# GCN_circulars

GRB_name: GRB211223B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31292
SUBJECT: Fermi GRB 211223B: Global MASTER-Net observations report 
DATE:    21/12/23 23:00:25 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 211223B ( Fermi GBM team, GCN 31287) errorbox  48951 sec after notice time and 48978 sec after trigger time at 2021-12-23 21:59:40 UT, with upper limit up to  16.5 mag. The observations began at zenith distance = 81 deg. The sun  altitude  is -48.9 deg. 

The galactic latitude b = 14 deg., longitude l = 73 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1824738

We obtain a following upper limits.  

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

   49008 | 2021-12-23 21:59:40 |          MASTER-IAC | (19h 50m 57.14s , +48d 39m 52.2s) |   C |    60 | 16.5 |        
   49088 | 2021-12-23 22:01:00 |          MASTER-IAC | (19h 52m 29.69s , +46d 44m 47.5s) |   C |    60 | 16.1 |        
   49935 | 2021-12-23 22:15:07 |          MASTER-IAC | (19h 50m 58.21s , +48d 38m 53.4s) |   C |    60 | 16.0 |        
   50016 | 2021-12-23 22:16:27 |          MASTER-IAC | (19h 52m 32.18s , +46d 46m 10.9s) |   C |    60 | 15.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211223A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31293
SUBJECT: GRB 211223A: Insight-HXMT/HE detection
DATE:    21/12/24 02:03:26 GMT
FROM:    Xiaolu Zhang at IHEP  <xlzhang@ihep.ac.cn>

X.L.Zhang, 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,
G. Li, J. Y. Liao, X. Y. Song, S. L. Xiong, C. Z. Liu,  C. K. Li, 
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 2021-12-23T02:40:35.450 (T0), Insight-HXMT/HE detected 
GRB 211223A (trigger ID: HEB211223111) in a routine search of the data, 
which also triggered GECAM (GECAM Team, GCN #31286) and CALET.

URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB211223111lc.png

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: GRB211223C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31294
SUBJECT: Swift GRB 211223C: Global MASTER-Net observations report 
DATE:    21/12/24 05:50:09 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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) was pointed to the Swift GRB 211223C ( P. A. Evans et al., GCN 31288) errorbox  54750 sec after notice time and 54769 sec after trigger time at 2021-12-24 05:42:16 UT, with upper limit up to  16.4 mag. The observations began at zenith distance = 82 deg. The sun  altitude  is -27.6 deg. 

The galactic latitude b = 26 deg., longitude l = 338 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1824979

We obtain a following upper limits.  

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

   54860 |          MASTER-IAC |   C |   180 | 16.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211223C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31295
SUBJECT: GRB 211223C: BOOTES-4/MET optical upper limit
DATE:    21/12/24 09:15:36 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 211223C by Swift (Evans et al. GCNC 31288), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical Observatory (China) automatically responded to this burst starting on Dec. 23 at 21:58:25 UT (~7.5 hours after trigger). No new source is detected within the BAT error region in the co-added image (60 x 20 s, clear filter) down to 20.1 mag.

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


GRB_name: GRB211223C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31297
SUBJECT: GRB 211223C: Swift-BAT refined analysis
DATE:    21/12/24 14:01:07 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC), 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 from the recent telemetry
downlink, we report further analysis of BAT GRB 211223C (trigger #1090656)
(Evans, et al., GCN Circ. 31288).  The BAT ground-calculated position is
RA, Dec = 227.165, -26.878 deg which is

   RA(J2000)  =  15h 08m 39.7s

   Dec(J2000) = -26d 52' 41.0"

with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment). The
partial coding was 32%.



The BAT light curve showed a complex structure with a duration of about 20
sec. T90 (15-350 keV) is 15.00 +- 5.00 sec (estimated error including
systematics).



The time-averaged spectrum from T-13.01 to T+8.99 sec is best fit by a
simple power-law model.  The power law index of the time-averaged spectrum
is 1.15 +- 0.09.  The fluence in the 15-150 keV band is 2.4 +- 0.1 x 10^-06
erg/cm2. The 1-sec peak photon flux measured from T-0.01 sec in the 15-150
keV band is 3.1 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90%
confidence level.



The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1090656/BA/


GRB_name: GRB211211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31299
SUBJECT: GRB 211211A: observations with the 3.6m Devasthal Optical Telescope
DATE:    21/12/24 16:40:23 GMT
FROM:    Rahul Gupta at ARIES, India  <rahulbhu.c157@gmail.com>

Rahul Gupta, S. B. Pandey, A. Ror, A. Kumar, A. Aryan, Dimple, A. Ghosh, B.
Kumar, and K. Misra (ARIES) as a part of larger international collaboration:


We performed late-time photometric observations of the optical afterglow (Zheng
and Filipenko GCN 31203) of Fermi (Fermi GBM team, GCN 31201) and Swift (D'Ai
et al., GCN 31202) detected GRB 211211A using the 4Kx4K CCD Imager (Pandey
et al. 2017, arXiv:1711.05422v1) mounted at the axial port of the 3.6m
Devasthal Optical Telescope of ARIES Nainital at multiple epochs in several
filters. We report the preliminary brightness of the afterglow to be R =
21.66 +/- 0.07 mag ~ 1.41 days after the GBM trigger. At successive epochs,
we obtained the limiting mag of 23.7 mag ~ 4.42 days post-burst. Our
observations are consistent with the rapid decay nature of the afterglow
reported by de Ugarte Postigo et al. GCN 31229 and A. Moskvitin et al. GCN
31234.

The magnitude value reported is calibrated against UNSO B1 nearby stars.

This circular may be cited. 3.6m Devasthal Optical Telescope (DOT) is
the recently commissioned facility in the Northern Himalayan region of
India (long:79 41 04E, lat:29 21 40N, alt:2540m) owned and operated by the
Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital (
https://www.aries.res.in). Authors of this GCN circular thankfully
acknowledge consistent support from the staff members to run and maintain
the 3.6m DOT.


GRB_name: GRB211106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31300
SUBJECT: GRB 211106A: Third HST Observation
DATE:    21/12/24 20:01:28 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 obtained a third observation at the site of the short GRB 211106A (GCNC #31049) with the Hubble Space Telescope starting on 2021 December 24.35 (48.15 days post-trigger, 29.0 days after Visit 1 - GCNC #31146, and 22.9 days after Visit 2 - GCNC #31157) using ACS/F814W for 2 orbits and WFC3/F110W for 2 orbits, as part of program 16303 (PI: Berger).  

The source identified in both our previous HST observations and near the reported CXO position of GRB 211106A (GCNC #31145) is still detected, with unchanged magnitudes of m(F110W) ~ 25.6 mag and m(F814W) ~ 25.7 mag.  We also detect an extension to the north of the source in stacked F814W imaging (Visit 1 + Visit 3) as previously noted in the F110W imaging (GCNC #31049). The lack of any change over this 29-day baseline, the relatively flat m(F814W)-m(F110W) color, the extension in both bands, and the small offset from the CXO position (GCNC #31145) support the hypothesis that this source is the more likely host galaxy of GRB 211106A."


GRB_name: GRB211224A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31301
SUBJECT: GRB 211224A: Fermi GBM Final Real-time Localization
DATE:    21/12/24 23:43:05 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 23:31:40 UT on 24 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211224A (trigger 662081505.061428 / 211224980).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 220.9, Dec = -41.6 (J2000 degrees, equivalent to J2000 14h 43m, -41d 36'), with a statistical uncertainty of 11.9 degrees.

The angle from the Fermi LAT boresight is 32.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211224980/quicklook/glg_skymap_all_bn211224980.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/bn211224980/quicklook/glg_healpix_all_bn211224980.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211224980/quicklook/glg_lc_medres34_bn211224980.gif


GRB_name: GRB211225B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31305
SUBJECT: GRB 211225B: Swift detection of a burst
DATE:    21/12/25 13:27:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (U Tampa),
F. E. Marshall (NASA/GSFC), T. M. Parsotan (GSFC/UMBC/CRESSTII) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 13:12:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211225B (trigger=1090853).  Swift did not slew because
of Sun constraint.  The BAT on-board calculated location is 
RA, Dec 258.568, +17.262 which is 
   RA(J2000)  =  17h 14m 16s
   Dec(J2000) = +17d 15' 45"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve is missing data from T+8 to T+108
sec, but there is an increase of 1400 event/sec at ~T+5 sec. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 23:13 UT on 2022 January 02. There will thus be no XRT
or UVOT data for this trigger before this time. 

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: GRB211225C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31306
SUBJECT: GRB 211225C: Fermi GBM Final Real-time Localization
DATE:    21/12/25 18:24:37 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 18:14:04 UT on 25 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211225C (trigger 662148849.44199 / 211225760).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 339.9, Dec = -59.0 (J2000 degrees, equivalent to J2000 22h 39m, -59d 00'), with a statistical uncertainty of 36.0 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/bn211225760/quicklook/glg_skymap_all_bn211225760.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/bn211225760/quicklook/glg_healpix_all_bn211225760.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211225760/quicklook/glg_lc_medres34_bn211225760.gif


GRB_name: GRB211225C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31307
SUBJECT: Fermi GRB 211225C: Global MASTER-Net observations report 
DATE:    21/12/25 19:30:24 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 211225C ( Fermi GBM team, GCN 31306) errorbox  2856 sec after notice time and 2884 sec after trigger time at 2021-12-25 19:02:09 UT, with upper limit up to  17.1 mag. Observations started at twilight.  The observations began at zenith distance = 71 deg. The sun  altitude  is -10.6 deg. 

The galactic latitude b = -51 deg., longitude l = 329 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1827113

We obtain a following upper limits.  

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

    2915 | 2021-12-25 19:02:09 |          MASTER-IAC | (21h 21m 59.02s , -29d 17m 33.3s) |   C |    60 | 15.2 |        
    2915 | 2021-12-25 19:02:09 |          MASTER-IAC | (21h 31m 16.29s , -29d 23m 28.3s) |   C |    60 | 15.2 |        
    2995 | 2021-12-25 19:03:29 |          MASTER-IAC | (21h 04m 29.50s , -29d 15m 44.4s) |   C |    60 | 15.1 |        
    2995 | 2021-12-25 19:03:29 |          MASTER-IAC | (21h 13m 46.67s , -29d 21m 39.8s) |   C |    60 | 15.1 |        
    3075 | 2021-12-25 19:04:49 |          MASTER-IAC | (21h 16m 21.79s , -27d 23m 23.3s) |   C |    60 | 15.5 |        
    3075 | 2021-12-25 19:04:49 |          MASTER-IAC | (21h 25m 29.34s , -27d 29m 18.0s) |   C |    60 | 15.5 |        
    3155 | 2021-12-25 19:06:09 |          MASTER-IAC | (21h 19m 59.12s , -33d 03m 55.7s) |   C |    60 | 15.5 |        
    3155 | 2021-12-25 19:06:09 |          MASTER-IAC | (21h 29m 39.18s , -33d 09m 51.5s) |   C |    60 | 15.4 |        
    3255 | 2021-12-25 19:07:48 |          MASTER-IAC | (21h 12m 13.12s , -33d 08m 33.6s) |   C |    60 | 15.4 |        
    3255 | 2021-12-25 19:07:48 |          MASTER-IAC | (21h 02m 31.80s , -33d 03m 18.3s) |   C |    60 | 14.8 |        
    3334 | 2021-12-25 19:09:08 |          MASTER-IAC | (21h 39m 19.77s , -31d 14m 06.6s) |   C |    60 | 16.0 |        
    3334 | 2021-12-25 19:09:08 |          MASTER-IAC | (21h 29m 50.78s , -31d 08m 47.3s) |   C |    60 | 15.7 |        
    3414 | 2021-12-25 19:10:28 |          MASTER-IAC | (21h 03m 53.96s , -31d 14m 34.2s) |   C |    60 | 15.8 |        
    3414 | 2021-12-25 19:10:28 |          MASTER-IAC | (20h 54m 24.49s , -31d 09m 17.6s) |   C |    60 | 15.0 |        
    3494 | 2021-12-25 19:11:48 |          MASTER-IAC | (21h 22m 26.34s , -35d 03m 57.5s) |   C |    60 | 15.9 |        
    3494 | 2021-12-25 19:11:48 |          MASTER-IAC | (21h 12m 31.71s , -34d 58m 42.8s) |   C |    60 | 15.4 |        
    3574 | 2021-12-25 19:13:08 |          MASTER-IAC | (21h 09m 09.61s , -27d 27m 29.3s) |   C |    60 | 16.6 |        
    3574 | 2021-12-25 19:13:08 |          MASTER-IAC | (21h 00m 01.03s , -27d 22m 08.4s) |   C |    60 | 15.8 |        
    3654 | 2021-12-25 19:14:28 |          MASTER-IAC | (21h 43m 21.35s , -27d 26m 40.9s) |   C |    60 | 17.1 |        
    3654 | 2021-12-25 19:14:28 |          MASTER-IAC | (21h 34m 12.97s , -27d 21m 19.4s) |   C |    60 | 16.6 |        
    3734 | 2021-12-25 19:15:48 |          MASTER-IAC | (21h 41m 02.66s , -35d 03m 53.9s) |   C |    60 | 16.6 |        
    3734 | 2021-12-25 19:15:48 |          MASTER-IAC | (21h 31m 08.14s , -34d 58m 38.3s) |   C |    60 | 16.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211225B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31308
SUBJECT: Swift GRB 211225B: Global MASTER-Net observations report 
DATE:    21/12/26 06:56:11 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 211225B ( K. L. Page et al., GCN 31305) errorbox  50155 sec after notice time and 50206 sec after trigger time at 2021-12-26 03:09:05 UT, with upper limit up to  16.5 mag. Observations started at twilight.  The observations began at zenith distance = 67 deg. The sun  altitude  is -16.1 deg. 

The galactic latitude b = 28 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=1826927

We obtain a following upper limits.  

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

   50296 |   MASTER-Kislovodsk |   C |   180 | 16.5 |        
   50296 |   MASTER-Kislovodsk |   C |   180 | 15.5 |        
   51607 |   MASTER-Kislovodsk |   C |   180 | 13.3 |        
   51607 |   MASTER-Kislovodsk |   C |   180 | 13.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211226A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31309
SUBJECT: GRB 211226A: AGILE/MCAL detection of a burst
DATE:    21/12/26 12:10:53 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), F. Verrecchia, C. Pittori (SSDC, and INAF/OAR), F.
Longo (Univ. Trieste and INFN Trieste), 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 (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), A. Giuliani
(INAF/IASF-Mi), report on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected a long burst at T0 = 2021-12-26
05:25:41.00 +/- 0.01 s (UTC) (INTEGRAL SPI-ACS trigger Tri,Sub: 9576,0).

The event lasted about 20 s and released a total number of 2736 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 613 Hz. The MCAL light curve shows several peaks and can be found
at http://www.agilescienceapp.it/notices/GRB211226A_AGILE_MCAL.png .

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 released a total
number of 492 counts in the SA detector (above a background rate of 115
Hz), 5996 counts in the MCAL detector (above a background rate of 1290 Hz),
and 16770 counts in the AC detector (above a background rate of 3530 Hz).
The AGILE ratemeter light curves can be found at
http://www.agilescienceapp.it/notices/GRB211226A_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: GRB211225A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31310
SUBJECT: GRB 211225A: MITSuME Akeno optical upper limits
DATE:    21/12/26 13:16:55 GMT
FROM:    Naohiro Ito at Tokyo Tech  <n.ito@hp.phys.titech.ac.jp>

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

We performed tiling observations for the MAXI/GSC error region of GRB
211225A, MAXI J0827-071 (T. Kurihara et al. GCN Circular #31303, V.
Lipunov et al. GCN Circular #31304) with an optical tri-color (g', Rc,
and Ic) camera attached to the MITSuME 50 cm telescope Akeno.

The follow up observation started at 2021-12-25 12:43:40 UT, 9.4 hours
after the trigger.

Our tiling observation covered almost ~90% of the MAXI/GSC elliptical
error region (GCN Circular #31303). 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 | 8:27:04, -7:19:28 | 25.1 x 24.8 | g'>18.1, Rc>18.4, Ic>17.9
| 2021-12-25 15:30:02 | 1260
Field 01 | 8:28:39, -7:19:27 | 26.1 x 25.1 | g'>18.1, Rc>18.4, Ic>17.6
| 2021-12-25 15:36:28 | 1380
Field 02 | 8:27:01, -6:54:21 | 26.3 x 24.0 | g'>18.3, Rc>18.7 |
2021-12-25 16:31:42 | 2400
Field 03 | 8:28:37, -6:54:57 | 26.3 x 24.6 | g'>18.0, Rc>18.4, Ic>17.8
| 2021-12-25 16:48:59 | 1620
--------------------------------------------------------------------------------------------------------------------------
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: GRB211225B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31312
SUBJECT: GRB 211225B: Swift-BAT refined analysis
DATE:    21/12/27 00:17:54 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC),
H. A. Krimm (NSF), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), K. L. Page (U Leicester),
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 from the recent telemetry
downlink, we report further analysis of BAT GRB 211225B (trigger #1090853)
(Page et al., GCN Circ. 31305).  The BAT ground-calculated position is
RA, Dec = 258.545, 17.277 deg which is
   RA(J2000)  =  17h 14m 10.9s
   Dec(J2000) = +17d 16' 37.2"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~T-25 s and likely lasts beyond ~T+152 s when the burst went out of the
BAT
field of view. The main peak occurs at ~T+50 s. T90 (15-350 keV)
estimated from the available data when the burst was inside the BAT field
of view is 121.54 +- 2.94 sec (estimated error including systematics).

The time-averaged spectrum from T-24.78 to T+139.82 sec is best fit by
a power law with an exponential cutoff.  This fit gives a photon
index 1.31 +- 0.14, and Epeak of 139.9 +- 51.5 keV (chi squared 52.29
for 56 d.o.f.).  For this model the total fluence in the 15-150 keV
band is 1.5 +- 0.03 x 10^-5 erg/cm2 and the 1-sec peak flux measured
from T+50.19 sec in the 15-150 keV band is 6.1 +- 0.3 ph/cm2/sec.
A fit to a simple power law gives a photon index of 1.59 +- 0.03
(chi squared 64.87 for 57 d.o.f.).  All the quoted errors are at
the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1090853/BA/


GRB_name: GRB211226A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31313
SUBJECT: GRB 211226A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    21/12/27 14:18:01 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 211226A (T0: 2021-12-26T05:25:41 UTC,
INTEGRAL/SPI-ACS trig #9576, AGILE GCN 31309).

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), detects the burst with a sqrt(TS) of 86.7 in a
8.192 s analysis time bin.
The duration of the burst in BAT is ~12 seconds.

NITRATES results strongly indicate a burst coming from outside the
coded FOV, with DeltaLLHOut of -256.

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: GRB211227A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31316
SUBJECT: GRB 211227A: Swift detection of a burst
DATE:    21/12/27 23:48:49 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), S. D. Barthelmy (GSFC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. M. Parsotan (GSFC/UMBC/CRESSTII),
B. Sbarufatti (PSU), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 23:32:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211227A (trigger=1091101).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 132.126, -2.702 which is 
   RA(J2000) = 08h 48m 30s
   Dec(J2000) = -02d 42' 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 100 sec.  The peak count rate
was ~5200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 23:33:20.3 UT, 73.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 132.14898,
-2.73556 which is equivalent to:
   RA(J2000)  = 08h 48m 35.76s
   Dec(J2000) = -02d 44' 08.0"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 146 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 (2.37 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.3
(+3.24/-2.79) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 6.84e-09 erg cm^-2 s^-1 (0.2-10
keV). 

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 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
0.020. 

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


GRB_name: GRB211221A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31317
SUBJECT: GRB 211221A: Swift/UVOT Upper Limits
DATE:    21/12/28 00:14:08 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 211221A
63 s after the BAT trigger (Page et al., GCN Circ. 31273).
No optical afterglow consistent with the XRT position (Evans et al.
GCN Circ. 31275) 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            63          213          147         >20.7
u_FC               275          525          246         >20.1
white               63         1010          317         >21.1
v                  606          799           39         >18.6
b                  531          724           39         >19.4
u                  275          872          285         >20.0
w1                 655          848           39         >18.1
m2                 631          650           19         >17.8
w2                 582          774           39         >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.143 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB211227A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31318
SUBJECT: GRB 211227A: BOOTES-2/TELMA optical upper limit
DATE:    21/12/28 01:09:43 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, T.-R. Sun, E. Fernandez-Garcia, A. J. Castro-Tirado, M.D. Caballero-Garcia, R. Sanchez-Ramirez (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga), R. Fernandez-Munoz (IHSM/UMA-CSIC) and M. Jelinek (ASU-CAS), on behalf of a larger collaboration, report:

Following the detection of GRB 211227A by Swift (Beardmore et al. GCNC 31316), the 0.6m BOOTES-2/TELMA robotic telescope at IHSM La Mayora (UMA-CSIC) in Algarrobo Costa (Malaga, Spain) automatically responded to this burst starting on Dec. 27 at 23:32:49 UT (~43 s after trigger). But due to technical problems, only images taken after 23:42 UT (~10 min after trigger) could be used. No new source is detected within the XRT error region in the co-added image (20 x 10 s, clear filter) down to 19.9 mag. This non-detection is consistent with the report from MASTER (Lipunov et al. GCNC 31315) and UVOT (Beardmore et al. GCNC 31316).

We thank the staff at La Mayora for its excellent support.


GRB_name: GRB211227A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31319
SUBJECT: GRB 211227A: MAXI/GSC detection
DATE:    21/12/28 01:13:44 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

M. Tominaga (JAXA), Y. Kawakubo (LSU), M. Serino (AGU), 
H. Negoro, 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, T. Nagatsuka, T. 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 23:32:06 UT on 2021 December 27.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (132.253 deg, -2.658 deg) = (08 49 00, -02 39 28) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.12 deg and 0.09 deg, respectively. 
The roll angle of long axis from the north direction is 66.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 630 +- 48 mCrab
(4.0-10.0keV, 1 sigma error).

We conclude that this event is coincidence with the GRB event reported by Swift
(R.A., Dec) = (132.14898,-2.73556) (J2000)  (GCN #31316).


GRB_name: GRB211227A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31320
SUBJECT: GRB 211227A: Nanshan/NEXT optical observations and host galaxy candidate
DATE:    21/12/28 02:22:53 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 211227A (Beardmore et al. GCN Circ. 31316) 
using the NEXT-0.6m telescope located at Nanshan, Xinjiang, China. 
Observations automatically started at 23:33:37 UT on 2021-12-27 (i.e., 
90.14 s after the BAT trigger), and a series of 40 s, 60 s, 90 s frames 
were obtained in the Sloan r-filter.

Within the Swift/XRT error circle (Beardmore et al. GCN Circ. 31316), no 
uncatalogued optical transient is detected in our stacked image down to 
a limiting magnitude of r ~ 20.0 mag, calibrated with the nearby 
PanSTARRS field.

However, there exists a known source at the border of the Swift/XRT 
error circle at coordinates: R.A. (J2000)=08:48:35.975 and Dec (J2000)= 
-02:44:06.93, which has r ~ 19.6 mag from Nanshan/NEXT, r ~ 19.40 mag 
and classified as galaxy with a photo-redshift of 0.244 +/- 0.0888 from 
SDSS, r ~ 19.47 mag from PanSTARRS, as well as r ~ 19.25 from Legacy 
Survey. No apparent brightening of the galaxy is seen in comparison of 
Nanshan/NEXT and different surveys, indicating that the contribution of 
the optical counterpart of the burst is negligible if the galaxy is the 
host of the burst.


GRB_name: GRB211227A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31321
SUBJECT: GRB 211227A: LCO Optical Observations
DATE:    21/12/28 02:51:59 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 211227A (Beardmore, et al., GCN 31316) with the LCO 1-m Sinistro instrument at the Teide, Tenerife site, on December 28, from 00:39 to 01:11 UT (corresponding to 1.12 to 1.48 hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 4x240s exposures in R and I bands. We detect no sources within the Swift XRT detection region (Beardmore, et al., GCN 31316) in either band. The following upper limits are calculated using the USNO-B.1 catalog as reference:

R>22.81
I>22.42

We do note the presence of a faint uncatalogued source just outside the XRT region at RA, DEC = (132.1449185, -2.7343489) at the following magnitudes, calculated with respect to the USNO-B.1 catalog:

R=21.79+/-0.20
I=22.13+/-0.24

We recommend continued monitoring of this source to determine if it is fading.  These magnitudes are not corrected for galactic extinction.

R.S. is funded by NSF AST grant #1831682


GRB_name: GRB211227A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31322
SUBJECT: GRB 211227A: Enhanced Swift-XRT position
DATE:    21/12/28 03:27:50 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 789 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 211227A, 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 = 132.14889, -2.73531 which is equivalent
to:

RA (J2000): 08h 48m 35.73s
Dec (J2000): -02d 44' 07.1"

with an uncertainty of 2.6 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB211227A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31323
SUBJECT: GRB 211227A: Liverpool Telescope upper limits
DATE:    21/12/28 05:27:43 GMT
FROM:    Daniel Perley at Liverpool JMU  <d.a.perley@ljmu.ac.uk>

D. A. Perley (LJMU) reports:

We acquired imaging at the position of GRB 211227A (Beardmore et al., 
GCN 31316) using the IO:O camera of the 2m robotic Liverpool Telescope. 
The field was observed twice in the griz filters on 2021-12-28 UT, with 
the first epoch taking place between 00:36:10 and 00:45:43 and the 
second between 02:04:43 and 02:14:18.

No new source is detected within or near the XRT position (Goad et al., 
GCN 31322) after digital subtration of reference imaging from the 
Pan-STARRS 1 survey.  Photometry with reference to PS1 secondary 
standard stars in the field gives the following upper limits:

dt(days)    magnitude
0.04449     g > 21.99
0.04625     r > 22.62
0.04799     i > 22.68
0.04974     z > 21.36

The LCO source mentioned by Strausbaugh et al. (GCN 31321) is detected 
in PS1 reference imaging and is also marginally detected in both sets of 
(unsubtracted) LT images and is far from the enhanced XRT error circle, 
suggesting it is unlikely to be related to the GRB.





DisclaimerNone


GRB_name: GRB211227A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31324
SUBJECT: GRB 211227A: A possible short GRB with extended emission at z = 0.228?
DATE:    21/12/28 12:22:53 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Radboud Univ. and DAWN/NBI), L. Izzo (DARK/NBI), D. Xu 
(NAOC/CAS), A. de Ugarte Postigo (Obs. de la Cote d'Azur), D. A. Kann 
(IAA/CSIC), A. J. Levan (Radboud Univ.), Z.P. Zhu (NAOC, HUST), S.Y. Fu 
(NAOC), report on behalf of the Stargate collabaration:

We observed the location of GRB 211227A (Beardmore et al., GCN 31316) 
using the ESO VLT UT3 (Melipal) equipped with the X-shooter 
spectrograph. Short images were secured with the acquisition camera in 
the g, r, and z filters. No new object is detected inside the revised 
XRT error circle (Goad et al., GCN 31322) down to an AB magnitude r > 
24.7 (mean time Dec 28.191 UT).

The galaxy mentioned by Fu et al. (GCN 31320) is well detected in our 
image. Its core lies 3.66" away of the center of the XRT circle (2.4" 
90% error radius), though its wings extend towards it.

A spectrum of this object was secured, covering the wavelength range 
3000-21000 AA, and consisting of 4 exposures of 600 s each. The 
observation mid time was 2021 Dec 28.21 UT (5.60 hr after the GRB). We 
detect several emission lines, which we interpret as due to [O II], 
Hbeta, [O III] 5007, Halpha, [N II], [S II] all at a common redshift z = 
0.228. Absorption features due to Ca II 3933/3968 and the Na I D doublet 
5890/5896 are also visible at the same redshift. This value is 
consistent with the SDSS photometric redshift. The galaxy is fairly 
bright, with an absolute magnitude M_r ~ -21.3 (AB) using i = 18.84 (AB) 
from SDSS.

We point out the similarity of the gamma-ray light curve of GRB 211227A 
(e.g. https://gcn.gsfc.nasa.gov/notices_s/1091101/BA/) with that of GRB 
060614 (e.g. Gehrels et al. 2006, Nature, 444, 1044), suggested by some 
authors to be a merger event (e.g. Yang et al. 2015, Nat. Comm., 6, 
7323). The location of the GRB, slightly offset from a bright, nearby 
galaxy, would also be consistent with this interpretation. We raise the 
possibility that GRB 211227A is a short GRB with extended emission. 
However, a long GRB, either hosted by the z = 0.228 galaxy, or in the 
background, remains a viable possibility.

We encourage further observations of this potentially interesting event 
at all wavelengths.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Israel Blanchard, Robert De Rosa, and Fuyan Bian.


GRB_name: GRB211227A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31326
SUBJECT: GRB 211227A: Swift-BAT refined analysis
DATE:    21/12/28 17:01:31 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC),  H. A. Krimm (NSF), S. Laha
(GSFC/UMBC), 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 from the recent telemetry
downlink, we report further analysis of BAT GRB 211227A (trigger #1091101)
(Beardmore et al., GCN 31316).  The BAT ground-calculated position is RA,
Dec = 132.144, -2.736 deg which is

   RA(J2000)  =  08h 48m 34.5s

   Dec(J2000) = -02d 44' 10.9"

with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The
partial coding was 41%.



The BAT light curve showed a complex structure with a duration of about 100
sec. T90 (15-350 keV) is 83.79 +- 8.47 sec (estimated error including
systematics).



The time-averaged spectrum from 0.04 to 126.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is 1.60
+- 0.05.  The fluence in the 15-150 keV band is 8.0 +- 0.2 x 10^-06
erg/cm2. The 1-sec peak photon flux measured from T+0.06 sec in the 15-150
keV band is 5.1 +- 0.4 ph/cm2/sec.  All the quoted errors are at the 90%
confidence level.



The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1091101/BA/


GRB_name: GRB211227A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31327
SUBJECT: GRB 211227A: Swift-XRT refined Analysis
DATE:    21/12/28 18:27:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), A. D'Ai
(INAF-IASFPA), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), B.
Sbarufatti (PSU), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester) and A.P. Beardmore report on behalf of the Swift-XRT team:

We have analysed 8.1 ks of XRT data for GRB 211227A (Beardmore et al.
GCN Circ. 31316), from 63 s to 57.9 ks after the  BAT trigger. The data
comprise 182 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. 31322).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.27 (+0.21, -0.20). At T+105 s  the decay
steepens to an alpha of 2.27 (+0.20, -0.17) before breaking again at
T+220 s to a final decay with index alpha=5.49 (+0.37, -0.30).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.11 (+/-0.07). The
best-fitting absorption column is  2.2 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 2.4 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 6.1 x 10^-11 (6.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      2.2 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 7.8 sigma
Photon index:      1.11 (+/-0.07)

If the light curve continues to decay with a power-law decay index of
5.49, the count rate at T+24 hours will be 7.3 x 10^-14 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x
10^-24 (4.9 x 10^-24) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01091101.

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


GRB_name: GRB211227A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31328
SUBJECT: GRB 211227A: Swift/UVOT Upper Limits
DATE:    21/12/28 19:38:09 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and A. P. Beardmore (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 211227A
82 s after the BAT trigger (Beardmore et al., GCN Circ. 31316).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 31322)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            82          232          147         >19.4
u_FC               294          544          246         >19.2
white               82         1021          334         >19.5
v                  624         4923          241         >18.7
b                  550          742           39         >18.6
u                  294         5431          357         >19.4
w1                 673         5333          235         >19.7
m2                 648         5127          235         >20.4
w2                 772          792           19         >19.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.020 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB211229A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31329
SUBJECT: GRB 211229A: Fermi GBM Final Real-time Localization
DATE:    21/12/29 03:39:48 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 03:29:15 UT on 29 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211229A (trigger 662441360.901398 / 211229145).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 295.0, Dec = 22.9 (J2000 degrees, equivalent to J2000 19h 40m, 22d 53'), with a statistical uncertainty of 3.7 degrees.

The angle from the Fermi LAT boresight is 94.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211229145/quicklook/glg_skymap_all_bn211229145.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/bn211229145/quicklook/glg_healpix_all_bn211229145.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211229145/quicklook/glg_lc_medres34_bn211229145.gif


GRB_name: GRB211229A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31330
SUBJECT: Fermi GRB 211229A: Global MASTER-Net observations report 
DATE:    21/12/29 04:30:30 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 211229A ( Fermi GBM team, GCN 31329) errorbox  264 sec after notice time and 292 sec after trigger time at 2021-12-29 03:34:08 UT, with upper limit up to  16.0 mag. Observations started at twilight.  The observations began at zenith distance = 77 deg. The sun  altitude  is -11.9 deg. 

The galactic latitude b = -0 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=1831397

We obtain a following upper limits.  

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

     323 | 2021-12-29 03:34:08 |   MASTER-Kislovodsk | (19h 27m 54.52s , +27d 51m 45.4s) |   C |    60 | 15.5 |        
     323 | 2021-12-29 03:34:08 |   MASTER-Kislovodsk | (19h 32m 07.22s , +27d 27m 37.1s) |   C |    60 | 15.7 |        
     403 | 2021-12-29 03:35:28 |   MASTER-Kislovodsk | (19h 25m 20.18s , +25d 55m 56.8s) |   C |    60 | 16.0 |        
     403 | 2021-12-29 03:35:29 |   MASTER-Kislovodsk | (19h 29m 28.21s , +25d 31m 46.2s) |   C |    60 | 16.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211229A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31331
SUBJECT: GRB 211229A: GECAM detection
DATE:    21/12/29 05:33:48 GMT
FROM:    Guoying Zhao at IHEP  <gyzhao@ihep.ac.cn>

G. Y. Zhao, S. L. Xiong, X. L. Zhang , S. Xiao, C. Cai, J. J. He, Y. Huang,
Z. W. Guo, C. Y. Li, X. B. Li, J. C. Liu, X. Y. Song,Y. Zhao, 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, Z. Zhang,C. W. Wang, S. J. Zheng (IHEP),
report on behalf of GECAM team:

During the commissioning phase, GECAM-B was triggered in-flight by a long 
burst, GRB 211229A, at 2021-12-29T03:30:05.200 UTC (denoted as T0),
which was also observed by Fermi/GBM (GCN #31329).
 
