# GCN_circulars

GRB_name: GRB211024A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31027
SUBJECT: GRB 211024A: 1.3m DFOT observations
DATE:    21/11/01 15:36:39 GMT
FROM:    Dimple Panchal at ARIES, India  <dimplepanchal96@gmail.com>

Ankur Ghosh, Rahul Gupta, Dimple, Amit Kumar, Amit Ror, Amar Aryan, Arvind
K. Dattatrey, Shubham Kishore, Tushar Tripathi, S. B. Pandey, and Kuntal
Misra (ARIES) report:

We observed GRB 211024A which was triggered by Fermi GBM (Fermi GBM Team,
GCN 30962), and further, follow up observations were carried out by
Swift/BAT-GUANO (A. Tohuvavohu et al., GCN 31006)), 0.7m GROWTH-India
Telescope (GIT, Kumar et al,. (GCN 31014)), using 1.3m Devasthal Fast
Optical Telescope (DFOT) located at Devasthal observatory of Aryabhatta
Research Institute of Observational Sciences (ARIES), India. Our
observation was carried out in two epochs. The first epoch observation was
started on 2021-10-26 at 16:22:24, i.e., ~2.62 DAYS post-Fermi trigger
whereas the second epoch observation was started on 2021-10-27 at 17:43:00,
i.e., ~3.68 days the Fermi trigger. Multiple frames in the R filter were
taken in both epochs.

In the first epoch, we started observing the location mentioned in
Swift/BAT-GUANO A. Tohuvavohu et al., (GCN 31006). But we found no
uncatalogued source within the error circle of ~ 6 arcmin up to 22.73 mag.

In the second epoch, we continued our observation for the 4th X-ray source
given by Swift-XRT ToO observations (M. Perri et al. GCN 31013) which were
assumed to be the afterglow of Fermi GBM GRB 211024A (GCN 30962), A.
Tohuvavohu et al., (GCN #31006), with 0.7m GROWTH-India Telescope (GIT,
Kumar, et al,. (GCN 31014)). We detected one source at R.A.= 1:52:46.98 ,
DEC.= -7:00:27.30 which is coincident with an X-ray source (#4) by
Swift-XRT ToO observations (M. Perri et al. GCN 31013. However, the source
is not variable during our observation period. Hence this is not the optical
counterpart of GRB 211024A. We quote an upper limit of 22.54 mag.

These magnitudes are not corrected for the Galactic extinction in the
direction of the burst. The standard stars from the USNO-B1.0 catalog was
used to get the calibrated magnitude.

This circular may be cited.


GRB_name: GRB211024B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31028
SUBJECT: GRB 211024B: Optical afterglow observation by Ondrejov D50
DATE:    21/11/01 21:12:09 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

M. Jelinek, J. Strobl, R. Hudec, C. Polasek (ASU CAS Ondrejov)
report:

We observed the position of the very long GRB 211024B (Gropp et al., GCN
30980, Lien et al. GCN 30989 and Evans et al. GCN 30994) with the D50
telescope of the Astronomical Institute Ondrejov, near Prague, Czech
Republic. We obtained a set of 175x 60s exposures in Sloan i' filter as
soon as the position became accessible above the local horizon, between
3.16 and 6.35h after the trigger.

The optical afterglow (Lipunov et al., GCN 30981; Zhu et al., GCN 30984;
Kann et al., GCN 30995; Kuin et al., GCN 31005) is clearly detected in
weight-combined images. In particular, we measure i'=19.94+/-0.11 in a
38x60s frame with an exposure mid time T0+0.152d. The calibration was done
against Atlas stars in the field.


GRB_name: GRB211102A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31029
SUBJECT: GRB 211102A: Fermi GBM Final Real-time Localization
DATE:    21/11/02 08:17:17 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 LONG GRB

At 08:06:03 UT on 2 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211102A (trigger 657533168.218864 / 211102338).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 30.8, Dec = 56.8 (J2000 degrees, equivalent to J2000 02h 03m, 56d 47'), with a statistical uncertainty of 4.1 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/2021/bn211102338/quicklook/glg_skymap_all_bn211102338.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211102338/quicklook/glg_healpix_all_bn211102338.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211102338/quicklook/glg_lc_medres34_bn211102338.gif


GRB_name: GRB211102A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31030
SUBJECT: GRB 211102A: BALROG localization (Fermi Trigger 657533168 / GRB 211102338)
DATE:    21/11/02 08:25:00 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
657533168 at 08:06:03 on 02 Nov. 2021 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) = 37.1+/-3.1 deg
Decl.(2000.0) = 52.5+/-2.3 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB211102338/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB211102338/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB211102338/json

                        


GRB_name: GRB211023B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31031
SUBJECT: GRB 211023B: MITSuME Akeno optical upper limits
DATE:    21/11/02 11:51:41 GMT
FROM:    Yuri Imai at Tokyo Inst of Tech  <imai@hp.phys.titech.ac.jp>

R. Hosokawa, Y. Imai, K. L. Murata, M. Niwano, Y. Takamatsu, N. Ito,
R. Noto, S. Sato, M. Takaku, R. Yamaguchi, Y. Yatsu, and N. Kawai
(TokyoTech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 211023B (S. Dichiara et al. GCN Circular
#30960, V. Lipunov et al. GCN Circular #30964, A.P. Beardmore et al.
GCN Circular #30966, A.P. Beardmore et al. GCN Circular #30967, A.
Pozanenko et al. GCN Circular #30972, Alan M. Watson et al. GCN
Circular #30973, N. P. M. Kuin et al. GCN Circular #30975, Y.-D. Hu et
al. GCN Circular #30976, S. Laha et al. GCN Circular #30979, D. A.
Kann et al. GCN Circular #30992, B. O'Connor et al. GCN Circular
#31000, J. Rastinejad et al. GCN Circular #31002, A. Pozanenko et al.
GCN Circular #31003, B. Grossan et al. GCN Circular #31016) with the
optical three color (g', Rc, and Ic) CCD cameras attached to the
MITSuME 50 cm telescope Akeno. The observation with a series of 60 sec
exposures started at 21-10-24 17:18:57 UT (20.2 hours after Swift
trigger). We stacked the images with good conditions. We did not
detect any uncatalogued sources within the UVOT error region (S.
Dichiara et al. GCN Circular #30960). We obtained the 5-sigma limits
of the stacked images as follows.

T0+[days] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
2.9 2021-10-26 19:25:18 2160 g'>19.5, Rc>19.6, Ic>18.7
3.9 2021-10-27 19:10:47 4020 g'>19.5, Rc>20.1, Ic>19.4
4.9 2021-10-28 19:02:53 7020 g'>19.8, Rc>20.1, Ic>19.3
5.9 2021-10-29 18:56:59 6120 g'>20.3, Rc>20.5, Ic>19.9
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time

We used 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. 2021, PASJ, Vol.73, Issue 1, Pages
4-24; https://github.com/MNiwano/Eclaire).


GRB_name: GRB211102B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31032
SUBJECT: GRB 211102B: Fermi GBM Final Real-time Localization
DATE:    21/11/02 14:16:38 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:05:35 UT on 2 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211102B (trigger 657554740.140466 / 211102587).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 300.9, Dec = -2.6 (J2000 degrees, equivalent to J2000 20h 03m, -2d 36'), with a statistical uncertainty of 1.8 degrees.

The angle from the Fermi LAT boresight is 64.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211102587/quicklook/glg_skymap_all_bn211102587.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211102587/quicklook/glg_healpix_all_bn211102587.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211102587/quicklook/glg_lc_medres34_bn211102587.gif


GRB_name: GRB211102B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31033
SUBJECT: GRB 211102B: BALROG localization (Fermi Trigger 657554740 / GRB 211102587)
DATE:    21/11/02 14:24:49 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
657554740 at 14:05:35 on 02 Nov. 2021 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) = 315.4+/-3.0 deg
Decl.(2000.0) = 1.5+/-1.5 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB211102587/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB211102587/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB211102587/json

                        


GRB_name: GRB211102A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31034
SUBJECT: Fermi GRB 211102A: Global MASTER-Net observations report 
DATE:    21/11/02 15:30:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211102A ( Fermi GBM team, GCN 31029) errorbox  26099 sec after notice time and 26125 sec after trigger time at 2021-11-02 15:21:29 UT, with upper limit up to  17.3 mag. Observations started at twilight.  The observations began at zenith distance = 56 deg. The sun  altitude  is -9.4 deg. 

The galactic latitude b = -4 deg., longitude l = 133 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1772827

We obtain a following upper limits.  

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

   26156 | 2021-11-02 15:21:29 |      MASTER-Tavrida | (02h 19m 20.35s , +52d 42m 02.2s) |   C |    60 | 17.2 |        
   26235 | 2021-11-02 15:22:48 |      MASTER-Tavrida | (02h 32m 24.06s , +52d 41m 08.7s) |   C |    60 | 17.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211102B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31035
SUBJECT: GRB 211102B: GECAM detection
DATE:    21/11/03 14:06:08 GMT
FROM:    Chao Zheng at IHEP  <zhengchao97@ihep.ac.cn>

J. C. Liu, S. Xiao, Yi Zhao, S. L. Xiong, C. Cai, J. J. He, Y. Huang, Z. W. Guo, 
C. Y. Li, X. B. Li, J. C. Liu, X. Y. Song, P. Wang, S. L. Xie, W. C. Xue,
Q. B. Yi, Y. Q. Zhang, G. Y. Zhao, X. Y. Zhao, C. Zheng, Y. Q. Du, D. Y. Guo, 
J. Liang, F. J. Lu, Q. Luo, X. Ma, W. X. Peng, R. Qiao, L. M. Song, J. Wang, H. Wu, 
C. W. Wang, P. Zhang, S. N. Zhang, X. L. Zhang, Z. Zhang, S. J. Zheng (IHEP),
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a 
long bright burst, GRB 211102B, at 2021-11-02T14:05:35.350 UTC (denoted as T0), 
which is also observed by Fermi/GBM (GCN #31033).

Its alert data was promptly downlinked to the ground through the short
message service of BeiDou Navigation Satellite System (BDS). The time
latency of the first BeiDou message relative to the trigger time is about 1 minute.

According to the BDS alert data, this burst mainly consists of multiple
pulses with duration of about 20 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/211102BLC.png

GECAM-B localized this burst to the following position (J2000): 
Ra: 298.1 deg 
Dec: -2.9 deg
Err: 2.4 deg (1-sigma,statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/20211102Bloc.png

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211024A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31037
SUBJECT: GRB 211024A: MITSuME Akeno optical observation
DATE:    21/11/04 06:14:14 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

Y. Imai, R. Hosokawa, K. L. Murata, N. Ito, Y. Takamatsu, M. Takaku, M.
Niwano, R. Noto, S. Sato, R. Yamaguchi, Y. Yatsu, and N. Kawai (TokyoTech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 211024A (The Fermi GBM team GCN Circular
#30962, V. Lipunov et al. GCN Circular #30963, S. Xiao et al. GCN Circular
#30974, Aaron Tohuvavohu et al. GCN Circular #31006, P. A. Evans et al. GCN
Circular #31007, S. Poolakkil et al. GCN Circular #31011, M. Perri et al.
GCN Circular #31013, H. Kumar et al. GCN Circular #31014, H. Kumar et al.
GCN Circular #31017) with the optical three color (g', Rc, and Ic) CCD
cameras attached to the MITSuME 50 cm telescope Akeno. The observation with
a series of 60 sec exposures was carried out from 2021-10-27 13:34:50 UT
(~3.5 days after the Fermi trigger) to 2021-10-31. We stacked the images
with good conditions.

We detected the Source 4 reported by the Swift ToO observation (Perri et
al. GCN Circular #31013) and performed aperture photometry. The magnitudes
of the Source 4 and the 5-sigma limits of the stacked images are as follows.

T0+[day] | MID-UT | T-EXP[sec] | Source 4 magnitude | 5-sigma limits
------------------------------------------------------------------------------------------------
3.6 | 2021-10-27 15:18:55 | 4200 | g'=19.2 +/- 0.2, Rc=18.2 +/- 0.1,
Ic=17.6 +/- 0.1| g'>19.9, Rc>20.4, Ic>19.8
4.4 | 2021-10-28 11:42:32 | 10380 | g'=19.3 +/- 0.2, Rc=18.2 +/- 0.1,
Ic=17.7 +/- 0.1 | g'>19.9, Rc>20.2, Ic>19.9
5.4 | 2021-10-29 11:41:30 | 9240 | g'=19.1 +/- 0.2, Rc=18.2 +/- 0.1,
Ic=17.6 +/- 0.1 |g'>19.8, Rc>20.4, Ic>19.9
6.4 | 2021-10-30 10:34:24 | 960 |g'=18.5 +/- 0.3, Rc=18.1 +/- 0.1, Ic=17.5
+/- 0.1 | g'>18.6, Rc>19.1, Ic>18.5
7.4 | 2021-10-31 10:41:48 | 540 | g' no detection, Rc=17.9 +/- 0.2, Ic=17.7
+/- 0.2 | g'>18.6, Rc>18.9, Ic>18.3
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used 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. 2021, PASJ, Vol.73, Issue 1, Pages
4-24; https://github.com/MNiwano/Eclaire).


GRB_name: GRB211023B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31038
SUBJECT: GRB 211023B: Subaru optical observation
DATE:    21/11/04 10:42:09 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

T. Sakamoto (AGU), G.S.H. Paek (SNU), Y. Urata (NCU),
E. Troja (NASA/GSFC), M. Im (SNU), K. Aoki (NAOJ)
report on behalf of Subaru GRB team:

We observed the field of GRB 211023B (Dichiara et al., GCN Circ. 30960)
with Hyper Suprime-Cam (HSC) on the Subaru 8.2 m telescope starting from
13:36 on October 28 about 4.7 days after the trigger.  Observations were
performed in the r filter for a total of 4800 s (32 x 150 s) exposure.

At a position consistent with the UVOT localization (Kuin & Dichiara, GCN Circ. 30975)
and the Legacy Survey object (Pozanenko et al. GCN 30972), we detect an optical
source with magnitude r~23.6 AB. Since the source appears clearly extended in our images
and its brightness is consistent with the Gemini-North observation (Rastinejad et al., GCN Circ. 31002),
archival HSC g-band images of March 2016, and CFHT archival r-band images of September 2020,
we conclude that the source detected by Subaru is dominated by the host galaxy contribution,
in agreement with Rastinejad et al. (GCN Circ. 31002).

We would like to thank the Subaru director, Dr. Michitoshi Yoshida for
approving our ToO, and Dr. Tsuyoshi Terai and Dr. Ichi Tanaka for supporting
our observation.


GRB_name: GRB211104A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31039
SUBJECT: GRB 211104A: Fermi GBM Final Real-time Localization
DATE:    21/11/04 18:56:35 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 18:46:10 UT on 4 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211104A (trigger 657744375.805276 / 211104782).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 16.9, Dec = 17.5 (J2000 degrees, equivalent to J2000 01h 07m, 17d 30'), with a statistical uncertainty of 22.2 degrees.

The angle from the Fermi LAT boresight is 45.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211104782/quicklook/glg_skymap_all_bn211104782.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211104782/quicklook/glg_healpix_all_bn211104782.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211104782/quicklook/glg_lc_medres34_bn211104782.gif


GRB_name: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31041
SUBJECT: GRB 211023A: continued 1.3m DFOT Optical Observations and possible jet break
DATE:    21/11/05 06:00:44 GMT
FROM:    Rahul Gupta at ARIES, India  <rahulbhu.c157@gmail.com>

Rahul Gupta, S. B. Pandey, Amit Ror, Amit Kumar, Dimple, Ankur Ghosh, Amar
Aryan, Bhavya, and Kuntal Misra (ARIES) report:

We further observed the bright GRB 211023A (Fermi GBM Team 2021, GCN
30958; Lesage et al. 2021, GCN 30965; N. Di Lalla et al. 2021, GCN
30961; Ursi et al. 2021, GCN 30969; and Ridnaia et al. 2021, GCN
31022) with 1.3m Devasthal Fast Optical Telescope (DFOT) located at
Devasthal observatory of Aryabhatta Research Institute of
Observational Sciences (ARIES), India, starting on 2021-10-29 at
19:19:13 UT, i.e., ~ 6.26 days after the Fermi trigger. We obtained 24
and 18 frames having an exposure time of 300 sec in the R and I
filters, respectively. We detected the optical afterglow of GRB
211023A (Lipunov et al. 2021, GCN 30970; Zhirkov et al. 2021, GCN
30977; Kann et al. 2021, GCN 30982; Hu et al. 2021, GCN 30990; Belkin
et al. 2021, GCN 31004, 31018, 31020; Vinko et al. 2021, GCN 31008;
and Kumar et al. 2021, GCN 31023) in our stacked images of both the
filters. The preliminary photometric estimate of the afterglow in the
R filter is following :


Date Start UT   T-T0 (mid, days) Filter  Exp time (sec)   Magnitude

=========================================================2021-10-29
19:19:13   ~6.28      R           300*24          22.58 +/- 0.33



Based on the preliminary photometry reported by using various
ground-based optical telescopes (Kann et al. 2021, GCN 30982; Hu et
al. 2021, GCN 30990; and Belkin et al. 2021, GCN 31004, 31018, 31020)
and our first epoch observations using 1.3m DFOT (Kumar et al. 2021,
GCN 31023), we measure the optical flux decay power-law index of the
afterglow light curve (Galactic extinction corrected) of GRB 211023A
equal to 1.49 +/- 0.04, consistent with those reported earlier (Belkin
et al. 2021, GCN 31004, 31020; and Vinko et al. 2021, GCN 31008).
However, we noticed that our second epoch observations are fainter
than the extrapolation of the early temporal decay index of ~1.5,
suggesting a possible break in the light curve. However, due to the
unavailability of near-simultaneous X-ray afterglow observations, we
could not confirm if this optical steeping is due to the jet break.
Further deeper and multiwavelength observations with larger telescopes
will be helpful to establish the possible jet break.

   The reported magnitude value is not corrected for the Galactic
extinction in the direction of the burst. Photometric calibration is
performed using the standard stars from the USNO-B1.0 catalog.

This circular may be cited.


GRB_name: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31042
SUBJECT: GRB 211023A: optical detection by SBT in Ondrejov
DATE:    21/11/05 07:08:47 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Jan Strobl, Martin Jelinek, Rene Hudec, Cyril Polasek (ASU CAS Ondrejov, CZ)

We observed the optical afterglow of The Fermi/GBM/AGILE GRB 211023A (Fermi
GBM team, GCN 30958, Di Lalla et al. GCN 30961, Lesage et al. GCN 30965,
Ursi et al. GCN 30969, Poolakkil GCNC 30998) with the double 20cm
wide-field Small Binocular Telescope (SBT, cf. Strobl et al., AN
340,7,p.633, 2019) in Ondrejov observatory starting October 25 at 1:19 UT,
36.2h after the GRB detection. The afterglow (Vladimirov et al. GCN 30970,
Tiurina et al. GCN 30977, Kann et al. GCN 30982, Hu et al.  GCN 30990,
Belkin et al. GCN 31004, Vinko et al. GCN 31008, Belkin et al. GCN 31018,
Belkin et al.  GCN 31020, Ghosh et al. GCN 31023) is well detected in our
2x80x120s coadded exposure from both tubes:

Tmid-T0   Texp    mag   dmag   filter
1.5706d  10762s  19.61  0.13   clear, calibrated as SDSS-r'(AB)


GRB_name: GRB211105A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31044
SUBJECT: GRB 211105A: AGILE detection of a burst
DATE:    21/11/05 10:06:12 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi, E. Menegoni (INAF/IAPS), C. Pittori, F. Verrecchia (SSDC, and
INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M.
Cardillo, C. Casentini, Y. Evangelista, L. Foffano, G. Piano (INAF/IAPS),
F. Lucarelli (SSDC, and INAF/OAR), A. Bulgarelli, A. Di Piano, 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 211105A at T0 = 2021-11-05
04:36:04 s (UTC).

The burst is clearly visible in the AGILE scientific ratemeters of the
SuperAGILE (SA; 20-60 keV) and MiniCALorimeter (MCAL; 0.4-100 MeV)
detectors. The event lasted about 100 s and it released a total number of
14900 counts in the SA detector (above a background rate of 105 Hz) and
133500 counts in the MCAL detector (above a background rate of 1240 Hz).
The AGILE ratemeter light curves can be found at
http://www.agilescienceapp.it/notices/GRB211105A_AGILE_RM.png

Additional analysis of AGILE data is in progress.


GRB_name: GRB211105A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31046
SUBJECT: GRB 211105A: GECAM detection
DATE:    21/11/06 01:59:33 GMT
FROM:    Guoying Zhao at IHEP  <gyzhao@ihep.ac.cn>

G. Y. Zhao, C. W. Wang, S. Xiao, Yi Zhao, S. L. Xiong, C. Cai, J. J. He, 
Y. Huang, Z. W. Guo, C. Y. Li, X. B. Li, J. C. Liu, X. Y. Song, P. Wang,
S. L. Xie, W. C. Xue, Q. B. Yi, Y. Q. Zhang,  X. Y. Zhao, C. Zheng,
Y. Q. Du, D. Y. Guo, J. Liang, F. J. Lu, Q. Luo, X. Ma, W. X. Peng,
R. Qiao, L. M. Song, J. Wang, H. Wu, P. Zhang, S. N. Zhang,
X. L. Zhang, Z. Zhang, S. J. Zheng (IHEP),report on behalf of GECAM team:


During the commissioning phase, GECAM-B was triggered in-flight by a 
long bright burst, GRB 211105A, at 2021-11-05T04:35:20.200 UTC (denoted as T0)

Its alert data was promptly downlinked to the ground through the short
message service of BeiDou Navigation Satellite System (BDS). The time
latency of the first BeiDou message relative to the trigger time is about 1 minute.

According to the BDS alert data, this burst mainly consists of multiple
pulses with duration of about 100 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_16-25-24_89786120.png

GECAM-B localized this burst to the following position (J2000): 
Ra: 81.93 deg 
Dec: -57.38 deg
Err: 1.27 deg (1-sigma,statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_skymap_bdm_89786120_V01.png

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211105A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31047
SUBJECT: GRB 211105A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/11/06 02:15:09 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (UAlabama), Aaron Tohuvavohu (U Toronto), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT did not trigger on GRB 211105A (T0: 2021-11-05T04:35:20.2
UTC, GECAM-B GCN #31046).

The GECAM notice, distributed in near real-time, triggered the Swift
Mission Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 16 in a 16.384
s analysis time bin. This is the maximum test duration of the search
pipeline. The full burst duration in the detector is greater than 60
s.

NITRATES prefers an origin for this burst coming from outside the
coded FOV, with DeltaLLHOut of -4.
An out of FOV origin is consistent with the GECAM localization.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211105A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31048
SUBJECT: GRB 211105A: MASTER optical inspection
DATE:    21/11/06 09:54:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E.Gorbovskoy, K.Zhirkov, N.Tiurina, P.Balanutsa, A.Kuznetsov, 
O.Gress,G.Antipov, D. Vlasenko, V.Senik,V.Topolev, A.Chasovnikov, E.Minkina,
V.Grinshpun, D.Cheryasov (Lomonosov MSU,SAI,PhysicsDepartment),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley (South African Astronomical Observatory),
N.M. Budnev (Irkutsk State University, API),
C.Francile, R. Podesta, F. Podesta (OAFA),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)

MASTER Global robotic net (MASTER-Net:http://observ.pereplet.ru Lipunov et al.,2010,Advances in Astronomy,2010,30L)
started inspect of GECAM GRB 211105A (Zhao et al. GCN 31046, R.A.Dec(2000)=81.93,-57.38 +-1.27d;
Ttrigger=2021-11-05T 04:35:20.200 UT, Tnotice=2021-11-06 01:59:33UT)
by MASTER-OAFA (Argentina) at 2021-11-06 07:10:26UT (1 day 9306s after trigger time)
with upper limit up to  19.7 mag.

The observations began at zenith distance = 26 deg. The sun  altitude  is -27.4 deg.
The galactic latitude b = -34 deg., longitude l = 266 deg.

Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1777102

We obtained the following upper limits.

Tmid-T0  |      Date Time      |          Site       |             Coord (J2000)          |Filt.| Expt. | Limit| Comment
    95796 | 2021-11-06 07:10:26 |         MASTER-OAFA | (05h 24m 16.75s , -56d 44m 09.4s) |   C |   180 | 18.5 |
    95996 | 2021-11-06 07:13:46 |         MASTER-OAFA | (05h 24m 22.29s , -56d 44m 03.5s) |   C |   180 | 18.8 |
    96176 | 2021-11-06 07:13:46 |         MASTER-OAFA | (05h 24m 22.29s , -56d 44m 03.5s) |   C |   540 | 19.7 |  Coadd
    96196 | 2021-11-06 07:17:05 |         MASTER-OAFA | (05h 24m 18.69s , -56d 42m 43.7s) |   C |   180 | 18.8 |
    96395 | 2021-11-06 07:20:25 |         MASTER-OAFA | (05h 24m 18.52s , -56d 44m 01.5s) |   C |   180 | 18.8 |
    96595 | 2021-11-06 07:23:44 |         MASTER-OAFA | (05h 24m 21.21s , -56d 42m 41.0s) |   C |   180 | 18.9 |
    96775 | 2021-11-06 07:23:44 |         MASTER-OAFA | (05h 24m 21.21s , -56d 42m 41.0s) |   C |   540 | 19.7 |  Coadd
    96794 | 2021-11-06 07:27:04 |         MASTER-OAFA | (05h 24m 15.79s , -56d 43m 26.0s) |   C |   180 | 18.9 |
    96993 | 2021-11-06 07:30:23 |         MASTER-OAFA | (05h 24m 14.75s , -56d 42m 26.5s) |   C |   180 | 18.9 |
    97193 | 2021-11-06 07:33:43 |         MASTER-OAFA | (05h 24m 21.18s , -56d 43m 26.8s) |   C |   180 | 19.0 |
Filter C is a clear (unfiltred) band.

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


GRB_name: GRB211106A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31049
SUBJECT: GRB 211106A: Swift/BAT-GUANO candidate arcminute localization of a short burst
DATE:    21/11/06 14:51:34 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), Gayathri Raman (PSU), James DeLaunay
(UAlabama), Jamie A. Kennea (PSU), report:

Swift/BAT did not trigger on GRB 211106A (T0: 2021-11-06T04:37:31.2
UTC, INTEGRAL/SPI-ACS #9504).

The INTEGRAL notice, distributed in near real-time, triggered the
Swift Mission Operations Center operated Gamma-ray Urgent Archiver for
Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).

Upon trigger by this notice, GUANO sent a command to the Swift Burst
Alert Telescope (BAT) to save 90 seconds of BAT event-mode data from
[-45,+45] seconds around the time of the burst. All the requested
event mode data was delivered to the ground.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), confidently detects the burst in a 0.512 s analysis
time bin with a sqrt(TS) of 19.1.
Estimated T90 in the detector is 1.75 +/- 0.05 s (15-350 keV).

A candidate localization is found with DeltaLLHOut of 7.2 and a
DeltaLLHPeak of 6.7.
For this reason we can confidently claim detection, and preference for
an in FOV origin, but the best fit arcmin localization is not strongly
preferred over other positions.
Conventional imaging does not find a location for this burst.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretations of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

The BAT position is
RA, Dec = 343.643 -53.236 deg which is
   RA(J2000)  = 22h 54m 34.32s
   Dec(J2000) =  -53d 14â€² 0.9â€³
with an estimated uncertainty of 7 arcmin.
The partial coding fraction at this position is 3.9%.

XRT and UVOT follow-up has been requested.
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: GRB211106A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31050
SUBJECT: GRB 211106A: Swift ToO observations
DATE:    21/11/06 15:31:53 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-GUANO GRB 211106A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021466

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-GUANO 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: GRB211106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31051
SUBJECT: GRB 211106A: Swift-XRT observations
DATE:    21/11/07 10:05:35 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 211106A, collecting 5.0 ks of Photon
Counting (PC) mode data between T0+39.2 ks and T0+58.2 ks. 

Eight uncatalogued X-ray sources have been detected, however none of
them is above the RASS limit or shows definitive signs of fading.
Therefore, at the present time we cannot identify which, if any, is the
afterglow. Details of these sources are given below:

Source 2:
  RA (J2000):  343.5852  =  22:54:20.45
  Dec (J2000): -53.2303  =  -53:13:49.0
  Error: 3.4 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (8.7 +/- 1.6)e-3 ct s^-1  
  Distance: 126 arcsec from Swift/BAT-GUANO position.
  Flux: (4.42 +/- 0.81)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 3:
  RA (J2000):  343.7780  =  22:55:6.71
  Dec (J2000): -53.3150  =  -53:18:53.9
  Error: 5.9 arcsec (radius, 90% conf.)
  Count-rate: (2.24 [+1.04, -0.81])e-3 ct s^-1  
  Distance: 406 arcsec from Swift/BAT-GUANO position.
  Flux: (9.8 [+4.5, -3.5])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 4:
  RA (J2000):  343.7223  =  22:54:53.36
  Dec (J2000): -53.1215  =  -53:07:17.5
  Error: 5.5 arcsec (radius, 90% conf.)
  Count-rate: (3.18 [+1.21, -0.98])e-3 ct s^-1  
  Distance: 445 arcsec from Swift/BAT-GUANO position.
  Flux: (1.42 [+0.54, -0.44])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

The source position is 1" away from an AGN candidate (Assef et al,
2018, ApJS, 234, 23; Guo et al., 2018, A&A, 618, 144). 

Source 5:
  RA (J2000):  343.6827  =  22:54:43.86
  Dec (J2000): -53.1372  =  -53:08:14.1
  Error: 5.8 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (5.5 +/- 1.5)e-3 ct s^-1  
  Distance: 365 arcsec from Swift/BAT-GUANO position.
  Flux: (2.23 +/- 0.59)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 6:
  RA (J2000):  343.7423  =  22:54:58.14
  Dec (J2000): -53.2260  =  -53:13:33.6
  Error: 7.3 arcsec (radius, 90% conf.)
  Count-rate: (1.62 [+0.86, -0.66])e-3 ct s^-1  
  Distance: 216 arcsec from Swift/BAT-GUANO position.
  Flux: (7.5 [+4.0, -3.0])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)
The source position is 7" away from an AGN candidate (Assef et al,
2018, ApJS, 234, 23). 

Source 7:
  RA (J2000):  343.7343  =  22:54:56.22
  Dec (J2000): -53.3579  =  -53:21:28.5
  Error: 6.0 arcsec (radius, 90% conf.)
  Count-rate: (2.98 [+1.18, -0.94])e-3 ct s^-1  
  Distance: 481 arcsec from Swift/BAT-GUANO position.
The source position is 5" away from an AGN candidate (Assef et al,
2018, ApJS, 234, 23). 

Source 8:
  RA (J2000):  343.7230  =  22:54:53.51
  Dec (J2000): -53.2861  =  -53:17:10.0
  Error: 6.9 arcsec (radius, 90% conf.)
  Count-rate: (2.72 [+1.12, -0.90])e-3 ct s^-1  
  Distance: 249 arcsec from Swift/BAT-GUANO position.
  Flux: (9.7 [+4.0, -3.2])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)
The source position is 9.5" away from an AGN candidate (Assef et al,
2018, ApJS, 234, 23).

Source 9:
  RA (J2000):  343.8707  =  22:55:28.96
  Dec (J2000): -53.2028  =  -53:12:10.2
  Error: 5.3 arcsec (radius, 90% conf.)
  Count-rate: (2.17 [+1.02, -0.79])e-3 ct s^-1  
  Distance: 504 arcsec from Swift/BAT-GUANO position.
  Flux: (6.3 [+3.0, -2.3])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

A catalogued source was also detected.

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/00021466.

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


GRB_name: GRB211107A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31052
SUBJECT: GRB 211107A: Fermi GBM Final Real-time Localization
DATE:    21/11/07 20:31:01 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 20:20:40 UT on 7 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211107A (trigger 658009245.216482 / 211107848).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 183.4, Dec = -61.2 (J2000 degrees, equivalent to J2000 12h 13m, -61d 12'), with a statistical uncertainty of 17.9 degrees.

The angle from the Fermi LAT boresight is 87.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211107848/quicklook/glg_skymap_all_bn211107848.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211107848/quicklook/glg_healpix_all_bn211107848.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211107848/quicklook/glg_lc_medres34_bn211107848.gif


GRB_name: GRB211023A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31053
SUBJECT: GRB 211023A: BTA spectroscopic redshift
DATE:    21/11/08 15:16:33 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), A. Moiseev (SAO RAS), A. Moskvitin (SAO RAS), E. 
Malygin (SAO RAS), S. Belkin (IKI, HSE), N. Pankov (IKI, HSE), V. Kim 
(HSE, FAI) on behalf of GRB IKI FuN, A. Rossi (INAF-OAS), D. A. Kann 
(HETH/IAA-CSIC) report:

We observed the afterglow of GRB 211023A (Zhirkov et al, GCN 30977, see 
also  Kann et al, GCN 30982; Hu et al,  GCN 30990; Belkin et al, GCN 
31004; Vinko et al, GCN 31008; Belkin et al, GCN 31018; Belkin et al, 
GCN 31020; Kumar et al, GCN 31023; Gupta et al., GCN 31041; Strobl et 
al., GCN 31042)  with BTA  SAO RAS telescope equipped with SCORPIO-2 
(VPHG940@600 grism). A total of 7200 s (6x1200 s) of spectra were 
obtained starting on 21-11-05 (UT) 20:50:00, i.e. approximately 13.3016 
days after burst. The afterglow is well detected in the acquisition 
imaging with R = 21.61 +/- 0.04 (3 x 90 sec. 21-11-05 (UT) 20:43:59 -- 
20:50:58), and a continuum is visible across the bandwidth of a spectrum 
4000 - 8500 A. The spectrum contain  significant emission lines H_beta, 
[OII] 3727, [OIII] 5007,  at a common redshift of z=0.390. We assume 
that the lines are from a host galaxy and, therefore, this is the 
redshift of GRB 211023A. No evident lines of a possible SN were found.

Calibration of photometry is preliminary and based on nearby stars of 
PS1 catalogue, gri -> R by Lupton transformations.

We are grateful to the directorate of SAO RAS for the TOO allocation.


GRB_name: GRB211106A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31054
SUBJECT: Konus-Wind detection of GRB 211106A
DATE:    21/11/08 16:39:58 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The short-duration GRB 211106A
(Swift/BAT-GUANO localization: Tohuvavohu et al., GCN 31049)
triggered Konus-Wind at T0=16652.485 s UT (04:37:32.485).

The burst light curve shows a single pulse
started at ~T0-0.3 s with a total duration of ~0.5 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/GRB211106_T16652/

As observed by Konus-Wind, the burst
had a fluence of 6.09(-1.22,+1.41)x10^-7 erg/cm2,
and a 16-ms peak flux, measured from T0+0.070 s,
of 3.37(-1.59,+1.68)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the burst
(measured from T0 to T0+0.192 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.02(-0.80,+1.13)
and Ep = 196(-45,+78) keV (chi2 = 27/23 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 27/22 dof).

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


GRB_name: GRB211106A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31055
SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 211106A
DATE:    21/11/08 19:01:41 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

C. Fletcher (USRA) reports on behalf of the Fermi-GBM Team:

Swift/BAT-GUANO detected GRB 211106A at 04:37:31.2 UT (GCN 31049).  This event
was also detected by INTEGRAL/SPI-ACS #9504 and Konus-Wind (GCN 31054). 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 identified no counterparts.

The GBM targeted search [1], the most sensitive, coherent search for
GRB-like signals identified a transient most significantly on the 0.256 s
timescale, with a location consistent with the Swift/BAT-GUANO event, using
the standard search protocol with a S/N of 22. This event was detected
 ~10 s after GBM exited SAA. The GBM targeted search event was found with
the highest significance with a "normal" spectrum (Band function with
Epeak = 230 keV, alpha = -1.0, beta = -2.3) for a GRB.

