:36:53 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen and Markku Nissinen (Taurus Hill

Observatory, Varkaus, Finland) report:

 

We have detected GRB 200829A optical afterglow at Taurus 

Hill Observatory (A95) using C-14SC 0.35-m f/7.3 telescope,

SBIG STT-8300M CCD and RGB filters. The observations were 

started at 2020-08-29 18:48:29 (UT). 

 

The afterglow was detected at the position RA 16 44 49.16 

and DEC +72 19 45.9.

 

The following magnitudes were obtained from the observations 

using NOMAD1 1623-0124683 (R=17.05, V=17.32, B=17.55)

as a comparison star:

 

Tmid(h:min:sec)+T0   Filter      Exp.time(sec) Mag        MagErr


4:53:37            R          3x180        17.98          0.28


5:02:49            R          3x180        18.11          0.34

5:12:36            R          3x180        18.22          0.27

5:25:05            R          5x180        18.26          0.17

6:00:06            R          5x180        18.27          0.14

6:25:44            B          3x180        18.66          0.21

6:35:32            G         3x180        18.69          0.26

 

URL link for the RGB image:

www.kassiopeia.net/wp-content/uploads/2020/08/GRB200829A_RGB_web.png


GRB_name: GRB200826A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28319
SUBJECT: GRB 200826A
DATE:    20/08/30 07:28:22 GMT
FROM:    Barry Rothberg at Large Binocular Telescope Obs  <brothberg@lbto.org>

B. Rothberg (LBTO/George Mason University), O. Kuhn (LBTO), C. Veillet
(LBTO), S. Allanson (LBTO).

We observed the optical afterglow of GRB 200826A  (Gupta et al. GCN Circ.
28288, Hurley et al., GCN Circ. 28291) using the Large Binocular Telescope
Observatory equipped with the Multi-Object Double Spectrographs (MODS).
Our spectra cover the wavelength range 0.38-1.0 microns. The observations
consist of 4 exposures of 900 seconds each in three of the four available
channels (MODS-1 Red, MODS-2 Blue, and MODS-2 Red).  The observation mid
time was 09:39 UT 28 Aug 2020.

In two 60 second acquisition images taken simultaneously wiith the g-sloan
and r-sloan filters we measure a magnitude of g=22.96 +/- 0.07 and r=22.15
+/- 0.07 (both ABmags). The photometry was calibrated against the DR12
catalog magnitudes of nearby stars (Alam et al. 2015, ApJS 219,12A). The
acquisition images were taken at 08:52:34 and 08:54:35 UT 28 Aug 2020.

The spectroscopic observations were taken at a Position Angle = 17 degrees
in order to cover both GRB 200826A and a possible nearby galaxy 15" NE. The
observations used a 1" wide slit and the spectra were extracted for both
sources using a 1" wide aperture. We clearly detect a continuum from
0.38-0.9 microns. From the detection of multiple emission features, which
we interpret as [OII], [NeIII], H-gamma, H-beta, [OIII]/4959, [OIII]/5007,
we calculate a redshift of 0.7481 +/-0.0003.

The nearby galaxy, 15" NE, is determined to be unrelated to GRB 200826A.
From the detection of multiple emission features which we interpret as
[OII]/5007, [NII]/6548, H-alpha, [NII]/6583, [SII]/6716, and [SII]/6730, we
infer a redshift of 0.1730 +/- 0.0003.

Additional spectroscopic observations are planned.

We acknowledge and heartily thank the rest of the LBTO staff for excellent
support in readying the telescope for nighttime on-sky activities during
these chaotic times.
B. Rothberg also acknowledges the assistance of R.T. Gatto.


GRB_name: GRB200830A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28320
SUBJECT: GRB 200830A: Fermi GBM Final Real-time Localization
DATE:    20/08/30 10:04:40 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 09:54:18 UT on 30 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200830A (trigger 620474063.489866 / 200830413).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 344.8, Dec = 56.5 (J2000 degrees, equivalent to J2000 22h 59m, 56d 30'), with a statistical uncertainty of 7.2 degrees.

The angle from the Fermi LAT boresight is 56.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200830413/quicklook/glg_skymap_all_bn200830413.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/bn200830413/quicklook/glg_healpix_all_bn200830413.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200830413/quicklook/glg_lc_medres34_bn200830413.gif


GRB_name: GRB200830A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28321
SUBJECT: GRB 200830A: BALROG localization (Fermi Trigger 620474063 / GRB 200830413)
DATE:    20/08/30 10:20:03 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
620474063 at 09:54:18 on 30 Aug. 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) = 351.6+/-10.1 deg
Decl.(2000.0) = 44.2+/-3.1 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200830413/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200830413/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200830413/json

                        


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28322
SUBJECT: GRB 200829A: SAO RAS optical observations
DATE:    20/08/30 13:45:46 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. S. Moskvitin,  V. N. Aitov (SAO RAS)
on behalf of GRB follow-up team report.

We observed the field of the GRB 200829A (Siegel et al., GCN 28307)
with Zeiss-1000 (1-m telescope of SAO RAS) equipped with
Multi-Mode Photometer-Polarimeter (MMPP). We obtained 4 x 300 sec.
frames in Rc band and similar sequence in Ic band.

The OT (Siegel et al., GCN 28307; Pozanenko et al., GCN 28308;
Kuin and Siegel, GCN 28311; Lipunov et al., GCN 28315; Vinko et al.,
28316; Hentunen and Nissinen,  GCN 28318) is clearly detected
with the brightness R = 17.84 +/- 0.09 (T_mid - T0 = 4.587 h),
I = 17.65 +/- 0.09 (T_mid - T0 = 4.204 h).
Preliminary photometry is based on R2 and I magnitudes
of nearby USNO-B1 stars.


GRB_name: GRB200829A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28323
SUBJECT: Konus-Wind detection of GRB 200829A (a clone of GRB 200826B?)
DATE:    20/08/30 14:52:11 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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, very bright GRB 200829A
(Swift detection: Siegel et al., GCN 28307;
Goad et al., GCN 28313; Gropp et al., GCN 28317;
AGILE/MCAL detection: Ursi et al., GCN 28314)
triggered Konus-Wind at T0=50309.99 s UT (13:58:29.990).

The burst light curve shows a bright, multi-peaked pulse
which started at ~T0-24 s and had a total duration of ~39 s.
A weak post-burst emission is visible in the 18-70 keV band
up to the end of the KW trigger record at ~T0+250 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/GRB200829_T50309/

As observed by Konus-Wind, the burst
had a fluence of 3.02(-0.07,+0.07)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+3.456 s,
of 1.08(-0.07,+0.07)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+16.384 s)
can be described, in the 20 keV - 15 MeV range,
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.49(-0.03,+0.03),
the high energy photon index beta = -2.34(-0.05,+0.04),
the peak energy Ep = 336(-11,+11) keV
(chi2 = 163/98 dof).

The spectrum near the maximum count rate
(measured from T0+3.072 to T0+3.840 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.23(-0.07,+0.08),
the high energy photon index beta = -2.17(-0.06,+0.06),
the peak energy Ep = 372(-26,+27) keV
(chi2 = 78/71 dof).

We note, that this burst is very similar to GRB 200826B,
which, as detected by KW (Ridnaia et al., GCN 28304),
had the time-integrated spectrum with alpha = -0.54, beta = -2.38,
Ep = 337 keV; a factor of ~1.5 smaller energy fluence (~2.0x10^-4 erg/cm^2),
and a factor of ~2 smaller peak energy flux ~5x10^-5 erg/cm^2/s.
Interestingly, light curves of both bursts are also very similar
if we scale the time axis by a factor of ~1.5
(http://www.ioffe.ru/LEA/GRBs/GRB200829_T50309/gWind64_29A_26B.pdf).
Given the angular distance between the directions
to GRB 200829A (Swift-XRT GCN 28307) and GRB 200826B (IPN GCN 28303)
of ~38.6 arcdeg, and the ~3 day difference in the burst arrival times,
an idea of a lensed GRB cannot be excluded.

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


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28324
SUBJECT: GRB 200829A: Nanshan/NEXT optical observations
DATE:    20/08/30 15:27:43 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu, S.Y Fu, X. Liu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High 
School), X. Zhang,  J.Z. Liu (XAO) report:

We observed the field of GRB 200829A (Siegel et al., GCN 28307) using 
the NEXT-0.6m
telescope located at Nanshan, Xinjiang, China. We obtained a series of 
frames in the Sloan g-/r-/i- bands, starting at 19:55:23 UT on 
2020-08-29, i.e., 5.93 hr after the BAT trigger.

The GRB optical afterglow (e.g., Pozanenko et al., GCN 28308; Kuin et 
al., GCN 28311; Ursi et al., GCN 28314; Lipunov et al., GCN 28315; Vinko 
et al., GCN 28316; Hentunen & Nissinen, GCN 28318; Moskvitin et al., GCN 
28322) is clearly detected in our images.

Preliminary photometric measurements are as follows:
Filter       T-mid(hr)  Mag    Mag_err
SDSS-g 6.72     18.89 0.04
SDSS-r 5.98     18.77 0.04
SDSS-i 6.40     18.50 0.05

calibrated with nearby Pan-STARRS stars.


GRB_name: GRB200829A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28325
SUBJECT: GRB 200829A: Swift-BAT refined analysis
DATE:    20/08/30 17:01:36 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. H. Siegel (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 200829A (trigger #993768)
(Siegel, et al., GCN Circ. 28307).  The BAT ground-calculated position is
RA, Dec = 251.136, 72.363 deg which is
   RA(J2000)  =  16h 44m 32.7s
   Dec(J2000) = +72d 21' 45.6"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.


The mask weighted light curve shows a peak at ~ T-60 s followed by an extended emission.
The duration of the initial bright peak is ~15 sec. We note that Swift was slewing from T-150 s to T s.
The overall structure starts at ~T-75 s and lasts till ~T+200 s.
T90 (15-350 keV) is 13.04 +- 2.91 sec (estimated error including systematics).

The time-averaged spectrum from T-74 to T+204 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.83 +- 0.03.  The fluence in the 15-150 keV band is 5.1 +- 0.1 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T-60.07 sec in the 15-150 keV band
is 98.7 +- 1.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/993768/BA/


GRB_name: GRB200829A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28326
SUBJECT: GRB 200829A: Fermi GBM detection
DATE:    20/08/30 17:12:33 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

S. Lesage (UAH) and C. Meegan (UAH)

report on behalf of the Fermi GBM Team:


"At 13:58:14.66 UT on 29 August 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)

triggered and located GRB 200829A (trigger 620402299 / 200829582)

which was also detected by the Swift Burst Alert Telescope (BAT)

(M. H. Siegel et al. 2020, GCN 28307). GBM initially triggered on a weak

spike ~15-20 s before the very bright emission. The GBM on-ground location

is consistent with the Swift BAT position.


The angle from the Fermi LAT boresight at the GBM trigger time is ~148
degrees.


The GBM light curve shows an exceptionally bright long GRB

with a duration (T90) of about 6.9 s (50-300 keV).

The time-averaged spectrum from T0+16.64 s to T0+25.856 s is

best fit by a Band function with Epeak = 336.8 +/- 4.3  keV,

alpha = -0.43 +/- 0.01, and beta = -2.4 +/- 0.02

The event fluence (10-1000 keV) in this time interval is

(2.069 +/- 0.009)E-04 erg/cm^2.

The 1.024-sec peak photon flux measured starting from T0+19.7 s in

the 10-1000 keV band is 213.9 +/- 1.7 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: GRB200830A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28327
SUBJECT: Fermi GRB 200830A: Global MASTER-Net observations report 
DATE:    20/08/30 18:00:25 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200830A ( Fermi GBM team, GCN 28320) errorbox  26966 sec after notice time and 26992 sec after trigger time at 2020-08-30 17:24:11 UT, with upper limit up to  17.8 mag. Observations started at twilight.  The observations began at zenith distance = 40 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = -3 deg., longitude l = 108 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1430319

We obtain a following upper limits.  

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

   27023 | 2020-08-30 17:24:11 |      MASTER-Tavrida | (22h 18m 55.98s , +49d 54m 04.7s) |   C |    60 | 17.0 |        
   27103 | 2020-08-30 17:25:31 |      MASTER-Tavrida | (22h 26m 08.03s , +51d 53m 06.1s) |   C |    60 | 16.9 |        
   27184 | 2020-08-30 17:26:52 |      MASTER-Tavrida | (22h 43m 43.82s , +49d 53m 04.9s) |   C |    60 | 17.2 |        
   27345 | 2020-08-30 17:29:33 |      MASTER-Tavrida | (22h 18m 49.49s , +49d 55m 01.4s) |   C |    60 | 17.3 |        
   27425 | 2020-08-30 17:30:53 |      MASTER-Tavrida | (22h 31m 20.87s , +49d 53m 49.1s) |   C |    60 | 17.3 |        
   27506 | 2020-08-30 17:32:14 |      MASTER-Tavrida | (22h 26m 02.03s , +51d 52m 56.0s) |   C |    60 | 17.2 |        
   27586 | 2020-08-30 17:33:34 |      MASTER-Tavrida | (22h 39m 05.41s , +51d 52m 58.3s) |   C |    60 | 17.3 |        
   27667 | 2020-08-30 17:34:55 |      MASTER-Tavrida | (22h 43m 43.82s , +49d 54m 30.6s) |   C |    60 | 17.5 |        
   27748 | 2020-08-30 17:36:16 |      MASTER-Tavrida | (22h 56m 09.16s , +49d 52m 33.7s) |   C |    60 | 17.8 |        
   27828 | 2020-08-30 17:37:36 |      MASTER-Tavrida | (22h 37m 46.61s , +47d 54m 37.7s) |   C |    60 | 17.4 |        
   27908 | 2020-08-30 17:38:56 |      MASTER-Tavrida | (22h 49m 34.87s , +47d 53m 33.4s) |   C |    60 | 17.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28328
SUBJECT: GRB 200829A: further SAO RAS optical observations
DATE:    20/08/30 20:17:46 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. S. Moskvitin,  V. N. Aitov (SAO RAS)
on behalf of GRB follow-up team report.

We observed the field of the GRB 200829A (Siegel et al., GCN 28307)
with Zeiss-1000 (1-m telescope of SAO RAS) equipped with
Multi-Mode Photometer-Polarimeter (MMPP) on August 30. We obtained
5 x 300 sec. frames in Rc band and similar sequence in Ic band.

The OT (Siegel et al., GCN 28307; Pozanenko et al., GCN 28308;
Kuin and Siegel, GCN 28311; Lipunov et al., GCN 28315; Vinko et al.,
28316; Hentunen and Nissinen,  GCN 28318; Zhu et al., GCN 28324)
is clearly detected in individual images as well as stacked frames
with the brightness of R =  20.37 +/- 0.13 (T_mid - T0 = 1.1492 days),
I = 20.14 +/- 0.10 (T_mid - T0 = 1.1662 days).
Preliminary photometry is based on R2 and I magnitudes
of the same nearby USNO-B1 stars (Moskvitin and Aitov, GCN 28322).


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28329
SUBJECT: GRB 200829A: Kitab optical upper limit
DATE:    20/08/30 21:20:06 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (HSE), A. Novichonok (Petrozavodsk State University, KIAM), A. 
Zhornichenko (KIAM), A. Pozanenko (IKI), S. Belkin (IKI), E. Mazaeva 
(IKI), A. Volnova (IKI), Sh. Ehgamberdiev (UBAI) report on behalf of 
IKI-GRB-FuN:

We observed the field of a GRB 200829A (Siegel et al., GCN 28307; see 
also Ursi  et al., GCN  28314; Ridnaia et al., GCN  28323; Lesage et 
al., GCN 28326) with Kitab-ISON RC-36  telescope in R-filter. We do not 
detect optical afterglow  (Siegel et al., GCN 28307; Pozanenko et al., 
GCN 28308; Kuin and Siegel, GCN 28311; Lipunov et al., GCN 28315; Vinko 
et al., 28316; Hentunen et al.,  GCN 28318; Zhu et al., GCN 28324; 
Moskvitin et al., GCNs 28322, 28328).  Preliminary photometry of the 
filed is following

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

2020-08-30  15:57:25 1.08184  3600   R       n/d    n/d   18.8


The photometry is based on nearby USNO-B1.0 star, R2 magnitude

USNO_B10_id      R2
1626-0124132     14.76


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28330
SUBJECT: GRB 200829A: Continued Nanshan/NEXT optical observations
DATE:    20/08/31 07:52:40 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu, S.Y Fu, X. Liu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High 
School), X. Zhang,  J.Z. Liu (XAO) report:

We continued to observe the optical afterglow (e.g., Siegel et al., GCN 
28307; Pozanenko et al., GCN 28308; Kuin and Siegel, GCN 28311; Lipunov 
et al., GCN 28315; Vinko et al., 28316; Hentunen et al., GCN 28318; Zhu 
et al., GCN 28324; Moskvitin et al., GCNs 28322, 28328; Pankov et al., 
GCN 28329) of GRB 200829A (Siegel et al., GCN 28307; Ursi et al., GCN 
28314; Ridnaia et al., GCN  28323; Lesage et al., GCN 28326), using the 
NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We obtained 28 
frames in the Sloan r band, starting at 15:24:17 UT on 2020-08-30, i.e., 
about 1.058 d after the BAT trigger.

