# GCN_circulars

GRB_name: GRB221206A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33022
SUBJECT: GRB 221206A: Fermi GBM Final Real-time Localization
DATE:    22/12/06 11:19:21 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 11:07:27 UT on 6 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221206A (trigger 692017652.091436 / 221206464).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 244.1, Dec = -42.7 (J2000 degrees, equivalent to J2000 16h 16m, -42d 42'), with a statistical uncertainty of 4.7 degrees.

The angle from the Fermi LAT boresight is 42.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221206464/quicklook/glg_skymap_all_bn221206464.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/bn221206464/quicklook/glg_healpix_all_bn221206464.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221206464/quicklook/glg_lc_medres34_bn221206464.gif


GRB_name: GRB221206B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33023
SUBJECT: GRB 221206B: Fermi GBM Final Real-time Localization
DATE:    22/12/06 12:33:03 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 12:22:47 UT on 6 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221206B (trigger 692022172.359134 / 221206516).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 255.1, Dec = 44.5 (J2000 degrees, equivalent to J2000 17h 00m, 44d 30'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 129.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221206516/quicklook/glg_skymap_all_bn221206516.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/bn221206516/quicklook/glg_healpix_all_bn221206516.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221206516/quicklook/glg_lc_medres34_bn221206516.gif


GRB_name: GRB221206C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33024
SUBJECT: GRB 221206C: Fermi GBM Final Real-time Localization
DATE:    22/12/06 14:14:48 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 14:04:24 UT on 6 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221206C (trigger 692028269.2123 / 221206586).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 170.1, Dec = 56.8 (J2000 degrees, equivalent to J2000 11h 20m, 56d 47'), with a statistical uncertainty of 6.2 degrees.

The angle from the Fermi LAT boresight is 21.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221206586/quicklook/glg_skymap_all_bn221206586.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/bn221206586/quicklook/glg_healpix_all_bn221206586.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221206586/quicklook/glg_lc_medres34_bn221206586.gif


GRB_name: GRB221206B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33026
SUBJECT: GRB 221206B: Swift ToO observations
DATE:    22/12/06 20:22:07 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 221206B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021532

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: GRB221206B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33027
SUBJECT: GRB 221206B: Swift/BAT-GUANO candidate arcminute localization
DATE:    22/12/06 21:12:13 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not trigger on GRB 221206 (T0: 2022-12-06T12:22:47
UTC, Fermi/GBM GCN 33023).

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

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

The burst is detected in BAT with a duration of ~12 seconds.
The burst occurred during a Swift slew.
A candidate location for the burst was found with an SNR of 6.6.

The BAT position is
RA, Dec = 251.155, +42.671 deg which is
   RA(J2000)  = 16h 44m 37.13s
   Dec(J2000) =  +42d 40â€² 17.0â€³
with an estimated uncertainty of 4 arcmin.

This position is consistent with the Ferm/GBM localization (GCN 33023).
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: GRB221206B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33028
SUBJECT: GRB 221206B: Detection by GRBAlpha
DATE:    22/12/07 23:28:51 GMT
FROM:    Marianna Dafcikova at Masaryk University  <500025@mail.muni.cz>

M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal,  A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory),  T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Os
 aka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The long-duration GRB 221206B (Fermi/GBM detection: GCN Circ. 33023; Swift/BAT-GUANO detection: GCN Circ. 33027; Konus/Wind detection, trigger time at 2022-12-06 12:22:46.185 UT; INTEGRAL/SPI-ACS detection, peak time at ~2022-12-06 12:22:49 UT) was observed by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The detection was confirmed at the peak time 2022-12-06 12:22:49 UTC. The light curve observed by GRBAlpha shows a double-peak structure with a T90 duration of 8 s. The SNR during T90 reaches 36.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221206B_GCN.pdf

GRBAlpha is a demonstration mission for a future CubeSats constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. GRBAlpha was launched on 2021 March 22 from Baikonur. After its commissioning phase, the scientific observations are now under way. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.


GRB_name: GRB221206B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33029
SUBJECT: GRB 221206B: Swift-XRT observations
DATE:    22/12/08 08:11:35 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 221206B, collecting 4.8 ks of Photon
Counting (PC) mode data between T0+28.7 ks and T0+45.0 ks. 