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_94447805.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra:  302.7 deg 
Dec: 27.5 deg
Err: 8.7 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 location is very close to SGR J1935+2154 and cannot be ruled out as 
originating from it. The GECAM preliminary location could be found here: 
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_skymap_fit_94447805.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: GRB211225B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31332
SUBJECT: GRB 211225B: CALET Gamma-Ray Burst Monitor detection
DATE:    21/12/29 07:10:45 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

N. Cannady (GSFC/UMBC),
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, T. Tamura (Kanagawa U), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 211225B (Swift detection and refined analysis: Page et al.,
GCN Circ. 31305, Laha et al., GCN Circ. 31312;
https://gcn.gsfc.nasa.gov/other/211225B.gcn3) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 13:13:05.685 UTC on 25 December 2021 while exiting
the radiation belts. The burst signal was seen by all CGBM detectors.
Because of a problem in one of the ground alert processing script, the GCN
notice was not distributed automatically for this event.

The burst light curve shows a single pulse which starts at T-2.2 sec,
peaks at T+3.6 sec and ends at T+42.0 sec. The extended tail is seen in
the low energy channels as long as a hint of the preceding emission (which
is clearly seen in the Swift-BAT light curve: Laha et al. GCN Circ. 31312).
The T90 and T50 durations measured by the SGM data are 32.7 +- 8.1 sec and
14.6 +- 1.9 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1324473176/

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


GRB_name: GRB211227A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31333
SUBJECT: GRB 211227A: CALET Gamma-Ray Burst Monitor detection
DATE:    21/12/29 08:03:36 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

M. L. Cherry (LSU),
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, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 211227A (Swift detection and refined analysis:
Beardmore et al., GCN Circ. 31316, Lien et al., GCN Circ. 31326;
MAXI/GSC detection: Tominaga et al., GCN Circ. 31319;
https://gcn.gsfc.nasa.gov/other/211227A.gcn3) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 23:32:07.476 UTC on 27 December 2021.
The burst signal was seen by all CGBM detectors.
Because of a problem in one of the ground alert processing script, the GCN
notice was not distributed automatically for this event.

The burst light curve shows a multi-peaked structure which starts
at T-0.6 sec and ends at T+77.2 sec.
The T90 and T50 durations measured by the SGM data are 64.5 +- 10.3 sec and
22.0 +- 2.0 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1324683113/

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


GRB_name: GRB211229A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31334
SUBJECT: GRB 211229A: Swift/BAT-GUANO arcminute localization
DATE:    21/12/29 14:16:59 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 localize GRB 211229A onboard (T0:
2021-12-29T03:29:15 UTC, Fermi/GBM GCN 31329, GECAM GCN 31331).

The Fermi 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), confidently detects the burst in a 16.384 s
analysis time bin with a sqrt(TS) of 50.
Estimated duration in the detector is greater than 60 s.

A confident arcminute localization is found with DeltaLLHOut of 567
and a DeltaLLHPeak of 269.

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 = 295.044, 23.133  deg which is
   RA(J2000)  = 19h 40m 10.56s
   Dec(J2000) =  +23d 07â€² 58â€³
with an estimated uncertainty of 4 arcmin.

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: GRB211229A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31335
SUBJECT: GRB 211229A: Swift ToO observations
DATE:    21/12/29 15:06:32 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 211229A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021475

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: GRB211229B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31336
SUBJECT: GRB 211229B: Fermi GBM Final Real-time Localization
DATE:    21/12/29 22:29:19 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:18:43 UT on 29 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211229B (trigger 662509128.09648 / 211229930).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 185.0, Dec = -18.4 (J2000 degrees, equivalent to J2000 12h 20m, -18d 23'), with a statistical uncertainty of 1.1 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/bn211229930/quicklook/glg_skymap_all_bn211229930.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/bn211229930/quicklook/glg_healpix_all_bn211229930.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211229930/quicklook/glg_lc_medres34_bn211229930.gif


GRB_name: GRB211229B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31337
SUBJECT: Fermi GRB 211229B: Global MASTER-Net observations report 
DATE:    21/12/29 22:45:22 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 211229B ( Fermi GBM team, GCN 31336) errorbox  706 sec after notice time and 746 sec after trigger time at 2021-12-29 22:31:09 UT, with upper limit up to  15.0 mag. The observations began at zenith distance = 86 deg. The sun  altitude  is -64.4 deg. 

The galactic latitude b = 44 deg., longitude l = 293 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1832170

We obtain a following upper limits.  

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

     822 | 2021-12-29 22:31:09 |   MASTER-Kislovodsk | (12h 18m 50.50s , -18d 16m 56.8s) |  P- |   150 | 14.6 |        
    1007 | 2021-12-29 22:34:00 |   MASTER-Kislovodsk | (12h 18m 40.48s , -18d 41m 39.4s) |   C |   180 | 15.0 |        
    1208 | 2021-12-29 22:37:21 |   MASTER-Kislovodsk | (12h 18m 41.80s , -18d 40m 33.5s) |   C |   180 | 14.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211229C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31338
SUBJECT: GRB 211229C: Swift/BAT-GUANO detection likely outside the coded FOV
DATE:    21/12/30 01:23:12 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 localize GRB 211229C (T0: 2021-12-29T09:36:08
UTC,INTEGRAL/SPI-ACS 9580).

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), detects the burst with a sqrt(TS) of 10.4 in a
4.096 s analysis time bin.

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FOV, with a
borderline DeltaLLHOut of 7 and no specific location in the FOV
preferred.

Independent spectral or fluence measurements of this burst from other
instruments could help determine the preferred origin.

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: GRB211229B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31339
SUBJECT: GRB 211229B: GECAM detection
DATE:    21/12/30 03:35:18 GMT
FROM:    Guoying Zhao at IHEP  <gyzhao@ihep.ac.cn>

G. Y. Zhao, S. L. Xiong, X. L. Zhang , S. Xiao, C. Cai, J. J. He, Y. Huang,
Z. W. Guo, C. Y. Li, X. B. Li, J. C. Liu, X. Y. Song,Y. Zhao, 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, Z. Zhang,C. W. Wang, 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 211229B, at 2021-12-29T22:18:43.150 UTC (denoted as T0)ï¼Œ
which was also observed by Fermi/GBM (GCN #31336).

This burst mainly consists of multiple pulses with duration of about 15 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/211229B_LightCurve.png

The GECAM preliminary location could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/SkyMap.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: GRB211229A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31340
SUBJECT: GRB 211229A: Fermi GBM observation
DATE:    21/12/30 05:30:27 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

"At 03:29:15.90 UT on 29 December 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211229A (trigger 662441360 / 211229145),
which was also detected by the Swift/BAT-GUANO (Tohuvavohu et al, GCN 31334).
The Fermi GBM Final Real-time Localization (GCN 31329) is consistent
with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 95 degrees.

The GBM light curve shows multiple pulses
with a duration (T90) of about 120 s (50-300 keV).
The time-averaged spectrum from T0-10 s to T0+147 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.24 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 280 +/- 27 keV.

The event fluence (10-1000 keV) in this time interval is
(3.07 +/- 0.11)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+53.2 s in the 10-1000 keV band
is 3.74 +/- 0.28 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: GRB211227A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31341
SUBJECT: GRB 211227A: Deep early CAHA 2.2m/CAFOS observation
DATE:    21/12/30 11:25:54 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (Obs. Cote d'Azur), C. 
C. Thoene, M. Blazek (both HETH), J. F. Agui Fernandez (HETH/IAA-CSIC),  
and S. Gongora (CAHA) report:

We observed the localization of GRB 211227A (Swift detection: Beardmore 
et al., GCN #31316; Enhanced XRT position: Goad et al., GCN #31322; 
MAXI/GSC Detection: Tominaga et al., GCN #31319) with CAFOS, mounted on 
the 2.2 m telescope, at the Calar Alto Observatory (Almeria, Spain). The 
observation started at 00:08:45 UT on 28 December 2021 (36.65 min after 
the GRB) and consisted of 30 x 90 s integrations in the i' band. 
Observing conditions were mediocre (wind, some clouds, 3" seeing).

Our combined image is centered at 0.04233 d after the trigger. No 
afterglow is detected in the XRT error circle, in agreement with other 
observations (Lipunov et al., GCN #31315; Hu et al., GCN #31318; Fu et 
al., GCN #31320; Strausbaugh et al., GCN #31321; Perley, GCN #31323; 
Malesani et al., GCN #31324; Belles et al., GCN #31328). This area is 
affected by the outer PSF wing of a bright nearby star, causing a 
variable background. Using an isolated SDSS star, we measure a limit 
away from the stellar PSF of i' > 23.4 mag, but caution this limit will 
be somewhat less deep in the XRT error circle.

Assuming the GRB is associated with the nearby galaxy at redshift z = 
0.228 (Malesani et al., GCN #31324), a comparison with the light curve 
of GRB 060614 (Kann et al. 2011, ApJ, 734, 96) reveals this limit is 
about 3 magnitudes fainter than the equivalent afterglow magnitude for 
GRB 060614 at the same redshift.


GRB_name: GRB211229A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31342
SUBJECT: GRB 211229A: Swift-XRT and UVOT observations
DATE:    21/12/30 17:29:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (SSDC & INAF-OAR), S. R. Oates (U.Birmingham), A. D'Ai
(INAF-IASFPA), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), D.N.
Burrows (PSU), J.P. Osborne (U. Leicester), K.L. Page (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 211229A (Tohuvavohu et al., GCN
Circ. 31334), also detected by Fermi/GBM and GECAM  (Fermi GBM team,
GCN Circ. 31329, Zhao et al., GCN Circ. 31331), collecting 5.0 ks of
Photon Counting (PC) mode data between T0+43.6 ks and T0+66.8 ks. 

Four uncatalogued X-ray sources have been detected consistent with
being within 394 arcsec of the Swift/BAT-GUANO position, however none
of them is above the RASS limit or shows definitive signs of fading.
Therefore, at the present time we cannot identify which, if any, is the
afterglow. Details of these sources are given below:

Source 1:
  RA (J2000):  295.1317  =  19:40:31.60
  Dec (J2000): +23.1983  =  +23:11:53.8
  Error: 6.3 arcsec (radius, 90% conf.)
  Count-rate: (3.5 [+1.3, -1.0])e-3 ct s^-1   
  Distance: 252 arcsec from Swift/BAT-GUANO position.
  Flux: (2.78 [+1.01, -0.83])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 2:
  RA (J2000):  295.0615  =  19:40:14.76
  Dec (J2000): +23.2617  =  +23:15:42.0
  Error: 9.7 arcsec (radius, 90% conf.)
  Count-rate: (1.60 [+0.88, -0.66])e-3 ct s^-1  
  Distance: 398 arcsec from Swift/BAT-GUANO position.

Source 5:
  RA (J2000):  295.0738  =  19:40:17.70
  Dec (J2000): +23.1573  =  +23:09:26.3
  Error: 6.6 arcsec (radius, 90% conf.)
  Count-rate: (2.12 [+0.97, -0.76])e-3 ct s^-1  
  Distance: 20 arcsec from Swift/BAT-GUANO position.
  Flux: (1.59 [+0.72, -0.57])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 6:
  RA (J2000):  295.1187  =  19:40:28.49
  Dec (J2000): +23.1638  =  +23:09:49.7
  Error: 5.3 arcsec (radius, 90% conf.)
  Count-rate: (2.94 [+1.13, -0.91])e-3 ct s^-1  
  Distance: 151 arcsec from Swift/BAT-GUANO position.

An uncatalogued source was also detected, however this was too far from
the GRB position to be the afterglow.

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/00021475.

No optical afterglow consistent with the GUANO position
(Tohuvavohu et al., GCN Circ. 31334)
is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial
exposures are:

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

u   43722       66830       4882    >21.0

The magnitudes in the table are not corrected for the Galactic
extinction
due to the reddening of E(B-V) = 5.811 in the direction of the burst
(Schlegel et al. 1998).

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


GRB_name: GRB211231A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31343
SUBJECT: GRB 211231A: Fermi GBM Final Real-time Localization
DATE:    21/12/31 07:11:46 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 07:00:31 UT on 31 Dec 2021, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 211231A (trigger 662626836.787242 / 211231292).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 292.2, Dec = -24.9 (J2000 degrees, equivalent to J2000 19h 28m, -24d 53'), with a statistical uncertainty of 1.8 degrees.

The angle from the Fermi LAT boresight is 62.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211231292/quicklook/glg_skymap_all_bn211231292.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/bn211231292/quicklook/glg_healpix_all_bn211231292.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2021/bn211231292/quicklook/glg_lc_medres34_bn211231292.gif


GRB_name: GRB211229B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31344
SUBJECT: GRB 211229B: AGILE detection
DATE:    21/12/31 14:35:32 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (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, E. Menegoni, 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 211229B at T0 = 2021-12-29
22:18:43 (UTC), reported by Fermi GBM (GCN #31336) and GECAM (GCN #31339).

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 40 s and
it released a total number of 5440 counts in the SA detector (above a
background rate of 120 Hz), 48230 counts in the MCAL detector (above a
background rate of 1170 Hz), and 141030 counts in the AC detector (above a
background rate of 3440 Hz). The AGILE ratemeters light curves can be found
at http://www.agilescienceapp.it/notices/GRB211229B_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, covering the main peak of the burst, from T1 = 2021-12-29
22:18:45.12 s +/- 0.01 (UTC) to T2 = 2021-12-29 22:18:48.83 +/- 0.01 s
(UTC), and released 2354 counts in the detector, above a background rate of
620 Hz. The time-integrated spectrum of the burst in this time interval can
be fitted in the energy range 0.4-20 MeV with a power-law with ph. ind. =
-2.45 (-0.82/+1.53), resulting in a reduced chi-squared of 1.40 (34 d.o.f.)
and a fluence of 1.8e-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/GRB211229B_AGILE_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.


GRB_name: GRB211231A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31345
SUBJECT: GRB 211231A: GECAM detection
DATE:    21/12/31 14:40:56 GMT
FROM:    Xiaolu Zhang at IHEP  <xlzhang@ihep.ac.cn>

Z. W. Guo, S. L. Xiong, G. Y. Zhaoï¼ŒX. L. Zhang , S. Xiao, C. Cai, J. J. He, 
Y. Huang,C. Y. Li, X. B. Li, J. C. Liu, X. Y. Song,Y. Zhao, 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, Z. Zhang,C. W. Wang, 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 211231A, at 2021-12-31T07:00:35.050 UTC (denoted as T0)ï¼Œ
which was also observed by Fermi/GBM (GCN #31343).

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/GRB211231Alc.png

An automatic on-ground localization was calculated using the light curves
and spectrum. Although the in-flight calibration of energy response and
localization has not been finalized yet, GECAM-B localized this burst to
the following position (J2000):
ra: 295.1 deg
dec: -7.0 deg
err: 5.0 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: GRB211219A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31346
SUBJECT: IPN triangulation of GRB 211219A
DATE:    21/12/31 15:44:38 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, D. Frederiks, A. Ridnaia, A. Lysenko, and
T. Cline on behalf of the Konus-Wind team,

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

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

A long-duration GRB 211219A
(Fermi-GBM detection: Fermi GBM Team, GCN Circ. 31265;
Swift/BAT-GUANO detection: Tohuvavohu et al., GCN Circ. 31269;
AGILE-MCAL detection: Ursi et al., GCN Circ. 31270;
AstroSat-CZTI detection: Prasad et al., GCN Circ. 31283)
was detected by Fermi (GBM trigger 661618527), Swift (BAT),
AGILE (MCAL), AstroSat (CZTI), Konus-Wind, INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND) and BepiColombo (MGNS) at
about 53722 s UT (14:55:22).
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:
    58.652 (03h 54m 37s) -34.619 (-34d 37' 09")
  Corners:
    59.468 (03h 57m 52s) -34.736 (-34d 44' 11")
    57.992 (03h 51m 58s) -34.656 (-34d 39' 23")
    57.835 (03h 51m 20s) -34.491 (-34d 29' 27")
    59.309 (03h 57m 14s) -34.575 (-34d 34' 30")
  ---------------------------------------------
The error box area is 676 sq. arcmin, and its maximum
dimension is 1.37 deg (the minimum one is 6 arcmin).
The Sun distance was 115 deg.

This box may be improved.

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

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB211219_T53724/IPN


GRB_name: GRB220101A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31347
SUBJECT: GRB 220101A: Swift detection of a burst with a bright optical counterpart
DATE:    22/01/01 05:32:40 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Tohuvavohu (U Toronto), J.D. Gropp (PSU), J. A. Kennea (PSU),
A. Y. Lien (U Tampa), 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 05:09:55 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220101A (trigger=1091101).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 1.380, +31.753 which is 
   RA(J2000) = 00h 05m 31s
   Dec(J2000) = +31d 45' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT lightcurve shows a complex lightcurve
extending to at least T+170 with a peak of 7000 counts/s (15-350 keV), 
at ~89 sec after the trigger. 

The XRT began observing the field at 05:11:32.2 UT, 80.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 1.3561, 31.7702 which is equivalent to:
   RA(J2000)  = 00h 05m 25.46s
   Dec(J2000) = +31d 46' 12.7"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 95 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 1.30e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 89 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 00:05:24.82 = 1.35340
  DEC(J2000) = +31:46:08.5  =  31.76903
with a 90%-confidence error radius of about 0.61 arc sec. This position is 9.3
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.60 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.056. 

Burst Advocate for this burst is A. Tohuvavohu (aaron.tohu 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: GRB220101A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31348
SUBJECT: GRB 220101A: Correction to GCN 31347
DATE:    22/01/01 05:53:46 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

GCN circular 31347 incorrectly referred to the BAT trigger number of the burst.
The correct trigger number for GRB 220101A is 1091527.

I apologize for any confusion this may have caused.
Happy new year!


GRB_name: GRB220101A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31349
SUBJECT: GRB 220101A: Enhanced Swift-XRT position
DATE:    22/01/01 08:34:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 1177 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 220101A, 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 = 1.35374, +31.76890 which is equivalent
to:

RA (J2000): 00h 05m 24.90s
Dec (J2000): +31d 46' 08.0"

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: GRB220101A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31350
SUBJECT: GRB 220101A: Fermi-LAT detection
DATE:    22/01/01 14:08:57 GMT
FROM:    Lorenzo Scotton at CNRS/IN2P3/LUPM  <lorenzo.scotton@lupm.in2p3.fr>

M. Arimoto (Kanazawa Univ.), L. Scotton (CNRS/IN2P3/LUPM) and F. Longo 
(University and INFN, Trieste)
report on behalf of the Fermi-LAT Collaboration:

On January 1st, 2022, Fermi-LAT detected high-energy emission from
GRB 220101A, which was also detected by Swift (trigger 1091527, 
Tohuvavohu et al. GCN Circ. 31347)

The best LAT on-ground location is found to be

RA, Dec = 1.52, 31.75 (degrees, J2000)

with an error radius of 0.46 deg (90% containment, statistical error only).
This was 18 deg from the LAT boresight at the time of the Swift trigger:

T0 =  05:10:11.5 UT.

The data from the Fermi-LAT show a significant increase
in the event rate after the Swift trigger that is spatially correlated 
with the
Swift emission (0.14 degrees from the Swift-XRT location) with high 
significance.
The photon flux above 100 MeV in the time interval 0-600s after the
Swift trigger is 2.5E-5 +/- 5E-6 ph/cm2/s.

The estimated photon index above 100 MeV is -2.46 +/- 0.25.

The Fermi-LAT point of contact for this burst is
Lorenzo Scotton (lorenzo.scotton AT lupm.in2p3.fr).

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


GRB_name: GRB220101A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31351
SUBJECT: GRB 220101: Swift/UVOT Detection
DATE:    22/01/01 14:09:07 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

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

The Swift/UVOT began settled observations of the field of GRB 220101
90 s after the BAT trigger ( Tohuvavohu et al., GCN Circ. 31347).
A rapidly decayig source consistent with the XRT position
(Osborne et al., GCN Circ. 31349) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  00:05:24.80 =   1.35334 (deg.)
    Dec (J2000) = +31:46:08.4  =  31.76899 (deg.)
with an estimated uncertainty of 0.42 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               90          240          147         14.68 +/- 0.02
v                 4448         4647          197         18.70 +/- 0.18
b                 3833         4032          197        >19.8
u                 3628         5201          334        >20.1
w1                4858         5057          197        >20.1
m2                4652         4852          197        >20.2
w2                4243         4443          197        >20.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.056 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31353
SUBJECT: GRB 220101A: Xinglong-2.16m photometry and spectroscopy
DATE:    22/01/01 15:51:07 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

S.Y. Fu (NAOC), Z.P. Zhu (NAOC, HUST), D. Xu, X. Liu, S.Q. Jiang (NAOC) 
report on behalf of a larger collaboration:

We observed the field of GRB 220101A detected by Swift (Tohuvavohu et 
al., GCN 31347) and Fermi (Arimoto et al., GCN 31350) using the 
Xinglong-2.16m telescope equipped with the BFOSC camera. Observations 
were carried out starting at 09:50:07 UT on 2022-01-01. We firstly 
obtained 4x300 s frames in each of the B, V, R and I bands, and then 
2x1800 s spectroscopy covering ~3800 - 8800 AA.

The optical afterglow of the burst (Tohuvavohu et al., GCN 31347) is 
clearly detected in each of our stacked images in the V, R and I bands, 
but no in the B band. Preliminary photometry is as follows:

Tmid-T0 (hr)   Mag     MagErr  Filter
   5.55           >21.43       N/A      B
   5.45            19.86        0.06      V
   5.36            18.65        0.02      R
   5.27            17.34        0.01      I

The spectrum is in low resolution and rather low S/N. However, a broad 
absorption feature is evident centering at ~ 6820 AA, which can 
interpreted as Ly_alpha absorption. Besides Ly_alpha, other weak lines 
such as Si II, C II, Si IV are also detected at the common redshift of z 
= 4.61. We thus conclude that z = 4.61 is likely the redshift of the GRB.

We thank the great support of the Xinglong-2.16m staff, in particular 
Junjun Jia, Yinan Zhu, Aiying Zhou, and Jie Zheng.


GRB_name: GRB220101A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31354
SUBJECT: GRB 220101A: AGILE detection
DATE:    22/01/01 19:53:20 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi, E. Menegoni (INAF/IAPS), F. Longo (Univ. Trieste and INFN
Trieste), C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), P. Tempesta
(TeleSpazio), 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), A. Giuliani (INAF/IASF-Mi), report
on behalf of the AGILE Team:

The AGILE satellite detected the long GRB 220101A at T0 = 2022-01-01
05:11:22 (UTC), reported by Swift  BAT (GCN #31347, #31348), Swift XRT (GCN
#31349), Swift UVOT (GCN #31351), and Fermi LAT (GCN #31350).

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 80 s and
it released a total number of 14577 counts in the SA detector (above a
background rate of 100 Hz), 95830 counts in the MCAL detector (above a
background rate of 1140 Hz), and 256390 counts in the AC detector (above a
background rate of 3215 Hz). The AGILE ratemeters light curves can be found
at http://www.agilescienceapp.it/notices/GRB220101A_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, from T1 = 2022-01-01 05:11:21.50 +/- 0.01 s (UTC) to T2 =
2022-01-01 05:11:55.74 +/- 0.01 s (UTC), and released 10934 counts in the
detector, above a background rate of 570 Hz. The time-integrated spectrum
of the burst in this time interval can be fitted in the energy range
0.4-100 MeV with a power-law with ph. ind. = -1.28 (-0.11/+0.11), resulting
in a reduced chi-squared of 0.96 (84 d.o.f.) and a fluence of 7.8e-05
ergs/cm^2 (90% confidence level), in the same energy range.

We divided the data acquisition into four time intervals: interval a
[T0-0.5 s, T0+10.0 s], interval b [T0+10.0 s, T0+17.0 s], interval c
[T0+17.0 s, T0+24.0 s], and interval d [T0+24.0 s, T0+34.0 s]. The spectral
analysis in the energy range 0.4-100 MeV shows an evolution of the power
law photon index in the first stages of the burst, passing from -0.98 to
-1.70. Details are reported below:

  | model | ph. ind.           | red chi^2 (dof) | fluence (erg/cm^2)
a | PL    | 0.98 (-0.29/+0.19) | 1.00 (75)       | (1.8+/-0.2)e-5
b | PL    | 0.93 (-0.40/+0.22) | 0.98 (75)       | (8.3+/-0.8)e-6
c | PL    | 1.31 (-0.22/+0.23) | 0.99 (75)       | (1.1+/-0.1)e-5
d | PL    | 1.70 (-0.13/+0.29) | 1.05 (75)       | (2.6+/-0.3)e-5

The MCAL light curve can be found at:
http://www.agilescienceapp.it/notices/GRB220101A_AGILE_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.


GRB_name: GRB220101A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31355
SUBJECT: GRB 220101A: Swift-XRT refined Analysis
DATE:    22/01/01 19:55:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.1 ks of XRT data for GRB 220101A (Tohuvavohu et al.
GCN Circ. 31347), from 73 s to 34.6 ks after the  BAT trigger. The data
comprise 322 s in Windowed Timing (WT) mode (the first 6 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN Circ. 31349).

The late-time light curve (from T0+3.6 ks) can be modelled with an
initial power-law decay with an index of alpha=1.6 (+0.8, -0.4),
followed by a break at T+4385 s to an alpha of 5.8 (+0.6, -0.4).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.519 (+0.023, -0.016). The
best-fitting absorption column is  consistent with the Galactic value
of 6.3 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.59 (+/-0.07) and a best-fitting absorption column
of 7 (+12, -7) x 10^21 cm^-2. The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 4.2 x
10^-11 (4.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 6.3 x 10^20 cm^-2
Intrinsic column:    7 (+12, -7) x 10^21 cm^-2 at z=4.61
Photon index:      1.59 (+/-0.07)

If the light curve continues to decay with a power-law decay index of
5.8, the count rate at T+24 hours will be 2.8 x 10^-7 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-17 (1.3 x 10^-17) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01091527.

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


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31356
SUBJECT: GRB 220101A: THO optical observations
DATE:    22/01/01 21:29:30 GMT
FROM:    Veli-Pekka Hentunen at Taurus Hill Obs,A95  <veli-pekka.hentunen@kassiopeia.net>

Veli-Pekka Hentunen, Markku Nissinen and Esa Heikkinen (Taurus Hill
Observatory, Varkaus, Finland) report:

We have detected GRB 220101A optical afterglow at Taurus Hill 
Observatory (A95) using Meade 16" ACF 0.40-m/f8.0 telescope 
and ASI2600MM Pro CMOS camera. We used Chroma Bessell 
photometric VRI filters. The observations were started at 2022-01-01 
14:40 (UT).

The optical afterglow was detected at the position RA 00:05:24.8 
and DEC +31:46:09.7.

The following magnitudes were obtained from the observations using 
USNO-B1.0 1217-1802 (V=15.29, R=14.70, I=14.74) as a comparison star:

Tmid(h)+T0    Filter Exp. time    Mag Mag. Err.    
9.733  V 300s >18.7 
9.994  I 300s 17.91 0.08
10.168  R 300s 19.26 0.13
10.661  I 3x300s 18.08 0.10
10.835  R 3x300s 19.16 0.13

URL-link to our image: 
https://www.kassiopeia.net/wp-content/uploads/2022/01/grb220101a_I2_nega_web.jpg


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31357
SUBJECT: GRB 220101A: Liverpool telescope imaging of a high-redshift afterglow
DATE:    22/01/01 22:14:13 GMT
FROM:    Daniel Perley at Liverpool JMU  <d.a.perley@ljmu.ac.uk>

D. A. Perley (LJMU) reports:

We acquired multicolor imaging of the optical afterglow of GRB 220101A
(Tohuvavohu et al., GCN 31347) using the IO:O camera of the 2m robotic
Liverpool Telescope.  The afterglow was observed twice in the griz
filters on 2022-01-01 UT, with the first epoch taking place between
20:07 and 20:17 and the second between 21:21 and 21:31.

Photometry with reference to SDSS secondary standard stars in
the field gives the following magnitudes:

dt(d)   filter mag   unc
0.6236  g      21.97 0.10
0.6254  r      19.84 0.03
0.6271  i      18.48 0.03
0.6288  z      18.20 0.03
0.6749  g      22.21 0.13
0.6767  r      19.92 0.03
0.6784  i      18.58 0.03
0.6802  z      18.27 0.03

Magnitudes are given in the SDSS system and uncorrected for extinction. 
Times are referenced to the BAT trigger time.

The colors are consistent with a moderately high-redshift (z = 4-5) 
afterglow, in agreement with the result of Fu et al. (GCN 31353).





DisclaimerNone


GRB_name: GRB220101A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31358
SUBJECT: GRB 220101A: CAHA 2.2m/CAFOS detection
DATE:    22/01/01 22:29:15 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

A. de Ugarte Postigo (Obs. Cote d'Azur), D  A. Kann (HETH/IAA-CSIC), C. 
C. Thoene, M. Blazek (both HETH), J. F. Agui Fernandez (HETH/IAA-CSIC), 
P. Martin, and I. Hermelo (both CAHA) report:

We observed the afterglow of GRB 220101A (Swift detection: Tohuvavohu et 
al., GCN #31347; Fermi/LAT Detection: Arimoto et al., GCN #31350; AGILE 
detection: Ursi et al., GCN #31354; afterglow detections: Kuin & 
Tohuvavohu, GCN #31351; Fu et al., GCN #31353; Hentunen et al., GCN 
#31356; Perley, GCN #31357; redshift z = 4.61: Fu et al., GCN #31353) 
with CAFOS, mounted on the 2.2 m telescope, at the Calar Alto 
Observatory (Almeria, Spain). The observation started at 19:35:31 UT on 
01 January 2022 (13.47 hr after the GRB) and consisted of 6 x 90 s 
integrations in the i' band.

The afterglow is well-detected in the individual images. Against 
comparison stars from SDSS, we measure i' = 18.45 +/- 0.03 mag (AB) in 
the stacked image at mid-time 0.60177 d after the trigger.

We note this is a very bright GRB and afterglow, further follow-up is 
encouraged.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31359
SUBJECT: GRB 220101A: NOT redshift confirmation
DATE:    22/01/01 23:43:26 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

J. P. U. Fynbo (DAWN/NBI), A. de Ugarte Postigo (Obs. Cote d'Azur), D. 
Xu (NAOC), D. B. Malesani (Univ. Radobud and DAWN/NBI), B. 
Milvang-Jensen (DAWN/NBI), J. Viuho (NOT and DAWN/NBI), report on behalf 
of a larger collaboration:

We observed the optical counterpart of GRB 220101A (Tohuvavohu et al., 
GCN 31347; Arimoto et al., GCN 31350) using the Nordic Optical Telescope 
(NOT) equipped with the ALFOSC spectrograph. A spectrum with exposure 
time 4x1200 s (grism #20) was secured starting on 2022 Jan 1.81 UT (14.3 
hr after the GRB), under good conditions, and covering the wavelength 
range 5600-10200 AA.

A very clear trace is detected from the afterglow continuum. A deep, 
broad trough is detected around 6800 AA, which we interpret as due to 
damped Lyman alpha. A number of narrow absorption features are also 
clearly visible and allow to determine accurately the GRB redshift. We 
identify, among others, N V, S II, Si II, Si II*, O I, Ni II, C II, Si 
IV, C IV, Fe II, Fe II*, and Al II, all at a common redshift z = 4.618. 
Our results thus fully confirm the finding of Fu et al. (GCN 31353).

Nice year start for GRBs: happy 2022 to all GCN readers!


GRB_name: GRB220101A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31360
SUBJECT: GRB 220101A: Fermi GBM Detection
DATE:    22/01/02 00:16:28 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

S. Lesage (UAH) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:

"At 05:17:12 UT on 01 January 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220101A (trigger 662706616/220101215)
which was also detected by Swift-BAT (A. Tohuvavohu et al. 2022, GCN 31347),
Swift-XRT (J.P. Osborne et al. 2022, GCN 31349), Fermi-LAT (M. Arimoto et
al. 2022, GCN 31350), Swift/UVOT (N. P. M. Kuin et al. 2022, GCN 31351),
and AGILE (A. Ursi et al. 2022, GCN 31354).
The Fermi GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 38 degrees.

The GBM light curve consists of multiple emission episodes with a duration (T90)
of about 128 s (10-1000 keV). The time-averaged spectrum
from T0-65 to T0+179 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.09 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 330 +/- 15 keV.

The event fluence (10-1000 keV) in this time interval is
(7.7 +/- 0.1)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+90.4 s in the 10-1000 keV band is 11 +/- 0.3 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 290 +/- 18 keV, alpha = -1.06 +/- 0.02 and beta = -2.3 +/- 0.2.