[1] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31056
SUBJECT: GRB 211023A: A BdHN of type I
DATE:    21/11/08 19:17:11 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

Y. Aimuratov, L. Becerra, C.L. Bianco, Y-C. Chen, C. Cherubini, S.
Eslamzadeh, S. Filippi, M. Karlica, Liang Li, G.J. Mathews, R. Moradi,
M. Muccino, G.B, Pisani, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet and ICRA-USTC
team, report:

The identification of the redshift z=0.36 of GRB 211023A (A. Pozanenko
et al. 2021, GCN 31053), with the isotropic energy of Eiso~6x10^52 erg
in 10-1000 keV (S. Lesage et al. 2021, GCN 30965, S. Poolakkil et al.
2021, GCN 30998), qualify GRB 211023A as a BdHN I, confirmed by the
observation of the GeV emission (N. Di Lalla et al. 2021, GCN 30961),
originated from the black hole (R. Ruffini et al. 2019 ApJ 886 82,
Moradi et al 2021. Phys. Rev. D 104, 063043) and the afterglow emission
(Jan Strobl et al. 2021 GCN 31042) originated from the newborn neutron
star (J.A. Rueda et al. 2020 ApJ 893 148).

Following Ruffini et al. 2021 (MNRAS, 504, 5301,
doi:10.1093/mnras/stab724) we indicate the appearance of the peak of
optical supernova to be observed at (18.4+/-2.6) days after the trigger
(November 10th 2021, uncertainty from November 8th 2021 to November
12th 2021), with the bolometric optical luminosity of
L=(9.0+/-2.7)x10^42 erg/s.

The follow-up optical observations for the SN are recommended.

-- 
Prof. Remo Ruffini
APS Fellow
Google Fellow
Director of ICRANet
Piazza della Repubblica 10
65122 Pescara (PE)  Italy
mobile: +39 339 4752566
Tel. Rome +39 06 49914304
Tel. Pescara +39 085 23054201
Fax: +39 085 4219252
e-mail: ruffini@icra.it


GRB_name: GRB211107B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31057
SUBJECT: GRB 211107B: Swift/BAT detection
DATE:    21/11/08 22:11:57 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Swift/BAT did not successfully trigger on GRB 211107B (T0: 2021-11-07
17:27:10 UTC).

Swift/BAT triggered in real-time onboard in the rates domain (trigger
#1082818), but no strong source was found to be associated in the
onboard imaging. This 'failed trigger' resulted in 10s of BAT TTE data
being saved and sent to the ground.

The duration of the burst, as seen by BAT, is ~15 seconds.

In ground analysis of the available TTE data, we find the position of
the burst with SNR 12.6 in the image domain.
The BAT position is
RA, Dec = 65.7949 -27.5524, which is:
    RA (J2000)     04h 23m 10.78s
    Dec (J2000)  -27d 33' 8.6"
with an estimated uncertainty of 2 arcminutes.

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


GRB_name: GRB211109A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31058
SUBJECT: GRB 211109A: Fermi GBM Final Real-time Localization
DATE:    21/11/09 00:50:08 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 00:39:44 UT on 9 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211109A (trigger 658111189.167684 / 211109028).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 129.1, Dec = -33.9 (J2000 degrees, equivalent to J2000 08h 36m, -33d 53'), with a statistical uncertainty of 5.5 degrees.

The angle from the Fermi LAT boresight is 49.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211109028/quicklook/glg_skymap_all_bn211109028.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211109028/quicklook/glg_healpix_all_bn211109028.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211109028/quicklook/glg_lc_medres34_bn211109028.gif


GRB_name: GRB211109A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31059
SUBJECT: Fermi GRB 211109A: Global MASTER-Net observations report 
DATE:    21/11/09 01:30:11 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211109A ( Fermi GBM team, GCN 31058) errorbox  2424 sec after notice time and 2450 sec after trigger time at 2021-11-09 01:20:34 UT, with upper limit up to  17.7 mag. The observations began at zenith distance = 75 deg. The sun  altitude  is -28.4 deg. 

The galactic latitude b =  4 deg., longitude l = 255 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1779459

We obtain a following upper limits.  

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

    2481 | 2021-11-09 01:20:34 |   MASTER-Kislovodsk | (08h 15m 26.97s , -30d 56m 58.4s) |   C |    60 | 16.8 |        
    2481 | 2021-11-09 01:20:34 |   MASTER-Kislovodsk | (08h 20m 10.07s , -31d 21m 55.0s) |   C |    60 | 17.6 |        
    2561 | 2021-11-09 01:21:55 |   MASTER-Kislovodsk | (08h 23m 30.65s , -29d 02m 47.5s) |   C |    60 | 16.9 |        
    2561 | 2021-11-09 01:21:55 |   MASTER-Kislovodsk | (08h 28m 08.95s , -29d 27m 41.8s) |   C |    60 | 17.7 |        
    2641 | 2021-11-09 01:23:15 |   MASTER-Kislovodsk | (08h 07m 46.58s , -32d 49m 13.3s) |   C |    60 | 16.6 |        
    2641 | 2021-11-09 01:23:15 |   MASTER-Kislovodsk | (08h 12m 34.87s , -33d 14m 11.3s) |   C |    60 | 17.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211109B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31060
SUBJECT: GRB 211109B: Fermi GBM Final Real-time Localization
DATE:    21/11/09 02:53:35 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 02:42:47 UT on 9 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211109B (trigger 658118572.33636 / 211109113).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 252.8, Dec = -45.1 (J2000 degrees, equivalent to J2000 16h 51m, -45d 06'), with a statistical uncertainty of 1.9 degrees.

The angle from the Fermi LAT boresight is 13.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211109113/quicklook/glg_skymap_all_bn211109113.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211109113/quicklook/glg_healpix_all_bn211109113.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211109113/quicklook/glg_lc_medres34_bn211109113.gif


GRB_name: GRB211107B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31061
SUBJECT: GRB 211107B: Swift ToO observations
DATE:    21/11/09 02:59:25 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 211107B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021467

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: GRB211109C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31062
SUBJECT: GRB 211109C: GECAM detection
DATE:    21/11/09 09:47:37 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, S. L. Xiong, S. Xiao, C. Cai, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu, S. L. Xie,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. Y. Li,
C. W. Wang, Q. B. Yi, B. X. Zhang, P. Zhang, W. X. Peng, R. Qiao, D. Y. Guo,
X. B. Li, X. Ma, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, J. J. He, 
G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang,
L. M. Song, F. J. Lu, S. N. Zhang (IHEP), report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long
burst, GRB 211109C, at 2021-11-09T07:51:02.200 UTC (denoted as T0).

GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 50 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_90143462.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 183.6 deg 
Dec: -55.9 deg
Err: 5.6 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_skymap_bdm_90143462_V01.png

Given that the location is consistent with the Galactic plane, we cannot rule
out the galactic origin of this burst.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31063
SUBJECT: MeerLICHT follow-up of GRB 211106A
DATE:    21/11/09 10:31:00 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

S. de Wet (UCT), P.M. Vreeswijk (Radboud), A.J. Levan (Radboud),

P.J. Groot (Radboud/UCT/SAAO) report on behalf of the MeerLICHT

consortium and the Stargate collaboration:


We observed the field of the Swift/BAT-GUANO short GRB candidate

GRB211106A (Tohuvavohu et al., GCN 31049) with the 0.6m wide-field

MeerLICHT optical telescope located at Sutherland, South Africa,

taking 10x60s exposures in the q-band starting at 2021-11-06,

18:37:17 UT, approximately 14 hours after the GRB trigger.


We co-added the images to reach a full-frame 5-sigma AB limiting

magnitude of q = 21.90. An archival reference image with limiting

magnitude of q = 20.54 was used to perform image subtraction

through our transient detection pipeline. The MeerLICHT field-of-view

fully covers the BAT-GUANO error box and includes all the X-ray

sources found through Swift-XRT follow-up observations

(D'Elia et al., GCN 31051).


Our transient pipeline finds 1 candidate in the BAT-GUANO error

box, at the same position as the XRT source coincident with a known

X-ray source. The coordinates of the transient coincide with a star

with brightness G = 17.49 in the Gaia EDR3 catalogue, spatially

very close to galaxy LEDA 432583. We believe the transient detection

is due to the star showing variable behaviour rather than a transient

in the galaxy, owing to an increase in brightness of the star from

q = 17.73 mag in the reference image to q = 17.47 in the new image.

We detect no source in our images at the position of the known X-ray

source 1RXS J225507.9-531312.


No other promising transient candidates are found in the error boxes

of the 9 XRT sources nor the BAT-GUANO error box, down to a transient

limiting magnitude of 20.34.


There is one other potential transient candidate in our FOV, but it

is 15.6â€™ away from the centre of the BAT-GUANO error box, so unlikely

to be associated with GRB 211106A. The coordinates are

RA, Dec (J2000) = 22:54:17.88, -52:58:35.22. The Legacy Survey DR9

images show a spiral galaxy at this position, which could be showing

variable behaviour or may be due to a transient near the galaxies' core.


MeerLICHT is built and run by a consortium consisting of Radboud

University, University of Cape Town, the South African Astronomical

Observatory, the University of Oxford, the University of Manchester

and the University of Amsterdam.


GRB_name: GRB211107B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31064
SUBJECT: GRB 211107B: Swift-XRT observations
DATE:    21/11/09 16:34:27 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-detected burst GRB 211107B (Swift/BAT did not successfully
trigger on GRB 211107B et al. GCN Circ. 31057), collecting 1.7 ks of
Photon Counting (PC) mode data between T0+124.3 ks and T0+131.0 ks. 

One uncatalogued X-ray source has been detected consistent with being
within 197 arcsec of the Swift/BAT 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):  65.80807  =  04:23:13.94
  Dec (J2000): -27.56097  =  -27:33:39.5
  Error: 2.9 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.0220 +/- 0.0042 ct s^-1   
  Distance: 52 arcsec from Swift/BAT position.
  Flux: (5.15 +/- 0.98)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

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/00021467.

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


GRB_name: GRB211107B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31065
SUBJECT: æœ±å­ä½© Autoreply: GRB 211107B: Swift-XRT observations
DATE:    21/11/09 16:48:44 GMT
FROM:    Zipei Zhu at NAOC  <zpzhu@nao.cas.cn>

604660733@qq.com


GRB_name: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31066
SUBJECT: GRB 211023A: SAO RAS optical observations
DATE:    21/11/09 17:32:28 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. S. Moskvitin and O. I. Spiridonova (SAO RAS),
on behalf of the GRB follow-up team report:

We observed the field of GRB 211023A (Fermi GBM team, GCN 30958,
Di Lalla et al. GCN 30961, Lesage et al. GCN 30965, Ursi et al.
GCN 30969, Poolakkil GCN 30998, Ridnaia et al., GCN 31022)
with the SAO RAS 1-m telescope Zeiss-1000 + CCD-photometer
on November 9. We obtained 6 x 300 sec. frames in Rc band
(00:25:41 -- 01:31:04 UT, T_mid-T0 = 16.4949 days) and 6 x 300 sec.
frames in Ic (00:31:28 -- 01:36:45 UT, T_mid-T0 = 16.4989 days).

The afterglow (Zhirkov et al. GCN 30977, Kann et al. GCN 30982,
Hu et al.GCN 30990, Belkin et al. GCN 31004, Vinko et al. GCN 31008,
Belkin et al. GCN 31018, Belkin et al.  GCN 31020, Amit Kumar et al.
GCN 31023, Rahul Gupta et al. GCN 31041, Strobl et al. GCN 31042,
Pozanenko et al. GCN 31053) is clearly detected in our stacked frames
with the following brightness: R = 21.69 +/- 0.09, I = 21.27 +/- 0.14
(the preliminary photometry is based on nearby stars of PS1 catalogue,
gri -> R and I by Lupton 2005 transformations).


GRB_name: GRB211109B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31067
SUBJECT: Fermi GRB 211109B: Global MASTER-Net observations report 
DATE:    21/11/09 19:30:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211109B ( Fermi GBM team, GCN 31060) errorbox  54876 sec after notice time and 54904 sec after trigger time at 2021-11-09 17:57:51 UT, with upper limit up to  18.0 mag. Observations started at twilight.  The observations began at zenith distance = 65 deg. The sun  altitude  is -9.9 deg. 

The galactic latitude b = -1 deg., longitude l = 341 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1779572

We obtain a following upper limits.  

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

   54934 | 2021-11-09 17:57:51 |         MASTER-SAAO | (16h 48m 34.14s , -48d 04m 20.4s) |   C |    60 | 15.9 |        
   55093 | 2021-11-09 18:00:30 |         MASTER-SAAO | (16h 35m 02.47s , -46d 10m 32.6s) |   C |    60 | 16.2 |        
   55174 | 2021-11-09 18:01:51 |         MASTER-SAAO | (16h 45m 21.48s , -46d 12m 01.6s) |   C |    60 | 16.4 |        
   55254 | 2021-11-09 18:03:11 |         MASTER-SAAO | (16h 57m 02.72s , -46d 12m 24.5s) |   C |    60 | 16.9 |        
   55334 | 2021-11-09 18:04:31 |         MASTER-SAAO | (16h 54m 46.77s , -44d 16m 48.5s) |   C |    60 | 16.4 |        
   55414 | 2021-11-09 18:05:51 |         MASTER-SAAO | (17h 05m 58.43s , -44d 18m 55.1s) |   C |    60 | 17.0 |        
   55497 | 2021-11-09 18:07:13 |         MASTER-SAAO | (16h 33m 34.54s , -44d 15m 37.0s) |   C |    60 | 16.6 |        
   55576 | 2021-11-09 18:08:33 |         MASTER-SAAO | (16h 44m 40.62s , -44d 16m 49.7s) |   C |    60 | 16.9 |        
   55656 | 2021-11-09 18:09:53 |         MASTER-SAAO | (16h 44m 00.25s , -42d 21m 44.9s) |   C |    60 | 16.6 |        
   55736 | 2021-11-09 18:11:13 |         MASTER-SAAO | (16h 54m 56.21s , -42d 23m 16.2s) |   C |    60 | 17.5 |        
   55818 | 2021-11-09 18:12:34 |         MASTER-SAAO | (16h 36m 29.90s , -48d 05m 21.8s) |   C |    60 | 16.8 |        
   55897 | 2021-11-09 18:13:54 |         MASTER-SAAO | (16h 48m 33.85s , -48d 05m 28.5s) |   C |    60 | 17.1 |        
   56057 | 2021-11-09 18:16:34 |         MASTER-SAAO | (16h 35m 00.32s , -46d 10m 50.7s) |   C |    60 | 17.2 |        
   56137 | 2021-11-09 18:17:53 |         MASTER-SAAO | (16h 45m 27.44s , -46d 10m 06.6s) |   C |    60 | 17.3 |        
   56216 | 2021-11-09 18:19:13 |         MASTER-SAAO | (16h 56m 56.95s , -46d 11m 12.3s) |   C |    60 | 18.0 |        
   56296 | 2021-11-09 18:20:33 |         MASTER-SAAO | (16h 54m 43.61s , -44d 16m 03.9s) |   C |    60 | 17.3 |        
   56376 | 2021-11-09 18:21:53 |         MASTER-SAAO | (17h 06m 01.81s , -44d 17m 36.5s) |   C |    60 | 17.9 |        
   56458 | 2021-11-09 18:23:15 |         MASTER-SAAO | (16h 33m 29.32s , -44d 16m 59.5s) |   C |    60 | 17.1 |        
   56538 | 2021-11-09 18:24:34 |         MASTER-SAAO | (16h 44m 46.14s , -44d 17m 19.4s) |   C |    60 | 17.4 |        
   56617 | 2021-11-09 18:25:54 |         MASTER-SAAO | (16h 44m 03.91s , -42d 21m 45.9s) |   C |    60 | 17.0 |        
   56697 | 2021-11-09 18:27:14 |         MASTER-SAAO | (16h 54m 53.35s , -42d 23m 25.3s) |   C |    60 | 17.9 |        
   56779 | 2021-11-09 18:28:36 |         MASTER-SAAO | (16h 36m 35.75s , -48d 03m 12.0s) |   C |    60 | 17.1 |        
   56859 | 2021-11-09 18:29:56 |         MASTER-SAAO | (16h 48m 28.07s , -48d 04m 33.7s) |   C |    60 | 17.3 |        
   57020 | 2021-11-09 18:32:37 |         MASTER-SAAO | (16h 35m 04.14s , -46d 09m 52.0s) |   C |    60 | 17.3 |        
   57100 | 2021-11-09 18:33:57 |         MASTER-SAAO | (16h 59m 21.15s , -48d 05m 37.2s) |   C |    60 | 17.6 |        
   57261 | 2021-11-09 18:36:38 |         MASTER-SAAO | (17h 07m 26.62s , -46d 10m 34.0s) |   C |    60 | 17.7 |        
   57820 | 2021-11-09 18:45:57 |         MASTER-SAAO | (17h 04m 42.08s , -42d 23m 48.3s) |   C |    60 | 17.3 |        
   58143 | 2021-11-09 18:51:19 |         MASTER-SAAO | (16h 59m 16.47s , -48d 03m 38.9s) |   C |    60 | 17.1 |        
   58303 | 2021-11-09 18:54:00 |         MASTER-SAAO | (17h 07m 20.70s , -46d 11m 59.8s) |   C |    60 | 17.5 |        
   58795 | 2021-11-09 19:02:12 |         MASTER-SAAO | (17h 04m 38.84s , -42d 23m 39.9s) |   C |    60 | 17.2 |        
   59119 | 2021-11-09 19:07:35 |         MASTER-SAAO | (16h 59m 23.14s , -48d 04m 21.3s) |   C |    60 | 17.0 |        
   59278 | 2021-11-09 19:10:15 |         MASTER-SAAO | (17h 07m 28.33s , -46d 11m 27.2s) |   C |    60 | 17.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211106A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31068
SUBJECT: GRB 211106A: Swift-XRT afterglow detection
DATE:    21/11/09 19:35:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has conducted further observations of the field of the
Swift/BAT-GUANO-detected burst GRB 211106A (Ridnaia et al. GCN Circ.
31054). The observations now extend from T0+39.3 ks to T0+290.7 ks. 

Of the sources reported by D'Elia et al. (GCN Circ. 31051), "Source 2"
is fading with 2.5 sigma significance and thus is believed to be the
GRB afterglow. Using 2766 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 = 343.58521,
-53.23028 which is equivalent to:

RA (J2000): 22h 54m 20.45s
Dec(J2000): -53d 13' 49.0"

with an uncertainty of 3.4 arcsec (radius, 90% confidence). This
position is 2.1 arcmin from the Swift/BAT-GUANO position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.7 (+0.5, -0.4).

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021466.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021466.

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


GRB_name: GRB211106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31069
SUBJECT: GRB 211106A, GROND observations
DATE:    21/11/09 22:36:52 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Klose (both TLS Tautenburg), and
A. Rau (MPE Garching) report:

We observed the field of the short GRB 211106A (Tohuvavohu et al., GCN
31049; D'Elia et al., GCN 31051; Ridnaia et al., GCN 31054; Fletcher,
GCN 31055; de Wet et al., GCN 31063) centered at the location of the
X-ray source #2 (D'Elia et al., GCN 31051, 31068) with GROND mounted
at the 2.2m MPG telescope at La Silla Observatory (Chile).

Inside the XRT error circle of 'Source #2' no object is detected.
At a midtime of November 9, 2021, 02:10 UT, we measure the following
3-sigma AB upper limits:

g' > 24.8,
r' > 25.0,
i' > 24.0,
z' > 22.0,
J  > 21.7,
H  > 21.1,
K  > 19.8.

Magnitudes are calibrated against the SkyMapper catalog (Wolf et
al., 2018, PASA 35, e010) in g'r'i'z' and 2MASS field stars in JHK
(Skrutskie et al., 2006, AJ 131, 1163).

We thank Paul Eigentaler for excellent support and for performing
the observations.


GRB_name: GRB211106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31070
SUBJECT: GRB 211106A: VLT/FORS2 optical observations
DATE:    21/11/09 23:17:48 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

Daniele B. Malesani (Radboud Univ. and DAWN/NBI), Paolo D'Avanzo 
(INAF/OABr), Andrew J. Levan (Radboud Univ.), Ana Nicuesa Guelbenzu (TLS 
Tautenburg), report on behalf of the Stargate consortium:


We observed the location of XRT source #2 (D'Elia et al., GCNs 31051, 
31068), indicated as the X-ray afterglow of the short GRB 211106A 
(Tohuvavohu et al., GCN 31049; Ridnaia et al., GCN 31054; Fletcher, GCN 
31055) using the ESO VLT UT1 equipped with the FORS2 camera. A total of 
20 minutes on source were obtained in the R band, with mid time 2021 Nov 
9.116 UT (that is, 2.92 days after the GRB).

No bright sources are detected inside the XRT error circle, down to R > 
26.2 (Vega, preliminary calibration based on faint USNO-B1 stars). 
However, there are two extended (FWHM ~ 2") objects at the following 
coordinates:

RA = 22:54:21.31
Dec = -53:13:47.2

RA = 22:54:20.29
Dec = -53:13:53.6

The second one is partially blended with a brighter star. These two 
galaxies are 7.9" and 4.8" away, respectively, from the center of the 
XRT position (which has currently a 90% uncertainty radius of 3.4"). A 
faint extension of the most nearby object, or a separate, very faint 
source, is also marginally detected inside the XRT error circle.


Should the GRB be associated with one of the closeby galaxies, this 
would indicate a relatively low redshift. Lacking a reference image, we 
cannot yet ascertain whether a faint transient could be present, 
superposed on top of the galaxy light. Chandra X-ray observations would 
help pinpoint the precise location of the source.


We acknowledge excellent support from the ESO staff at Paranal, still 
operating at reduced capacity because of the COVID pandemic, in 
particular Eleonora Sani, Aleksandra Solarz, Rodrigo Palominos, Pedro 
Figuera and Thomas Rivinius.


GRB_name: GRB211107A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31071
SUBJECT: GRB 211107A: GECAM detection
DATE:    21/11/10 07:26:02 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, S. L. Xiong, S. Xiao, C. Cai, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu, S. L. Xie,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. Y. Li,
C. W. Wang, Q. B. Yi, B. X. Zhang, P. Zhang, W. X. Peng, R. Qiao, D. Y. Guo,
X. B. Li, X. Ma, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, J. J. He, 
G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang,
L. M. Song, F. J. Lu, S. N. Zhang (IHEP), report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered on-ground by a weak burst, 
GRB 211107A, at 2021-11-07T20:20:40.220 UTC (denoted as T0),
which was also observed by Fermi/GBM (GCN #31052). 

According to the GECAM-B light curves in about 20-500 keV, 
this burst mainly consists of multiple pulses with a duration of 5 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_90015640_v01.PNG

GECAM location is consistent with the Fermi/GBM position within the error.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211107B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31072
SUBJECT: GRB 211107B: Swift-XRT afterglow detection
DATE:    21/11/10 11:36:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has conducted further observations of the field of the
Swift/BAT-detected burst GRB 211107B (Swift/BAT did not successfully
trigger on GRB 211107B et al. GCN Circ. 31057). The observations now
extend from T0+124.3 ks to T0+147.5 ks. The source previously reported
by D'Ai et al. (GCN Circ. 31064), "Source 1", is fading with 1.8 sigma
significance and thus is believed to be the GRB afterglow. Using 2958 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 = 65.80812, -27.56084 which is equivalent
to:

RA (J2000): 04h 23m 13.95s
Dec(J2000): -27d 33' 39.0"

with an uncertainty of 2.7 arcsec (radius, 90% confidence). This
position is 51 arcsec from the Swift/BAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.84 (+0.04, -2.67).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.5 (+0.9, -0.7). The
best-fitting absorption column is  1.6 (+2.5, -1.2) x 10^21 cm^-2,
consistent with the Galactic value of 4.3 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 2.7 x 10^-11 (4.5 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+2.5, -1.2) x 10^21 cm^-2
Galactic foreground: 4.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.5 (+0.9, -0.7)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021467.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021467.

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


GRB_name: GRB211110A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31074
SUBJECT: GRB 211110A: GECAM detection
DATE:    21/11/11 07:22:25 GMT
FROM:    Shenglun Xie at IHEP  <xiesl@ihep.ac.cn>

S. L. Xie, S. L. Xiong, S. Xiao, C. Cai, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu, Y. Q. Zhang,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. Y. Li,
C. W. Wang, Q. B. Yi, B. X. Zhang, P. Zhang, W. X. Peng, R. Qiao, D. Y. Guo,
X. B. Li, X. Ma, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, J. J. He, 
G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang,
L. M. Song, F. J. Lu, S. N. Zhang (IHEP), report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long
burst, GRB 211110A, at 2021-11-10T03:26:29.600 UTC (denoted as T0).

GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 15 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/multiLCvsE_2021-11-10T033A263A28.450.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 324.19 deg 
Dec: -3.15 deg
Err: 7.59 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_skymap_bdm_90213989_V01.png

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31075
SUBJECT: Short GRB 211106A: spectroscopy of galaxies in the field
DATE:    21/11/11 10:49:00 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

L. Christensen (DAWN/NBI), L. Izzo (DARK/NBI), P. Schady (Univ. Bath), 
D. B. Malesani (Univ. Radboud and DAWN/NBI), P. D'Avanzo (INAF/OABr), A. 
J. Levan (Radboud Univ.), S. Campana (INAF/OABr), D. Alexander Kann 
(HETH, IAA/CSIC), report on behalf of the Stargate consortium:

We observed the field surrounding the candidate afterglow (source #2) of 
the short GRB 211106A (Tohuvavohu et al., GCN 31049; D'Elia et al., GCNs 
31051, 31068) with the ESO VLT equipped with the MUSE panoramic 
integral-field spectrograph, covering a square 1'x1' region around the 
XRT position. Spectra of each spaxel cover the wavelength range 
4750-9350 AA. The mean time of our observation was November 10.03 UT 
(3.84 days after the GRB).

We report the redshift of three galaxies close to the XRT error circle 
(D'Elia et al., GCN 31068; see also Malesani et al., GCN 31070):

#1)
RA = 22:54:20.29
Dec = -53:13:53.6
z = 0.097 as inferred by the detection of the [O iii] doublet and Hbeta 
in emission.
The projected separation from the center of the XRT error circle is 
4.8", or 8.6 kpc at z = 0.097.

A bright, pointlike object (RA = 22:54:20.32, Dec = -53:13:56.7) is 
spatially blended with this galaxy, which we confirm to be a star thanks 
to the detection of Balmer and Ca II absorption at z = 0.

#2)
RA = 22:54:21.31
Dec = -53:13:47.2
z = 0.294 as inferred by the detection of the [O iii] doublet and Hbeta 
in emission.
The projected separation from the center of the XRT error circle is 
7.9", or 34.9 kpc at z = 0.294.

#3)
RA = 22:54:20.34
Dec = -53:13:40.8
z = 1.012 as inferred by the detection of the (resolved) [O ii] doublet 
in emission.
The projected separation from the center of the XRT error circle is 
8.3", or 67.0 kpc at z = 1.012.


While the association of these sources with GRB 211106A cannot be 
confirmed based on our data, object #1 has the smallest chance 
association probability. With R ~ 21.5, using the formula by Bloom et 
al. (2002, AJ, 123, 1111), we compute a chance association probability 
of ~5%.


Stacking the MUSE cube along the wavelength axis, faint emission is also 
detected inside the XRT error circle, consistent with our FORS2 image 
(Malesani et al., GCN 31070). The S/N is too low to extract any spectral 
information, and no emission lines are identified.


An image showing the position of the three galaxies can be viewed at the 
following link:

https://www.astro.ru.nl/~dmalesani/GRB/211106A/GRB211106A_galaxies.jpg


We acknowledge expert support from the observing staff at Paranal, in 
particular Thomas "Rivi" Rivinius, Thomas Wevers, Israel Blanchard, Juan 
Carlos Olivares, and Joe Anderson.


GRB_name: GRB211110A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31076
SUBJECT: GRB 211110A: AstroSat CZTI detection
DATE:    21/11/11 14:22:57 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), P. Sawant (IUCAA), G. Waratkar (IITB), A. Vibhute
(IUCAA), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao
(IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat
CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of a long GRB 211110A, which was
also detected by GECAM (S. L. Xie et al., GCN 31074).

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2021-11-10 03:26:29.0 UT. The measured peak count rate associated with
the burst is 59 (+23, -8) cts/s above the background in the combined
data of two quadrants, with a total of 529 (+170, -154) cts. The local
mean background count rate was 230 (+1, -2) cts/s. Using cumulative
rates, we measure a T90 of 14 (+6, -6) 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 2021-11-10 03:26:22.54 UT. The
measured peak count rate is 257 (+72, -44) cts/s above the background in
the combined Veto data of four quadrants, with a total of 1442 (+426,
-393) cts. The local mean background count rate was 1530 (+5, -6) cts/s.
We measure a T90 of 14 (+4, -5) 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 [1]. 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. 

Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB211112A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31077
SUBJECT: GRB 211112A: Fermi GBM Final Real-time Localization
DATE:    21/11/12 14:42:58 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:34:22 UT on 12 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211112A (trigger 658420467.373122 / 211112607).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 138.4, Dec = -2.5 (J2000 degrees, equivalent to J2000 09h 13m, -2d 30'), with a statistical uncertainty of 3.0 degrees.

The angle from the Fermi LAT boresight is 15.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211112607/quicklook/glg_skymap_all_bn211112607.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211112607/quicklook/glg_healpix_all_bn211112607.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211112607/quicklook/glg_lc_medres34_bn211112607.gif


GRB_name: GRB211106A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31078
SUBJECT: IPN triangulation of GRB 211106A (short)
DATE:    21/11/12 20:06:39 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

K. Hurley, on behalf of the IPN,

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

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

and

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

The short-duration GRB 211106A
(Swift-BAT-GUANO detection: Tohuvavohu et al., GCN 31049;
Konus-Wind detection: Ridnaia et al., GCN 31054;
Fermi-GBM sub-threshold detection: Fletcher et al., GCN 31055)
was detected by INTEGRAL (SPI-ACS), Swift (BAT), Konus-Wind,
and Fermi (GBM) at about 16651 s UT (04:37:31).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   342.487 (22h 49m 57s) -52.039 (-52d 02' 19")
  Corners:
   359.734 (23h 58m 56s) -61.384 (-61d 23' 04")
   333.528 (22h 14m 07s) -40.998 (-40d 59' 52")
   331.989 (22h 07m 57s) -42.431 (-42d 25' 51")
     0.415 (00h 01m 40s) -63.951 (-63d 57' 05")
  ---------------------------------------------
The error box area is 45.2 sq. deg, and its maximum
dimension is 27.7 deg (the minimum one is 1.7 deg).
The Sun distance was 95 deg.

The Swift-BAT position reported in Tohuvavohu et al.
is consistent with the IPN error box.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB211106_T16652/IPN/

The Swift (BAT) event data used for the IPN localization
came from the GUANO system (https://www.swift.psu.edu/guano/).


GRB_name: GRB211106A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31079
SUBJECT: GRB 211106A: Swift/UVOT upper limits
DATE:    21/11/12 22:27:08 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N Paul Kuin (UCL-MSSL) and Aaron Tohuvavohu (U Toronto) report on
behalf of the Swift/UVOT team:

The Swift/UVOT observed the field of the Swift/BAT-GUANO localisation (
Tohuvavohu et al, GCN Circ. 31049) of the INTEGRAL/SPI-ACS #9504 discovery
of the short GRB211106A  using the white filter. The GRB was also reported
by Fermi GBM (Fletcher, GCN Circ. 31055), Konus-Wind (Ridnaia et al.,
GCN Circ. 31054). Ground-based follow up on XRT Source 2 by MeerLicht
(de Wet et al, GCN Circ. 31063) at 17 hours past trigger found an upper
limit of q = 21.90; GROND around seventy hours after the trigger while
mounted on the 2.2m MPG telescope find upper limits only ranging from
g' > 24.8 to K > 19.8 (GCN Circ. 31069); Malesani et al used the VLT
UT1/FORS2 also at 70 hours after triggger to place a limit R > 26.2.

Here we report on upper limits for the XRT Source number 2 (see D'Elia et
al, GCN Circ. 31051) which is the candidate afterglow (D'Elia et al, GCN
Circ. 31068).

Swift UVOT observed discontinuously starting day 0.45-0.67d, then day
1.45-1.97, 2.6-3.7, 4.6-5.0 for a total of 19.5 ks. For these periods, the
3-sigma UVOT upper limits are white > 23.2, 22.4, 22.7, 22.9 mag (Vega,
Breeveld et al. 2011).

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: GRB211112A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31080
SUBJECT: Fermi GRB 211112A: Global MASTER-Net observations report 
DATE:    21/11/13 00:30:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211112A ( Fermi GBM team, GCN 31077) errorbox  31142 sec after notice time and 31169 sec after trigger time at 2021-11-12 23:13:52 UT, with upper limit up to  12.4 mag. Observations started at twilight.  The observations began at zenith distance = 52 deg. The sun  altitude  is -10.3 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 211112A errorbox  32320 sec after notice time and 32347 sec after trigger time at 2021-11-12 23:33:29 UT, with upper limit up to  18.6 mag. The observations began at zenith distance = 71 deg. The sun  altitude  is -37.3 deg. 

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 211112A errorbox  33146 sec after notice time and 33174 sec after trigger time at 2021-11-12 23:47:16 UT, with upper limit up to  18.9 mag. The observations began at zenith distance = 66 deg. The sun  altitude  is -50.7 deg. 

The galactic latitude b = 30 deg., longitude l = 234 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1783555

We obtain a following upper limits.  