Preliminary photometric measurements are as follows:
Filter         T_exp/s T_mid/d Mag      Mag_err
SDSS-r 8x120 1.062       >20.6
SDSS-r 20x120 1.307       21.20        0.16

calibrated with nearby Pan-STARRS stars.


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28331
SUBJECT: GRB 200829A: Liverpool Telescope observations
DATE:    20/08/31 11:52:24 GMT
FROM:    Luca Izzo at DARK/NBI  <luca.izzo@gmail.com>

L. Izzo (DARK/NBI) reports:

We observed the field of GRB 200829A (Siegel et al., GCN #28307; Ursi et al., GCN #28314; Ridnaia et al., GCN #28323; Lesage & Meegan, GCN #28326) with the IO:O camera mounted on the 2-m Liverpool Telescope located in La Palma, Spain. Observations started on August 29 at 20:31:39 UT (0.272 days after the GRB trigger) and a second epoch was obtained on August 30 at 22:38:42 UT (1.362 days). In both epochs, we obtained a series of 5x60s images in the griz filters.
The optical afterglow (Siegel et al., GCN #28307, Pozanenko et al., GCN #28308; Kuin & Siegel, GCN #28311; Lipunov et al., GCN #28315; Vinko et al., GCN #28316; Hentunen et al., GCN #28318; Moskvitin et al., GCN #28322, GCN #28328, Zhu et al., GCN #28324, GCN #28330; Pankov et al., GCN #28329) is visible in the stacked images in both epochs. We measure the following preliminary AB magnitudes, calibrated against Pan-STARRS catalog stars:

Filter      mag     err     MJD

SDSS-g  18.91  0.05  (59090.855)
SDSS-g  21.17  0.09  (59091.944)
SDSS-r  18.76  0.04  (59090.860)
SDSS-r  21.34  0.10  (59091.948)
SDSS-i  18.65  0.04  (59090.865)
SDSS-i  21.25  0.09  (59091.953)
SDSS-z  18.57  0.04  (59090.870)
SDSS-z  20.50  0.08  (59091.958)


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28333
SUBJECT: GRB 200829A: Koshka Zeiss-1000 optical observations
DATE:    20/08/31 19:52:13 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), S. Naroenkov (INASAN),  A. Pozanenko (IKI), N. Pankov 
(HSE), S. Belkin (IKI), E. Mazaeva (IKI)  report on behalf of larger GRB 
IKI FuN collaboration:

We observed the the field of GRB 200829A (Siegel et al., GCN 28307; Ursi 
et al., GCN 28314; Ridnaia et al., GCN 28323; Lesage & Meegan, GCN 
28326)  with Zeiss-1000 1-m telescope of Koshka Observatory on August, 
30  starting (UT) 19:18:21 in I- and R-filters. The optical afterglow 
(Siegel et al., GCN 28307, Pozanenko et al., GCN 28308; Kuin & Siegel, 
GCN 28311; Lipunov et al., GCN 28315; Vinko et al., GCN 28316; Hentunen 
et al., GCN 28318; Moskvitin et al., GCNs 28322, 28328, Zhu et al., GCN 
28324, GCN 28330; Pankov et al., GCN 28329; Izzo, GCN 28331)  is 
detected  in stacked images of both filters. Preliminary photometry of 
the afterglow is following.

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

2020-08-30 19:18:21   1.29067    I     47*120  20.14  0.20  20.8
2020-08-30 19:20:31   1.29217    R     47*120  21.0   0.25  21.4


The photometry is based on nearby USNO-B1.0 stars.


GRB_name: GRB200901A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28335
SUBJECT: GRB 200901A: Swift detection of a burst
DATE:    20/09/01 03:56:30 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. K. Simpson (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL), B. Sbarufatti (PSU) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 03:47:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200901A (trigger=994143).  Swift did not slew immediately
due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 61.758, -59.880 which is 
   RA(J2000) = 04h 07m 02s
   Dec(J2000) = -59d 52' 47"
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 ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+47.5
minutes. There will be no XRT or UVOT data until this time. 

This source lies within the current (Sector 29) field-of-view of TESS camera 3. 

Burst Advocate for this burst is K. K. Simpson (kira.simpson1984 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: GRB200901A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28336
SUBJECT: GRB 200901A: Swift-XRT observations
DATE:    20/09/01 05:22:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 200901A at 04:38:21.9 UT,
3050.4 seconds after the BAT trigger. No source was detected in 1.9 ks
of promptly downlinked data, which covered 54% of the BAT error circle.
We are waiting for the full dataset to detect and localise the XRT
counterpart.


GRB_name: GRB200901B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28337
SUBJECT: GRB 200901B: Swift detection of a burst
DATE:    20/09/01 07:25:54 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

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

At 07:09:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200901B (trigger=994165).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 217.879, -38.716 which is 
   RA(J2000) = 14h 31m 31s
   Dec(J2000) = -38d 42' 58"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual with an image trigger, 
the available BAT light curve shows no significant structure. 

The XRT began observing the field at 07:12:16.1 UT, 169.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 217.8572, -38.7117 which is equivalent to:
   RA(J2000)  = 14h 31m 25.73s
   Dec(J2000) = -38d 42' 42.1"
with an uncertainty of 5.5 arcseconds (radius, 90% containment). This
location is 63 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 1.11e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
175 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
0.09. 

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: GRB200829A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28338
SUBJECT: GRB 200829A: Swift/UVOT-XRT photometric redshift
DATE:    20/09/01 11:55:48 GMT
FROM:    Samantha Oates at MSSL  <samantha.oates@alumni.ucl.ac.uk>

S. R. Oates (U.Birmingham), N.P.M. Kuin (MSSL-UCL),
M. De Pasquale (Istanbul U.), S. Campana (INAF-OAB),
A. Tohuvavohu (U Toronto) and M. H. Siegel (PSU)
report on behalf of the Neil Gehrels Swift
Observatory Team:

We have performed a joint spectral analysis of Swift UVOT and XRT
observations of GRB 200829A (Siegel et al., GCN Circ. 28307; Kuin et al.
GCN Circ. 28311, Goad et al., GCN Circ. 28313), based on the methodology
of Schady et al. (2010, MNRAS, 401, 2773). Using this method, we created
an SED at 900s after the BAT trigger consisting of 6 UVOT filters and
WT mode XRT data. The model with the best fit, broken power-law with a
Milky Way extinction curve for the host extinction, gives a photometric
redshift for GRB 200829A of 1.25 +\- 0.02 (1 sigma uncertainty;
chi^2/dof = 586/538).

This circular is an official product of the Swift team.


GRB_name: GRB200901B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28339
SUBJECT: GRB 200901B: Enhanced Swift-XRT position
DATE:    20/09/01 14:48:11 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 903 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200901B, 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 = 217.85911, -38.71147 which is equivalent
to:

RA (J2000): 14h 31m 26.19s
Dec (J2000): -38d 42' 41.3"

with an uncertainty of 4.2 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB200901A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28340
SUBJECT: GRB 200901A: Fermi GBM observation
DATE:    20/09/01 18:08:49 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

"At 03:47:27.62 UT on 1 September 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered on GRB 200901A (trigger 620624852 / 200901158)
which was also detected by the Swift/BAT (Simpson et al., GCN 28335).
The GBM on-ground location is consistent with the Swift position.

The event was classified as particle activity by the flight software, but
it is in fact a GRB.

The angle from the Fermi LAT boresight at the GBM trigger time is 151
degrees.

The GBM light curve consists of overlapping pulses
with a duration (T90) of about 10.2 s (50-300 keV).
The time-averaged spectrum from T0-0.9 s to T0+10.4 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.52 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 410 +/- 150 keV.

The event fluence (10-1000 keV) in this time interval is
(9.4 +/- 0.54)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.8 s in the 10-1000 keV band
is 11.2 +/- 0.96 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: GRB200901A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28341
SUBJECT: GRB 200901A: Swift-XRT refined Analysis
DATE:    20/09/01 18:09:03 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

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

We have analysed 2.5 ks of XRT data for GRB 200901A (Simpson et al. GCN
Circ. 28335), from 3.1 ks to 11.1 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. Using 1707 s of PC mode data
and 4 UVOT images, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 61.78319, -59.89084 which is equivalent to:

RA (J2000): 04h 07m 07.97s
Dec(J2000): -59d 53' 27.0"

with an uncertainty of 1.8 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.95 (+0.28, -0.24).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.31 (+0.30, -0.28). The
best-fitting absorption column is  2.2 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 1.5 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.0 x 10^-11 (4.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.2 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 1.5 x 10^20 cm^-2
Excess significance: 4.2 sigma
Photon index:      2.31 (+0.30, -0.28)

If the light curve continues to decay with a power-law decay index of
0.95, the count rate at T+24 hours will be 7.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.3 x
10^-13 (3.8 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/00994143.

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


GRB_name: GRB200901A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28342
SUBJECT: GRB 200901A: Swift/UVOT Detection
DATE:    20/09/01 20:16:07 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and K. K. Simpson (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200901A 3053 s after the BAT trigger 
(Simpson et al., GCN Circ. 28335).
A possible optical afterglow consistent with the XRT position (Kennea et al., GCN Circ. 28341) is 
detected in the initial UVOT exposures in the white filter only. It is not clear whether the source 
is fading.
Preliminary detections and 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          3053         3202          147         20.6 +/- 0.3
white             3916         4115          197         20.5 +/- 0.2
v                 4326         4526          197         >19.1
b                 3711         3910          197         >20.4
u                 3211         4987          290         >20.0
w1                4736         4936          197         >19.1
m2                4531         4731          197         >19.1
w2                4121         4321          197         >19.3

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


GRB_name: GRB200901B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28343
SUBJECT: GRB 200901B: Swift/UVOT Detection
DATE:    20/09/01 20:17:40 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (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 200901B 176 s after the BAT trigger 
(Sbarufatti et al., GCN Circ. 28337).
A source consistent with the XRT position (Sbarufatti et al. GCN Circ. 28337)is detected in the 
initial UVOT exposures in the u filter only, but many exposures are smeared, so the magnitudes may 
not be reliable.

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

v                  482          801           58        >18.1
b                  431          750           58        >19.1
u                  176          426          245         19.3 Â± 0.3
w1                 531          851           58        >18.1
m2                 506          826           58        >17.9
w2                 457          776           58        >18.2

The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of 
E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB200901A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28344
SUBJECT: GRB 200901A: Swift-BAT refined analysis
DATE:    20/09/01 23:39:29 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@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),
K. K. Simpson (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 200901A (trigger #994143)
(Simpson et al., GCN Circ. 28335).  The BAT ground-calculated position is
RA, Dec = 61.759, -59.901 deg which is
   RA(J2000)  =  04h 07m 02.3s
   Dec(J2000) = -59d 54' 03.4"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 21%.

The mask-weighted light curve shows several overlapping pulses that start
at ~T-5 s and end at ~T+27 s. The main peak occurs at ~T0.
The burst location went out of the BAT field of view at ~T+514 s.
T90 (15-350 keV) is 20.37 +- 7.55 sec (estimated error including
systematics).

The time-averaged spectrum from T-4.43 to T+26.59 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.72 +- 0.11.  The fluence in the 15-150 keV band is 2.9 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T-0.01 sec in the 15-150 keV band
is 7.7 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/994143/BA/


GRB_name: GRB200901B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28345
SUBJECT: GRB 200901B: Swift-BAT refined analysis
DATE:    20/09/01 23:41:52 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), D. M. Palmer (LANL),
T. Sakamoto (AGU), B. Sbarufatti (PSU),
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 200901B (trigger #994165)
(Sbarufatti et al., GCN Circ. 28337).  The BAT ground-calculated position is
RA, Dec = 217.860, -38.704 deg which is
   RA(J2000)  =  14h 31m 26.5s
   Dec(J2000) = -38d 42' 15.2"
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 82%.

The mask-weighted light curve shows some weak emission that
starts at ~T0 and ends at ~T+900 s. The available event data end
at T+963 s, and the burst went out of the BAT FOV soon afterwards
(~T+1000 s). T90 (15-350 keV) is 705.94 +- 148.71 sec (estimated error
including systematics).

The time-averaged spectrum from T+32.14 to T+901.32 sec is best fit by a
power law
with an exponential cutoff.  This fit gives a photon index 0.95 +- 0.63,
and Epeak of 46.7 +- 8.6 keV (chi squared 61.80 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 4.3 +- 0.4 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+68.62 sec in the 15-150 keV band is
0.4 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.95 +- 0.13 (chi squared 71.14 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/994165/BA/


GRB_name: GRB200901B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28347
SUBJECT: GRB 200901B: Swift-XRT refined Analysis
DATE:    20/09/02 07:26:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 4.6 ks of XRT data for GRB 200901B (Sbarufatti et al.
GCN Circ. 28337), from 11.3 ks to 35.0 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Osborne et al. (GCN Circ. 28339).

The light curve can be modelled with a series of power-law decays. The
light curve initially rises, with an index alpha=-0.6 (+0.7, -0.9). At
T+239 s it breaks to an alpha of 0.54 (+0.08, -0.07) before breaking
again at T+950 s to a final decay with index alpha=2.61 (+1.29, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.15 (+/-0.05). The
best-fitting absorption column is  1.66 (+0.27, -0.26) x 10^21 cm^-2,
in excess of the Galactic value of 1.2 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 5.8 x 10^-11 (6.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      1.66 (+0.27, -0.26) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 2.9 sigma
Photon index:      1.15 (+/-0.05)

If the light curve continues to decay with a power-law decay index of
2.61, the count rate at T+24 hours will be 8.7 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.1 x
10^-15 (5.5 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00994165.

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


GRB_name: GRB200901A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28348
SUBJECT: GRB 200901A: MASTER OT early detection
DATE:    20/09/02 12:59:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

MASTER-OAFA robotic telescope (Global MASTER-Net http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, v.2010, 30L)
started in alert mode (Lipunov et al. GCN 28334)
Swift GRB 200901A  (Simpson et al. GCN 28335,  Sakamoto et al. GCN 28344) 
errorbox observation 25s after notice time (46s after trigger time) at 2020-09-01 03:48:18 UT.

There is OT at XRT (Kennea et al. GNC 28341) and UVOT (Breeveld et al. GCN 28342) position
first 20 minutes after trigger time.

Data analysis will continue.


GRB_name: GRB200903A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28349
SUBJECT: GRB 200903A: Fermi GBM Final Real-time Localization
DATE:    20/09/03 00:55:04 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 00:44:19 UT on 3 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200903A (trigger 620786664.250206 / 200903031).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 159.0, Dec = 54.9 (J2000 degrees, equivalent to J2000 10h 35m, 54d 53'), with a statistical uncertainty of 3.6 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/2020/bn200903031/quicklook/glg_skymap_all_bn200903031.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/bn200903031/quicklook/glg_healpix_all_bn200903031.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200903031/quicklook/glg_lc_medres34_bn200903031.gif


GRB_name: GRB200903A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28350
SUBJECT: GRB 200903A: Swift detection of a burst
DATE:    20/09/03 01:06:11 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), J.D. Gropp (PSU),
A. Y. Lien (GSFC/UMBC), M. J. Moss (GWU), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 00:44:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200903A (trigger=994389).  Swift did not slew immediately 
due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 164.311, +50.501 which is 
   RA(J2000) = 10h 57m 15s
   Dec(J2000) = +50d 30' 02"
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 ~5000 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 14:33 UT on 2020 September 12. There will thus be no XRT
or UVOT data for this trigger before this time. 

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: GRB200903B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28352
SUBJECT: GRB 200903B: Fermi GBM Final Real-time Localization
DATE:    20/09/03 02:53:01 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 02:42:40 UT on 3 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200903B (trigger 620793765.87189 / 200903113).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 53.9, Dec = -13.0 (J2000 degrees, equivalent to J2000 03h 35m, -13d 00'), with a statistical uncertainty of 4.8 degrees.