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: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31361
SUBJECT: GRB220101A: optical afterglow detection from Konkoly Observatory
DATE:    22/01/02 00:53:01 GMT
FROM:    Jozsef Vinko at Konkoly Observator  <vinko@konkoly.hu>

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

We observed the field of GRB220101A (Tohuvavohu et al., GCN #31347; Arimoto et al., 
GCN #31350; AGILE Ursi et al., GCN #31354) 
with the RC80 robotic telescope at Piszkesteto Station of Konkoly
Observatory on 2022 Jan 01  starting at 21:32:18 UT. A series of 5x300 sec
frames were collected through Sloan r'- and i' bands. The bright optical afterglow
(Kuin & Tohuvavohu, GCN #31351; Fu et al., GCN #31353; Hentunen et al., GCN
#31356; Perley, GCN #31357; Ugarte Postigo et al. GCN #31358; Fynbo et al. GCN #31359)
is clearly detected on the stacked frames with the following magnitudes, calibrated
via nearby PS1 stars:

Date         UT-middle   t-T0(hr)  Exp(s)   r'(AB-mag)       i'(AB-mag)
2022-01-01   21:52:52    16.73     5x300    19.81 +/- 0.12   18.67 +/- 0.14 


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31363
SUBJECT: GRB 220101A: Asiago spectroscopic and photometric detection
DATE:    22/01/02 01:19:25 GMT
FROM:    Lina Tomasella at INAF,Padova  <lina.tomasella@inaf.it>

L. Tomasella (INAF-OAPadova),  E. Brocato (INAF-OAAbruzzo), M. Dâ€™Onofrio (DFA UniPd),  E. Cappellaro, S. Benetti (INAF-OAPadova)


On behalf a larger collaboration report:

We observed the optical counterpart of GRB 220101A (Tohuvavohu et al., 
GCN 31347; Arimoto et al., GCN 31350) using the Asiago Copernico and Schmidt Robotic telescopes (INAF-OAPadova). 
The Copernico Telescope is equipped with the AFOSC spectrograph. A  low S/N spectrum was obtained starting on 2022-01-01 UT 22:21:03, covering the wavelength range 3400-8200 AA.

As reported by Fu at al., GCN 31353 and by Fymbo et al., GCN 31359, a deep, broad feature is detected around 6800 AA, interpreted as the damped Lyman alpha. Other narrow absorption lines are also detected, which allow to confirm the GRB redshift z = 4.61

The afterglow was observed starting on 2022-01-01 between 22:01 and 22:05 UT using Copernico Telescope with BV filters  and with gri Sloan filters (two series) using Schmidt 67/92 Robotic Telescope between 22:08 and 22:25 UT. 
The afterglow is detected in several individual images. 
We measure V-Bessel = 20.48 +/- 0.1 mag in the Copernico image taken at UT 22:01. 

The spectral and photometric analysis results presented above are preliminary; data analysis is ongoing. 


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31364
SUBJECT: GRB 220101A: GMG observation
DATE:    22/01/02 03:43:02 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, B.-L. Lun, and J.-M. Bai (YNAO) report:




We observed the field of GRB 220101A (Tohuvavohu et al. GCN 31347) with the 2.4-meter optical

telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at

UT 12:31:35, 1, Jan. 2022, about 7.3 hours after the trigger. We clearly detected the afterglow.

The preliminary magnitude was measured to be R~19.0. The weather turned to be cloudy, and it

prevented us from further observations.




We appreciate all the astronomers working during the holidays. Happy new year!     


GRB_name: GRB220101A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31365
SUBJECT: GRB 220101A : Eiso equals the maximum isotropic GRB energy
DATE:    22/01/02 09:38:15 GMT
FROM:    Jean-Luc Atteia at IRAP  <jean-luc.atteia@irap.omp.eu>

J.-L. Atteia reports:

A quick calculation of the isotropic energy of GRB 220101A, whose prompt emission was detected from space by Swift/BAT (A. Tohuvavohu et al. 2022, GCN 31347), Fermi/LAT (M. Arimoto et al. 2022, GCN 31350), AGILE (A. Ursi et al. 2022, GCN 31354), and Fermi/GBM (Lesage et al. 2022, GCN 31360) was done using the redshift z = 4.618 measured at Xinlong (Fu et al. 2022, GCN 31353) and NOT (Fynbo te al. 2022, GCN 31359) and the spectral parameters measured by Fermi/GBM (Lesage et al. 2022, GCN 31360).

The isotropic energy of GRB 220101A reaches 3.7 10^54 ergs, equaling the maximum isotropic energy measured for GRBs to date (Atteia et al. 2017, ApJ 837, 119).


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31366
SUBJECT: GRB 220101A: OASDG optical observations
DATE:    22/01/02 11:29:48 GMT
FROM:    Luca Izzo at DARK/NBI  <luca.izzo@gmail.com>

A. Noschese, L. Dâ€™Avino (OASDG), A. Di Dato (INAF/Naples & OASDG), L. Izzo (DARK/NBI) report:

We observed the field of GRB 220101A (Tohuvavohu et al., GCN #31347; Arimoto et al., GCN #31350; Ursi et al., GCN #31354) with the 0.5m telescope of the Osservatorio Astronomico S. Di Giacomo located in Agerola, Italy ( https://osservatorio.astrocampania.it/ ). We obtained three sets of 7x180s images in the Rc filter and two sets of 7x180s images in the Ic filter under moderate weather conditions (average humidity ~87%). The afterglow is clearly detected in the stacked Ic images, being quite fainter in the Rc stacked images, at the position reported by Swift-UVOT (Kuin & Tohuvavohu, GCN #31351) and by optical telescopes (Fu et al., GCN #31353; Hentunen et al., GCN #31356; Perley et al., GCN #31357; de Ugarte Postigo et al., GCN #31358; Fynbo et al., GCN #31359; Vinko et al., GCN #31361; Tomasella et al., GCN #31363; Mao et al., GCN #31364). We report the following preliminary magnitudes (AB)

Filter   Tmid-T0(days)   Mag.      Delta Mag.
Rc       0.568                 19.10     0.09  
Ic        0.586                 18.13     0.07
Rc       0.604                 19.40     0.20
Ic        0.620                 18.16     0.09
Rc       0.638                 19.09     0.17

The calibration was performed using nearby stars in the Pan-STARRS PS1 catalog, using transformation equations to Rc and Ic magnitudes.

We want to mention that these observations were done exactly one year after the damage caused to the OASDG instrumentation by a lightning storm. The detection of a GRB at z=4.618 (Fu et al., GCN #31353; Fynbo et al., GCN #31359) during one of the first observing nights following last year's disaster represents a big result for our group.


GRB_name: GRB211231A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31367
SUBJECT: GRB 211231A: AstroSat CZTI detection
DATE:    22/01/02 12:16:26 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), A. Suresh (IITB), 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 211231A which was
also detected by Fermi-GBM (GCN 31343) and GECAM (Guo et al. GCN 31345).
 

The source was clearly detected in the 20-200 keV energy range. The
light curve peaks at 2021-12-31 07:00:35.75 UT. The measured peak count
rate associated with the burst is 193 (+60, -27) cts/s above the
background in the combined data of three quadrants, with a total of 599
(+188, -196) cts. The local mean background count rate was 362 (+4, -4)
cts/s. Using cumulative rates, we measure a T90 of 13 (+1, -7) s. 

It was also clearly detected in the CsI anticoincidence (Veto) detector
in the 100-500 keV energy range. The light curve peaks at 2021-12-31
07:00:35.88 UT. The measured peak count rate is 562 (+73, -75) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 1536 (+452, -569) cts. The local mean background count rate was
1590 (+4, -4) cts/s. We measure a T90 of 8 (+3, -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. 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: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31368
SUBJECT: GRB 220101A: GMG observation (2nd epoch)
DATE:    22/01/02 13:50:03 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, B.-L. Lun, and J.-M. Bai (YNAO) report:




We observed the field of GRB 220101A (Tohuvavohu et al. GCN 31347) with the 2.4-meter optical

telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories again. The observation began at

UT 11:39:51, 2, Jan. 2022, about 30.5 hours after the trigger. We still clearly detected the

afterglow. The preliminary magnitude was measured to be R~20.1. We encourage the continued

follow-up observations.  


GRB_name: GRB220101A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31369
SUBJECT: GRB 220101A: Swift-BAT refined analysis
DATE:    22/01/02 14:20:30 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),  H. A. Krimm (NSF), S. Laha
(GSFC/UMBC), A. Y. Lien (U Tampa), 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-240 to T+962 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220101A (trigger #1091527)
(Tohuvavohu et al. GCN 31347).  The BAT ground-calculated position is RA,
Dec = 1.360, 31.758 deg which is

   RA(J2000)  =  00h 05m 26.4s

   Dec(J2000) = +31d 45' 28.3"

with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment). The
partial coding was 64%.



The BAT lightcurve shows a complex lightcurve extending to at least T+170
with a peak of 7000 counts/s (15-350 keV), at ~89 sec after the trigger.
T90 (15-350 keV) is 173.36 +- 12.76 sec (estimated error including
systematics).



The time-averaged spectrum from T-58.08 to T+259.11 sec is best fit by a
power law with an exponential cutoff.  This fit gives a photon index 1.13
+- 0.13,  and Epeak of 249.1 +- 161.8 keV (chi squared 42.49 for 56
d.o.f.).  For this model the total fluence in the 15-150 keV band is 2.5 +-
0.0 x 10^-05 erg/cm2 and the 1-sec peak flux measured from T+89.07 sec in
the 15-150 keV band is 7.3 +- 0.3 ph/cm2/sec.  A fit to a simple power law
gives a photon index of 1.34 +- 0.03 (chi squared 50.91 for 57 d.o.f.).  All
the quoted errors are at the 90% confidence level.



The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1091527/BA/


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31370
SUBJECT: GRB 220101A: Tautenburg observations
DATE:    22/01/02 14:42:12 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Klose, S. Melnikov, B. Stecklum, U. Laux (all
TLS Tautenburg) report:

We observed the field of GRB 220101A (Tohuvavohu et al., GCN 31347) with
the Tautenburg 1.34m Schmidt telescope equipped with the TAUKAM 6kx6k CCD
camera.

Observations were performed on January 1, 2022, at a midtime of 22.14 UT.
For the optical transient (Tohuvavohu et al., GCN 31347; Kuin &
Tohuvavohu, GCN 31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356;
Perley et al., GCN 31357; de Ugarte Postigo et al., GCN 31358; Fynbo et
al., GCN 31359; Vinko et al., GCN 31361; Tomasella et al., GCN 31363; Mao
et al., GCN 31364; Noschese et al., GCN 31366; Mao et al., GCN 31368) we
measure

r = 19.86 +/- 0.13 mag (AB),

calibrated against the SDSS catalogue.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31371
SUBJECT: GRB 220101A: LCO Optical Observations
DATE:    22/01/02 22:42:55 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 220101A (Tohuvavohu, et al., GCN 31347) with the LCO 1-m Sinistro instrument at the Teide, Tenerife site, on January 2, from 21:41 to 22:03 UT (corresponding to 40.53 to 40.90 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 clearly detect the source at the UVOT detection coordinates and other optical observations (Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN 31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356;
Perley et al., GCN 31357; de Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko et al., GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCN 31364; Noschese et al., GCN 31366; Mao et al., GCN 31368) in both bands. The following magnitudes are calculated using the USNO-B.1 catalog as reference:

R=19.76+/-0.11
I=18.03+/-0.13

These magnitudes are not corrected for galactic extinction.

R.S. is funded by NSF AST grant #1831682


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31372
SUBJECT: GRB 220101A: ALMA detection
DATE:    22/01/02 23:28:47 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (Radboud U.) reports on behalf of a larger collaboration:

"We observed GRB 220101A (Tohuvavohu et al., GCN 31347) with the Atacama
Large Millimeter/Submillimeter Array (ALMA) at 97.5 GHz beginning on 2021
January 02 20:37:22 UT (39.5 h after the burst)

Preliminary analysis reveals a mm source with flux density of ~ 0.1 mJy at
position:

RA (J2000) = 00:05:24.80
Dec (J2000) = +31:46:08.41

with uncertainty ~ 0.03" in each coordinate, consistent with the X-ray
position (Osborne et al., GCN 31349) and optical position (Tohuvavohu et
al., GCN 31347; Hentunen et al., GCN 31356). Further observations are
planned.

We thank the JAO staff, AoD, P2G, and the entire ALMA team for their help
with these observations."


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31373
SUBJECT: GRB 220101A: TNG NIR afterglow detection
DATE:    22/01/03 12:20:15 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. D'Avanzo (INAF-OAB), A. Melandri, S. Covino (INAF-OAB), V. D'Elia (ASI-SSDC), M. De Pasquale (Univ. Messina), D. B. Malesani (Radboud), 
S. Piranomonte (INAF-OAR), V. Lorenzi, C. Padilla (INAF-TNG), Paolo Giacobbe (INAF-OATO) on behalf of the CIBO collaboration report:

We observed the field of GRB 220101A (Tohuvavohu et al., GCN Circ. 31347; Arimoto et al., GCN Circ. 31350; Ursi et al., GCN Circ. 31354; 
Lesage & Meegan, GCN Circ. 31360) with the Italian 3.6m TNG telescope equipped with the near-infrared camera NICS. A series of images 
were obtained with the J, H, K filters on 2022-01-02 from 20:21:15 UT to 21:57:47 UT (i.e. at a mid time of about 1.67 days after the burst). 

A source is clearly detected in all bands at the optical and mm afterglow position (Kuin & Tohuvavohu, GCN Circ. 31351; Laskar, GCN Circ. 31372). 
From preliminary photometry we derive the following magnitude:

J = 18.29 +/- 0.05

(Vega; calibrated against the 2MASS catalogue).

We report the presence of a possibly extended source which lies about 1.8â€ North with respect to the NIR GRB afterglow. For this source we derive J ~ 20 mag (Vega). 
We note that this source is present in the CatWISE2020 catalogue (Marocco et al., 2021, ApJSS, 253, 22; arXiv:2012.13084).  


GRB_name: GRB211229B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31375
SUBJECT: GRB 211229B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/01/03 17:54:26 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 211229B (T0: 2021-12-29T22:18:43 UTC,
Fermi/GBM GCN 31336, GECAM GCN 31339, AGILE GCN 31344,
INTEGRAL/SPI-ACS #9581).

The INTEGRAL, Fermi, 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 12.4 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.

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: GRB211227A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31376
SUBJECT: GRB 211227A: Gemini South Optical Observations
DATE:    22/01/03 18:44:12 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (GWU, UMD), E. Troja (NASA-GSFC), A. Gottlieb (UMD, NASA-GSFC)
report on behalf of a larger collaboration:

We observed the field of GRB 211227A (Beardmore et al., GCN #31316)
with Gemini/GMOS-S on December 30, 2021 starting at 05:36:43 UT
(corresponding to ~2.3 d post-trigger). The observations were performed
in i-band with a total exposure of 15x120 s at airmass 1.2 with good
weather conditions and seeing ~0.7".

Within the XRT enhanced position (Goad et al., GCN #31322), we do not
detect any source to depth i>26 AB mag. This is consistent with
other non-detections currently reported (Lipunov et al., GCN #31315;
Hu et al., GCN #31318; Fu et al., GCN #31320; Strausbaugh et al.,
GCN #31321; Perley, GCN #31323; Malesani et al., GCN #31324;
Belles et al., GCN #31328, Kann et al., GCN #31341).
Due to the potentially nearby distance (z=0.228; Malesani et al.,
GCN #31324), these observations disfavor a GRB-supernova similar
to SN1998bw. In terms of probing potential kilonova emission,
this limit would have detected an AT2017gfo-like event at z=0.228.

We thank the staff of the Gemini Observatory, in particular Janice
Lee and Venu Kalari, for rapid scheduling of these observations.


GRB_name: GRB220103A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31377
SUBJECT: GRB 220103A: Fermi GBM Final Real-time Localization
DATE:    22/01/03 21:13:33 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 21:03:12 UT on 3 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220103A (trigger 662936597.88881 / 220103877).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 36.9, Dec = -15.7 (J2000 degrees, equivalent to J2000 02h 27m, -15d 41'), with a statistical uncertainty of 8.4 degrees.

The angle from the Fermi LAT boresight is 63.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220103877/quicklook/glg_skymap_all_bn220103877.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220103877/quicklook/glg_healpix_all_bn220103877.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220103877/quicklook/glg_lc_medres34_bn220103877.gif


GRB_name: GRB220103A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31378
SUBJECT: Fermi GRB 220103A: Global MASTER-Net observations report 
DATE:    22/01/03 21:46:32 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220103A ( Fermi GBM team, GCN 31377) errorbox  30 sec after notice time and 58 sec after trigger time at 2022-01-03 21:04:11 UT, with upper limit up to  18.4 mag. The observations began at zenith distance = 49 deg. The sun  altitude  is -35.4 deg. 

The galactic latitude b = -64 deg., longitude l = 191 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1836950

We obtain a following upper limits.  

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

      63 | 2022-01-03 21:04:11 |          MASTER-IAC | (02h 14m 13.48s , -19d 40m 00.4s) |  P| |    10 | 16.1 |        
      83 | 2022-01-03 21:04:11 |          MASTER-IAC | (02h 14m 13.48s , -19d 40m 00.4s) |  P| |    50 | 17.3 |  Coadd 
      63 | 2022-01-03 21:04:11 |          MASTER-IAC | (02h 15m 11.64s , -19d 46m 35.0s) |  P- |    10 | 15.7 |        
      83 | 2022-01-03 21:04:11 |          MASTER-IAC | (02h 15m 11.64s , -19d 46m 35.0s) |  P- |    50 | 16.9 |  Coadd 
      99 | 2022-01-03 21:04:41 |          MASTER-IAC | (02h 14m 19.59s , -19d 39m 44.1s) |  P| |    20 | 16.8 |        
      99 | 2022-01-03 21:04:41 |          MASTER-IAC | (02h 15m 17.72s , -19d 46m 18.6s) |  P- |    20 | 16.4 |        
     139 | 2022-01-03 21:05:21 |          MASTER-IAC | (02h 14m 17.38s , -19d 38m 13.8s) |  P| |    20 | 16.7 |        
     139 | 2022-01-03 21:05:21 |          MASTER-IAC | (02h 15m 15.46s , -19d 44m 48.3s) |  P- |    20 | 16.4 |        
     184 | 2022-01-03 21:06:01 |          MASTER-IAC | (02h 14m 17.38s , -19d 39m 33.0s) |  P| |    30 | 17.2 |        
     229 | 2022-01-03 21:06:01 |          MASTER-IAC | (02h 14m 17.38s , -19d 39m 33.0s) |  P| |   120 | 17.9 |  Coadd 
     184 | 2022-01-03 21:06:01 |          MASTER-IAC | (02h 15m 15.43s , -19d 46m 06.7s) |  P- |    30 | 16.9 |        
     229 | 2022-01-03 21:06:01 |          MASTER-IAC | (02h 15m 15.43s , -19d 46m 06.7s) |  P- |   120 | 17.8 |  Coadd 
     239 | 2022-01-03 21:06:51 |          MASTER-IAC | (02h 14m 19.94s , -19d 38m 03.3s) |  P| |    40 | 17.4 |        
     239 | 2022-01-03 21:06:51 |          MASTER-IAC | (02h 15m 17.98s , -19d 44m 37.2s) |  P- |    40 | 17.0 |        
     304 | 2022-01-03 21:07:51 |          MASTER-IAC | (02h 14m 14.94s , -19d 39m 00.8s) |  P| |    50 | 17.6 |        
     304 | 2022-01-03 21:07:51 |          MASTER-IAC | (02h 15m 12.96s , -19d 45m 34.8s) |  P- |    50 | 17.3 |        
     384 | 2022-01-03 21:09:01 |          MASTER-IAC | (02h 14m 15.27s , -19d 38m 01.3s) |  P| |    70 | 17.7 |        
     384 | 2022-01-03 21:09:01 |          MASTER-IAC | (02h 15m 13.24s , -19d 44m 34.7s) |  P- |    70 | 17.5 |        
     628 | 2022-01-03 21:13:10 |          MASTER-IAC | (02h 25m 19.39s , -25d 29m 21.6s) |   C |    60 | 18.4 |        
     628 | 2022-01-03 21:13:10 |          MASTER-IAC | (02h 34m 20.43s , -25d 34m 51.2s) |   C |    60 | 18.1 |        
     790 | 2022-01-03 21:15:52 |          MASTER-IAC | (01h 55m 37.60s , -19d 53m 42.3s) |   C |    60 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB211229B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31379
SUBJECT: GRB 211229B: Fermi GBM observation
DATE:    22/01/03 22:56:35 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

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

"At 22:18:43.10 UT on 29 December 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211229B (trigger 662509128 / 211229930)
which was also detected by the Swift/BAT-GUANO (Raman et al. 2022, GCN 31375),
GECAM (Zhao et al. 2021, GCN 31339), AGILE (Ursi et al. 2021, GCN 31344)
and INTEGRAL/SPI-ACS (#9581). The Fermi GBM Final Real-time Localization (GCN 31336)
is consistent with the GECAM position.

The angle from the Fermi LAT boresight at the GBM trigger time is 59 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 24 s (50-300 keV).
The time-averaged spectrum from T0-15 s to T0+8.6 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.14 +/- 0.05 and
the cutoff energy, parameterized as Epeak, is 565 +/- 110 keV.

The event fluence (10-1000 keV) in this time interval is
(8.8 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.3 s in the 10-1000 keV band
is 12.4 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB220104A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31380
SUBJECT: GRB 220104A: Fermi GBM Final Real-time Localization
DATE:    22/01/04 04:11:29 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:01:02 UT on 4 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220104A (trigger 662961667.603716 / 220104167).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 197.8, Dec = 42.1 (J2000 degrees, equivalent to J2000 13h 11m, 42d 06'), with a statistical uncertainty of 3.1 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/2022/bn220104167/quicklook/glg_skymap_all_bn220104167.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220104167/quicklook/glg_healpix_all_bn220104167.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220104167/quicklook/glg_lc_medres34_bn220104167.gif


GRB_name: GRB220104A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31381
SUBJECT: Fermi GRB 220104A: Global MASTER-Net observations report 
DATE:    22/01/04 05:00:41 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220104A ( Fermi GBM team, GCN 31380) errorbox  581 sec after notice time and 619 sec after trigger time at 2022-01-04 04:11:22 UT, with upper limit up to  18.6 mag. The observations began at zenith distance = 40 deg. The sun  altitude  is -48.4 deg. 

The galactic latitude b = 75 deg., longitude l = 107 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1837544

We obtain a following upper limits.  

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

     680 | 2022-01-04 04:11:22 |          MASTER-IAC | (13h 09m 03.78s , +42d 14m 31.9s) |  P| |   120 | 18.3 |        
     680 | 2022-01-04 04:11:22 |          MASTER-IAC | (13h 10m 16.14s , +42d 07m 48.5s) |  P- |   120 | 17.9 |        
     835 | 2022-01-04 04:13:42 |          MASTER-IAC | (13h 09m 03.68s , +42d 12m 57.0s) |  P| |   150 | 18.5 |        
     835 | 2022-01-04 04:13:42 |          MASTER-IAC | (13h 10m 16.14s , +42d 06m 14.2s) |  P- |   150 | 18.0 |        
    1020 | 2022-01-04 04:16:32 |          MASTER-IAC | (13h 09m 05.78s , +42d 14m 34.3s) |  P| |   180 | 18.6 |        
    1020 | 2022-01-04 04:16:32 |          MASTER-IAC | (13h 10m 18.33s , +42d 07m 51.9s) |  P- |   180 | 18.3 |        
    1219 | 2022-01-04 04:19:52 |          MASTER-IAC | (13h 09m 00.64s , +42d 13m 50.3s) |  P| |   180 | 18.6 |        
    1219 | 2022-01-04 04:19:52 |          MASTER-IAC | (13h 10m 13.28s , +42d 07m 08.1s) |  P- |   180 | 18.3 |        


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


GRB_name: GRB220104A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31382
SUBJECT: GRB 220104Aï¼šGECAM detection
DATE:    22/01/04 08:29:45 GMT
FROM:    Guoying Zhao at IHEP  <gyzhao@ihep.ac.cn>

Z. W. Guo, 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, Y. Q. Zhang, 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 bright burst, GRB 220104A, at 2022-01-04T04:01:02.850 UTC (denoted as T0)ï¼Œ
which was also observed by Fermi/GBM (GCN #31380).

According to the BDS alert data, this burst mainly consists of a broad pulse
with a duration of about 2 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_94968062.png

GECAM-B localized this burst to the following position (J2000): 
ra: 192.9 deg
dec: 37.3 deg
err: 10.1 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_sky_fit_94968062.png

This position is consistent with the Fermi GBM team localization 
(trigger #662961667) 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: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31383
SUBJECT: GRB 220101A: LCO Continued Optical Observations
DATE:    22/01/04 10:40:05 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 220101A (Tohuvavohu, et al., GCN 31347) for a second time with the LCO 1-m Sinistro instrument at the McDonald Observatory, Texas, USA site, on January 4, from 03:14 to 03:35 UT (corresponding to 69.70 to 70.05 hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 2x400s exposures in R and I bands. We detect the source at the UVOT detection coordinates and other optical observations (Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN 31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356;
Perley et al., GCN 31357; de Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko et al., GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCN 31364; Noschese et al., GCN 31366; Mao et al., GCN 31368; Guelbenzu, et al., GCN 31370; Strausbaugh et al., GCN 31371, D'Avanzo et al., 31373) in both bands. The following magnitudes are calculated using the USNO-B.1 catalog as reference:

R=20.95+/-0.21
I=19.09+/-0.25

These magnitudes are not corrected for galactic extinction.

R.S. is funded by NSF AST grant #1831682


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31384
SUBJECT: GRB 220101A: 1.3m DFOT observations
DATE:    22/01/04 12:26:23 GMT
FROM:    Dimple Panchal at ARIES, India  <dimplepanchal96@gmail.com>

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

We carried out the follow-up observations of GRB 220101A (Tohuvavohu, et
al., GCN 31347) using 1.3m Devasthal Fast Optical Telescope (DFOT) at
Devasthal observatory of Aryabhatta Research Institute of observational
sciencES (ARIES), India. The observation was started on  2022-01-01 at
12:45:02 UT. We observed a series of images with an exposure time of 300
seconds in R band covering Swift UVOT position and that provided by other
optical observations (Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN
31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356; Perley et al., GCN
31357; de Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko
et al., GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCN 31364;
Noschese et al., GCN 31366; Mao et al., GCN 31368; Guelbenzu et al., GCN
31370; Strausbaugh et al., GCN 31371). An uncataloged source is clearly
visible at the location of the burst with a magnitude of 18.19+-0.15 in the
R-band at around 7.73 hours after the burst.

Photometry is done based on the USNO-B1.0 catalog. The magnitude is not
corrected for Galactic extinction in the direction of the GRB.


GRB_name: GRB220101A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31385
SUBJECT: GRB 220101A: VLA detection
DATE:    22/01/04 13:43:49 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (Radboud U.) reports on behalf of a larger collaboration:

"We observed GRB 220101A (Tohuvavohu et al., GCN 31347) with the Karl G.
Jansky Very Large Array (VLA) beginning on 2022 January 04 04:00 UT (2.96 d
after the burst). At a mean frequency of 6.0 GHz, we detect a radio source
with a preliminary flux density of ~ 0.2 mJy at the position:

RA (J2000) = 00:05:24.816 +/- 0.005
Dec (J2000) = 31:46:08.37 +/- 0.02

consistent with the X-ray position (Osborne et al., GCN 31349), optical
position (Tohuvavohu et
al., GCN 31347; Hentunen et al., GCN 31356), and mm-band position (Laskar,
GCN 31372). Further observations are planned.

We thank the VLA staff for rapidly executing these observations."


GRB_name: GRB211227A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31386
SUBJECT: GRB 211227A:  Lijiang 2.4m Telescope Optical Observations
DATE:    22/01/04 15:35:42 GMT
FROM:    Liping Xin at NAOC, SVOM  <xlp@nao.cas.cn>

Enwei Liang (GXU), Tingfeng Yi(YNNU), Liping Xin (NAOC), 
Haicheng Feng (YNAO CAS), Houjun Lv (GXU), Xianggao Wang (GXU)
and Youdong Hu (IAA) report:

We observed the field of GRB 211227A (Beardmore et al., GCN #31316)
with the Lijiang 2.4m telescope on January 3, 2022ï¼Œstarting at 18:23:25 UTï¼Œ
about 6.8 day after trigger. The observations were performed in R band 
with a total exposure of 1200 s at airmass of 1.2 and a seeing of ~1.7, 
under good weather conditions.

Within the XRT enhanced errorbox (Goad et al., GCN #31322), we did not
detect any source to a depth of R &gt; 21.5 mag calibrated by nearby 
SDSS DR12 stars (SDSS J084838.92-024405.9ï¼ŒJ084838.22-024355.7ï¼Œ 
J084836.33-024403.8). This is consistent with other non-detections 
reported (Lipunov et al., GCN #31315; Hu et al., GCN #31318; 
Fu et al., GCN #31320; Strausbaugh et al.,GCN #31321; Perley, GCN #31323;
Malesani et al., GCN #31324; Belles et al., GCN #31328, 
Kann et al., GCN #31341,GCN #31376 O'Connor et al.). 

We thank the staff of the Lijiang 2.4m telescope, 
in particular Jiangguo Wang for scheduling of these observations.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31387
SUBJECT: GRB 220101A: iTelescope optical observations
DATE:    22/01/04 19:11:01 GMT
FROM:    Filipp Dmitrievich Romanov at Amateur astronomer  <filipp.romanov.27.04.1997@gmail.com>

I observed the field of GRB 220101A (Tohuvavohu et al., GCN Circ.
31347) using remote telescope T21 (0.43-m f/6.8 reflector + CCD +
f/4.5 focal reducer) of iTelescope.Net in Observatory New Mexico Skies
at Mayhill (New Mexico, USA). Four images (with exposures 300 seconds,
BINx1) were obtained with Ic filter on 2022-01-04 from 01:29:50 to
01:51:05 UTC.

I detected faint (SNR â‰ˆ 3) optical afterglow with UVOT position in
stacked image (mid time = 01:40:27 UTC, that is 2.854 days after the
trigger) and measured its magnitude from comparison to magnitudes of
nearby stars from the SDSS Photometric Catalogue, Release 12 (Alam et
al., 2015), transformed to Ic by Lupton's (2005) formulas.

Measured magnitude (was not corrected for Galactic extinction) = 19.4
+/- 0.4 Ic. Stacked image available here:
https://www.flickr.com/photos/filipp-romanov/51800218870

I also observed the field of GRB 220101A remotely with telescope T18
(0.32-m f/8.0 reflector + CCD) in AstroCamp observatory (Nerpio,
Spain). I did not detect the source (magnitude limit of about 19 R) in
a 300-sec image taken with a red filter, started on 2022-01-02 at
18:40:52 UTC.

F. D. Romanov.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31388
SUBJECT: GRB 220101A: 2.2m CAHA (+CAFOS) first day optical detection
DATE:    22/01/04 23:06:26 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

M. D. Caballero-Garcia, R. Sanchez-Ramirez, Y.-D. Hu, A. J. Castro-Tirado, E. Fernandez-Garcia (IAA-CSIC), G. Bergond and I. Hermelo (CAHA) report:

Following the detection of the bright GRB 220101A by Swift (Tohuvavohu et al., GCNC 31347), Fermi (Arimoto et al., GCNC 31350, Lesage et al., GCNC 31360) and AGILE (Ursi et al., GCNC 31354) we observed the optical afterglow (Kuin & Tohuvavohu, GCNC 31351; Fu et al., GCNC 31353; Hentunen et al., GCNC 31356; Perley, GCNC 31357; de Ugarte Postigo et al., GCNC 31358; Vinko et al., GCNC 31361; Tomasella et al., GCNC 31363; Mao et al., GCNC 31364; Noschese et al., GCNC 31366; Mao et al., GCNC 31368; Nicuesa Guelbenzu et al., GCNC 31370; Strausbaugh et al., GCNC 31371; D'Avanzo et al., GCNC 31373; Strausbaugh et al., GCNC 31383; Dimple et al., GCNC 31384; Romanov, GCNC31387) with the CAFOS instrument, mounted on the 2.2 m telescope, at the Calar Alto Observatory (Almeria, Spain). The observation started at 18:12:07 UT on 1st January 2022 (13.78 hr after the GRB) and consisted of 3 x 60 s, 4 x 60 s and 1 x 300 s exposures in the sdss_i, sdss_r and sdss_g bands. Against comparison stars from SDSS, we measure r=19.75+-0.05 for the GRB 220101A optical afterglow.

We thank the staff at Calar Alto observatory for their excellent support.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31389
SUBJECT: GRB 220101A: 3rd LCO Optical Observation
DATE:    22/01/05 00:16:11 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 220101A (Tohuvavohu, et al., GCN 31347) for a third time with the LCO 1-m Sinistro instrument at the Teide Observatory, Tenerife site, on January 4, from 21:35 to 22:02 UT (corresponding to 88.43 to 88.88 hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 2x500s exposures in R and I bands. We still detect the source at the UVOT detection coordinates and other optical observations (Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN 31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356;
Perley et al., GCN 31357; de Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko et al., GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCN 31364; Noschese et al., GCN 31366; Mao et al., GCN 31368; Guelbenzu, et al., GCN 31370; Strausbaugh et al., GCN 31371, D'Avanzo et al., GCN 31373; Strausbaugh et al., GCN 31383; Dimple et al., GCN 31384; Romanov, GCN 31387; Caballero-Garcia, GCN 31388) in both bands. The following magnitudes are calculated using the USNO-B.1 catalog as reference:

R=21.31+/-0.18
I=20.43+/-0.12

These magnitudes are not corrected for galactic extinction.