No X-ray sources have been detected within the Swift/BAT-GUANO error
circle. The 3-sigma upper limit in the field ranges from ~0.002 to
~0.003 ct s^-1, corresponding to a 0.3-10 keV observed flux of 7.7e-14
to 1.0e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum).

Five uncatalogued sources were detected too far from the GRB position
to be likely afterglow candidates.

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/00021532.

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


GRB_name: GRB221206B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33030
SUBJECT: GRB 221206B: Fermi GBM observation
DATE:    22/12/08 10:24:03 GMT
FROM:    Christian Malacaria at ISSI  <cmalacaria.astro@gmail.com>

C. Malacaria (ISSI) and C. Meegan (UAH) report on behalf of the Fermi 
GBM Team: "At 12:22:47.36 UT on 06 December 2022, the Fermi Gamma-Ray 
Burst Monitor (GBM) triggered and located GRB 221206B (trigger 692022172 
/ 221206516). The GBM Final Real-time Localization was reported in GCN 
33023. The event was also detected by the Swift/BAT-GUANO (DeLaunay et 
al. 2022, GCN 33027) at a consistent position. The angle from the Fermi 
LAT boresight at the GBM trigger time is 121 degrees. The GBM light 
curve consists of two main peaks with a duration (T90) of about 8 s 
(50-300 keV). The time-averaged spectrum from T0-0 s to T0+5.9 s is best 
fit by a Band function with Epeak = 151 +/- 6 keV, alpha = -0.36 +/- 
0.06, and beta = -3.1 +/- 0.2 The event fluence (10-1000 keV) in this 
time interval is (2.19 +/- 0.05)E-06 erg/cm^2. The 1-sec peak photon 
flux measured starting from T0+7.5 s in the 10-1000 keV band is 26.7 +/- 
0.7 ph/s/cm^2. The spectral analysis results presented above are 
preliminary; final results will be published in the GBM GRB Catalog: 
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html 
<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/ 
<https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/>"


GRB_name: GRB221209A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33031
SUBJECT: GRB 221209A: Fermi GBM Final Real-time Localization
DATE:    22/12/09 06:00:47 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:50:24 UT on 9 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221209A (trigger 692257829.852778 / 221209243).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 241.7, Dec = 48.1 (J2000 degrees, equivalent to J2000 16h 06m, 48d 06'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 97.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221209243/quicklook/glg_skymap_all_bn221209243.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/bn221209243/quicklook/glg_healpix_all_bn221209243.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221209243/quicklook/glg_lc_medres34_bn221209243.gif


GRB_name: GRB221209A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33032
SUBJECT: GRB 221209A: BALROG localization (Fermi Trigger 692257829 / GRB 221209243)
DATE:    22/12/09 07:02:34 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
692257829 at 05:50:24 on 09 Dec. 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) = 234.9+/-0.9 deg
Decl.(2000.0) = 48.7+/-0.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB221209243/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB221209243/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB221209243/json

                        


GRB_name: GRB221203C
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33033
SUBJECT: GRB 221203C: AstroSat CZTI detection
DATE:    22/12/09 08:47:47 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

M. Dixit (IITB), G. Waratkar (IITB), R. Gopalakrishnan (IUCAA), A. 
Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka 
University/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 the detection of GRB 221203C which was also 
detected by KONUS-Wind (reported in GCN Notices).

The source was detected in the CsI anticoincidence (Veto) detector in 
the 100-500 keV energy range. The light curve peaks at 2022-12-03 
17:40:54.0 UTC. The measured peak count rate is 393.6 (+69.9, -74.5) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 1483 (+379, -412) counts. The local mean 
background count rate was 1466.2 (+5.3, -6.2) counts/s. We measure a T90 
of 9.10 (+5.86, -4.66) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB221209A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33034
SUBJECT: GRB 221209A: Fermi GBM observation
DATE:    22/12/09 15:04:36 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

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


"At 05:50:24.85 UT on 9 December 2022,
the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221209A
(trigger 692257829 / 221209243).
The Fermi GBM Final Real-time Localization
is reported in GCN 33031.