The angle from the Fermi LAT boresight is 32.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200903113/quicklook/glg_skymap_all_bn200903113.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/bn200903113/quicklook/glg_healpix_all_bn200903113.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200903113/quicklook/glg_lc_medres34_bn200903113.gif


GRB_name: GRB200903B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28353
SUBJECT: Fermi GRB 200903B: Global MASTER-Net observations report 
DATE:    20/09/03 05:45:11 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),

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-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) started inspect of the Fermi GRB 200903B ( Fermi GBM team, GCN 28352) errorbox  3567 sec after notice time and 3594 sec after trigger time at 2020-09-03 03:42:35 UT, with upper limit up to  18.6 mag. The observations began at zenith distance = 76 deg. The sun  altitude  is -63.6 deg. 

The galactic latitude b = -49 deg., longitude l = 201 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1432912

We obtain a following upper limits.  

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

    3625 | 2020-09-03 03:42:35 |         MASTER-OAFA | (03h 28m 58.40s , -14d 45m 45.9s) |   C |    60 | 17.0 |        
    3704 | 2020-09-03 03:43:55 |         MASTER-OAFA | (03h 27m 18.24s , -12d 45m 19.8s) |   C |    60 | 16.9 |        
    3784 | 2020-09-03 03:45:14 |         MASTER-OAFA | (03h 25m 48.38s , -10d 45m 20.8s) |   C |    60 | 16.8 |        
    3863 | 2020-09-03 03:46:34 |         MASTER-OAFA | (03h 30m 56.48s , -16d 47m 17.0s) |   C |    60 | 17.4 |        
    3943 | 2020-09-03 03:47:53 |         MASTER-OAFA | (03h 29m 01.54s , -14d 46m 52.6s) |   C |    60 | 17.0 |        
    4022 | 2020-09-03 03:49:12 |         MASTER-OAFA | (03h 37m 13.53s , -14d 45m 29.6s) |   C |    60 | 17.0 |        
    4101 | 2020-09-03 03:50:32 |         MASTER-OAFA | (03h 27m 16.64s , -12d 47m 17.9s) |   C |    60 | 17.0 |        
    4181 | 2020-09-03 03:51:52 |         MASTER-OAFA | (03h 35m 29.34s , -12d 45m 27.2s) |   C |    60 | 17.0 |        
    4261 | 2020-09-03 03:53:11 |         MASTER-OAFA | (03h 25m 48.73s , -10d 46m 18.9s) |   C |    60 | 16.9 |        
    4340 | 2020-09-03 03:54:30 |         MASTER-OAFA | (03h 33m 55.58s , -10d 45m 06.4s) |   C |    60 | 16.8 |        
    4420 | 2020-09-03 03:55:50 |         MASTER-OAFA | (03h 31m 02.58s , -16d 46m 16.2s) |   C |    60 | 17.6 |        
    4499 | 2020-09-03 03:57:09 |         MASTER-OAFA | (03h 39m 16.24s , -16d 47m 03.1s) |   C |    60 | 17.3 |        
    4579 | 2020-09-03 03:58:29 |         MASTER-OAFA | (03h 37m 16.08s , -14d 46m 44.3s) |   C |    60 | 17.1 |        
    4658 | 2020-09-03 03:59:48 |         MASTER-OAFA | (03h 35m 27.61s , -12d 45m 28.7s) |   C |    60 | 17.2 |        
    4737 | 2020-09-03 04:01:08 |         MASTER-OAFA | (03h 33m 58.65s , -10d 46m 56.7s) |   C |    60 | 16.9 |        
    4817 | 2020-09-03 04:02:27 |         MASTER-OAFA | (03h 39m 20.96s , -16d 45m 19.2s) |   C |    60 | 17.3 |        
    4896 | 2020-09-03 04:03:47 |         MASTER-OAFA | (03h 43m 35.39s , -12d 44m 52.8s) |   C |    60 | 17.0 |        
    4976 | 2020-09-03 04:05:06 |         MASTER-OAFA | (03h 45m 26.48s , -14d 46m 50.6s) |   C |    60 | 17.3 |        
    5055 | 2020-09-03 04:06:26 |         MASTER-OAFA | (03h 42m 06.23s , -10d 45m 08.7s) |   C |    60 | 17.1 |        
    5367 | 2020-09-03 04:11:37 |         MASTER-OAFA | (03h 43m 34.98s , -12d 46m 01.5s) |   C |    60 | 17.3 |        
    5447 | 2020-09-03 04:12:57 |         MASTER-OAFA | (03h 51m 46.34s , -12d 44m 45.1s) |   C |    60 | 17.4 |        
    5526 | 2020-09-03 04:14:17 |         MASTER-OAFA | (03h 45m 31.39s , -14d 45m 55.5s) |   C |    60 | 17.4 |        
    5606 | 2020-09-03 04:15:36 |         MASTER-OAFA | (03h 53m 39.63s , -14d 46m 40.4s) |   C |    60 | 17.4 |        
    5685 | 2020-09-03 04:16:55 |         MASTER-OAFA | (03h 42m 09.36s , -10d 46m 41.4s) |   C |    60 | 17.3 |        
    5764 | 2020-09-03 04:18:15 |         MASTER-OAFA | (03h 50m 13.42s , -10d 44m 50.3s) |   C |    60 | 17.1 |        
    6049 | 2020-09-03 04:22:59 |         MASTER-OAFA | (03h 10m 52.85s , -12d 46m 48.3s) |   C |    60 | 17.5 |        
    6333 | 2020-09-03 04:27:44 |         MASTER-OAFA | (03h 51m 51.53s , -12d 45m 51.5s) |   C |    60 | 17.5 |        
    6413 | 2020-09-03 04:29:03 |         MASTER-OAFA | (03h 53m 39.74s , -14d 46m 47.5s) |   C |    60 | 17.6 |        
    6492 | 2020-09-03 04:30:23 |         MASTER-OAFA | (03h 50m 15.88s , -10d 46m 19.3s) |   C |    60 | 17.3 |        
    6774 | 2020-09-03 04:35:04 |         MASTER-OAFA | (03h 10m 55.15s , -12d 47m 29.0s) |   C |    60 | 17.6 |        
    6853 | 2020-09-03 04:36:24 |         MASTER-OAFA | (03h 19m 08.73s , -12d 45m 44.6s) |   C |    60 | 17.4 |        
    6933 | 2020-09-03 04:37:43 |         MASTER-OAFA | (03h 12m 27.24s , -14d 45m 44.8s) |   C |    60 | 17.6 |        
    7012 | 2020-09-03 04:39:02 |         MASTER-OAFA | (03h 14m 17.38s , -16d 47m 43.3s) |   C |    60 | 17.5 |        
    7092 | 2020-09-03 04:40:22 |         MASTER-OAFA | (03h 33m 16.32s , -18d 45m 28.1s) |   C |    60 | 18.4 |        
    7374 | 2020-09-03 04:45:05 |         MASTER-OAFA | (03h 19m 08.22s , -12d 46m 08.8s) |   C |    60 | 17.3 |        
    7454 | 2020-09-03 04:46:24 |         MASTER-OAFA | (03h 12m 27.33s , -14d 46m 47.0s) |   C |    60 | 17.6 |        
    7533 | 2020-09-03 04:47:44 |         MASTER-OAFA | (03h 20m 40.64s , -14d 45m 34.4s) |   C |    60 | 17.6 |        
    7613 | 2020-09-03 04:49:03 |         MASTER-OAFA | (03h 14m 21.97s , -16d 46m 43.1s) |   C |    60 | 17.9 |        
    7693 | 2020-09-03 04:50:23 |         MASTER-OAFA | (03h 22m 36.75s , -16d 47m 31.2s) |   C |    60 | 17.9 |        
    7773 | 2020-09-03 04:51:43 |         MASTER-OAFA | (03h 33m 20.11s , -18d 47m 09.7s) |   C |    60 | 18.5 |        
    7852 | 2020-09-03 04:53:03 |         MASTER-OAFA | (03h 41m 41.33s , -18d 45m 33.0s) |   C |    60 | 18.3 |        
    8134 | 2020-09-03 04:57:45 |         MASTER-OAFA | (03h 20m 47.96s , -14d 45m 54.7s) |   C |    60 | 17.6 |        
    8214 | 2020-09-03 04:59:04 |         MASTER-OAFA | (03h 22m 36.50s , -16d 46m 33.5s) |   C |    60 | 17.8 |        
    8293 | 2020-09-03 05:00:23 |         MASTER-OAFA | (03h 41m 38.88s , -18d 45m 07.4s) |   C |    60 | 18.3 |        
    8378 | 2020-09-03 05:01:49 |         MASTER-OAFA | (03h 47m 34.14s , -16d 46m 57.2s) |   C |    60 | 17.8 |        
    8458 | 2020-09-03 05:03:08 |         MASTER-OAFA | (03h 40m 51.81s , -08d 45m 31.3s) |   C |    60 | 17.7 |        
    8537 | 2020-09-03 05:04:27 |         MASTER-OAFA | (03h 24m 44.53s , -08d 45m 36.5s) |   C |    60 | 17.3 |        
    8616 | 2020-09-03 05:05:47 |         MASTER-OAFA | (03h 09m 33.05s , -10d 45m 43.1s) |   C |    60 | 17.5 |        
    8775 | 2020-09-03 05:08:26 |         MASTER-OAFA | (03h 47m 42.19s , -16d 46m 49.2s) |   C |    60 | 17.6 |        
    8855 | 2020-09-03 05:09:45 |         MASTER-OAFA | (03h 55m 57.66s , -16d 45m 11.5s) |   C |    60 | 17.9 |        
    8935 | 2020-09-03 05:11:05 |         MASTER-OAFA | (03h 40m 52.13s , -08d 46m 46.6s) |   C |    60 | 17.7 |        
    9014 | 2020-09-03 05:12:25 |         MASTER-OAFA | (03h 48m 59.79s , -08d 44m 49.3s) |   C |    60 | 17.6 |        
    9094 | 2020-09-03 05:13:44 |         MASTER-OAFA | (03h 24m 39.80s , -08d 46m 23.1s) |   C |    60 | 17.4 |        
    9173 | 2020-09-03 05:15:03 |         MASTER-OAFA | (03h 32m 44.88s , -08d 45m 12.0s) |   C |    60 | 17.5 |        
    9252 | 2020-09-03 05:16:23 |         MASTER-OAFA | (03h 09m 40.92s , -10d 46m 42.5s) |   C |    60 | 17.7 |        
    9332 | 2020-09-03 05:17:42 |         MASTER-OAFA | (03h 17m 40.79s , -10d 47m 32.5s) |   C |    60 | 17.6 |        
    9491 | 2020-09-03 05:20:21 |         MASTER-OAFA | (03h 24m 51.97s , -18d 45m 38.1s) |   C |    60 | 18.6 |        
    9571 | 2020-09-03 05:21:41 |         MASTER-OAFA | (03h 55m 57.80s , -16d 46m 17.3s) |   C |    60 | 18.0 |        
    9650 | 2020-09-03 05:23:00 |         MASTER-OAFA | (03h 48m 59.38s , -08d 45m 05.6s) |   C |    60 | 17.8 |        
    9729 | 2020-09-03 05:24:19 |         MASTER-OAFA | (03h 32m 45.09s , -08d 46m 09.7s) |   C |    60 | 17.5 |        
    9809 | 2020-09-03 05:25:39 |         MASTER-OAFA | (03h 17m 41.51s , -10d 45m 29.1s) |   C |    60 | 17.6 |        
    9888 | 2020-09-03 05:26:58 |         MASTER-OAFA | (03h 24m 54.71s , -18d 46m 23.2s) |   C |    60 | 18.5 |        
    9967 | 2020-09-03 05:28:18 |         MASTER-OAFA | (03h 50m 10.43s , -18d 46m 28.7s) |   C |    60 | 18.2 |        
   10127 | 2020-09-03 05:30:57 |         MASTER-OAFA | (03h 39m 51.52s , -06d 45m 56.6s) |   C |    60 | 17.5 |        
   10285 | 2020-09-03 05:33:36 |         MASTER-OAFA | (03h 50m 03.83s , -18d 46m 49.8s) |   C |    60 | 18.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200817B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28354
SUBJECT: GRB200817B: AstroSat CZTI detection 
DATE:    20/09/03 09:58:27 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

V. Shenoy (IITB), V. Bhalerao (IITB), S. Gupta, V. Sharma, A. Vibhute, 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 200817B.

The source was detected in the 20-200 keV energy range. The light curve showed multiple pulses of emission with the strongest peak at 2020-08-17 06:03:44 UT. The measured peak count rate associated with the burst is 453 cts/s above the background in the combined data of four quadrants, with a total of 3726 cts. The local mean background count rate was 488 cts/s. Using cumulative rates, we measure a T90 of 21.0 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: GRB200817B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28355
SUBJECT: ZTF20abtxwfx/AT2020sev : AstroSat CZTI non-detection of a transient 
DATE:    20/09/03 10:04:12 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

V. Shenoy, V. Bhalerao (IITB), I. Andreoni, M. Kasliwal (Caltech), D. Bhattacharya (IUCAA), A. R. Rao (TIFR), S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration and GROWTH collaborations:

We fit the optical emission ZTF20abtxwfx/AT2020sev (Andreoni et al., GCN #28305) with a (t-t0)^-alpha power law decay, we obtain a decay rate alpha=0.68+-0.12. The best-fit explosion time is MJD 59078.77 +- 0.17 (2020-08-17 18:34:32 UT +- 4.08 hours), 1-sigma errors.

We searched AstroSat CZTI data for a coincident transient within the 3-sigma time span, and do not find any significant candidates. The closest candidate is GRB200817B (Shenoy et al., GCN #28354) which is 3.01 sigma from the calculated T0. While CZTI has limited localisation abilities for GRBs, the illumination of the detectors (Detector Plane Histogram) is inconsistent with this GRB arising from the location of AT2020sev. Hence we rule out an association between the long GRB 200817B and ZTF20abtxwfx/ AT2020sev.


GRB_name: GRB200903B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28356
SUBJECT: AGILE detection of a burst (AGILE trigger no. 526185273)
DATE:    20/09/03 11:17:47 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected a long burst at T0 = 2020-09-03 02:34:34 (UT).
The event is clearly visible in the scientific ratemeters of the SuperAGILE
(SA; 18-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and AntiCoincidence
(AC; 50-200 keV) detectors. The light curves show multiple emission
episodes. The main episode lasted ~30 s and released 155300 counts in the
SA detector (above a background rate of 62 Hz), 70500 counts in the MCAL
detector (above a background rate of 1240 Hz), and 3850 counts in the AC
detector (above a background rate of 3070 Hz). Several successive spikes
follow the main episode. The AGILE ratemeters light curves can be found at:
http://www.agilescienceapp.it/notices/burst200903023434_AGILE_RMs.png .

The event also triggered a MCAL high time resolution data acquisition
covering the first ~5 s of the GRB. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB_069402_526185273.882807.png .

The event is compatible with the event reported by CALET (trigger ID
1283135531) and INTEGRAL SPI-ACS (trigger ID 8707,0).

The burst might be related with GRB 200903B reported by Fermi-GBM (GCN
#28352), occurring at 2020-09-03 02:42:40 (UT).

Additional analysis of AGILE data is in progress.