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

   31200 | 2021-11-12 23:13:52 |        MASTER-Tunka | (09h 22m 36.19s , -00d 36m 07.1s) |   C |    60 | 12.4 |  Coadd 
   31600 | 2021-11-12 23:20:31 |        MASTER-Tunka | (09h 24m 18.50s , -04d 23m 10.4s) |   C |    60 | 12.3 |  Coadd 
   32378 | 2021-11-12 23:33:29 |         MASTER-SAAO | (09h 06m 42.71s , -06d 24m 07.7s) |   C |    60 | 17.5 |        
   32457 | 2021-11-12 23:34:49 |         MASTER-SAAO | (09h 14m 52.71s , -06d 24m 50.7s) |   C |    60 | 16.7 |        
   32537 | 2021-11-12 23:36:09 |         MASTER-SAAO | (09h 04m 58.14s , -04d 32m 08.9s) |   C |    60 | 17.6 |        
   32617 | 2021-11-12 23:37:29 |         MASTER-SAAO | (09h 13m 06.50s , -04d 31m 26.6s) |   C |    60 | 16.7 |        
   32696 | 2021-11-12 23:38:48 |         MASTER-SAAO | (09h 03m 52.74s , -02d 36m 31.4s) |   C |    60 | 17.1 |        
   32776 | 2021-11-12 23:40:08 |         MASTER-SAAO | (09h 11m 53.54s , -02d 37m 50.9s) |   C |    60 | 16.2 |        
   32936 | 2021-11-12 23:42:48 |         MASTER-SAAO | (08h 56m 37.29s , -02d 37m 25.4s) |   C |    60 | 17.3 |        
   33204 | 2021-11-12 23:47:16 |      MASTER-Tavrida | (09h 23m 44.30s , +01d 36m 12.8s) |   C |    60 | 18.0 |        
   33283 | 2021-11-12 23:48:35 |      MASTER-Tavrida | (09h 19m 08.04s , -06d 01m 46.7s) |   C |    60 | 17.9 |        
   33563 | 2021-11-12 23:53:15 |      MASTER-Tavrida | (09h 27m 15.72s , -05d 59m 49.1s) |   C |    60 | 17.7 |        
   33872 | 2021-11-12 23:58:23 |         MASTER-SAAO | (09h 03m 22.05s , -00d 43m 23.7s) |   C |    60 | 17.6 |        
   33951 | 2021-11-12 23:59:43 |         MASTER-SAAO | (09h 11m 17.81s , -00d 44m 08.8s) |   C |    60 | 17.6 |        
   34101 | 2021-11-13 00:02:13 |      MASTER-Tavrida | (09h 08m 59.29s , -02d 11m 53.4s) |   C |    60 | 18.2 |        
   34145 | 2021-11-13 00:02:57 |         MASTER-SAAO | (08h 57m 46.02s , -04d 31m 03.0s) |   C |    60 | 18.6 |        
   34180 | 2021-11-13 00:03:32 |      MASTER-Tavrida | (09h 15m 50.90s , +01d 35m 10.2s) |   C |    60 | 18.6 |        
   34225 | 2021-11-13 00:04:17 |         MASTER-SAAO | (09h 06m 44.08s , -06d 26m 14.6s) |   C |    60 | 18.6 |        
   34260 | 2021-11-13 00:04:51 |      MASTER-Tavrida | (09h 23m 44.59s , +01d 34m 16.7s) |   C |    60 | 18.7 |        
   34305 | 2021-11-13 00:05:37 |         MASTER-SAAO | (09h 14m 49.51s , -06d 24m 28.8s) |   C |    60 | 18.4 |        
   34339 | 2021-11-13 00:06:10 |      MASTER-Tavrida | (09h 19m 14.03s , -06d 01m 19.1s) |   C |    60 | 18.4 |        
   34385 | 2021-11-13 00:06:56 |         MASTER-SAAO | (09h 04m 56.29s , -04d 31m 20.6s) |   C |    60 | 17.2 |        
   34418 | 2021-11-13 00:07:29 |      MASTER-Tavrida | (09h 02m 10.72s , -04d 07m 53.5s) |   C |    60 | 18.7 |        
   34497 | 2021-11-13 00:08:48 |      MASTER-Tavrida | (09h 10m 14.75s , -04d 06m 18.1s) |   C |    60 | 18.7 |        
   34576 | 2021-11-13 00:10:07 |      MASTER-Tavrida | (09h 27m 11.10s , -06d 00m 33.3s) |   C |    60 | 18.5 |        
   34655 | 2021-11-13 00:11:26 |      MASTER-Tavrida | (09h 00m 34.13s , -00d 19m 08.6s) |   C |    60 | 18.5 |        
   34734 | 2021-11-13 00:12:46 |      MASTER-Tavrida | (09h 08m 27.76s , -00d 19m 58.1s) |   C |    60 | 18.7 |        
   34949 | 2021-11-13 00:16:21 |      MASTER-Tavrida | (09h 24m 13.75s , -02d 11m 37.0s) |   C |    60 | 18.7 |        
   35028 | 2021-11-13 00:17:40 |      MASTER-Tavrida | (09h 01m 06.74s , -02d 13m 06.9s) |   C |    60 | 18.5 |        
   35107 | 2021-11-13 00:18:59 |      MASTER-Tavrida | (09h 08m 59.53s , -02d 13m 55.5s) |   C |    60 | 18.7 |        
   35186 | 2021-11-13 00:20:18 |      MASTER-Tavrida | (09h 15m 50.44s , +01d 34m 17.3s) |   C |    60 | 18.9 |        
   35265 | 2021-11-13 00:21:37 |      MASTER-Tavrida | (09h 23m 47.45s , +01d 36m 01.0s) |   C |    60 | 18.7 |        
   35345 | 2021-11-13 00:22:56 |      MASTER-Tavrida | (09h 19m 12.54s , -06d 01m 18.0s) |   C |    60 | 18.5 |        
   35424 | 2021-11-13 00:24:16 |      MASTER-Tavrida | (09h 02m 13.88s , -04d 06m 07.5s) |   C |    60 | 18.8 |        
   35503 | 2021-11-13 00:25:35 |      MASTER-Tavrida | (09h 10m 10.03s , -04d 06m 55.9s) |   C |    60 | 18.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211023A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31081
SUBJECT: GRB 211023A: classification and SPI-ACS/INTEGRAL registration
DATE:    21/11/13 19:43:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

P. Minaev (IKI), A. Pozanenko (IKI), S. Grebenev (IKI), I. Chelovekov 
(IKI) report on behalf of GRB IKI FuN

We analyzed GRB 211023A (Di Lalla et al. GCN 30961; Lesage et al. GCN 
30965; Ursi et al. GCN 30969; Ridnaia et al. GCN 31022) using publicly 
available data of GBM/Fermi and SPI-ACS/INTEGRAL.

Using GBM/Fermi we clearly detect early emission, starting about 80 s 
before the GBM trigger. The extended emission (possibly associated with 
the activity detected by LAT, Di Lalla et al. GCN 30961, and/or its 
extremely bright afterglow, Zhirkov et al. GCN 30977; Kann et al. GCN 
30982) was also found, becoming dominant since approximately 150 s the 
trigger. Thus, a time profile consists of three episodes with a total 
burst duration of more than 300 s in GBM/Fermi (7 - 850 keV), while T90 
= 117 +/- 0.5 s. GRB 211023A was also registered by SPI-ACS/INTEGRAL 
with marginal detection of the early and the extended emission (T90 = 
120 +/- 9 s). Time profiles of GBM and SPI-ACS are presented at 
http://grb.rssi.ru/GRB211023A/GRB211023A_GBM_ACS_light_curve.png

We performed spectral analysis of the burst using GBM/Fermi data in the 
time interval of (-20, 160) s after the GBM trigger, covering the main 
part of GRB activity. The best parameters of Band model are following: 
Ep = 96 +/- 5 keV, alpha = -1.67 +/- 0.03, beta = -2.21 +/- 0.05 and 
fluence F = (1.341 +/- 0.004)*10^-4 erg/cm^2 in 10 - 1000 keV range. 
Assuming a redshift z = 0.390 (Pozanenko et al., GCN 31053) we estimated 
Eiso = (7.45 +/- 0.05)*10^52 erg in the 1 keV - 10 MeV energy band.

The position of the burst at Ep,i - Eiso and T90,i - EH diagram [1,2] is 
shown by black annuli at
http://grb.rssi.ru/GRB211023A/GRB211023A_Ep-Eiso_two_episodes_SN.png
and
http://grb.rssi.ru/GRB211023A/GRB211023A_EHD_two_episoses_SN.png

The position is typical for type II (long) GRBs, although it is in the 
lower bound of their 2 sigma correlation region. This is because of its 
relatively low value of the Ep,i parameter. Note that low values of Ep,i 
are typical for the nearby bursts (z < 0.5), associated with supernovae 
(shown by red annuli at
http://grb.rssi.ru/GRB211023A/GRB211023A_Ep-Eiso_two_episodes_SN.png
and
http://grb.rssi.ru/GRB211023A/GRB211023A_EHD_two_episoses_SN.png )

[1] - Minaev et al., MNRAS, 492, 1919, 2020
[2] - Minaev et al., Astronomy Letters, 46, 9, 573, 2020


GRB_name: GRB211115A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31082
SUBJECT: GRB 211115A: MAXI/GSC detection
DATE:    21/11/15 17:53:48 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

M. Serino (AGU), Y. Kawakubo (LSU),
H. Negoro, M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.),
T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU),
Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.),
M. Shidatsu (Ehime U.),
N. Kawai, M. Niwano, R. Hosokawa (Tokyo Tech),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, M. Kurihara (JAXA),
Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu, K. Inaba (Kyoto U.),
H. Tsunemi (Osaka U.),
M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/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 2021-11-15T16:31:19 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (122.977 deg, -25.709 deg) = (08 11 54, -25 42 32) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.13 deg and 0.11 deg, respectively.
The roll angle of long axis from the north direction is 61.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(122.347, -24.737) deg = (08 09 23, -24 44 13) (J2000)
(122.123, -24.889) deg = (08 08 29, -24 53 20) (J2000)
(123.589, -26.633) deg = (08 14 21, -26 37 58) (J2000)
(123.815, -26.479) deg = (08 15 15, -26 28 44) (J2000).
The X-ray flux averaged over the scan was 336 +- 35 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at 14:58 UT
with an upper limit of 20 mCrab.


GRB_name: GRB211115A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31084
SUBJECT: GRB 211115A: CALET Gamma-Ray Burst Monitor detection
DATE:    21/11/16 09:24:38 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 211115A (MAXI/GSC detection: Serino et al., GCN Circ. 31082;
Fermi-GBM trigger #658686687) was detected in ground analysis
of the CALET Gamma-ray Burst Monitor (CGBM) data near the MAXI trigger time
at 16:31:19 UTC on 15 November 2021.
The burst signal was weakly seen by all CGBM detectors.

The burst light curve shows a single pulse with a duration of ~10 sec.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1321029033/

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


GRB_name: GRB211107B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31086
SUBJECT: Konus-Wind detection of GRB 211107B
DATE:    21/11/16 14:29:21 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long-duration GRB 211107B
(Swift-BAT detection: Tohuvavohu, GCN Circ. 31057)
triggered Konus-Wind at T0=62836.647 s UT (17:27:16.647).

The burst light curve shows the initial pulse,
which starts at ~T0-3.7 s and has a total duration of ~24 s,
followed by a weaker emission seen up to T0+205 s.
The emission is seen up to ~1 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB211107_T62836/

As observed by Konus-Wind, the burst
had a fluence of 8.95(-1.76,+1.88)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.108 s,
of 1.42(-0.68,+0.69)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The spectrum of the initial pulse
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.88(-0.40,+0.47)
and Ep = 152(-26,+41) keV (chi2 = 51/56 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.7
(chi2 = 51/55 dof).

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


GRB_name: GRB211118A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31096
SUBJECT: GRB211118A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/11/19 15:52:44 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Gayathri Raman (PSU), James DeLaunay (UAlabama), Aaron Tohuvavohu (U
Toronto), Jamie A. Kennea (PSU) report:

Swift/BAT did not trigger on GRB 211118A (T0: 2021-11-18 23:38:14 UT,
Fermi Trigger: 658971499, INTEGRAL/SPI-ACS trigger 9523).

The Fermi + INTEGRAL triggers, distributed in near real-time,
triggered the Swift Mission Operations Center operated Gamma-ray
Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al.
2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 27.5 in a
1.024 s analysis time bin.
The estimated T90 in the detector is 3.0 +/- 0.05 s (15-350 keV)

NITRATES prefers an origin for this burst coming from outside the
coded FOV, with DeltaLLHOut of 2.7.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

An out of FOV origin is consistent with the Fermi/GBM localization.

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: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31098
SUBJECT: GRB 211023A: optical observations and photometric evidence of supernova
DATE:    21/11/20 14:54:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), I. Sokolov (INASAN, KIAM), E. 
Klunko (ISTP), A. S. Moskvitin (SAO RAS), V. Kim (HSE, FAI), V. 
Rumyantsev (CrAO),  R. Ya. Inasaridze (AbAO),  M. Krugov (FAI), D. 
Berezin (IC AMER NASU), G. Butenko (IC AMER NASU), N. Pankov (HSE), D. 
Datashvili (AbAO), V. R. Ayvazian (AbAO),  G. V. Kapanadze (AbAO) report 
  on behalf of GRB IKI FuN:

We observed the field of the GRB 211023A (Fermi GBM team, GCN 30958; Di
Lalla et al., GCN 30961; Lesage et al, GCN 30965; Ursi et al, GCN 30969;
Poolakkil, GCN 30998; Ridnaia et al., GCN 31022) with Zeiss-2000 and
Zeiss-600 telescopes of Terskol observatory, AZT-33IK telescope of Sayan
observatory (Mondy), AZT-20 telescope of Assy-Turgen observatory, ZTSh
2.6m-telescope of CrAO observatory, AS-32 telescope of AbAO observatory,
and Zeiss-1000 1-m telescope of SAO RAS. The optical counterpart
(Lipunov et al., GCN 30970; Zhirkov et al, GCN 30977; Kann et al, GCN
30982; Hu et al, GCN 30990; Belkin et al, GCN 31004; Vinko et al, GCN
31008; Belkin et al, GCN 31018; Belkin et al, GCN 31020; Kumar et al,
GCN 31023; Gupta et al., GCN 31041; Strobl et al., GCN 31042; Pozanenko
et al., GCN 31053; Moskvitin et al., GCN 31066) was detected in most of
the stacked images. A preliminary light curve based on our observations 
and GCN Circulars cited above can cab be found at

http://grb.rssi.ru/GRB211023A/GRB211023A_LC.png

Starting from the fifth day, a systematic flux excess over the
approximation of the afterglow by a single power law is observed. After 
subtraction of the afterglow approximated by the light curve with
a power law (Belkin et al, GCN 31020), and neglecting a contribution of
the host galaxy we determine a preliminary light curve of possible SN, see

http://grb.rssi.ru/GRB211023A/GRB211023A_AG_subtracted_LC.png

Using redshift of GRB 211023A (Pozanenko et al., GCN 31053)
we calculated an absolute magnitude at the maximum of the supposed
supernova (M_R=-19.9 +0.40 -0.29; adjusted by a Galactic extinction
(Schlafly & Finkbeiner, 2011)) and a time since the burst trigger in
the observer frame (t-T0 = 16.9+/-1.5). These parameters are in
agreement with parameters of known SN-GRB (e.g. see Figure 12 from 
Belkin et al., Astronomy Letters, 2020). The supernova associated with 
GRB 211012A is in agreement with early predictions (Kann et al, GCN 
30982; Aimuratov et al., GCN 31056; Minaev et al., GCN 31081).


GRB_name: GRB211118A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31099
SUBJECT: GRB 211118A: AstroSat CZTI detection
DATE:    21/11/20 18:21:36 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), P. Sawant (IUCAA), G. Waratkar (IITB), A. Vibhute
(IUCAA), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao
(IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat
CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of GRB 211118A, which was also
detected by Swift/BAT-GUANO (Raman et al., GCN 31096).

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2021-11-18 23:38:13.65 UT. The measured peak count rate associated with
the burst is 915 (+217, -92) cts/s above the background in the combined
data of two quadrants, with a total of 806 (+94, -109) cts. The local
mean background count rate was 446 (+7, -8) cts/s. Using cumulative
rates, we measure a T90 of 2.2 (+0.6, -0.4) s.

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

CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=grb [1]. 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.

  

Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB211120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31100
SUBJECT: GRB 211120A: GECAM detection
DATE:    21/11/21 09:11:34 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

C. Y. Li, S. L. Xie, S. L. Xiong, S. Xiao, C. Cai, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu, Y. Q. Zhang,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. W. Wang, 
Q. B. Yi, B. X. Zhang, P. Zhang, W. X. Peng, R. Qiao, D. Y. Guo,
X. B. Li, X. Ma, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, J. J. He, 
G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang,
L. M. Song, F. J. Lu, S. N. Zhang (IHEP), report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long
burst, GRB 211120A, at 2021-11-20T23:05:20.600 UTC (denoted as T0).

GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 6 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_91148720.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 304.99 deg 
Dec: 41.42 deg
Err: 1.34 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_skymap_bdm_91148720_V01.png

Given that the location is consistent with the Galactic plane, we cannot rule
out the galactic origin of this burst.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211120B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31101
SUBJECT: GRB 211120B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/11/21 14:44:02 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (UAlabama), Gayathri Raman (PSU), Aaron Tohuvavohu (U
Toronto), Jamie A. Kennea (PSU), report:

Swift/BAT did not successfully trigger on GRB 211120B (T0: 2021-11-20
13:09:46.8 UT, Fermi Trigger: 659106591).

The Fermi notice, distributed in near real-time, triggered the Swift
Mission Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 23.1 in a
8.192 s analysis time bin.
The estimated T90 in the detector is 24.5 s (15-350 keV).

NITRATES prefers an origin for this burst coming from outside the
coded FOV, with DeltaLLHOut of -6.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

An out of FOV origin is consistent with the Fermi/GBM localization.

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: GRB211120A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31104
SUBJECT: GRB 211120A: AstroSat CZTI detection
DATE:    21/11/23 05:52:20 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), P. Sawant (IUCAA), G. Waratkar (IITB), A. Vibhute
(IUCAA), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), A. R. Rao
(IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat
CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of a long GRB 211120A, which was
also detected by GECAM (Li et al., GCN 31100).

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2021-11-20 23:05:22.85 UT. The measured peak count rate associated with
the burst is 1756 (+251, -174) cts/s above the background in the
combined data of two quadrants, with a total of 2263 (+183, -134) cts.
The local mean background count rate was 443 (+4, -8) cts/s. Using
cumulative rates, we measure a T90 of 4.8 (+0.6, -0.2) s.

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

CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=grb [1]. 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. 

Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB211120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31105
SUBJECT: GRB 211120A: AGILE detection
DATE:    21/11/23 15:05:36 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), C. Pittori (SSDC, and INAF/OAR), A. Trois
(INAF/OA-Cagliari), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A.
Argan, M. Cardillo, C. Casentini, Y. Evangelista, E. Menegoni, L. Foffano,
G. Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and INAF/OAR), A.
Bulgarelli, A. Di Piano, V. Fioretti, F. Fuschino, N. Parmiggiani
(INAF/OAS-Bologna), M. Marisaldi (INAF/OAS-Bologna, and Bergen University),
M. Pilia (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 GRB 211120A at T0 = 2021-11-20 23:05:20
(UTC), reported by GECAM (GCN #31100) and AstroSat CZTI (GCN #31104).

The burst is clearly visible in the AGILE scientific ratemeters of the
SuperAGILE (SA; 20-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and
AntiCoincidence (AC; 50-200 keV) detectors. The event lasted about 6 s and
it released a total number of 821 counts in the SA detector (above a
background rate of 96 Hz), 9275 counts in the MCAL detector (above a
background rate of 1210 Hz), and 23969 counts in the AC detector (above a
background rate of 3440 Hz). The AGILE ratemeter light curves can be found
at http://www.agilescienceapp.it/notices/GRB211120A_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, covering the main peak of the burst, from T1 = 2021-11-20
23:05:20.0 s +/- 0.5 (UTC) to T2 = 2021-11-20 23:05:26.0 +/- 0.5 s (UTC),
and released 2291 counts in the detector, above a background rate of 710
Hz. The time-integrated spectrum of the burst between T1 and T1+2.43 s can
be fitted in the energy range 0.4-20 MeV with a single power-law with ph.
ind. = -2.43 (-0.34/+0.44), resulting in a reduced chi-squared of 1.09 (62
d.o.f.) and a fluence of 5.9e-06 ergs/cm^2 (90% confidence level), in the
same energy range. The MCAL light curve can be found at:
http://www.agilescienceapp.it/notices/GRB211120A_MCAL.png .

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. Please
note that in the MCAL notice #564534599 the T0 was affected by a temporal
shift of about +279 sec due to a temporary ground software problem now
solved.


GRB_name: GRB211023B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31107
SUBJECT: GRB 211023B: LBT likely spectroscopic redshift of the host galaxy
DATE:    21/11/23 16:00:07 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi, E. Palazzi, L. Amati, E. Pian (INAF-OAS), D. B. Malesani 
(Univ. Radboud and DAWN/NBI), S. Savaglio (UNICAL), P. D'Avanzo 
(INAF/OABr), and V. D'Elia (SSDC & INAF-OAR), M. De Pasquale (University 
of Messina),  report on behalf of the CIBO collaboration:

We report the results of the photometric and spectroscopic follow-up of 
the short GRB 211023B (Dichiara et al., GCN Circ. 30960) obtained with 
the Multi-Object Double Spectrographs (MODS) instrument mounted on the 
2x8.4-m LBT telescope (Mt Graham, AZ, USA). Data were obtained at the 
mid time of 12:40 UT on 2021-11-06, ~13.6 days after the burst trigger.

At the position of the UVOT localization (Kuin & Dichiara, GCN 30975) 
and the Legacy Survey object (Pozanenko et al., GCN 30972), we detect 
the GRB host galaxy (Sakamato et al. GCN 31038, Rastinejad et al. GCN 
31002). We measure the following AB magnitudes:
g = 24.02+-0.17
r = 23.99+-0.15
calibrated against Pan-STARRS field stars and not corrected for Galactic 
extinction.

Spectroscopy of the source was obtained for a total of 4550s, covering 
the wavelength range 3200-10000 AA.Continuum is faintly detected over 
the wavelength range 3200-10000 AA, and a single emission line is 
visible at ~6940 AA. The most likely interpretation is [O II] at z = 
0.862. At this redshift, [O III] would unfortunately fall on top of a 
region affected by sky lines, so its non-detection is not very 
constraining. Other interpretations are less likely. We can disregard 
Lyalpha, since there is no drop in the continuum blueward of the line. 
We deem Halpha unlikely, as the corresponding redshift z = 0.057 would 
imply an extremely faint host galaxy (absolute magnitude ~ -13), and we 
don't see the expected [O III] and Hbeta lines. The interpretation of 
the observed feature as [O III] 5008 seems to be also unlikely as we 
would expect to detect hints of [O III] 4959 as well as Halpha which 
would fall in a wavelength region clean of skylines.

Assuming the redshift z=0.862, standard cosmology (Planck 2016) and 
Swift/BAT refined and on-line automated spectral analysis (Laha et al., 
GCN 30979, and http://gcn.gsfc.nasa.gov/notices_s/1080859/BA/ 
<http://gcn.gsfc.nasa.gov/notices_s/1080859/BA/>) we estimate an 
isotropic-equivalent radiated energy Eiso (1-10000 keV) of about 
(0.9-1.2)x E^51 erg, which is typical of short GRBs. However, we note that:
a) despite its short duration, the burst has a rather soft spectrum 
(simple power with index ~2) which is consistent with a spectral peak 
energy Ep close to (or even below) the BAT low-energy threshold and 
would imply a rest-frame peak energy Ep,i < ~30-40 keV, thus locating 
this GRB in the region of the Ep,i - Eiso plane populated by long GRBs. 
The preliminary automatic modelling with a cut-off power-law or a Band 
function is consistent with a larger Ep,i, which would make this burst 
more similar to other short GRBs, but with a very large uncertainty.
b) the soft spectra and short duration put GRB 211023B closer to the 
region populated by long GRBs than to to the one populated by short 
events also in the HR-T90 diagram, even though it is still consistent 
with belonging to the tail of the distribution of short GRBs in this plane.

We acknowledge the excellent support from the LBTO and LBT-INAF staff, 
particularly O. Kuhn, S. Allanson, F. Cusano, S. Bisogni, and D. Paris, 
in obtaining these observations.


GRB_name: GRB211124A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31113
SUBJECT: GRB 211124A: Swift/BAT-GUANO detection of a short burst outside the coded FOV
DATE:    21/11/24 15:35:23 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (UAlabama), Aaron Tohuvavohu (U Toronto), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT did not successfully trigger on GRB 211124A (T0:
2021-11-24T02:29:53.5 UTC, Fermi/GBM #659413798).

The Fermi/GBM notice, distributed in near real-time, triggered the
Swift Mission Operations Center operated Gamma-ray Urgent Archiver for
Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 10.4 in a
0.512 s analysis time bin.
The estimated T90 in the detector is 0.4 +/- 0.2 s (15-350 keV).

NITRATES results are consistent with a burst coming from outside the
coded FOV, with DeltaLLHOut of 5.
An out of FOV origin is consistent with the Fermi/GBM localization.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211124A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31116
SUBJECT: IPN triangulation of GRB 211124A (short)
DATE:    21/11/24 20:09:59 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, D. Frederiks, A. Ridnaia,
A. Lysenko, 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,

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

and

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

The short-duration GRB 211124A
(Swift/BAT-GUANO detection: DeLaunay et al., GCN Circ. 31113)
has been detected by Fermi (GBM trigger 659413798),
Swift (BAT), INTEGRAL (SPI-ACS), and Konus-Wind in the waiting mode,
so far, at about 8994 s UT (02:29:54).
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:
   85.2              -59.2
  Corners:
   22.5              -32.8
   18.6              -46.6
   85.9              -76.2
  129.3              -71.6
  ----------------------------------
The error box area is about 736 sq. deg, and its maximum
dimension is 64 deg (the minimum one is 12.5 deg).
The Sun distance was about 96 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi final position and BALROG 
(https://grb.mpe.mpg.de/grb/GRB211124104/) localizations.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB211124_T08993/IPN


GRB_name: GRB211118A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31125
SUBJECT: GRB 211118A: Fermi GBM detection
DATE:    21/11/25 15:18:49 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 23:38:14.587 UT on 18 November 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211118A (trigger 658971499 / 211118985).
which was also detected by the Swift/BAT-GUANO (Raman et al. 2021, GCN 31096).

The on-ground calculated location, using the Fermi GBM trigger data,
is RA = 33.7, Dec = 71.1(J2000 degrees, equivalent to J2000 02h 15m, 71d 03'),
with a statistical uncertainty of 2.7 degrees (radius, 1-sigma
containment, statistical only;
there is additionally a systematic error which we have characterized
as a core-plus-tail model,
with 90% of GRBs having a 3.7 deg error and a small tail suffering
a larger than 10 deg systematic error. [Connaughton et al. 2015, ApJS,
216, 32] )

The angle from the Fermi LAT boresight at the GBM trigger time is 127 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 7.2 s (50-300 keV).
The time-averaged spectrum from T0-0.002 s to T0+7.776 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.21 +/- 0.07 and
the cutoff energy, parameterized as Epeak, is 2176 +/- 865 keV

The event fluence (10-1000 keV) in this time interval is
(3.975 +/- 0.272)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 7.1 +/- 0.5 ph/s/cm^2.

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

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


GRB_name: GRB210905A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31127
SUBJECT: Chandra observations of GRB 210905A
DATE:    21/11/25 16:55:36 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (Radboud University), R. Margutti (UC Berkeley), K. D. Alexander
(Northwestern), E. Berger (Harvard), and R. Chornock (UC Berkeley) report:

"We observed GRB 210905A (Sonbas et al., GCN 30765) with Chandra/ACIS,
starting on 2021 November 24 at 13:08:25 UT (80.7 days after the GRB
trigger), for a total exposure of 20 ks. We detect a point source at the
position of the Swift/XRT afterglow with a 0.5-8 keV (observed) count rate
of ~ 3.1e-4 counts/s. Using spectral parameters from fitting the Swift/XRT
PC-mode spectrum at a redshift of z=6.318 (Tanvir et al., GCN 30771), we
find a preliminary unabsorbed flux of ~ 5.4e-15 erg/(s cm^2) in the 0.3-10
keV band (observer frame).

This measurement confirms a potential break in the Swift/XRT observations
at ~ 30 days after the trigger. The post-break decline rate is consistent
with -2. Interpreting this break as a jet break, assuming EKiso ~
Egamma,iso, and using the isotropic-equivalent gamma-ray energy from
Konus-Wind (Frederiks et al., GCN 30780), the inferred opening angle is ~ 9
deg * (E/1.1e54 erg) / (n/ (1particle/cm^3))] ^(-3/8) for a uniform density
environment, leading to a beaming-corrected energy of ~ 1.3e52 erg. Further
analysis is underway.

We thank Harvey Tananbaum and Pat Slane for approving our DDT request and
the entire CXC staff for arranging and executing the observations."


GRB_name: GRB211120A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31129
SUBJECT: IPN triangulation of GRB 211120A
DATE:    21/11/26 13:51:12 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the MGNS/BepiColombo and HEND/Mars Odyssey teams,

J. Benkhoff on behalf of the BepiColombo team,

K. Hurley on behalf of the IPN,

D. Svinkin, S. Golenetskii, D. Frederiks, A. Ridnaia,
A. Lysenko, and T. Cline on behalf of the Konus-Wind 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 211120A
(GECAM-B detection: Li et al., GCN Circ. 31100;
AstroSat-CZTI detection: Prasad et al., GCN Circ. 31104;
AGILE-MCAL detection: Ursi et al., GCN Circ. 31105)
was detected by GECAM-B (GRD), AstroSat (CZTI), AGILE (MCAL),
Konus-Wind, Mars-Odyssey (HEND),
and BepiColombo (MGNS; see introductory GCN Circ. 30949)
at about 83120 s UT (23:05:20).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   315.138 (21h 00m 33s) +42.856 (+42d 51' 20")
  Corners:
   315.108 (21h 00m 26s) +43.024 (+43d 01' 25")
   315.128 (21h 00m 31s) +42.774 (+42d 46' 28")
   315.185 (21h 00m 44s) +42.640 (+42d 38' 25")
   315.164 (21h 00m 39s) +42.890 (+42d 53' 23")
  ---------------------------------------------
The error box area is 30 sq. arcmin, and its maximum
dimension is 23 arcmin (the minimum one is 0.7 arcmin).
The Sun distance was 95 deg.

This box may be improved.

The distance between the box and the GECAM position
(RA, Dec, Err = 304.99, 41.42, 1.34; GCN 31100) is
7.6 deg, thus it is inconsistent with the box.

The box Galactic latitude is -2.2 deg (noticed by Shaolin XIONG),
so the Galactic origin can not be ruled out
using the burst localization only.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB211120_T83120/IPN/

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


GRB_name: GRB211120A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31130
SUBJECT: Konus-Wind detection of GRB 211120A
DATE:    21/11/26 14:31:29 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 211120A (GECAM detection: Li et al., GCN 31100;
AstroSat CZTI detection: Prasad et al., GCN 31104;
AGILE detection: Ursi et al., GCN 31105;
IPN localization: Kozyrev et al., GCN 31129)
triggered Konus-Wind (KW) at T0=83120.396 s UT (23:05:20.396).

The burst light curve shows a bright, multi-peaked pulse
which starts at ~T0-1 s and has a total duration of ~8 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/GRB211120_T83120/

As observed by Konus-Wind, the burst had
a fluence of (3.5 Â± 0.4)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 1.984 s,
of (2.4 Â± 0.2)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+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 = -0.65 (-0.07,+0.08),
the high energy photon index beta = -2.71 (-0.30,+0.20),
the peak energy Ep = 315 (-24,+24) keV,
chi2 = 113/95 dof.

The spectrum near the peak count rate (measured from T0+0.256
to T0+3.072 s) is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.55 (-0.10,+0.12),
the high energy photon index beta = -2.48 (-0.28,+0.18),
the peak energy Ep = 325 (-36,+40) keV,
chi2 = 96/84 dof.

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


GRB_name: GRB211120B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31131
SUBJECT: GRB 211120548: Fermi GBM observation
DATE:    21/11/26 15:39:53 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

"At 13:09:46.84 UT on 20 November 2021, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 211120B (trigger 659106591 / 211120548).
which was also detected by the Swift/BAT-GUANO (DeLaunay et al. 2021, GCN
31101)

The GBM on-ground calculated location, using the GBM trigger
data, is RA = 47.9, DEC = 47.1 (J2000 degrees,
equivalent to 03 h 11 m, 47 d 6 '), with a statistical uncertainty
of 1.9 degrees (radius, 1-sigma containment, statistical only;
there is additionally a systematic error which we have characterized as a
core-plus-tail model,
with 90% of GRBs having a 3.7 deg error and a small tail suffering
a larger than 10 deg systematic error. [Connaughton et al. 2015, ApJS, 216,
32] )

The angle from the Fermi LAT boresight at the GBM trigger time is 62
degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 36.1 s (50-300 keV).
The time-averaged spectrum from T0-6.400 s to T0+33.537 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.99 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 298.2 +/- 26.3 keV

The event fluence (10-1000 keV) in this time interval is
(1.184 +/- 0.60)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.28 s in the 10-1000 keV band
is 6.5 +/- 0.2 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 180.1 +/- 24.3 keV, alpha = -0.79 +/- 0.08 and beta = -1.87 +/-
0.08.

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: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31133
SUBJECT: GRB 211023A: Xinglong 2.16m optical observations
DATE:    21/11/29 05:06:21 GMT
FROM:    Liping Xin at NAOC, SVOM  <xlp@nao.cas.cn>



GRB_name: GRB211023A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31134
SUBJECT: GRB 211023A: Xinglong 2.16m optical observations
DATE:    21/11/29 05:33:13 GMT
FROM:    Liping Xin at NAOC, SVOM  <xlp@nao.cas.cn>

L. P. Xin (NAOC), J. Wang(GXU), C. Gao(GXU), Y. L. Qiu(NAOC),
J. Y. Wei(NAOC),  B. Ren(GXU),  L. H. Li (NAOC),  C. Wu(NAOC),  
E. W. Liang(GXU),  X. H. Han (NAOC) and J. S. Deng(NAOC) report:

We observed the field of the GRB 211023A (Fermi GBM team, GCN 30958; Di
Lalla et al., GCN 30961; Lesage et al, GCN 30965; Ursi et al, GCN 30969;
Poolakkil, GCN 30998; Ridnaia et al., GCN 31022 ) 
with 2.16m optical telescope at Xinglong observatory, China. 
Ten images in R band were obtained from 2021-11-12T16:46:10 UT to 
2021-11-12T17:32:18 UT, about 20.16 days after the burst. 
The exposure time for each image was 300 sec. 

The optical counterpart (Lipunov et al., GCN 30970; Zhirkov et al, GCN 30977; 
Kann et al, GCN 30982; Hu et al, GCN 30990; Belkin et al, GCN 31004; Vinko et al, GCN
31008; Belkin et al, GCN 31018; Belkin et al, GCN 31020; Kumar et al,
GCN 31023; Gupta et al., GCN 31041; Strobl et al., GCN 31042; Pozanenko
et al., GCN 31053; Moskvitin et al., GCN 31066, , Belkin et al., GCN 31098) 
was clearly detected in our the stacked image with a brightness of 22.0 magnitude 
in R-band. The photometry was calibrated with several nearby USNO B1.0 catalogs.


GRB_name: GRB211129A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31136
SUBJECT: GRB 211129A: Swift detection of a burst
DATE:    21/11/29 10:11:32 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.D. Gropp (PSU), S. D. Barthelmy (GSFC), P. A. Evans (U Leicester),
N. J. Klingler (GSFC/UMBC/CRESSTII), K. L. Page (U Leicester) and
B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 09:51:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211129A (trigger=1085430).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 274.557, +31.776 which is 
   RA(J2000)  =  18h 18m 14s
   Dec(J2000) = +31d 46' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows 3 major peaks
with a duration of about 200 sec.  The peak count rate was ~1400 counts/sec
(15-350 keV),
at ~3 sec after the trigger. 

The XRT began observing the field at 09:52:19.7 UT, 73.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 274.58129, 31.78820 which
is equivalent to:
  RA(J2000)  = 18h 18m 19.51s
  Dec(J2000) = +31d 47' 17.5"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 86 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/1085430. 
We cannot determine whether the source is fading at the present time. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 1.41e-09 erg cm^-2 s^-1 (0.2-10
keV). 

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
0.082. 

Burst Advocate for this burst is J.D. Gropp (jdg44 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: GRB211129A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31137
SUBJECT: GRB 211129A: MITSuME Akeno optical upper limits
DATE:    21/11/29 10:36:23 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

R. Yamaguchi, R. Hosokawa, Y. Imai, K. L. Murata, M. Niwano, Y.
Takamatsu, N. Ito, R. Noto, S. Sato, M. Takaku, Y. Yatsu, and N. Kawai
(TokyoTech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 211129A(J.D. Gropp et al. GCN Circular
#31136) with the optical three color (g', Rc, and Ic) CCD cameras
attached to the MITSuME 50 cm telescope Akeno. The observation with a
series of 10 sec exposures started at 2021-11-29 09:52:06 UT (60
seconds after Swift trigger). We stacked the images with good
conditions. We did not detect any uncatalogued sources within the XRT
error region (J.D. Gropp et al. GCN Circular #31136). We obtained the
5-sigma limits of the stacked images as follows.

T0+[sec] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
159 2021-11-29 09:53:45 70 g'>17.0, Rc>17.3, Ic>16.4
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time

We used 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. 2021, PASJ, Vol.73, Issue 1, Pages
4-24; https://github.com/MNiwano/Eclaire).