R.S. is funded by NSF AST grant #1831682


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31390
SUBJECT: GRB 220101A: Mondy optical observations
DATE:    22/01/05 13:03:41 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI, HSE), A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov 
(HSE)  report  on behalf of GRB IKI FuN:

We observed Swift GRB 220101A (Tohuvavohu, et al., GCN 31347) also 
detected by Fermi/LAT (M. Arimoto et al. 2022, GCN 31350), AGILE (A. 
Ursi et al. 2022, GCN 31354), and Fermi/GBM (Lesage et al. 2022, GCN 
31360)  with AZT-33IK telescope of Sayan observatory (Mondy)  starting 
on 2022-01-04  (UT) 15:16:32.  We detect the optical afterglow 
(Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN 31351; Fu et al., 
GCN 31353; Hentunen et al., GCN 31356; Perley et al., GCN 31357; de 
Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko et al., 
GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCN 31364; Noschese 
et al., GCN 31366; Mao et al., GCN 31368; Guelbenzu, et al., GCN 31370; 
Strausbaugh et al., GCN 31371, D'Avanzo et al., GCN 31373; Strausbaugh 
et al., GCNs 31383, 31389; Dimple et al., GCN 31384; Romanov, GCN 31387; 
Caballero-Garcia, GCN 31388).    Preliminary photometry of the afterglow 
in a stacked image is following

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

2022-01-04 12:36:19   3.33083    R      30*120 21.50 0.12  23.1


The photometry is based on the nearby SDSS-DR12 stars
RA DEC R(Lupton)
00:05:20.64408 +31:45:46.0728 18.562
00:05:34.81464 +31:45:50.5224 15.734
00:05:32.53944 +31:44:51.9396 15.369
00:05:36.69864 +31:44:42.4176 14.677

We searched for the nearest galaxy in catalogs. The nearest galaxy was 
found in Legacy Survey 1.5 arcsec apart  from afterglow UVOT position 
with r=23.98, z=21.33 and not detected in g-filter (Brick: 0013p317, 
Objid: 4276). The galaxy is not presented in SDSS and PS1 catalogs. This 
red galaxy might be a host galaxy of GRB 220101A, in this case the 
distance from the source to the center of the galaxy will be about 10 
kpc at redshift z = 4.618 (Fu et al., GCN 31353; Fynbo et al., GCN 
31359; Tomasella et al., GCN 31363).


GRB_name: GRB220104A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31392
SUBJECT: GRB 220104A: Fermi GBM Observation
DATE:    22/01/05 20:14:11 GMT
FROM:    Boyan A. Hristov at UAH  <bah0046@uah.edu>

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

"At 04:01:02.60 UT on 04 January 2022, the Fermi Gamma-Ray
Burst Monitor (GBM) triggered and located GRB 220104A
(trigger 662961667 / 220104167) which was also detected by
GECAM (Z. W. Guo et al. 2022, GCN 31382).

The GBM on-ground location (GCN 31380) is consistent with the
GECAM position.

The GBM light curve consists of multiple peaks with a duration
(T90) of about 2.624 s (50-300 keV).  The time-averaged
spectrum from T0-0.128 s to T0+0.320 s is best fit by a simple
power law function with index -1.28 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(3.5 +/- 0.34)E-07 erg/cm^2.
The 64-miliseconds peak photon flux measured starting from
T0-0.064 s in the 10-1000 keV band
is 4.00 +/- 0.98 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: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31394
SUBJECT: GRB 220101A: continued 1.3m DFOT Optical Observations
DATE:    22/01/06 07:39:50 GMT
FROM:    Rahul Gupta at ARIES, India  <rahulbhu.c157@gmail.com>

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

We further observed the bright GRB 220101A (Tohuvavohu, et al., GCN 31347)
with 1.3m Devasthal Fast Optical Telescope (DFOT) located at Devasthal
observatory of Aryabhatta Research Institute of Observational Sciences
(ARIES), India. The observation was started on  2022-01-02 at 13:39:49 UT.
We obtained a series of images with an exposure time of 300 seconds in R,
and I filters, respectively.  We clearly detected the optical afterglow of
GRB 220101A (Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN 31351; Fu
et al., GCN 31353; Hentunen et al., GCN 31356; Perley, GCN 31357; de Ugarte
Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko et al., GCN
31361; Tomasella et al., GCN 31363; Mao et al., GCNs 31364, 31368; Noschese
et al., GCN 31366; Guelbenzu et al., GCN 31370; Strausbaugh et al., GCNs
31371, 31383, 31389; Dimple et al., GCN 31384; Romanov, GCN 31387;
Caballero-Garcia
et al., GCN 31388; and Belkin et al., GCN 31390) in our individual images
of both the filters. We report the preliminary brightness of the afterglow
to be R = 19.46 +/- 0.06 mag ~ 32.50 hours post burst.

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: GRB220101A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31395
SUBJECT: GRB 220101A: further TNG NIR observations
DATE:    22/01/06 12:52:54 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. D'Avanzo (INAF-OAB), A. Melandri (INAF-OAB), D. Fugazza (INAF-OAB), S. Campana (INAF-OAB), D. B. Malesani (Radboud Univ. and DAWN/NBI), 
V. D'Elia (ASI-SSDC), M. De Pasquale (Univ. Messina), E. Palazzi (INAF-OAS), S. Piranomonte (INAF-OAR), A. Rossi (INAF-OAS), G. Tagliaferri (INAF-OAB); 
V. Lorenzi, D. Carosati (INAF-TNG), Paolo Giacobbe (INAF-OATO) on behalf of the CIBO collaboration report:

We observed the field of GRB 220101A (Tohuvavohu et al., GCN Circ. 31347; Arimoto et al., GCN Circ. 31350; Ursi et al., GCN Circ. 31354; 
Lesage & Meegan, GCN Circ. 31360) with the Italian 3.6m TNG telescope equipped with the near-infrared camera NICS. A series of images 
were obtained with the J and K filters on 2022-01-05 from 19:31:36 UT to 20:55:35 UT (i.e. at a mid time of about 4.63 days after the burst). 

The NIR  afterglow (Dâ€™Avanzo et al., GCN Circ. 31373) is clearly detected in all bands. From preliminary photometry we derive the following magnitude:

J = 19.71 +/- 0.10

(Vega; calibrated against the 2MASS catalogue).


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31398
SUBJECT: GRB 220101A: Continued Mondy optical observations
DATE:    22/01/07 12:25:31 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (HSE), A. Pozanenko (IKI), E. Klunko (ISTP), Belkin (IKI, HSE)
report  on behalf of GRB IKI FuN:

We observed Swift GRB 220101A (Tohuvavohu, et al., GCN 31347) also
detected by Fermi/LAT (Arimoto et al. 2022, GCN 31350), AGILE (Ursi et 
al. 2022, GCN 31354), and Fermi/GBM (Lesage et al. 2022, GCN 31360) with 
AZT-33IK telescope of Sayan observatory (Mondy) starting on 2022-01-06 
(UT) 13:57:13. We detected the afterglow (Tohuvavohu et al., GCN 31347; 
Kuin & Tohuvavohu, GCN 31351; Fu et al., GCN 31353; Hentunen et al., GCN 
31356; Perley et al., GCN 31357; de Ugarte Postigo et al., GCN 31358; 
Fynbo et al., GCN 31359; Vinko et al., GCN 31361; Tomasella et al., GCN 
31363; Mao et al., GCN 31364; Noschese et al., GCN 31366; Mao et al., 
GCN 31368; Guelbenzu, et al., GCN 31370; Strausbaugh et al., GCN 31371, 
D'Avanzo et al., GCN 31373; Strausbaugh et al., GCNs 31383, 31389; 
Dimple et al., GCN 31384; Romanov, GCN 31387; Caballero-Garcia, GCN 
31388; Belkin et al, GCN 31390; Gupta et al, GCN 31394; D'Avanzo et al, 
GCN 31395) in  a stacked image.

Preliminary photometry of the afterglow is following

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

2022-01-06 13:57:13   5.38683    R    30*120 22.17 0.18  23.0

The photometry is based on the nearby SDSS-DR12 stars
RA DEC R(Lupton)
00:05:20.64408 +31:45:46.0728 18.562
00:05:34.81464 +31:45:50.5224 15.734
00:05:32.53944 +31:44:51.9396 15.369
00:05:36.69864 +31:44:42.4176 14.677


GRB_name: GRB220107A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31399
SUBJECT: GRB 220107A: Fermi GBM Final Real-time Localization
DATE:    22/01/07 14:55:38 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 14:45:31 UT on 7 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220107A (trigger 663259536.927164 / 220107615).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 168.2, Dec = 35.0 (J2000 degrees, equivalent to J2000 11h 12m, 35d 00'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 77.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220107615/quicklook/glg_skymap_all_bn220107615.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220107615/quicklook/glg_healpix_all_bn220107615.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220107615/quicklook/glg_lc_medres34_bn220107615.gif


GRB_name: GRB220107A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31400
SUBJECT: GRB 220107A: BALROG localization (Fermi Trigger 663259536 / GRB 220107615)
DATE:    22/01/07 15:05:36 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
663259536 at 14:45:31 on 07 Jan. 2022 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) = 168.5+/-1.4 deg
Decl.(2000.0) = 34.9+/-1.0 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB220107615/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB220107615/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB220107615/json

                        


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31401
SUBJECT: GRB 220101A: Tautenburg observations
DATE:    22/01/07 18:12:34 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

A. Nicuesa Guelbenzu, S. Melnikov, S. Klose, B. Stecklum, F. Ludwig (all 
TLS Tautenburg) report:

We continued observing the field of GRB 220101A (Tohuvavohu et al., GCN 
31347) with the Tautenburg 1.34m Schmidt telescope equipped with the 
TAUKAM 6kx6k CCD camera (Stecklum et al. 2021; arXiv:2101.12554).

For the optical transient (discovered by Swift/UVOT: Tohuvavohu et al., 
GCN 31347; Kuin et al., GCN 31351) we measure the following AB magnitudes:

g > 22.9  (3 sigma), January 6, 20:23 UT (midtime),
r = 22.54 +/- 0.24,  January 6, 19:32 UT (midtime),
i = 21.27 +/- 0.10,  January 6, 18:44 UT (midtime),
z = 21.17 +/- 0.22,  January 6, 18:26 UT (midtime),

calibrated against the SDSS catalogue.


GRB_name: GRB220107A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31402
SUBJECT: GRB 220107A: Swift/BAT-GUANO arcminute localization
DATE:    22/01/07 20:07:49 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 localize GRB 220107A onboard (T0:
2022-01-07T14:45:31 UTC, Fermi/GBM GCN 31399), due to a slew.

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 burst is detected in BAT, on the approach to SAA and during a slew.
The location was found in a mosaiced slew image with an SNR ~9.

The BAT position is
RA, Dec = 169.761, 34.139 deg which is
   RA(J2000)  = 11h 19m 02.58s
   Dec(J2000) =  34d 08â€² 19.26â€³
with an estimated uncertainty of 10 arcmin.

The position is consistent with the Fermi/GBM RoboBA (GCN 31399) and
BALROG (GCN 31400) localizations.

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: GRB220107A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31403
SUBJECT: Fermi GRB 220107A: Global MASTER-Net observations report 
DATE:    22/01/07 20:15:25 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220107A ( Fermi GBM team, GCN 31399) errorbox  14945 sec after notice time and 14974 sec after trigger time at 2022-01-07 18:55:06 UT, with upper limit up to  18.6 mag. The observations began at zenith distance = 73 deg. The sun  altitude  is -48.3 deg. 

The galactic latitude b = 68 deg., longitude l = 187 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1841973

We obtain a following upper limits.  

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

   15004 | 2022-01-07 18:55:06 |      MASTER-Tavrida | (11h 04m 15.78s , +35d 40m 05.4s) |   C |    60 | 13.2 |        
   15163 | 2022-01-07 18:57:45 |      MASTER-Tavrida | (11h 07m 37.93s , +33d 44m 04.2s) |   C |    60 | 12.8 |        
   15243 | 2022-01-07 18:59:04 |      MASTER-Tavrida | (11h 17m 11.22s , +33d 45m 44.4s) |   C |    60 | 13.6 |        
   18102 | 2022-01-07 19:46:44 |      MASTER-Tavrida | (11h 11m 38.28s , +37d 34m 23.5s) |   C |    60 | 18.0 |        
   18182 | 2022-01-07 19:48:03 |      MASTER-Tavrida | (11h 04m 13.64s , +35d 40m 14.4s) |   C |    60 | 17.5 |        
   18261 | 2022-01-07 19:49:23 |      MASTER-Tavrida | (11h 14m 10.15s , +35d 39m 14.1s) |   C |    60 | 18.0 |        
   18341 | 2022-01-07 19:50:42 |      MASTER-Tavrida | (11h 07m 30.05s , +33d 44m 06.6s) |   C |    60 | 18.2 |        
   18421 | 2022-01-07 19:52:02 |      MASTER-Tavrida | (11h 17m 13.08s , +33d 44m 18.7s) |   C |    60 | 16.7 |        
   18581 | 2022-01-07 19:54:42 |      MASTER-Tavrida | (11h 23m 01.66s , +35d 39m 47.5s) |   C |    60 | 13.3 |        
   19251 | 2022-01-07 20:05:52 |      MASTER-Tavrida | (11h 11m 42.85s , +37d 33m 19.8s) |   C |    60 | 18.6 |        
   19330 | 2022-01-07 20:07:11 |      MASTER-Tavrida | (11h 04m 17.45s , +35d 38m 35.9s) |   C |    60 | 17.6 |        
   19409 | 2022-01-07 20:08:31 |      MASTER-Tavrida | (11h 14m 05.38s , +35d 40m 09.3s) |   C |    60 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220107A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31404
SUBJECT: GRB 220107A: Swift ToO observations
DATE:    22/01/07 22:10:20 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 220107A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021476

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: GRB220107A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31406
SUBJECT: GRB 220107A: Fermi GBM observations
DATE:    22/01/08 03:49:49 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

"At 14:45:31.93 UT on 7 January 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220107A (trigger 663259536 / 220107615),
which was also detected by the Swift/BAT-GUANO (DeLaunay et al., GCN 31402).

The Fermi GBM Final Real-time Localization (GCN 31399) is consistent
with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 78 degrees.

The GBM light curve shows multiple peaks
with a duration (T90) of about 33 s (50-300 keV).
The time-averaged spectrum from T0-0.3 s to T0+36.6 s is
best fit by a Band function with Epeak = 168 +/- 11 keV,
alpha = -0.55 +/- 0.06, and beta = -1.94 +/- 0.06.

The event fluence (10-1000 keV) in this time interval is
(2.24 +/- 0.05)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0 + 10.2 s in the 10-1000 keV band
is 13.9 +/- 0.3 ph/s/cm^2.


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

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


GRB_name: GRB220107B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31407
SUBJECT: GRB 220107B: Tiled Swift observations
DATE:    22/01/08 04:36:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 220107B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00103

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

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

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


GRB_name: GRB220107A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31408
SUBJECT: GRB 220107A: AstroSat CZTI detection
DATE:    22/01/08 05:33:42 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

A. Suresh (IITB), G. Waratkar (IITB), V. Prasad (IUCAA), 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 220107A, which was
also detected by Fermi-GBM (GCN 31399, 31406), and Swift/BAT-GUANO
(Tohuvavohu et al., GCN 31402) with BALROG localization (Greiner et al.
GCN 31400).

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
2022-01-07 14:46:59.50 UT. The measured peak count rate associated with
the burst is 382 (+36 -38) cts/s above the background in the combined
data of four quadrants, with a total of 4724 (+364 -472) cts. The local
mean background count rate was 149 (+1 -1) cts/s. Using cumulative
rates, we measure a T90 of 97 (+4 -5) 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 2022-01-07 14:46:57.70 UT. The
measured peak count rate is 1451 (+86 -94) cts/s above the background in
the combined Veto data of four quadrants, with a total of 13589 (+1062
-1220) cts. The local mean background count rate was 1500 (+4 -4) cts/s.
We measure a T90 of 87 (+2 -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: GRB220107B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31409
SUBJECT: GRB 220107B: Fermi-LAT detection
DATE:    22/01/08 06:05:07 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

M. Arimoto (Kanazawa Univ.), N. Di Lalla (Stanford Univ.), M. Axelsson (KTH & Stockholm Univ.) and S. Cutini (INFN Perugia) report on behalf of the Fermi-LAT Collaboration:

On January 7th, 2022, Fermi-LAT detected high-energy emission from GRB 220107B, which was also detected by Fermi-GBM  (trigger 663274898/220107793).

The best LAT on-ground location is found to be

RA, Dec = 216.5, 20.0 (degrees, J2000)

with an error radius of 0.22 deg (90% containment, statistical error only).
This was 54 deg from the LAT boresight at the time of the GBM trigger:

T0 =  19:01:33.52 UT.

The data from the Fermi-LAT show a significant increase in the event rate after the GBM trigger that is temproally and spatially correlated with the GBM emission (2.3 degrees from the GBM location) with high significance. The photon flux above 100 MeV in the time interval 0-500s after the GBM trigger is 1.4E-5 +/- 2.4E-6 ph/cm2/s.

The estimated photon index above 100 MeV is -2.14 +/- 0.17.

The highest-energy photon is a 2.4 GeV event which is observed ~8 seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Sara Cutini (sara.cutini@pg.infn.it).

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


GRB_name: GRB220107A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31410
SUBJECT: GRB 220107A: Swift-XRT afterglow detection
DATE:    22/01/08 06:39:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 220107A (DeLaunay et al. GCN Circ.
31402), collecting 699 s of Photon Counting (PC) mode data between
T0+26.7 ks and T0+27.4 ks. 

An uncatalogued X-ray source is detected and is above the RASS 3-sigma
upper limit at this position, and is therefore likely the GRB
afterglow. Using 698 s of PC mode data and 1 UVOT image, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 169.80648, +34.17014
which is equivalent to:

RA (J2000): 11h 19m 13.55s
Dec(J2000): +34d 10' 12.5"

with an uncertainty of 2.3 arcsec (radius, 90% confidence). This
position is 3.0 arcmin from the Swift/BAT-GUANO position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.5 (+0.5, -2.4).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.84 (+0.27, -0.18). The
best-fitting absorption column is  3.1 (+6.1, -0.9) x 10^20 cm^-2,
consistent with the Galactic value of 2.2 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.5 x 10^-11 (3.7 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+6.1, -0.9) x 10^20 cm^-2
Galactic foreground: 2.2 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.84 (+0.27, -0.18)

If the light curve continues to decay with a power-law decay index of
2.5, the count rate at T+24 hours will be 0.054 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-12 (2.0 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/00021476.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021476.

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


GRB_name: GRB220107B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31411
SUBJECT: GRB 220107B: Swift-XRT afterglow detection
DATE:    22/01/08 09:33:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 220107B (Arimoto et al. GCN Circ. 31409)
in a series of observations tiled on the sky. The total exposure time
is 1.3 ks, distributed over 2 tiles; the maximum exposure at a single
sky location was 1.0 ks. The data were collected between T0+35.7 ks and
T0+36.2 ks, and are entirely in Photon Counting (PC) mode. 

An uncatalogued X-ray source is detected and is above the RASS 3-sigma
upper limit at this position, and is therefore likely the GRB
afterglow. Using 546 s of PC mode data and 1 UVOT image, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 216.40652, +20.17064
which is equivalent to:

RA (J2000): 14h 25m 37.56s
Dec(J2000): +20d 10' 14.3"

with an uncertainty of 3.4 arcsec (radius, 90% confidence). This
position is 11.5 arcmin from the Fermi/LAT position.  The source has a
mean count rate of 1.3e-01 ct/sec; while we cannot determine at the
present time whether it is fading, the fact that the source is well
above RASS limit strongly suggests it is the X-ray afterglow of GRB
220107B. More data are currently being collected.

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/xrt_products/TILED_GRB00103/Source1.php.

The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00103.

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


GRB_name: GRB220107B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31412
SUBJECT: GRB 220107B: AstroSat CZTI detection
DATE:    22/01/08 13:20:02 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

 A. Suresh (IITB), 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 220107B, which was
also detected by Fermi-GBM (trigger 663274898/220107793), Fermi-LAT
(Axelsson et al., GCN 31409) and Swift-XRT (Gropp et al., GCN 31411). 

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
2022-01-07 19:01:45.50 UT. Quadrant B was noisy, and we exclude it from
further analysis. The measured peak count rate associated with the burst
is 372 (+44 -42) cts/s above the background in the combined data of
three quadrants (out of four), with a total of 2558 (+225 -239) cts. The
local mean background count rate was 382 (+2 -2) cts/s. Using cumulative
rates, we measure a T90 of 19 (+3 -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 2022-01-07 19:01:35.775 UT. The
measured peak count rate is 826 (+81 -85) cts/s above the background in
the combined Veto data of four quadrants, with a total of 5424 (+496
-555) cts. The local mean background count rate was 1721 (+4 -5) cts/s.
We measure a T90 of 22 (+2 -3) 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: GRB220107A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31413
SUBJECT: GRB 220107A: MITSuME Akeno optical observation
DATE:    22/01/08 14:40:52 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

R. Hosokawa, Y. Imai, M. Niwano, K. L. Murata, N. Ito, Y. Takamatsu,
M. Takaku, 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 220107A (The Fermi GBM team et al. GCN
Circular #31399, F. Kunzweiler et al. GCN Circular #31400, James
DeLaunay et al. GCN Circular #31402, V. Lipunov et al. GCN Circular
#31403, P. A. Evans et al. GCN Circular #31404, P. Veres et al. GCN
Circular #31406, A. Suresh et al. GCN Circular #31408, D.N. Burrows et
al. GCN Circular #31410) 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
2022-01-07 20:21:55 UT (~5.6 hours after the Fermi GBM trigger). We
stacked the images with good conditions.

Our observation covered 100% of the Swift/BAT-GUANO error region
(James DeLaunay et al. GCN Circular #31402). Comparing our co-added
images with the GSC2.3 and PS1 catalog, we marginally detected one
uncatalogued source at RA, Dec = (169.80774, 34.17079), which is
equivalent to:
RA (J2000): 11h19m13.859s
Dec(J2000): +34d 10' 14.845"
This position is 4.4 arcsec from the center of Swift XRT position
(D.N. Burrows et al. GCN Circular #31410).
The magnitudes of the source are as follows.

T0+[hour] | MID-UT | T-EXP[sec] | candidate magnitude | 5-sigma limits
------------------------------------------------------------------------------------------------
5.4 | 2022-01-07 20:55:27 | 1620 | g'=19.8 +/- 0.5, Rc=18.9 +/- 0.2,
Ic=18.3 +/- 0.2 | g'>20.9, Rc>21.0, Ic>20.3
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time

We used 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: GRB220107B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31414
SUBJECT: GRB 220107B: Fermi GBM observations
DATE:    22/01/08 15:59:52 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

"At 19:01:33.52 UT on 7 January 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220107B (trigger 663274898 / 220107793),
which was also detected by the Fermi LAT (Arimoto et al., GCN 31409).
The GBM on-ground location is consistent with the LAT position.

The GBM light curve consists of multiple separated pulses
with a duration (T90) of about 25 s (50-300 keV).
The time-averaged spectrum from T0-1.7 s to T0+27 s is
best fit by a Band function with Epeak = 391 +/- 21 keV,
alpha = -0.86 +/- 0.03, and beta = -2.40 +/- 0.16.

The event fluence (10-1000 keV) in this time interval is
(2.68 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+12.0 s in the 10-1000 keV band
is 14.4 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB220107A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31415
SUBJECT: GRB 220107A: Swift/UVOT Detection
DATE:    22/01/09 00:24:42 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) reports on behalf of the Swift UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220107A 26.7 ks after
the Fermi detection (GCN Circ. 31399). An uncatalogued fading source consistent with 
the GUANO localization (DeLaunay et al., GCN Circ. 31402) and the XRT position
(Burrows et al., GCN Circ. 31410) is detected in the initial UVOT exposures.
This appears consistent with the optical transient reported by Hosokawa et al.
(GCN Circ. 31413).

The preliminary UVOT position is:
    RA  (J2000) =  11:19:13.71 =  169.80713 (deg.)
    Dec (J2000) = +34:10:14.5  =  34.17070 (deg.)
with an estimated uncertainty of 0.4 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(ks)  T_stop(ks)      Exp(s)           Mag

white             26.7         28.5         1834         20.16 +/- 0.08
white             32.4         33.0         2708         20.35 +/- 0.07
white             37.6         39.4          247         20.43 +/- 0.24

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.056 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31416
SUBJECT: GRB 220107A: Nanshan/NEXT optical observations
DATE:    22/01/09 03:07:24 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu (NAOC,HUST), S.Q. Jiang, 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 220107A detected by Fermi (the Fermi/GBM 
team, GCN Circ. 31399, Kunzweiler et al. GCN Circ. 31400) and Swift 
(DeLaunay et al. GCN Circ. 31402), using the NEXT-0.6m telescope located 
at Nanshan, Xinjiang, China. Observations started at 19:46:36 UT on 
2022-01-08 (i.e., 29.46 hrs after the Fermi GBM trigger), and 10x300 s 
frames were obtained in the Sloan r-filter.

The previously reported optical afterglow (Hosokawa et al. GCN Circ. 
31413, Siegel et al. GCN Circ. 31415) is clearly detected in our stacked 
image, and has decayed to r = 20.22 +/- 0.05, calibrated by nearby SDSS 
stars.


GRB_name: GRB220107B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31417
SUBJECT: GRB 220107B: Nanshan/NEXT optical upper limits and host galaxy candidate
DATE:    22/01/09 04:04:47 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 220107B detected by Fermi (Arimoto et al., 
GCN 31409; Veres & Meegan, GCN 31414) and AstroSat (Suresh et al., GCN 
31412), using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. We obtained 6x300 s frames in the Sloan r-band and 5x300 s frames 
in Sloan z-band, starting at 21:30:31 UT on 2022-01-08.

No optical source is detected in our stacked images at the Swift-XRT 
position (Gropp et al., GCN 31411). Preliminary photometric results are 
as follows:

Tmid-T0 (hr)  Filter   Upper Limit(5-sigma)
    26.97           r          >21.3
    27.44           z          >19.3

calibrated with the nearby PanSTARRS field.

In addition, from Legacy Survey there exists a faint source at the 
border of the Swift-XRT error circle at coordinates R.A. (J2000) = 
14:25:37.66 and Dec. (J2000) = +20:10:17.01, and magnitudes of g ~ 
24.62, r ~ 24.51, z ~ 23.32 as well as a photo_redshift = 1.13 +/- 0.23. 
The source is not present in SDSS and PanSTARR, and might be the host of 
the burst.


GRB_name: GRB220107B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31418
SUBJECT: GRB 220107B: MITSuME Akeno optical upper limits
DATE:    22/01/09 09:54:23 GMT
FROM:    Masafumi Niwano at Tokyo Institute of Tech  <niwano@hp.phys.titech.ac.jp>

M. Niwano, R. Hosokawa, Y. Imai, K. L. Murata, 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 220107B (M. Arimoto et al. GCN Circular 
#31409, P. A. Evans et al. #31407, J. D. Gropp et al. #31411,  A. Suresh 
et al. #31412, P. Veres and C. Meegan #31414, S.Q. Jiang et al. #31417) 
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 2022-01-08 17:04:13 UT (22 hours after Fermi 
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 #31411). We obtained the 5-sigma limits of the stacked 
images as follows.

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

22.0 2022-01-08 18:58:13 11820 g'>20.7, Rc>20.9, Ic>20.1
------------------------------------------------------------------------------------------------ 

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: GRB220107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31419
SUBJECT: GRB 220107A: AbAO and Terskol optical observations
DATE:    22/01/09 12:27:19 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (IKI), S. Belkin (IKI), A. Pozanenko (IKI), R. Ya. Inasaridze 
(AbAO), V. Agletdinov (KIAM), V. R. Ayvazian (AbAO),  D. Datashvili 
(AbAO), G. V. Kapanadze (AbAO) report on behalf of GRB IKI FuN:

We observed the field of GRB 220107A till now detected by GBM/Fermi (the 
Fermi/GBM team, GCN  1399; Kunzweiler et al. GCN  31400) and Swift
(DeLaunay et al. GCN  31402) with AS-32 telescope of Abastumani 
observatory (AbAO) and K-800 telescope of Mnt. Terskol observatory. The 
optical afterglow (Hosokawa et al. GCN 31413; Siegel et al. GCN 31415; 
Zhu et al. GCN 31416) is detected in stacked images. Preliminary 
photometry of the afterglow is following.

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

2022-01-08 23:38:28 1.38573 R     42*60   20.26 0.14 21.4 AS-32
2022-01-09 01:58:01 1.48613 Clear 108*30  20.24 0.14 22.0 K-800

Photometry is based on the SDSS-DR12 nearby stars
RA DEC R(Lupton transformations)
11:19:03.5786 +34:06:35.141 17.75
11:19:08.2856 +34:14:46.786 16.73
11:18:58.9570 +34:17:07.910 17.46

We note a presence of a galaxy 8.7 arcsec West presented as 
J111913.15+341014.4 in SDSS DR12 with r =19.623, i = 19.126 at 
photometric redshift of z_ph = 0.34 +/- 0.066. Despite the galaxy is 
unlikely to be the host galaxy of GRB 220107A, it might affect 
photometry of the afterglow in a crude plate scale images.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31420
SUBJECT: GRB 220101A: SAO RAS optical observations
DATE:    22/01/09 14:22:05 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. S. Moskvitin (SAO), N. Pankov (HSE, IKI),  A. S. Medvedev (SAO), S. 
Belkin (IKI), A. Pozanenko (IKI)  report on behalf of GRB IKI FuN:

We observed Swift GRB 220101A (Tohuvavohu, et al., GCN 31347) also
detected by Fermi/LAT (Arimoto et al. 2022, GCN 31350), AGILE (Ursi et
al. 2022, GCN 31354), and Fermi/GBM (Lesage et al. 2022, GCN 31360) with 
Zeiss-1000 telescope of SAO RAS in Rc-filter starting on 2022-01-08 (UT) 
15:40:16.

We detected the afterglow (Tohuvavohu et al., GCN 31347; Kuin & 
Tohuvavohu, GCN 31351; Fu et al., GCN 31353; Hentunen et al., GCN
31356; Perley et al., GCN 31357; de Ugarte Postigo et al., GCN 31358;
Fynbo et al., GCN 31359; Vinko et al., GCN 31361; Tomasella et al., GCN
31363; Mao et al., GCN 31364; Noschese et al., GCN 31366; Mao et al., 
GCN 31368; Guelbenzu, et al., GCNs 31370, 31401; Strausbaugh et al., GCN 
31371; D'Avanzo et al., GCN 31373; Strausbaugh et al., GCNs 31383, 
31389; Dimple et al., GCN 31384; Romanov, GCN 31387; Caballero-Garcia, 
GCN 31388; Belkin et al., GCNs 31390, 31398; Gupta et al., GCN 31394; 
D'Avanzo et al., GCN 31395) in  a stacked image.

Preliminary photometry of the afterglow is following

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

2022-01-08 15:40:16   7.46534   Rc   16*300  22.8 0.3   23.2


The photometry is based on the nearby SDSS-DR12 stars
RA DEC R(Lupton transformations)
00:05:20.64408 +31:45:46.0728 18.562
00:05:34.81464 +31:45:50.5224 15.734
00:05:32.53944 +31:44:51.9396 15.369
00:05:36.69864 +31:44:42.4176 14.677


GRB_name: GRB220108A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31421
SUBJECT: GRB 220108A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/01/09 15:55:52 GMT
FROM:    James DeLaunay at PSU  <jjd330@psu.edu>

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

Swift/BAT did not localize GRB 220108A (T0: 2022-01-08T23:05:29.05 UTC,
INTEGRAL/SPI-ACS #9600).

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), detects the burst with a sqrt(TS) of 9.6 in a 0.256 s
analysis time bin.
Estimated T90 in the detector is 0.30 +/- 0.05 s (15-350 keV).

NITRATES results are consistent with a burst coming from outside the coded
FOV, with DeltaLLHOut of 6.8.

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: GRB220107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31422
SUBJECT: GRB 220107A: SAO RAS optical observations
DATE:    22/01/09 20:00:03 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO), A. Medvedev (SAO), A. Pozanenko (IKI)
and N. Pankov (HSE) on behalf of larger GRB follow-up team report:

We observed the field of GRB 220107A (The Fermi GBM team, GCN 31399;
Kunzweiler et al. GCN 31400; DeLaunay et al. GCN 31402; Suresh et al.,
GCN 31408) with the SAO RAS 1-m telescope Zeiss-1000 + CCD-photometer
in BVRc bands on January 9.

The OT (Hosokawa et al. GCN 31413; Siegel GCN 31415; Zhu et al.
GCN 31416; Pankov et al., GCN 31419) is detected in stacked images
in each filter. Preliminary photometry of the afterglow is as follows.

UT start -- UT end    T_mid-T0, d  Filter Exp., s  mag +/- err

02:19:16 -- 03:00:13  1.4960       Rc     5 x 300  20.41 +/- 0.03
03:01:27 -- 03:18:33  1.5170       V      3 x 300  20.97 +/- 0.06
03:19:40 -- 03:36:26  1.5295       B      3 x 300  22.08 +/- 0.18

Photometry is based on nearby SDSS-DR12 stars
(magnitudes are converted with the Lupton 2005 transformations).