GRB_name: GRB200903A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28357
SUBJECT: GRB 200903A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/09/03 12:06:27 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 (ICRR), S. Torii, Y. Akaike, K. Kobayashi (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 long soft GRB 200903A (Swift detection: Beardmore et al.,
GCN Circ. 28350; https://gcn.gsfc.nasa.gov/other/200903A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 00:44:17.477 UTC
on 3 September 2020 (http://cgbm.calet.jp/cgbm_trigger/flight/1283129005/).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure which starts
at T+1.5 sec, peaks at T+5.9 sec, and ends at T+10.5 sec.
The T90 and T50 durations measured by the SGM data are 8.2 +- 0.8 sec
and 4.2 +- 0.8 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1283129005/

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


GRB_name: GRB200903B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28358
SUBJECT: GRB 200903B: Insight-HXMT/HE detection
DATE:    20/09/03 13:36:42 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, C. Cai, 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 2020-09-03T02:42:40.87 (T0), Insight-HXMT/HE detected 
GRB 200903B (trigger ID: HEB200903112) in a routine search of the data, 
which also triggered Fermi-GBM (Fermi GBM team, GCN#28352).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 70.88 s measured from T0-27.86 s. 
The 1-ms peak rate, measured from T0+38.32 s, is 622 cnts/sec. 
The total counts from this burst is 11739 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200903112_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: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28359
SUBJECT: GRB 200829A: optical observations, a light curve in R-filter
DATE:    20/09/03 15:15:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), N. Pankov (HSE), S. Belkin (IKI), A. Volnova (IKI), 
I. Reva (FAPHI), A. Zhornichenko (KIAM), A. Novichonok (Petrozavodsk 
State University, KIAM), S. Naroenkov (INASAN), K.  Antoniuk (CrAO), 
R.Ya. Inasaridze (AbAO), E. Mazaeva (IKI), Sh. Ehgamberdiev (UBAI) 
report on behalf of larger GRB IKI FuN collaboration:

We observed the the field of GRB 200829A (Siegel et al., GCN 28307; Ursi
et al., GCN 28314; Ridnaia et al., GCN 28323; Lesage & Meegan, GCN
28326)  with Zeiss-1000 telescope of TShAO observatory, RC-36 telescope 
of Kitab observatory, Zeiss-1000 telescope of Koshka Observatory, AZT-11 
telescope of CrAO observatory, and AS-23 telescope of AbAO observatory. 
The optical afterglow (Siegel et al., GCN 28307, Pozanenko et al., GCN 
28308; Kuin & Siegel, GCN 28311; Lipunov et al., GCN 28315; Vinko et 
al., GCN 28316; Hentunen et al., GCN 28318; Moskvitin et al., GCNs 
28322, 28328, Zhu et al., GCNs 28324,  28330; Pankov et al., GCN 28329; 
Izzo, GCN 28331; Volnova et al., GCN  28333)  is detected on first two 
days   after GRB trigger. Preliminary light curve of the afterglow in 
R-filter can be found at

http://grb.rssi.ru/GRB200829A/GRB200829A_LC1_R.png

One can tentatively assume a jet break in the light curve at ~0.33 days.

(The photometry is based on nearby USNO-B1.0 stars identical for all 
observations.)


GRB_name: GRB200903A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28360
SUBJECT: GRB 200903A: Swift-BAT refined analysis
DATE:    20/09/03 18:48:09 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), 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-239 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 200903A (trigger #994389)
(Beardmore et al., GCN Circ. 28350).  The BAT ground-calculated position is
RA, Dec = 164.313, 50.488 deg which is
   RA(J2000)  =  10h 57m 15.1s
   Dec(J2000) = +50d 29' 15.7"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67%.

The mask-weighted light curve shows a precursor at ~T-19 s, followed by the
main structure with several overlapping pulses that starts at ~T-5 s and
ends at ~T+20 s. The burst went out of the BAT FOV at T+64 s.
T90 (15-350 keV) is 24.15 +- 7.68 sec (estimated error including
systematics).

The time-averaged spectrum from T-19.18 to T+22.13 sec is best fit by a
power
law with an exponential cutoff.  This fit gives a photon index 1.15 +-
0.28,
and Epeak of 107.4 +- 65.8 keV (chi squared 45.20 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.8 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.14 sec in the 15-150 keV band is
3.8 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.56 +- 0.07 (chi squared 51.88 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/994389/BA/


GRB_name: GRB200903C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28361
SUBJECT: GRB 200903C: Fermi GBM Final Real-time Localization
DATE:    20/09/03 21:49:19 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 SHORT GRB

At 21:38:58 UT on 3 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200903C (trigger 620861943.576056 / 200903902).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 9.8, Dec = -2.9 (J2000 degrees, equivalent to J2000 00h 39m, -2d 53'), with a statistical uncertainty of 14.6 degrees.

The angle from the Fermi LAT boresight is 85.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200903902/quicklook/glg_skymap_all_bn200903902.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/bn200903902/quicklook/glg_healpix_all_bn200903902.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200903902/quicklook/glg_lc_medres34_bn200903902.gif


GRB_name: GRB200903A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28362
SUBJECT: GRB 200903A: Fermi GBM detection
DATE:    20/09/04 00:48:15 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

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

"At 00:44:19.25 UT on 3 September 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200903A (trigger 620786664 / 200903031)
which was also detected by the Swift/BAT (A. P. Beardmore et al. 2020, GCN
28350).
The Fermi GBM Final Real-time Localization (GCN 28349) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is ~61
degrees.

The GBM light curve shows a single bright peak
with a duration (T90) of about 26.9 s (50-300 keV).
The time-averaged spectrum from T0-5.4 s to T0+21.5 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.9 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 111.4 +/- 8.9 keV.

The event fluence (10-1000 keV) in this time interval is
(4.6 +/- 0.2)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+3.3 s in the 10-1000 keV band
is 6.03 +/- 0.24 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: GRB200903D
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28363
SUBJECT: GRB 200903D: MAXI/GSC detection
DATE:    20/09/04 01:00:17 GMT
FROM:    Motoko Serino at RIKEN/MAXI  <motoko@crab.riken.jp>

S. Ogawa (Kyoto U.),
H. Negoro, M. Nakajima, M. Aoki, K. Kobayashi, R. Takagi, K, Asakura, K, Seino (Nihon U.),
T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, R. Adachi, M. Niwano (Tokyo Tech),
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA),
Y. Ueda, S. Yamada, K. Setoguchi, T. Yoshitake (Kyoto U.),
H. Tsunemi (Osaka U.),
M. Yamauchi, 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 15:32:04 UT .
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (312.777 deg, -0.598 deg) = (20 51 06, -00 35 52) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.26 deg and 0.22 deg, respectively.
The roll angle of long axis from the north direction is 55.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 182 +- 36 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
There was no significant excess flux in the previous transit at UT 13:59
and in the next transit at 17:04 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB200903C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28364
SUBJECT: Fermi GRB 200903C: Global MASTER-Net observations report 
DATE:    20/09/04 01:30:59 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),

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-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) started inspect of the Fermi GRB 200903C ( Fermi GBM team, GCN 28361) errorbox  8291 sec after notice time and 8323 sec after trigger time at 2020-09-03 23:57:42 UT, with upper limit up to  17.9 mag. The observations began at zenith distance = 77 deg. The sun  altitude  is -21.6 deg. 

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200903C errorbox  11113 sec after notice time and 11145 sec after trigger time at 2020-09-04 00:44:44 UT, with upper limit up to  16.5 mag. The observations began at zenith distance = 51 deg. The sun  altitude  is -24.3 deg. 

The galactic latitude b = -65 deg., longitude l = 117 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1433346

We obtain a following upper limits.  

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

    8414 | 2020-09-03 23:57:42 |         MASTER-OAFA | (23h 45m 43.67s , -12d 49m 48.0s) |   C |   180 | 17.9 |        
   10209 | 2020-09-04 00:27:37 |         MASTER-OAFA | (00h 02m 47.84s , -16d 48m 14.1s) |   C |   180 | 17.1 |        
   11236 | 2020-09-04 00:44:44 |      MASTER-Tavrida | (00h 44m 08.68s , -04d 02m 46.7s) |   C |   180 | 15.4 |        
   11437 | 2020-09-04 00:48:05 |      MASTER-Tavrida | (01h 00m 04.67s , -04d 03m 05.0s) |   C |   180 | 14.9 |        
   11637 | 2020-09-04 00:51:25 |      MASTER-Tavrida | (01h 08m 06.78s , -04d 01m 49.9s) |   C |   180 | 15.4 |        
   11838 | 2020-09-04 00:54:46 |      MASTER-Tavrida | (00h 44m 09.09s , -04d 04m 10.7s) |   C |   180 | 16.5 |        
   12039 | 2020-09-04 00:58:07 |      MASTER-Tavrida | (00h 52m 02.97s , -04d 04m 55.6s) |   C |   180 | 16.3 |        
   12241 | 2020-09-04 01:01:29 |      MASTER-Tavrida | (01h 08m 11.79s , -04d 03m 50.0s) |   C |   180 | 15.7 |        
   12441 | 2020-09-04 01:04:50 |      MASTER-Tavrida | (00h 44m 29.40s , -08d 05m 45.3s) |   C |   180 | 15.8 |        
   12642 | 2020-09-04 01:08:10 |      MASTER-Tavrida | (00h 52m 09.85s , -04d 03m 39.9s) |   C |   180 | 15.9 |        
   13245 | 2020-09-04 01:18:13 |      MASTER-Tavrida | (00h 52m 32.44s , -08d 06m 10.8s) |   C |   180 | 15.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200904A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28365
SUBJECT: GRB 200904A: Fermi GBM Final Real-time Localization
DATE:    20/09/04 02:13:11 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 02:02:55 UT on 4 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200904A (trigger 620877780.28243 / 200904085).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 15.8, Dec = -16.0 (J2000 degrees, equivalent to J2000 01h 03m, -16d 00'), with a statistical uncertainty of 11.6 degrees.

The angle from the Fermi LAT boresight is 102.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200904085/quicklook/glg_skymap_all_bn200904085.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/bn200904085/quicklook/glg_healpix_all_bn200904085.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200904085/quicklook/glg_lc_medres34_bn200904085.gif


GRB_name: GRB200904A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28366
SUBJECT: Fermi GRB 200904A: Global MASTER-Net observations report 
DATE:    20/09/04 02:45:07 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),

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-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) started inspect of the Fermi GRB 200904A ( Fermi GBM team, GCN 28365) errorbox  533 sec after notice time and 651 sec after trigger time at 2020-09-04 02:13:46 UT, with upper limit up to  17.2 mag. The observations began at zenith distance = 62 deg. The sun  altitude  is -49.5 deg. 

The galactic latitude b = -78 deg., longitude l = 140 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1433460

We obtain a following upper limits.  

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

     742 | 2020-09-04 02:13:46 |         MASTER-OAFA | (01h 00m 58.86s , -16d 47m 45.9s) |   C |   180 | 17.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200903E
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28367
SUBJECT: GRB 200903E: AstroSat CZTI detection
DATE:    20/09/05 05:31:08 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a bright long GRB 200903E.

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 2020-09-03 02:34:50.40 UT. The measured peak count rate associated with the burst is 1061 +/- 38 cts/s above the background in the combined data of four quadrants, with a total of 22806 +/- 104 cts. The local mean background count rate was 597 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 90.78 +/- 0.02 s. In preliminary analysis, we find that 1885 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. The light curve showed multiple peaks of emission with the strongest peak at 2020-09-03 02:34:49.00 UT. The measured peak count rate is 3999 +/- 75 cts/s above the background in the combined Veto data of four quadrants, with a total of 79278 +/- 173 cts. The local mean background count rate was 1611 +/- 1 cts/s.  We measure a T90 of 90.50 +/- 0.03 s from the cumulative Veto light curve.

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: GRB200906A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28370
SUBJECT: GRB 200906A: Fermi GBM Final Real-time Localization
DATE:    20/09/06 13:22:12 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 LONG GRB

At 13:11:53 UT on 6 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200906A (trigger 621090718.377264 / 200906550).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 270.0, Dec = 68.6 (J2000 degrees, equivalent to J2000 18h 00m, 68d 35'), with a statistical uncertainty of 4.1 degrees.

The angle from the Fermi LAT boresight is 83.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200906550/quicklook/glg_skymap_all_bn200906550.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/bn200906550/quicklook/glg_healpix_all_bn200906550.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200906550/quicklook/glg_lc_medres34_bn200906550.gif


GRB_name: GRB200906A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28371
SUBJECT: GRB 200906A: Swift detection of a burst
DATE:    20/09/06 13:26:53 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), D. N. Burrows (PSU), J.D. Gropp (PSU),
S. Laha (GSFC/UMBC/CRESST), A. Y. Lien (GSFC/UMBC) and
D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 13:11:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200906A (trigger=994856).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 272.293, +67.852 which is 
   RA(J2000) = 18h 09m 10s
   Dec(J2000) = +67d 51' 08"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed two main peaks
with a duration of about 80 sec.  The second, larger, peak extends 
past the end of the slew and into the interval observed by XRT and UVOT.  
The peak count rate was ~3000 counts/sec (15-350 keV), 
at ~52 sec after the trigger. 

The XRT began observing the field at 13:12:10.8 UT, 66.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 272.2731,
67.8791 which is equivalent to:
   RA(J2000)  = 18h 09m 05.54s
   Dec(J2000) = +67d 52' 44.8"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 101 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 in excess of the Galactic value (5.25 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 5.5
(+6.91/-5.25) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 0.1 s image was 2.09e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 76 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
0.05. 

Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB200906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28372
SUBJECT: GRB 200906A: Nanshan/NEXT optical upper limit
DATE:    20/09/06 16:18:07 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

S.Y. Fu, Z.P. Zhu, X. Liu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High 
School), X. Zhang, J.Z. Liu (XAO) report:

We observed the field of GRB 200906A (Page et al., GCN 28371) using the 
NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We only 
obtained 2x120s frames in the Sloan r-band due to the cloudy weather, 
starting at 15:03:47 UT on 2020-09-06, i.e., 1.88 hr after the BAT trigger.

No optical source is detected in our stacked image at the XRT position 
(Page et al., GCN 28371), down to a limiting magnitude of r~19.3, 
calibrated with the nearby PanSTARRS field.


GRB_name: GRB200906A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28373
SUBJECT: GRB 200906A: Enhanced Swift-XRT position
DATE:    20/09/06 21:22:01 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 687 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200906A, 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 = 272.27532, +67.88001 which is equivalent
to:

RA (J2000): 18h 09m 6.08s
Dec (J2000): +67d 52' 48.1"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB200906A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28374
SUBJECT: GRB 200906A: Fermi GBM detection
DATE:    20/09/07 00:03:11 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

R. Hamburg (UAH), C. Malacaria (NASA-MSFC/USRA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:


"At 13:11:53.38 UT on 06 September 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200906A (trigger 621090718 / 200906550)
which was also detected by the Swift/BAT and Swift/XRT (Page et al. 2020, GCN 28371).
The Fermi GBM Final Real-time Localization (GCN 28370) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 74 degrees.

The GBM light curve shows two peaks
with a duration (T90) of about 67.3 s (50-300 keV), starting at  T0-49 s.
The time-averaged spectrum from T0-4.1 s to T0+16.4 s is
best fit by a Band function with Epeak = 50.5 +/- 9.9 keV,
alpha = -1.1 +/- 0.2 , and beta = -2.1 +/- 0.1

The event fluence (10-1000 keV) in this time interval is
(3.9 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.8 s in the 10-1000 keV band
is 4.5 +/- 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: GRB200906A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28375
SUBJECT: GRB 200906A: Swift-XRT refined Analysis
DATE:    20/09/07 03:03:23 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.8 ks of XRT data for GRB 200906A (Page et al. GCN
Circ. 28371), from 70 s to 41.5 ks after the  BAT trigger. The data
comprise 121 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN Circ. 28373).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.60 (+/-0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.11 (+/-0.09). The
best-fitting absorption column is  7.2 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 5.2 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.22 (+0.26, -0.24)
and a best-fitting absorption column of 7.0 (+1.7, -1.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.9 x 10^-11 (8.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.0 (+1.7, -1.5) x 10^21 cm^-2
Galactic foreground: 5.2 x 10^20 cm^-2
Excess significance: 7.1 sigma
Photon index:      2.22 (+0.26, -0.24)

If the light curve continues to decay with a power-law decay index of
0.60, the count rate at T+24 hours will be 0.013 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.2 x
10^-13 (1.1 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00994856.

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


GRB_name: GRB200906A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28376
SUBJECT: GRB 200906A: OSN 1.5m Upper Limit
DATE:    20/09/07 03:31:53 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), C. C. Thoene, M. Blazek, J. F. Agui Fernandez (all 
HETH/IAA-CSIC), and V. Casanova (IAA-CSIC) report:

We observed the location (Beardmore et al., GCN #28373) of the Swift GRB 
200906A (Page et al., GCN #28371; GBM detection: Fermi GBM Team, GCN 
#28370, Hamburg et al., GCN #28374) with the 1.5m telescope of the 
Observatorio Sierra Nevada, in Granada, Spain. We obtained 78 x 100 s 
images beginning 2020-09-06 21:29:03.51 UT, after clouds had cleared.

In a stack of all images, centered at 0.39467 days after the GRB, no 
source is detected at the enhanced XRT position. Measured against two 
nearby USNO-B1.0 stars, we derive an upper limit of

Ic > 23.4 mag.