GRB_name: GRB211118A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31138
SUBJECT: IPN triangulation of GRB 211118A
DATE:    21/11/29 13:54:51 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

A. Ridnaia, S. Golenetskii, D. Frederiks, D. Svinkin,
A. Lysenko, 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,

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

and

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

The long-duration GRB 211118A
(Swift/BAT-GUANO detection: Raman et al., GCN 31096;
AstroSat CZTI detection: Prasad et al., GCN 31099;
Fermi GBM detection: Mangan et al., GCN 31125)
was detected by Fermi (GBM trigger 658971499),
Konus-Wind, INTEGRAL (SPI-ACS), Swift-BAT, and
AstroSat (CZTI) at about 85093 s UT (23:38:13).
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:
   26.464 (01h 45m 51s) +73.778 (+73d 46' 40")
 Corners:
   20.795 (01h 23m 11s) +68.534 (+68d 32' 02")
   13.882 (00h 55m 32s) +68.354 (+68d 21' 14")
   39.770 (02h 39m 05s) +78.696 (+78d 41' 47")
   54.289 (03h 37m 09s) +77.757 (+77d 45' 24")
 ---------------------------------------------
The error box area is 28.9 sq. deg, and its maximum
dimension is 14.5 deg (the minimum one is 2.3 deg).
The Sun distance was 120 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi GBM on-ground calculated localization (GCN Circ. 31125).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB211118_T85093/IPN

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


GRB_name: GRB211129A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31139
SUBJECT: GRB 211129A: Enhanced Swift-XRT position
DATE:    21/11/29 14:07:46 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 1213 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 211129A, 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 = 274.58031, +31.78886 which is equivalent
to:

RA (J2000): 18h 18m 19.27s
Dec (J2000): +31d 47' 19.9"

with an uncertainty of 2.1 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: GRB211129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31140
SUBJECT: GRB 211129A: Nanshan/NEXT optical upper limit
DATE:    21/11/29 14:24:12 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of Swift GRB 211129A (Gropp et al. GCN Circ. 
31136) using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. We obtained 18x120 s frames in the Sloan r-band, starting at 
12:38:57 UT on 2021-11-29, i.e., 2.8 hr after the BAT trigger.

No optical source is detected at the Enhanced Swift/XRT position (Goad 
et al. GCN Circ. 31139) in our stacked image, down to a limiting 
magnitude of r~21.2, calibrated with the nearby PanSTARRS field.


GRB_name: GRB211129A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31141
SUBJECT: Swift GRB 211129A: Global MASTER-Net observations report 
DATE:    21/11/29 14:48:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 211129A ( J.D. Gropp et al., GCN 31136) errorbox  17290 sec after notice time and 17308 sec after trigger time at 2021-11-29 14:39:34 UT, with upper limit up to  16.0 mag. Observations started at twilight.  The observations began at zenith distance = 45 deg. The sun  altitude  is -11.1 deg. 

The galactic latitude b = 20 deg., longitude l = 59 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1799491

We obtain a following upper limits.  

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

   17399 |   MASTER-Kislovodsk |   C |   180 | 16.0 |        
   17399 |   MASTER-Kislovodsk |   C |   180 | 12.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211129A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31142
SUBJECT: GRB 211129A: Fermi GBM observation
DATE:    21/11/29 16:53:17 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

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


"At 09:51:06.36 UT on 29 November 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211129A (trigger 659872271 / 211129410),
which was also detected by the Swift/BAT (Gropp et al. 2021, GCN 31136).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 22 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 111 s (50-300 keV).
The time-averaged spectrum from T0-8 s to T0+41 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.54 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 220 +/- 90 keV.

The event fluence (10-1000 keV) in this time interval is
(4.3 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+27 s in the 10-1000 keV band
is 2.81 +/- 0.22 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: GRB211106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31145
SUBJECT: GRB 211106A: Chandra Observations
DATE:    21/11/29 19:30:50 GMT
FROM:    Edo Berger at Harvard  <eberger@cfa.harvard.edu>

E. Berger (Harvard), A. Rouco Escorial, and W. Fong (Northwestern) report
on behalf of a larger collaboration:

"We observed the location of the short GRB 211106A (GCNC #31049) with the
Chandra X-ray Observatory + ACIS-S starting on 2021 November 16.58 UT
(10.38 days post-burst) for 19.8 ksec as part of program 22500107 (PI:
Berger).  Within the XRT error circle (GCNC #31068) we detect a single
X-ray source at (J2000):

        RA = 22:54:20.51

        Dec = -53:13:51.2

with a preliminary uncertainty of about 0.8 arcsec.  This source is located
3.1" from the center of galaxy #1 at z=0.097 identified in earlier VLT
observations (GCNC #31070 and #31075).  The angular offset corresponds to a
projected physical offset of 5.6 kpc at the redshift of the galaxy.  The
flux of the X-ray source indicates continued fading with a power law index
of about -1.

We thank the CXO staff for rapidly scheduling these observations."


GRB_name: GRB211106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31146
SUBJECT: GRB 211106A: HST Observations
DATE:    21/11/29 19:37:00 GMT
FROM:    Charles Kilpatrick at Northwestern U  <ckilpatrick@northwestern.edu>

C. D. Kilpatrick (Northwestern), E. Berger (Harvard), and W. Fong (Northwestern) report on behalf of a larger collaboration: "We observed the location of the short GRB 211106A (GCNC #31049) with the Hubble Space Telescope starting on 2021 November 25.37 (19.17 days post-trigger) using ACS/F814W and WFC3/F110W for 2 orbits each, as part of program 16303 (PI: Berger). Within the 0.8-arcsec error circle of the X-ray afterglow detected with Chandra (GCNC #31145) we detect a single source in both filters at (J2000): RA = 22:54:20.54 Dec = -53:13:50.6 with an uncertainty of about 0.05 arcsec. Preliminary photometry indicates AB magnitudes of m(F814W) ~ 25.7 and m(F110W) ~ 25.6. We note that the source may be slightly extended (northward) in the F110W image. The origin of the optical/NIR source is unclear at the present. If it is the afterglow, then a similar decline rate as observed in the X-rays (about t^-1; GCNC #31145) would indicate an expected optical magnitude of ~23.7 at the time of the VLT/FORS2 observations, over 2 mag brighter than the limit of R~26 mag listed in GCNC #31070. If the source is a kilonova, and the event is associated with the galaxy at z=0.097 identified in VLT data (GCNC #31075), then it is about 2.5 mag (a factor of 10) more luminous in J-band than the kilonova associated with GW170817 (Villar et al. 2017, ApJ, 851, L21), and moreover significantly bluer, with m(F814W)-m(F110W) ~ 0 mag. Finally, it is possible that the optical/NIR source is the actual host galaxy of GRB 211106A, most likely placing the burst at a higher redshift than z=0.097. Additional HST observations are planned to shed light on the nature of the source.


GRB_name: GRB211129A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31147
SUBJECT: GRB 211129A: Swift/UVOT Upper Limits
DATE:    21/11/29 23:54:11 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 211129A
84 s after the BAT trigger (Gropp et al., GCN Circ. 31136).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 31139)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            84          234          147         >20.7
u_FC               297          547          246         >20.4
white               84          769          186         >20.9
v                  626          818           39         >18.8
b                  552          744           39         >19.6
u                  297          719          265         >20.5
w1                 675          695           19         >19.6
m2                 651          831           28         >19.2
w2                 602          794           39         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.081 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB211129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31148
SUBJECT: GRB 211129A: Swift-XRT refined Analysis
DATE:    21/11/30 01:32:32 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.2 ks of XRT data for GRB 211129A (Gropp et al. GCN
Circ. 31136), from 62 s to 50.9 ks after the  BAT trigger. The data
comprise 325 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 31139).

The late-time light curve (from T0+4.5 ks) can be modelled with a
power-law decay with a decay index of alpha=1.02 (+/-0.08).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.63 (+/-0.05). The
best-fitting absorption column is  4.8 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 8.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.30 (+0.16, -0.15)
and a best-fitting absorption column of 5.9 (+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 3.6 x 10^-11 (7.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.9 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 8.8 x 10^20 cm^-2
Excess significance: 10.1 sigma
Photon index:      2.30 (+0.16, -0.15)

If the light curve continues to decay with a power-law decay index of
1.02, the count rate at T+24 hours will be 0.038 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x
10^-12 (2.9 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/01085430.

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


GRB_name: GRB211129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31149
SUBJECT: GRB 211129A: Swift-BAT refined analysis
DATE:    21/11/30 03:22:44 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. D. Gropp (PSU), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team):

Using the data set from T-239 to T+800 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 211129A (trigger #1085430)
(Gropp et al., GCN Circ. 31136).  The BAT ground-calculated position is
RA, Dec = 274.565, 31.781 deg which is
   RA(J2000)  =  18h 18m 15.6s
   Dec(J2000) = +31d 46' 51.5"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~T-2 s and ends at ~T+120 s. The three main peaks occur at ~T+1 s,
~T+29 s, and ~T+91 s, respectively. T90 (15-350 keV) is 113.01 +- 9.14 sec
(estimated error including systematics).

The time-averaged spectrum from T-1.80 to T+124.11 sec is best fit by
a simple power-law model.  The power law index of the time-averaged
spectrum is 1.75 +- 0.13.  The fluence in the 15-150 keV band
is 2.3 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+0.99 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/1085430/BA/


GRB_name: GRB211106A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31150
SUBJECT: GRB 211106A: GECAM detection
DATE:    21/11/30 10:08:36 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, S. L. Xiong, C. Cai, S. Xiao, P. Zhang, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered by a short burst, 
GRB 211106A, at 2021-11-06T04:37:31.250 UTC (denoted as T0), which was 
also observed by Swift/BAT-GUANO (GCN #31049), Fermi/GBM Sub-Threshold
(GCN #31055), Konus-Wind (GCN #31054), INTEGRAL/SPI-ACS (TrigID #9504)
and IPN (GCN #31078).

According to the GECAM-B light curves, this burst mainly consists of 
two pulses with duration of about 2 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_89872651.PNG

GECAM location is consistent with the Swift/BAT position within the error.

The time-integrated spectrum (measured from T0-0.25 s to T0+1.85 s) 
is best fit by the power law model (in the 20 keV - 5 MeV range):
A(E) ~ k * E^(-alpha) with alpha = 1.32 (-0.13, 0.15).
The burst had a fluence of 6.35 (3.72, 7.05)x10^-7 erg/cm^2 (20 - 200 keV)
during the time interval metioned above. 
All parameters in parenthesis are for 90% confidence level.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211130A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31151
SUBJECT: GRB 211130A: Fermi GBM Final Real-time Localization
DATE:    21/11/30 15:26:55 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 15:16:27 UT on 30 Nov 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211130A (trigger 659978192.028088 / 211130636).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 18.3, Dec = -24.3 (J2000 degrees, equivalent to J2000 01h 13m, -24d 18'), with a statistical uncertainty of 1.4 degrees.

The angle from the Fermi LAT boresight is 72.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211130636/quicklook/glg_skymap_all_bn211130636.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211130636/quicklook/glg_healpix_all_bn211130636.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211130636/quicklook/glg_lc_medres34_bn211130636.gif


GRB_name: GRB211130A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31152
SUBJECT: GRB 211130A: BALROG localization (Fermi Trigger 659978192 / GRB 211130636)
DATE:    21/11/30 16:17:17 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
659978192 at 15:16:27 on 30 Nov. 2021 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) = 18.8+/-3.0 deg
Decl.(2000.0) = -28.5+/-3.8 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB211130636/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB211130636/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB211130636/json

                        


GRB_name: GRB211130A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31154
SUBJECT: Fermi GRB 211130A: Global MASTER-Net observations report 
DATE:    21/11/30 17:30:11 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211130A ( Fermi GBM team, GCN 31151) errorbox  693 sec after notice time and 732 sec after trigger time at 2021-11-30 15:28:39 UT, with upper limit up to  17.5 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -19.8 deg. 

The galactic latitude b = -84 deg., longitude l = 185 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1800540

We obtain a following upper limits.  

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

     802 | 2021-11-30 15:28:39 |   MASTER-Kislovodsk | (01h 12m 10.65s , -24d 10m 36.9s) |  P- |   140 | 15.5 |        
     802 | 2021-11-30 15:28:39 |   MASTER-Kislovodsk | (01h 12m 21.91s , -24d 33m 47.5s) |   C |   140 | 13.6 |        
     983 | 2021-11-30 15:31:19 |   MASTER-Kislovodsk | (01h 12m 07.92s , -24d 09m 06.7s) |  P- |   180 | 16.8 |        
     983 | 2021-11-30 15:31:19 |   MASTER-Kislovodsk | (01h 12m 25.40s , -24d 32m 24.1s) |   C |   180 | 13.2 |        
    1183 | 2021-11-30 15:34:40 |   MASTER-Kislovodsk | (01h 12m 08.03s , -24d 10m 12.7s) |  P- |   180 | 16.5 |        
    1183 | 2021-11-30 15:34:40 |   MASTER-Kislovodsk | (01h 12m 20.64s , -24d 33m 26.8s) |   C |   180 | 12.8 |        
    1384 | 2021-11-30 15:38:00 |   MASTER-Kislovodsk | (01h 12m 10.08s , -24d 08m 56.4s) |  P- |   180 | 16.6 |        
    1564 | 2021-11-30 15:38:00 |   MASTER-Kislovodsk | (01h 12m 10.08s , -24d 08m 56.4s) |  P- |   540 | 17.5 |  Coadd 
    1384 | 2021-11-30 15:38:00 |   MASTER-Kislovodsk | (01h 12m 22.20s , -24d 32m 06.5s) |   C |   180 | 13.5 |        
    1584 | 2021-11-30 15:41:21 |   MASTER-Kislovodsk | (01h 12m 04.09s , -24d 09m 34.1s) |  P- |   180 | 17.0 |        
    1584 | 2021-11-30 15:41:21 |   MASTER-Kislovodsk | (01h 12m 16.60s , -24d 32m 42.7s) |   C |   180 | 13.7 |        
    1784 | 2021-11-30 15:44:41 |   MASTER-Kislovodsk | (01h 12m 05.14s , -24d 08m 31.6s) |  P- |   180 | 17.1 |        
    1785 | 2021-11-30 15:44:41 |   MASTER-Kislovodsk | (01h 12m 18.01s , -24d 31m 39.2s) |   C |   180 | 15.0 |        
    6472 | 2021-11-30 17:03:49 |   MASTER-Kislovodsk | (01h 22m 39.34s , -25d 13m 11.6s) |   C |    60 | 12.8 |        
    6793 | 2021-11-30 17:09:10 |   MASTER-Kislovodsk | (01h 04m 47.15s , -23d 20m 56.2s) |   C |    60 | 15.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211201A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31155
SUBJECT: GRB 211201A: Fermi GBM Final Real-time Localization
DATE:    21/12/01 20:50:50 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 20:42:52 UT on 1 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211201A (trigger 660084177.881018 / 211201863).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 355.4, Dec = 2.6 (J2000 degrees, equivalent to J2000 23h 41m, 2d 36'), with a statistical uncertainty of 5.0 degrees.

The angle from the Fermi LAT boresight is 108.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211201863/quicklook/glg_skymap_all_bn211201863.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211201863/quicklook/glg_healpix_all_bn211201863.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211201863/quicklook/glg_lc_medres34_bn211201863.gif


GRB_name: GRB211201A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31156
SUBJECT: Fermi GRB 211201A: Global MASTER-Net observations report 
DATE:    21/12/01 21:15:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211201A ( Fermi GBM team, GCN 31155) errorbox  1138 sec after notice time and 1166 sec after trigger time at 2021-12-01 21:02:19 UT, with upper limit up to  12.7 mag. The observations began at zenith distance = 75 deg. The sun  altitude  is -68.9 deg. 

The galactic latitude b = -56 deg., longitude l = 92 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1801667

We obtain a following upper limits.  

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

    1197 | 2021-12-01 21:02:19 |   MASTER-Kislovodsk | (23h 49m 38.72s , +01d 09m 30.8s) |   C |    60 | 12.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31157
SUBJECT: GRB 211106A: Second HST Observation
DATE:    21/12/02 17:42:39 GMT
FROM:    Charles Kilpatrick at Northwestern U  <ckilpatrick@northwestern.edu>

C. D. Kilpatrick (Northwestern), E. Berger (Harvard), and W. Fong (Northwestern) report on behalf of a larger collaboration:

"We re-observed the location of the short GRB 211106A (GCNC #31049) with the Hubble Space Telescope starting on 2021 December 1.46 (25.26 days post-trigger; 6.1 days after Visit 1 - GCNC #31146) using WFC3/F110W for 2 orbits, as part of program 16303 (PI: Berger).  

The source identified in our first HST observation (GCNC #31146) is still detected, with an unchanged magnitude of m(F110W) ~ 25.6.  Digital image subtraction between the two epochs does not reveal any emission at the location of the source to a 5-sigma limit of ~27 mag.

The lack of fading over the 6-day time baseline suggests that this source is not an afterglow or kilonova.  Instead, it is likely to be either the host galaxy of GRB 211106A, or an unrelated background galaxy if the GRB itself is associated with the galaxy at z=0.097. The absolute magnitude of the NIR source if it is also located at z=0.097 is M(F110W) ~ -12.7,  too luminous to be a globular cluster."


GRB_name: GRB211201A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31158
SUBJECT: GRB 211201A: Swift/BAT-GUANO detection likely outside the coded FOV
DATE:    21/12/02 21:06:16 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (UAlabama), Aaron Tohuvavohu (U Toronto), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT did not trigger on GRB 211201A (T0: 2021-12-01T20:42:52 UTC,
Fermi/GBM GCN 31155).

The Fermi/GBM notice, distributed in near real-time, triggered the
Swift Mission Operations Center operated Gamma-ray Urgent Archiver for
Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 13.1 in a
16.384 s analysis time bin.
Estimated T90 in the detector is 30.5 +/- 0.5 s (15-350 keV).

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FOV, with a
borderline DeltaLLHOut of 9.57.
An out of FOV origin is more consistent with the Fermi/GBM
localization, and the Fermi/GBM spectral fit (private comm.) is
consistent with the best fit OFOV model from NITRATES.
Therefore we think it likely that this burst originates from outside
the coded FOV.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211201A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31159
SUBJECT: GRB 211201A: GECAM detection
DATE:    21/12/03 01:04:55 GMT
FROM:    Guoying Zhao at IHEP  <gyzhao@ihep.ac.cn>

G. Y. Zhao, S. L. Xiong,X. L. Zhang, S. Xiao, Yi Zhao, C. Cai, J. J. He, 
Y. Huang, Z. W. Guo, C. Y. Li, X. B. Li, J. C. Liu, X. Y. Song, P. Wang,
S. L. Xie, W. C. Xue, Q. B. Yi, Y. Q. Zhang,  X. Y. Zhao, C. Zheng,
Y. Q. Du, D. Y. Guo, J. Liang, F. J. Lu, Q. Luo, X. Ma, W. X. Peng,
R. Qiao, L. M. Song, J. Wang, H. Wu, P. Zhang, S. N. Zhang,
C. W. Wang,Z. Zhang, S. J. Zheng (IHEP),report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered on-ground by a 
long bright burst, GRB 211201A, at 2021-12-01T20:43:06.000 UTC (denoted as T0)ï¼Œ
which was also observed by Fermi/GBM (GCN #31155).

This burst mainly consists of multiple pulses with duration of about 50 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/LightCurve.png

GECAM location is consistent with the Fermi/GBM position within the error.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211203A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31160
SUBJECT: GRB 211203A: Swift detection of a burst
DATE:    21/12/03 09:33:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

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

At 09:02:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211203A (trigger=1086826).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 170.174, +16.256 which is 
   RA(J2000) = 11h 20m 42s
   Dec(J2000) = +16d 15' 21"
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 25 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~7 sec after the trigger. 

The XRT began observing the field at 09:03:56.8 UT, 78.5 seconds after
the BAT trigger. No source was detected in 2 s of promptly downlinked
data, which covered 93% of the BAT error circle. We are waiting for the
full dataset to detect and localise the XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 81 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.023. 

Burst Advocate for this burst is P. A. Evans (pae9 AT star.le.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB211130A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31161
SUBJECT: IPN triangulation of GRB 211130A
DATE:    21/12/03 14:20:30 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the MGNS/BepiColombo and HEND/Mars Odyssey teams,

J. Benkhoff on behalf of the BepiColombo team,

A. Ridnaia, D. Frederiks, D. Svinkin, A. Lysenko,
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

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

The long-duration GRB 211130A
(Fermi GBM Final Real-time localization: The Fermi GBM team, GCN 31151;
BALROG localization: Kunzweiler et al., GCN 31152)
was detected by Fermi (GBM trigger 659978192), Konus-Wind,
INTEGRAL (SPI-ACS), and BepiColombo (MGNS) at about 54987 s UT (15:16:27).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
   21.148 (01h 24m 35s) -27.829 (-27d 49' 46")
 Corners:
   20.183 (01h 20m 44s) -27.190 (-27d 11' 25")
   20.317 (01h 21m 16s) -27.403 (-27d 24' 10")
   22.106 (01h 28m 25s) -28.433 (-28d 25' 58")
   21.973 (01h 27m 54s) -28.233 (-28d 13' 58")
 ---------------------------------------------
The error box area is 734 sq. arcmin, and its maximum
dimension is 2.1 deg (the minimum one is 6.5 arcmin).
The Sun distance was 113 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi final position and BALROG localizations.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB211130_T54992/IPN

The time history and spectrum will be given in forthcoming GCN Circulars.


GRB_name: GRB211130A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31162
SUBJECT: Konus-Wind detection of GRB 211130A
DATE:    21/12/03 17:19:17 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The long-duration GRB 211130A
(Fermi GBM Final Real-time localization: The Fermi GBM team, GCN 31151;
BALROG localization: Kunzweiler et al., GCN 31152;
IPN triangulation: Kozyrev et al., GCN 31161)
triggered Konus-Wind at T0=54992.505 s UT (15:16:32.505).

The burst light curve starts with a smooth pulse, which was followed,
after a period of low-level emission, by a more intense, multi-peaked
emission complex. The total burst duration is ~21.4 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/GRB211130_T54992/

As observed by Konus-Wind, the burst
had a fluence of 9.57(-0.68,+0.75)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+13.456 s,
of 8.39(-2.23,+2.99)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 6 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.54(-0.24,+0.27)
and Ep = 164(-15,+19) keV (chi2 = 82/75 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.5
(chi2 = 82/74).

The spectrum near the maximum count rate
(measured from T0+8.448 to T0+16.640 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 = -0.40(-0.34,+0.47),
the high energy photon index beta = -2.69(-1.55,+0.43),
the peak energy Ep = 177(-31,+34) keV
(chi2 = 56/73 dof).

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


GRB_name: GRB211203A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31163
SUBJECT: Fermi GBM Upper limits for GRB 211203A
DATE:    21/12/03 17:30:32 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

C. Malacaria (USRA) reports on behalf of the Fermi-GBM Team:

Swift/BAT detected GRB 211203A at 09:02:38 UT (GCN 31160). 
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 identified no counterparts.
 
The GBM targeted search [1], the most sensitive, coherent search for
GRB-like signals, was run from +/-30 s around the Swift/BAT time.
From this search, no significant signal was found related
to GRB 211203A.

We set upper limits on impulsive gamma-ray emission. Using the
representative soft, normal, and hard GRB-like templates described in
arXiv:1612.02395, we set the following 3 sigma flux upper limits over
10-1000 keV (in units of 10^-7 erg/s/cm^2):

Timescale   Soft     Normal   Hard
-------------------------------------------
0.128 s:    4.7      9.2      17.0
1.024 s:    1.6      3.8      8.2
8.192 s:    0.4      0.9      2.0

These results are preliminary.

[1] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB211203A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31164
SUBJECT: Swift GRB 211203A: Global MASTER-Net observations report 
DATE:    21/12/03 17:40:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) was pointed to the Swift GRB 211203A ( P. A. Evans et al., GCN 31160) errorbox  27509 sec after notice time and 28199 sec after trigger time at 2021-12-03 16:52:37 UT, with upper limit up to  18.6 mag. The observations began at zenith distance = 70 deg. The sun  altitude  is -56.8 deg. 

The galactic latitude b = 67 deg., longitude l = 237 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1802853

We obtain a following upper limits.  

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

   28289 |         MASTER-Amur |   C |   180 | 18.5 |        
   28896 |         MASTER-Amur |   C |   180 | 18.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211203A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31165
SUBJECT: Swift Trigger 1086826 (possible GRB 211203A) is likely not an astrophysical event
DATE:    21/12/03 17:57:24 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

T. Parsotan (GSFC/UMBC), S. D. Barthelmy (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), (i.e. the Swift-BAT team):
 
Using the full data set from recent downlinks, we report further ground data analysis for Swift trigger 1086826 (Evans, et al., GCN Circ. 31160).
 
The BAT analysis uses data from T-50 to T+250 sec. The BAT image significance is 3.9 sigma (15-350 keV). Also, the mask-weighted light curve does not show anything significant and there is no identified source in the ground analysis of the scaled map.
 
We therefore conclude that this event is likely due to noise and is not an astrophysical event.


GRB_name: GRB211124A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31166
SUBJECT: GRB 211124A: Fermi GBM Observation
DATE:    21/12/03 22:29:45 GMT
FROM:    Boyan A. Hristov at UAH  <bah0046@uah.edu>

Boyan A. Hristov (UAH) reports on behalf of the Fermi GBM Team:

"At 02:29:53.56 UT on 24 November 2021, the Fermi Gamma-Ray Burst
Monitor (GBM) triggered and located GRB 211124A (trigger 659413798
/ 211124104),

The results from Swift/BAT + NITRATES (DeLaunay et al. 2021, GCN 31113)
are consistent with a burst coming from out of the FOV,
which is also consistent with the GBM in-flight location.

The GBM location, using the GBM trigger data, is RA = 94.967,
DEC = -61.433 (J2000 degrees, equivalent to 06h 20m, -61d 26'), with a
statistical uncertainty of 5.98 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic error which we
have characterized as a core-plus-tail model, with 90% of GRBs having
a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).

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

The GBM light curve shows two peaks with a duration (T90) of about
0.5 s (50-300 keV).  The time-averaged spectrum from T0-0.128 s to
T0+0.576 s is well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.65 +/- 0.16 and the
cutoff energy, parameterized as Epeak, is 357.50 +/- 80.10 keV.
The event fluence (10-1000 keV) in this time interval is
(1.004 +/- 0.120)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0 s in the 10-1000 keV band is 27 +/- 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: GRB211204A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31167
SUBJECT: GRB 211204A: Fermi GBM Final Real-time Localization
DATE:    21/12/04 03:38:02 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 03:27:36 UT on 4 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211204A (trigger 660281261.437168 / 211204144).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 35.4, Dec = -49.5 (J2000 degrees, equivalent to J2000 02h 21m, -49d 30'), with a statistical uncertainty of 10.3 degrees.

The angle from the Fermi LAT boresight is 59.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204144/quicklook/glg_skymap_all_bn211204144.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204144/quicklook/glg_healpix_all_bn211204144.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204144/quicklook/glg_lc_medres34_bn211204144.gif


GRB_name: GRB211204A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31168
SUBJECT: Fermi GRB 211204A: Global MASTER-Net observations report 
DATE:    21/12/04 03:45:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211204A ( Fermi GBM team, GCN 31167) errorbox  425 sec after notice time and 452 sec after trigger time at 2021-12-04 03:35:08 UT, with upper limit up to  18.4 mag. The observations began at zenith distance = 32 deg. The sun  altitude  is -35.5 deg. 

The galactic latitude b = -62 deg., longitude l = 270 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1803448

We obtain a following upper limits.  

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

     482 | 2021-12-04 03:35:08 |         MASTER-OAFA | (02h 22m 56.00s , -59d 01m 07.3s) |   C |    60 | 18.3 |        
     562 | 2021-12-04 03:36:28 |         MASTER-OAFA | (02h 38m 43.63s , -58d 58m 59.5s) |   C |    60 | 18.2 |        
     642 | 2021-12-04 03:37:48 |         MASTER-OAFA | (02h 16m 25.09s , -49d 29m 44.3s) |   C |    60 | 18.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211204B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31169
SUBJECT: GRB 211204B: Fermi GBM Final Real-time Localization
DATE:    21/12/04 12:00:38 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 11:50:05 UT on 4 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211204B (trigger 660311410.858238 / 211204493).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 267.9, Dec = 13.5 (J2000 degrees, equivalent to J2000 17h 51m, 13d 30'), with a statistical uncertainty of 2.9 degrees.

The angle from the Fermi LAT boresight is 90.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204493/quicklook/glg_skymap_all_bn211204493.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204493/quicklook/glg_healpix_all_bn211204493.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204493/quicklook/glg_lc_medres34_bn211204493.gif


GRB_name: GRB211204B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31170
SUBJECT: Fermi GRB 211204B: Global MASTER-Net observations report 
DATE:    21/12/04 15:00:15 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211204B ( Fermi GBM team, GCN 31169) errorbox  9427 sec after notice time and 9453 sec after trigger time at 2021-12-04 14:27:39 UT, with upper limit up to  17.5 mag. Observations started at twilight.  The observations began at zenith distance = 60 deg. The sun  altitude  is -9.2 deg. 

The galactic latitude b = 19 deg., longitude l = 39 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1803767

We obtain a following upper limits.  

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

    9484 | 2021-12-04 14:27:39 |   MASTER-Kislovodsk | (18h 03m 36.78s , +14d 27m 59.2s) |   C |    60 | 13.5 |        
    9565 | 2021-12-04 14:29:01 |   MASTER-Kislovodsk | (17h 57m 48.43s , +16d 22m 15.0s) |   C |    60 | 13.2 |        
    9646 | 2021-12-04 14:30:21 |   MASTER-Kislovodsk | (17h 41m 55.16s , +16d 23m 20.5s) |   C |    60 | 12.6 |        
    9646 | 2021-12-04 14:30:21 |   MASTER-Kislovodsk | (17h 37m 46.68s , +16d 45m 20.5s) |   C |    60 | 15.0 |        
    9726 | 2021-12-04 14:31:41 |   MASTER-Kislovodsk | (17h 39m 27.88s , +12d 33m 20.9s) |   C |    60 | 12.7 |        
    9726 | 2021-12-04 14:31:41 |   MASTER-Kislovodsk | (17h 35m 25.80s , +12d 55m 14.3s) |   C |    60 | 14.1 |        
    9806 | 2021-12-04 14:33:01 |   MASTER-Kislovodsk | (18h 03m 15.18s , +10d 41m 33.4s) |   C |    60 | 12.6 |        
    9806 | 2021-12-04 14:33:01 |   MASTER-Kislovodsk | (17h 59m 13.52s , +11d 03m 34.1s) |   C |    60 | 14.1 |        
    9886 | 2021-12-04 14:34:22 |   MASTER-Kislovodsk | (17h 47m 40.77s , +10d 40m 25.3s) |   C |    60 | 12.5 |        
    9967 | 2021-12-04 14:35:42 |   MASTER-Kislovodsk | (17h 52m 55.02s , +18d 17m 25.3s) |   C |    60 | 13.4 |        
   10047 | 2021-12-04 14:37:02 |   MASTER-Kislovodsk | (18h 10m 40.56s , +12d 34m 48.2s) |   C |    60 | 12.9 |        
   10047 | 2021-12-04 14:37:02 |   MASTER-Kislovodsk | (18h 06m 35.75s , +12d 56m 55.0s) |   C |    60 | 15.0 |        
   10127 | 2021-12-04 14:38:22 |   MASTER-Kislovodsk | (17h 32m 11.63s , +14d 26m 58.4s) |   C |    60 | 13.4 |        
   10207 | 2021-12-04 14:39:42 |   MASTER-Kislovodsk | (17h 48m 01.00s , +14d 27m 36.9s) |   C |    60 | 13.7 |        
   10207 | 2021-12-04 14:39:42 |   MASTER-Kislovodsk | (17h 43m 56.31s , +14d 49m 36.3s) |   C |    60 | 15.8 |        
   10287 | 2021-12-04 14:41:02 |   MASTER-Kislovodsk | (17h 53m 05.90s , +09d 09m 03.4s) |   C |    60 | 15.6 |        
   10367 | 2021-12-04 14:42:22 |   MASTER-Kislovodsk | (17h 55m 02.32s , +12d 33m 22.2s) |   C |    60 | 14.4 |        
   10367 | 2021-12-04 14:42:23 |   MASTER-Kislovodsk | (17h 50m 59.68s , +12d 55m 22.8s) |   C |    60 | 16.3 |        
   10447 | 2021-12-04 14:43:43 |   MASTER-Kislovodsk | (18h 03m 41.65s , +14d 29m 26.8s) |   C |    60 | 15.0 |        
   10447 | 2021-12-04 14:43:43 |   MASTER-Kislovodsk | (17h 59m 35.55s , +14d 51m 31.8s) |   C |    60 | 16.8 |        
   10527 | 2021-12-04 14:45:03 |   MASTER-Kislovodsk | (17h 57m 43.44s , +16d 22m 19.5s) |   C |    60 | 14.9 |        
   10527 | 2021-12-04 14:45:03 |   MASTER-Kislovodsk | (17h 53m 34.94s , +16d 44m 24.5s) |   C |    60 | 16.4 |        
   10608 | 2021-12-04 14:46:23 |   MASTER-Kislovodsk | (17h 41m 51.06s , +16d 22m 59.9s) |   C |    60 | 13.6 |        
   10608 | 2021-12-04 14:46:23 |   MASTER-Kislovodsk | (17h 37m 43.92s , +16d 44m 58.7s) |   C |    60 | 15.5 |        
   10688 | 2021-12-04 14:47:43 |   MASTER-Kislovodsk | (17h 39m 31.33s , +12d 33m 55.3s) |   C |    60 | 13.0 |        
   10688 | 2021-12-04 14:47:43 |   MASTER-Kislovodsk | (17h 35m 32.52s , +12d 55m 47.8s) |   C |    60 | 16.0 |        
   10768 | 2021-12-04 14:49:03 |   MASTER-Kislovodsk | (18h 03m 09.60s , +10d 39m 24.1s) |   C |    60 | 14.7 |        
   10768 | 2021-12-04 14:49:03 |   MASTER-Kislovodsk | (17h 59m 11.21s , +11d 01m 23.4s) |   C |    60 | 16.8 |        
   10848 | 2021-12-04 14:50:23 |   MASTER-Kislovodsk | (17h 47m 48.46s , +10d 39m 13.7s) |   C |    60 | 14.5 |        
   10848 | 2021-12-04 14:50:23 |   MASTER-Kislovodsk | (17h 43m 51.51s , +11d 01m 07.6s) |   C |    60 | 16.7 |        
   10928 | 2021-12-04 14:51:44 |   MASTER-Kislovodsk | (17h 52m 57.28s , +18d 16m 48.2s) |   C |    60 | 14.9 |        
   11008 | 2021-12-04 14:53:04 |   MASTER-Kislovodsk | (18h 10m 37.58s , +12d 33m 54.2s) |   C |    60 | 15.2 |        
   11008 | 2021-12-04 14:53:04 |   MASTER-Kislovodsk | (18h 06m 36.33s , +12d 55m 58.0s) |   C |    60 | 17.5 |        
   11089 | 2021-12-04 14:54:24 |   MASTER-Kislovodsk | (17h 32m 16.73s , +14d 28m 32.1s) |   C |    60 | 15.4 |        
   11169 | 2021-12-04 14:55:44 |   MASTER-Kislovodsk | (17h 47m 54.17s , +14d 27m 54.3s) |   C |    60 | 15.7 |        
   11169 | 2021-12-04 14:55:44 |   MASTER-Kislovodsk | (17h 43m 52.73s , +14d 49m 51.0s) |   C |    60 | 17.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211204C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31171
SUBJECT: GRB 211204C: Fermi GBM Final Real-time Localization
DATE:    21/12/04 21:47:28 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 21:37:00 UT on 4 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211204C (trigger 660346625.552088 / 211204901).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 346.4, Dec = 55.8 (J2000 degrees, equivalent to J2000 23h 05m, 55d 47'), with a statistical uncertainty of 1.7 degrees.