J2000 coordinates       B        V        R
11:19:13.93 +34:08:38.8   16.244   15.691   15.363
11:19:13.74 +34:11:49.6   18.811   17.880   17.327
11:19:12.27 +34:11:18.1   18.959   18.506   18.241


GRB_name: GRB220107A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31423
SUBJECT: GRB 220107A: 6m BTA spectroscopic redshift
DATE:    22/01/09 20:07:17 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

A. J. Castro-Tirado (IAA-CSIC), A. F. Valeev, A. Vinokurov and N. 
Burenkov (SAO-RAS), Y.-D. Hu, M.D. Caballero-Garcia, R. Sanchez-Ramirez 
and T-R. Sun (IAA-CSIC), on behalf of a larger collaboration, report:

Following the detection of GRB 220107A by Fermi/GRB (Fermi team GCNC 
31399), Swift/BAT (DeLaunay et al. GCNC 31402) and AstroSat/CZTI (Suresh 
et al. GCNC 31408), three spectra (600 s each, covering the 3700-8500 A 
spectral range) of the optical afterglow (Hosokawa et al. GCNC 31413, 
Siegel et al. GCNC 31415, Zhu et al. GCNC 31416, Pankov et al. GCNC 
31419, Moskvitin et al. GCNC 31422) were obtained by the 6m BTA 
(+SCORPIO-II) at the Special Astrophysical Observatory in Zelenchuk, 
Russia, on Jan 8, 23:25 UT (mid-exposure time, 1.36 days postburst). 
Several absorption lines (Fe II, Fe III, Mn II, Ni II and the Mg II 
doublet) are clearly identified, all consistent with a redshift z = 
1.246, which we propose to be the GRB redshift. We also confirm a 
redshift z = 0.309 Â± 0.001 for the unrelated foreground galaxy reported 
by Pankov et al. (GCNC 31419), in agreement with the photometric redshift.

We acknowledge the excellent support of the BTA technical staff.


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31425
SUBJECT: GRB 220101A: Additional Liverpool telescope photometry
DATE:    22/01/09 20:17:08 GMT
FROM:    Daniel Perley at Liverpool JMU  <d.a.perley@ljmu.ac.uk>

D. A. Perley (LJMU) reports:

We acquired additional multicolor imaging of the optical afterglow of 
GRB 220101A (Tohuvavohu et al., GCN 31347) using the IO:O camera of the 
2m robotic Liverpool Telescope, on the nights (UT) of 2022-01-02, 
2022-01-03, 2022-01-04, 2022-01-05, and 2022-01-07.

Photometry with reference to SDSS secondary standard stars in
the field gives the following magnitudes:

dt(d)   filter mag   unc
1.5924 r    21.17 0.06
1.5958 i    19.70 0.04
1.5991 z    19.48 0.05
2.7070 z    19.97 0.12
2.7120 i    20.39 0.08
2.7154 r    21.58 0.17
3.6932 z    20.61 0.12
3.6983 r    22.31 0.17
3.7032 i    20.89 0.09
4.5961 z    20.63 0.11
4.6011 i    21.25 0.11
4.6045 r    23.13 0.34
6.7021 i    21.34 0.19

Magnitudes are given in the SDSS system and uncorrected for extinction.
Times are referenced to the BAT trigger time.





DisclaimerNone


GRB_name: GRB220107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31426
SUBJECT: GRB 220107A: further SAO RAS optical observations
DATE:    22/01/09 23:40:53 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO) and A. Medvedev (SAO),
on behalf of larger GRB follow-up team report:

We observed the field of GRB 220107A (The Fermi GBM team, GCN 31399;
Kunzweiler et al. GCN 31400; DeLaunay et al. GCN 31402; Suresh et al.,
GCN 31408) with the SAO RAS 1-m telescope Zeiss-1000 + CCD-photometer.
6 x 300 sec. images were obtained in Rc band on January 9,
22:27:09 -- 23:10:20 UT (T_mid - T0 = 2.3356 days).

The OT (Hosokawa et al. GCN 31413; Siegel GCN 31415; Zhu et al.
GCN 31416; Pankov et al., GCN 31419; Moskvitin et al., GCN 31422;
Castro-Tirado et al., GCN 31423) is clearly visible in the stacked
frame. Preliminary photometry of the afterglow is R = 21.01 +/- 0.04
(based on nearby SDSS-DR12 stars mentioned in GCN 31422).


GRB_name: GRB220107B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31427
SUBJECT: Confirmation of the X-ray afterglow of GRB 220107B
DATE:    22/01/10 14:39:41 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

Swift-XRT has performed a second follow-up observation of the
Fermi/LAT-detected GRB 220107B (Arimoto et al., GCN 31409), ~184 ks after
the trigger. The source suggested to be the X-ray counterpart in GCN 31411
(Gropp et al.) has clearly faded, with a power-law slope of alpha = 1.54
(+0.32, -0.24), and is therefore confirmed as the X-ray afterglow.

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


GRB_name: GRB220107A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31429
SUBJECT: Konus-Wind detection of GRB 220107A
DATE:    22/01/10 19:41:10 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 220107A
(Fermi/GBM trigger #663259536: Fermi GBM Team, GCN 31399;
Kunzweiler et al., GCN 31400; Veres and Meegan, GCN 31406;
Swift/BAT-GUANO localization: DeLaunay et al., GCN 31402;
AstroSat CZTI detection: Suresh et al., GCN 31408)
triggered Konus-Wind at T0=53142.427 s UT (14:45:42.427).

The burst light curve shows a multipeaked structure
started at ~T0-7.6 s with a total duration of ~110.8 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/GRB220107_T53142/

As observed by Konus-Wind, the burst
had a fluence of 5.48(-0.30,+0.34)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+81.344 s,
of 8.18(-1.55,+1.54)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+105.984 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.02(-0.11,+0.12)
and Ep = 247(-24,+30) keV (chi2 = 53/61 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 53/60 dof).

The spectrum near the maximum count rate
(measured from T0+73.984 to T0+89.600 s)
is best fit in the 20 keV - 2 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.86(-0.11,+0.12),
the high energy photon index beta = -2.91(-1.53,+0.32),
the peak energy Ep = 186(-15,+17) keV
(chi2 = 46/60 dof).

Assuming the redshift z=1.246 (Castro-Tirado et al., GCN 31423)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the isotropic energy release E_iso to (2.3 Â± 0.1)x10^53 erg,
the isotropic luminosity L_iso to (7.8 Â± 1.5)x10^52 erg/s,
the rest-frame peak energy of the time-integrated spectrum Epi,z to (555 Â±
67) keV,
and the rest-frame peak energy of the 'peak' spectrum Epp,z to (418 Â± 38)
keV.
With these values, GRB 220107A is within 68% prediction bands for
for both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW
GRBs
with known redshifts (Tsvetkova et al., 2021, ApJ, 908, 83),
see http://www.ioffe.ru/LEA/GRBs/GRB220107_T53142/GRB220107A_rest_frame.pdf

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


GRB_name: GRB220107B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31430
SUBJECT: Konus-Wind detection of GRB 220107B
DATE:    22/01/10 19:42:50 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 220107B
(Fermi-LAT detection: Arimoto et al., GCN 31409;
AstroSat CZTI detection: Suresh et al., GCN 31412;
Fermi-GBM observation: Veres and Meegan et al., GCN 31414)
triggered Konus-Wind at T0=68494.81 s UT (19:01:34.810).

The burst light curve shows a multipeaked structure
started at ~T0-1.2 s with a total duration of ~26.4 s.
The emission is seen up to ~4 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220107_T68494/

As observed by Konus-Wind, the burst
had a fluence of 4.20(-0.78,+0.91)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.728 s,
of 8.07(-2.17,+2.27)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+32.768 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.73(-0.19,+0.27),
the high energy photon index beta = -2.18(-0.38,+0.22),
the peak energy Ep = 309(-65,+72) keV
(chi2 = 54/69 dof).

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+8.192 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.58(-0.17,+0.20),
the high energy photon index beta = -2.21(-0.37,+0.21),
the peak energy Ep = 334(-56,+68) keV
(chi2 = 54/70 dof).

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


GRB_name: GRB220107A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31431
SUBJECT: GRB 220107A: SAO RAS optical observations
DATE:    22/01/11 05:08:48 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin (SAO), on behalf of larger GRB follow-up team report:

We observed the field of GRB 220107A (The Fermi GBM team, GCN 31399;
Kunzweiler et al. GCN 31400; DeLaunay et al. GCN 31402; Suresh et al.,
GCN 31408; Ridnaia et al., GCN 31429) with the SAO RAS 1-m telescope
Zeiss-1000 + CCD-photometer. Two series of images in Rc band
were obtained: the 1st under moderate weather conditions
and the 2nd with relatively clear sky.

The OT (Hosokawa et al. GCN 31413; Siegel GCN 31415; Zhu et al.
GCN 31416; Pankov et al., GCN 31419; Moskvitin et al., GCN 31422;
Castro-Tirado et al., GCN 31423, Moskvitin & Medvedev, GCN 31426)
is clearly visible in the stacked frames.  Preliminary photometry
of the afterglow is as follows (based on nearby SDSS-DR12 stars
mentioned in GCNs 31422, 31426).

UT start -- UT end    T_mid-T0, d  Exp., s   R_mag +/- err   series

Jan. 10     Jan. 11
23:22:13 -- 02:06:39  3.41592      23 x 300  21.69 +/- 0.10  1st

Jan. 11     Jan. 11
02:49:39 -- 03:30:10  3.51694       8 x 300  22.03 +/- 0.09  2nd


GRB_name: GRB220101A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31433
SUBJECT: Konus-Wind detection of GRB 220101A
DATE:    22/01/11 18:45:24 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The long-duration, bright GRB 220101A (Swift-BAT trigger #1091101:
Tohuvavohu  et al., GCN 31347; Markwardt et al., GCN 31369;
Fermi-LAT detection: Arimoto et al., GCN 31350;
AGILE detection: Ursi et al., GCN 31354;
Fermi-GBM detection: Lesage & Meegan, GCN 31360)
triggered Konus-Wind at T0=18695.828 s UT (05:11:35.828).

The burst light curve shows a bright, multi-peaked pulse
which starts at ~T0-147 s and has a total duration of~237 s.
The emission is seen up to ~15 MeV.

The total energy fluence of the burst is 9.05(-0.55,+0.60) erg/cm^2
and the 64-ms peak energy flux, measured from T0 + 18.624 s,
is 4.0(-0.7, +0.7)x10^-6 erg/cm^2/s
(both in the 10 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+90.112 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 = -0.58 (-0.13,+0.15),
the high energy photon index beta = -2.62 (-0.53,+0.25),
the peak energy Ep = 257 (-27,+28) keV,
chi2 = 126/119 dof.

The spectrum near the peak count rate (measured from T0+16.640
to T0+24.576 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 = -0.51 (-0.16,+0.18),
the high energy photon index beta = -2.55 (-0.64,+0.31),
the peak energy Ep = 314 (-39,+43) keV,
chi2 = 105/96 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220101_T18695/

Assuming the redshift z = 4.618 (Fynbo et al., GCN 31359)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following burst rest-frame parameters:
the isotropic energy release Eiso = 3.64(-0.22,+0.25)x10^54 erg,
which is in agreement with Atteia, GCN 31365;
the isotropic luminosity Liso = 9.05(-1.58,+1.58)x10^53 erg/s;
the rest-frame peak energy of the time-integrated spectrum Epi,z = 
1416(-157,+152) keV;
and the rest-frame peak energy of the 'peak' spectrum Epp,z = 
1764(-219,+242) keV.

With these values, GRB 220101A is within 68% prediction bands for
for both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW 
GRBs
with known redshifts (Tsvetkova et al., 2021, ApJ, 908, 83),
see http://www.ioffe.ru/LEA/GRBs/GRB220101_T18695/GRB220101A_rest_frame.pdf.

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


GRB_name: GRB220111A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31434
SUBJECT: GRB 220111A: Fermi GBM Final Real-time Localization
DATE:    22/01/11 19:32:17 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 19:21:49 UT on 11 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220111A (trigger 663621714.433092 / 220111807).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 149.1, Dec = 0.5 (J2000 degrees, equivalent to J2000 09h 56m, 0d 30'), with a statistical uncertainty of 1.6 degrees.

The angle from the Fermi LAT boresight is 70.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220111807/quicklook/glg_skymap_all_bn220111807.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220111807/quicklook/glg_healpix_all_bn220111807.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220111807/quicklook/glg_lc_medres34_bn220111807.gif


GRB_name: GRB220111A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31435
SUBJECT: GRB 220111A: BALROG localization (Fermi Trigger 663621714 / GRB 220111807)
DATE:    22/01/11 19:47:26 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
663621714 at 19:21:49 on 11 Jan. 2022 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) = 149.9+/-0.9 deg
Decl.(2000.0) = 0.6+/-0.8 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB220111807/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB220111807/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB220111807/json

                        


GRB_name: GRB220101A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31436
SUBJECT: Konus-Wind detection of GRB 220101A (correction to GCN 31433)
DATE:    22/01/11 20:01:39 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, on behalf of the Konus-Wind team:

Reported in GCN 31433, the total energy fluence of GRB 220101A misses 
the exponent. The correct fluence value is 9.05(-0.55,+0.60)x10^-5 erg/cm^2.

We thank Jean-Luc Atteia for pointing this out and apologize for 
possible inconvenience.


GRB_name: GRB220111A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31437
SUBJECT: Fermi GRB 220111A: Global MASTER-Net observations report 
DATE:    22/01/12 00:30:53 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220111A ( Fermi GBM team, GCN 31434) errorbox  8157 sec after notice time and 8188 sec after trigger time at 2022-01-11 21:38:18 UT, with upper limit up to  17.2 mag. Observations started at twilight.  The observations began at zenith distance = 68 deg. The sun  altitude  is -16.6 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 220111A errorbox  8419 sec after notice time and 8450 sec after trigger time at 2022-01-11 21:42:40 UT, with upper limit up to  19.5 mag. The observations began at zenith distance = 58 deg. The sun  altitude  is -34.1 deg. 

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 220111A errorbox  10681 sec after notice time and 10712 sec after trigger time at 2022-01-11 22:20:21 UT, with upper limit up to  18.2 mag. The observations began at zenith distance = 77 deg. The sun  altitude  is -51.0 deg. 

The galactic latitude b = 41 deg., longitude l = 239 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1846225

We obtain a following upper limits.  

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

    8279 | 2022-01-11 21:38:18 |         MASTER-Amur | (09h 53m 32.49s , -00d 00m 52.5s) |   C |   180 | 16.4 |        
    8481 | 2022-01-11 21:42:40 |         MASTER-SAAO | (09h 48m 52.42s , +01d 12m 00.1s) |   C |    60 | 18.6 |        
    8563 | 2022-01-11 21:43:02 |         MASTER-Amur | (09h 53m 30.03s , -00d 00m 04.8s) |   C |   180 | 17.1 |        
    8763 | 2022-01-11 21:46:22 |         MASTER-Amur | (09h 53m 31.26s , +00d 00m 53.1s) |   C |   180 | 17.3 |        
    8767 | 2022-01-11 21:46:26 |         MASTER-SAAO | (09h 56m 28.94s , +02d 27m 35.1s) |   C |   180 | 17.1 |        
    8963 | 2022-01-11 21:49:42 |         MASTER-Amur | (09h 53m 36.46s , -00d 00m 06.9s) |   C |   180 | 17.0 |        
    8966 | 2022-01-11 21:49:45 |         MASTER-SAAO | (09h 56m 22.78s , +02d 27m 02.4s) |   C |   180 | 19.5 |        
    9164 | 2022-01-11 21:53:03 |         MASTER-Amur | (09h 53m 29.67s , -00d 01m 05.9s) |   C |   180 | 17.0 |        
    9368 | 2022-01-11 21:56:27 |         MASTER-Amur | (09h 53m 37.02s , +01d 59m 20.1s) |   C |   180 | 17.1 |        
    9568 | 2022-01-11 21:59:47 |         MASTER-Amur | (09h 53m 34.21s , +02d 00m 44.2s) |   C |   180 | 17.0 |        
   10364 | 2022-01-11 22:13:03 |         MASTER-SAAO | (09h 56m 28.48s , -01d 27m 25.6s) |   C |   180 | 19.3 |        
   10563 | 2022-01-11 22:16:22 |         MASTER-SAAO | (09h 56m 23.23s , -01d 28m 07.0s) |   C |   180 | 19.4 |        
   10742 | 2022-01-11 22:20:21 |          MASTER-IAC | (09h 47m 50.16s , +03d 15m 32.2s) |   C |    60 | 17.5 |        
   10983 | 2022-01-11 22:24:22 |          MASTER-IAC | (09h 47m 01.57s , -00d 33m 12.3s) |   C |    60 | 17.5 |        
   11673 | 2022-01-11 22:35:52 |          MASTER-IAC | (09h 47m 50.89s , +03d 14m 48.9s) |   C |    60 | 17.7 |        
   11713 | 2022-01-11 22:36:32 |         MASTER-SAAO | (09h 57m 06.07s , +01d 11m 39.8s) |   C |    60 | 18.6 |        
   11793 | 2022-01-11 22:37:52 |         MASTER-SAAO | (09h 48m 56.51s , +01d 11m 08.5s) |   C |    60 | 18.9 |        
   11873 | 2022-01-11 22:39:12 |         MASTER-SAAO | (10h 04m 22.09s , +01d 11m 23.2s) |   C |    60 | 18.4 |        
   11913 | 2022-01-11 22:39:52 |          MASTER-IAC | (09h 46m 59.27s , -00d 32m 18.3s) |   C |    60 | 17.6 |        
   12115 | 2022-01-11 22:43:14 |         MASTER-SAAO | (10h 04m 07.82s , -00d 43m 26.4s) |   C |    60 | 18.6 |        
   12419 | 2022-01-11 22:48:18 |          MASTER-IAC | (09h 47m 01.59s , +01d 19m 46.5s) |   C |    60 | 17.7 |        
   12419 | 2022-01-11 22:48:18 |          MASTER-IAC | (09h 55m 13.34s , +01d 14m 53.2s) |   C |    60 | 14.9 |        
   12579 | 2022-01-11 22:50:57 |          MASTER-IAC | (09h 47m 47.15s , +03d 15m 10.4s) |   C |    60 | 17.9 |        
   12579 | 2022-01-11 22:50:57 |          MASTER-IAC | (09h 55m 59.33s , +03d 10m 20.0s) |   C |    60 | 16.5 |        
   12772 | 2022-01-11 22:54:11 |         MASTER-SAAO | (09h 56m 57.71s , +01d 11m 24.8s) |   C |    60 | 18.8 |        
   12818 | 2022-01-11 22:54:57 |          MASTER-IAC | (09h 46m 56.27s , -00d 33m 22.0s) |   C |    60 | 17.8 |        
   12819 | 2022-01-11 22:54:57 |          MASTER-IAC | (09h 55m 07.86s , -00d 38m 15.8s) |   C |    60 | 15.6 |        
   12851 | 2022-01-11 22:55:30 |         MASTER-SAAO | (09h 48m 56.76s , +01d 12m 20.3s) |   C |    60 | 18.6 |        
   12931 | 2022-01-11 22:56:50 |         MASTER-SAAO | (10h 04m 15.14s , +01d 11m 32.2s) |   C |    60 | 18.4 |        
   12979 | 2022-01-11 22:57:38 |          MASTER-IAC | (09h 55m 49.49s , -02d 32m 16.4s) |   C |    60 | 14.7 |        
   13326 | 2022-01-11 23:03:25 |          MASTER-IAC | (09h 47m 03.78s , +01d 20m 07.8s) |   C |    60 | 17.8 |        
   13326 | 2022-01-11 23:03:25 |          MASTER-IAC | (09h 55m 15.26s , +01d 15m 17.6s) |   C |    60 | 16.7 |        
   13989 | 2022-01-11 23:14:28 |          MASTER-IAC | (10h 03m 00.58s , +03d 14m 15.3s) |   C |    60 | 18.2 |        
   14257 | 2022-01-11 23:18:56 |          MASTER-IAC | (09h 47m 01.59s , +01d 21m 41.4s) |   C |    60 | 18.0 |        
   14257 | 2022-01-11 23:18:56 |          MASTER-IAC | (09h 55m 13.11s , +01d 16m 53.9s) |   C |    60 | 17.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220111A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31440
SUBJECT: GRB 220111A: AstroSat CZTI detection
DATE:    22/01/12 07:34:03 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 the CIFT framework (Sharma et al., 2021,
JApA, 42, 73), showed detection of a long GRB 220111A, which was also
detected by Fermi-GBM (GCN 31434), with localization reported by BALROG
(Biltzinger et al., GCN 31435). 

The source was clearly detected in the 20-200 keV energy range. The
light curve peaks at 2022-01-11 19:21:52.75 UT. The measured peak count
rate associated with the burst is 1028 (+208, -77) cts/s above the
background in the combined data of four quadrants, with a total of 3672
(+250, -232) cts. The local mean background count rate was 471 (+4, -7)
cts/s. Using cumulative rates, we measure a T90 of 10 (+1, -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 2022-01-11
19:21:51.95 UT. The measured peak count rate is 509 (+72, -80) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 1900 (+429, -475) cts. The local mean background count rate was
1580 (+5, -5) cts/s. We measure a T90 of 5 (+6, -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: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31442
SUBJECT: GRB 220101A: continued 1.3m DFOT optical observations of a high-redshift afterglow
DATE:    22/01/12 11:11:42 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

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

We further observed the optical afterglow of the Swift detected GRB 220101A
(Tohuvavohu et al., GCN 31347) at z = 4.618 (Fu et al., GCN 31353; Fynbo et
al., GCN 31359) with the 1.3m Devsthal Fast Optical Telescope (DFOT) at
Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital
(India), from 2022-01-03 UT 12:54:68 to 2022-01-03 UT 15:04:14 (from ~55.75
to 57.91 hours after the burst). We obtained 40 frames each of 120 seconds
in Bessell R and I filters. We clearly detected the optical afterglow of
GRB 220101A in stacked frames within the Swift XRT enhanced error circle
(Tohuvavohu et al., GCN 31347) as also reported by Kuin & Tohuvavohu, GCN
31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356; Perley, GCN 31357;
de Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; Vinko et al.,
GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCNs 31364, 31368;
Noschese et al., GCN 31366; Guelbenzu et al., GCN 31370; Strausbaugh et
al., GCNs 31371, 31383, 31389; Dimple et al., GCN 31384; Romanov, GCN
31387; Caballero-Garcia et al., GCN 31388; Belkin et al., GCN 31390; Ror et
al., GCN 31394; Avanzo et al., GCN 31395; Pankov et al., GCN 31398;
Guelbenzu et al., GCN 31401; Moskvitin et al., GCN 31420; and Perley, GCN
31425.

The estimated preliminary magnitudes for the R and I-band images are as
follows:

T_start-T0(hours)           Filter           Magnitude (mag)
-----------------------------------------------------------------------
55.75                              I                   19.52 +- 0.02
57.91                              R                   20.95 +- 0.04

Aperture photometry is performed, and calibration is done based on the
standard stars in the USNO-B1.0 catalogue. The quoted magnitudes are not
corrected for the Galactic extinction in the direction of GRB 220101A.

This message may be cited.


GRB_name: GRB220114A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31449
SUBJECT: GRB 220114A: Fermi GBM Final Localization
DATE:    22/01/15 02:08:39 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

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

At 14:01:47.41 UT on 14 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220114A (trigger 663861712 / 220114585).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 202.9, Dec = -11.8 (J2000 degrees, equivalent to J2000 13h 31m, -11d 48'), with a statistical uncertainty of 2.4 degrees.

The angle from the Fermi LAT boresight is 65.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220114585/quicklook/glg_skymap_all_bn220114585.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220114585/quicklook/glg_healpix_all_bn220114585.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220114585/quicklook/glg_lc_medres34_bn220114585.gif


GRB_name: GRB220115A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31452
SUBJECT: GRB 220115A: Fermi GBM Final Real-time Localization
DATE:    22/01/15 17:10:53 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 17:00:27 UT on 15 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220115A (trigger 663958832.581364 / 220115709).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 101.9, Dec = 11.0 (J2000 degrees, equivalent to J2000 06h 47m, 11d 00'), with a statistical uncertainty of 2.8 degrees.

The angle from the Fermi LAT boresight is 29.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220115709/quicklook/glg_skymap_all_bn220115709.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220115709/quicklook/glg_healpix_all_bn220115709.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220115709/quicklook/glg_lc_medres34_bn220115709.gif


GRB_name: GRB210919A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31453
SUBJECT: GRB 210919A: LBT spectroscopic redshift of the host galaxy candidates
DATE:    22/01/15 17:52:12 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi, F. Cusano, E. Palazzi, L. Amati (INAF-OAS Bologna), D. B. 
Malesani (Radboud U. Nijmegen and DAWN/NBI), S. Savaglio (UNICAL), on 
behalf of the CIBO collaboration, and D. A. Kann (HETH/IAA-CSIC) report:

We report the results of spectroscopic observations of two galaxies 
close to the position of the GRB (O'Connor et al. GCN #30934, Kann et 
al., GCN #30983) of the short GRB 210919A (Tohuvavohu et al., GCN 
#30846), obtained with the Multi-Object Double Spectrographs (MODS) 
instrument mounted on the 2x8.4-m LBT telescope (Mt. Graham, AZ, USA). 
Spectra were obtained at a mid-time of 12:35 UT on 2021-10-16, ~27.5 
days after the burst trigger, for a total on-source time of 5400 s, 
covering the wavelength range 3200-10000 AA.

The MODS slit inclination was adjusted to cover the positions of the two 
objects singled out by O'Connor et al. (GCN #30934), with offsets of 
~3.4 and 13" with respect to the candidate afterglow by Kann et al. 
(GCNs #30883 and #30884) respectively, and of the faint source at the 
eastern edge of the XRT error circle detected in the ESO-VLT/FORS2 
images (Kann et al., GCN #30983). This latter source was not detected in 
the MODS data. The spectra of the other two galaxies show several well 
detected emission lines which we interpret as [OII] 3727AA, H-beta, 
[OIII] 4959,5007AA and H-alpha at a common redshift for both sources of 
z=0.2411. The clear detection of these emission lines, and especially 
H-beta, indicates that these are two star forming galaxies.

At this redshift, the projected distances to the two galaxies at ~3.4" 
and ~13" from the afterglow corresponds to ~13 and ~50 kpc. The distance 
between the two galaxies corresponds to 63 kpc, similar to the distance 
between the Milky Way and the SMC. There is at least another galaxy (RA, 
DEC = 05:21:04.01, +01:18:49.23) within 0.5 arcmin with similar 
photometric redshifts (SDSS DR16), suggesting that the two galaxies are 
probably not isolated, but part of a larger group.

If GRB 210919A was at z = 0.2411, using standard cosmology (Planck 2016) 
and the analysis of the BAT spectra (Barthelmy et al., GCN #30863 and 
http://gcn.gsfc.nasa.gov/notices_s/1073893/BA), we find that it would be 
consistent with the population of short GRBs in the Ep,i - Eiso plane.

We acknowledge the excellent support from the LBTO and LBT-INAF staff, 
particularly D. Thompson, S. Allanson, and S. Paiano, in obtaining these 
observations.


GRB_name: GRB220115B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31457
SUBJECT: GRB 220115B: Fermi GBM Final Real-time Localization
DATE:    22/01/15 22:48:15 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:37:50 UT on 15 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220115B (trigger 663979075.514384 / 220115943).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 317.8, Dec = -14.8 (J2000 degrees, equivalent to J2000 21h 11m, -14d 48'), with a statistical uncertainty of 6.7 degrees.

The angle from the Fermi LAT boresight is 60.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220115943/quicklook/glg_skymap_all_bn220115943.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220115943/quicklook/glg_healpix_all_bn220115943.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220115943/quicklook/glg_lc_medres34_bn220115943.gif


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31465
SUBJECT: GRB 220101A: The most powerful GRB and BDHN I in 26 years
DATE:    22/01/17 11:00:26 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

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


GRB 220101A, first detected by Swift (Tohuvavohu et al., GCN 31347) with
redshift z=4.618 (Fu et al 2022., GCN 31353; Fynbo et al 2022., GCN 31359)
and energy of 3.7E54 (J.-L. Atteia 2022, GCN 31365) is categorized as a
BdHN I with the most powerful and the highest ever observed X-ray afterglow
luminosity in 26 years, as well as the highest supernova rise (SN-rise) and
the new neutron star rise (vNS-rise) (Ruffini et al. 2021 MNRAS, 504, 5301)
see Fig. 1. There is evidence for the ultrarelativistic prompt emission
(UPE) phase (Moradi et al. 2021 PRD 104, 063043).

We encourage optical and radio observations to identify the corresponding
UPE phase as well as the synchrotron emission originating from the spinning
vNS.


Fig. 1: http://www.icranet.org/figure1.pdf


GRB_name: GRB220117A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31466
SUBJECT: GRB 220117A: Swift detection of a burst
DATE:    22/01/17 16:31:16 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), T. Sbarrato (INAF-OAB) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 16:18:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220117A (trigger=1093592).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 91.578, -28.410 which is 
   RA(J2000) = 06h 06m 19s
   Dec(J2000) = -28d 24' 35"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 65 sec.  The peak count rate
was ~900 counts/sec (15-350 keV), at ~15 sec after the trigger. 

The XRT began observing the field at 16:21:23.4 UT, 151.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 91.57277, -28.43760 which
is equivalent to:
   RA(J2000)  = 06h 06m 17.46s
   Dec(J2000) = -28d 26' 15.4"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 100 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper.  We cannot determine whether the source
is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.57
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 6.01e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 161 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
0.029. 

Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB220117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31467
SUBJECT: GRB 220117A: Nanshan/NEXT optical observations and a nearby PanSTARRS source
DATE:    22/01/17 18:51:10 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 220117A detected by Swift (Melandri et al., 
GCN 31466) using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. Observations automatically started at 16:21:57 UT on 2022-01-17 
(i.e., 186 s after the BAT trigger), and a series of 40 s, 60 s, 90 s, 
200 s frames were obtained in the Sloan r- and z- filters.

No uncatalogued optical transient is detected in our stacked images at 
the Swift-XRT position (GCN 31466), down to limiting magnitudes of 
r~19.6 and z~18.7, calibrated with the nearby PanSTARRS field.

Nevertheless, we note that from PanSTARRS there exists a source at the 
border of the Swift-XRT error circle at coordinates R.A. (J2000) = 
6:06:17.32 and Dec. (J2000) = -28:26:13.07, which has magnitudes of g 
~21.51, r~21.05, i~20.99, and z~21.02, rasing the possibility as the 
host galaxy of the GRB. This sky area is not covered by SDSS and Legacy 
Survey. SkyMapper covered the sky area with upper limits of r~19.0 and 
z~19.0, comparable to the NEXT's level. It is thus unclear if the 
PanSTARRS source is related to the GRB or not.


GRB_name: GRB220117B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31468
SUBJECT: GRB 220117B: Swift detection of a burst
DATE:    22/01/17 20:18:29 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Melandri (INAF-OAB), M. G. Bernardini (INAF-OAB), J.D. Gropp (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), A. Y. Lien (U Tampa),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), T. Sbarrato (INAF-OAB) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 20:05:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220117B (trigger=1093611).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 191.947, -28.744 which is 
   RA(J2000) = 12h 47m 47s
   Dec(J2000) = -28d 44' 38"
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 ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 20:07:04.0 UT, 95.9 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 191.9514, -28.7446 which is equivalent to:
   RA(J2000)  = 12h 47m 48.34s
   Dec(J2000) = -28d 44' 40.6"
with an uncertainty of 6.5 arcseconds (radius, 90% containment). This
location is 14 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 4.69e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of nominal 150.000 seconds with the White
filter starting 104 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 0.075. 

Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB220117B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31469
SUBJECT: Swift GRB 220117B: Global MASTER-Net observations report 
DATE:    22/01/17 20:24:34 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220117B ( A. Melandri et al., GCN 31468) errorbox  380 sec after notice time and 437 sec after trigger time at 2022-01-17 20:12:45 UT, with upper limit up to  12.4 mag. The observations began at zenith distance = 79 deg. The sun  altitude  is -29.8 deg. 

The galactic latitude b = 34 deg., longitude l = 303 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1852756

We obtain a following upper limits.  

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

     483 |         MASTER-Amur |  P/ |    90 | 12.4 |        


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


GRB_name: GRB220117A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31470
SUBJECT: Swift GRB 220117A: Global MASTER-Net observations report 
DATE:    22/01/17 20:50:22 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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) was pointed to the Swift GRB 220117A ( A. Melandri et al., GCN 31466) errorbox  15547 sec after notice time and 15645 sec after trigger time at 2022-01-17 20:39:37 UT, with upper limit up to  17.5 mag. The observations began at zenith distance =  5 deg. The sun  altitude  is -28.9 deg. 

The galactic latitude b = -21 deg., longitude l = 235 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1852619

We obtain a following upper limits.  

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

   15736 |         MASTER-SAAO |   C |   180 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31471
SUBJECT: GRB 220101A: TSHAO optical observation, Terskol, AbAO upper limits
DATE:    22/01/17 22:02:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (HSE), A. Pozanenko (IKI), A. Kusakin (FAP), I. Reva (FAP), R. 
Ya. Inasaridze (AbAO), V. Agletdinov (KIAM), S. Belkin (IKI, HSE), I. 
Sokolov (KIAM), M. Krugov (FAP) report on behalf of GRB IKI FuN:

We observed Swift GRB 220101A (Tohuvavohu, et al., GCN 31347) also
detected by Fermi/LAT (Arimoto et al. 2022, GCN 31350), AGILE (Ursi et
al. 2022, GCN 31354),  Fermi/GBM (Lesage et al. 2022, GCN 31360), and 
Konus-Wind (Tsvetkova et al., GCN 31433)  with Zeiss-1000 telescope of 
THSAO observatory (Kazakhstan) in R-filter starting on 2022-01-05 (UT) 
14:39:20. We were also observing the afterglow position with with AS-32 
telescope of Abastumani observatory (AbAO) and K-800 telescope of Mnt. 
Terskol observatory on 2022-01-06.