The angle from the Fermi LAT boresight
at the GBM trigger time is 97 degrees.


The GBM light curve consists of a single
bright emission episode with a duration (T90)
of about 4 s (50-300 keV).
The time-averaged spectrum from T0 to T0+7 s is
best fit by a Band function with
Epeak = 325 +/- 12 keV, alpha = -0.62 +/- 0.02,
and beta = -2.08 +/- 0.03.

The event fluence (10-1000 keV) in this
time interval is (3.35 +/- 0.03)E-05 erg/cm^2.
The 1-sec peak photon flux measured starting
from T0+1.2 in the 10-1000 keV band
is 67.1 +/- 0.6 ph/s/cm^2.


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

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


GRB_name: GRB221209B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33035
SUBJECT: GRB 221209B: Fermi GBM Final Real-time Localization
DATE:    22/12/09 21:13:45 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 21:03:27 UT on 9 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221209B (trigger 692312612.788022 / 221209877).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 142.1, Dec = -5.2 (J2000 degrees, equivalent to J2000 09h 28m, -5d 12'), with a statistical uncertainty of 10.6 degrees.

The angle from the Fermi LAT boresight is 92.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221209877/quicklook/glg_skymap_all_bn221209877.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/bn221209877/quicklook/glg_healpix_all_bn221209877.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221209877/quicklook/glg_lc_medres34_bn221209877.gif


GRB_name: GRB221210A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33036
SUBJECT: GRB 221210A: Fermi GBM Final Real-time Localization
DATE:    22/12/10 02:46:04 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 02:35:38 UT on 10 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221210A (trigger 692332543.436908 / 221210108).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 259.0, Dec = -12.9 (J2000 degrees, equivalent to J2000 17h 15m, -12d 54'), with a statistical uncertainty of 8.1 degrees.

The angle from the Fermi LAT boresight is 50.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221210108/quicklook/glg_skymap_all_bn221210108.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/bn221210108/quicklook/glg_healpix_all_bn221210108.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221210108/quicklook/glg_lc_medres34_bn221210108.gif


GRB_name: GRB221209A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33037
SUBJECT: GRB 221209A: AstroSat CZTI detection
DATE:    22/12/10 02:55:52 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

R. Gopalakrishnan (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. 
Bhalerao (IITB), D. Bhattacharya (Ashoka University/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 the detection of a bright GRB 221209A which was 
also detected by Fermi-GBM (Fermi GBM team, GCN Circ. 33031) and BALROG 
(Kunzweiler et al., GCN Circ. 33032).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-12-09 05:50:26.45 UTC. The measured peak count 
rate associated with the burst is 6052 (+437, -209) counts/s above the 
background in the combined data of all quadrants, with a total of 9174 
(+346, -285) counts. The local mean background count rate was 445 (+8, 
-10) counts/s. Using cumulative rates, we measure a T90 of 2.7 (+0.2, 
-0.1) s. In the preliminary analysis, we find 1078 Compton events 
associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-12-09 
05:50:26.18 UTC. The measured peak count rate is 5980 (+136, -150) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 12635 (+713, -729) counts. The local mean 
background count rate was 1402 (+8, -7) counts/s. We measure a T90 of 
3.5 (+1.0, -0.6) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33038
SUBJECT: GRB 221009A: MuSCAT3 observations
DATE:    22/12/10 03:40:25 GMT
FROM:    Mariko Kimura at RIKEN  <mariko.kimura@riken.jp>

M. Kimura (RIKEN), K. Isogai (Tokyo Univ./Kyoto Univ.), M. Arimoto,
D. Yonetoku (Kanazawa Univ.),
N. Narita, M. Tamura (Tokyo Univ./Astrobiology Center),
A. Fukui  (Tokyo Univ.), M. Ikoma (NAOJ)

We have monitored the afterglow of GRB 221009A since three days
after the Swift and Fermi alerts (GCN 32632; GCN 32636) by MuSCAT3
on the 2-meter telescope at Las Cumbres Observatory.
MuSCAT3 is multi-channel imagers with the filters of SDSS g', r', i', zs,
which is designed for observing transiting exoplanets.
https://lco.global/observatory/instruments/muscat3/