This agrees with the non-detection reported by Fu et al. (GCN #28372). 
We note the refined XRT analysis (Beardmore et al., GCN #28375) also 
reports an NH column density significantly exceeding the Galactic value, 
indicating this is a dark GRB.


GRB_name: GRB200906A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28377
SUBJECT: GRB 200906A: GROWTH-India Telescope (GIT) optical r band upper limit
DATE:    20/09/07 05:16:01 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar (IITB), P. Dorje (IIA), V. Bhalerao(IITB), G. C. Anupama(IIA), S.
Barway(IIA), report on behalf of the GROWTH-India collaboration:


We observed GRB200906A reported by Swift-BAT (K. L. Page et al., (GCN
28371), see also S.Y. Fu et al.,(GCN 28372), A.P. Beardmore

Et al., (GCN 28373), R. Hamburg et al., (GCN 28374) & D. A. Kann et al.,
(GCN 28376) with 0.7m GROWTH-India telescope. The field was observed in the
SDSS r filter starting at 2020-09-06T16:34:48 UT i.e. ~ 3.33 hrs after the
event detection by Swift-BAT. We didnâ€™t find any new source within an
uncertainty region of 1.9 arcsec around Ra(J2000) = 18:09:06.08, Dec(J2000)
= +67:52:48.1 (GCN 28373) with an upper limit of*: *

r  > 20.14 mag

(calibrated against PanSTARRs PS1 data release, Flewelling et al., 2018)



The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government

of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB200907A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28378
SUBJECT: GRB 200907A: AGILE/MCAL detection of a burst
DATE:    20/09/07 16:09:14 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), 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), M. Pilia, A. Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), F.
Longo (Univ. Trieste and INFN Trieste), A. Giuliani (INAF/IASF-Mi), report
on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected a short burst at T0 = 2020-09-07
14:24:24.73 +/- 0.01 s (UTC).

The event lasted about 1.6 s and released a total number of ~350 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 680 Hz.

The light curve shows a single sharp peak and it can be found at
http://www.agilescienceapp.it/notices/GRB_069464_526573464.733762.png .

The event is also clearly visible in the AGILE Scientific Ratemeters of the
SuperAGILE [SA; 18-60 keV], MiniCALorimeter [MCAL; 0.4-100 MeV], and
AntiCoincidence [AC; 50-200 keV] detectors.

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.
Automatic MCAL GRB alert Notices can be found at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.


GRB_name: GRB200906A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28379
SUBJECT: GRB 200906A: Swift/UVOT Upper Limits
DATE:    20/09/07 16:13:35 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

GRB 200906A: Swift/UVOT Upper Limits

J. D. Gropp (PSU) and K. L. Page (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200906A
76 s after the BAT trigger (Page et al., GCN Circ. 28371).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 28373)
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            76          226          147         >21.2
u_FC               289          538          246         >20.4
white               76         5054          472         >21.3
v                  618         1413           97         >19.4
b                  544         4948          274         >20.1
u                  289         1487          324         >20.4
w1                 668         1462           97         >19.3
m2                 643         1438           78         >20.1
w2                 594         1389           97         >19.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200906A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28380
SUBJECT: GRB 200906A: Swift-BAT refined analysis
DATE:    20/09/07 16:58:46 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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), 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-240 to T+962 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 200906A (trigger #994856)
(Page et al., GCN Circ. 28371).  The BAT ground-calculated position is
RA, Dec = 272.284, 67.887 deg which is
   RA(J2000)  =  18h 09m 08.2s
   Dec(J2000) = +67d 53' 13.4"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.

The mask-weighted light curve shows a double-peaked structure. The first
pulse starts at ~T-9 s and peaks at ~T+5 s. The second pulse starts
at ~T+46 s, peaks at ~T+51 s, and ends at ~T+90 s. T90 (15-350 keV)
is 70.90 +- 7.63 sec (estimated error including systematics).

The time-averaged spectrum from T-8.70 to T+90.01 sec is best fit by
a simple power-law model.  The power law index of the time-averaged
spectrum is 2.00 +- 0.09.  The fluence in the 15-150 keV band
is 2.8 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+50.96 sec in the 15-150 keV band is 2.5 +- 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/994856/BA/


GRB_name: GRB200906A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28381
SUBJECT: GRB 200906A: LBT near-infrared upper limit
DATE:    20/09/07 18:02:35 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi (INAF-OAS) reports on behalf of the CIBO collaboration:

We observed the location of the X-ray afterglow (Beardmore et al., GCN 
28373) of the Swift GRB 200906A (Page et al., GCN 28371) simultaneously 
in the H and Ks bands with the LUCI near-infrared imager and 
spectrograph mounted on the Large Binocular Telescope (LBT, Mt Graham, 
AZ, USA).
Observations started at 03:57 UT on 2020-09-07, and allowed us to obtain 
18 min of exposure in each band. Unfortunately, observations were 
performed under variable sky conditions with passing clouds.

Inspection of the combined H-band images (mid-time of 0.628 days after 
the GRB), does not reveal any source down to the limiting magnitude 
H<21.8 mag (AB system).

A preliminary comparison of the simultaneous Swift/XRT flux of 1.06e-07 
Jy at a mid-frequency 3.8E+17 Hz (1.6 keV), gives a X-ray to infrared 
slope-index b_OX<0.5, confirming the dark nature of this GRB. This XRT 
flux has been obtained modelling the XRT lightcurve after 200 seconds 
with a power-law with decay-index 0.60+-0.04.

We acknowledge the excellent support from the LBTO and LBT-INAF staff, 
particularly B. Rothberg, F. Cusano, S. Paiano and D. Paris, in 
obtaining these observations.


GRB_name: GRB200906A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28382
SUBJECT: GRB 200906A: EMIR/GTC NIR upper limit
DATE:    20/09/07 18:26:14 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. A. Kann, 
C. C. Thoene, M. Blazek, J. F. Agui Fernandez (all HETH/IAA-CSIC), 
D. Reverte Paya (GTC) report:

We observed the field of GRB 200906A (Page et al., GCN #28371; 
GBM detection: Fermi GBM Team, GCN #28370; Hamburg et al., 
GCN #28374) with EMIR on the 10.4m GTC telescope, at the Roque 
de los Muchachos Observatory (La Palma, Spain). The observation 
consisted of H-band imaging with a total integration time of 955 s, and 
a mean epoch on the 6th of September at 23:57:35 UT (10.5753 hr 
after the Swift trigger).

No source is detected within the refined XRT error circle (Beardmore 
et al., GCN #28373) down to a 3-sigma limit of 

H(AB) > 23.5 mag 

This non detection is consistent with the previously reported limits 
(Fu et al., GCN#28372; Kann et al., GCN#28376; Kumar et al., 
GCN#28377; Gropp et al., GCN#28379; Rossi et al. GCN#28381)
and confirms the dark nature of the burst.


GRB_name: GRB200903E
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28383
SUBJECT: IPN triangulation of GRB 200903E
DATE:    20/09/07 18:57:54 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

A. Ursi, F. Verrecchia, M. Tavani, N. Parmiggiani, C. Pittori,
A. Bulgarelli, on behalf of the AGILE 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 200903E
(AGILE detection: Ursi et al., GCN Circ. 28356;
AstroSat CZTI detection: Gupta et al., GCN Circ. 28367)
was detected by Konus-Wind, INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND), AGILE (MCAL), and AstroSat (CZTI)
at about 9267 s UT (02:34:27).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  177.108 (11h 48m 26s) -31.594 (-31d 35' 40")
 Corners:
  178.077 (11h 52m 19s) -31.782 (-31d 46' 55")
  177.058 (11h 48m 14s) -32.482 (-32d 28' 55")
  176.149 (11h 44m 36s) -31.391 (-31d 23' 27")
  177.164 (11h 48m 39s) -30.696 (-30d 41' 45")
 ---------------------------------------------
The error box area is 1.5 sq. deg, and its maximum
dimension is 1.8 deg (the minimum one is 1.1 deg).
The Sun distance was 41 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200903_T09267/IPN/

The localization of GRB 200903E is inconsistent with the localization
of GRB 200903B (GCN Circ. 28352).

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


GRB_name: GRB200907B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28384
SUBJECT: GRB 200907B: Swift detection of a short burst
DATE:    20/09/07 19:01:32 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), S. D. Barthelmy (GSFC),
J. A. Kennea (PSU), N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
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 18:51:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200907B (trigger=995004).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 89.013, +6.911 which is 
   RA(J2000) = 05h 56m 03s
   Dec(J2000) = +06d 54' 38"
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 1 sec.  The peak count rate
was ~4000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 18:52:31.3 UT, 80.1 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 89.02837, 6.90752 which is equivalent
to:
   RA(J2000)  = 05h 56m 06.81s
   Dec(J2000) = +06d 54' 27.1"
with an uncertainty of 3.8 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 4.23
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 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
0.61. 

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: GRB200907B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28385
SUBJECT: GRB 200907B: Prompt enhanced Swift-XRT position
DATE:    20/09/07 19:21:53 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 200907B, we find an
enhanced XRT position of the afterglow: RA, Dec: 89.0289, 6.9063 which
is equivalent to:
   RA (J2000)  = 05 56 06.93
   Dec (J2000) = +06 54 22.8
with an uncertainty of 2.2 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/995004.

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: GRB200906A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28386
SUBJECT: Fermi GRB 200906A: Global MASTER-Net observations report 
DATE:    20/09/07 21:32:09 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200906A ( Fermi GBM team, GCN 28370) errorbox  1 days 28040 sec after notice time and 1 days 28073 sec after trigger time at 2020-09-07 20:59:46 UT, with upper limit up to  18.7 mag. The observations began at zenith distance = 41 deg. The sun  altitude  is -39.4 deg. 

The galactic latitude b = 30 deg., longitude l = 99 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1434684

We obtain a following upper limits.  

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

  114563 | 2020-09-07 20:59:46 |      MASTER-Tavrida | (18h 06m 25.68s , +67d 46m 47.4s) |   C |   180 | 18.6 |        
  114764 | 2020-09-07 21:03:07 |      MASTER-Tavrida | (18h 06m 28.97s , +67d 47m 45.3s) |   C |   180 | 18.7 |        
  114965 | 2020-09-07 21:06:28 |      MASTER-Tavrida | (18h 06m 23.16s , +67d 46m 55.2s) |   C |   180 | 18.6 |        
  115166 | 2020-09-07 21:09:49 |      MASTER-Tavrida | (18h 06m 25.23s , +67d 47m 41.8s) |   C |   180 | 18.7 |        
  115366 | 2020-09-07 21:13:09 |      MASTER-Tavrida | (18h 06m 30.87s , +67d 46m 28.9s) |   C |   180 | 18.7 |        
  115567 | 2020-09-07 21:16:30 |      MASTER-Tavrida | (18h 06m 25.58s , +67d 45m 15.3s) |   C |   180 | 18.6 |        
  115769 | 2020-09-07 21:19:52 |      MASTER-Tavrida | (18h 06m 32.36s , +67d 45m 24.9s) |   C |   180 | 18.6 |        
  115970 | 2020-09-07 21:23:13 |      MASTER-Tavrida | (18h 06m 30.08s , +67d 46m 46.7s) |   C |   180 | 18.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200907A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28387
SUBJECT: GRB200907A: GROWTH-India optical upper limit
DATE:    20/09/07 22:25:42 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar (IITB), P. Dorje (IIA), V. Bhalerao(IITB), G. C. Anupama(IIA), S.
Barway(IIA), report on behalf of the GROWTH-India collaboration:

We observed GRB200907A reported by Swift-BAT (A.P. Beardmore et al., GCN
#28384, P.A. Evans et al., GCN #28385) with 0.7m GROWTH-India telescope.
The field was observed in the SDSS r filter starting at
2020-09-07T20:59:05.36 UT i.e. ~2.1 hrs after the event detection by
Swift-BAT. We didnâ€™t find any new source in stacked image of 7*500 sec
exposure, within an uncertainty region of 2.2 arcsec around RA(J2000) =
05:56:06.93, Dec(J2000)= +06:54:22.8 (GCN 28385) up to r > 20.83 mag
(5-sigma)(Calibrated against PanSTARRs PS1 data release, Flewelling et al.,
2018)


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government

of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB200907B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28388
SUBJECT: Correction to GCN 28387: GRB 200907B GROWTH-India optical upper limit
DATE:    20/09/07 23:01:18 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar (IITB), P. Dorje (IIA), V. Bhalerao(IITB), G. C. Anupama(IIA), S.
Barway(IIA), report on behalf of the GROWTH-India collaboration:

We apologize for the confusion caused in GRB name. GROWTH-India Telescope
followed-up GRB 200907B, not GRB 200907A.


Here is the corrected GCN:-

We observed GRB 200907B reported by Swift-BAT (A.P. Beardmore et al., GCN
#28384, P.A. Evans et al., GCN #28385) with 0.7m GROWTH-India telescope.
The field was observed in the SDSS r filter starting at
2020-09-07T20:59:05.36 UT i.e. ~2.1 hrs after the event detection by
Swift-BAT. We didnâ€™t find any new source in stacked image of 7*500 sec
exposure, within an uncertainty region of 2.2 arcsec around RA(J2000) =
05:56:06.93, Dec(J2000)= +06:54:22.8 (GCN 28385) up to

r > 20.83 mag (5-sigma) (calibrated against PanSTARRs PS1 data
release, Flewelling
et al., 2018).



The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB200907C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28389
SUBJECT: GRB 200907C: Fermi GBM Final Real-time Localization
DATE:    20/09/07 23:07:52 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 22:57:28 UT on 7 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200907C (trigger 621212253.091068 / 200907957).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 34.5, Dec = -78.4 (J2000 degrees, equivalent to J2000 02h 17m, -78d 24'), with a statistical uncertainty of 1.1 degrees.

The angle from the Fermi LAT boresight is 24.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200907957/quicklook/glg_skymap_all_bn200907957.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/bn200907957/quicklook/glg_healpix_all_bn200907957.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200907957/quicklook/glg_lc_medres34_bn200907957.gif


GRB_name: GRB200907C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28390
SUBJECT: Fermi GRB 200907C: Global MASTER-Net observations report 
DATE:    20/09/08 00:08:43 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),

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-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) started inspect of the Fermi GRB 200907C ( Fermi GBM team, GCN 28389) errorbox 69 sec after trigger time at 2020-09-07 22:58:37 UT, with upper limit up to  18.5 mag. Observations started at twilight.  The observations began at zenith distance = 67 deg. The sun  altitude  is -8.5 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200907C errorbox  109 sec after notice time and 211 sec after trigger time at 2020-09-07 23:00:59 UT, with upper limit up to  20.3 mag. The observations began at zenith distance = 48 deg. The sun  altitude  is -63.1 deg. 

The galactic latitude b = -38 deg., longitude l = 297 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1435444

We obtain a following upper limits.  