The afterglow (Tohuvavohu et al., GCN 31347; Kuin & Tohuvavohu, GCN 
31351; Fu et al., GCN 31353; Hentunen et al., GCN 31356; Perley et al., 
GCN 31357; de Ugarte Postigo et al., GCN 31358; Fynbo et al., GCN 31359; 
Vinko et al., GCN 31361; Tomasella et al., GCN 31363; Mao et al., GCN 
31364; Noschese et al., GCN 31366; Mao et al., GCN 31368; Guelbenzu, et 
al., GCNs 31370, 31401; Strausbaugh et al., GCN 31371; D'Avanzo et al., 
GCN 31373; Strausbaugh et al., GCNs 31383, 31389; Dimple et al., GCN 
31384; Romanov, GCN 31387; Caballero-Garcia, GCN 31388; Belkin et al., 
GCNs 31390, 31398; Gupta et al., GCN 31394; D'Avanzo et al., GCN 31395; 
Pankov et al., GCN 31398; Moskvitin et al., GCN 31420; Perley, GCN 
31425; Kumar et al., GCN 31442) is detected in THSAO observation, and 
upper limits obtained in Terskol K-800 and AbAO AS-32 observations.
Preliminary photometry of the afterglow and upper limits is following

Date UT start t-T0 Filter Exp. OT Err UL(3sigma) Telescope
2022-01-05 14:39:20 4.42129 R     25*180 22.19 0.23  22.5 Zeiss-1000
2022-01-06 15:06:30 5.45091 R    106*60  n/d   n/d   21.9 AS-32
2022-01-06 17:21:42 5.51841 Clear 30*60  n/d   n/d   21.5 K-800

The photometry is based on the nearby SDSS-DR12 stars
RA DEC R(Lupton transformations)
00:05:20.64408 +31:45:46.0728 18.562
00:05:34.81464 +31:45:50.5224 15.734
00:05:32.53944 +31:44:51.9396 15.369
00:05:36.69864 +31:44:42.4176 14.677

Based on multiple observations cited above and our own observations the 
light curve in R-filter  can be approximated by a single power law 
(after one day after the trigger) with the power law index of -1.9. The 
light curve can be be found in
http://grb.rssi.ru/GRB220101A/GRB220101A_LC.png


GRB_name: GRB220117A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31472
SUBJECT: GRB 220117A: Enhanced Swift-XRT position
DATE:    22/01/17 23:36:13 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 428 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220117A, 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 = 91.57218, -28.43765 which is equivalent
to:

RA (J2000): 06h 06m 17.32s
Dec (J2000): -28d 26' 15.5"

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: GRB220117B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31473
SUBJECT: GRB 220117B: Enhanced Swift-XRT position
DATE:    22/01/18 02:07:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 867 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 220117B, 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 = 191.95292, -28.74540 which is equivalent
to:

RA (J2000): 12h 47m 48.70s
Dec (J2000): -28d 44' 43.4"

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: GRB220117B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31474
SUBJECT: GRB 220117B: MITSuME Akeno optical upper limits
DATE:    22/01/18 02:45:51 GMT
FROM:    Naohiro Ito at Tokyo Tech  <n.ito@hp.phys.titech.ac.jp>

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

We observed the field of GRB 220117B (A. Melandri et al. GCN Circular
#31468, V. Lipunov et al. GCN Circular #31469) with the optical three color
(g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno.
The observation started at 2022-01-17 20:06:58 UT (1.5 minutes after Swift
trigger). We stacked the images with good conditions. We did not detect any
sources within the XRT error region (A. Melandri et al. GCN Circular
#31468). We obtained the 5-sigma limits of the stacked images as follows.

T0+[minutes] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
2.9 2022-01-17 20:08:19 80 g'>16.3, Rc>16.4, Ic>15.8
28.7 2022-01-17 20:34:10 2280 g'>16.5, Rc>17.0, Ic>16.5
------------------------------------------------------------------------------------------------
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: GRB220117B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31475
SUBJECT: GRB 220117B: Nanshan/NEXT optical upper limit
DATE:    22/01/18 03:25:24 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 220117B detected by Swift (Melandri et al., 
GCN 31468) using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. Observations automatically started at 20:07:36 UT on 2022-01-17, 
i.e., 128 s after the BAT trigger, and a series of 40 s, 60 s, 90 s 
frames were obtained in the Sloan r-band.

No uncatalogued optical transient is detected in our stacked images at 
the Swift-XRT position (GCN 31468), down to limiting magnitudes of 
r~18.5, calibrated with the nearby PanSTARRS field.


GRB_name: GRB220117A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31477
SUBJECT: GRB 220117A: Swift-XRT refined Analysis
DATE:    22/01/18 09:06:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.4 ks of XRT data for GRB 220117A (Melandri et al.
GCN Circ. 31466), from 142 s to 51.2 ks after the  BAT trigger. The
data comprise 98 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
Beardmore et al. (GCN Circ. 31472).

The late-time light curve (from T0+4.3 ks) can be modelled with a
power-law decay with a decay index of alpha=1.48 (+0.11, -0.10).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.69 (+/-0.10). The
best-fitting absorption column is  1.95 (+0.24, -0.23) x 10^21 cm^-2,
in excess of the Galactic value of 2.6 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.80 (+/-0.11) and a
best-fitting absorption column of 4.5 (+2.6, -1.9) x 10^20 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.5 x 10^-11 (3.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.5 (+2.6, -1.9) x 10^20 cm^-2
Galactic foreground: 2.6 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.80 (+/-0.11)

If the light curve continues to decay with a power-law decay index of
1.48, the count rate at T+24 hours will be 6.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.3 x
10^-13 (2.5 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01093592.

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


GRB_name: GRB220117B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31478
SUBJECT: GRB 220117B: Swift-XRT refined Analysis
DATE:    22/01/18 09:11:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.7 ks of XRT data for GRB 220117B (Melandri et al.
GCN Circ. 31468), from 88 s to 28.6 ks after the  BAT trigger. The data
comprise 203 s in Windowed Timing (WT) mode (the first 6 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 31473).

The late-time light curve (from T0+3.5 ks) can be modelled with a
power-law decay with a decay index of alpha=0.79 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.65 (+0.11, -0.10). The
best-fitting absorption column is  4.5 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 7.6 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.04 (+0.19, -0.18)
and a best-fitting absorption column of 3.0 (+0.8, -0.7) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.6 x 10^-11 (5.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.0 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 7.6 x 10^20 cm^-2
Excess significance: 5.2 sigma
Photon index:      2.04 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
0.79, the count rate at T+24 hours will be 0.024 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.8 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01093611.

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


GRB_name: GRB220117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31480
SUBJECT: GRB 220117A: VLT/X-shooter optical afterglow and redshift
DATE:    22/01/18 12:25:23 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

J. Palmerio (CNRS, GEPI - Paris Observatory), D. B. Malesani (Radboud 
Univ. and DAWN/NBI), J. P. U. Fynbo (DAWN/NBI), D. Xu (NAOC), L. Izzo 
(DARK/NBI), S. Y. Fu (NAOC), Z. P. Zhu (NAOC, HUST), D. A. Kann 
(IAA/CSIC), N. R. Tanvir (Univ. Leicester) report on behalf of the 
Stargate collaboration:

We observed the field of GRB 220117A (Melandri et al., GCN 31466) using 
the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our 
first observations were carried out using the acquisition camera, using 
the g, r and z filters (3x60 s in each band). Inside the XRT error 
circle (Beardmore et al., GCN 31472), we detect a new source, not 
visible in the archival Pan-STARRS images, which we identify as the GRB 
afterglow. The source is very red, being detected strongly in z, only 
weakly in r, and completely missing in g. Calibrated against nearby 
stars from the Pan-STARRS catalog, we measure z = 20.81 +- 0.12 mag and 
z - r ~ 2.1 mag (all AB magnitudes). The afterglow coordinates are 
(J2000, 0.2" error):

RA = 06:06:17.409
Dec = -28:26:15.78

A spectrum was secured covering the wavelength range 3000-21000 AA, and 
consisting of 4 exposures of 1200 s each. The observation mid time was 
2022 Jan 18.15 UT (11.3 hr after the GRB).

In a preliminary reduction, continuum is detected in the red part of the 
spectrum down to ~7260 AA. We interpret the break as due to Lyman alpha. 
The absorption system is rather weak and, at the present time, we 
identify with confidence only the Lyman-alpha trough and the Si II 1260 
AA feature, which correspond to a redshift z = 4.961 for GRB 220117A.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Michael Abdul-Masih, Diego Parraguez, and 
Jonathan Smoker.


GRB_name: GRB220117A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31481
SUBJECT: GRB 220117A: LCO Optical Observations
DATE:    22/01/18 13:39:22 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 220117A (Melandri et al., GCN 31466) with the LCO 1-m Sinistro instrument at the Cerro Tololo Interamerican Observatory, Chile site, on January 18, from 01:16 to 01:33 UT (corresponding to 6.97 to 7.25 hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 3x320s exposures in I band and 1x152s in R band (the planned observations in R were interrupted). We detect the source at the XRT enhanced coordinates (Beardmore et al., GCN 31472) and VLT observations (Palmerio et al., GCN 31480) in I band, but not R band. The following magnitudes and upper limits are calculated using the USNO-B.1 catalog as reference:

R>19.14
I=20.64+/-0.30

These magnitudes are not corrected for galactic extinction.

R.S. is funded by NSF AST grant #1831682


GRB_name: GRB220117A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31482
SUBJECT: GRB 220117A: Swift/UVOT Upper Limits
DATE:    22/01/18 14:13:23 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and A. Melandri (INAF-OAB) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220117A 162 s after the BAT trigger 
(Melandri et al., GCN Circ. 31466).
No optical afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 31472) 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           162          311          147         >20.5
u_FC               320          570          246         >20.0
white              162          998          306         >20.7
v                  650          845           39         >18.4
b                  576          770           39         >19.4
u                  320          744          265         >20.0
w1                 700          720           19         >19.3
m2                 675          869           39         >18.7
w2                 626          821           39         >18.9

The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of 
E(B-V) = 0.028 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB220117B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31483
SUBJECT: GRB 220117B: Swift/UVOT Upper Limits
DATE:    22/01/18 14:15:21 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and A. Melandri (INAF-OAB) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220117B 104 s after the BAT trigger 
(Melandri et al., GCN Circ. 31468).
No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 31473) is detected in 
the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. 
Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are:

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

white_FC           104          254          147         >19.7
white              104         3930          344         >20.5
v                 4141         4341          197         >19.2
b                 3525         5048          281         >20.7
u                  262         4957          239         >19.8
w1                4552         4752          197         >20.0
m2                4346         4546          197         >20.3
w2                3936         4136          197         >20.4

The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of 
E(B-V) = 0.075 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB220117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31485
SUBJECT: GRB 220117A: Swift-BAT refined analysis
DATE:    22/01/18 15:35:31 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
A. Melandri (INAF-OAB), 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+939 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220117A (trigger #1093592)
(Melandri et al., GCN Circ. 31466).  The BAT ground-calculated position is
RA, Dec = 91.590, -28.402 deg which is
   RA(J2000)  =  06h 06m 21.5s
   Dec(J2000) = -28d 24' 08.5"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 26%.

The mask-weighted light curve shows a multi-peaked structure that
starts at ~T+15 s and ends at ~T+65 s. The two larger peaks occur
at ~T+15 s and ~T+44 s, respectively. T90 (15-350 keV) is
49.81 +- 2.37 sec (estimated error including systematics).

The time-averaged spectrum from T+14.79 to T+66.14 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.84 +- 0.18.  The fluence in the 15-150 keV band
is 1.6 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+14.81 sec in the 15-150 keV band is 1.9 +- 0.4 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1093592/BA/


GRB_name: GRB220117B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31486
SUBJECT: GRB 220117B: Swift-BAT refined analysis
DATE:    22/01/18 15:36:36 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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),
A. Melandri (INAF-OAB), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+717 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220117B (trigger #1093611)
(Melandri et al., GCN Circ. 31468).  The BAT ground-calculated position is
RA, Dec = 191.989, -28.762 deg which is
   RA(J2000)  =  12h 47m 57.3s
   Dec(J2000) = -28d 45' 42.8"
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The mask-weighted light curve shows a weak structure that starts
at ~T-3 s and ends at ~T+23 s. T90 (15-350 keV) is 24.37 +- 4.63 sec
(estimated error including systematics).

The time-averaged spectrum from T-2.73 to T+23.29 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.94 +- 0.32.  The fluence in the 15-150 keV band is
2.9 +- 0.6 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from
T-0.13 sec in the 15-150 keV band is 0.5 +- 0.2 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1093611/BA/


GRB_name: GRB220117A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31487
SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 220117A
DATE:    22/01/18 16:53:23 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres (UAH)
reports on behalf of the Fermi-GBM Team:

â€œSwift-BAT detected GRB 220117A at T0=2022-01-17T16:18:51.5 UT
(Melandri et al, GCN 31466). There was no Fermi-GBM onboard trigger
around the event.

The GBM targeted search [1], the most sensitive, coherent search for
GRB-like signals was run from +/-30 s around the BAT trigger time.  A
transient source was identified whose most significant timescale according
to the search is 4.096 s with a false alarm rate of 1.9e-5 Hz, and a
location consistent with the Swift-BAT event, using the standard search
protocol with a S/N of 11.4.  The GBM targeted search event was found with
the highest significance with a â€œsoftâ€ spectral template (Band
function with Epeak = 70 keV, alpha = -1.9, beta = -3.7).

The GBM light curve consists of multiple overlapping pulses. The
time-averaged spectrum from T0 + 11.7 s to T0 + 69.0 s is best fit by
a power law function with an exponential high-energy cutoff. The
power law index is -1.39 +/- 0.20 and the cutoff energy, parameterized
as Epeak, is 40.0 +/- 4.8 keV.

The event fluence (10-1000 keV) in this time interval for the best fitting
model is (2.40 +/- 0.17)E-6 erg/cm^2. Using the redshift z=4.961 reported
by Palmerio et al. (GCN 31480), we derive an isotropic equivalent energy in
the 1-10,000 keV range of (1.56 +/- 0.11)E+53 erg.

This analysis is preliminary.

[1] Goldstein et al. 2019 arXiv:1903.12597
â€


GRB_name: GRB220117A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31488
SUBJECT: GRB 220117A: MITSuME Akeno optical upper limits
DATE:    22/01/18 17:30:21 GMT
FROM:    Naohiro Ito at Tokyo Tech  <n.ito@hp.phys.titech.ac.jp>

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

We observed the field of GRB 220117A (A. Melandri et al. GCN Circular
#31466, S.Y. Fu et al. GCN Circular #31467, V. Lipunov et al. GCN
Circular #31470, A.P. Beardmore et al. GCN Circular #31472, J.A.
Kennea et al. GCN Circular #31477, J. Palmerio et al. GCN Circular
#31480, R. Strausbaugh et al. GCN Circular #31481, A. A. Breeveld et
al. GCN Circular #31482, D. M. Palmer et al. GCN Circular #31485, P.
Veres et al. GCN Circular #31487) 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
2022-01-18 10:26:37 UT (18.1 hours after Swift trigger). We stacked
the images with good conditions. We did not detect any sources within
the XRT error region (A.P. Beardmore et al. GCN Circular #31472). We
obtained the 5-sigma limits of the stacked images as follows.

T0+[hours] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
21.3 2022-01-18 13:34:36 7740 g'>19.0, Rc>19.5, Ic>19.2
------------------------------------------------------------------------------------------------
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: GRB220118A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31489
SUBJECT: GRB 220118A: Fermi GBM Final Real-time Localization
DATE:    22/01/18 18:30:59 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 18:20:35 UT on 18 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220118A (trigger 664222840.838306 / 220118764).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 191.4, Dec = 23.6 (J2000 degrees, equivalent to J2000 12h 45m, 23d 36'), with a statistical uncertainty of 5.0 degrees.

The angle from the Fermi LAT boresight is 52.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220118764/quicklook/glg_skymap_all_bn220118764.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220118764/quicklook/glg_healpix_all_bn220118764.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220118764/quicklook/glg_lc_medres34_bn220118764.gif


GRB_name: GRB220118A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31490
SUBJECT: GRB 220118A: Swift detection of a burst with an optical counterpart
DATE:    22/01/18 18:33:38 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

N. J. Klingler (GSFC/UMBC/CRESSTII), E. Ambrosi (INAF-IASFPA),
A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC & INAF-OAR), S. Dichiara (PSU),
J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC),
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 18:20:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220118A (trigger=1093742).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 192.274, +22.909 which is 
   RA(J2000) = 12h 49m 06s
   Dec(J2000) = +22d 54' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~1400 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 18:22:08.3 UT, 90.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 192.26936,
22.91600 which is equivalent to:
   RA(J2000)  = 12h 49m 04.65s
   Dec(J2000) = +22d 54' 57.6"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 29 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 (2.25 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.4
(+2.60/-2.24) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.57e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 99 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 12:49:04.53 = 192.26888
  DEC(J2000) = +22:54:56.2  =  22.91562
with a 90%-confidence error radius of about 0.75 arc sec. This position is 1.8
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.83 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.025. 

Burst Advocate for this burst is N. J. Klingler (noelklin AT umbc.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: GRB220118A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31491
SUBJECT: Swift GRB 220118A: Global MASTER-Net observations report 
DATE:    22/01/18 19:56:19 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220118A ( N. J. Klingler et al., GCN 31490) errorbox  4483 sec after notice time and 4505 sec after trigger time at 2022-01-18 19:35:43 UT, with upper limit up to  15.9 mag. The observations began at zenith distance = 29 deg. The sun  altitude  is -35.6 deg. 

The galactic latitude b = 86 deg., longitude l = 303 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1853598

We obtain a following upper limits.  

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

    4595 |         MASTER-Amur |   C |   180 | 14.5 |        
    5133 |         MASTER-Amur |   C |    60 | 15.0 |        
    5353 |         MASTER-Amur |   C |   180 | 15.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220117B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31492
SUBJECT: GRB 220117B: z-band limit
DATE:    22/01/18 21:55:44 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

A. Rossi (INAF/OAS), J. Palmerio (CNRS, GEPI - Paris Observatory), D. B. 
Malesani (Radboud Univ. and DAWN/NBI), N. R. Tanvir (Univ. Leicester), 
D. A. Kann (IAA/CSIC) report on behalf of the Stargate collaboration:

We observed the field of GRB 220117B (Melandri et al., GCN 31468) using 
the acquisition camera of the X-shooter spectrograph, mounted on the ESO 
VLT UT3 (Melipal). A single z-band image (120 s exposure time) is 
available to us, taken approximately on January 18.2 UT (about 8.3 hr 
after the GRB).

Inside the XRT position (Evans et al., GCN 31473), we detect no source 
down to a limiting magnitude z > 21.5 mag (AB, 3 sigma limit).

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Michael Abdul-Masih, Diego Parraguez, and 
Jonathan Smoker.


GRB_name: GRB220118A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31493
SUBJECT: GRB 220118A: MITSuME Akeno optical observation
DATE:    22/01/18 23:03:56 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

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

We observed the field of GRB 220118A(The Fermi GBM team GCN Circular
#31489, N. J. Klingler et al. GCN Circular #31490) with the optical
three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope Akeno. The observation started at 2022-01-18 18:21:29 UT (51
sec after Swift BAT trigger). We stacked the images with good
conditions. We detected the optical afterglow candidate reported by
the Swift UVOT observation (N. J. Klingler et al. GCN Circular
#31490).
The magnitudes and the 5-sigma limits of the stacked images are as follows.

T0+[sec] MID-UT T-EXP[sec] magnitude(or 5-sigma limits) 5-sigma limits
-----------------------------------------------------------------------------------------------------------------
56   | 2022-01-18 18:21:34 | 10   |g'>15.9,         Rc>16.8,
Ic>16.8        | g'>15.9, Rc>16.8, Ic>16.8 |
84   | 2022-01-18 18:22:02 | 40   |g'=18.36+/-0.70, Rc=18.57+/-0.78,
Ic>17.5        | g'>17.3, Rc>17.9, Ic>17.5 |
171  | 2022-01-18 18:23:29 | 50   |g'=17.45+/-0.20, Rc=16.90+/-0.15,
Ic=17.12+/-0.41| g'>17.5, Rc>18.1, Ic>17.5 |
256  | 2022-01-18 18:24:54 | 60   |g'=17.31+/-0.18, Rc=16.87+/-0.09,
Ic=16.64+/-0.11| g'>17.7, Rc>18.5, Ic>18.1 |
325  | 2022-01-18 18:26:03 | 60   |g'=17.31+/-0.22, Rc=17.31+/-0.13,
Ic=17.08+/-0.15| g'>17.7, Rc>18.4, Ic>18.1 |
535  | 2022-01-18 18:29:33 | 300  |g'=18.21+/-0.17, Rc=17.80+/-0.10,
Ic=17.47+/-0.10| g'>18.7, Rc>19.5, Ic>19.1 |
1471 | 2022-01-18 18:45:09 | 1020 |g'=19.82+/-0.33, Rc=19.26+/-0.14,
Ic=18.81+/-0.15| g'>19.5, Rc>20.3, 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: GRB220118A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31495
SUBJECT: GRB 220118A: Enhanced Swift-XRT position
DATE:    22/01/19 10:09:15 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 300 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220118A, 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 = 192.26849, +22.91528 which is equivalent
to:

RA (J2000): 12h 49m 4.44s
Dec (J2000): +22d 54' 55.0"

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: GRB220118A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31496
SUBJECT: GRB 220118A: GIT optical observations
DATE:    22/01/19 11:29:04 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar(IITB), J. Stanzin (IAO), V. Bhalerao(IITB), G. C. Anupama(IIA), S.
Barway(IIA) report on behalf of the GIT team:

We observed GRB 220118A detected by Fermi-GBM (GCN #31489) and Swift-BAT (N.
J. Klingler et al., GCN #31490) with 0.7m GROWTH-India Telescope (GIT). We
obtained multiple 300-sec exposures in the g', r', i' and z' filters. We
detect a faint (~ 3.5 sigma) afterglow in our stacked images. The obtained
upper magnitudes and upper limits follow as:

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

 JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Mag(AB)/Lim_mag
(5-sigma)

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

2459598.2802666 | 0.38 | 300 | r' | > 17.23

2459598.2839984 | 0.47 | 300 | i' | > 17.78

2459598.2877512 | 0.56 | 300 | g' | > 17.38

2459598.2915685 | 0.65 | 300 | z' | > 16.99

2459598.3202152 | 1.34 | 3000(stacked) | r' | > 19.84

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

2459598.3568823 | 2.22 | 3000(stacked) | i' | 20.35 +/- 0.05

2459598.5042212 | 5.75 | 3000(stacked) | r' | 21.53 +/- 0.09

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

The detected magnitudes and upper limits are in agreement with R. Hosokawa
et al., (GCN #31493). The magnitudes are calibrated against PanSTARRS DR1
(Chambers et al., 2016) and not corrected for Galactic extinction.

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: GRB220118A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31498
SUBJECT: GRB 220118A: Swift/UVOT Detection
DATE:    22/01/19 17:27:54 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and N. J. Klingler (GSFC/UMBC/CRESSTII)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220118A
99 s after the BAT trigger (Klingler et al., GCN Circ. 31490).
A fading source consistent with the XRT position
(Goad et al., GCN Circ. 31495) is detected in the initial
UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  12:49:04.52 = 192.26885 (deg.)
    Dec (J2000) = +22:54:56.2  =  22.91562 (deg.)
with an estimated uncertainty of 0.44 arc sec. (radius, 90% confidence).

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

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

wh                 119          268          145      17.73+/-0.07
wh               11382        11797          404            >20.26
u                  276          454          175      17.33+/-0.12
b                10470        11377          885            >20.56


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.025 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220118A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31499
SUBJECT: GRB 220118A: Swift-BAT refined analysis
DATE:    22/01/19 21:02:06 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
N. J. Klingler (GSFC/UMBC/CRESSTII), 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+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220118A (trigger #1093742)
(Klingler et al., GCN Circ. 31490).  The BAT ground-calculated position is
RA, Dec = 192.277, 22.911 deg which is
   RA(J2000)  =  12h 49m 06.4s
   Dec(J2000) = +22d 54' 37.8"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 22%.

The mask-weighted light curve shows a single-peaked structure that
starts at ~T-4 s, peaks at ~T+1 s, and ends at ~T+10 s.
T90 (15-350 keV) is 10.61 +- 1.78 sec (estimated error including
systematics).

The time-averaged spectrum from T-3.90 to T+9.54 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.67 +- 0.12.  The fluence in the 15-150 keV band
is 1.8 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from
T+0.68 sec in the 15-150 keV band is 3.3 +- 0.5 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1093742/BA/


GRB_name: GRB220117C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31501
SUBJECT: GRB 220117C: Swift/BAT-GUANO arcminute localization
DATE:    22/01/20 02:41:26 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 localize GRB 220117C onboard (T0:
2022-01-17T04:45:55 UTC, Fermi/GBM trigger #664087560).

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), confidently detects the burst in a 8.192 s analysis
time bin with a sqrt(TS) of 19.5.
Estimated T90 in the detector is 8.55+/-0.07 s (10-350 keV).

An arcminute localization is found with DeltaLLHOut of 96.3 and a
DeltaLLHPeak of 58.7.
Using the conventional BAT imaging technique, we find an SNR of 6.1 at
the same location.

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 = 286.457, +16.791 deg which is
   RA(J2000)  = 19h 05m 49.7s
   Dec(J2000) = +16d 47â€² 27.6â€³
with an estimated uncertainty of 2 arcmin.

The position is consistent with the Fermi/GBM localization.

No XRT/UVOT followup will take place (GCN 31500).
We encourage followup from other facilities.

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.


GRB_name: GRB220118A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31502
SUBJECT: GRB 220118A: NUTTelA-TAO / BSTI Early Optical Limits (Preliminary)
DATE:    22/01/20 08:11:17 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), K. Baigarin (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 
220118A 11 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 18:21:08 UT on 2022-01-18, 30 s after the BAT 
trigger. Observations were made in cloudy conditions starting at about 
25 deg. target altitude. No source consistent with the XRT (M.R. Goad et 
al., GCN Circ. 31495) was detected.  We report the following results:

start time    t-t0(s)  end time        ULi'       exposure_time (s)
------------    --------  ------------          ------ --------------------
18:21:08     30     18:22:08          15.3           60
18:22:32     114   18:25:02          16.0         150
18:25:02     264   18:27:32          16.4         150
18:27:32     414   18:30:02          17.2         150
18:30:02     564   18:32:32          17.4         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 following rows correspond to co-adds from a continuing series 
of 15 s exposures.  Calibration was done with the 4 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: GRB211221A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31503
SUBJECT: GRB 211221A: No V & R detection, KAO telescope
DATE:    22/01/20 13:50:20 GMT
FROM:    Ahmed Fouad at NRIAG  <ahmed.fouad@nriag.sci.eg>

Ahmed M. Fouad, Ali Takey & Yosry Azzam at KAO observatory, Egypt report:

The observation of GRB 211221A started on 2021-12-21 from 22:25:01 UT to
23:10:10 UT,
i.e. 1hr_36m_21s  to  2hr_21m_30s  after the BAT trigger (Evans et al. GCN
Circ. 31273).

No detection of the afterglow in the optical Bessel V & R bands consistent
with the XRT position,
the magnitude limit in the GRB field according to the faintest objects is V
= 22.92 & R = 22.15.
The instrumental magnitudes were computed using aperture photometry in
photutils (python package).


GRB_name: GRB220101A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31504
SUBJECT: GRB 220101A: KAO optical-R observation
DATE:    22/01/20 14:03:51 GMT
FROM:    Ahmed Fouad at NRIAG  <ahmed.fouad@nriag.sci.eg>

Ahmed M. Fouad (NRIAG), Ali Takey (NRIAG), Dia Fouda (NRIAG) and
Ola Ali  (NRIAG) report:

We observed the optical counterpart of GRB 220101A
(Tohuvavohu et al., GCN 31347; Arimoto et al., GCN 31350)
using 1.88-m telescope at the Kottamia Astronomical Observatory (KAO),
NRIAG, Egypt.

The source was visible at RA: 00:05:24.77, DEC: +31:46:08.7 ,
9.72 arc seconds from the XRT position.

We measured R-Bessel magnitude = 21.5 +/- 0.616
in a combined image of 3x90 seconds images taken at
17:10:00 UT on 3-Jan-2022, 60 hr after the BAT trigger.

Photometry was done based on the brightest 10 stars around the GRB in
a FoV = 8' x 8', selected from the USNO-A1.0 catalog.

The magnitude is not corrected for Galactic extinction
in the direction of the GRB.


GRB_name: GRB220118A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31505
SUBJECT: GRB 220118A: COATLI Optical Observations
DATE:    22/01/20 14:10:36 GMT
FROM:    Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada  <mpereyra@astro.unam.mx>

Margarita Pereyra (UNAM), Alan M. Watson (UNAM),  Nat Butler (ASU), Rosa L.
Becerra (UNAM), OcÃ©lotl LÃ³pez (UNAM), Diego GonzÃ¡lez (UNAM), Alexander
Kutyrev (GSFC), William H. Lee (UNAM), Eleonora Troja (GSFC) and Tzveti
Dimitrova (ASU) report:

We observed the field of GRB 220118A (Klingler et al., GCN Circ. 31490 ;
Fermi GBM Team, GCN Circ. 31489) with the COATLI 50-cm telescope and
interim imager at the Observatorio AstronÃ³mico Nacional on the Sierra de
San Pedro MÃ¡rtir (http://coatli.astroscu.unam.mx) from 2022-01-19 07:32 UTC
to 13:26 UTC (13.24 to 19.1 hours after the trigger), obtaining a total of
16215 seconds of exposure in the r filter.

We do not detect any uncataloged sources in the enhanced XRT error region
(Goad et al., GCN Circ. 31495) to a 3-sigma limit of r = 22.9, which
confirms the afterglow fading reported by the GTI and Swift/UVOT teams
(Kumar et al., GCN Circ. 31496; Belles et al., GCN Circ. 31498)

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

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


GRB_name: GRB220118A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31506
SUBJECT: GRB 220118A: Fermi GBM detection
DATE:    22/01/20 16:39:29 GMT
FROM:    Boyan A. Hristov at UAH  <bah0046@uah.edu>

Cori Fletcher (USRA) and C. Meegan (UAH) and Boyan A. Hristov
(UAH) report on behalf of the Fermi GBM Team:

"At 18:20:35.84 UT on 18 January 2022, the Fermi Gamma-Ray
Burst Monitor (GBM) triggered and located GRB 220118A
(trigger 664222840 / 220118764), which was also detected by
the Swift BAT/XRT (N. J. Klingler et al. 2022, GCN 31490) and
observed by SWIFT UVOT (A. Belles et al. 2022, GCN 31498).
The Fermi GBM Final Real-time Localization (GCN 31489) is
consistent with the Swift position.

The GBM light curve shows a single peak with a duration (T90)
of about 19 s (50-300 keV).  The time-averaged spectrum from
T0+0.003 s to T0+18.176 s is best fit by a power law function
with an exponential high-energy cutoff.  The power law index is
-1.08 +/- 0.09 and the cutoff energy, parameterized as Epeak,
is 148.30 +/- 17.50 keV.

The event fluence (10-1000 keV) in this time interval is
(3.017 +/- 0.182)E-06.  The 1-sec peak photon flux measured
starting from T0+3.39204 s in the 10-1000 keV band is
4.0 +/- 0.28 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: GRB220118A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31507
SUBJECT: GRB 220118A: 2.2m CAHA/CAFOS detections
DATE:    22/01/20 17:33:32 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), D. B. Malesani (Radboud Univ. and DAWN/NBI), 
A. de Ugarte Postigo (Obs. Cote d'Azur), C. C. Thoene (HETH/ASU CAS 
Ondrejov), M. Blazek (HETH), J. F. Agui Fernandez (HETH/IAA-CSIC), A. 
Guijarro, and A. Fernandez (both CAHA) report:

We observed the afterglow of GRB 220118A (Swift detection: Klingler et 
al., GCN #31490; Fermi/GBM Detection: Fletcher et al., GCN #31506; 
afterglow detections: Hosokawa et al., GCN #31493; Kumar et al., GCN 
#31496; Belles & Klingler, GCN #31498) with CAFOS, mounted on the 2.2 m 
telescope, at the Calar Alto Observatory (Almeria, Spain). The 
observation started at 01:09:11 UT on 19 January 2022 (6.81 hr after the 
GRB) and consisted of 10 x 150 s integrations in the r' band and 9 x 150 
s in the i' band. Observations were hampered by the Wolf Moon, but 
otherwise conditions were very good (1".1 seeing, very good 
transparency).

The afterglow is faintly detected in the stacked images in each filter. 
Against several Pan-STARRS stars, we measure:

r' = 22.40 +/- 0.18 mag at 0.29916 d after trigger, and

i' = 22.07 +/- 0.17 mag at 0.32064 d after trigger.

No further observations are planned.


GRB_name: GRB220117C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31508
SUBJECT: GRB 220117C: Fermi GBM Observation
DATE:    22/01/20 20:58:15 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

S. Lesage (UAH) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:

"At 04:45:55 UT on 17 January 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220117C (trigger 664087560/220117199)
which was also detected by Swift/BAT-GUANO (Raman et al. 2022, GCN 31501).
The Fermi GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 73 degrees.