The measurements are here:
BJD                     Mag    Err   Filter
2459864.82404  21.33  0.15  g
2459864.82404  20.01  0.03  r
2459864.82404  19.48  0.03  i
2459864.82404  18.26  0.01  z
2459870.80681  23.55  0.21  g
2459870.80681  21.74  0.05  r
2459870.80681  20.47  0.04  i
2459870.80681  19.90  0.03  z
2459872.82760  23.64  0.26  g
2459872.82760  21.91  0.07  r
2459872.82760  20.82  0.06  i
2459872.82760  20.22  0.05  z
2459876.80690  23.99  0.34  g
2459876.80690  21.96  0.09  r
2459876.80690  21.00  0.08  i
2459876.80690  20.50  0.07  z

By plotting these data with the other optical measurements reported to GCN
(GCNs 32625, 32640, 32644, 32645, 32646, 32652, 32659, 32662, 32666,
32667, 32670, 32678, 32679, 32692, 32693, 32705, 32709, 32729, 32730,
32743, 32750, 32758, 32769, 32771, 32799, 32809, 32818),
we found that the optical afterglow light curve shows a power-law decay, and
only i'-band light curve fluctuates along the decline possibly because of
systematic errors.
We did not find a bump reported by GCN 32818 at least around a week after
the Swift and Fermi trigger.

If you have any queries, please contact M. Kimura at the following address.
mariko.kimura@riken.jp


GRB_name: GRB221211A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33041
SUBJECT: GRB 221211A: Fermi GBM Final Real-time Localization
DATE:    22/12/11 06:45:18 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:34:53 UT on 11 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221211A (trigger 692433298.712892 / 221211274).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 160.9, Dec = 52.2 (J2000 degrees, equivalent to J2000 10h 43m, 52d 12'), with a statistical uncertainty of 4.7 degrees.

The angle from the Fermi LAT boresight is 79.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221211274/quicklook/glg_skymap_all_bn221211274.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/bn221211274/quicklook/glg_healpix_all_bn221211274.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221211274/quicklook/glg_lc_medres34_bn221211274.gif


GRB_name: GRB221208A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33042
SUBJECT: GRB 221208A: AstroSat CZTI detection
DATE:    22/12/11 13:27:27 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

M. Dixit (IITB), G. Waratkar (IITB), R. Gopalakrishnan (IUCAA), A. 
Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka 
University/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 the detection of GRB 221208A which was also 
detected by KONUS-Wind and GECAM (both reported in GCN Notices).

The source was faintly detected with the CZT detectors in the 20-200 keV 
energy range. The light curve peaks at 2022-12-08 03:10:54.5 UTC. The 
measured peak count rate associated with the burst is 45.6 (+21.8, -8.6) 
counts/s above the background in the combined data of three quadrants, 
with a total of 184 (+103, -98) counts. The local mean background count 
rate was 102.5 (+1.3, -1.7) counts/s. Using cumulative rates, we measure 
a T90 of 6.86 (+4.20, -3.59) s.

It was also clearly detected in the CsI anticoincidence (Veto) detectors 
in the 100-500 keV energy range. The light curve peaks at 2022-12-08 
03:10:54.2 UTC. The measured peak count rate is 581.1 (+71.1, -76.6) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 1622 (+380, -416) counts. The local mean 
background count rate was 1452.6 (+4.5, -5.2) counts/s. We measure a T90 
of 4.81 (+6.88, -2.38) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB221211A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33043
SUBJECT: Fermi GRB 221211A: Global MASTER-Net observations report 
DATE:    22/12/11 20:45:09 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 221211A ( Fermi GBM team, GCN 33041) errorbox  13333 sec after notice time and 13366 sec after trigger time at 2022-12-11 10:17:40 UT, with upper limit up to  16.8 mag. The observations began at zenith distance = 70 deg. The sun  altitude  is -25.9 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 221211A errorbox  42897 sec after notice time and 42930 sec after trigger time at 2022-12-11 18:30:24 UT, with upper limit up to  18.7 mag. The observations began at zenith distance = 72 deg. The sun  altitude  is -52.6 deg. 