The angle from the Fermi LAT boresight is 146.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204901/quicklook/glg_skymap_all_bn211204901.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204901/quicklook/glg_healpix_all_bn211204901.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211204901/quicklook/glg_lc_medres34_bn211204901.gif


GRB_name: GRB211204C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31172
SUBJECT: Fermi GRB 211204C: Global MASTER-Net observations report 
DATE:    21/12/04 22:00:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 211204C ( Fermi GBM team, GCN 31171) errorbox  113 sec after notice time and 142 sec after trigger time at 2021-12-04 21:39:22 UT, with upper limit up to  17.9 mag. The observations began at zenith distance = 36 deg. The sun  altitude  is -46.1 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211204C errorbox  592 sec after notice time and 621 sec after trigger time at 2021-12-04 21:47:21 UT, with upper limit up to  13.2 mag. The observations began at zenith distance = 59 deg. The sun  altitude  is -67.2 deg. 

The galactic latitude b = -4 deg., longitude l = 109 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1804120

We obtain a following upper limits.  

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

     157 | 2021-12-04 21:39:22 |          MASTER-IAC | (23h 28m 59.46s , +57d 30m 33.7s) |  P| |    30 | 16.9 |        
     202 | 2021-12-04 21:39:22 |          MASTER-IAC | (23h 28m 59.46s , +57d 30m 33.7s) |  P| |   120 | 17.7 |  Coadd 
     212 | 2021-12-04 21:40:12 |          MASTER-IAC | (23h 28m 51.98s , +57d 29m 37.7s) |  P| |    40 | 17.2 |        
     277 | 2021-12-04 21:41:12 |          MASTER-IAC | (23h 28m 57.77s , +57d 29m 49.8s) |  P| |    50 | 17.3 |        
     352 | 2021-12-04 21:42:22 |          MASTER-IAC | (23h 28m 54.98s , +57d 31m 18.2s) |  P| |    60 | 17.4 |        
     641 | 2021-12-04 21:46:41 |          MASTER-IAC | (23h 02m 55.70s , +55d 44m 36.6s) |  P| |   120 | 17.7 |        
     641 | 2021-12-04 21:46:41 |          MASTER-IAC | (23h 04m 33.66s , +55d 38m 30.9s) |  P- |   120 | 16.5 |        
     681 | 2021-12-04 21:47:21 |   MASTER-Kislovodsk | (23h 05m 40.54s , +55d 45m 23.3s) |  P- |   120 | 12.3 |        
     846 | 2021-12-04 21:47:21 |   MASTER-Kislovodsk | (23h 05m 40.54s , +55d 45m 23.3s) |  P- |   450 | 12.3 |  Coadd 
     791 | 2021-12-04 21:49:01 |          MASTER-IAC | (23h 02m 50.22s , +55d 44m 07.7s) |  P| |   140 | 17.8 |        
     791 | 2021-12-04 21:49:01 |          MASTER-IAC | (23h 04m 28.38s , +55d 38m 01.6s) |  P- |   140 | 16.7 |        
     837 | 2021-12-04 21:49:42 |   MASTER-Kislovodsk | (23h 05m 37.26s , +55d 46m 40.5s) |  P- |   150 | 12.4 |        
     966 | 2021-12-04 21:51:41 |          MASTER-IAC | (23h 02m 49.52s , +55d 45m 09.1s) |  P| |   170 | 17.9 |        
     966 | 2021-12-04 21:51:41 |          MASTER-IAC | (23h 04m 27.93s , +55d 39m 02.5s) |  P- |   170 | 16.9 |        
    1022 | 2021-12-04 21:52:32 |   MASTER-Kislovodsk | (23h 05m 37.19s , +55d 45m 32.4s) |  P- |   180 | 13.2 |        


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


GRB_name: GRB211204C
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31173
SUBJECT: GRB 211204C: GECAM detection
DATE:    21/12/05 07:11:50 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, S. L. Xiong, C. Cai, S. Xiao, P. Zhang, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long burst, 
GRB 211204C, at 2021-12-04T21:37:00.250 UTC (denoted as T0), which was also 
observed by Fermi/GBM (GCN #31171) and INTEGRAL/SPI-ACS (TrigID #9552).
 
GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 25 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_92353020.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 334.1 deg 
Dec: 55.1 deg
Err: 3.8 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_skymap_bdm_92353020_V01.png

GECAM location is consistent with the Fermi/GBM position within the error.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211204C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31174
SUBJECT: GRB 211204C: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/12/05 15:40:48 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (UAlabama), Aaron Tohuvavohu (U Toronto), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT did not successfully trigger on GRB 211204C (T0:
2021-12-04T21:37:00 UTC, Fermi/GBM GCN 31171, GECAM GCN 31173,
INTEGRAL/SPI-ACS trig #9552).

The Fermi/GBM, INTEGRAL, and GECAM notices, distributed in near
real-time, triggered the Swift Mission Operations Center operated
Gamma-ray Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu
et al. 2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 116.1 in a
8.192 s analysis time bin.
Estimated T90 in the detector is 19.5 +/- 0.1 s (15-350 keV).

NITRATES strongly prefers an origin for the burst coming from outside
the coded FOV, with DeltaLLHOut of -520.
An out of FOV origin is consistent with the Fermi/GBM and GECAM localizations.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211206A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31175
SUBJECT: GRB 211206A: AGILE/MCAL detection of a burst
DATE:    21/12/06 22:32:53 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, L. Foffano, E. Menegoni, 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 a burst at T0 = 2021-12-06
19:51:10.80 +/- 0.01 s (UTC). The event lasted about 4.5 s and released a
total number of ~3374 counts in the detector (in the 0.4-100 MeV energy
range), above an average background rate of 599 Hz. The MCAL light curve
shows two main peaks and can be found at
http://www.agilescienceapp.it/notices/075998_GRB_MCAL_565905070.805285.png

The burst is also clearly visible in the AGILE scientific ratemeters of the
SuperAGILE (SA; 20-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and
AntiCoincidence (AC; 50-200 keV) detectors. The event lasted about 5 s and
it released a total number of 853 counts in the SA detector (above a
background rate of 90 Hz), 8286 counts in the MCAL detector (above a
background rate of 1260 Hz), and 18890 counts in the AC detector (above a
background rate of 3600 Hz). The AGILE ratemeter light curves can be found
at http://www.agilescienceapp.it/notices/GRB211206A_AGILE_RM.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: GRB211206A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31176
SUBJECT: GRB 211206A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/12/07 02:42:06 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (UAlabama), Aaron Tohuvavohu (U Toronto), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT detected a rate increase onboard (trigger ##1088092) but did
not localize GRB 211206A (T0: 2021-12-06T19:51:10 UTC, AGILE/MCAL GCN
31175, CALET trig #1322855382).

The CALET notice, distributed in near real-time, triggered the Swift
Mission Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).

Upon trigger by this notice, GUANO sent a command to the Swift Burst
Alert Telescope (BAT) to save 90 seconds of BAT event-mode data from
[-45,+45] seconds around the time of the burst. All the requested
event mode data was delivered to the ground.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 74.6 in a
4.096 s analysis time bin.
Estimated T90 in the detector is 6.6 +/- 0.2 s (15-350 keV).

NITRATES results strongly prefer an origin for the burst coming from
outside the coded FOV, with DeltaLLHOut of -55.5.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211204C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31177
SUBJECT: IPN triangulation of GRB 211204C
DATE:    21/12/07 04:14:27 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the HEND/Mars Odyssey teams,

K. Hurley, on behalf of the IPN,

A. Ridnaia, D. Frederiks, D. Svinkin, A. Lysenko,
and T. Cline on behalf of the Konus-Wind team,

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

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

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

and

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

The long-duration GRB 211204C
(Fermi GBM detection: Fermi GBM team, GCN 31171;
GECAM detection: Zhang et al., GCN 31173;
Swift/BAT-GUANO detection: DeLaunay et al., GCN 31174)
was detected by Fermi (GBM trigger 660346625), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), GECAM-B (GRD),
and Swift (BAT) at about 77820 s UT (21:37:00).
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:
  338.952 (22h 35m 48s) +52.171 (+52d 10' 15")
 Corners:
  338.910 (22h 35m 38s) +49.891 (+49d 53' 29")
  338.806 (22h 35m 14s) +49.979 (+49d 58' 43")
  339.068 (22h 36m 16s) +54.400 (+54d 24' 01")
  339.176 (22h 36m 42s) +54.316 (+54d 18' 59")
 ---------------------------------------------
The error box area is 1084 sq. armin, and its maximum
dimension is 4.5 deg (the minimum one is 4.1 arcmin).
The Sun distance was 105 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi GBM on-ground calculated localization (GCN Circ. 31171) and
GECAM-B automatic on-ground localization (GCN Circ. 31173).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB211204_T77823/IPN

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


GRB_name: GRB211204C
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31178
SUBJECT: GRB 211204C: AstroSat CZTI detection
DATE:    21/12/07 06:17:15 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

 V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao
(IITB), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale
(PRL) report on behalf of the AstroSat CZTI collaboration: 

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of the long GRB 211204C, which was
also detected by Fermi (GCN 31171), GECAM (Zhang et al., GCN 31173) and
Swift/BAT-GUANO (DeLaunay et al., GCN 31174) with IPN triangulation
reported (GCN 31177).  

The source was clearly detected in the 20-200 keV energy range. The
light curve peaks at 2021-12-04 21:37:06.50 UT. The measured peak count
rate associated with the burst is 426 (+57, -23) cts/s above the
background in the combined data of two quadrants, with a total of 3173
(+195, -220) cts. The local mean background count rate was 500 (+2, -2)
cts/s. Using cumulative rates, we measure a T90 of 13 (+2,  -1) s. 

It was also clearly detected in the CsI anticoincidence (Veto) detector
in the 100-500 keV energy range. The light curve peaks at 2021-12-04
21:37:04.16 UT. The measured peak count rate is 592 (+80, -46) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 4150 (+285, -354) cts. The local mean background count rate was
1677 (+4, -4) cts/s. We measure a T90 of 10 (+1, -1) 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: GRB211206B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31179
SUBJECT: GRB 211206B: AstroSat CZTI detection
DATE:    21/12/07 09:58:49 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

 V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao
(IITB), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale
(PRL) report on behalf of the AstroSat CZTI collaboration: 

Analysis of AstroSat CZTI data with the ML pipeline (Abraham et al.,
2021, MNRAS, 504, 3084) and CIFT framework (Sharma et al., 2021, JApA,
42, 73) showed the detection of a long GRB 211206B.  

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2021-12-06 15:10:29.50 UT. The measured peak count rate associated with
the burst is 910 (+60, -65) cts/s above the background in the combined
data of two quadrants, with a total of 8746 (+348, -398) cts. The local
mean background count rate was 467 (+2, -2) cts/s. Using cumulative
rates, we measure a T90 of 27 (+1, -1) 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 2021-12-06 15:10:29.09 UT. The
measured peak count rate is 823 (+77, -80) cts/s above the background in
the combined Veto data of four quadrants, with a total of 7227 (+633,
-607) cts. The local mean background count rate was 1432 (+3, -5) cts/s.
We measure a T90 of 27 (+4, -2) 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: GRB211206A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31180
SUBJECT: GRB 211206A: AstroSat CZTI detection
DATE:    21/12/07 10:12:35 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao
(IITB), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale
(PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of a long GRB 211206A which was
also detected by AGILE/MCAL (Ursi et al., GCN 31175) and Swift/BAT-GUANO
(DeLaunay et al., GCN 31176). 

The source was clearly detected in the 20-200 keV energy range. The
light curve peaks at 2021-12-06 19:51:12.450 UT. The measured peak count
rate associated with the burst is 776 (+198, -60) cts/s above the
background in the combined data of two quadrants, with a total of 1947
(+221, -223) cts. The local mean background count rate was 443 (+7, -10)
cts/s. Using cumulative rates, we measure a T90 of 4.3 (+1.3, -0.6) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector
in the 100-500 keV energy range. The light curve peaks at 2021-12-06
19:51:12.088 UT. The measured peak count rate is 1509 (+86, -95) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 5582 (+310, -365) cts. The local mean background count rate was
1466 (+4, -4) cts/s. We measure a T90 of 6.6 (+1.5, -1.6) 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 [1]. 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. 

Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB211206A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31181
SUBJECT: GRB 211206A: Not observable by Fermi-GBM
DATE:    21/12/07 18:45:02 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

O.J. Roberts (USRA/NASA-MSFC) reports on behalf of the Fermi-GBM team:

Fermi-GBM was passing through the South Atlantic Anomaly from 9.4 minutes prior to the trigger time of GRB 211206A (GCNs 31175,31176 and 31180), until 14.3 minutes after, over which time the GBM detectors were disabled.


GRB_name: GRB211207A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31182
SUBJECT: GRB 211207A: Swift detection of a burst with an optical counterpart
DATE:    21/12/07 21:04:39 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC & INAF-OAR),
S. Dichiara (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), T. M. Parsotan (GSFC/UMBC/CRESSTII) and
B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 20:52:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211207A (trigger=1088376).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 149.625, -24.352 which is 
   RA(J2000) = 09h 58m 30s
   Dec(J2000) = -24d 21' 05"
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 4 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 20:54:17.2 UT, 80.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 149.62449, -24.35970 which is
equivalent to:
   RA(J2000)  = 09h 58m 29.88s
   Dec(J2000) = -24d 21' 34.9"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 27 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 (4.94 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.1
(+3.50/-2.89) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 84 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 09:58:29.78 = 149.62408
  DEC(J2000) = -24:21:31.1  = -24.35863
with a 90%-confidence error radius of about 0.62 arc sec. This position is 3.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.45 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.050. 

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: GRB211207A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31183
SUBJECT: Swift GRB 211207A: Global MASTER-Net observations report 
DATE:    21/12/07 22:18:25 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 211207A ( E. Ambrosi et al., GCN 31182) errorbox  4112 sec after notice time and 4128 sec after trigger time at 2021-12-07 22:01:45 UT, with upper limit up to  15.3 mag. The observations began at zenith distance = 87 deg. The sun  altitude  is -66.2 deg. 

The galactic latitude b = 24 deg., longitude l = 261 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1807266

We obtain a following upper limits.  

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

    4219 |   MASTER-Kislovodsk |   C |   180 | 14.6 |        
    4219 |   MASTER-Kislovodsk |   C |   180 | 14.3 |        
    4419 |   MASTER-Kislovodsk |   C |   180 | 14.5 |        
    4419 |   MASTER-Kislovodsk |   C |   180 | 14.2 |        
    4619 |   MASTER-Kislovodsk |   C |   180 | 14.8 |        
    4619 |   MASTER-Kislovodsk |   C |   180 | 14.4 |        
    4819 |   MASTER-Kislovodsk |   C |   180 | 15.3 |        
    4819 |   MASTER-Kislovodsk |   C |   180 | 14.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211207A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31184
SUBJECT: GRB 211207A: Enhanced Swift-XRT position
DATE:    21/12/08 00:01:26 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 1514 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 211207A, 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 = 149.62381, -24.35968 which is equivalent
to:

RA (J2000): 09h 58m 29.71s
Dec (J2000): -24d 21' 34.8"

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

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

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


GRB_name: GRB211207A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31185
SUBJECT: GRB 211207A: Swift-XRT refined Analysis
DATE:    21/12/08 10:17:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.3 ks of XRT data for GRB 211207A (Ambrosi et al. GCN
Circ. 31182), from 87 s to 39.7 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Osborne et al. (GCN Circ. 31184).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.92 (+0.08, -0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.08 (+0.29, -0.27). The
best-fitting absorption column is  1.7 (+0.9, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 4.9 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 4.9 x 10^20 cm^-2
Excess significance: 2.7 sigma
Photon index:      2.08 (+0.29, -0.27)

If the light curve continues to decay with a power-law decay index of
0.92, the count rate at T+24 hours will be 1.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.3 x
10^-14 (8.7 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01088376.

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


GRB_name: GRB211204C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31186
SUBJECT: GRB 211204C: Fermi GBM detection
DATE:    21/12/08 13:29:44 GMT
FROM:    Boyan A. Hristov at UAH  <bah0046@uah.edu>

Boyan A. Hristov (UAH) reports on behalf of the Fermi GBM Team:

At 21:37:00.55 UT on 04 December 2021, the Fermi Gamma-Ray Burst
Monitor (GBM) triggered and located GRB 211204C (trigger 660346625
/ 211204901), which was also detected by GECAM-B (Zhang et al. 2021,
GCN 31173), INTEGRAL SPI_ACS (trigger num. 9552), Swift/BAT-GUANO
(Tohuvavohu et al., GCN 31174), AstroSat CZTI detection (Waratkar et
al., GCN 31178) and was triangulated by IPN (Ridnaia et al., GCN
31177).

The GECAM localization and the IPN triangulation are consistent with
the GBM localization (GCN 31171).

The GBM light curve consists of a single spike with a duration (T90)
of about 17.41 s +/- 2.00 s (50-300 keV).  The time-averaged spectrum
from T0+0.003 s to T0+19.456 s is adequately fit by a Band function
with Epeak = 287.90 +/- 34.30 keV, alpha = -0.71 +/- 0.09, and beta =
-2.37 +/- 0.19.

The event fluence (10-1000 keV) in this time interval is (2.827 +/-
0.105)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting
from T0+7.040 s in the 10-1000 keV band is 19.9063 +/- 1.1 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: GRB211207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31188
SUBJECT: GRB 211207A: VLT/X-shooter redshift
DATE:    21/12/08 14:25:11 GMT
FROM:    Benjamin Schneider at CEA  <benjamin.schneider@cea.fr>

B. Schneider (CEA Paris-Saclay), L. Izzo (DARK/NBI), D. B. Malesani (Univ. Radboud and DAWN/NBI), J. P. U. Fynbo (DAWN/NBI), K. Wiersema (Univ. Lancaster), V. Dâ€™Elia (ASI/SSDC, INAF/OAR), K. E. Heintz (Univ. Iceland and DAWN/NBI), report on behalf of the Stargate collaboration:

We observed the afterglow of GRB 211207A (Ambrosi et al., GCN 31182) using the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-21000 AA, and consist of 4 exposures of 1200 s each. The observation mid time was 2021 Dec 8.288 UT (10.04 hr after the GRB).

In a 60 s image taken with the acquisition camera on Dec 8.249 UT, we detect the optical afterglow, for which we measure an AB magnitude r = 22.16 +/- 0.05 mag (calibrated against two nearby stars from the Pan-STARRS catalog).

We clearly detect continuum over the wavelength range 3400 - 18000 AA. A trough is visible around 3960 AA, which we identify as due to H I. From detection of multiple absorption features, which we interpret as due to Si II, O I, C II, Fe II, Si IV, C IV, Al II, Mg II, we infer a redshift z = 2.272. An emission line is also detected at 16390 AA, which we interpret as due to [O III] from the GRB host galaxy.

We acknowledge excellent support from the ESO observing staff in Paranal, in particular Joe Anderson, Zahed Wahhaj and Rob van Holstein.


GRB_name: GRB211207A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31189
SUBJECT: GRB 211207A: Swift-BAT refined analysis
DATE:    21/12/08 17:51:09 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),

H. A. Krimm (NSF), S. Laha (GSFC/UMBC),

A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),

D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC),

M. Stamatikos (OSU), (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 211207A (trigger #1088376)
(Ambrosi et al., GCN 31182).  The BAT ground-calculated position is RA, Dec
= 149.601, -24.360 deg which is

   RA(J2000)  =  09h 58m 24.1s

   Dec(J2000) = -24d 21' 37.3"

with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment). The
partial coding was 62%.



The BAT light curve showed a complex structure with a duration of about 4
sec. T90 (15-350 keV) is 3.73 +- 0.87 sec (estimated error including
systematics).



The time-averaged spectrum from T-1.30 to T+2.97 sec is best fit by a
simple power-law model.  The power law index of the time-averaged spectrum
is 1.72 +- 0.30.  The fluence in the 15-150 keV band is 1.9 +- 0.4 x 10^-07
erg/cm2. The 1-sec peak photon flux measured from T-0.15 sec in the 15-150
keV band is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90%
confidence level.



The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1088376/BA/


GRB_name: GRB211130A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31196
SUBJECT: GRB 211130A: MeerLICHT identification of possible afterglow candidate
DATE:    21/12/10 09:16:11 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

S. de Wet (UCT), P.J. Groot (Radboud/UCT/SAAO), A.J. Levan (Radboud),
P.M. Vreeswijk (Radboud), report on behalf of the MeerLICHT consortium:

We observed the field of the Fermi/GBM long GRB candidate GRB 211130A
(Fermi GBM Team, GCN 31151) with the 0.6m wide-field MeerLICHT
optical telescope located at Sutherland, South Africa, starting at
2021-11-30,
18:31:26 UT, approximately 3 hours 15 minutes after the GRB trigger.
With a field of view of 2.7 square degrees, 72 MeerLICHT pointings were
required to cover the GBM sky map to a probability level of 90%. We
observed 67 out of the 72 fields three times on the first night of
observations.
The remaining 5 fields were observed once. All observations were conducted
in the q-band (g+r) with a 60s exposure time. The average 5-sigma full-frame
limiting magnitude was q = 20.79 across the observations.

Following the IPN triangulation of GRB 211130A (Kozyrev et al., GCN 31161),
a refined search for transient candidates in our data reveals a single
promising
afterglow candidate at coordinates:

RA (J2000) = 01:24:52.46 (21.2186d)
Dec (J2000) = -27:41:57.48 (-27.6993d)

calibrated against Gaia DR2. The candidate is, however, located just North
of
the IPN triangulation region, an angular distance of 8.7' from the centre
of the
IPN region and still consistent with the Konus-Wind/GBM triangulation
region.
The candidate was detected at three epochs and appears to show fading
behaviour, with 5-sigma AB magnitudes at time post-trigger of:

q = 19.83 +/- 0.07 at 3.74 hours
q = 20.05 +/- 0.10 at 5.57 hours
q = 20.66 +/- 0.20 at 7.05 hours.

No underlying source is visible in PanSTARRS and Legacy Survey DR9 images
at this position.

MeerLICHT is built and run by a consortium consisting of Radboud
University,
University of Cape Town, the South African Astronomical Observatory, the
University of Oxford, the University of Manchester and the University of
Amsterdam.


GRB_name: GRB211211A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31201
SUBJECT: GRB 211211A: Fermi GBM Final Real-time Localization
DATE:    21/12/11 13:20:10 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 13:09:59 UT on 11 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211211A (trigger 660921004.65092 / 211211549).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 211.3, Dec = 27.1 (J2000 degrees, equivalent to J2000 14h 05m, 27d 06'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 111.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211211549/quicklook/glg_skymap_all_bn211211549.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211211549/quicklook/glg_healpix_all_bn211211549.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211211549/quicklook/glg_lc_medres34_bn211211549.gif


GRB_name: GRB211211A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31202
SUBJECT: GRB 211211A: Swift detection of a bright burst
DATE:    21/12/11 13:32:57 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA),
V. D'Elia (SSDC & INAF-OAR), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (U Tampa),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. M. Parsotan (GSFC/UMBC/CRESSTII) and
B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 13:09:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211211A (trigger=1088940).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 212.272,  +27.884d which is 
   RA(J2000) = 14h 09m 05s
   Dec(J2000) = +27d 53' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Due to a telemetry dropout, the immediately
available BAT lightcurve starts at T+8s, and shows a bright complex
burst that extends at least to T+100s.  At T+8s the count rate is 
300k counts/sec (15-350 keV), but the earlier peak may be significantly
higher. 

The XRT began observing the field at 13:11:18.7 UT, 79.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 212.2912, 27.8899 which is equivalent to:
   RA(J2000)  = 14h 09m 9.89s
   Dec(J2000) = +27d 53' 23.6"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of nominal 150.000 seconds with the White
filter starting 87 seconds after the BAT trigger. No credible afterglow
candidate has been found in the initial data products. Data from the 2.7'x2.7'
sub-image are not available at this time. 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 0.018. 

Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31203
SUBJECT: GRB 211211A: KAIT Optical Afterglow Candidate
DATE:    21/12/11 14:37:08 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on

behalf of the KAIT GRB team:


The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at

Lick Observatory, responded to Swift GRB 211211A (Trigger 1088940)

starting at Dec. 11, 13:46:25 UT. We detected an uncataloged

optical afterglow candidate at position (error ~0.5"):

RA:  14:09:10.09  (J2000)

Dec: +27:53:18.23 (J2000)

We estimate the clear band magnitude ~20.3 in out clear band image

at ~0.63 hours after burst. We can not estimate the variability

at this time, further observations are encouraged.

We also notice the afterglow candidate location is very close to a

SDSS galaxy (SDSS ID: 1237665429707096375, with r = 19.53 mag),

it is unclear if the galaxy is related to the GRB.


GRB_name: GRB211207A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31204
SUBJECT: GRB 211207A: Swift/UVOT Detection
DATE:    21/12/11 16:03:37 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) and Ambrosi (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 211207A
85 s after the BAT trigger (Ambrosi et al., GCN Circ. 31182).
A source consistent with the XRT position
(Osborne et al. GCN Circ. 31184)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  09:58:29.79 = 149.62412 (deg.)
    Dec (J2000) = -24:21:31.3  = -24.35869 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: 

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

white               85          234          147         17.52 +/- 0.04
v                  627         1595          117        >18.5
b                  553          743           36         19.08 +/- 0.31
u                  297          546          246         18.15 +/- 0.09
w1                 677         1470           97        >18.7
m2                 652         1272           39        >18.7
w2                 776         1570           78        >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.050 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB211211A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31205
SUBJECT: GRB 211211A: Enhanced Swift-XRT position
DATE:    21/12/11 19:41:53 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 1514 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 211211A, 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 = 212.29202, +27.88857 which is equivalent
to:

RA (J2000): 14h 09m 10.09s
Dec (J2000): +27d 53' 18.8"

with an uncertainty of 2.1 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: GRB211211A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31206
SUBJECT: Fermi GRB 211211A: Global MASTER-Net observations report 
DATE:    21/12/11 21:45:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 211211A ( Fermi GBM team, GCN 31201) errorbox  29692 sec after notice time and 29701 sec after trigger time at 2021-12-11 21:25:00 UT, with upper limit up to  13.5 mag. The observations began at zenith distance = 39 deg. The sun  altitude  is -17.3 deg. 

The galactic latitude b = 73 deg., longitude l = 37 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1810719

We obtain a following upper limits.  

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

   29791 | 2021-12-11 21:25:00 |         MASTER-Amur | (14h 05m 02.43s , +27d 44m 17.7s) |   C |   180 | 13.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211211B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31207
SUBJECT: GRB 211211B: Fermi GBM Final Real-time Localization
DATE:    21/12/11 21:58:52 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 21:48:42 UT on 11 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211211B (trigger 660952127.842124 / 211211909).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 228.1, Dec = 48.4 (J2000 degrees, equivalent to J2000 15h 12m, 48d 23'), with a statistical uncertainty of 7.3 degrees.

The angle from the Fermi LAT boresight is 128.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211211909/quicklook/glg_skymap_all_bn211211909.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211211909/quicklook/glg_healpix_all_bn211211909.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211211909/quicklook/glg_lc_medres34_bn211211909.gif


GRB_name: GRB211211B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31208
SUBJECT: Fermi GRB 211211B: Global MASTER-Net observations report 
DATE:    21/12/11 23:15:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211211B ( Fermi GBM team, GCN 31207) errorbox  48 sec after notice time and 56 sec after trigger time at 2021-12-11 21:49:39 UT, with upper limit up to  17.7 mag. The observations began at zenith distance = 78 deg. The sun  altitude  is -68.9 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211211B errorbox  54 sec after notice time and 62 sec after trigger time at 2021-12-11 21:49:45 UT, with upper limit up to  18.0 mag. The observations began at zenith distance = 78 deg. The sun  altitude  is -67.9 deg. 

MASTER-Amur robotic telescope  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 211211B errorbox  927 sec after notice time and 935 sec after trigger time at 2021-12-11 22:04:17 UT, with upper limit up to  15.4 mag. Observations started at twilight.  The observations began at zenith distance = 31 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = 55 deg., longitude l = 80 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1811001

We obtain a following upper limits.  