The GBM light curve consists of multiple pulses with a duration (T90)
of about 115 s (10-1000 keV). The time-averaged spectrum
from T0-1.8 to T0+114.9 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is 0.1 +/- 0.3 and the cutoff energy,
parameterized as Epeak, is 82 +/- 6 keV.

The event fluence (10-1000 keV) in this time interval is
(4.6 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+4.7 s in the 10-1000 keV band is 6.4 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB220120A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31509
SUBJECT: GRB 220120A: Fermi GBM Final Localization
DATE:    22/01/20 22:40:12 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

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

At 14:51:55.92 UT on 20 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220120A (trigger 664383120 / 220120619).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 249.7, Dec = -45.6 (J2000 degrees, equivalent to J2000 16h 38m, -45d 36'), with a statistical uncertainty of 8.4 degrees.

The angle from the Fermi LAT boresight is 74.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220120619/quicklook/glg_skymap_all_bn220120619.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220120619/quicklook/glg_healpix_all_bn220120619.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220120619/quicklook/glg_lc_medres34_bn220120619.gif


GRB_name: GRB211226A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31510
SUBJECT: IPN triangulation of GRB 211226A
DATE:    22/01/21 13:31:08 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,

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

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

S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu
on behalf of the Swift-BAT team, 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 211226A
(AGILE/MCAL detection: Ursi et al., GCN Circ. 31309;
Swift/BAT-GUANO detection: Tohuvavohu et al., GCN Circ. 31313)
was detected by AGILE (MCAL), Swift (BAT), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and BepiColombo (MGNS)
at about 19540 s UT (05:25:40).
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:
   241.834 (16h 07m 20s) -31.406 (-31d 24' 20")
  Corners:
   242.222 (16h 08m 53s) -31.675 (-31d 40' 30")
   241.641 (16h 06m 34s) -31.445 (-31d 26' 41")
   241.450 (16h 05m 48s) -31.118 (-31d 07' 03")
   242.025 (16h 08m 06s) -31.364 (-31d 21' 50")
  ---------------------------------------------
The error box area is 424 sq. arcmin, and its maximum
dimension is 52 arcmin (the minimum one is 12 arcmin).
The Sun distance was 30 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB211226_T19539/IPN


GRB_name: GRB220117A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31511
SUBJECT: GRB 220117A: Konus-Wind detection and joint Konus-Wind + Swift-BAT spectral analysis
DATE:    22/01/21 15:54:26 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, A.Lysenko, A. Ridnaya, D. Svinkin, A. Tsvetkova,  M. Ulanov,
on behalf of the Konus-Wind team;
and A. Melandri (INAF-OAB), A.Y. Lien (U Tampa), D.M. Palmer (LANL), S.D. Barthelmy (GSFC),
on behalf of the Swift-BAT team, report:

The long GRB 220117A (Swift-BAT trigger #1093592, T0 = T0(BAT)= 16:18:51.546 UT:
Melandri et al. GCN 31466; Palmer et al., GCN 31485;
Fermi GBM Sub-Threshold Detection: Veres, GCN 31487)
was detected by Konus-Wind (KW) in the waiting mode.

A Bayesian block analysis of the KW waiting mode data in the 20-400 keV band
reveals a >10 sigma count rate increase over background in the interval
from ~T0+10 s to ~T0+50 s. No statistically significant
emission has been detected above 400 keV throughout the burst.
The KW light curve of this burst is available
at http://www.ioffe.ru/LEA/GRBs/GRB220117A/

To derive broad-band spectral parameters of this burst, we performed
a joint spectral analysis of the Swift/BAT data (15-150 keV) and
the KW 3-channel spectral data (20-1500 keV).
A fit to the time-averaged spectrum, measured from  T0+10.557 s to T0+48.829 s,
by a power law with an exponential cutoff (CPL) model gives a photon index
alpha = -1.14 (-0.32,+0.37), and Ep = 71 (-11,+17) keV, chi^2 = 65.0/ 58 dof.
The Band GRB function fits this spectrum equally well, with alpha = -1.04 (-0.40,+0.58),
Ep = 65 (-14,+20) keV, and beta = -2.59 (-7.41, +0.43), chi^2 = 64.7/57 dof.
A fit to a simple power law gives a photon index of 1.89 (-0.08, +0.09), chi^2 = 72.4/ 59 dof.

In the 15-1500 keV band, the total burst fluence, estimated from the Band model,
is (2.8 Â± 0.7)x10^-6 erg/cm^2, and the 2.944 s peak energy flux is (1.7 Â± 0.4)x10^-7 erg/cm^2/s.

Assuming the redshift z=4.961 (Palmero et al., GCN 31480)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the isotropic energy release E_iso to (1.26 Â± 0.31)x10^53 erg,
which is consistent with that estimated from the GBM detection (GCN 31487),
the isotropic peak luminosity L_iso to (4.5 Â± 1.2)x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum Ep,z to 387(-84,+120) keV.
With the obtained estimates, GRB 220117A lies inside 68% prediction bands
for both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW GRBs
with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021),
see http://www.ioffe.ru/LEA/GRBs/GRB220117A/GRB220117A_rest_frame.pdf


GRB_name: GRB220121B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31517
SUBJECT: GRB 220121B: GECAM detection
DATE:    22/01/22 13:41:24 GMT
FROM:    Chao Zheng at IHEP  <zhengchao97@ihep.ac.cn>

C. Zheng, S. L. Xiong, S. Xiao, Y. Q. Zhang,  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, 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 220121B, at 2022-01-21T02:07:37.100 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 multiple pulses
with a duration of about 15 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/multiLCvsE_tn220121_020737_v00.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 48.45 deg 
Dec: -23.96 deg
Err: 4.58 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.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: GRB220117B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31518
SUBJECT: GRB 220117B: TARGET optical upper limit
DATE:    22/01/23 08:06:29 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Koyanagi, K. Hasuda, T. Sakamoto (AGU)

We observed the field of GRB 220117B detected by Swift
(Melandri et al., GCN Circ. 31468) with The AGU Robotic
Gravitational-wave Electromagnetic Telescope (TARGET)
equipped with the Veloce RH200 (20 cm OTA) and the large
format CCD camera (ATK11000) located at the Machida field
of Aoyama Gakuin University. 18 images of 60 sec exposures
were taken in the R filter starting from January 17
20:08:41 (UT) about 3.2 minutes after the trigger and
stopped on January 17 20:41:42 (UT). We do not detect the
optical afterglow both in the individual images and the
stacked image at the enhanced XRT position (Evans, et al.
GCN Circ. 31473).  The estimated five sigma upper limit of
the combined image (total exposure of 1080 sec)
is ~15.3 mag using the USNO-B1 catalog.


GRB_name: GRB220118A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31519
SUBJECT: GRB 220118A: TARGET optical upper limit
DATE:    22/01/23 08:08:05 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Koyanagi, K. Hasuda, T. Sakamoto (AGU)

We observed the field of GRB 220118A detected by Swift
(Klingler et al., GCN Circ. 31490) with The AGU Robotic
Gravitational-wave Electromagnetic Telescope (TARGET)
equipped with the Veloce RH200 (20 cm OTA) and the large
format CCD camera (ATK11000) located at the Machida field
of Aoyama Gakuin University. 20 images of 60 sec exposures
were taken in the R filter starting from January 18
18:25:04 (UT) about 4.4 minutes after the trigger and
stopped on January 18 18:57:56 (UT). We do not detect the
optical afterglow both in the individual images and the
stacked image at the enhanced XRT position (Goad, et al.
GCN Circ. 31495).  The estimated five sigma upper limit of
the combined image (total exposure of 1200 sec)
is ~16.1 mag using the USNO-B1 catalog.


GRB_name: GRB220117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31520
SUBJECT: GRB 220117A: Terskol and AbAO optical upper limits
DATE:    22/01/23 16:24:09 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), I. Sokolov (INASAN, KIAM),  I. Izvekova (Institute of 
Physics of NAS, ICAMBR of NAS), A. Shein (INASAN), Y. Markus (Institute 
of Physics of NAS, ICAMBR NAS), Y. Markelov (KIAM), R. Ya. Inasaridze 
(AbAO), N. Pankov (HSE),   G. Butenko (ICAMBR NAS), S. Belkin (IKI, 
HSE), A. Pozanenko (IKI) report on behalf of GRB IKI:

We observed the field of GRB 220117A (Melandri et al., GCN 31466) also 
detected by Fermi GBM Sub-Threshold (Veres, GCN 31487), and Konus-Wind 
(Frederiks et al. GCN 31511)  with Zeiss-2000, Zeiss-600  and K-800 
telescopes of Terskol observatory and with AS-32 telescope of Abastumani 
observatory. Within the enhanced XRT  Swift-XRT error circle (Beardmore 
et al., GCN 31472) we did not find any optical source. In particular we 
do not find the afterglow reported by Nanshan/NEXT (Fu et al., GCN 
31467), VLT (Palmerio et al., GCN 31480), LCO (Strausbaugh et al., GCN 
31481). Preliminary  upper limits are following

Date UT start t-T0 Filter Exp. OT Err UL(3sigma) Telescope

2022-01-17 18:32:01 0.12671 R     90*60  n/d   n/d   19.3 Zeiss-600
2022-01-17 19:41:36 0.16134 R     19*180 n/d   n/d   20.5 Zeiss-2000
2022-01-17 20:53:30 0.20545 R     35*60  n/d   n/d   19.4 AS-32

The photometry is based on the nearby PS1 stars.


GRB_name: GRB220124A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31521
SUBJECT: GRB 220124A: AstroSat CZTI detection of a bright long GRB
DATE:    22/01/24 08:11:18 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), G. Waratkar (IITB), A. Suresh (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 the CIFT framework (Sharma et al., 2021,
JApA, 42, 73) showed detection of a long GRB 220124A.

The source, consisting of three distinct bursts, was clearly detected in
the 20-200 keV energy range. The strongest peak is at 2022-01-24
03:39:19.00 UT. The measured peak count rate associated with the burst
is 441 (+16, -17) cts/s above the background in the combined data of
four quadrants, with a total of 25670 (+1334, -1297) cts. The local mean
background count rate was 496 (+1, -1) cts/s. Using cumulative rates, we
measure a T90 of 231 (+4, -5) s.

All three bursts from the source were also clearly detected in the CsI
anticoincidence (Veto) detector in the 100-500 keV energy range. The
strongest peak is at 2022-01-24 03:39:24.32 UT. The measured peak count
rate is 6829 (+76, -81) cts/s above the background in the combined Veto
data of four quadrants, with a total of 362309 (+6293, -4918) cts. The
local mean background count rate was 16030 (+5, -11) cts/s. We measure a
T90 of 231 (+38, -2) s from the cumulative Veto light curve. 

We note that the burst has not been localised, and we cannot rule out an
association with any SGRs. The ASIMOV tool
(http://astrosat-ssc.iucaa.in:8080/ASIMOV/ASIMOV [1]) indicates that
other active missions were covering different parts of the sky, hence
confirmed non-detections from other missions can help localise the
source by inferring earth-occulted regions.

CZTI GRB detections are reported regularly on the payload site at
http://astrosat.iucaa.in/czti/?q=grb [2]. 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-ssc.iucaa.in:8080/ASIMOV/ASIMOV
[2] http://astrosat.iucaa.in/czti/?q=grb


GRB_name: GRB220117A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31522
SUBJECT: GRB 220117A, GROND observations
DATE:    22/01/24 11:56:35 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 220117A (Melandri et al., GCN
31466) with GROND mounted at the 2.2m MPG telescope at La Silla
Observatory (Chile).

Observations started at 02:55 UT on January 19, about 34.5 hr after the
GRB trigger. They were performed at an average seeing of 1.3 arcsec and at
an airmass of 1.0.

Inside the XRT error circle (Beardmore et al., GCN 31472),  the
reported optical transient (Palmerio et al., GCN 31480;  Strausbaugh
et al., GCN 31481) is not detected anymore down to the following upper
limits (AB mags; 3 sigma):

g' > 23.2,
r' > 23.4,
i' > 23.0,
J  > 21.4,
H  > 21.1,
K  > 19.3.

The given limits are derived based on calibrating the optical images
against the Pan-STARRS catalog and the JHK data against 2MASS stars.
We thank Sam Kim for excellent support and for performing the observations.


GRB_name: GRB220124A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31524
SUBJECT: GRB 220124A: GECAM detection
DATE:    22/01/25 14:48:59 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

J. C. Liu, S. L. Xiong, S. Xiao, Y. Q. Zhang,  C. Cai, P. Zhang, 
C. Y. Li, S. L. Xie, X. Y. Zhao, Y. Huang, X. Y. Song,
C. Zheng,  Y. Zhao, Z. W. Guo, 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 220124A, at 2022-01-24T03:37:38.200 UTC (denoted as T0)ï¼Œ
which was also observed by CALET/GBM(triggerID: 1327030648), 
AstroSAT/CZTI(GCN #31521).
 
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 240 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB220124ALC_.png.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 246.18 deg 
Dec: 42.29 deg
Err: 2.96 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/GRB_220124Aloc.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: GRB220124A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31525
SUBJECT: IPN triangulation of GRB 220124A
DATE:    22/01/25 15:07:51 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 HEND/Mars Odyssey team,

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

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

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

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

The long-duration GRB 220124A
(AstroSat-CZTI detection: Prasad et al., GCN Circ. 31521;
GECAM detection: Liu et al., GCN Circ. 31524)
has been detected by AstroSat (CZTI), Konus-Wind, Swift (BAT),
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), CALET (CGBM),
and GECAM-B (GRD) ,so far, at about 13058 s UT (03:37:38).
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:
   241.945 (16h 07m 47s) +41.979 (+41d 58' 45")
  Corners:
   244.220 (16h 16m 53s) +42.801 (+42d 48' 02")
   239.771 (15h 59m 05s) +41.164 (+41d 09' 51")
   239.711 (15h 58m 51s) +41.082 (+41d 04' 54")
   244.155 (16h 16m 37s) +42.723 (+42d 43' 23")
  ---------------------------------------------
The error box area is 678 sq. arcmin, and its maximum
dimension is 3.8 deg (the minimum one is 3.1 arcmin).
The Sun distance was 84 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB220124_T13059/IPN/

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


GRB_name: GRB220124A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31526
SUBJECT: Konus-Wind detection of GRB 220124A
DATE:    22/01/25 15:13:25 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220124A (AstroSat-CZTI  detection: Prasad et al., GCN Circ. 31521;
GECAM detection: Liu et al., GCN 31524;
IPN localization: Kozyrev et al., GCN 31525)
triggered Konus-Wind (KW) at T0=13059.043 s UT (03:37:39.043).

The burst light curve shows a series of bright, multi-peaked pulses,
which starts at ~T0-10 s and has a total duration of ~250 s.
The emission is seen up to ~10 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220124_T13059/

As observed by Konus-Wind, the burst had
a fluence of (2.0 Â± 0.2)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 40.512 s,
of (6.0 Â± 0.9)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+242.432 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 = -0.81 (-0.06,+0.07),
the high energy photon index beta = -2.64 (-0.36,+0.22),
the peak energy Ep = 262 (-18,+18) keV,
chi2 = 86/97 dof.

The spectrum near the peak count rate (measured from T0+39.168 s
to T0+44.544 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 = -0.75 (-0.09,+0.10),
the high energy photon index beta = -2.61 (-0.89,+0.31),
the peak energy Ep = 381 (-45,+53) keV,
chi2 = 109/91 dof.

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


GRB_name: GRB220127A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31528
SUBJECT: GRB 220127A: GECAM detection
DATE:    22/01/28 04:34:33 GMT
FROM:    Shenglun Xie at IHEP  <xiesl@ihep.ac.cn>

S. L. Xie, S. L. Xiong, S. Xiao, Y. Q. Zhang,  C. Cai, P. Zhang, 
C. Y. Li, J. C. Liu, X. Y. Zhao, Y. Huang, X. Y. Song,
C. Zheng,  Y. Zhao, Z. W. Guo, 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 220127A, at 2022-01-27T18:53:26.100 UTC (denoted as T0),
which was also observed by INTEGRAL/SPI-ACS(TrigID=9654), WIND-KONUS.
 
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 single pulse
with a duration of about 0.2 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/gecamb_lc_grd_all_combine_97008806.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 306.36 deg 
Dec: -44.3 deg
Err: 5.14 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_flt_97008806.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: GRB220129A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31530
SUBJECT: GRB 220129A: Fermi GBM Final Real-time Localization
DATE:    22/01/29 21:07:55 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 20:57:30 UT on 29 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220129A (trigger 665182655.40502 / 220129873).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 244.4, Dec = 2.9 (J2000 degrees, equivalent to J2000 16h 17m, 2d 53'), with a statistical uncertainty of 22.5 degrees.

The angle from the Fermi LAT boresight is 16.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220129873/quicklook/glg_skymap_all_bn220129873.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220129873/quicklook/glg_healpix_all_bn220129873.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220129873/quicklook/glg_lc_medres34_bn220129873.gif


GRB_name: GRB220129A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31531
SUBJECT: Fermi GRB 220129A: Global MASTER-Net observations report 
DATE:    22/01/30 00:45:34 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220129A ( Fermi GBM team, GCN 31530) errorbox  11830 sec after notice time and 11857 sec after trigger time at 2022-01-30 00:15:07 UT, with upper limit up to  17.0 mag. The observations began at zenith distance = 80 deg. The sun  altitude  is -46.0 deg. 

The galactic latitude b = 35 deg., longitude l = 16 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1864208

We obtain a following upper limits.  

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

   11887 | 2022-01-30 00:15:07 |   MASTER-Kislovodsk | (17h 35m 07.65s , +14d 09m 34.0s) |   C |    60 | 17.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220131A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31532
SUBJECT: GRB 220131A: Fermi GBM Final Real-time Localization
DATE:    22/01/31 05:50:49 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:40:28 UT on 31 Jan 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220131A (trigger 665300433.513374 / 220131236).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 75.6, Dec = -24.9 (J2000 degrees, equivalent to J2000 05h 02m, -24d 53'), with a statistical uncertainty of 5.2 degrees.

The angle from the Fermi LAT boresight is 20.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220131236/quicklook/glg_skymap_all_bn220131236.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220131236/quicklook/glg_healpix_all_bn220131236.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220131236/quicklook/glg_lc_medres34_bn220131236.gif


GRB_name: GRB220130A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31533
SUBJECT: GRB 220130A: GECAM detection
DATE:    22/01/31 08:33:43 GMT
FROM:    Zhao Yi at POLAR  <yizhao@ihep.ac.cn>

Y. Zhao, S. L. Xiong, J. C. Liu, Y. Q. Zhang, C. Y. Li, S. L. Xie, 
S. Xiao, C. Cai, P. Zhang, X. Y. Zhao, Y. Huang, X. Y. Song,
C. Zheng,  Y. Zhao, Z. W. Guo, 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 220130A, at 2022-01-30T23:15:59.600 UTC (denoted as T0),
which was also observed by INTEGRAL/SPI-ACS.
 
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 70 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB220130A_lc.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra:  356.8 deg 
Dec: -50.1 deg
Err:   3.3 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/GRB220130A_loc.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: GRB220131B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31534
SUBJECT: GRB 220131B: GECAM detection
DATE:    22/01/31 08:34:33 GMT
FROM:    Zhao Yi at POLAR  <yizhao@ihep.ac.cn>

Y. Zhao, S. L. Xiong, J. C. Liu, Y. Q. Zhang, C. Y. Li, S. L. Xie, 
S. Xiao, C. Cai, P. Zhang, X. Y. Zhao, Y. Huang, X. Y. Song,
C. Zheng,  Y. Zhao, Z. W. Guo, 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 220131B, at 2022-01-31T01:09:16.700 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 single pulse
with a duration of about 20 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB220131B_lc.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra:  304.6 deg 
Dec:   8.6 deg
Err:   3.2 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/GRB220131B_loc.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: GRB220131A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31535
SUBJECT: Fermi GRB 220131A: Global MASTER-Net observations report 
DATE:    22/01/31 15:30:11 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220131A ( Fermi GBM team, GCN 31532) errorbox  34431 sec after notice time and 34458 sec after trigger time at 2022-01-31 15:14:46 UT, with upper limit up to  16.1 mag. Observations started at twilight.  The observations began at zenith distance = 72 deg. The sun  altitude  is -10.1 deg. 

The galactic latitude b = -34 deg., longitude l = 226 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1865459

We obtain a following upper limits.  

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

     177 | 2022-01-31 05:43:10 |             MASTER- | (04h 59m 52.03s , -25d 04m 35.3s) |   C |    30 | 19.1 |        
     177 | 2022-01-31 05:43:10 |             MASTER- | (04h 59m 15.60s , -24d 36m 30.4s) |   C |    30 | 19.1 |        
     233 | 2022-01-31 05:44:01 |             MASTER- | (04h 59m 50.06s , -25d 03m 13.6s) |   C |    40 | 19.3 |        
     233 | 2022-01-31 05:44:01 |             MASTER- | (04h 59m 13.57s , -24d 35m 08.5s) |   C |    40 | 19.4 |        
     299 | 2022-01-31 05:45:02 |             MASTER- | (04h 59m 50.19s , -25d 04m 45.2s) |   C |    50 | 19.4 |        
     299 | 2022-01-31 05:45:02 |             MASTER- | (04h 59m 13.63s , -24d 36m 39.9s) |   C |    50 | 19.4 |        
     380 | 2022-01-31 05:46:13 |             MASTER- | (04h 59m 52.27s , -25d 03m 33.1s) |   C |    70 | 19.4 |        
     380 | 2022-01-31 05:46:13 |             MASTER- | (04h 59m 15.65s , -24d 35m 27.6s) |   C |    70 | 19.5 |        
     647 | 2022-01-31 05:50:15 |             MASTER- | (05h 02m 37.43s , -25d 08m 44.0s) |   C |   120 | 19.2 |        
     647 | 2022-01-31 05:50:15 |             MASTER- | (05h 02m 01.32s , -24d 40m 32.8s) |   C |   120 | 19.4 |        
     798 | 2022-01-31 05:52:36 |             MASTER- | (05h 02m 42.69s , -25d 09m 58.3s) |   C |   140 | 19.4 |        
     798 | 2022-01-31 05:52:36 |             MASTER- | (05h 02m 06.36s , -24d 41m 47.7s) |   C |   140 | 19.4 |        
     979 | 2022-01-31 05:55:17 |             MASTER- | (05h 02m 36.99s , -25d 11m 14.6s) |   C |   180 | 19.4 |        
     979 | 2022-01-31 05:55:17 |             MASTER- | (05h 02m 00.46s , -24d 43m 04.1s) |   C |   180 | 19.4 |        
    1181 | 2022-01-31 05:58:39 |             MASTER- | (05h 02m 44.33s , -25d 11m 28.1s) |   C |   180 | 19.4 |        
    1181 | 2022-01-31 05:58:39 |             MASTER- | (05h 02m 07.65s , -24d 43m 17.4s) |   C |   180 | 19.6 |        
   34488 | 2022-01-31 15:14:46 |   MASTER-Kislovodsk | (04h 57m 14.66s , -21d 49m 09.4s) |   C |    60 | 15.8 |        
   34568 | 2022-01-31 15:16:06 |   MASTER-Kislovodsk | (04h 48m 58.53s , -25d 37m 44.3s) |   C |    60 | 15.3 |        
   34889 | 2022-01-31 15:21:27 |   MASTER-Kislovodsk | (05h 05m 52.82s , -25d 38m 51.8s) |   C |    60 | 15.9 |        
   34969 | 2022-01-31 15:22:47 |   MASTER-Kislovodsk | (05h 05m 15.31s , -19d 30m 52.5s) |   C |    60 | 12.3 |        
   34969 | 2022-01-31 15:22:47 |   MASTER-Kislovodsk | (05h 09m 40.56s , -19d 55m 18.4s) |   C |    60 | 15.8 |        
   35050 | 2022-01-31 15:24:08 |   MASTER-Kislovodsk | (05h 01m 17.79s , -23d 44m 50.2s) |   C |    60 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220128A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31536
SUBJECT: IPN triangulation of GRB 220128A (long)
DATE:    22/01/31 17:40:47 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 HEND/Mars-Odyssey team,

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

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

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

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

The long-duration GRB 220128A
was detected by Konus-Wind, Swift (BAT), INTEGRAL (SPI-ACS),
and Mars-Odyssey (HEND) at about 11897 s UT (03:18:17).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   350.191 (23h 20m 46s) -49.734 (-49d 44' 02")
  Corners:
   349.616 (23h 18m 28s) -46.520 (-46d 31' 11")
   350.856 (23h 23m 25s) -52.699 (-52d 41' 57")
   350.687 (23h 22m 45s) -52.865 (-52d 51' 53")
   349.478 (23h 17m 55s) -46.702 (-46d 42' 08")
  ---------------------------------------------
The error box area is 2688 sq. arcmin, and its maximum
dimension is 6.38 deg (the minimum one is 7 arcmin).
The Sun distance was 42 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220128_T11896/IPN/

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


GRB_name: GRB220128A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31537
SUBJECT: Konus-Wind detection of GRB 220128A
DATE:    22/01/31 17:46:00 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220128A (IPN localization: Kozyrev et al., GCN 31536)
triggered Konus-Wind (KW) at T0=11896.619 s UT (03:18:16.619).

The burst light curve shows a multi-peaked structure,
which starts at ~T0-10 s and has a total duration of ~47 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/GRB220128_T11896/

As observed by Konus-Wind, the burst had
a fluence of (3.2 Â± 0.7)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 10.496 s,
of (5.9 Â± 1.1)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.92 (-0.18,+0.28),
the high energy photon index beta = -2.19 (-1.92,+0.32),
the peak energy Ep = 406 (-135,+174) keV,
chi2 = 88/97 dof.

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


GRB_name: GRB220130A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31538
SUBJECT: GRB 220130A: Fermi GBM Observation
DATE:    22/02/01 00:01:22 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

S. Lesage (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:

"At 23:14:35 UT on 30 January 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220130A (trigger 665277280/220130968)
which was also detected by GECAM (Y. Zhao, et al. 2022, GCN 31533).
The Fermi GBM on-ground location is consistent with the GECAM position.

The angle from the Fermi LAT boresight is 69 degrees.

The GBM light curve contains a small peak followed by a
larger emission episode with a duration (T90)
of about 61 s (10-1000 keV). The time-averaged spectrum
from T0-2.0 to T0+163.8 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.85 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 233 +/- 8 keV.

A Band function fits the spectrum equally well
with Epeak= 203 +/- 10 keV, alpha = -0.79 +/- 0.03 and beta = -2.4 +/- 0.1.

The event fluence (10-1000 keV) in this time interval is
(5.7 +/- 0.1)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+115.2 s in the 10-1000 keV band is 11.8 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB220128A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31539
SUBJECT: GRB 220128A: AstroSat CZTI detection
DATE:    22/02/01 16:15:59 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

V. Prasad (IUCAA), G. Waratkar (IITB), A. Suresh (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 220128A, which was
also detected by Konus-Wind (Frederiks et al. GCN 31537) with IPN
localization (Kozyrev et al., GCN 31536).

The source was 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 2022-01-28
03:18:22.65 UT. The measured peak count rate is 617 (+71, -81) cts/s
above the background in the combined Veto data of four quadrants, with a
total of 4281 (+424, -589) cts. The local mean background count rate was
1477 (+4, -4) cts/s. We measure a T90 of 26 (+4, -4) 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: GRB220201A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31540
SUBJECT: GRB 220201A: Fermi GBM Final Localization
DATE:    22/02/01 18:32:13 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

The Fermi Gamma-Ray Burst Monitor (GBM) team reports the detection of a
likely long GRB.

At 16:11:15.73 UT on 01 February 2022, the  triggered and located GRB
220201A (trigger 665424680 / 220201674).

The on-ground calculated location, using the GBM trigger data, is RA =
14.7, DEC = -38.7 (J2000 degrees, equivalent to +00h 59m, -38d 41'), with a
statistical uncertainty of 4.4 degrees.

The angle from the Fermi LAT boresight is 16 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220201674/quicklook/glg_skymap_all_bn220201674.png

The HEALPix FITS file, including the estimated localization systematic, can
be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220201674/quicklook/glg_healpix_all_bn220201674.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220201674/quicklook/glg_lc_medres34_bn220201674.gif


GRB_name: GRB220131B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31541
SUBJECT: GRB 220131B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/02/01 18:46:38 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 localize GRB 220131B onboard (T0: 2022-01-31T01:09:16.7
UTC, GECAM GCN 31534).

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 90 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 9.2 in a 2.048 s
analysis time bin.


NITRATES results are consistent with a burst coming from outside the coded
FOV, with DeltaLLHOut of 1.9. The best fit sky position from NITRATES is
consistent with the GECAM localization within the stated error (GCN 31534).

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: GRB211227A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31544
SUBJECT: GRB 211227A: Konus-Wind detection and joint Konus-Wind+Swift-BAT spectral analysis
DATE:    22/02/03 10:32:43 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, D. Frederiks, A.Lysenko, D. Svinkin,
A. Ridnaia, M. Ulanov (all Ioffe), and A.Y. Lien (U Tampa), report:

The long GRB 211227A (Swift-BAT detection:
Beardmore et al., GCN 31316; Lien et al., GCN 31326;
MAXI/GSC detection: Tominaga et al., GCN 31319;
CALET-GRBM detection: Cherry et al., GCN 31333),
T0 (BAT) = 23:32:06.867, was detected by Konus-Wind (KW)
in the waiting mode.

A Bayesian block analysis of the KW waiting mode data in 25-400 keV range
reveals two episodes with count rate excess >10 sigma over background.
The first one, lasting from ~T0-50 s to ~T0-10 s, is due to the solar
activity and is not associated with the GRB.
The second episode, from ~T0-1.5 s to ~T0+81 s, is consistent in time
with the BAT detection. It has a double-peaked structure,
with the first, narrow pulse peaking at ~T0, and the second,
more broad pulse - at ~T0 + 11 s.

To derive broad-band spectral parameters of this burst,
we performed a joint spectral analysis of the Swift/BAT data (15-150 keV)
and the KW 3-channel spectral data (25-1700 keV).

A fit to the time-averaged spectrum, measured from T0-1.540 s  to 
T0+83.836 s,
by the Band GRB function gives alpha = -1.34 (-0.08,+0.10),
beta = -2.26 (-1.11,+0.24), and Ep = 192 (-42,+45) keV; chi^2 = 48.5/ 57 
dof.

A fit to the spectrum near the peak KW count rate, measured from 
T0+10.236 s to T0+19.068 s,
by the Band function gives alpha = -1.09 (-0.07,+0.08), beta = -2.29 
(-0.11,+0.28),
and Ep = 374 (-70,+66) keV; chi^2 = 47.1/58 dof.

The spectrum of the short initial pulse, measured from T0-1.540 s to 
T0+4.348 s,
is well fit by a power law with an exponential cutoff (CPL), with
alpha = -1.56 (-0.06,+0.15) and Ep = 366 (-179,+1201) keV; chi^2 = 
49.3/59 dof.
Although the Band model fit to this spectrum is not constrained,
fixing beta to the value -2.26, obtained for the time-integrated spectrum,
gives alpha = -1.49 (-0.18, +0.24) and Ep = 240 (-116, +759) keV; chi^2 
= 49.0/59 dof.

In the 15-1500 keV band, the total burst fluence is 
2.60(-0.21,+0.21)x10^-5 erg/cm^2,
and the 64 ms peak energy flux is 2.0(-0.4,+0.4)x10^-6 erg/cm^2/s.

Assuming the redshift z=0.228 (Malesani et al., GCN 31324)
of the host galaxy candidate (Fu et al., GCN 31320),
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the isotropic energy release E_iso to 4.9(-0.4,+0,4)x10^51 erg,
the isotropic luminosity L_iso to 4.7(-1.0,+1,0)x10^50 erg/s,
and the rest-frame peak energies of the time-integrated and peak spectra
to 235(-51,+56) keV and 460 (-86, +81) keV, correspondingly.
With these values, GRB 211227A is consistent with the 90% prediction 
bands for the 'Amati'
relation and is an outlier in the 'Yonetoku' relation for the sample of  
 >300 long KW GRBs
with known redshifts (Tsvetkova et al., 2021, ApJ, 908, 83).
However, if we assume a higher burst redshift (z>0.5), GRB 211227A is 
consistent
with both 'Amati' and 'Yonetoku' relations,
see http://www.ioffe.ru/LEA/GRBs/GRB211227A/GRB211227A_rest_frame.pdf

All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.