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

      74 | 2020-09-07 22:58:37 |         MASTER-OAFA | (01h 55m 11.92s , -77d 24m 44.7s) |   C |    10 | 15.8 |        
     179 | 2020-09-07 23:00:12 |         MASTER-OAFA | (01h 55m 35.91s , -76d 03m 45.6s) |   C |    30 | 16.8 |        
     231 | 2020-09-07 23:00:59 |         MASTER-SAAO | (02h 03m 44.94s , -77d 08m 12.6s) |   C |    40 | 19.3 |        
     231 | 2020-09-07 23:00:59 |         MASTER-SAAO | (02h 35m 28.31s , -77d 06m 11.2s) |   C |    40 | 19.5 |        
     255 | 2020-09-07 23:01:18 |         MASTER-OAFA | (02h 17m 07.16s , -77d 51m 43.1s) |   C |    50 | 16.2 |        
     296 | 2020-09-07 23:01:59 |         MASTER-SAAO | (02h 03m 51.69s , -77d 09m 14.7s) |   C |    50 | 19.5 |        
     296 | 2020-09-07 23:01:59 |         MASTER-SAAO | (02h 35m 37.20s , -77d 07m 12.5s) |   C |    50 | 19.6 |        
     342 | 2020-09-07 23:02:39 |         MASTER-OAFA | (02h 17m 29.35s , -76d 30m 31.9s) |   C |    60 | 17.1 |        
     375 | 2020-09-07 23:03:08 |         MASTER-SAAO | (02h 03m 45.07s , -77d 10m 17.2s) |   C |    70 | 19.6 |        
     375 | 2020-09-07 23:03:08 |         MASTER-SAAO | (02h 35m 32.76s , -77d 08m 14.1s) |   C |    70 | 19.7 |        
     441 | 2020-09-07 23:04:09 |         MASTER-OAFA | (02h 17m 11.19s , -77d 52m 09.7s) |   C |    80 | 16.9 |        
     486 | 2020-09-07 23:04:48 |         MASTER-SAAO | (02h 32m 06.95s , -77d 06m 18.4s) |   C |    90 | 19.7 |        
     486 | 2020-09-07 23:04:48 |         MASTER-SAAO | (02h 00m 23.44s , -77d 06m 45.2s) |   C |    90 | 19.7 |        
     563 | 2020-09-07 23:06:00 |         MASTER-OAFA | (02h 17m 26.50s , -76d 29m 44.2s) |   C |   100 | 17.6 |        
     605 | 2020-09-07 23:06:38 |         MASTER-SAAO | (02h 32m 02.21s , -77d 04m 44.4s) |   C |   110 | 19.9 |        
     605 | 2020-09-07 23:06:38 |         MASTER-SAAO | (02h 00m 23.10s , -77d 05m 11.5s) |   C |   110 | 19.9 |        
     707 | 2020-09-07 23:08:09 |         MASTER-OAFA | (02h 17m 47.88s , -79d 11m 04.3s) |   C |   130 | 17.1 |        
     745 | 2020-09-07 23:08:47 |         MASTER-SAAO | (02h 34m 29.36s , -78d 25m 33.1s) |   C |   130 | 20.1 |        
     745 | 2020-09-07 23:08:47 |         MASTER-SAAO | (01h 59m 12.63s , -78d 25m 58.6s) |   C |   130 | 20.1 |        
     884 | 2020-09-07 23:10:51 |         MASTER-OAFA | (02h 18m 18.57s , -77d 48m 52.0s) |   C |   160 | 18.0 |        
     909 | 2020-09-07 23:11:17 |         MASTER-SAAO | (02h 34m 30.87s , -78d 23m 59.1s) |   C |   160 | 20.1 |        
     909 | 2020-09-07 23:11:17 |         MASTER-SAAO | (01h 59m 18.43s , -78d 24m 25.3s) |   C |   160 | 20.3 |        
    1083 | 2020-09-07 23:14:00 |         MASTER-OAFA | (02h 17m 49.90s , -79d 12m 59.2s) |   C |   180 | 17.8 |        
    1099 | 2020-09-07 23:14:16 |         MASTER-SAAO | (02h 34m 26.50s , -78d 24m 41.3s) |   C |   180 | 20.2 |        
    1099 | 2020-09-07 23:14:16 |         MASTER-SAAO | (01h 59m 11.69s , -78d 25m 08.0s) |   C |   180 | 20.2 |        
    1298 | 2020-09-07 23:17:35 |         MASTER-OAFA | (02h 18m 17.36s , -77d 49m 41.9s) |   C |   180 | 18.5 |        
    1298 | 2020-09-07 23:17:36 |         MASTER-SAAO | (02h 34m 25.02s , -78d 23m 39.5s) |   C |   180 | 20.3 |        
    1298 | 2020-09-07 23:17:36 |         MASTER-SAAO | (01h 59m 13.37s , -78d 24m 06.7s) |   C |   180 | 20.3 |        
    1498 | 2020-09-07 23:20:55 |         MASTER-SAAO | (02h 34m 32.62s , -78d 24m 37.4s) |   C |   180 | 20.2 |        
    1498 | 2020-09-07 23:20:55 |         MASTER-SAAO | (01h 59m 18.34s , -78d 25m 04.9s) |   C |   180 | 20.3 |        
    1512 | 2020-09-07 23:21:09 |         MASTER-OAFA | (02h 17m 54.08s , -79d 11m 10.8s) |   C |   180 | 18.5 |        
    1697 | 2020-09-07 23:24:15 |         MASTER-SAAO | (02h 34m 27.96s , -78d 25m 35.1s) |   C |   180 | 20.3 |        
    1697 | 2020-09-07 23:24:15 |         MASTER-SAAO | (01h 59m 10.75s , -78d 26m 03.2s) |   C |   180 | 20.2 |        
    1728 | 2020-09-07 23:24:46 |         MASTER-OAFA | (02h 18m 14.46s , -77d 49m 22.9s) |   C |   180 | 18.5 |        
    1842 | 2020-09-07 23:27:40 |         MASTER-SAAO | (02h 25m 47.29s , -76d 02m 26.8s) |   C |    60 | 19.5 |        
    1842 | 2020-09-07 23:27:40 |         MASTER-SAAO | (01h 56m 26.65s , -76d 02m 58.5s) |   C |    60 | 19.6 |        
    1922 | 2020-09-07 23:28:59 |         MASTER-SAAO | (02h 49m 55.80s , -78d 00m 43.0s) |   C |    60 | 19.5 |        
    1922 | 2020-09-07 23:28:59 |         MASTER-SAAO | (02h 15m 51.06s , -78d 01m 13.2s) |   C |    60 | 19.7 |        
    2081 | 2020-09-07 23:31:39 |         MASTER-SAAO | (01h 32m 21.36s , -78d 01m 20.6s) |   C |    60 | 19.5 |        
    2641 | 2020-09-07 23:40:58 |         MASTER-SAAO | (02h 25m 38.90s , -76d 02m 34.7s) |   C |    60 | 19.5 |        
    2641 | 2020-09-07 23:40:58 |         MASTER-SAAO | (01h 56m 17.85s , -76d 03m 08.1s) |   C |    60 | 19.7 |        
    2721 | 2020-09-07 23:42:18 |         MASTER-SAAO | (02h 49m 56.97s , -78d 01m 56.9s) |   C |    60 | 19.6 |        
    2721 | 2020-09-07 23:42:18 |         MASTER-SAAO | (02h 15m 48.99s , -78d 02m 29.5s) |   C |    60 | 19.7 |        
    2880 | 2020-09-07 23:44:58 |         MASTER-SAAO | (01h 32m 19.62s , -78d 03m 03.1s) |   C |    60 | 19.5 |        
    2960 | 2020-09-07 23:46:17 |         MASTER-SAAO | (01h 50m 56.24s , -80d 01m 02.0s) |   C |    60 | 19.5 |        
    3130 | 2020-09-07 23:49:07 |         MASTER-SAAO | (02h 47m 32.47s , -80d 03m 50.6s) |   C |    60 | 19.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200907B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28391
SUBJECT: GRB 200907B: Enhanced Swift-XRT position
DATE:    20/09/08 00:36:18 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 742 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200907B, 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 = 89.02906, +6.90625 which is equivalent
to:

RA (J2000): 05h 56m 6.97s
Dec (J2000): +06d 54' 22.5"

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: GRB200907B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28392
SUBJECT: Swift GRB 200907B: Global MASTER-Net observations report 
DATE:    20/09/08 01:15:06 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 200907B ( A. P. Beardmore et al., GCN 28384) errorbox  22142 sec after notice time and 22169 sec after trigger time at 2020-09-08 01:00:40 UT, with upper limit up to  17.6 mag. The observations began at zenith distance = 59 deg. The sun  altitude  is -23.0 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 200907B errorbox  22375 sec after notice time and 22402 sec after trigger time at 2020-09-08 01:04:33 UT, with upper limit up to  15.9 mag. The observations began at zenith distance = 73 deg. The sun  altitude  is -46.6 deg. 

The galactic latitude b = -8 deg., longitude l = 201 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1435309

We obtain a following upper limits.  

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

   22260 |      MASTER-Tavrida |   C |   180 | 17.3 |        
   22461 |      MASTER-Tavrida |   C |   180 | 17.6 |        
   22493 |         MASTER-SAAO |   C |   180 | 15.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200907B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28393
SUBJECT: GRB 200907B: MITSuME Okayama optical upper limits
DATE:    20/09/08 01:35:11 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

R. Hosokawa, K. L. Murata, R. Adachi, M. Niwano, F. Ogawa, N.
Nakamura, N. Ito, S. Ogata, H. Takamatsu, H. Hara, Y. Yatsu, and N.
Kawai (TokyoTech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 200907B (Beardmore et al., GCN 28384;
Evans et al., GCN 28385,28391) 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 with a series of 60 sec exposures started at
2020-09âˆ’07 18:52:16UT. We did not find any new point sources within
the enhanced Swift/XRT error circle (Evans et al., GCN 28391) in the
60 sec exposure images and the stacked images. We obtained the 5-sigma
limits of the stacked images as follows.

T0+[sec] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
65 2020-09-07T19:19:48 2100 g'>17.1, Rc>17.9, Ic>17.3
------------------------------------------------------------------------------------------------
T0+: Elapsed time after the burst
T-EXP: Total Exposure time

We used the PS1 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., accepted
for publication in PASJ, https://arxiv.org/abs/2008.11486;
https://github.com/MNiwano/Eclaire).


GRB_name: GRB200907B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28394
SUBJECT: GRB 200907B: Swift-XRT refined Analysis
DATE:    20/09/08 01:38:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Capalbi (INAF-IASFPA), M. Perri (ASDC), V. D'Elia (ASDC), D.N.
Burrows (PSU), J. D. Gropp (PSU), J.A. Kennea (PSU), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester) and A.P. Beardmore report on
behalf of the Swift-XRT team:

We have analysed 6.7 ks of XRT data for GRB 200907B (Beardmore et al.
GCN Circ. 28384), from 83 s to 18.0 ks after the  BAT trigger. The data
comprise 5 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. 28385).

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.09 (+/-0.18).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.5, -0.4). The
best-fitting absorption column is  5.7 (+3.0, -1.4) x 10^21 cm^-2,
consistent with the Galactic value of 4.2 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.4 x 10^-11 (7.1 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.7 (+3.0, -1.4) x 10^21 cm^-2
Galactic foreground: 4.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.9 (+0.5, -0.4)

If the light curve continues to decay with a power-law decay index of
2.09, the count rate at T+24 hours will be 1.3 x 10^-6 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.8 x
10^-17 (9.2 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/00995004.

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


GRB_name: GRB200907B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28395
SUBJECT: GRB 200907B: AstroSat CZTI detection
DATE:    20/09/08 20:42:51 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed a weak detection of a short GRB 200907B, which was also detected by Swift (Beardmore A. et al., GCN #28384),  Swift-XRT (Evans P. et al., GCN #28385),  GROWTH-India optical (Kumar H. et al., GCN #28388), Global MASTER-Net (Lipunov V. et al., GCN #28392), and  MITSuME Okayama optical (Hosokawa R. et al., GCN #28393).

The source was clearly detected in the 40-200 keV energy range. The light curve showed a single peak of emission peaking at 2020-09-07 18:51:10.019 UT. The measured peak count rate associated with the burst is 160 +/- 24 cts/s above the background in the combined data of four quadrants, with a total of 259 +/- 3 cts. The local mean background count rate was 515+/- 1 cts/s. Using cumulative rates, we measure a T90 of 1.60 +/- 0.01 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed a single peak of emission peaking at 2020-09-07 18:51:09.00 UT. The measured peak count rate is 513 +/- 44 cts/s above the background in the combined Veto data of four quadrants, with a total of 560 +/- 5 cts. The local mean background count rate was 1494 +/- 2 cts/s. We measure a T90 of 1.48 +/- 0.06 s from the cumulative Veto light curve.

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: GRB200908A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28396
SUBJECT: GRB 200908A: Fermi GBM Final Real-time Localization
DATE:    20/09/08 21:24:52 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 SHORT GRB

At 21:15:41 UT on 8 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200908A (trigger 621292546.429748 / 200908886).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 169.5, Dec = -67.0 (J2000 degrees, equivalent to J2000 11h 18m, -67d 00'), with a statistical uncertainty of 9.2 degrees.

The angle from the Fermi LAT boresight is 16.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200908886/quicklook/glg_skymap_all_bn200908886.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/bn200908886/quicklook/glg_healpix_all_bn200908886.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200908886/quicklook/glg_lc_medres34_bn200908886.gif


GRB_name: GRB200903E
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28397
SUBJECT: Konus-Wind detection of GRB 200903E
DATE:    20/09/08 21:25:50 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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, very bright GRB 200903E
(AGILE detection: Ursi et al., GCN Circ. 28356;
AstroSat CZTI detection: Gupta et al., GCN Circ. 28367;
IPN triangulation: Hurley et al., GCN Circ. 28383)
triggered Konus-Wind at T0=9267.293 s UT (02:34:27.293).

The burst light curve shows a bright, multi-peaked structure
which started at ~T0-114.6 s and had a total duration of ~268.4 s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200903_T09267/

As observed by Konus-Wind, the burst
had a fluence of 4.84(-0.24,+0.23)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+20.464 s,
of 5.12(-0.57,+0.57)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+98.816 s)
is best fit in the 20 keV - 6 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.23(-0.03,+0.03),
the high energy photon index beta = -2.30(-0.14,+0.10),
the peak energy Ep = 413(-30,+33) keV
(chi2 = 100/74 dof).

The spectrum near the maximum count rate
(measured from T0+17.152 to T0+22.272 s)
is best fit in the 20 keV - 6 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.04(-0.05,+0.06),
the high energy photon index beta = -2.37(-0.35,+0.20),
the peak energy Ep = 717(-95,+106) keV
(chi2 = 74/71 dof).

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


GRB_name: GRB200907B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28398
SUBJECT: GRB 200907B: Swift-BAT refined analysis
DATE:    20/09/08 22:17:25 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J. R. Cummings (CPI),
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 200907B (trigger #995004)
(Beardmore et al., GCN Circ. 28384).  The BAT ground-calculated position is
RA, Dec = 89.019, 6.905 deg which is
   RA(J2000)  =  05h 56m 04.5s
   Dec(J2000) = +06d 54' 17.7"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.

The mask-weighted light curve shows a multi-peaked structure that
starts at ~T-0.6 and ends at ~T+0.3 s. The main peak occurs
at ~T+0.1 s. T90 (15-350 keV) is 0.83 +- 0.13 sec (estimated error
including systematics).

The time-averaged spectrum from T-0.64 to T+0.28 sec is best fit by
a simple power-law model.  The power law index of the time-averaged
spectrum is 0.68 +- 0.25.  The fluence in the 15-150 keV band
is 1.6 +- 0.2 x 10^-7 erg/cm2. The 1-sec peak photon flux measured
from T-0.68 sec in the 15-150 keV band is 1.5 +- 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/995004/BA/


GRB_name: GRB200908A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28399
SUBJECT: Fermi GRB 200908A: Global MASTER-Net observations report 
DATE:    20/09/08 23:00:29 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),

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) started inspect of the Fermi GRB 200908A ( Fermi GBM team, GCN 28396) errorbox  8 sec after notice time and 65 sec after trigger time at 2020-09-08 21:16:47 UT, with upper limit up to  18.3 mag. The observations began at zenith distance = 81 deg. The sun  altitude  is -57.5 deg. 

The galactic latitude b = -6 deg., longitude l = 294 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1436605

We obtain a following upper limits.  