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

      62 | 2021-12-11 21:49:39 |      MASTER-Tavrida | (15h 19m 29.04s , +54d 09m 36.8s) |   C |    10 | 13.2 |        
      87 | 2021-12-11 21:49:39 |      MASTER-Tavrida | (15h 19m 06.97s , +54d 08m 19.9s) |   C |    60 | 14.1 |  Coadd 
      68 | 2021-12-11 21:49:45 |   MASTER-Kislovodsk | (15h 28m 31.52s , +53d 24m 51.8s) |   C |    10 | 15.9 |        
      68 | 2021-12-11 21:49:45 |   MASTER-Kislovodsk | (15h 21m 58.64s , +53d 50m 33.7s) |   C |    10 | 16.1 |        
      88 | 2021-12-11 21:49:45 |   MASTER-Kislovodsk | (15h 21m 58.63s , +53d 50m 33.7s) |   C |    50 | 17.1 |  Coadd 
      96 | 2021-12-11 21:50:08 |      MASTER-Tavrida | (15h 19m 22.56s , +54d 08m 37.1s) |   C |    20 | 13.8 |        
     102 | 2021-12-11 21:50:15 |   MASTER-Kislovodsk | (15h 28m 31.16s , +53d 23m 30.2s) |   C |    20 | 16.5 |        
     103 | 2021-12-11 21:50:15 |   MASTER-Kislovodsk | (15h 21m 58.79s , +53d 49m 12.9s) |   C |    20 | 16.5 |        
     135 | 2021-12-11 21:50:48 |      MASTER-Tavrida | (15h 19m 29.05s , +54d 08m 39.9s) |   C |    20 | 13.8 |        
     142 | 2021-12-11 21:50:55 |   MASTER-Kislovodsk | (15h 28m 33.12s , +53d 24m 46.6s) |   C |    20 | 16.4 |        
     142 | 2021-12-11 21:50:55 |   MASTER-Kislovodsk | (15h 22m 00.64s , +53d 50m 30.5s) |   C |    20 | 16.5 |        
     180 | 2021-12-11 21:51:27 |      MASTER-Tavrida | (15h 19m 26.15s , +54d 10m 30.8s) |   C |    30 | 14.5 |        
     187 | 2021-12-11 21:51:35 |   MASTER-Kislovodsk | (15h 28m 27.33s , +53d 24m 12.0s) |   C |    30 | 16.6 |        
     187 | 2021-12-11 21:51:35 |   MASTER-Kislovodsk | (15h 21m 55.00s , +53d 49m 57.0s) |   C |    30 | 16.8 |        
     232 | 2021-12-11 21:51:35 |   MASTER-Kislovodsk | (15h 21m 55.00s , +53d 49m 57.0s) |   C |   120 | 17.8 |  Coadd 
     234 | 2021-12-11 21:52:16 |      MASTER-Tavrida | (15h 19m 26.25s , +54d 08m 42.8s) |   C |    40 | 14.8 |        
     294 | 2021-12-11 21:52:16 |      MASTER-Tavrida | (15h 19m 26.24s , +54d 08m 42.8s) |   C |   160 | 15.4 |  Coadd 
     242 | 2021-12-11 21:52:24 |   MASTER-Kislovodsk | (15h 28m 27.53s , +53d 25m 10.1s) |   C |    40 | 16.7 |        
     242 | 2021-12-11 21:52:25 |   MASTER-Kislovodsk | (15h 21m 55.10s , +53d 50m 56.4s) |   C |    40 | 17.1 |        
     298 | 2021-12-11 21:53:15 |      MASTER-Tavrida | (15h 19m 29.93s , +54d 10m 14.2s) |   C |    50 | 15.1 |        
     307 | 2021-12-11 21:53:24 |   MASTER-Kislovodsk | (15h 28m 33.19s , +53d 24m 10.4s) |   C |    50 | 16.9 |        
     307 | 2021-12-11 21:53:24 |   MASTER-Kislovodsk | (15h 22m 00.97s , +53d 49m 57.8s) |   C |    50 | 17.4 |        
     377 | 2021-12-11 21:54:25 |      MASTER-Tavrida | (15h 19m 22.55s , +54d 09m 34.8s) |   C |    70 | 14.8 |        
     387 | 2021-12-11 21:54:34 |   MASTER-Kislovodsk | (15h 28m 27.37s , +53d 23m 09.2s) |   C |    70 | 17.1 |        
     387 | 2021-12-11 21:54:34 |   MASTER-Kislovodsk | (15h 21m 55.37s , +53d 48m 57.6s) |   C |    70 | 17.7 |        
     793 | 2021-12-11 22:01:26 |   MASTER-Kislovodsk | (15h 03m 20.24s , +48d 17m 01.7s) |   C |    60 | 17.5 |        
     793 | 2021-12-11 22:01:26 |   MASTER-Kislovodsk | (14h 57m 35.40s , +48d 42m 39.2s) |   C |    60 | 17.6 |        
     873 | 2021-12-11 22:02:45 |   MASTER-Kislovodsk | (15h 15m 23.56s , +50d 11m 46.1s) |   C |    60 | 17.6 |        
     873 | 2021-12-11 22:02:45 |   MASTER-Kislovodsk | (15h 09m 24.59s , +50d 37m 27.7s) |   C |    60 | 17.5 |        
     965 | 2021-12-11 22:04:17 |         MASTER-Amur | (15h 11m 57.70s , +48d 34m 22.0s) |   C |    60 | 15.0 |        
    1034 | 2021-12-11 22:05:26 |   MASTER-Kislovodsk | (15h 39m 17.59s , +50d 09m 32.2s) |   C |    60 | 17.4 |        
    1034 | 2021-12-11 22:05:26 |   MASTER-Kislovodsk | (15h 32m 54.37s , +50d 35m 18.8s) |   C |    60 | 17.5 |        
    1052 | 2021-12-11 22:05:44 |         MASTER-Amur | (15h 01m 31.13s , +46d 39m 07.4s) |   C |    60 | 15.4 |        
    1114 | 2021-12-11 22:06:46 |   MASTER-Kislovodsk | (15h 04m 40.67s , +52d 04m 22.8s) |   C |    60 | 17.9 |        
    1114 | 2021-12-11 22:06:46 |   MASTER-Kislovodsk | (14h 57m 59.20s , +52d 29m 57.6s) |   C |    60 | 17.9 |        
    1140 | 2021-12-11 22:07:13 |         MASTER-Amur | (15h 23m 36.85s , +46d 38m 23.4s) |   C |    60 | 15.1 |        
    1154 | 2021-12-11 22:07:26 |      MASTER-Tavrida | (14h 36m 41.26s , +50d 57m 43.7s) |   C |    60 | 13.7 |        
    1194 | 2021-12-11 22:08:06 |   MASTER-Kislovodsk | (14h 53m 12.04s , +46d 24m 20.3s) |   C |    60 | 17.6 |        
    1194 | 2021-12-11 22:08:06 |   MASTER-Kislovodsk | (14h 47m 16.29s , +46d 49m 47.5s) |   C |    60 | 17.5 |        
    1227 | 2021-12-11 22:08:39 |         MASTER-Amur | (15h 14m 03.89s , +44d 44m 34.7s) |   C |    60 | 15.2 |        
    1274 | 2021-12-11 22:09:26 |   MASTER-Kislovodsk | (15h 29m 33.47s , +52d 04m 07.2s) |   C |    60 | 17.5 |        
    1274 | 2021-12-11 22:09:26 |   MASTER-Kislovodsk | (15h 22m 53.07s , +52d 29m 44.6s) |   C |    60 | 17.3 |        
    1318 | 2021-12-11 22:10:10 |         MASTER-Amur | (14h 52m 34.06s , +44d 45m 42.6s) |   C |    60 | 15.1 |        
    1354 | 2021-12-11 22:10:46 |   MASTER-Kislovodsk | (14h 40m 29.24s , +48d 18m 30.0s) |   C |    60 | 17.8 |        
    1354 | 2021-12-11 22:10:46 |   MASTER-Kislovodsk | (14h 34m 19.38s , +48d 43m 49.9s) |   C |    60 | 17.6 |        
    1425 | 2021-12-11 22:11:57 |         MASTER-Amur | (15h 35m 02.56s , +48d 32m 41.3s) |   C |    60 | 14.5 |        
    1514 | 2021-12-11 22:13:26 |         MASTER-Amur | (15h 06m 01.53s , +42d 52m 01.5s) |   C |    60 | 14.6 |        
    1604 | 2021-12-11 22:14:56 |         MASTER-Amur | (15h 35m 24.20s , +44d 45m 24.3s) |   C |    60 | 14.2 |        
    1694 | 2021-12-11 22:16:26 |         MASTER-Amur | (14h 45m 08.95s , +42d 51m 52.7s) |   C |    60 | 14.4 |        
    1782 | 2021-12-11 22:17:55 |         MASTER-Amur | (15h 26m 47.66s , +42d 51m 18.2s) |   C |    60 | 13.9 |        
    1793 | 2021-12-11 22:18:06 |      MASTER-Tavrida | (14h 49m 24.58s , +50d 58m 43.9s) |   C |    60 | 14.4 |        
    1955 | 2021-12-11 22:20:48 |   MASTER-Kislovodsk | (15h 03m 25.56s , +48d 18m 28.4s) |   C |    60 | 17.5 |        
    1955 | 2021-12-11 22:20:48 |   MASTER-Kislovodsk | (14h 57m 36.27s , +48d 43m 48.7s) |   C |    60 | 17.6 |        
    2036 | 2021-12-11 22:22:08 |   MASTER-Kislovodsk | (15h 15m 28.60s , +50d 10m 45.5s) |   C |    60 | 17.7 |        
    2036 | 2021-12-11 22:22:08 |   MASTER-Kislovodsk | (15h 09m 25.52s , +50d 36m 11.1s) |   C |    60 | 17.5 |        
    2116 | 2021-12-11 22:23:28 |   MASTER-Kislovodsk | (15h 39m 26.60s , +50d 11m 23.0s) |   C |    60 | 17.4 |        
    2116 | 2021-12-11 22:23:28 |   MASTER-Kislovodsk | (15h 33m 24.69s , +50d 37m 00.4s) |   C |    60 | 17.3 |        
    2196 | 2021-12-11 22:24:48 |   MASTER-Kislovodsk | (15h 04m 35.48s , +52d 05m 31.5s) |   C |    60 | 17.8 |        
    2196 | 2021-12-11 22:24:48 |   MASTER-Kislovodsk | (14h 58m 16.33s , +52d 30m 53.4s) |   C |    60 | 17.9 |        
    2206 | 2021-12-11 22:24:58 |      MASTER-Tavrida | (15h 17m 40.23s , +54d 45m 44.4s) |   C |    60 | 13.2 |        
    2276 | 2021-12-11 22:26:09 |   MASTER-Kislovodsk | (14h 53m 11.30s , +46d 24m 55.2s) |   C |    60 | 17.5 |        
    2276 | 2021-12-11 22:26:09 |   MASTER-Kislovodsk | (14h 47m 35.23s , +46d 50m 12.3s) |   C |    60 | 17.5 |        
    2356 | 2021-12-11 22:27:29 |   MASTER-Kislovodsk | (15h 29m 39.21s , +52d 05m 03.7s) |   C |    60 | 17.4 |        
    2356 | 2021-12-11 22:27:29 |   MASTER-Kislovodsk | (15h 23m 20.91s , +52d 30m 35.1s) |   C |    60 | 17.2 |        
    2364 | 2021-12-11 22:27:36 |      MASTER-Tavrida | (14h 36m 42.00s , +50d 57m 48.0s) |   C |    60 | 14.5 |        
    2437 | 2021-12-11 22:28:49 |   MASTER-Kislovodsk | (14h 40m 23.07s , +48d 17m 12.8s) |   C |    60 | 17.7 |        
    2437 | 2021-12-11 22:28:49 |   MASTER-Kislovodsk | (14h 34m 33.60s , +48d 42m 22.3s) |   C |    60 | 17.7 |        
    2517 | 2021-12-11 22:30:09 |   MASTER-Kislovodsk | (14h 39m 18.39s , +44d 54m 30.2s) |   C |    60 | 17.5 |        
    2517 | 2021-12-11 22:30:09 |   MASTER-Kislovodsk | (14h 44m 42.79s , +44d 29m 18.4s) |   C |    60 | 17.5 |        
    2999 | 2021-12-11 22:38:11 |   MASTER-Kislovodsk | (14h 57m 29.97s , +48d 43m 11.7s) |   C |    60 | 17.7 |        
    2999 | 2021-12-11 22:38:11 |   MASTER-Kislovodsk | (15h 03m 31.06s , +48d 18m 12.2s) |   C |    60 | 17.9 |        
    3079 | 2021-12-11 22:39:31 |   MASTER-Kislovodsk | (15h 09m 11.73s , +50d 35m 59.9s) |   C |    60 | 17.6 |        
    3079 | 2021-12-11 22:39:31 |   MASTER-Kislovodsk | (15h 15m 26.97s , +50d 10m 55.6s) |   C |    60 | 17.9 |        
    3159 | 2021-12-11 22:40:51 |   MASTER-Kislovodsk | (15h 33m 13.90s , +50d 35m 40.6s) |   C |    60 | 17.5 |        
    3159 | 2021-12-11 22:40:51 |   MASTER-Kislovodsk | (15h 39m 27.64s , +50d 10m 26.1s) |   C |    60 | 17.6 |        
    3239 | 2021-12-11 22:42:11 |   MASTER-Kislovodsk | (14h 58m 09.07s , +52d 32m 01.9s) |   C |    60 | 17.2 |        
    3239 | 2021-12-11 22:42:11 |   MASTER-Kislovodsk | (15h 04m 41.08s , +52d 07m 00.1s) |   C |    60 | 17.5 |        
    3319 | 2021-12-11 22:43:31 |   MASTER-Kislovodsk | (14h 47m 27.42s , +46d 48m 42.7s) |   C |    60 | 17.6 |        
    3319 | 2021-12-11 22:43:31 |   MASTER-Kislovodsk | (14h 53m 14.39s , +46d 23m 46.6s) |   C |    60 | 17.8 |        
    3332 | 2021-12-11 22:43:44 |      MASTER-Tavrida | (14h 36m 44.62s , +50d 58m 08.0s) |   C |    60 | 12.9 |        
    3399 | 2021-12-11 22:44:52 |   MASTER-Kislovodsk | (15h 23m 10.29s , +52d 31m 47.8s) |   C |    60 | 17.1 |        
    3399 | 2021-12-11 22:44:52 |   MASTER-Kislovodsk | (15h 29m 40.77s , +52d 06m 38.1s) |   C |    60 | 17.6 |        
    3479 | 2021-12-11 22:46:12 |   MASTER-Kislovodsk | (14h 34m 23.97s , +48d 43m 39.8s) |   C |    60 | 17.4 |        
    3479 | 2021-12-11 22:46:12 |   MASTER-Kislovodsk | (14h 40m 24.33s , +48d 18m 49.1s) |   C |    60 | 17.6 |        
    3560 | 2021-12-11 22:47:32 |   MASTER-Kislovodsk | (14h 39m 06.34s , +44d 56m 38.7s) |   C |    60 | 17.6 |        
    3560 | 2021-12-11 22:47:32 |   MASTER-Kislovodsk | (14h 44m 36.77s , +44d 31m 48.2s) |   C |    60 | 18.0 |        
    3640 | 2021-12-11 22:48:52 |   MASTER-Kislovodsk | (14h 33m 22.36s , +52d 31m 38.2s) |   C |    60 | 17.8 |        
    3640 | 2021-12-11 22:48:52 |   MASTER-Kislovodsk | (14h 39m 48.67s , +52d 06m 46.7s) |   C |    60 | 18.0 |        
    3720 | 2021-12-11 22:50:12 |   MASTER-Kislovodsk | (15h 39m 21.09s , +54d 23m 34.1s) |   C |    60 | 17.4 |        
    3720 | 2021-12-11 22:50:13 |   MASTER-Kislovodsk | (15h 46m 01.90s , +53d 58m 19.4s) |   C |    60 | 17.8 |        
    3800 | 2021-12-11 22:51:33 |   MASTER-Kislovodsk | (15h 07m 11.54s , +41d 06m 44.3s) |   C |    60 | 17.1 |        
    3800 | 2021-12-11 22:51:33 |   MASTER-Kislovodsk | (15h 12m 08.11s , +40d 41m 46.6s) |   C |    60 | 16.8 |        
    3881 | 2021-12-11 22:52:53 |   MASTER-Kislovodsk | (15h 03m 36.52s , +56d 19m 40.2s) |   C |    60 | 17.5 |        
    3881 | 2021-12-11 22:52:53 |   MASTER-Kislovodsk | (15h 10m 25.45s , +55d 54m 44.6s) |   C |    60 | 17.7 |        
    3961 | 2021-12-11 22:54:13 |   MASTER-Kislovodsk | (14h 25m 29.97s , +46d 49m 27.1s) |   C |    60 | 17.5 |        
    3961 | 2021-12-11 22:54:13 |   MASTER-Kislovodsk | (14h 31m 00.83s , +46d 24m 51.5s) |   C |    60 | 17.8 |        
    4027 | 2021-12-11 22:55:19 |      MASTER-Tavrida | (14h 49m 26.00s , +50d 57m 49.9s) |   C |    60 | 13.3 |        
    4041 | 2021-12-11 22:55:33 |   MASTER-Kislovodsk | (15h 54m 18.95s , +46d 49m 22.7s) |   C |    60 | 16.7 |        
    4041 | 2021-12-11 22:55:33 |   MASTER-Kislovodsk | (15h 59m 45.87s , +46d 24m 09.1s) |   C |    60 | 16.5 |        
    4106 | 2021-12-11 22:56:38 |      MASTER-Tavrida | (15h 03m 57.00s , +54d 43m 31.1s) |   C |    60 | 13.9 |        
    4185 | 2021-12-11 22:57:58 |      MASTER-Tavrida | (15h 17m 48.48s , +54d 43m 33.8s) |   C |    60 | 14.1 |        
    4201 | 2021-12-11 22:58:13 |   MASTER-Kislovodsk | (15h 30m 55.06s , +56d 19m 44.4s) |   C |    60 | 17.6 |        
    4201 | 2021-12-11 22:58:13 |   MASTER-Kislovodsk | (15h 37m 43.52s , +55d 54m 46.7s) |   C |    60 | 18.0 |        
    4281 | 2021-12-11 22:59:34 |   MASTER-Kislovodsk | (14h 47m 03.07s , +41d 07m 46.3s) |   C |    60 | 17.6 |        
    4281 | 2021-12-11 22:59:34 |   MASTER-Kislovodsk | (14h 52m 01.22s , +40d 43m 08.7s) |   C |    60 | 17.8 |        
    4343 | 2021-12-11 23:00:36 |      MASTER-Tavrida | (14h 25m 26.24s , +50d 58m 56.1s) |   C |    60 | 17.0 |        
    4362 | 2021-12-11 23:00:54 |   MASTER-Kislovodsk | (14h 32m 21.12s , +43d 01m 00.6s) |   C |    60 | 17.7 |        
    4362 | 2021-12-11 23:00:54 |   MASTER-Kislovodsk | (14h 37m 29.56s , +42d 36m 30.0s) |   C |    60 | 18.0 |        
    4422 | 2021-12-11 23:01:55 |      MASTER-Tavrida | (14h 37m 46.29s , +54d 45m 17.2s) |   C |    60 | 17.6 |        
    4442 | 2021-12-11 23:02:14 |   MASTER-Kislovodsk | (16h 06m 47.23s , +48d 41m 53.8s) |   C |    60 | 17.1 |        
    4501 | 2021-12-11 23:03:14 |      MASTER-Tavrida | (15h 39m 16.15s , +52d 51m 09.4s) |   C |    60 | 13.0 |        
    4522 | 2021-12-11 23:03:34 |   MASTER-Kislovodsk | (14h 39m 19.05s , +44d 56m 31.0s) |   C |    60 | 17.6 |        
    4522 | 2021-12-11 23:03:34 |   MASTER-Kislovodsk | (14h 44m 37.49s , +44d 31m 57.7s) |   C |    60 | 18.0 |        
    4660 | 2021-12-11 23:05:52 |      MASTER-Tavrida | (14h 51m 33.35s , +54d 43m 54.0s) |   C |    60 | 17.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31209
SUBJECT: GRB 211211A: Swift-BAT refined analysis
DATE:    21/12/12 03:14:09 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+360 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 211211A (trigger #1088940)
(D'Ai et al., GCN Circ. 31202).  The BAT ground-calculated position is
RA, Dec = 212.272, 27.884 deg which is
   RA(J2000)  =  14h 09m 05.2s
   Dec(J2000) = +27d 53' 03.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 21%.

The mask-weighted light curve shows a multi-peaked structure that
starts at ~T0 and ends at ~T+140 s. The main peak occurs at ~T+7 s.
T90 (15-350 keV) is 51.37 +- 0.80 sec (estimated error including
systematics).

The time-averaged spectrum from T0 to T+142.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.02.  The fluence in the 15-150 keV band is 1.5 +- 0.02 x 10^-04
erg/cm2.
The 1-sec peak photon flux measured from T+6.86 sec in the 15-150 keV band
is 155.0 +- 3.1 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/1088940/BA/


GRB_name: GRB211211A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31210
SUBJECT: GRB 211211A: Fermi GBM observation
DATE:    21/12/12 07:31:36 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 13:09:59.651 UT on 11 December 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211211A (trigger 660921004 / 211211549)
which was also detected by the Swift/BAT (D'Ai et al., GCN 31202). The
Fermi GBM Final Real-time Localization (GCN 31201) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 106.5 degrees.

The GBM light curve consists of an exceptionally bright emission made
up of three separate pulses
with a duration (T90) of about 34.3s (50-300 keV).
The time-averaged spectrum from T0-1.264 s to T0+54.033 s is
best fit by a Band function with Epeak = 646.8 +/- 7.8 keV,
alpha = -1.3 +/- 0.00, and beta = -2.4 +/- 0.02

The event fluence (10-1000 keV) in this time interval is
(5.4 +/- 0.01)E-04 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+6.8 s in the 10-1000 keV band
is 324.9 +/- 1.5 ph/s/cm^2.

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

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


GRB_name: GRB211212A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31211
SUBJECT: GRB 211212A: Fermi GBM Final Real-time Localization
DATE:    21/12/12 09:38:28 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 09:28:03 UT on 12 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211212A (trigger 660994088.510652 / 211212394).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 144.4, Dec = -2.3 (J2000 degrees, equivalent to J2000 09h 37m, -2d 17'), with a statistical uncertainty of 4.8 degrees.

The angle from the Fermi LAT boresight is 114.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211212394/quicklook/glg_skymap_all_bn211212394.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211212394/quicklook/glg_healpix_all_bn211212394.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211212394/quicklook/glg_lc_medres34_bn211212394.gif


GRB_name: GRB211211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31212
SUBJECT: GRB 211211A: Swift-XRT refined Analysis
DATE:    21/12/12 11:39:52 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), E. Ambrosi 
(INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR),
D.N. Burrows (PSU), J. D. Gropp (PSU), J.A. Kennea (PSU), A.P.
Beardmore (U. Leicester) and A. D'Ai report on behalf of the Swift-XRT
team:

We have analysed 8.1 ks of XRT data for GRB 211211A (D'Ai et al. GCN
Circ. 31202), from 69 s to 74.2 ks after the  BAT trigger. The data
comprise 214 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN Circ. 31205).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.99 (+0.13, -0.10). At T+171 s  the decay
steepens to an alpha of 4.19 (+0.31, -0.21). The light curve breaks
again at T+704 s to a decay with alpha=-0.4 (+0.7, -0.6),  before a
final break at T+5861 s s after which the decay index is 1.63 (+0.15,
-0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.80 (+/-0.03). The
best-fitting absorption column is  4.5 (+/-0.8) x 10^20 cm^-2, in
excess of the Galactic value of 1.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.50 (+0.12, -0.06)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.2 x 10^-11 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.8 (+2.5, -0.0) x 10^20 cm^-2
Galactic foreground: 1.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.50 (+0.12, -0.06)

If the light curve continues to decay with a power-law decay index of
1.63, the count rate at T+24 hours will be 0.020 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.7 x
10^-13 (8.9 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/01088940.

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


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31213
SUBJECT: GRB 211211A: Nanshan/NEXT optical observations
DATE:    21/12/12 11:42:12 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 211211A detected by Fermi (Fermi GBM team, 
GCN 31201) and Swift (D'Ai et al., GCN 31202) using the NEXT-0.6m 
optical telescope located at Nanshan, Xinjiang, China. Observations 
started at 23:01:09 UT on 2021-12-11, i.e., 9.85 hr after the BAT 
trigger, and 10x200 s frames in the Sloan r-filter as well as 12x200 s 
frames in the Sloan z-filter were obtained.

The optical afterglow candidate of the GRB reported by KAIT (Zheng & 
Filippenko, GCN 31203), consistent with the enhanced Swift-XRT position 
(Beardmore et al., GCN 31205), is detected in our stacked r- and z-band 
images. Preliminary photometry is as follows:

T_mid-T0 (hr)    Mag     MagErr  Filter
10.34               20.29    0.07        r
10.68               19.9      0.3         z

both calibrated with nearby PS1 stars.

We note that the NEXT's r-band magnitude is comparable to that of KAIT 
in the clear band, although the time interval of the two observations is 
~10 hr.


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31214
SUBJECT: GRB 211211A: LCO Optical Observations
DATE:    21/12/12 12:50:00 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

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

We observed Swift GRB 211211A (D'Ai et al., GCN 31202) with the LCO 1-m Sinistro instrument at the Teide Observatory, Tenerife site, on December 12, from 05:57 to 06:33 UT (corresponding to 16.8 to 17.4 hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 3x400s exposures in R and I bands. We detect a source in both R-band and I-band that is consistent with the Swift Enhanced XRT coordinates (Osborne, et al., GCN 31212) and the optical observations by KAIT (Zheng et al., GCN 31203) and Nanshan/NEXT (Jiang et al., GCN 31213); there appears to be fading in the R band compared to those earlier observations. The following magnitudes are calculated using the USNO-B.1 catalog as reference:

R=20.83+/-0.09

I=21.49+/-0.25

These magnitudes are not corrected for galactic extinction.

R.S. is funded by NSF AST grant #1831682


GRB_name: GRB211212B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31215
SUBJECT: GRB 211212B: Fermi GBM Final Real-time Localization
DATE:    21/12/12 12:56:37 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 LONG GRB

At 12:46:26 UT on 12 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211212B (trigger 661005991.438832 / 211212532).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 41.8, Dec = -25.6 (J2000 degrees, equivalent to J2000 02h 47m, -25d 36'), with a statistical uncertainty of 5.7 degrees.

The angle from the Fermi LAT boresight is 98.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211212532/quicklook/glg_skymap_all_bn211212532.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211212532/quicklook/glg_healpix_all_bn211212532.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211212532/quicklook/glg_lc_medres34_bn211212532.gif


GRB_name: GRB211211A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31216
SUBJECT: Swift GRB 211211A: Global MASTER-Net observations report 
DATE:    21/12/12 13:10:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) was pointed to the Swift GRB 211211A ( A. D'Ai et al., GCN 31202) errorbox  29687 sec after notice time and 29621 sec after trigger time at 2021-12-11 21:25:00 UT, with upper limit up to  13.5 mag. The observations began at zenith distance = 39 deg. The sun  altitude  is -17.3 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 211211A errorbox  35200 sec after notice time and 35135 sec after trigger time at 2021-12-11 22:56:53 UT, with upper limit up to  19.1 mag. The observations began at zenith distance = 80 deg. The sun  altitude  is -59.4 deg. 

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 211211A errorbox  37423 sec after notice time and 37358 sec after trigger time at 2021-12-11 23:33:56 UT, with upper limit up to  17.2 mag. The observations began at zenith distance = 79 deg. The sun  altitude  is -58.1 deg. 

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory) was pointed to the Swift GRB 211211A errorbox  52860 sec after notice time and 52795 sec after trigger time at 2021-12-12 03:51:13 UT, with upper limit up to  18.9 mag. The observations began at zenith distance = 76 deg. The sun  altitude  is -50.4 deg. 

The galactic latitude b = 72 deg., longitude l = 39 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1810696

We obtain a following upper limits.  

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

   29712 |         MASTER-Amur |   C |   180 | 13.5 |        
   35165 |   MASTER-Kislovodsk |   C |    60 | 17.4 |        
   35165 |   MASTER-Kislovodsk |   C |    60 | 17.5 |        
   35706 |   MASTER-Kislovodsk |   C |   180 | 18.0 |        
   35706 |   MASTER-Kislovodsk |   C |   180 | 18.2 |        
   36851 |   MASTER-Kislovodsk |   C |    60 | 17.4 |        
   36851 |   MASTER-Kislovodsk |   C |    60 | 17.7 |        
   37448 |      MASTER-Tavrida |   C |   180 | 17.1 |        
   37472 |   MASTER-Kislovodsk |   C |   180 | 18.3 |        
   37472 |   MASTER-Kislovodsk |   C |   180 | 18.6 |        
   38013 |   MASTER-Kislovodsk |   C |    60 | 17.5 |        
   38013 |   MASTER-Kislovodsk |   C |    60 | 18.0 |        
   38452 |      MASTER-Tavrida |   C |    60 | 17.0 |        
   39166 |      MASTER-Tavrida |   C |    60 | 17.2 |        
   39404 |      MASTER-Tavrida |   C |    60 | 17.1 |        
   40330 |      MASTER-Tavrida |   C |    60 | 15.6 |        
   40488 |      MASTER-Tavrida |   C |    60 | 15.1 |        
   40697 |   MASTER-Kislovodsk |   C |   180 | 18.3 |        
   40697 |   MASTER-Kislovodsk |   C |   180 | 18.4 |        
   41906 |      MASTER-Tavrida |   C |    60 | 12.8 |        
   41960 |   MASTER-Kislovodsk |   C |    60 | 18.0 |        
   42458 |      MASTER-Tavrida |   C |    60 | 12.2 |        
   42921 |   MASTER-Kislovodsk |   C |    60 | 18.3 |        
   43375 |      MASTER-Tavrida |   C |   180 | 13.2 |        
   43594 |      MASTER-Tavrida |   C |    60 | 12.0 |        
   43883 |   MASTER-Kislovodsk |   C |    60 | 18.3 |        
   48892 |   MASTER-Kislovodsk |   C |   180 | 18.9 |        
   48892 |   MASTER-Kislovodsk |   C |   180 | 19.1 |        
   49751 |      MASTER-Tavrida |   C |   180 | 14.4 |        
   49972 |      MASTER-Tavrida |   C |    60 | 13.9 |        
   50256 |   MASTER-Kislovodsk |   C |   180 | 18.5 |        
   50256 |   MASTER-Kislovodsk |   C |   180 | 18.5 |        
   50288 |      MASTER-Tavrida |   C |    60 | 13.2 |        
   51619 |   MASTER-Kislovodsk |   C |   180 | 16.8 |        
   51619 |   MASTER-Kislovodsk |   C |   180 | 14.5 |        
   52825 |          MASTER-IAC |   C |    60 | 16.3 |        
   52905 |          MASTER-IAC |   C |    60 | 14.0 |        
   52985 |          MASTER-IAC |   C |    60 | 17.3 |        
   54066 |      MASTER-Tavrida |   C |    60 | 15.2 |        
   54626 |          MASTER-IAC |   C |    60 | 17.4 |        
   54706 |          MASTER-IAC |   C |    60 | 17.4 |        
   54786 |          MASTER-IAC |   C |    60 | 17.6 |        
   55666 |          MASTER-IAC |   C |    60 | 17.5 |        
   55746 |          MASTER-IAC |   C |    60 | 17.9 |        
   56120 |          MASTER-IAC |   C |    60 | 17.9 |        
   59363 |          MASTER-IAC |   C |   180 | 18.7 |        
   59363 |          MASTER-IAC |   C |   180 | 18.7 |        
   60352 |          MASTER-IAC |   C |   180 | 18.9 |        
   60352 |          MASTER-IAC |   C |   180 | 18.7 |        
   61693 |          MASTER-IAC |   C |   180 | 18.9 |        
   61693 |          MASTER-IAC |   C |   180 | 18.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211211A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31217
SUBJECT: GRB 211211A: MITSuME Akeno optical observation
DATE:    21/12/12 13:18:20 GMT
FROM:    Naohiro Ito at Tokyo Tech  <n.ito@hp.phys.titech.ac.jp>

N. Ito, R. Hosokawa, K. L. Murata, Y. Imai, Y. Takamatsu, M. Takaku, M.
Niwano, R. Noto, S. Sato, R. Yamaguchi, Y. Yatsu, and N. Kawai (TokyoTech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 211211A (The Fermi GBM team GCN Circular
#31201, A. D'Ai et al. GCN Circular #31202, WeiKang Zheng and Alexei V.
Filippenko GCN Circular #31203, A.P. Beardmore et al. GCN Circular #31205,
V. Lipunov et al. GCN Circular #31206, M. Stamatikos et al. GCN Circular
#31209, J.Mangan et al. GCN Circular #31210, J.P. Osborne et al. GCN
Circular #31212, S.Q. Jiang et al. GCN Circular #31213, R. Strausbaugh and
A. Cucchiara GCN Circular #32214) with the optical three color (g', Rc, and
Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno. The
observation with a series of 60 sec exposures was carried out from
2021-12-11 17:32:12 UT (~4.4 hours after the Fermi trigger) to 2021-12-11
21:20:21 UT. We stacked the images with good conditions.

We marginally detected the optical afterglow candidate reported by the KAIT
observation (WeiKang Zheng and Alexei V. Filippenko GCN Circular #31203),
Nanshan/NEXT observation (S.Q. Jiang et al. GCN Circular #31213) and LCO
observation (R. Strausbaugh and A. Cucchiara GCN Circular #32214) in our
g'-, Rc- and Ic- band images. The candidate in our images is blended with
the nearby SDSS galaxy (SDSS ID: 1237665429707096375, reported by GCN
Circular #31203). We performed forced photometry at the position of the
candidate against the nearby galaxy. The magnitudes and the 5-sigma limits
of the stacked images are as follows.

T0+[hour] | MID-UT | T-EXP[sec] | candidate magnitude | 5-sigma limits
------------------------------------------------------------------------------------------------
6.3 | 2021-12-11 19:25:34 | 6600 | g'=20.4 +/- 0.2, Rc=20.3 +/- 0.1,
Ic=20.4 +/- 0.3 | g'>20.2, Rc>20.7, Ic>19.7
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time

We used id 141492123232234127 of PS1 catalog for flux calibration. The
conversion from PS1 r and i band to our Rc and Ic band is by the equation
of Tonry et al. (2012), Table. 6. The magnitudes are expressed in the AB
system. The images were processed in real-time through the MITSuME GPU
reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24;
https://github.com/MNiwano/Eclaire).


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31218
SUBJECT: GRB 211211A: Afterglow detection from CAFOS/2.2m CAHA
DATE:    21/12/12 13:53:45 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (Obs. Cote dâ€™Azur), D.A. Kann, C. Thoene, 
J.F. Agui Fernandez, M. Blazek (HETH/IAA-CSIC) and 
A. Guijarro (CAHA) report:

We observed the optical afterglow of GRB 211211A (Fermi team 
GCN31201; Dâ€™Ai et al. GCN31202; Zheng and Filipenko GCN 
31203) with CAFOS, mounted on the 2.2m telescope, at the Calar 
Alto Observatory (AlmerÃ­a, Spain). The observation started at 
04:54 UT (15.73 hr after the GRB) and consisted of 30x90s in i-band.

The optical afterglow is well detected at a magnitude (AB) of 
i = 20.83+/-0.05, as compared to field stars from the SDSS catalogue. 
This magnitude confirms the plateau or very shallow decay phase 
undergone by the afterglow light curve since the early detection 
(Zheng and Filipenko GCN 31203) already noted by Jiang et al. 
(GCN 31213) and consistent with the observations of Strausbaugh 
& Cucchiara (GCN 31214) and Ito et al. (GCN 31217).


GRB_name: GRB211212B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31219
SUBJECT: Fermi GRB 211212B: Global MASTER-Net observations report 
DATE:    21/12/12 15:30:22 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211212B ( Fermi GBM team, GCN 31215) errorbox  8709 sec after notice time and 8719 sec after trigger time at 2021-12-12 15:11:46 UT, with upper limit up to  16.5 mag. Observations started at twilight.  The observations began at zenith distance = 79 deg. The sun  altitude  is -16.8 deg. 

The galactic latitude b = -64 deg., longitude l = 216 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1811649

We obtain a following upper limits.  

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

    8750 | 2021-12-12 15:11:46 |   MASTER-Kislovodsk | (02h 41m 53.74s , -21d 27m 00.2s) |   C |    60 | 15.2 |        
    8750 | 2021-12-12 15:11:46 |   MASTER-Kislovodsk | (02h 46m 15.18s , -21d 51m 32.5s) |   C |    60 | 14.2 |        
    8830 | 2021-12-12 15:13:06 |   MASTER-Kislovodsk | (02h 27m 34.20s , -23d 22m 20.3s) |   C |    60 | 16.0 |        
    8830 | 2021-12-12 15:13:06 |   MASTER-Kislovodsk | (02h 31m 59.43s , -23d 46m 57.2s) |   C |    60 | 14.6 |        
    8910 | 2021-12-12 15:14:26 |   MASTER-Kislovodsk | (02h 39m 57.26s , -19d 33m 20.3s) |   C |    60 | 15.9 |        
    8910 | 2021-12-12 15:14:26 |   MASTER-Kislovodsk | (02h 44m 16.08s , -19d 57m 50.2s) |   C |    60 | 14.8 |        
    8991 | 2021-12-12 15:15:46 |   MASTER-Kislovodsk | (02h 56m 00.66s , -19d 34m 20.2s) |   C |    60 | 15.9 |        
    8991 | 2021-12-12 15:15:47 |   MASTER-Kislovodsk | (03h 00m 18.76s , -19d 58m 55.3s) |   C |    60 | 14.7 |        
    9391 | 2021-12-12 15:22:27 |   MASTER-Kislovodsk | (02h 44m 07.50s , -23d 21m 15.0s) |   C |    60 | 16.4 |        
    9391 | 2021-12-12 15:22:27 |   MASTER-Kislovodsk | (02h 48m 32.74s , -23d 45m 57.3s) |   C |    60 | 15.0 |        
    9471 | 2021-12-12 15:23:47 |   MASTER-Kislovodsk | (02h 29m 47.79s , -25d 16m 23.8s) |   C |    60 | 16.5 |        
    9471 | 2021-12-12 15:23:47 |   MASTER-Kislovodsk | (02h 34m 17.22s , -25d 41m 08.8s) |   C |    60 | 14.6 |        
    9551 | 2021-12-12 15:25:07 |   MASTER-Kislovodsk | (02h 58m 17.43s , -21d 27m 52.8s) |   C |    60 | 16.2 |        
    9551 | 2021-12-12 15:25:07 |   MASTER-Kislovodsk | (03h 02m 38.95s , -21d 52m 34.8s) |   C |    60 | 14.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211211B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31220
SUBJECT: GRB 211211B: GECAM detection
DATE:    21/12/12 15:31:57 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, Y. Q. Zhang, S. L. Xiong, C. Cai, P. Zhang, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, W. C. Xue, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long burst, 
GRB 211211B, at 2021-12-11T21:48:43.050 UTC (denoted as T0), which was also 
observed by Fermi/GBM (GCN #31207).
 
GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 20 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_92958523.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 225.2 deg 
Dec: 55.28 deg
Err: 3.52 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

GECAM location is consistent with the Fermi/GBM position within the error.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31221
SUBJECT: GRB 211211A: NOT optical spectroscopy
DATE:    21/12/12 16:24:56 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Univ. Radboud and DAWN/NBI), J. P. U. Fynbo (DAWN/NBI), 
A. de Ugarte Postigo (Obs. Cote d'Azur), L. Izzo (DARK/NBI), S. Fu, D. 
Xu, Z. Zhu (NAOC/CAS), N. R. Tanvir (Univ. Leicester), A. A. Djupvik 
(NOT), report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 211211A (D'Ai et al., GCN 
31202; Zheng & Filippenko, GCN 31203) using the Nordic Optical Telescope 
(NOT) equipped with the ALFOSC instrument. Images were secured in the 
SDSS r, g and i filters.

At the mean time of Dec 12.24 UT (16.6 hr after the GRB), we measure a 
magnitude r = 20.89 +- 0.05 AB, calibrated against nearby stars from the 
Pan-STARRS survey. Our measurement is in agreement with those by 
Strausbaugh & Cucchiara (GCN 31214) and de Ugarte Postigo et al. (GCN 
31218), taken at a comparable epoch. Compared to the magnitudes reported 
by Zheng & Filippenko (GCN 31203), Ito et al. (GCN 31217) and Jang (GCN 
31213), our data confirm the unusually slow decay,

We report for the afterglow the following coordinates (0.3" uncertainty):

RA = 14:09:10.12
Dec = +27:53:18.1

A bright, extended object (r ~ 19.5) is visible about 5.5" to the N-E of 
the afterglow (as already pointed out by Zheng & Filippenko, GCN 31203), 
which is also visible in the SDSS, Pan-STARRS, and Legacy surveys.

A spectrum was secured covering both the afterglow and the nearby galaxy 
(wavelength range 3700-9400 AA). A weak emission line is detected on top 
of the host galaxy trace at 7063 AA, which could be due to Halpha at z = 
0.076. This is marginally consistent with the SDSS photometric redshift 
0.140 +- 0.0375, unlike other interpretations of the same line.

No clear absorption or emission features are detected in the afterglow 
trace. This may be due to the modest S/N, and is also consistent with a 
low redshift, as is the detection of the afterglow in all the UVOT UV 
filters (Swift observation ID 1088940000).

It is not clear at the present stage whether the afterglow is physically 
associated with the galaxy at z = 0.076. While the sky proximity and the 
low redshift are indeed suggestive, the physical offset at z = 0.076 
would be about 8 kpc (in projection), an unusually large value for long 
GRBs. There is also no visible emission in the archival images down to r 
~ 24 (AB) at the location of the afterglow, which would be unusual for a 
long GRB at z = 0.076.

Moreover, if placed at z = 0.076, GRB 211211A would be an outlier of the 
the Amati relation (e.g. Nava et al. 2012, MNRAS, 421, 1256), with E_iso 
= 1.4*10^54 erg and E_peak ~ 700 keV (using the Fermi/GBM prompt 
properties from Mangan et al., GCN 31210).

Overall, a moderate-redshift GRB (with z > 0.076) is consistent with the 
available information. The detection of an emerging supernova could 
clarify the situation. We encourage further photometric and 
spectroscopic follow-up of this potentially interesting event.


GRB_name: GRB211211A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31222
SUBJECT: GRB 211211A: Swift/UVOT detection
DATE:    21/12/12 18:19:57 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 211211A
92 s after the BAT trigger (D'Ai et al., GCN Circ. 31202).
A fading source consistent with the XRT position
(Beardmore et al. GCN Circ. 31205) and optical position
(Zheng & Filippenko, GCN Circ. 31203) is detected in the initial
UVOT exposures.

Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag
wh_FC               92          242          147      18.93+/-0.22
wh                3906         4106          196      18.33+/-0.09
wh               68215        68397          179            >19.74
b                 3701         3901          196      18.97+/-0.28
b                16837        17437          587      19.27+/-0.28
b                67303        68210          885      19.70+/-0.24
v                 4317         4517          196            >18.33
u                 3496         5012          275      18.26+/-0.16
u                15924        16831          885      18.44+/-0.11
u                57177        74247          362            >18.89
w1                4727         4927          196      17.46+/-0.16
m2                4522         4721          196      17.58+/-0.19
m2               21678        22153          467      18.18+/-0.18
w2                4112         4312          196      17.30+/-0.15
w2               61756        62656          885      18.94+/-0.24

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.018 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB211211A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31223
SUBJECT: GRB 211211A: incorrect E_iso value in GCN 31221
DATE:    21/12/12 18:45:59 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Radboud Univ. and DAWN/NBI) reports:

The GRB 211211A E_iso value reported by Malesani et al. (GCN 31221) is 
incorrect. Using the Fermi GBM fluence 5.4*10^-4 erg cm^-2 (Mangan et 
al., GCN 31210), the corresponding E_iso value is 6.9*10^51 erg, 
assuming the GRB is at z = 0.076.