The KW light curve of this burst is available at 
http://www.ioffe.ru/LEA/GRBs/GRB211227A/


GRB_name: GRB220130A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31548
SUBJECT: IPN triangulation of GRB 220130A
DATE:    22/02/04 22:57:14 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

A. 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 220130A
(GECAM detection: Zhao et al., GCN Circ. 31533;
Fermi-GBM detection: Lesage et al., GCN Circ. 31538)
was detected by Fermi (GBM trigger 665277280), GECAM-B (GRD),
Konus-Wind, and INTEGRAL (SPI-ACS) at about 83676 s UT (23:14:36).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
-----------------------
RA(2000)    Dec(2000)
    deg          deg
-----------------------
Corners:
    5.551      -47.554
  358.843      -46.178
  343.052      -61.567
  348.140      -66.257
------------------------
The error box area is 94.5 deg2, and its maximum
dimension is 19 deg (the minimum one is 4.9 deg).
The Sun distance was about 58 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi (GBM) and GECAM localizations.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220130_T83760/IPN/

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


GRB_name: GRB220203A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31549
SUBJECT: IPN triangulation of GRB 220203A (short)
DATE:    22/02/04 23:00:29 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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

and

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

The short-duration GRB 220203A
has been detected by Konus-Wind, INTEGRAL (SPI-ACS), and
Swift (BAT), so far, at about 76530 s UT (21:15:30).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  -----------------------
  RA(2000)    Dec(2000)
     deg          deg
  -----------------------
  Corners:
   323.108        5.323
   301.728        6.767
   285.535       -7.425
   301.509        7.331
  ------------------------
The error box area is 28.4 deg2, and its maximum
dimension is 39.6 deg (the minimum one is 47.5 arcmin).
The Sun distance was about 16 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220203_T76534/IPN/

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


GRB_name: GRB220203A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31550
SUBJECT: GRB 220203A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/02/05 00:28:41 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 localize GRB 220203A onboard (T0: 2022-02-03T21:15:39.8 UTC,
INTEGRAL #9677, IPN GCN 31549).

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), detects the burst with a sqrt(TS) of 14.6 in a 0.256 s
analysis time bin.

The duration of the burst is ~0.3 seconds.

NITRATES results are consistent with a burst coming from outside the coded
FOV, with DeltaLLHOut of 4. An out of FOV origin is consistent with the IPN
localization (GCN 31549).

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: GRB220203A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31552
SUBJECT: GRB 220203A: GECAM detection
DATE:    22/02/05 14:58:40 GMT
FROM:    Zhao Yi at POLAR  <yizhao@ihep.ac.cn>

Z. W. Guo, Y. Zhao, S. L. Xiong, J. C. Liu, Y. Q. Zhang, C. Y. Li, S. L. Xie, 
S. Xiao, C. Cai, P. Zhang, X. Y. Zhao, Y. Huang, X. Y. Song,
C. Zheng,  Y. Zhao,  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 on ground by a short burst, 
GRB 220203A, at 2022-02-03T21:15:39.750 UTC (denoted as T0), which has been 
detected by Konus-Wind, INTEGRAL/SPI-ACS, and Swift/BAT.

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 multiple pulses
with a duration of about 0.3 s.

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB220203A_lc.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra:  316.4 deg 
Dec:   11.9 deg
Err:   13.3 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.
This position is consistent with the IPN localization (GCN 31549) within the error.

The GECAM preliminary location could be found here:  
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/GRB220203A_loc.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: GRB220203A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31553
SUBJECT: Konus-Wind detection of GRB 220203A
DATE:    22/02/05 15:37:19 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The short-duration GRB 220203A
(IPN triangulation: Svinkin et al., GCN Circ. 31549;
Swift/BAT-GUANO detection: Tohuvavohu et al., GCN Circ. 31550;
GECAM detection: Guo et al., GCN Circ. 31552)
triggered Konus-Wind at T0=76534.783 s UT (21:15:34.783).

The burst light curve shows a multi-peaked structure
which starts at ~T0-0.1 s and has a total duration of ~0.3 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/GRB220203_T76534/

As observed by Konus-Wind, the burst
had a fluence of 1.02(-0.26,+0.38)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.072 s,
of 8.81(-3.98,+5.24)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+0.256 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.60(-0.52,+0.87)
and Ep = 408(-159,+377) keV (chi2 = 7/18 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.9
(chi2 = 8/17 dof).

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


GRB_name: GRB220130A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31555
SUBJECT: Konus-Wind detection of GRB 220130A
DATE:    22/02/06 12:47:42 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220130A (GECAM detection: Zhao et al., GCN Circ. 31533;
Fermi-GBM detection: Lesage et al., GCN Circ. 31538;
IPN localization: Svinkin et al., GCN 31548)
triggered Konus-Wind (KW) at T0=83760.565 s UT (23:16:00.565).

The burst light curve shows a weak emission episode in the interval
from ~T0-90 s to ~T0-50 s, followed by a bright, multi-peaked pulse,
which starts at ~T0-40 s and has a total duration of ~130 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/GRB220130_T83760/

As observed by Konus-Wind, the burst had
a fluence of (7.6 Â± 1.2)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 13.824 s,
of (4.9 Â± 1.2)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+98.560 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 = -0.74 (-0.13,+0.15),
the high energy photon index beta = -2.50 (-0.53,+0.25),
the peak energy Ep = 236 (-25,+28) keV,
chi2 = 89/97 dof.

The spectrum near the peak count rate (measured from T0+8.448 s
to T0+16.640 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 = -0.78 (-0.14,+0.22),
the high energy photon index beta = -2.59 (-0.70,+0.34),
the peak energy Ep = 397 (-95,+86) keV,
chi2 = 110/97 dof.

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


GRB_name: GRB220209A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31561
SUBJECT: GRB 220209A: Fermi GBM Final Real-time Localization
DATE:    22/02/09 23:11:06 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 23:00:50 UT on 9 Feb 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220209A (trigger 666140455.423452 / 220209959).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 352.3, Dec = 72.0 (J2000 degrees, equivalent to J2000 23h 29m, 72d 00'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 62.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220209959/quicklook/glg_skymap_all_bn220209959.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220209959/quicklook/glg_healpix_all_bn220209959.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220209959/quicklook/glg_lc_medres34_bn220209959.gif


GRB_name: GRB220209A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31562
SUBJECT: Fermi GRB 220209A: Global MASTER-Net observations report 
DATE:    22/02/10 10:00:18 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220209A ( Fermi GBM team, GCN 31561) errorbox  28670 sec after notice time and 28704 sec after trigger time at 2022-02-10 06:59:14 UT, with upper limit up to  13.9 mag. Observations started at twilight.  The observations began at zenith distance = 75 deg. The sun  altitude  is -10.6 deg. 

MASTER-Amur robotic telescope  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 220209A errorbox  38592 sec after notice time and 38625 sec after trigger time at 2022-02-10 09:44:35 UT, with upper limit up to  14.6 mag. Observations started at twilight.  The observations began at zenith distance = 37 deg. The sun  altitude  is -10.9 deg. 

The galactic latitude b = 10 deg., longitude l = 117 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1876477

We obtain a following upper limits.  

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

   28734 | 2022-02-10 06:59:14 |          MASTER-IAC | (23h 47m 25.56s , +69d 30m 47.3s) |   C |    60 | 13.9 |        
   38656 | 2022-02-10 09:44:35 |         MASTER-Amur | (23h 01m 26.56s , +71d 09m 13.9s) |   C |    60 | 14.3 |        
   38735 | 2022-02-10 09:45:55 |         MASTER-Amur | (23h 26m 44.90s , +71d 10m 06.6s) |   C |    60 | 14.6 |        
   38815 | 2022-02-10 09:47:15 |         MASTER-Amur | (23h 49m 22.42s , +71d 09m 55.0s) |   C |    60 | 14.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220209A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31563
SUBJECT: GRB 220209A: AGILE/MCAL detection
DATE:    22/02/10 11:25:15 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), A. Di Piano (INAF/OAS-Bologna), 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), F. Lucarelli (SSDC, and INAF/OAR), A.
Bulgarelli, V. Fioretti, F. Fuschino, N. Parmiggiani (INAF/OAS-Bologna), M.
Marisaldi (INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois
(INAF/OA-Cagliari), I. Donnarumma (ASI), A. Giuliani (INAF/IASF-Mi), F.
Longo (Univ. Trieste and INFN Trieste), and P. Tempesta (TeleSpazio),
report on behalf of the AGILE Team:

The AGILE satellite detected the long GRB 220209A at T0 = 2022-02-09
23:00:58.72 +/- 0.01 s (UTC), reported by Fermi GBM (GCN #31561).

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 T90 = 14.5 +/-
0.5 s (in the 0.4-100 MeV energy range) and it released a total number of
2230 counts in the SA detector (above a background rate of 80 Hz), 25480
counts in the MCAL detector (above a background rate of 1110 Hz), and 48110
counts in the AC detector (above a background rate of 3015 Hz). The AGILE
ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/GRB220209A_AGILE_RM.png .

The event also triggered a high time resolution MCAL data acquisition, and
released 13500 counts in the detector, above a background rate of 525 Hz.
The time-integrated spectrum of the burst, from T0-2 s to T0+13 s, can be
fitted in the energy range 0.4-10 MeV with a Band model with alpha = -0.29
(-0.15/+0.11), beta = -2.50 (-0.23,+0.25), and Ep = 2.06 (-1.94,+2.38) MeV,
resulting in a reduced chi-squared of 1.42 (46 d.o.f.) and a fluence of
4.45e-05 erg/cm^2 (90% confidence level), in the same energy range. The
MCAL light curve can be found at
http://www.agilescienceapp.it/notices/076934_GRB_571532458.721385.png and
the best-fit spectrum can be found at
http://www.agilescienceapp.it/notices/GRB220209A_MCALsp.png . At the T0,
the event was 12 deg off-axis.


At T0+192 s, we notice another bursting episode, possibly related to GRB
220209A, and also visible in the Fermi GBM public light curves. This
episode lasted about 30 s and released a total number of 3610 counts in the
SA detector (above a background rate of 140 Hz), 38820 counts in the MCAL
detector (above a background rate of 1135 Hz), and 108520 counts in the AC
detector (above a background rate of 4160 Hz). This episode also triggered
a second partial high time resolution MCAL data acquisition, and released
6875 counts in the detector, above a background rate of 535 Hz. Assuming
that this event belongs to GRB 220209A, the time-integrated spectrum from
T0+187 s to T0+197 s can be fitted in the energy range 0.4-5 MeV with a
power-law with ph.ind. = -2.62 (-0.17,+0.19), resulting in a reduced
chi-squared of 1.33 (36 d.o.f.) and a fluence of 1.38e-05 erg/cm^2 (90%
confidence level), in the same energy range. At T0+192 s, the event was 140
deg 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: GRB220209A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31564
SUBJECT: GRB 220209A: GECAM detection
DATE:    22/02/10 15:26:50 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 220209A, at 2022-02-09T23:00:59.200 UTC (denoted as T0), which was also 
observed by Fermi/GBM (GCN #31561) and AGILE/MCAL (GCN #31563).
 
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 30 s. 

The GECAM light curve could be found here:
http://twiki.ihep.ac.cn/pub/GECAM/GRBList/multiLCvsE_2022-02-09T23_00_59.150.png

Using the automatic on-ground localization pipeline with the BDS alert data, 
GECAM-B localized this burst to the following position (J2000): 
Ra: 355.5 deg 
Dec: 65.3 deg
Err: 3.9 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.

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: GRB220209A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31565
SUBJECT: GRB 220209A: Fermi GBM Detection
DATE:    22/02/10 16:40:22 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

S. Lesage (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:

"At 23:00:50 UT on 09 February 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220209A (trigger 666140455/220209959)
which was also detected by AGILE (A. Ursi, et al. 2022, GCN 31563)
and GECAM (Y. Q. Zhang, et al. 2022, GCN 31564).
The Fermi GBM Final Real-time Localization (GCN 31561) is
consistent with the GECAM position.

The GBM light curve shows two bright emission episodes
with a duration (T90) of about 201 s (10-1000 keV).

The time-averaged spectrum for the first emission episode
from T0+7.2 to T0+51.2 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.92 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 1097 +/- 118 keV.
The event fluence (10-1000 keV) in this time interval is
(3.48 +/- 0.05)E-05 erg/cm^2.

The time-averaged spectrum for the second emission episode
from T0+159.7 to T0+220.2 s is also best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.95 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 307 +/- 12 keV.
The event fluence (10-1000 keV) in this time interval is
(2.6 +/- 0.04)E-05 erg/cm^2.

The 1-sec peak photon flux measured starting from T0+198.3 s
in the 10-1000 keV band is 17.8 +/- 0.4 ph/s/cm^2.

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

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


GRB_name: GRB210919A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31566
SUBJECT: GRB 210919A: SPI-ACS/INTEGRAL observation and evaluation of Ep
DATE:    22/02/10 18:14:13 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 investigated SPI-ACS/INTEGRAL data of GRB 210919A detected by Swift 
(Tohuvavohu et al. GCN 30846).  GRB 210919A was not triggered by IBAS at 
INTEGRAL observatory. We find the burst in SPI-ACS/INTEGRAL data with a 
significance of 5 sigma and duration of 0.15 s. The total count fluence 
of the burst is 900 Â± 185 counts, which corresponds to the fluence of 
2.4e-7 erg/cm^2 in 10-1000 keV energy band (the 95% confidence region is 
7.2e-8 -- 8.4e-7 erg/cm^2, incl. systematics). We do not find both 
precursor and extended emission components for the burst. Light curve of 
GRB 210919A can be found in

http://grb.rssi.ru/GRB210919A/GRB210919A_SPI-ACS_light_curve.png

Using spectral data of BAT/Swift (Barthelmy et al. GCN 30863) and 
possible redshift of z = 0.2411 (Rossi et al. GCN 31453) we estimated 
Eiso = (1.3 Â± 0.3)e49 erg in 15-150 keV energy band. Although spectral 
parameter Ep was not constrained yet, we can estimate Ep using T90,i - 
EH diagram [1] by constructing a trajectory depending on the Ep,i 
parameter, where Ep,i is Ep in a rest frame. The most probable value is 
found to be Ep,i = 90 keV with 95% confidence region of (14 â€“ 640) keV 
which is converted into observable Ep = 73 (11 --  516) keV. Since GRB 
210919A was detected by SPI-ACS with a nominal lower threshold of >80 
keV, Ep can be further limited to the energy range of 80 - 516 keV.

The T90,i - EH diagram can be found in

http://grb.rssi.ru/GRB210919A/GRB210919A_EHD.png

[1] - Minaev et al., MNRAS, 492, 1919, 2020


GRB_name: GRB210919A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31567
SUBJECT: GRB 210919A: Maidanak optical observations
DATE:    22/02/10 18:18:46 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (HSE, IKI), A. Pozanenko (IKI), S. Belkin (IKI, HSE), O. 
Burhonov (UBAI),  Sh. Ehgamberdiev (UBAI) report on behalf of GRB IKI FuN:

We observed the filed of GRB 210919A detected by Swift (Tohuvavohu et 
al. GCN 30846) with AZT-22 1.5m telescope of Maidanak observatory on 
Sep. 19, and 20, 2021. Within enhanced Swift-XRT position (Goad et al. 
GNC 30850) we do not detect the potential afterglow (Kann et al. GCN 
30883, 30884) in both epochs. In the deep observation on 2021-09-19 with 
a mean seeing of 1" we  marginally detected the host galaxy candidate 
reported by O'Connor et al. (GCN 30934) and Kann et al. (GCN 30983) at 
the redshift of z=0.2411 (Rossi et al. GCN 31453). Using aperture 
photometry we found R = 24.05 +/- 0.35 of the host galaxy candidate. We 
do not detect the source at the eastern edge of the XRT error circle 
reported by  Kann et al. (GCN 30983).

Preliminary photometry of the field in following

Date       UT start  t-T0      Filter Exp.   OT  Err.  UL(3sigma)
                      (mid, days)        (s)
2021-09-19 22:27:50   0.94950    R    32*180 n/d n/d 24.2
2021-09-20 23:04:55   1.95651    R    14*180 n/d n/d 22.9

The photometry is based on the nearby SDSS-DR12 stars, R magnitude 
calculated by Lupton' transformations.


GRB_name: GRB220210A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31568
SUBJECT: GRB 220210A: Fermi GBM Final Real-time Localization
DATE:    22/02/11 00:07:02 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 23:56:38 UT on 10 Feb 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220210A (trigger 666230203.371058 / 220210998).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 7.9, Dec = 61.5 (J2000 degrees, equivalent to J2000 00h 31m, 61d 30'), with a statistical uncertainty of 5.0 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/2022/bn220210998/quicklook/glg_skymap_all_bn220210998.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220210998/quicklook/glg_healpix_all_bn220210998.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220210998/quicklook/glg_lc_medres34_bn220210998.gif


GRB_name: GRB220210A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31569
SUBJECT: Fermi GRB 220210A: Global MASTER-Net observations report 
DATE:    22/02/11 00:15:18 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220210A ( Fermi GBM team, GCN 31568) errorbox  552 sec after notice time and 587 sec after trigger time at 2022-02-11 00:06:25 UT, with upper limit up to  16.7 mag. The observations began at zenith distance = 78 deg. The sun  altitude  is -68.6 deg. 

The galactic latitude b = -1 deg., longitude l = 121 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1878625

We obtain a following upper limits.  

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

     647 | 2022-02-11 00:06:25 |          MASTER-IAC | (00h 31m 39.20s , +61d 20m 50.9s) |  P| |   120 | 16.7 |        
     647 | 2022-02-11 00:06:25 |          MASTER-IAC | (00h 30m 02.27s , +61d 27m 11.3s) |  P- |   120 | 16.1 |        


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


GRB_name: GRB220211A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31570
SUBJECT: GRB 220211A: Fermi GBM Final Real-time Localization
DATE:    22/02/11 01:18:13 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 01:07:48 UT on 11 Feb 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220211A (trigger 666234473.877152 / 220211047).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 207.2, Dec = 40.0 (J2000 degrees, equivalent to J2000 13h 48m, 40d 00'), with a statistical uncertainty of 8.7 degrees.

The angle from the Fermi LAT boresight is 145.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220211047/quicklook/glg_skymap_all_bn220211047.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220211047/quicklook/glg_healpix_all_bn220211047.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220211047/quicklook/glg_lc_medres34_bn220211047.gif


GRB_name: GRB220211A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31571
SUBJECT: Fermi GRB 220211A: Global MASTER-Net observations report 
DATE:    22/02/11 01:30:21 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220211A ( Fermi GBM team, GCN 31570) errorbox  33 sec after notice time and 64 sec after trigger time at 2022-02-11 01:08:53 UT, with upper limit up to  17.6 mag. The observations began at zenith distance = 53 deg. The sun  altitude  is -76.1 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 220211A errorbox  54 sec after notice time and 85 sec after trigger time at 2022-02-11 01:09:14 UT, with upper limit up to  18.0 mag. The observations began at zenith distance =  6 deg. The sun  altitude  is -34.3 deg. 

The galactic latitude b = 72 deg., longitude l = 82 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1878703

We obtain a following upper limits.  

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

      69 | 2022-02-11 01:08:53 |          MASTER-IAC | (13h 46m 25.74s , +40d 09m 02.1s) |  P| |    10 | 15.9 |        
      69 | 2022-02-11 01:08:53 |          MASTER-IAC | (13h 47m 33.50s , +40d 02m 18.2s) |  P- |    10 | 16.0 |        
      95 | 2022-02-11 01:09:14 |   MASTER-Kislovodsk | (13h 47m 31.06s , +40d 10m 14.0s) |   C |    20 | 16.2 |        
      95 | 2022-02-11 01:09:14 |   MASTER-Kislovodsk | (13h 53m 25.68s , +39d 46m 25.9s) |   C |    20 | 15.6 |        
     105 | 2022-02-11 01:09:23 |          MASTER-IAC | (13h 47m 38.91s , +40d 01m 15.3s) |  P- |    20 | 16.6 |        
     105 | 2022-02-11 01:09:23 |          MASTER-IAC | (13h 46m 31.14s , +40d 07m 59.6s) |  P| |    20 | 16.9 |        
     135 | 2022-02-11 01:09:54 |   MASTER-Kislovodsk | (13h 47m 30.69s , +40d 11m 15.9s) |   C |    20 | 17.1 |        
     170 | 2022-02-11 01:09:54 |   MASTER-Kislovodsk | (13h 47m 30.71s , +40d 11m 15.7s) |   C |    90 | 18.0 |  Coadd 
     135 | 2022-02-11 01:09:54 |   MASTER-Kislovodsk | (13h 53m 25.53s , +39d 47m 27.9s) |   C |    20 | 15.9 |        
     151 | 2022-02-11 01:10:04 |          MASTER-IAC | (13h 46m 25.35s , +40d 06m 57.5s) |  P| |    30 | 17.2 |        
     151 | 2022-02-11 01:10:04 |          MASTER-IAC | (13h 47m 33.09s , +40d 00m 12.7s) |  P- |    30 | 16.5 |        
     180 | 2022-02-11 01:10:34 |   MASTER-Kislovodsk | (13h 47m 36.70s , +40d 10m 16.5s) |   C |    30 | 17.4 |        
     180 | 2022-02-11 01:10:34 |   MASTER-Kislovodsk | (13h 53m 31.51s , +39d 46m 30.2s) |   C |    30 | 16.0 |        
     206 | 2022-02-11 01:10:54 |          MASTER-IAC | (13h 46m 31.49s , +40d 07m 24.1s) |  P| |    40 | 17.4 |        
     206 | 2022-02-11 01:10:54 |          MASTER-IAC | (13h 47m 39.21s , +40d 00m 38.6s) |  P- |    40 | 17.0 |        
     235 | 2022-02-11 01:11:24 |   MASTER-Kislovodsk | (13h 47m 30.48s , +40d 09m 18.4s) |   C |    40 | 17.4 |        
     235 | 2022-02-11 01:11:24 |   MASTER-Kislovodsk | (13h 53m 25.29s , +39d 45m 33.1s) |   C |    40 | 16.3 |        
     270 | 2022-02-11 01:11:54 |          MASTER-IAC | (13h 46m 28.24s , +40d 08m 38.5s) |  P| |    50 | 17.5 |        
     270 | 2022-02-11 01:11:54 |          MASTER-IAC | (13h 47m 35.97s , +40d 01m 52.2s) |  P- |    50 | 17.1 |        
     300 | 2022-02-11 01:12:24 |   MASTER-Kislovodsk | (13h 47m 36.57s , +40d 09m 24.1s) |   C |    50 | 16.9 |        
     300 | 2022-02-11 01:12:24 |   MASTER-Kislovodsk | (13h 53m 31.46s , +39d 45m 39.3s) |   C |    50 | 16.0 |        
     345 | 2022-02-11 01:13:04 |          MASTER-IAC | (13h 46m 28.28s , +40d 06m 54.9s) |  P| |    60 | 17.6 |        
     345 | 2022-02-11 01:13:04 |          MASTER-IAC | (13h 47m 35.89s , +40d 00m 08.0s) |  P- |    60 | 17.2 |        
     380 | 2022-02-11 01:13:34 |   MASTER-Kislovodsk | (13h 47m 34.24s , +40d 10m 51.1s) |   C |    70 | 17.7 |        
     380 | 2022-02-11 01:13:34 |   MASTER-Kislovodsk | (13h 53m 29.36s , +39d 47m 07.7s) |   C |    70 | 16.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220210A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31572
SUBJECT: GRB 220210A: Swift/BAT-GUANO localization
DATE:    22/02/11 04:27:48 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 220210A onboard (T0: 2022-02-10T23:56:38
 UTC, Fermi/GBM GCN 31568, CALET trig 1328572556).

The Fermi and CALET 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, 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 GRB is clearly detected in the BAT data, with a duration of ~15 seconds.
A location for the burst is found with conventional BAT imaging, with SNR 11.4.

While the derived location is precise to ~2 arcminute with respect to
the spacecraft pointing, the conversion to celestial coordinates is
complicated by the current operational mode of Swift (GCN 31500,
31547).

The BAT position is
RA, Dec = 345.778, +61.826 deg which is
   RA(J2000)  = 23h 03m 6.9s
   Dec(J2000) = +61d 49â€² 33.2â€³
with an estimated uncertainty of 2 arcmin with respect to the
spacecraft pointing.
The uncertainty in the Swift attitude in the current mode is believed
to be ~1-2 degrees (M. Ajello et al, 2008 ApJ 689, 666).

The position is consistent with the Fermi/GBM localization (GCN 31568).

NITRATES results are not yet available, and will be reported in a
future circular.

There will be no XRT/UVOT followup (GCN 31547).
We encourage followup from other instruments.

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.


GRB_name: GRB220210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31573
SUBJECT: GRB 220210A: BOOTES-5/JGT optical afterglow candidate
DATE:    22/02/11 05:26:21 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

I. M. Carrasco-Garcia (UMA), A. J. Castro-Tirado, M.D. Caballero-Garcia, 
Y.-D. Hu, T.-R. Sun, E. Fernandez-Garcia, R. Sanchez-Ramirez and I. 
Olivares (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), S. 
Castillo-Carrion and C. J. Perez del Pulgar (UMA) and I. H. Park (SKKU) 
on behalf of a larger collaboration, report:

The 60cm BOOTES-5/JGT robotic telescope at Observatorio Astronomico 
Nacional in San Pedro Martir (Mexico) observed the Swift/BAT-GUANO error 
box for GRB 220210A (Tohuvavohu et al., GCNC 31572) also detected by 
Fermi (The Fermi Team, GCNC 31568) starting at 04:35 UT (i.e. 4.6 h post 
burst). In the single clear images (60 s exposure), we find an 
uncataloged optical source at (J2000) coordinates RA: 23:03:17.1, 
DEC:+61:49:36.6 (+/- 1â€) within the Swift/BAT-GUANO error box and for 
which we measure a preliminary magnitude R = 18.5 mag. We propose this 
source to be the GRB 220210A optical afterglow, pending confirmation of 
its variability. Further multicolour observations are ongoing. 
Spectroscopic observations are encouraged.

We thank the staff at San Pedro Martir for their support.


GRB_name: GRB220210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31574
SUBJECT: GRB 220210A: BOOTES-5/JGT optical afterglow candidate discarded
DATE:    22/02/11 05:35:10 GMT
FROM:    Alberto J. Castro-Tirado at IAA-CSIC  <ajct@iaa.es>

I. M. Carrasco-Garcia (UMA) and A. J. Castro-Tirado (IAA-CSIC) on behalf of a larger collaboration, report:

The optical afterglow candidate reported in GCNC 31573 (Carrasco-Garcia et al.) is ruled out as it is detected in DDS-2 Infrared Survey and therefore is a highly reddened object unrelated to the GRB. We apologize for the inconveniences this may have caused. Further observations are still ongoing at San Pedro Martir reaching a limiting magnitude of 20.5.


GRB_name: GRB220210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31575
SUBJECT: GRB 220210A: AGILE detection
DATE:    22/02/11 11:44:38 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi, L. Foffano (INAF/IAPS), F. Verrecchia, C. Pittori (SSDC, and
INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M.
Cardillo, C. Casentini, Y. Evangelista, E. Menegoni, 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), A. Giuliani (INAF/IASF-Mi), F.
Longo (Univ. Trieste and INFN Trieste), and P. Tempesta (TeleSpazio),
report on behalf of the AGILE Team:

The AGILE satellite detected the long GRB 220210A at T0 = 2022-02-10
23:56:38.40 +/- 0.01 s (UTC), reported by Fermi GBM (GCN #31568) and Swift
BAT (GCN #31572).

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 1.9 s (in the 0.4-100 MeV energy range)
and it released a total number of 2110 counts in the MCAL detector (above a
background rate of 1230 Hz), and 3910 counts in the AC detector (above a
background rate of 3330 Hz). The AGILE ratemeters light curves can be found
at http://www.agilescienceapp.it/notices/GRB220210A_AGILE_RM.png .

The event also triggered a high time resolution MCAL data acquisition,
which released 1440 counts in the detector, above a background rate of 505
Hz. The time-integrated spectrum of the burst, from T0-0.19 s to T0+1.73 s,
can be fitted in the energy range 0.4-5 MeV with a power-law with ph.ind. =
-1.81 (-0.19,+0.21), resulting in a reduced chi-squared of 1.18 (36 d.o.f.)
and a fluence of 3.40e-06 erg/cm^2 (90% confidence level), in the same
energy range. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/076950_GRB_571622198.404213.png . At
the T0, the event was 15 deg 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: GRB220210A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31576
SUBJECT: GRB 220210A: Fermi-LAT detection
DATE:    22/02/11 12:58:50 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

F. Longo (University and INFN, Trieste), F. Piron (CNRS/IN2P3/LUPM), M. Axelsson (KTH & Stockholm Univ.), M.Ohno (Hiroshima Univ. & Eotvos Univ.), E. Bissaldi (Politecnico and INFN, Bari) and N. Di Lalla (Stanford) report on behalf of the Fermi-LAT Collaboration:


On February 10th, 2022, Fermi-LAT detected high-energy emission from GRB 220210A,  which was also detected by Fermi-GBM  (GCN 31568) Swift/BAT-GUANO (GCN 31572) and AGILE (GCN 31575). The best LAT on-ground location is found to be


RA, Dec = 347.4, 61.1 (degrees, J2000)


with an error radius of 1.5 deg (90% containment, statistical error only).


This was 15 deg from the LAT boresight at the time of the GBM trigger:

T0 =  23:56:38 UT.


The data from the Fermi-LAT show a significant increase in the event rate after the GBM trigger that is temporally correlated with the GBM emission with high significance. The GRB has a very soft estimated photon index (above 50 MeV) of  -3.3 +/- 0.5 in the time interval 0-30 s after the GBM trigger. The corresponding estimated photon flux above 50 MeV is 3.8 +/- 1.4 E-5 ph/cm2/s. The highest-energy photon is a 190 MeV event which is observed 1 second after the GBM trigger.


The Fermi-LAT point of contact for this burst is Niccolo' di Lalla (niccolo.dilalla@stanford.edu)


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


GRB_name: GRB220209A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31577
SUBJECT: GRB 220209A: Fermi-LAT detection
DATE:    22/02/11 15:10:25 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

M. Pesce-Rollins (INFN Pisa), D. Horan (CNRS/IN2P3/LLR), F. Piron (CNRS/IN2P3/LUPM), M. Axelsson (KTH & Stockholm Univ.), F. Longo (University and INFN, Trieste), and N. Di Lalla (Stanford) report on behalf of the Fermi-LAT Collaboration:


On February 9th, 2022, Fermi-LAT detected high-energy emission from GRB 220209A, which was also detected by Fermi-GBM  (GCN 31561), GECAM (GCN 31564) and AGILE (GCN 31565).


The best LAT on-ground location is found to be


RA, Dec = 352.13, 73.11 (degrees, J2000)

with an error radius of 1.4 deg (90% containment, statistical error only).


This was 68 deg from the LAT boresight at the time of the GBM trigger:

T0 =  23:00:50  UT.


The data from the Fermi-LAT show a significant increase in the event rate about 10 s after the GBM trigger that is temporally correlated with the GBM emission with high significance. The GRB has a very soft estimated photon index (above 50 MeV) of  -4.7 +/- 0.7 in the time interval 0 - 20 s  after the GBM trigger. The corresponding estimated photon flux above 50 MeV is 1.1E-4 +/- 5.1E-5 ph/cm2/s. The highest-energy photon is a 200 MeV event which is observed 13 seconds after the GBM trigger.


The Fermi-LAT point of contact for this burst is Niccolo' di Lalla (niccolo.dilalla@stanford.edu<http://stanford.edu>).


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


GRB_name: GRB220211B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31578
SUBJECT: GRB 220211B: Fermi GBM Final Real-time Localization
DATE:    22/02/11 15:56:52 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 15:46:28 UT on 11 Feb 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220211B (trigger 666287193.962164 / 220211657).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 3.8, Dec = 46.2 (J2000 degrees, equivalent to J2000 00h 15m, 46d 12'), with a statistical uncertainty of 7.0 degrees.

The angle from the Fermi LAT boresight is 28.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220211657/quicklook/glg_skymap_all_bn220211657.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220211657/quicklook/glg_healpix_all_bn220211657.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220211657/quicklook/glg_lc_medres34_bn220211657.gif


GRB_name: GRB220211B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  31579
SUBJECT: Fermi GRB 220211B: Global MASTER-Net observations report 
DATE:    22/02/11 16:30:20 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),

B.L.Carrasco, J.R.Valdes,V.Chavushyan, C.J.Martinez, V.M.Patino Alvarez,
M.L.H.Rodriguez (INAOE, OAGH)

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 220211B ( Fermi GBM team, GCN 31578) errorbox  288 sec after notice time and 320 sec after trigger time at 2022-02-11 15:51:48 UT, with upper limit up to  16.9 mag. Observations started at twilight.  The observations began at zenith distance = 43 deg. The sun  altitude  is -14.3 deg. 

The galactic latitude b = -16 deg., longitude l = 117 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1879384

We obtain a following upper limits.  

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

     350 | 2022-02-11 15:51:48 |   MASTER-Kislovodsk | (00h 00m 04.54s , +44d 53m 56.1s) |   C |    60 | 16.8 |        
     350 | 2022-02-11 15:51:49 |   MASTER-Kislovodsk | (23h 53m 54.19s , +45d 16m 03.2s) |   C |    60 | 14.9 |        
     430 | 2022-02-11 15:53:09 |   MASTER-Kislovodsk | (00h 00m 04.28s , +43d 00m 53.6s) |   C |    60 | 16.7 |        
     430 | 2022-02-11 15:53:09 |   MASTER-Kislovodsk | (23h 54m 06.65s , +43d 23m 02.3s) |   C |    60 | 15.1 |        
    1713 | 2022-02-11 16:14:31 |   MASTER-Kislovodsk | (23h 59m 58.26s , +44d 52m 36.2s) |   C |    60 | 16.8 |        
    1713 | 2022-02-11 16:14:31 |   MASTER-Kislovodsk | (23h 53m 59.23s , +45d 14m 45.9s) |   C |    60 | 14.3 |        
    1793 | 2022-02-11 16:15:51 |   MASTER-Kislovodsk | (00h 00m 01.37s , +42d 59m 43.9s) |   C |    60 | 16.9 |        
    1793 | 2022-02-11 16:15:52 |   MASTER-Kislovodsk | (23h 54m 14.60s , +43d 21m 52.8s) |   C |    60 | 14.2 |        
Filter C is a clear (unfiltred) band. 


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