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

      71 | 2020-09-08 21:16:47 |         MASTER-SAAO | (11h 55m 12.24s , -63d 29m 16.0s) |   C |    10 | 16.0 |        
      71 | 2020-09-08 21:16:47 |         MASTER-SAAO | (12h 11m 02.18s , -63d 28m 35.7s) |   C |    10 | 16.7 |        
     105 | 2020-09-08 21:17:16 |         MASTER-SAAO | (11h 55m 19.60s , -63d 30m 11.7s) |   C |    20 | 16.3 |        
     105 | 2020-09-08 21:17:16 |         MASTER-SAAO | (12h 11m 09.55s , -63d 29m 32.8s) |   C |    20 | 17.0 |        
     150 | 2020-09-08 21:17:56 |         MASTER-SAAO | (11h 55m 13.14s , -63d 31m 08.5s) |   C |    30 | 16.5 |        
     150 | 2020-09-08 21:17:56 |         MASTER-SAAO | (12h 11m 03.27s , -63d 30m 31.0s) |   C |    30 | 17.2 |        
     204 | 2020-09-08 21:18:45 |         MASTER-SAAO | (11h 55m 18.92s , -63d 30m 41.6s) |   C |    40 | 16.5 |        
     204 | 2020-09-08 21:18:45 |         MASTER-SAAO | (12h 11m 08.42s , -63d 30m 05.5s) |   C |    40 | 17.3 |        
     269 | 2020-09-08 21:19:45 |         MASTER-SAAO | (11h 55m 17.05s , -63d 29m 11.6s) |   C |    50 | 16.5 |        
     269 | 2020-09-08 21:19:45 |         MASTER-SAAO | (12h 11m 05.54s , -63d 28m 38.1s) |   C |    50 | 17.3 |        
     343 | 2020-09-08 21:20:54 |         MASTER-SAAO | (11h 55m 16.70s , -63d 30m 42.2s) |   C |    60 | 16.7 |        
     343 | 2020-09-08 21:20:54 |         MASTER-SAAO | (12h 11m 05.96s , -63d 30m 09.1s) |   C |    60 | 17.4 |        
     423 | 2020-09-08 21:22:14 |         MASTER-SAAO | (11h 53m 28.22s , -71d 52m 51.2s) |   C |    60 | 18.0 |        
     423 | 2020-09-08 21:22:14 |         MASTER-SAAO | (12h 16m 10.18s , -71d 51m 50.2s) |   C |    60 | 18.3 |        
     513 | 2020-09-08 21:23:44 |         MASTER-SAAO | (13h 02m 08.68s , -69d 51m 59.6s) |   C |    60 | 17.7 |        
     593 | 2020-09-08 21:25:04 |         MASTER-SAAO | (13h 05m 00.17s , -71d 49m 42.8s) |   C |    60 | 17.8 |        
     593 | 2020-09-08 21:25:04 |         MASTER-SAAO | (12h 42m 20.79s , -71d 50m 07.4s) |   C |    60 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200907B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28400
SUBJECT: GRB 200907B: Swift/UVOT Upper Limits
DATE:    20/09/09 03:50:55 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 200907B
84 s after the BAT trigger (Beardmore et al., GCN Circ. 28384).
No optical afterglow consistent with the XRT position
(Evans GCN Circ. 28385) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            84          233          147         >20.4
u_FC               296          546          246         >19.7
white               84         4892          383         >21.0
v                  625          819           39         >17.7
b                  551         4687          236         >19.4
u                  296         4482          462         >20.4
w1                 675         4277          216         >19.2
m2                 650          670           19         >18.3
w2                 601         5048          186         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.61 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200909A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28401
SUBJECT: GRB 200909A: Fermi GBM Final Real-time Localization
DATE:    20/09/09 04:11:29 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 04:01:22 UT on 9 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200909A (trigger 621316887.38726 / 200909168).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 338.9, Dec = -16.3 (J2000 degrees, equivalent to J2000 22h 35m, -16d 18'), with a statistical uncertainty of 5.2 degrees.

The angle from the Fermi LAT boresight is 104.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200909168/quicklook/glg_skymap_all_bn200909168.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/bn200909168/quicklook/glg_healpix_all_bn200909168.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200909168/quicklook/glg_lc_medres34_bn200909168.gif


GRB_name: GRB200909A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28402
SUBJECT: GRB 200909A: BALROG localization (Fermi Trigger 621316887 / GRB 200909168)
DATE:    20/09/09 04:21:57 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
621316887 at 04:01:22 on 09 Sept. 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) = 342.2+/-2.1 deg
Decl.(2000.0) = -17.8+/-2.6 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200909168/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200909168/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200909168/json

                        


GRB_name: GRB200909A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28403
SUBJECT: Fermi GRB 200909A: Global MASTER-Net observations report 
DATE:    20/09/09 05:19:40 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),

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) started inspect of the Fermi GRB 200909A ( Fermi GBM team, GCN 28401) errorbox  43 sec after notice time and 54 sec after trigger time at 2020-09-09 04:02:16 UT, with upper limit up to  15.4 mag. Observations started at twilight.  The observations began at zenith distance = 78 deg. The sun  altitude  is -10.0 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200909A errorbox  78 sec after notice time and 89 sec after trigger time at 2020-09-09 04:02:51 UT, with upper limit up to  17.2 mag. The observations began at zenith distance = 11 deg. The sun  altitude  is -63.4 deg. 

The galactic latitude b = -57 deg., longitude l = 46 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1436974

We obtain a following upper limits.  

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

      59 | 2020-09-09 04:02:16 |         MASTER-SAAO | (22h 42m 59.37s , -19d 50m 01.9s) |   C |    10 | 15.1 |        
      94 | 2020-09-09 04:02:45 |         MASTER-SAAO | (22h 42m 55.65s , -19d 48m 15.1s) |   C |    20 | 15.4 |        
      99 | 2020-09-09 04:02:51 |         MASTER-OAFA | (22h 39m 23.38s , -20d 28m 57.0s) |   C |    20 | 13.1 |        
     143 | 2020-09-09 04:03:30 |         MASTER-SAAO | (22h 42m 55.72s , -19d 49m 40.7s) |   C |    30 | 14.6 |        
     139 | 2020-09-09 04:03:31 |         MASTER-OAFA | (22h 39m 22.97s , -20d 27m 57.2s) |   C |    20 | 12.1 |        
     183 | 2020-09-09 04:04:10 |         MASTER-OAFA | (22h 39m 28.01s , -20d 28m 57.3s) |   C |    30 | 13.2 |        
     193 | 2020-09-09 04:04:20 |         MASTER-SAAO | (22h 42m 58.41s , -19d 48m 30.9s) |   C |    30 | 15.2 |        
     238 | 2020-09-09 04:05:00 |         MASTER-OAFA | (22h 39m 21.89s , -20d 29m 57.9s) |   C |    40 | 13.7 |        
     302 | 2020-09-09 04:05:59 |         MASTER-OAFA | (22h 39m 28.76s , -20d 29m 34.4s) |   C |    50 | 14.5 |        
     382 | 2020-09-09 04:07:08 |         MASTER-OAFA | (22h 39m 25.88s , -20d 28m 22.2s) |   C |    70 | 15.0 |        
     466 | 2020-09-09 04:08:38 |         MASTER-OAFA | (22h 36m 37.57s , -20d 46m 37.4s) |   C |    60 | 15.6 |        
     545 | 2020-09-09 04:09:57 |         MASTER-OAFA | (22h 37m 07.72s , -18d 46m 33.2s) |   C |    60 | 16.0 |        
     655 | 2020-09-09 04:11:17 |         MASTER-OAFA | (22h 34m 10.35s , -17d 03m 07.9s) |   C |   120 | 16.6 |        
     809 | 2020-09-09 04:13:36 |         MASTER-OAFA | (22h 34m 04.21s , -17d 04m 09.3s) |   C |   150 | 16.6 |        
     994 | 2020-09-09 04:16:26 |         MASTER-OAFA | (22h 34m 09.95s , -17d 04m 09.0s) |   C |   180 | 17.2 |        
    1193 | 2020-09-09 04:19:45 |         MASTER-OAFA | (22h 34m 07.04s , -17d 02m 18.3s) |   C |   180 | 16.5 |        
    1592 | 2020-09-09 04:26:24 |         MASTER-OAFA | (22h 47m 32.69s , -18d 34m 44.7s) |   C |   180 | 17.0 |        
    1792 | 2020-09-09 04:29:44 |         MASTER-OAFA | (22h 47m 25.82s , -18d 35m 41.9s) |   C |   180 | 16.4 |        
    1991 | 2020-09-09 04:33:03 |         MASTER-OAFA | (22h 47m 26.51s , -18d 34m 43.0s) |   C |   180 | 15.0 |        
    2191 | 2020-09-09 04:36:23 |         MASTER-OAFA | (22h 47m 32.60s , -18d 35m 44.5s) |   C |   180 | 16.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200829A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28404
SUBJECT: GRB 200829A: T100 observations
DATE:    20/09/09 08:28:19 GMT
FROM:    Massimiliano De Pasquale at Istanbul U/FOGTWA  <m.depasquale@ucl.ac.uk>

De Pasquale, M. (Istanbul Univ.) Sonbas, E. (Adiyaman Univ.), Ozdonmez, A., Er, H. (Ataturk Univ.), Ivantsov, A., (Akdeniz Univ.), Eryilmaz, S. (TUG) on behalf of a larger collaboration:

We observed the field of GRB 200829A (Siegel et al., GCN #28307) with the
1.0 meter T100 telescope (TUBITAK National Observatory, Antalya - Turkey),
starting on 2020-09-01, at 20:36:18 UT (~78 hours after the trigger). We obtained 12 x 300 s exposures with R filter under good weather conditions. The Moon was present in the sky during observations.

We do not detect an optical afterglow within the reported XRT error circle down to a 3 sigma limiting magnitude of 21 in the combined R band image.


We are grateful to the TUBITAK National Observatory staff for promptly scheduling the observations and their technical support.


GRB_name: GRB200909A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28405
SUBJECT: GRB 200909A: AstroSat CZTI detection
DATE:    20/09/09 14:31:28 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed a weak detection of a long GRB 200909A, which was also detected by Fermi GBM (GCN #28401), BALROG (Biltzinger B. et al., GCN #28402) and Global MASTER-Net (Lipunov V. et al., GCN #28403).

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 2020-09-09 04:01:27.86 UT. The measured peak count rate associated with the burst is 264 +/- 22 cts/s above the background in the combined data of four quadrants, with a total of 1437 +/- 20 cts. The local mean background count rate was 424 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 21.68 +/- 0.02 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-09-09 04:01:21.254 UT. The measured peak count rate is 354 +/- 45 cts/s above the background in the combined Veto data of four quadrants, with a total of 1126 +/- 32 cts. The local mean background count rate was 1744 +/- 1  cts/s. We measure a T90 of 21.12 +/- 0.01 s from the cumulative Veto light curve.

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: GRB200909B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28406
SUBJECT: GRB 200909B: Swift detection of a burst
DATE:    20/09/09 23:26:50 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB),
J. A. Kennea (PSU), N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
T. Sbarrato (INAF-OAB) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 23:17:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200909B (trigger=995288).  Swift did not slew to the
location due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 175.176, -31.179 which is 
   RA(J2000) = 11h 40m 42s
   Dec(J2000) = -31d 10' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single complex peak
structure with a duration of about 40 sec.  The peak count rate
was ~1500 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 03:23 UT on 2020 November 09. 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: GRB200909B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28408
SUBJECT: GRB 200909B: Swift-BAT refined analysis
DATE:    20/09/10 12:14:36 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

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),
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 200909B (trigger #995288)
(Melandri, et al., GCN Circ. 28406).  The BAT ground-calculated position is
RA, Dec = 175.171, -31.199 deg which is
    RA(J2000)  =  11h 40m 41.1s
    Dec(J2000) = -31d 11' 54.7"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
  
The mask-weighted light curve shows a single peak that stars at T-6 sec,
peaks at T+1 sec, and ends at T+20 sec.  A hint of an extended emission
is visible until T+40 sec.  T90 (15-350 keV) is 16.9 +- 2.2 sec (estimated error
including systematics).
  
The time-averaged spectrum from T-5.6 to T+14.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.60 +- 0.14.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.44 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/995288/BA/


GRB_name: GRB200907A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28409
SUBJECT: IPN triangulation of GRB 200907A (short)
DATE:    20/09/11 14:22:19 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@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. 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, D. Palmer, and A. Tohuvavohu
on behalf of the Swift-BAT team,

A. Ursi, F. Verrecchia, M. Tavani, N. Parmiggiani, C. Pittori,
A. Bulgarelli, on behalf of the AGILE Team, and

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

The short-duration GRB 200907A
(AGILE/MCAL detection: Ursi et al., GCN 28378)
was detected by AGILE (MCAL), Konus-Wind, INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND), and Swift (BAT) at about 51860 s UT (14:24:20).
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:
  141.475 (09h 25m 54s)  -1.433 ( -1d 26' 00")
 Corners:
  141.200 (09h 24m 48s)  -1.061 ( -1d 03' 41")
  141.151 (09h 24m 36s)  -1.497 ( -1d 29' 48")
  141.752 (09h 27m 01s)  -1.796 ( -1d 47' 45")
  141.799 (09h 27m 12s)  -1.366 ( -1d 21' 58")
 ---------------------------------------------
The error box area is 986 sq. arcmin, and its maximum
dimension is 55 arcmin (the minimum one is 24.5 arcmin).
The Sun distance was 26 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200907_T51859/IPN

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


GRB_name: GRB200826A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28410
SUBJECT: GRB 200826A: uGMRT radio upper limit at 1.25 GHz
DATE:    20/09/11 17:23:21 GMT
FROM:    Sonalika Purkayastha at NCRA-TIFR  <spurkayastha@ncra.tifr.res.in>

P. Chandra (NCRA-TIFR), S. Purkayastha (NCRA-TIFR), V. Bhalerao (IIT-B), 
H. Kumar (IIT-B),  M. Kasliwal (IPAC)

We observed the Fermi short GRB200826A (Fermi GBM Team GCN 28284; Mangan 
et al. GCN 28287) with the Giant Metrewave Radio Telescope (uGMRT), 
India, beginning 2020 September 9.53 UT (14.47 days after the burst) at 
a central frequency of 1.25 GHz. We report non-detection of radio 
afterglow from GRB200826A, with no evidence of radio emission above a 
3-sigma upper limit of 48.6 microJy/beam. The final image has a 
resolution of 4.13 arcsec by 1.65 arcsec at a position angle of 83.10 
degrees. We thank the staff of the GMRT that made these observations 
possible.


GRB_name: GRB200914A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28417
SUBJECT: GRB 200914A: Fermi GBM Final Real-time Localization
DATE:    20/09/14 12:59:03 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 12:48:30 UT on 14 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200914A (trigger 621780515.03441 / 200914534).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 256.4, Dec = -37.6 (J2000 degrees, equivalent to J2000 17h 05m, -37d 36'), with a statistical uncertainty of 1.8 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/2020/bn200914534/quicklook/glg_skymap_all_bn200914534.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/bn200914534/quicklook/glg_healpix_all_bn200914534.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200914534/quicklook/glg_lc_medres34_bn200914534.gif


GRB_name: GRB200914A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28418
SUBJECT: GRB 200914A: BALROG localization (Fermi Trigger 621780515 / GRB 200914534)
DATE:    20/09/14 13:19:09 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
621780515 at 12:48:30 on 14 Sept. 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) = 261.8+/-4.0 deg
Decl.(2000.0) = -35.8+/-2.0 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200914534/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200914534/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200914534/json

                        


GRB_name: GRB200914A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28419
SUBJECT: GRB 200914A : A long GRB detected by INTEGRAL
DATE:    20/09/14 13:32:19 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro.mereghetti@inaf.it>

S.Mereghetti (INAF, IASF-Milano), D.Gotz (CEA, Saclay),
C.Ferrigno, E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany
and ISDC, Versoix)
and J.Borkowski (CAMK, Torun) report:

a gamma ray burst lasting about 70 s has been detected by IBAS in the
IBIS/ISGRI data at 12:48:30  UT of 2020 September 14.

The refined coordinates (J2000) are:

R.A.=  254.512 deg
DEC.=  -36.2914 deg

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

The burst had a peak flux of about 2 counts/cm2/s (20-200 keV, 1-s
integration
time) and a fluence in the same energy range of about 3e-6  erg/cmq.

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


GRB_name: GRB200914A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28420
SUBJECT: GRB 200914A: Swift ToO observations
DATE:    20/09/14 14:36:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the INTEGRAL GRB 200914A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021033

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

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

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


GRB_name: GRB200914A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28424
SUBJECT: GRB 200914A: Fermi GBM observation
DATE:    20/09/15 02:33:43 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

R. Dunwoody (UCD), J. Mangan (UCD) and C. Meegan (UAH) report on
behalf of the Fermi GBM Team:

"At 12:48:30.03 UT on 14 September 2020, the Fermi Gamma-Ray Burst
Monitor (GBM) triggered and located GRB 200914A (trigger 621780515 /
200914534) which was also detected by INTEGRAL (S. Mereghetti et al.,
GCN 28419). The GBM on-ground location is consistent with the INTEGRAL
position. The on-ground calculated location, using the GBM trigger
data, is provided in GCN 28417.

The angle from the Fermi LAT boresight at the GBM trigger time is 62 degrees.

The GBM light curve shows a long GRB with multiple features with a
duration (T90) of about 65 s (50-300 keV). The time-averaged spectrum
from T0 + 1.1 s to T0 + 24.6 s is best fit by a power law function
with an exponential high-energy cutoff.  The power law index is -0.89
+/- 0.03 and the cutoff energy, parameterized as Epeak, is 1260 +/-
140 keV.

The event fluence (10-1000 keV) in this time interval is (9.80 +/-
0.71)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from
T0 + 1.95 s in the 10-1000 keV band is 7.9 +/- 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: GRB200914A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28425
SUBJECT: GRB 200914A: Swift-XRT observations
DATE:    20/09/15 09:57:10 GMT
FROM:    Paolo D'Avanzo at INAF - OAB  <paolo.davanzo@inaf.it>

M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J. D. Gropp
(PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), 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 INTEGRAL-detected
burst GRB 200914A (Mereghetti et al. GCN Circ. 28419), collecting 3.2
ks of Photon Counting (PC) mode data between T0+8.9 ks and T0+49.2 ks. 