The conclusion that GRB 211211A would not be consistent with the Amati 
relation if at z = 0.076 was based on the correct E_iso value, and still 
holds. This may indicate that the GRB lies in fact at a higher redshift.

I sincerely apologize for any confusion caused by this mistake, and I am 
grateful to those who pointed it out, including Peter Veres, D. 
Alexander Kann, and Lorenzo Amati. No blame should be assigned to the 
other co-authors of GCN 31221, who saw an earlier draft which did not 
contain the mistake.


GRB_name: GRB211212A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31224
SUBJECT: Fermi GRB 211212A: Global MASTER-Net observations report 
DATE:    21/12/12 19:00:20 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 211212A ( Fermi GBM team, GCN 31211) errorbox  21907 sec after notice time and 21915 sec after trigger time at 2021-12-12 15:33:19 UT, with upper limit up to  15.4 mag. The observations began at zenith distance = 69 deg. The sun  altitude  is -63.1 deg. 

The galactic latitude b = 35 deg., longitude l = 238 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1811480

We obtain a following upper limits.  

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

   21946 | 2021-12-12 15:33:19 |         MASTER-Amur | (09h 15m 49.56s , +01d 02m 52.5s) |   C |    60 | 15.2 |        
   22303 | 2021-12-12 15:39:16 |         MASTER-Amur | (09h 31m 47.79s , +02d 57m 44.9s) |   C |    60 | 14.7 |        
   22842 | 2021-12-12 15:48:15 |         MASTER-Amur | (09h 30m 59.57s , +01d 03m 34.5s) |   C |    60 | 14.9 |        
   22932 | 2021-12-12 15:49:45 |         MASTER-Amur | (09h 15m 45.16s , +01d 04m 23.1s) |   C |    60 | 15.4 |        
   23112 | 2021-12-12 15:52:45 |         MASTER-Amur | (09h 46m 54.10s , +02d 56m 29.7s) |   C |    60 | 14.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211211A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31226
SUBJECT: GRB 211211A: CALET Gamma-Ray Burst Monitor detection
DATE:    21/12/13 08:58:30 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, Y. Akaike, K. Kobayashi (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:

The long bright GRB 211211A (Swift detection: Ambrosi et al.,
GCN Circ. 31202, Stamatikos et al., GCN Circ. 31209;
Fermi GBM observation: Mangan et al., GCN Circ. 31210;
https://gcn.gsfc.nasa.gov/other/211211A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 13:09:57.513 UTC
on 11 December 2021
(http://cgbm.calet.jp/cgbm_trigger/flight/1323263412/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows several partially overlapped multi-peaked
pulses which start at T+3.6 sec, peak at T+9.1 sec,and end at T+73.1 sec.
The T90 and T50 durations measured by the SGM data are 33.8 +- 0.9 sec and
12.1 +- 0.4 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1323263412/

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


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31227
SUBJECT: GRB 211211A: HCT and GIT optical follow up observations
DATE:    21/12/13 11:11:53 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar(IITB), V. Bhalerao(IITB), Rahul Gupta(ARIES), Rigzin Norbu (IAO),
G. C. Anupama(IIA), D. K. Sahu (IIA), S. Barway(IIA), A. Dutta (IIA), B.
Kumar (ARIES), Dimple (ARIES), S.B. Pandey (ARIES), Kuntal Mishra (ARIES)
report on behalf of the HCT and GIT team:

We observed GRB 211211A detected by Fermi GBM (GCN #31201) and Swift-BAT
(A. D'Ai et al., GCN #31202); optical counterpart first reported by W Zheng
and A V. Filippenko, (GCN #31203) with 2.0m Himalayan Chandra Telescope
(HCT) and 0.7m GROWTH-India Telescope (GIT). We obtained a 900-sec exposure
in the Bessell R filter using HCT and multiple 300-sec r' band exposures
with GIT. We obtained the following photometric results:-

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

 JD (mid) | T_mid-T0(hrs) | Exposure | Filter | Magnitude | Tel |

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

 2459560.50469 | 10.94 | 900 sec | Bessell R | 20.30 +/- 0.13 | HCT |

 2459561.47439 | 34.21 | 1500 sec | r' | > 21.19 | GIT |

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

Our results from HCT are similar to R band magnitudes reported in N. Ito
et. al, (GCN #31217) which suggests that there was no significant decay in
the early hours ( <~11 hrs). GIT r' band observations at ~34 hrs did not
detect the afterglow, with a limiting magnitude of 21.19 - confirming the
fading of the afterglow at late times reported by R. Strausbaugh et. al.,
(GCN #31214).

The magnitudes were calibrated by querying the SDSS catalog (Alam+, 2015).
We converted magnitudes to the R band using Lupton (2005) equations for HCT
calibration.


HCT observations were carried out under the ToO program HCT-2021-C3-P02. We
thank HCT and GIT observers, staff for undertaking the observations.

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 (IIA) and the
Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and
IUSSTF. It is located at the Indian Astronomical Observatory (Hanle),
operated by IIA. We acknowledge funding by the IITB alumni batch of 1994,
which partially supports operations of the telescope. Telescope technical
details are available at https://sites.google.com/view/growthindia/.


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31228
SUBJECT: GRB 211211A: Further observations from CAFOS/2.2m CAHA 
DATE:    21/12/13 17:22:44 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (Obs. Cote dâ€™Azur), D.A. Kann, C. Thoene, 
J.F. Agui Fernandez, M. Blazek (HETH/IAA-CSIC), I. Vico and 
A. Guijarro (CAHA) report: 

We obtained a second imaging observation of the optical afterglow 
of GRB 211211A (Fermi team GCN31201; Dâ€™Ai et al. GCN31202; 
Zheng and Filipenko GCN 31203) with CAFOS, mounted on the 
2.2m telescope, at the Calar Alto Observatory (AlmerÃ­a, Spain). 

The observation started at 04:47 UT (39.6 hr after the GRB) and 
consisted of 30x90s in i-band. The optical afterglow is still detected, 
at a magnitude (AB) of i = 22.45+/-0.09, as compared to field stars 
from the SDSS catalogue. With respect to our earlier CAFOS 
photometry (de Ugarte Postigo et al. GCN 31218) this implies a 
rapid decay rate of alpha = 1.65, where F_nu ~ t^-alpha, which 
would indicate a post-jet break evolution.


GRB_name: GRB211211A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31229
SUBJECT: GRB 211211A: Very fast decay observed from CAFOS/2.2mCAHA
DATE:    21/12/14 16:25:45 GMT
FROM:    Antonio de Ugarte Postigo at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (Obs. Cote dâ€™Azur), D.A. Kann, C. Thoene, 
J.F. Agui Fernandez, M. Blazek (HETH/IAA-CSIC), I. Vico and 
A. Guijarro (CAHA) report: 

We obtained further i-band imaging of the afterglow of GRB 211211A 
(Fermi team GCN31201; Dâ€™Ai et al. GCN31202; Zheng and Filipenko 
GCN 31203) from CAFOS/2.2m CAHA 2.66 days after the burst onset.

The observation consisted of 20x120s exposures under good seeing 
and yielded a faint detection. The light curve decay, compared to our 
previous observation from Calar Alto (de Ugarte Postigo et al., GCN 
31228) indicates an extreme decay index of alpha = 3.25+/-0.40. 
This is similar to what is observed from the XRT light curve, which 
currently decays with an index of 3.2 (-0.7,+0.8) 
(https://www.swift.ac.uk/xrt_live_cat/01088940/ <https://www.swift.ac.uk/xrt_live_cat/01088940/>; Evans et al. 2007; 
Evans et al. 2009). We note that this is amongst the fastest post-break
decays that are normally observed for GRB afterglows.

Further observations with larger telescopes are encouraged.


GRB_name: GRB211211A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31230
SUBJECT: GRB 211211A: redshift estimation and SPI-ACS/INTEGRAL detection
DATE:    21/12/14 17:35:39 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

P. Minaev (IKI), A. Pozanenko (IKI) report on behalf of GRB IKI FuN:

We analyzed GRB 211211A (D'Ai et al. GCN 31202; Mangan et al. GCN 31210; 
Tamura et al. GCN 31226) using publicly available data of GBM/Fermi and 
SPI-ACS/INTEGRAL. Using GBM/Fermi we estimate a duration in 7 - 850 keV 
energy band T_90 = 50.6 +/- 0.1 s, while the emission is seen at least 
up to 130 s after the trigger. We performed spectral analysis in time 
interval of (-0.5, 60) s, covering the main part of GRB activity. The 
best fit is obtained for (Band model + thermal component) with following 
parameters: E_p = 758 +/- 13 keV, alpha = -1.21 +/- 0.01, beta = -2.54 
+/- 0.03 and thermal spectral component with kT = 13.9 +/- 0.3 keV. The 
fluence of F = (5.47 +/- 0.01)E-4 erg/cm**2 is obtained in 10 - 1000 keV 
energy band. The  parameter E_p = 758 +/- 13 keV is higher than 
preliminary value presented by GBM team (Mangan et al., GCN 31210) due 
to inclusion of the thermal component in the fit.

Assuming a redshift of z = 0.076 (Malesani et al., GCN 31221) we 
estimated E_iso = (1.161 +/- 0.006)E52 erg in the 1 keV - 10 MeV energy 
band. The burst is placed very close but outside the 2 sigma correlation 
region at E_p,i - E_iso and T_90,i - EH diagrams [1,2], see the Figures in

http://grb.rssi.ru/GRB211211A/GRB211211A_Ep-Eiso-2.png
http://grb.rssi.ru/GRB211211A/GRB211211A_EHD.png

Using T_90,i - EH diagram we found minimal possible redshift value of z 
= 0.080, very close to the redshift of z = 0.076 (Malesani et al., GCN 
31221). Therefore, we consider GRB 211211A as not a significant outlier.

The burst was also detected by SPI-ACS/INTEGRAL. Its duration in the 
SPI-ACS energy band (> 80 keV) is T_90 = 30.0 +/- 0.2 s, while the 
emission is seen up to 70 s. Comparing fluences of long-duration GRBs 
simultaneously recorded by SPI-ACS and Fermi/GBM (Chelovekov et al., in 
preparation) we estimated the GRB 211211A fluence to be 5.5E-4 erg/cm**2 
in the 10-1000 keV energy band (the 95% confidence region 1.6-4 â€“ 1.9E-3 
erg/cm**2, incl. systematics). GRB 211211A is one of the brightest GRBs 
of SPI-ACS/INTEGRAL sample in terms of peak flux (about 40000 cnts/50 
ms). The SPI-ACS light curve of GRB 211211A can be found in

http://grb.rssi.ru/GRB211211A/GRB211211A_SPI-ACS_lc-2.png

[1] - Minaev et al., MNRAS, 492, 1919, 2020
[2] - Minaev et al., Astronomy Letters, 46, 9, 573, 2020


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31232
SUBJECT: GRB 211211A: GMG upper limit
DATE:    21/12/15 02:00:51 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, Y.-X. Xin, and J.-M. Bai (YNAO) report:


We observed the field of GRB 211211A (D'Ai et al. GCN 31202) by the GMG telescope in Yunnan observatories.

The observation began from UT 22:41:02 Dec 12, 2021, about 33.5 hours from the trigger. We could not observe

the optical afterglow down to a magnitude limit of r~22.0.   


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31233
SUBJECT: GRB 211211A: AbAO optical observations
DATE:    21/12/15 15:44:10 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (HSE, IKI), A. Pozanenko (IKI), S. Belkin (IKI), R. Ya. 
Inasaridze (AbAO), D. Datashvili (AbAO), V. R. Ayvazian (AbAO),  G. V. 
Kapanadze (AbAO)  report on behalf of GRB IKI FuN:

We observed  the field of GRB 211211A (Fermi team GCN 31201, D'Ai et al. 
GCN 31202; Mangan et al. GCN 31210; Tamura et al. GCN 31226) with AS-32 
telescope of Abastumani observatory (AbAO) in R-filter on 2021-12-13 
(UT) 02:21:44 and 2021-12-14 (UT) 01:49:33.

In the first epoch we marginally detected an afterglow (Zheng and 
Filippenko GCN 31203; Jiang  et al. GCN  31213; Strausbaugh et al. GCN 
31214; Ito  et al. GCN  31217;  de Ugarte Postigo et al. GCN 
31218,31228,31229; Malesani  et al. GCN 31221; Belles et al. GCN 31222; 
Kumar et al. GCN 31227). In the second epoch we obtained only an upper 
limit.

Preliminary photometry of the field  is following

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

2021-12-13 02:21:44   1.56233  R     36*60   21.6 S/N=3  21.6
2021-12-14 01:49:33   2.52748  R     43*60   n/d  n/d    21.8

The photometry is based on the nearby SDSS stars:
SDSS-DR12
RA DEC R(Lupton transfoemations)
14:09:08.84448 +27:53:54.5604 15.833
14:09:04.53240 +27:54:10.4760 16.701
14:08:57.03480 +27:54:50.2632 17.677
14:08:57.87816 +27:55:06.0924 17.805
14:09:03.80928 +27:55:56.5464 17.104
14:09:07.89072 +27:55:43.9968 18.640


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31234
SUBJECT: GRB 211211A: SAO RAS optical observations
DATE:    21/12/15 17:28:29 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO), O. Spiridonova (SAO), S. Belkin (IKI),
A. Pozanenko (IKI), N. Pankov (HSE, IKI)  report
on behalf of GRB IKI FuN:

We observed  the field of GRB 211211A (Fermi team GCN 31201,
D'Ai et al. GCN 31202; Mangan et al. GCN 31210; Tamura et al.
GCN 31226) with Zeiss-1000 telescope of SAO RAS in Rc-filter
on 2021.12.14 (UT) 02:03:33.

We marginally detected an afterglow (Zheng and Filippenko GCN 31203;
Jiang  et al. GCN 31213; Strausbaugh et al. GCN 31214; Ito  et al.
GCN 31217; de Ugarte Postigo et al. GCN 31218,31228,31229; Malesani et
al. GCN 31221; Belles et al. GCN 31222; Kumar et al. GCN 31227; Pankov
et al. GCN 31233).

Preliminary photometry of the afterglow is following

Date       UT start   t-T0    Filter Exp.   OT   Err.     UL(3sigma)
                        (mid, days)    (s)
2021-12-14 02:03:33   2.55803   Rc   6*600  23.2 S/N=2.5  23.1

The photometry is based on the nearby SDSS stars:
SDSS-DR12
RA          DEC          R(Lupton transformations)
14:09:08.84 +27:53:54.56 15.833
14:09:04.53 +27:54:10.48 16.701
14:08:57.03 +27:54:50.26 17.677
14:08:57.88 +27:55:06.09 17.805
14:09:03.81 +27:55:56.55 17.104
14:09:07.89 +27:55:44.00 18.640

The light curve based on published photometry can be found in
http://grb.rssi.ru/GRB211211A/GRB211211A_LC.png

Using R-photometry we found a single power law decay index of -1.5
between 0.4 and 2.6 days after the burst trigger. However the power
law index between 1.6 days (Pankov et al. GCN 31233) and 2.6 days
(this circ.) we may assume power law index of -3.25 which confirm
very fast decay in i-filter observed by CAFOS/2.2mCAHA
(de Ugarte Postigo et al. GCN 31229). Based on a typical power law
decay of afterglows we may suggest a bump in the LC at ~ 2.5 days
followed by a power law decay index of 1.5.


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31235
SUBJECT: GRB 211211A - Gemini K-band detection
DATE:    21/12/15 21:19:50 GMT
FROM:    Andrew Levan at U.of Leicester  <a.levan@astro.ru.nl>

A.J. Levan (Radboud), J. Rastinejad (Northwestern), B. Gompertz (Birmingham), W. Fong (Northwestern), D. B. Malesani (Radboud), M. Nicholl (Birmingham) report for a larger collaboration:

â€œWe obtained K-band observations of GRB 211211A (Dâ€™Ai et al., GCN 31202) with the Gemini-North Telescope and NIRI. Observations began at 14:40 UT on 15 Dec 2021 (~4 days after the GRB). A total of 900 s of exposure were obtained. 

At the location of the afterglow identified by Zheng & Fillipenko (GCN 31203) we clearly detect a K-band source. Photometry is complicated by the narrow field of view, however, using the 2MASS source at RA, DEC(J2000)=14:09:08,86, 27:53:54.4 with a magnitude of K=12.8, we determine an afterglow magnitude of K = 20.5 +/- 0.1 (Vega) or 22.4 +/- 0.1 (AB). This magnitude is substantially brighter than expected for afterglow emission given the rapid decay observed in the i-band (de Ugarte Postigo et al., GCN 31229), and the relatively blue colours and spectra of the source at earlier times (Malesani et al., GCN 31221; Belles & Dâ€™Ai, GCN 31222).

The rapid fading and relative faintness in the optical apparently rules out a classical long-GRB at z = 0.076, since a supernova akin to those seen in long GRBs at this epoch would have i ~ 20, 4 magnitudes brighter than observed by de Ugarte Postigo et al. (GCN 31229). Alternatively, the prompt light curve appears to show some similarities with GRB 060614, another suggested short-GRB with extended emission (Gehrels et al. 2006 Nature 444 1044). If GRB 211211A is associated with a compact object merger, its large offset relative to the putative host at z = 0.076 may be expected. The absolute magnitude of the source seen in the K-band is -15.2 (AB), comparable to that of AT2017gfo at the same epoch. Hence, while it remains possible that GRB 211211A is a higher redshift event in chance projection with a low redshift galaxy, a compact binary merger at z=0.076 provides a good explanation of the galactic location, rapid optical fading and red colour of the source. 

We thank the Gemini staff for the rapid execution of these observations."


GRB_name: GRB211211A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31236
SUBJECT: GRB 211211A: Insight-HXMT/HE detection
DATE:    21/12/16 06:44:10 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, S. L. Xiong, X. B. Li, C. Cai, Q. Luo, S. Xiao, 
J. C. Liu, W. C. Xue, Q. B. Yi, C. Zhengï¼ŒY. Huang, C. K. Li, 
G. Li, J. Y. Liao, X. Y. Song, 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 2021-12-11T13:09:59.500 (T0), Insight-HXMT/HE detected 
GRB 211211A (trigger ID: HEB211211548) in a routine search of the data, 
which also triggered Fermi/GBM (Fermi GBM Team, GCN #31201),
Swift/BAT (D'Ai A. et al., GCN #31202),  
CALET (Tamura T. et al., GCN #31226) and
INTEGRAL/SPI-ACS (Minaev P. et al., GCN #31230)

URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB211211548_lc.jpg

It should be noted that there is a significant saturation effect (data loss)
during bright parts of this GRB in HXMT. 

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: GRB211216A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31237
SUBJECT: GRB 211216A: Fermi GBM Final Real-time Localization
DATE:    21/12/16 06:57:07 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:45:52 UT on 16 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211216A (trigger 661329957.05626 / 211216282).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 44.4, Dec = -64.3 (J2000 degrees, equivalent to J2000 02h 57m, -64d 17'), with a statistical uncertainty of 1.1 degrees.

The angle from the Fermi LAT boresight is 31.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211216282/quicklook/glg_skymap_all_bn211216282.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211216282/quicklook/glg_healpix_all_bn211216282.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211216282/quicklook/glg_lc_medres34_bn211216282.gif


GRB_name: GRB211216A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31238
SUBJECT: Fermi GRB 211216A: Global MASTER-Net observations report 
DATE:    21/12/16 07:15:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211216A ( Fermi GBM team, GCN 31237) errorbox 2 sec after trigger time at 2021-12-16 06:45:54 UT, with upper limit up to  18.5 mag. The observations began at zenith distance = 56 deg. The sun  altitude  is -26.7 deg. 

The galactic latitude b = -48 deg., longitude l = 283 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1816175

We obtain a following upper limits.  

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

      12 | 2021-12-16 06:45:54 |         MASTER-OAFA | (02h 53m 22.27s , -62d 10m 10.3s) |   C |    20 | 17.1 |        
      57 | 2021-12-16 06:45:54 |         MASTER-OAFA | (02h 53m 22.27s , -62d 10m 10.4s) |   C |   110 | 17.7 |  Coadd 
      57 | 2021-12-16 06:46:33 |         MASTER-OAFA | (03h 00m 27.56s , -62d 56m 56.5s) |   C |    30 | 17.2 |        
     111 | 2021-12-16 06:47:23 |         MASTER-OAFA | (02h 53m 25.66s , -62d 10m 21.1s) |   C |    40 | 16.5 |        
     176 | 2021-12-16 06:48:23 |         MASTER-OAFA | (02h 53m 18.92s , -62d 10m 50.7s) |   C |    50 | 17.3 |        
     253 | 2021-12-16 06:49:35 |         MASTER-OAFA | (02h 53m 18.87s , -62d 09m 50.3s) |   C |    60 | 17.6 |        
     420 | 2021-12-16 06:52:22 |         MASTER-OAFA | (02h 40m 59.42s , -62d 49m 23.1s) |   C |    60 | 17.7 |        
     499 | 2021-12-16 06:53:41 |         MASTER-OAFA | (02h 58m 51.51s , -62d 47m 34.8s) |   C |    60 | 17.7 |        
     614 | 2021-12-16 06:55:01 |         MASTER-OAFA | (02h 57m 39.11s , -63d 45m 40.4s) |   C |   130 | 18.4 |        
     778 | 2021-12-16 06:57:30 |         MASTER-OAFA | (02h 57m 41.60s , -63d 44m 08.1s) |   C |   160 | 18.4 |        
     968 | 2021-12-16 07:00:29 |         MASTER-OAFA | (02h 57m 35.23s , -63d 45m 07.3s) |   C |   180 | 18.5 |        
    1167 | 2021-12-16 07:03:49 |         MASTER-OAFA | (02h 57m 36.92s , -63d 44m 08.1s) |   C |   180 | 18.5 |        
    1367 | 2021-12-16 07:07:08 |         MASTER-OAFA | (02h 57m 42.14s , -63d 45m 07.7s) |   C |   180 | 18.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211216A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31239
SUBJECT: GRB 211216A: BALROG localization (Fermi Trigger 661329957 / GRB 211216282)
DATE:    21/12/16 07:22:31 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
661329957 at 06:45:52 on 16 Dec. 2021 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) = 51.0+/-2.4 deg
Decl.(2000.0) = -62.2+/-4.0 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB211216282/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB211216282/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB211216282/json

                        


GRB_name: GRB211216A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31240
SUBJECT: GRB 211216A: GECAM detection
DATE:    21/12/16 08:22:21 GMT
FROM:    Wangchen Xue at IHEP  <xuewc@ihep.ac.cn>

W. C. Xue, S. Xiao, Y. Q. Zhang, S. L. Xiong, C. Cai, P. Zhang, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long burst, 
GRB 211216A, at 2021-12-16T06:45:56.050 UTC (denoted as T0), which was also 
observed by Fermi/GBM (GCN #31237).
 
GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 20 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_93336356.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 57.22 deg 
Dec: -63.04 deg
Err: 5.71 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

GECAM location is consistent with the Fermi/GBM position within the error.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31242
SUBJECT: GRB 211211A: TNG NIR observations
DATE:    21/12/16 12:40:41 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. D'Avanzo (INAF-OAB), A. Rossi (INAF-OAS), D. B. Malesani (Radboud), V. D'Elia (ASI-SSDC), A. Melandri (INAF-OAB), 
M. De Pasquale (Univ. Messina), S. Piranomonte (INAF-OAR), G. Andreuzzi, A. Garcia de Gurtubai (INAF-TNG) 
on behalf of the CIBO collaboration report:

We observed the field of GRB 211211A (Dâ€™Ai et al., GCN Circ. 31202) with the Italian 3.6m TNG telescope equipped with the 
near-infrared camera NICS. A series of images were obtained with the H filter on 2021-12-16 from 05:51:36 UT to 07:00:51 UT 
(i.e. at a mid time of about 4.7 days after the burst). 

No source is detected at the optical and NIR counterpart position (Zheng & Filippenko, GCN Circ. 31203; Levan et al., GCN Circ. 
31235) down to the following 3sigma upper limit:

H > 20.5 (Vega) or H > 21.9 (AB) 

(calibrated against the 2MASS catalogue).


GRB_name: GRB211216B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31244
SUBJECT: GRB 211216B: Fermi GBM Final Real-time Localization
DATE:    21/12/16 13:31:20 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 13:21:07 UT on 16 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211216B (trigger 661353672.391664 / 211216556).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 100.8, Dec = 60.1 (J2000 degrees, equivalent to J2000 06h 43m, 60d 06'), with a statistical uncertainty of 4.3 degrees.

The angle from the Fermi LAT boresight is 100.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211216556/quicklook/glg_skymap_all_bn211216556.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211216556/quicklook/glg_healpix_all_bn211216556.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211216556/quicklook/glg_lc_medres34_bn211216556.gif


GRB_name: GRB211216B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31246
SUBJECT: GRB 211216B: GECAM detection
DATE:    21/12/16 15:15:27 GMT
FROM:    Wangchen Xue at IHEP  <xuewc@ihep.ac.cn>

W. C. Xue, S. Xiao, Y. Q. Zhang, S. L. Xiong, C. Cai, P. Zhang, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long burst, 
GRB 211216B, at 2021-12-16T13:21:08.550 UTC (denoted as T0), which was also 
observed by Fermi/GBM (GCN #31244).
 
GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of multiple pulses
with a duration of about 30 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_93360068.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 101.95 deg 
Dec: 49.58 deg
Err: 6.23 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

GECAM location is consistent with the Fermi/GBM position within the error.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211216B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31247
SUBJECT: Fermi GRB 211216B: Global MASTER-Net observations report 
DATE:    21/12/16 15:30:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211216B ( Fermi GBM team, GCN 31244) errorbox  5497 sec after notice time and 5506 sec after trigger time at 2021-12-16 14:52:53 UT, with upper limit up to  16.8 mag. Observations started at twilight.  The observations began at zenith distance = 62 deg. The sun  altitude  is -13.3 deg. 

The galactic latitude b = 23 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=1816527

We obtain a following upper limits.  

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

    5536 | 2021-12-16 14:52:53 |   MASTER-Kislovodsk | (06h 36m 03.28s , +60d 06m 50.8s) |   C |    60 | 16.8 |        
    5536 | 2021-12-16 14:52:53 |   MASTER-Kislovodsk | (06h 44m 05.60s , +59d 42m 12.6s) |   C |    60 | 15.8 |        
    5616 | 2021-12-16 14:54:13 |   MASTER-Kislovodsk | (06h 43m 24.96s , +58d 14m 40.6s) |   C |    60 | 16.4 |        
    5616 | 2021-12-16 14:54:13 |   MASTER-Kislovodsk | (06h 50m 59.87s , +57d 50m 00.9s) |   C |    60 | 15.1 |        
    5697 | 2021-12-16 14:55:34 |   MASTER-Kislovodsk | (06h 28m 09.61s , +62d 01m 05.7s) |   C |    60 | 16.2 |        
    5697 | 2021-12-16 14:55:34 |   MASTER-Kislovodsk | (06h 36m 41.23s , +61d 36m 24.5s) |   C |    60 | 14.5 |        
    5937 | 2021-12-16 14:59:34 |   MASTER-Kislovodsk | (07h 00m 11.18s , +62d 02m 28.7s) |   C |    60 | 13.6 |        
    6018 | 2021-12-16 15:00:55 |   MASTER-Kislovodsk | (07h 03m 23.70s , +63d 30m 55.4s) |   C |    60 | 14.2 |        
    6018 | 2021-12-16 15:00:55 |   MASTER-Kislovodsk | (06h 53m 59.70s , +63d 55m 34.8s) |   C |    60 | 16.2 |        
    6258 | 2021-12-16 15:04:55 |   MASTER-Kislovodsk | (06h 19m 33.73s , +63d 57m 13.0s) |   C |    60 | 16.2 |        
    6258 | 2021-12-16 15:04:55 |   MASTER-Kislovodsk | (06h 28m 46.22s , +63d 32m 46.8s) |   C |    60 | 15.7 |        
    6338 | 2021-12-16 15:06:15 |   MASTER-Kislovodsk | (06h 14m 31.88s , +58d 13m 43.4s) |   C |    60 | 14.7 |        
    6339 | 2021-12-16 15:06:15 |   MASTER-Kislovodsk | (06h 22m 09.19s , +57d 49m 29.2s) |   C |    60 | 13.9 |        
    6418 | 2021-12-16 15:07:35 |   MASTER-Kislovodsk | (06h 23m 09.19s , +56d 21m 08.8s) |   C |    60 | 14.4 |        
    6418 | 2021-12-16 15:07:35 |   MASTER-Kislovodsk | (06h 30m 20.94s , +55d 56m 54.9s) |   C |    60 | 13.4 |        
    6908 | 2021-12-16 15:15:45 |   MASTER-Kislovodsk | (06h 36m 03.28s , +60d 08m 15.1s) |   C |    60 | 16.5 |        
    6908 | 2021-12-16 15:15:45 |   MASTER-Kislovodsk | (06h 44m 02.61s , +59d 44m 09.3s) |   C |    60 | 16.1 |        
    6988 | 2021-12-16 15:17:05 |   MASTER-Kislovodsk | (06h 43m 23.49s , +58d 13m 11.9s) |   C |    60 | 15.7 |        
    6988 | 2021-12-16 15:17:05 |   MASTER-Kislovodsk | (06h 50m 55.79s , +57d 49m 07.8s) |   C |    60 | 15.8 |        
    7068 | 2021-12-16 15:18:25 |   MASTER-Kislovodsk | (06h 28m 12.51s , +62d 01m 42.0s) |   C |    60 | 16.2 |        
    7068 | 2021-12-16 15:18:25 |   MASTER-Kislovodsk | (06h 36m 41.97s , +61d 37m 32.2s) |   C |    60 | 15.8 |        
    7229 | 2021-12-16 15:21:06 |   MASTER-Kislovodsk | (07h 06m 29.06s , +60d 07m 15.7s) |   C |    60 | 16.1 |        
    7229 | 2021-12-16 15:21:06 |   MASTER-Kislovodsk | (07h 14m 27.47s , +59d 43m 00.6s) |   C |    60 | 15.2 |        
    7309 | 2021-12-16 15:22:26 |   MASTER-Kislovodsk | (07h 00m 34.68s , +62d 02m 38.0s) |   C |    60 | 16.1 |        
    7309 | 2021-12-16 15:22:26 |   MASTER-Kislovodsk | (07h 09m 03.35s , +61d 38m 20.1s) |   C |    60 | 15.9 |        
    7389 | 2021-12-16 15:23:46 |   MASTER-Kislovodsk | (06h 54m 12.21s , +63d 56m 02.2s) |   C |    60 | 15.2 |        
    7389 | 2021-12-16 15:23:46 |   MASTER-Kislovodsk | (07h 03m 15.20s , +63d 31m 40.9s) |   C |    60 | 14.6 |        
    7469 | 2021-12-16 15:25:06 |   MASTER-Kislovodsk | (06h 50m 28.82s , +56d 21m 15.1s) |   C |    60 | 16.4 |        
    7469 | 2021-12-16 15:25:06 |   MASTER-Kislovodsk | (06h 57m 39.01s , +55d 57m 08.8s) |   C |    60 | 16.2 |        
    7549 | 2021-12-16 15:26:26 |   MASTER-Kislovodsk | (07h 19m 50.85s , +57d 49m 33.2s) |   C |    60 | 15.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31250
SUBJECT: GRB 211216A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/12/17 03:15:52 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), James DeLaunay (UAlabama), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT did not localize GRB 211216A (T0: 2021-12-16T06:45:52 UTC,
Fermi/GBM GCN 31237, GECAM GCN 31240, BALROG GCN 31239,
INTEGRAL/SPI-ACS trig #9564).

The Fermi, INTEGRAL, and GECAM notices, distributed in near real-time,
triggered the Swift Mission Operations Center operated Gamma-ray
Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al.
2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 11.2 in a
8.192 s analysis time bin.

NITRATES results are consistent with a burst coming from outside the
coded FOV, with DeltaLLHOut of 6.
An out of FOV origin is consistent with the Fermi/GBM RoboBA, GECAM,
and BALROG localizations.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211217A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31251
SUBJECT: GRB 211217A: GECAM detection
DATE:    21/12/17 08:09:59 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

C. Y. Li, W. C. Xue, S. Xiao, Y. Q. Zhang, S. L. Xiong, C. Cai, 
P. Zhang, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, X. L. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long burst, 
GRB 211217A, at 2021-12-17T07:04:30.550 UTC (denoted as T0).
 
GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 10 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_93423870.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 356.78 deg 
Dec: 24.1 deg
Err: 8.23 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31259
SUBJECT: GRB 211106A: XMM-Newton monitoring campaign detections
DATE:    21/12/18 02:09:26 GMT
FROM:    Alicia Rouco Escorial at CIERA  <alicia.rouco.escorial@northwestern.edu>

A. Rouco Escorial, W. Fong, C. D. Kilpatrick, J. Rastinejad, G. Schroeder, A. Nugent (Northwestern), E. Berger (Harvard), and T. Laskar (Radboud) report:


â€œWe initiated our afterglow monitoring campaign, consisting of two EPIC-pn observations, with the XMM-Newton Observatory on the short-duration GRB 211106A (Tohuvavohu et al., GCN #31049) on 2021 November 20 (22:37:51 UT) and 2021 December 8 (19:46:37 UT) UT, with median observation times of ~15 and ~33 days post-trigger. The two XMM-Newton observations were obtained under the Proposal 086286 (PI: Fong), with effective exposure times of ~20 ks and ~47 ks, respectively.

In the combined XMM-Newton dataset, we detect the X-ray counterpart to GRB 211106A at the position:

RA(J2000) = 22h54m20.8s
Dec(J2000) = -53d13m50.9s

with a total positional uncertainty of 1.7 arcsec (dominated by XMM-Newtonâ€™s systematic uncertainty). The XMM-Newton position of the X-ray afterglow and the Chandra position reported by Berger et al. (2021, GCN #31145) are consistent with each other within the errors. The afterglow is detected in both epochs at a significance of ~5.5 sigma and ~3.4 sigma, with total net source counts of ~83 and ~73 (0.3-10 keV), respectively.

The XRT, Chandra and XMM-Newton afterglow unabsorbed flux, starting at ~0.5 days post-burst, can be modeled with a single power-law decline characterized by a decay index (F~t^alpha) of alpha=-1.02 (-0.06,+0.05). Additionally, from our jointly spectral fitting of both data sets, we derive an intrinsic neutral hydrogen absorption column of ~1.4E21 cm^2 for z=0.097 (Malasani et al., GCN #31075; Christensen et al., GCN #31075). We obtain higher inferred intrinsic column density for greater presumed source redshifts (Kilpatrick et al., GCNs #31146, #31157).

We thank the XMM-Newton Project Scientist, Norbert Shartel, and staff for the rapid planning and scheduling of these observations.â€


GRB_name: GRB211218A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31261
SUBJECT: GRB 211218A, MAXI J0909-041: MAXI/GSC detection
DATE:    21/12/18 05:17:50 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro.hitoshi@nihon-u.ac.jp>

R. Uematsu (Kyoto U.), H. Negoro (Nihon U.), M. Serino (AGU), 
M. Nakajima, K. Kobayashi, K. Asakura, K. Seino (Nihon U.), 
T. Mihara, T. Tamagawa, J. Li, M. Matsuoka (RIKEN), 
T. Sakamoto, S. Sugita, K. Komachi, H. Hiramatsu, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), 
M. Shidatsu, M. Iwasaki (Ehime U.),
N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), 
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, M. Kurihara (JAXA), 
Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, K. Inaba (Kyoto U.), 
H. Tsunemi (Osaka U.), 
M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/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 01:01:29 UT 2021 December 18. Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (137.278 deg, -4.110 deg) = (09 09 06, -04 06 36) (J2000) 
with a statistical 90% C.L. elliptical error region with long and short radii of 0.42 deg and 0.38 deg, 
respectively. 
The roll angle of long axis from the north direction is 62.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 118 +- 31 mCrab (4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (135.984, -5.236) deg = (09 03 56, -05 14 09) (J2000)
(R.A., Dec) = (136.566, -5.656) deg = (09 06 15, -05 39 21) (J2000)
(R.A., Dec) = (138.302, -3.262) deg = (09 13 12, -03 15 43) (J2000)
(R.A., Dec) = (137.722, -2.843) deg = (09 10 53, -02 50 34) (J2000)
There was no significant excess flux in the previous transit at 12/17 23:28 UT 
and in the next transit at 12/18 02:34 UT with an upper limit of 20 mCrab for each.

 Finally, we note that due to the poor statistics, we can not confirm that this event is a GRB.
 Therefore, we also name the source MAXI J0909-041.


GRB_name: GRB211216A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31263
SUBJECT: GRB 211216A: Fermi GBM observation
DATE:    21/12/18 09:27:56 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico and INFN Bari) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:


"At 06:45:52.06 UT on 16 December 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211216A (trigger 661329957 / 211216282),
which was also detected by the Swift/BAT-GUANO (Tohuvavohu et al. 2021, GCN 31250)
and by GECAM-B (Xue et al. 2021, GCN 31240).
The GBM on-ground location is reported in GCN 31237.

The GBM light curve shows a FRED-like emission episode
with a duration (T90) of about 20 s (50-300 keV).

The time-averaged spectrum from T0 to T0+20 s is
well fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.47 +/- 0.05 and
the cutoff energy, parameterized as Epeak, is 208 +/- 7 keV.

The event fluence (10-1000 keV) in this time interval is
(9.16 +/- 0.02)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+6.3 s in the 10-1000 keV band
is  5.4 +/- 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: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31264
SUBJECT: GRB 211211A: MMT/MMIRS Observations Indicate Fading of K-band Source
DATE:    21/12/18 21:26:07 GMT
FROM:    Wen-fai Fong at Northwestern U  <wfong@northwestern.edu>

J. Rastinejad, W. Fong (Northwestern), A. J. Levan, D. B. Malesani (Radboud), J. Jencson, D. Sand (U. Arizona), N. R. Tanvir (Leicester) report:

We observed the location of GRB 211211A (Dâ€™Ai et al., GCN 31202) with the MMT and Magellan Infrared Spectrograph (MMIRS) instrument mounted on the MMT 6.5-meter telescope on Mount Hopkins, Arizona. At a mid-time of 2021 December 18.52 UT (~6.9 days post-burst), we obtained 126 x 30 s of K-band imaging at a median airmass of 1.5 and seeing of 0.8 arcsec. A faint K-band source is still detected at the location of the optical afterglow (first reported by Zheng & Fillipenko; GCN 31203). Based on calibration to 2MASS, we estimate a preliminary magnitude for the source of K_AB ~ 24 mag, although we caution that the faintness of the source precludes a precise measure at this time. Visual inspection relative to our Gemini K-band imaging (Levan et al. GCN 31235) is in support of clear fading of the source.

Taken at face value, the K-band source has declined by ~1.5 mag between ~4 and 7 days post-burst, while AT2017gfo only faded by ~0.4 mag in the K band (Villar et al., 2017, ApJL, 851, L21) on these same timescales.

Further observations are planned. We thank Joannah Hinz and ShiAnne Kattner at MMT for the rapid planning and execution of these observations.


GRB_name: GRB211219A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31265
SUBJECT: GRB 211219A: Fermi GBM Final Real-time Localization
DATE:    21/12/19 15:05:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:55:22 UT on 19 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211219A (trigger 661618527.567338 / 211219622).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 60.5, Dec = -30.5 (J2000 degrees, equivalent to J2000 04h 01m, -30d 30'), with a statistical uncertainty of 3.3 degrees.

The angle from the Fermi LAT boresight is 100.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211219622/quicklook/glg_skymap_all_bn211219622.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211219622/quicklook/glg_healpix_all_bn211219622.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211219622/quicklook/glg_lc_medres34_bn211219622.gif


GRB_name: GRB211219A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31266
SUBJECT: Fermi GRB 211219A: Global MASTER-Net observations report 
DATE:    21/12/19 16:45:16 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 211219A ( Fermi GBM team, GCN 31265) errorbox  4877 sec after notice time and 4903 sec after trigger time at 2021-12-19 16:17:06 UT, with upper limit up to  14.3 mag. The observations began at zenith distance = 80 deg. The sun  altitude  is -28.1 deg. 

The galactic latitude b = -48 deg., longitude l = 229 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1819804

We obtain a following upper limits.  

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

    4934 | 2021-12-19 16:17:06 |   MASTER-Kislovodsk | (03h 58m 29.45s , -25d 40m 02.5s) |   C |    60 | 14.2 |        
    5913 | 2021-12-19 16:33:25 |   MASTER-Kislovodsk | (03h 58m 23.82s , -25d 41m 23.6s) |   C |    60 | 14.3 |        
    6073 | 2021-12-19 16:36:05 |   MASTER-Kislovodsk | (03h 45m 18.21s , -27d 33m 24.6s) |   C |    60 | 13.0 |        
    6314 | 2021-12-19 16:40:06 |   MASTER-Kislovodsk | (04h 02m 20.29s , -27d 34m 30.9s) |   C |    60 | 12.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211219B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31267
SUBJECT: GRB 211219B: Fermi GBM Final Real-time Localization
DATE:    21/12/19 22:00:03 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 21:49:46 UT on 19 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211219B (trigger 661643391.008452 / 211219910).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 68.5, Dec = -63.2 (J2000 degrees, equivalent to J2000 04h 33m, -63d 12'), with a statistical uncertainty of 3.0 degrees.

The angle from the Fermi LAT boresight is 151.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211219910/quicklook/glg_skymap_all_bn211219910.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211219910/quicklook/glg_healpix_all_bn211219910.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211219910/quicklook/glg_lc_medres34_bn211219910.gif


GRB_name: GRB211219B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31268
SUBJECT: Fermi GRB 211219B: Global MASTER-Net observations report 
DATE:    21/12/20 05:15:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

A. Gabovich, V.Yurkov 
(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 211219B ( Fermi GBM team, GCN 31267) errorbox  25126 sec after notice time and 25134 sec after trigger time at 2021-12-20 04:48:40 UT, with upper limit up to  17.9 mag. The observations began at zenith distance = 37 deg. The sun  altitude  is -35.4 deg. 

The galactic latitude b = -39 deg., longitude l = 274 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1820147

We obtain a following upper limits.  

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

   25164 | 2021-12-20 04:48:40 |         MASTER-OAFA | (04h 23m 47.22s , -64d 09m 14.6s) |   C |    60 | 17.9 |        
   25446 | 2021-12-20 04:53:22 |         MASTER-OAFA | (04h 41m 43.78s , -64d 06m 58.4s) |   C |    60 | 17.7 |        
   25527 | 2021-12-20 04:54:42 |         MASTER-OAFA | (04h 39m 30.62s , -62d 12m 59.3s) |   C |    60 | 17.6 |        
   25606 | 2021-12-20 04:56:02 |         MASTER-OAFA | (04h 56m 12.55s , -62d 13m 23.7s) |   C |    60 | 17.7 |        
   25686 | 2021-12-20 04:57:21 |         MASTER-OAFA | (04h 42m 48.47s , -66d 01m 55.2s) |   C |    60 | 17.7 |        
   25971 | 2021-12-20 05:02:07 |         MASTER-OAFA | (05h 01m 59.43s , -66d 02m 11.3s) |   C |    60 | 17.5 |        
   26050 | 2021-12-20 05:03:26 |         MASTER-OAFA | (04h 07m 34.30s , -62d 15m 39.0s) |   C |    60 | 17.7 |        
   26335 | 2021-12-20 05:08:10 |         MASTER-OAFA | (04h 24m 17.72s , -62d 14m 19.0s) |   C |    60 | 17.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211219A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31269
SUBJECT: GRB 211219A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/12/20 15:25:02 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), James DeLaunay (UAlabama), Gayathri
Raman (PSU), Jamie A. Kennea (PSU), report:

Swift/BAT did not localize GRB 211219A (T0: 2021-12-19T14:55:22 UTC,
Fermi/GBM GCN 31265, INTEGRAL/SPI-ACS trig #9569).

The Fermi and INTEGRAL notices, distributed in near real-time,
triggered the Swift Mission Operations Center operated Gamma-ray
Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al.
2020, ApJ, 900, 1).

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.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 11.8 in a
4.096 s analysis time bin.

NITRATES results are consistent with a burst coming from outside the
coded FOV, with DeltaLLHOut of 5.5.
An out of FOV origin is consistent with the Fermi/GBM localization.

See Section 9.1 and Figure 20 in the NITRATES paper for brief
descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

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: GRB211219A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31270
SUBJECT: GRB 211219A: AGILE detection
DATE:    21/12/20 17:27:59 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), F. Lucarelli, C. Pittori, F. Verrecchia (SSDC, and
INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M.
Cardillo, C. Casentini, Y. Evangelista, L. Foffano, E. Menegoni, G. Piano
(INAF/IAPS), 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 211219A at T0 = 2021-12-19
14:55:22 (UTC), reported by Fermi GBM (GCN #31265).

The burst is clearly visible in the AGILE scientific ratemeters of the
MiniCALorimeter (MCAL; 0.4-100 MeV) and AntiCoincidence (AC; 50-200 keV)
detectors. The event lasted about 6.0 s and it released a total number of
7115 counts in the MCAL detector (above a background rate of 1240 Hz), and
18620 counts in the AC detector (above a background rate of 3450 Hz). The
AGILE ratemeter light curves can be found at
http://www.agilescienceapp.it/notices/GRB211219A_AGILE_RM.png . At the T0,
the event was about 63Â° off-axis.

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: GRB211221A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31273
SUBJECT: GRB 211221A: Swift detection of a burst
DATE:    21/12/21 21:04:45 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC),
J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and B. Sbarufatti (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 20:48:40 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211221A (trigger=1090472).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 78.938, +0.940 which is 
   RA(J2000) = 05h 15m 45s
   Dec(J2000) = +00d 56' 25"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex peak
structure with a duration of about 20 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 20:49:34.9 UT, 54.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 78.89820, 0.91421 which is
equivalent to:
   RA(J2000)  = 05h 15m 35.57s
   Dec(J2000) = +00d 54' 51.2"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 170 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 (1.37 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 9
(+4.75/-2.44) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 6.82e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 63 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
0.143. 

Burst Advocate for this burst is K. L. Page (kimlpage1978 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: GRB211221A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31274
SUBJECT: Swift GRB 211221A: Global MASTER-Net observations report 
DATE:    21/12/22 00:56:25 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 211221A ( K. L. Page et al., GCN 31273) errorbox  3401 sec after notice time and 3560 sec after trigger time at 2021-12-21 21:48:01 UT, with upper limit up to  14.8 mag. The observations began at zenith distance = 46 deg. The sun  altitude  is -68.8 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB 211221A errorbox  13726 sec after notice time and 13885 sec after trigger time at 2021-12-22 00:40:06 UT, with upper limit up to  16.7 mag. Observations started at twilight.  The observations began at zenith distance = 54 deg. The sun  altitude  is -12.1 deg. 

The galactic latitude b = -20 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=1823335

We obtain a following upper limits.  

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

    3651 |   MASTER-Kislovodsk |   C |   180 | 12.7 |        
    3651 |   MASTER-Kislovodsk |   C |   180 | 12.2 |        
    3851 |   MASTER-Kislovodsk |   C |   180 | 13.0 |        
    3851 |   MASTER-Kislovodsk |   C |   180 | 13.4 |        
    4052 |   MASTER-Kislovodsk |   C |   180 | 14.2 |        
    4052 |   MASTER-Kislovodsk |   C |   180 | 14.2 |        
    4252 |   MASTER-Kislovodsk |   C |   180 | 14.8 |        
    4252 |   MASTER-Kislovodsk |   C |   180 | 14.5 |        
    4453 |   MASTER-Kislovodsk |   C |   180 | 14.4 |        
    4453 |   MASTER-Kislovodsk |   C |   180 | 13.5 |        
   10415 |   MASTER-Kislovodsk |   C |   180 | 14.5 |        
   10896 |   MASTER-Kislovodsk |   C |   180 | 13.8 |        
   10896 |   MASTER-Kislovodsk |   C |   180 | 14.4 |        
   11497 |   MASTER-Kislovodsk |   C |   180 | 13.4 |        
   11497 |   MASTER-Kislovodsk |   C |   180 | 13.1 |        
   11897 |   MASTER-Kislovodsk |   C |   180 | 13.5 |        
   12787 |   MASTER-Kislovodsk |   C |   180 | 14.1 |        
   12787 |   MASTER-Kislovodsk |   C |   180 | 14.1 |        
   13976 |         MASTER-OAFA |   C |   180 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211221A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31275
SUBJECT: GRB 211221A: Enhanced Swift-XRT position
DATE:    21/12/22 01:29:16 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 892 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 211221A, 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 = 78.89745, +0.91449 which is equivalent
to:

RA (J2000): 05h 15m 35.39s
Dec (J2000): +00d 54' 52.2"

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: GRB211221A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31276
SUBJECT: GRB 211221A: NOT optical limits
DATE:    21/12/22 01:41:13 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Univ. Radboud and DAWN/NBI), Z. Zhu (NAOC/CAS), A. 
Viitanen (Univ. Helsinki and NOT), E. Biancalani (Leiden Obs. and NOT) 
report on behalf of a larger collaboration:

We observed the field of the solstice GRB 211221A (Page et al., GCN 
31273) using the Nordic Optical Telescope (NOT) equipped with the ALFOSC 
camera. Observations were carried out under good conditions in the r and 
z bands, with mean times 2021 Dec 22.00 and 22.01 UT, respectively (3.2 
and 3.5 hr after the GRB). The exposure times were 3x300 (in r) and 
5x200 s (in z).

We detect no new objects inside or close to the UVOT-enhanced XRT error 
circle (Evans et al., GCN 31275), down to (preliminary) limits:

r > 23.5 AB
z > 23.0 AB

Calibration of the photometry is relative to nearby stars from the 
Pan-STARRS catalogue.


GRB_name: GRB211221A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31277
SUBJECT: GRB 211221A: MeerLICHT optical limits
DATE:    21/12/22 10:54:04 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

P.J. Groot (Radboud/UCT/SAAO), S. de Wet (UCT), D. B. Malesani
(Radboud/DAWN,NBI),
P.M. Vreeswijk (Radboud), report on behalf of the MeerLICHT consortium:

The position of GRB211221A (Page et al., GCN 31273; Evans et al., GCN
31275; Lipunov et al., GCN 31274; Malesani et al., GCN 31276) was
observed with the 0.6m wide-field MeerLICHT telescope, located at
Sutherland, South Africa, starting at 2021-12-22, 00:24 UT,
approximately 3.5 hr after the detection by Swift. A series of 60s
observations in the u,g,q,r,i,z bands was started that lasted until
2021-12-22, 01:21 UT. All data was processed automatically using the
BlackBOX/ZOGY pipeline (Vreeswijk et al, forthcoming). Cloudy
conditions prevented observations earlier in the night.

Co-adding the single exposures in each filter leads to deeper 3-sigma
AB-magnitude limits at the Swift-XRT position reported by
Evans et al. (GCN 31275) of:

u > 19.97 at 00:51:03 UT
g > 20.55 at 01:02:18 UT
q > 21.85 at 00:59:14 UT
r > 20.67 at 00:56:55 UT
i > 20.32 at 00:52:09 UT
z > 19.70 at 00:56:24 UT.

These limits are consistent with those reported by Malesani et
al. (GCN 31276) taken at the same time.

MeerLICHT is built and run by a consortium consisting of Radboud
University, University of Cape Town, the South African Astronomical
Observatory, the University of Oxford, the University of Manchester
and the University of Amsterdam


GRB_name: GRB211218A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31278
SUBJECT: GRB 211218A: MITSuME Akeno optical upper limits
DATE:    21/12/22 11:58:51 GMT
FROM:    Yuri Imai at Tokyo Inst of Tech  <imai@hp.phys.titech.ac.jp>

Y. Imai, R. Hosokawa, K. L. Murata, M. Niwano, Y. Takamatsu, N. Ito,
R. Yamaguchi, R. Noto, S. Sato, M. Takaku, Y. Yatsu, and N. Kawai
(TokyoTech) report on behalf of the MITSuME collaboration:

We performed tiling observations for the MAXI/GSC error region of GRB
211218A, MAXI J0909-041 (R. Uematsu et al. GCN Circular #31261, V.
Lipunov et al. GCN Circular #31260) with an optical tri-color (g', Rc,
and Ic) camera attached to the MITSuME 50 cm telescope Akeno.

The follow up observation started at 2021-12-18 13:35:14 UT, 12.6
hours after the trigger.
Our tiling observation covered almost ~70% of the MAXI/GSC error
region (GCN Circular #31261). Comparing our co-added images with the
GSC2.3 catalog, we found no optical transients in the observed region.
The 5-sigma upper limits of the co-added images are listed below.

Field num. | center position(R.A., Dec.) | size of field(R.A.(arcmin)
x Dec.(arcmin)) | 5-sigma upper limit | MID-UT(UT) | exposure
time(sec)
-----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------
Field 00 | 9:08:47, -4:06:36 | 27.1 x 24.7 | g'>18.2, Rc>19.0, Ic>18.7
| 2021-12-18 17:57:09 | 360.0
Field 01 | 9:08:01, -4:22:05 | 26.6 x 26.5 | g'>18.3, Rc>19.1, Ic>18.7
| 2021-12-18 17:19:28 | 390.0
Field 02 | 9:09:42, -4:17:55 | 26.4 x 26.5 | g'>18.2, Rc>19.0, Ic>18.6
| 2021-12-18 17:45:57 | 330.0
Field 03 | 9:09:01, -4:31:20 | 27.4 x 24.2 | g'>18.2, Rc>19.0, Ic>18.6
| 2021-12-18 17:37:16 | 330.0
Field 04 | 9:07:45, -3:55:46 | 26.0 x 24.3 | g'>18.3, Rc>19.2, Ic>18.8
| 2021-12-18 16:58:53 | 450.0
Field 05 | 9:07:04, -4:08:57 | 26.5 x 27.5 | g'>17.9, Rc>18.7, Ic>18.4
| 2021-12-18 15:49:39 | 240.0
Field 06 | 9:09:26, -3:51:26 | 26.2 x 25.5 | g'>18.2, Rc>18.9, Ic>18.6
| 2021-12-18 17:24:50 | 360.0
Field 07 | 9:07:20, -4:34:20 | 26.5 x 26.1 | g'>18.0, Rc>18.7, Ic>18.4
| 2021-12-18 17:04:52 | 240.0
Field 08 | 9:10:28, -4:03:20 | 26.6 x 26.5 | g'>18.3, Rc>19.2, Ic>18.8
| 2021-12-18 16:49:06 | 540.0
Field 09 | 9:08:17, -4:47:13 | 26.4 x 26.7 | g'>18.1, Rc>18.9, Ic>18.5
| 2021-12-18 17:33:11 | 300.0
Field 10 | 9:08:29, -3:40:30 | 26.5 x 25.1 | g'>18.3, Rc>19.0, Ic>18.7
| 2021-12-18 17:11:30 | 390.0
Field 11 | 9:06:22, -4:25:47 | 25.8 x 26.1 | g'>18.2, Rc>19.1, Ic>18.7
| 2021-12-18 16:00:21 | 480.0
Field 12 | 9:10:10, -3:37:09 | 26.3 x 26.7 | g'>18.0, Rc>18.9, Ic>18.6
| 2021-12-18 16:24:58 | 300.0
Field 13 | 9:06:39, -4:50:05 | 26.4 x 26.6 | g'>17.9, Rc>18.8, Ic>18.4
| 2021-12-18 15:17:23 | 270.0
Field 14 | 9:11:06, -3:48:44 | 26.6 x 26.5 | g'>18.1, Rc>18.8, Ic>18.4
| 2021-12-18 17:11:04 | 210.0
Field 15 | 9:09:11, -3:27:56 | 26.0 x 26.9 | g'>18.1, Rc>19.0, Ic>18.6
| 2021-12-18 16:13:00 | 330.0
Field 16 | 9:07:35, -5:00:29 | 27.3 x 27.6 | g'>17.7, Rc>18.5, Ic>18.3
| 2021-12-18 15:36:49 | 180.0
Field 17 | 9:05:40, -4:40:29 | 27.2 x 26.4 | g'>18.0, Rc>18.8, Ic>18.6
| 2021-12-18 16:07:28 | 330.0
Field 18 | 9:10:52, -3:22:30 | 26.4 x 26.5 | g'>18.0, Rc>18.9, Ic>18.5
| 2021-12-18 15:30:13 | 300.0
Field 19 | 9:11:49, -3:34:14 | 26.6 x 26.5 | g'>18.0, Rc>18.7, Ic>18.4
| 2021-12-18 16:57:19 | 180.0
Field 20 | 9:05:56, -5:04:58 | 26.5 x 26.6 | g'>18.1, Rc>19.0, Ic>18.6
| 2021-12-18 17:02:01 | 420.0
Field 21 | 9:09:48, -3:03:38 | 28.5 x 28.6 | g'>17.1, Rc>17.8, Ic>17.4
| 2021-12-18 20:31:34 | 60.0
-----------------------------------------------------------------------------------------------------------------------------------------------------------------------------------
We used 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. 2021, PASJ, Vol.73, Issue 1, Pages
4-24; https://github.com/MNiwano/Eclaire).


GRB_name: GRB211221A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31279
SUBJECT: GRB 211221A: BOOTES-4/MET optical upper limit
DATE:    21/12/22 13:49:01 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, T.-R. Sun, A. J. Castro-Tirado, E. Fernandez-Garcia, M. D. Caballero-Garcia, R. Sanchez-Ramirez, M. A. Castro Tirado (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga), S. Guziy (Univ. of Nikolaev) and D. R. Xiong, Y. F. Fan, J. M. Bai, C. J. Wang, Y. X. Xin, X. H. Zhao (Yunnan Observatories of CAS) on behalf of a larger collaboration, report:

Following the detection of GRB 211221A by Swift (Page et al. GCNC 31273), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical Observatory (China) automatically responded to this burst starting on Dec. 21 at 20:51:37 UT (~177 sec after trigger). No new source is detected at the position reported by Swift-XRT (Page et al. GCNC 31273) which down to 19.7 mag in the co-added image of first achieved 10 x 20 s exposure frames in the clear filter. This non-detection is consistent with the reports from UVOT (Page et al. GCNC 31273), MASTER (Lipunov et al. GCNC 31274), NOT (Malesani et al. GCNC 31276) and MeerLICHT (Groot et al. GCNC 31277).

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


GRB_name: GRB211222A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31280
SUBJECT: GRB 211222A: Fermi GBM Final Real-time Localization
DATE:    21/12/22 18:36:35 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 18:26:12 UT on 22 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211222A (trigger 661890377.228366 / 211222768).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 103.4, Dec = -53.8 (J2000 degrees, equivalent to J2000 06h 53m, -53d 47'), with a statistical uncertainty of 20.6 degrees.

The angle from the Fermi LAT boresight is 64.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211222768/quicklook/glg_skymap_all_bn211222768.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211222768/quicklook/glg_healpix_all_bn211222768.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211222768/quicklook/glg_lc_medres34_bn211222768.gif


GRB_name: GRB211221A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31281
SUBJECT: GRB 211221A: Swift-XRT refined Analysis
DATE:    21/12/22 22:38:35 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 5.9 ks of XRT data for GRB 211221A (Page et al. GCN
Circ. 31273), from 44 s to 73.7 ks after the  BAT trigger. The data
comprise 52 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 31275).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.02 (+0.05, -0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.59 (+0.31, -0.29). The
best-fitting absorption column is  1.1 (+0.4, -0.3) x 10^22 cm^-2, in
excess of the Galactic value of 1.4 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 6.2 x 10^-11 (9.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+0.4, -0.3) x 10^22 cm^-2
Galactic foreground: 1.4 x 10^21 cm^-2
Excess significance: 5.0 sigma
Photon index:      1.59 (+0.31, -0.29)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01090472.

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


GRB_name: GRB211222A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31282
SUBJECT: Fermi GRB 211222A: Global MASTER-Net observations report 
DATE:    21/12/22 23:15:11 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, 
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, 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
(Irkutsk State University, API),

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

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


MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 211222A ( Fermi GBM team, GCN 31280) errorbox  16726 sec after notice time and 16754 sec after trigger time at 2021-12-22 23:05:26 UT, with upper limit up to  16.8 mag. The observations began at zenith distance = 78 deg. The sun  altitude  is -63.5 deg. 

The galactic latitude b = -21 deg., longitude l = 264 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1824183

We obtain a following upper limits.  

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

   16785 | 2021-12-22 23:05:26 |          MASTER-IAC | (06h 15m 48.74s , -44d 20m 10.0s) |   C |    60 | 16.8 |        
   16785 | 2021-12-22 23:05:26 |          MASTER-IAC | (06h 27m 13.44s , -44d 25m 12.1s) |   C |    60 | 16.8 |        
   16864 | 2021-12-22 23:06:46 |          MASTER-IAC | (07h 01m 51.93s , -38d 37m 38.8s) |   C |    60 | 16.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211219A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31283
SUBJECT: GRB 211219A: AstroSat CZTI detection
DATE:    21/12/23 03:06:33 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao
(IITB), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale
(PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of a long GRB 211219A which was
also detected by Fermi (GCN 31265), MASTER-Net (Lipunov et al. GCN
31268), Swift/BAT-GUANO (Tohuvavohu et al., GCN 31269) and AGILE (Ursi
et al., GCN 31270). 

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2021-12-19 14:55:22.50 UT. The measured peak count rate associated with
the burst is 178 (+42, -26) cts/s above the background in the combined
data of two quadrants, with a total of 912 (+201, -218) cts. The local
mean background count rate was 382 (+2, -3) cts/s. Using cumulative
rates, we measure a T90 of 15 (+3, -8) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector
in the 100-500 keV energy range. The light curve peaks at 2021-12-19
14:55:23.063 UT. The measured peak count rate is 740 (+72, -70) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 3100 (+285, -308) cts. The local mean background count rate was
1243 (+4, -5) cts/s. We measure a T90 of 11.0 (+0.3, -5.2) 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 [1]. 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. 

Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB211219B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31284
SUBJECT: GRB 211219B: AstroSat CZTI detection
DATE:    21/12/23 03:18:31 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao
(IITB), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale
(PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al.,
2021, JApA, 42, 73) showed detection of a long GRB 211219B which was
also detected by Fermi-GBM (GCN 31267). 

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak at
2021-12-19 21:49:45.50 UT. The measured peak count rate associated with
the burst is 95 (+38, -18) cts/s above the background in the combined
data of two quadrants, with a total of 573 (+196, -205) cts. The local
mean background count rate was 398 (+2, -2) cts/s. Using cumulative
rates, we measure a T90 of 14 (+6, -8) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector
in the 100-500 keV energy range. The light curve peaks at 2021-12-19
21:49:45.056 UT. The measured peak count rate is 280 (+63, -50) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 1460 (+257, -400) cts. The local mean background count rate was
1339 (+5, -3) cts/s. We measure a T90 of 8 (+5, -2) s from the
cumulative Veto light curve. 

We also detected another fainter burst, likely from the same source,
that lasted for around 6 s in the CsI anticoincidence (Veto) detector
about 70 s after the primary burst. 

CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=grb [1]. 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. 

Links:
------
[1] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB211221A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31285
SUBJECT: GRB 211221A: NUTTelA-TAO / BSTI Early Optical Limits (Preliminary)
DATE:    21/12/23 04:17:37 GMT
FROM:    Toktarkhan Komesh at Nazarbayev University  <toktarkhan.komesh@nu.edu.kz>

T. Komesh (NU), B. Grossan (UCB, NU), Z. Maksut (NU), M. Krugov (FAI),  
E. Linder (UCB, NU), E. Abdikamalov (NU), G. F. Smoot (HKUST, UCB, NU), 
report on behalf of the Energetic Cosmos Laboratory:

The Nazarbayev University Transient Telescope at Assy-Turgen 
Astrophysical Observatory (NUTTelA-TAO) observed the field of GRB 
211221A 19 s after receipt an automated GCN / BAT position alert, 
observing in Sloan i' band, with the Burst Simultaneous Three-Channel 
Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32, 14).

We started observations at 20:51:35 UT on 2021-12-21, 175 s after the 
BAT trigger. Observations were made in clear conditions starting at 
about 30 deg. target altitude. No source consistent with the XRT (P. 
Evans et al., GCN Circ. 31275) was detected.  We report the following 
results:

start time    t-t0(s)  end time        ULi'       exposure_time (s)
------------    --------  ------------          ------ --------------------
20:51:35     175   20:52:35          17.9           60
20:52:50     257   22:12:50          18.4         150

start time is in UT. t-t0(s) gives the time since trigger, in seconds. 
UL i', gives the 5 sigma upper limit sensitivity in magnitudes, for 
images co-added to the given exposure time. The first row in the table 
corresponds to co-adds of an initial short exposure image sequence of 
7.5 s. The second row corresponds to co-adds from a continuing series of 
15 s exposures.  Calibration was done with the 3 bright Pan-STARRS 
catalog stars on our images.

We caution the reader that these are preliminary results, without color 
or other corrections. Please also note that times are approximate.
----------------------------------
NU = Nazarbayev University, Nur-Sultan, Kazakhstan
UCB = University of California, Berkeley, USA
HKUST = Hong Kong University of Science and Technology
FAI = Fesenkov Astrophysical Institute, Kazakhstan

The NUTTelA-TAO Team acknowledges the support of the staff of the 
Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the 
Fesenkov Astrophysical Institute, Almaty, Kazkhstan.


GRB_name: GRB211223A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31286
SUBJECT: GRB 211223A: GECAM detection
DATE:    21/12/23 04:30:44 GMT
FROM:    Xiaolu Zhang at IHEP  <xlzhang@ihep.ac.cn>

GRB 211223A: GECAM detection

X. L. Zhang, W. C. Xue, S. Xiao, Y. Q. Zhang, S. L. Xiong, C. Cai, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
J. C. Liu,  Y. Zhao, Z. W. Guo, C. Zheng, C. W. Wang, 
Q. B. Yi, B. X. Zhang,  W. X. Peng, R. Qiao, D. Y. Guo, X. B. Li, 
X. Ma, L. M. Song, P. Wang, J. Wang, Z. Zhang, S. J. Zheng, W. Chen, 
J. J. He, G. Y. Zhao, Y. Q. Du, H. Wu, J. Liang, Q. Luo, P. Zhang, 
H. M. Zhang, Z. H. An, M. Gao, K. Gong, B. Li, C. Li, J. H. Li, 
X. Q. Li, Y. G. Li, X. H. Liang, X. J. Liu, Y. Q. Liu, X. L. Sun, 
Y. L. Tuo, J. Z. Wang, X. Y. Wen, Y. B. Xu, Y. P. Xu, S. Yang, 
C. Y. Zhang, D. L. Zhang, Fan Zhang, Fei Zhang,
X. Zhou, F. J. Lu, S. N. Zhang (IHEP)
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long 
burst, GRB 211223A, at 2021-12-23T02:41:18.900 UTC (denoted as T0)
, which was also observed by CALET/GBM.
 
GECAM alert data was downlinked to the ground through the short message
service of BeiDou Navigation Satellite System (BDS) within ~60 s after T0.

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 40 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/211223Alc.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra:  320.20 deg 
Dec: -30.74 deg
Err: 4.45 deg (1-sigma, statistical only)
The current systematic error of location is estimated to be several degrees 
which could be minimized by the ongoing calibration.

The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/211223Alocation.png

Please note that all GECAM results here are preliminary. The final analysis
will be published in journal papers or GECAM online catalog.

Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission consists of two small satellites (GECAM-A and GECAM-B) in
Low Earth Orbit (600 km, 29 deg), launched on Dec 10, 2020 (Beijing Time),
which was funded by the Chinese Academy of Sciences (CAS).


GRB_name: GRB211223B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31287
SUBJECT: GRB 211223B: Fermi GBM Final Real-time Localization
DATE:    21/12/23 08:33:43 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 08:23:22 UT on 23 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211223B (trigger 661940607.257526 / 211223350).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 287.6, Dec = 42.2 (J2000 degrees, equivalent to J2000 19h 10m, 42d 12'), with a statistical uncertainty of 8.1 degrees.

The angle from the Fermi LAT boresight is 13.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211223350/quicklook/glg_skymap_all_bn211223350.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211223350/quicklook/glg_healpix_all_bn211223350.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211223350/quicklook/glg_lc_medres34_bn211223350.gif


GRB_name: GRB211223C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31288
SUBJECT: GRB 211223C: Swift detection of a burst
DATE:    21/12/23 14:39:35 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. A. Evans (U Leicester), S. D. Barthelmy (GSFC),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (U Tampa),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), B. Sbarufatti (PSU) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 14:29:26 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211223C (trigger=1090656).  Swift did not slew to the burst
due to a pointing constraint.  The BAT on-board calculated location is 
RA, Dec 227.164, -26.873 which is 
   RA(J2000) = 15h 08m 39s
   Dec(J2000) = -26d 52' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 20 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 23:31 UT on 2021 December 29. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is P. A. Evans (pae9 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: GRB211221A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31289
SUBJECT: GRB 211221A: Swift-BAT refined analysis
DATE:    21/12/23 15:01:27 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

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


Using the data set from T-239 to T+963 sec sec from the recent telemetry
downlink, we report further analysis of BAT GRB 211221A (trigger #1090472)
(Page et al., GCN 31273).  The BAT ground-calculated position is RA, Dec =
78.906, 0.902 deg which is

   RA(J2000)  =  05h 15m 37.4s

   Dec(J2000) = +00d 54' 06.2"

with an uncertainty of 2.6 arcmin, (radius, sys+stat, 90% containment). The
partial coding was 97%.


The BAT light curve showed a complex peak structure with a duration of
about 20 sec. There may be hints of precursor activity and low-level
post-peak emission from the GRB as seen in the mask weighted light curve.
The post-peak emission lasts beyond the available event data (which ends at
T+963). T90 (15-350 keV) is 671.67 +- 105.96 sec (estimated error including
systematics).


The time-averaged spectrum from T-129.40 to T+688.36 sec is best fit by a
simple power-law model.  The power law index of the time-averaged spectrum
is 1.48 +- 0.13.  The fluence in the 15-150 keV band is 4.0 +- 0.3 x 10^-06
erg/cm2. The 1-sec peak photon flux measured from T-0.27 sec in the 15-150
keV band is 0.5 +- 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/1090472/BA/


GRB_name: GRB211207A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31290
SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 211207A
DATE:    21/12/23 15:03:48 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

C. Fletcher (USRA) reports on behalf of the Fermi-GBM Team:

Swift-BAT detected GRB 211207A at 20:52:56 UT (GCN 31182). 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 identified no counterparts.

The GBM targeted search [1], the most sensitive, coherent search for
GRB-like signals identified a transient most significantly on the 2.048 s
timescale, with a false alarm rate of 3.2e-05 Hz and a location consistent with
the Swift-BAT event, using the standard search protocol with a S/N of 8.
The GBM targeted search event was found with the highest
significance with a "soft" spectrum (Band function with
Epeak = 70 keV, alpha = -1.9, beta = -3.7) for a GRB.

[1] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB211221A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31291
SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 211221A
DATE:    21/12/23 15:05:00 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

C. Fletcher (USRA) reports on behalf of the Fermi-GBM Team:

Swift-BAT detected GRB 211221A at 20:48:40 UT (GCN 31273). 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 identified no counterparts.

The GBM targeted search [1], the most sensitive, coherent search for
GRB-like signals identified a transient most significantly on the 8.192 s
timescale, with a location consistent with the Swift-BAT event and
a S/N of 21, using the standard search protocol.
The GBM targeted search event was found with the highest
significance with a "normal" spectrum (Band function with
Epeak = 230 keV, alpha = -1.0, beta = -2.3) for a GRB.

[1] Goldstein et al. 2019 arXiv:1903.12597