One uncatalogued X-ray source has been detected consistent with being
within 148 arcsec of the INTEGRAL position, it is below the RASS limit
and shows no definitive signs of fading. Therefore, at the present time
we cannot confirm this as the afterglow. Details of this source are
given below:

Source 1:
  RA (J2000):  254.5202  =  16:58:4.84
  Dec (J2000): -36.2782  =  -36:16:41.6
  Error: 6.5 arcsec (radius, 90% conf.)
  Count-rate: (2.42 [+1.23, -0.93])e-3 ct s^-1  
  Distance: 53 arcsec from INTEGRAL position.
  Flux: (10.0 [+5.0, -3.8])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Within the 90% error circle of Source 1 we note the presence of a
relatively bright IR source reported in the 2MASS and AllWISE
catalogues (2MASS 16580467-3616436 / AllWISE J165804.63-361643.5).

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/00021033.

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


GRB_name: GRB200914A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28426
SUBJECT: GRB 200914A: AGILE detection
DATE:    20/09/15 14:09:50 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the long GRB 200914A, reported by Fermi-GBM
(GCNs #28417, #28424), INTEGRAL (GCN #28419), and Swift-XRT (GCN #28425) at
T0 = 2020-09-14 12:48:30 (UT).

The event is clearly visible in the scientific ratemeters of the SuperAGILE
(SA; 18-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and AntiCoincidence
(AC; 50-200 keV) detectors. The light curves show a double peaked time
profile, lasting about 17 s. The burst released 1510 counts in the SA
detector (above a background rate of 80 Hz), 22600 counts in the MCAL
detector (above a background rate of 1280 Hz), and 61510 counts in the AC
detector (above a background rate of 3720 Hz). The emission detected by the
MCAL and AC detectors starts about ~9 s after the T0. The initial part of
the burst detected by AGILE triggered also a MCAL high time resolution data
acquisition. The AGILE ratemeter light curves can be found at:
http://www.agilescienceapp.it/notices/GRB200914A_AGILE_RMs.png .

Additional analysis of AGILE data is in progress.


GRB_name: GRB200914A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28427
SUBJECT: Fermi GRB 200914A: Global MASTER-Net observations report 
DATE:    20/09/15 21:19:52 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),

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-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) started inspect of the Fermi GRB 200914A ( Fermi GBM team, GCN 28417) errorbox  38039 sec after notice time and 38210 sec after trigger time at 2020-09-14 23:25:20 UT, with upper limit up to  18.1 mag. Observations started at twilight.  The observations began at zenith distance = 20 deg. The sun  altitude  is -13.4 deg. 

The galactic latitude b =  2 deg., longitude l = 348 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1440752

We obtain a following upper limits.  

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

   38301 | 2020-09-14 23:25:20 |         MASTER-OAFA | (16h 56m 29.13s , -36d 56m 30.6s) |   C |   180 | 17.7 |        
   38481 | 2020-09-14 23:25:20 |         MASTER-OAFA | (16h 56m 29.13s , -36d 56m 30.6s) |   C |   540 | 18.0 |  Coadd 
   39111 | 2020-09-14 23:25:20 |         MASTER-OAFA | (16h 56m 29.13s , -36d 56m 30.6s) |   C |  1800 | 18.1 |  Coadd 
   38500 | 2020-09-14 23:28:40 |         MASTER-OAFA | (16h 56m 34.98s , -36d 57m 34.1s) |   C |   180 | 17.9 |        
   38700 | 2020-09-14 23:31:59 |         MASTER-OAFA | (16h 56m 29.91s , -36d 58m 36.1s) |   C |   180 | 17.9 |        
   38899 | 2020-09-14 23:35:19 |         MASTER-OAFA | (16h 56m 34.57s , -36d 58m 21.9s) |   C |   180 | 17.9 |        
   39079 | 2020-09-14 23:35:19 |         MASTER-OAFA | (16h 56m 34.57s , -36d 58m 22.0s) |   C |   540 | 18.1 |  Coadd 
   39099 | 2020-09-14 23:38:39 |         MASTER-OAFA | (16h 56m 32.35s , -36d 57m 01.7s) |   C |   180 | 18.0 |        
   39299 | 2020-09-14 23:41:58 |         MASTER-OAFA | (16h 56m 32.25s , -36d 58m 28.7s) |   C |   180 | 17.9 |        
   39498 | 2020-09-14 23:45:18 |         MASTER-OAFA | (16h 56m 35.42s , -36d 56m 54.9s) |   C |   180 | 18.0 |        
   39678 | 2020-09-14 23:45:18 |         MASTER-OAFA | (16h 56m 35.42s , -36d 56m 54.9s) |   C |   540 | 18.1 |  Coadd 
   39698 | 2020-09-14 23:48:37 |         MASTER-OAFA | (16h 56m 29.19s , -36d 57m 42.1s) |   C |   180 | 17.9 |        
   39897 | 2020-09-14 23:51:57 |         MASTER-OAFA | (16h 56m 28.00s , -36d 56m 42.3s) |   C |   180 | 17.9 |        
   40097 | 2020-09-14 23:55:16 |         MASTER-OAFA | (16h 56m 35.44s , -36d 57m 43.0s) |   C |   180 | 18.0 |        
   40277 | 2020-09-14 23:55:16 |         MASTER-OAFA | (16h 56m 35.44s , -36d 57m 43.0s) |   C |   540 | 18.1 |  Coadd 
   40296 | 2020-09-14 23:58:36 |         MASTER-OAFA | (16h 56m 27.73s , -36d 58m 42.5s) |   C |   180 | 18.0 |        
   40495 | 2020-09-15 00:01:55 |         MASTER-OAFA | (16h 56m 34.80s , -36d 58m 34.5s) |   C |   180 | 18.0 |        
   40695 | 2020-09-15 00:05:15 |         MASTER-OAFA | (16h 56m 31.42s , -36d 56m 51.9s) |   C |   180 | 18.0 |        
   40875 | 2020-09-15 00:05:15 |         MASTER-OAFA | (16h 56m 31.42s , -36d 56m 51.9s) |   C |   540 | 18.1 |  Coadd 
   40894 | 2020-09-15 00:08:34 |         MASTER-OAFA | (16h 56m 31.25s , -36d 58m 30.5s) |   C |   180 | 18.0 |        
   41094 | 2020-09-15 00:11:53 |         MASTER-OAFA | (16h 56m 33.29s , -36d 56m 54.6s) |   C |   180 | 18.0 |        
   41293 | 2020-09-15 00:15:13 |         MASTER-OAFA | (16h 56m 27.73s , -36d 57m 44.2s) |   C |   180 | 18.0 |        
   41473 | 2020-09-15 00:15:13 |         MASTER-OAFA | (16h 56m 27.73s , -36d 57m 44.2s) |   C |   540 | 18.1 |  Coadd 
   41493 | 2020-09-15 00:18:32 |         MASTER-OAFA | (16h 56m 26.87s , -36d 56m 44.4s) |   C |   180 | 18.0 |        
   41692 | 2020-09-15 00:21:52 |         MASTER-OAFA | (16h 56m 34.63s , -36d 57m 44.6s) |   C |   180 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200916A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28431
SUBJECT: GRB 200916A: Fermi GBM Final Real-time Localization
DATE:    20/09/16 19:38:48 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 19:28:39 UT on 16 Sep 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200916A (trigger 621977324.956902 / 200916812).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 41.5, Dec = -4.7 (J2000 degrees, equivalent to J2000 02h 46m, -4d 42'), with a statistical uncertainty of 8.0 degrees.

The angle from the Fermi LAT boresight is 96.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200916812/quicklook/glg_skymap_all_bn200916812.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/bn200916812/quicklook/glg_healpix_all_bn200916812.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200916812/quicklook/glg_lc_medres34_bn200916812.gif


GRB_name: GRB200916A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28432
SUBJECT: Fermi GRB 200916A: Global MASTER-Net observations report 
DATE:    20/09/16 20:15:35 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),

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) started inspect of the Fermi GRB 200916A ( Fermi GBM team, GCN 28431) errorbox  40 sec after notice time and 52 sec after trigger time at 2020-09-16 19:29:32 UT, with upper limit up to  17.7 mag. The observations began at zenith distance = 82 deg. The sun  altitude  is -37.6 deg. 

The galactic latitude b = -54 deg., longitude l = 179 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1443073

We obtain a following upper limits.  

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

      58 | 2020-09-16 19:29:32 |         MASTER-SAAO | (02h 12m 36.56s , -05d 40m 53.8s) |   C |    10 | 16.7 |        
      93 | 2020-09-16 19:30:02 |         MASTER-SAAO | (02h 12m 42.52s , -05d 40m 30.0s) |   C |    20 | 17.5 |        
     132 | 2020-09-16 19:30:42 |         MASTER-SAAO | (02h 12m 39.48s , -05d 39m 05.4s) |   C |    20 | 17.5 |        
     177 | 2020-09-16 19:31:21 |         MASTER-SAAO | (02h 12m 39.15s , -05d 40m 39.6s) |   C |    30 | 17.7 |        
     231 | 2020-09-16 19:32:11 |         MASTER-SAAO | (02h 12m 42.72s , -05d 39m 20.7s) |   C |    40 | 17.7 |        
     296 | 2020-09-16 19:33:10 |         MASTER-SAAO | (02h 12m 35.54s , -05d 39m 57.2s) |   C |    50 | 16.5 |        
     375 | 2020-09-16 19:34:20 |         MASTER-SAAO | (02h 14m 44.42s , -05d 38m 54.0s) |   C |    70 | 17.0 |        
    1734 | 2020-09-16 19:56:04 |         MASTER-SAAO | (02h 14m 46.30s , -05d 00m 42.7s) |   C |   180 | 17.5 |        
    1934 | 2020-09-16 19:59:23 |         MASTER-SAAO | (02h 14m 56.05s , -05d 01m 39.7s) |   C |   180 | 16.1 |        
    2134 | 2020-09-16 20:02:43 |         MASTER-SAAO | (02h 22m 52.09s , -05d 02m 38.3s) |   C |   180 | 16.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200917A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28435
SUBJECT: GRB 200917A: Swift detection of a burst
DATE:    20/09/17 04:05:53 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

E. Sonbas (Adiyaman Univ.), E. Ambrosi (INAF-IASFPA),
S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA), N. J. Klingler (PSU),
D. M. Palmer (LANL), B. Sbarufatti (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 03:52:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200917A (trigger=996184).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 235.753, -4.695 which is 
   RA(J2000)  =  15h 43m 01s
   Dec(J2000) = -04d 41' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with a duration of about 15 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 03:54:09.0 UT, 100.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 235.7247, -4.7011 which
is equivalent to:
   RA(J2000)  = 15h 42m 53.93s
   Dec(J2000) = -04d 42' 04.0"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 103 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 (1.49 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 5.6
(+5.36/-4.35) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 104 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
0.19. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.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: GRB200917A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28436
SUBJECT: GRB 200917A: Enhanced Swift-XRT position
DATE:    20/09/17 06:37:05 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 1697 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200917A, 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 = 235.72435, -4.70058 which is equivalent
to:

RA (J2000): 15h 42m 53.84s
Dec (J2000): -04d 42' 02.1"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB200916B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28440
SUBJECT: IPN triangulation of GRB 200916B (short)
DATE:    20/09/17 17:18:42 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

A. Ridnaia, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
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

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

A short-duration GRB 200916B
has been detected by Konus-Wind, INTEGRAL (SPI-ACS),
and Swift (BAT), so far, at about 56490 s UT (15:41:30).
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:
   224.729 (14h 58m 55s) -39.130 (-39d 07' 47")
  Corners:
   225.036 (15h 00m 09s) -37.463 (-37d 27' 46")
   225.754 (15h 03m 01s) -37.404 (-37d 24' 14")
   224.398 (14h 57m 35s) -40.797 (-40d 47' 48")
   223.640 (14h 54m 34s) -40.848 (-40d 50' 53")
  ---------------------------------------------
The error box area is 1.88 sq. deg, and its maximum
dimension is 3.8 deg (the minimum one is 32 arcmin).
The Sun distance was about 61 deg.

This box may be improved.

This burst is spatially and temporally inconsistent with the 
IceCube-200916A event.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200916_T56489/IPN/

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

The Swift (BAT) event data used for the IPN localization
came from the GUANO system (https://www.swift.psu.edu/guano/).


GRB_name: GRB200917A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28442
SUBJECT: Swift GRB 200917A: Global MASTER-Net observations report 
DATE:    20/09/17 17:29:54 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),

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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 200917A ( E. Sonbas et al., GCN 28435) errorbox  46136 sec after notice time and 46245 sec after trigger time at 2020-09-17 16:43:13 UT, with upper limit up to  15.9 mag. Observations started at twilight.  The observations began at zenith distance = 64 deg. The sun  altitude  is -10.4 deg. 

The galactic latitude b = 37 deg., longitude l =  2 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1443272

We obtain a following upper limits.  

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

   46335 |      MASTER-Tavrida |   C |   180 | 15.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200917A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28444
SUBJECT: GRB 200917A: Swift-XRT refined Analysis
DATE:    20/09/17 19:24:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.1 ks of XRT data for GRB 200917A (Sonbas et al. GCN
Circ. 28435), from 112 s to 34.8 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN Circ. 28436).

The late-time light curve (from T0+5.1 ks) can be modelled with a
power-law decay with a decay index of alpha=1.31 (+0.17, -0.16).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.34 (+0.28, -0.26). The
best-fitting absorption column is  1.08 (+0.25, -0.22) x 10^22 cm^-2,
in excess of 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 4.1 x 10^-11 (1.1 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.08 (+0.25, -0.22) x 10^22 cm^-2
Galactic foreground: 1.5 x 10^21 cm^-2
Excess significance: 7.0 sigma
Photon index:      2.34 (+0.28, -0.26)

If the light curve continues to decay with a power-law decay index of
1.31, the count rate at T+24 hours will be 5.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.1 x
10^-13 (5.5 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/00996184.

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


GRB_name: GRB200917A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28445
SUBJECT: Fermi-GBM Sub-Threshold Detection of GRB 200917A
DATE:    20/09/17 20:40:02 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

J. Wood (NASA/MSFC) reports on behalf of the Fermi-GBM Team:



Swift-BAT detected GRB 200917A at 03:52:28 UT (Sonbas et al. 2020, GCN 28435).

There was no Fermi-GBM onboard trigger around the event.

An automated, blind search for short gamma-ray bursts below the onboard triggering

threshold in Fermi-GBM also identified no counterparts.



The GBM targeted search [1], the most sensitive, coherent search for GRB-like

signals, was run from +/-30 s around BAT trigger time.

A transient source was identified whose most significant timescale according to

the automated search is 4.096 s, with a log likelihood ratio of 21. This timescale

corresponds to the first peak in the lightcurve, occurring -11 seconds before the

BAT trigger time. The full light curve consists of multiple peaks spanning from

approximately 11 seconds before to 10 seconds after the BAT trigger time.



The location is consistent with that from Swift-BAT.

The spectrum is consistent with a "normal" GRB template

(Band function with Epeak = 230 keV, alpha = -1.0, beta = -2.3).



[1] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB200917A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28447
SUBJECT: GRB 200917A: Swift-BAT refined analysis
DATE:    20/09/17 21:05:06 GMT
FROM:    Tilan Ukwatta at LANL  <tilan.ukwatta@gmail.com>

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),
E. Sonbas (Adiyaman Univ.), 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 200917A (trigger #996184)
(Sonbas, et al., GCN Circ. 28435).  The BAT ground-calculated
position is RA, Dec = 235.742, -4.695 deg which is
   RA(J2000)  =  15h 42m 58.0s
   Dec(J2000) = -04d 41' 41.4"
with an uncertainty of 2.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 96%.

The mask-weighted light curve shows two peaks, a weak peak
at ~T-10 s and a stronger peak at ~T+5 s. T90 (15-350 keV) is
19.4 +- 2.9 sec (estimated error including systematics).

The time-averaged spectrum from T-15.76 to T+6.18 sec is best
fit by a simple power-law model.  The power law index of the
time-averaged spectrum is 2.24 +- 0.31.  The fluence in the
15-150 keV band is 3.0 +- 0.6 x 10^-07 erg/cm2. The 1-sec peak
photon flux measured from T+5.04 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/996184/BA/