The galactic latitude b = 56 deg., longitude l = 158 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2180853

We obtain a following upper limits.  

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

   13397 | 2022-12-11 10:17:40 |         MASTER-Amur | (10h 23m 18.99s , +58d 10m 49.2s) |   C |    60 | 14.9 |        
   13476 | 2022-12-11 10:18:59 |         MASTER-Amur | (10h 38m 27.39s , +58d 12m 24.4s) |   C |    60 | 14.8 |        
   14367 | 2022-12-11 10:33:51 |         MASTER-Amur | (10h 23m 10.84s , +58d 11m 05.3s) |   C |    60 | 14.7 |        
   14447 | 2022-12-11 10:35:10 |         MASTER-Amur | (10h 38m 21.10s , +58d 12m 31.4s) |   C |    60 | 14.3 |        
   15244 | 2022-12-11 10:48:27 |         MASTER-Amur | (10h 52m 08.90s , +58d 10m 57.0s) |   C |    60 | 14.9 |        
   15403 | 2022-12-11 10:51:06 |         MASTER-Amur | (10h 23m 13.85s , +58d 10m 10.2s) |   C |    60 | 14.7 |        
   15482 | 2022-12-11 10:52:25 |         MASTER-Amur | (10h 38m 27.35s , +58d 11m 42.9s) |   C |    60 | 14.9 |        
   15562 | 2022-12-11 10:53:45 |         MASTER-Amur | (10h 19m 13.91s , +56d 17m 53.6s) |   C |    60 | 15.0 |        
   15642 | 2022-12-11 10:55:05 |         MASTER-Amur | (10h 33m 45.26s , +56d 16m 57.1s) |   C |    60 | 14.6 |        
   15801 | 2022-12-11 10:57:44 |         MASTER-Amur | (10h 03m 58.02s , +54d 23m 09.0s) |   C |    60 | 15.1 |        
   16201 | 2022-12-11 11:04:24 |         MASTER-Amur | (10h 52m 07.33s , +58d 10m 25.6s) |   C |    60 | 14.8 |        
   16519 | 2022-12-11 11:09:42 |         MASTER-Amur | (10h 19m 14.09s , +56d 17m 39.7s) |   C |    60 | 14.6 |        
   16599 | 2022-12-11 11:11:02 |         MASTER-Amur | (10h 33m 42.98s , +56d 16m 51.4s) |   C |    60 | 14.5 |        
   16758 | 2022-12-11 11:13:41 |         MASTER-Amur | (10h 04m 00.23s , +54d 21m 16.7s) |   C |    60 | 14.8 |        
   17156 | 2022-12-11 11:20:19 |         MASTER-Amur | (10h 52m 00.98s , +58d 12m 05.4s) |   C |    60 | 14.6 |        
   17475 | 2022-12-11 11:25:38 |         MASTER-Amur | (10h 19m 15.48s , +56d 16m 59.1s) |   C |    60 | 14.8 |        
   17554 | 2022-12-11 11:26:58 |         MASTER-Amur | (10h 33m 40.68s , +56d 15m 53.8s) |   C |    60 | 14.4 |        
   17714 | 2022-12-11 11:29:37 |         MASTER-Amur | (10h 03m 54.53s , +54d 21m 54.1s) |   C |    60 | 15.0 |        
   18112 | 2022-12-11 11:36:15 |         MASTER-Amur | (10h 16m 20.07s , +54d 21m 15.4s) |   C |    60 | 14.7 |        
   18192 | 2022-12-11 11:37:35 |         MASTER-Amur | (10h 30m 06.95s , +54d 23m 00.2s) |   C |    60 | 14.7 |        
   18431 | 2022-12-11 11:41:34 |         MASTER-Amur | (10h 14m 16.22s , +52d 26m 50.5s) |   C |    60 | 14.6 |        
   18511 | 2022-12-11 11:42:54 |         MASTER-Amur | (10h 27m 31.33s , +52d 27m 10.6s) |   C |    60 | 14.5 |        
   18590 | 2022-12-11 11:44:13 |         MASTER-Amur | (10h 46m 39.38s , +56d 15m 49.8s) |   C |    60 | 14.8 |        
   18670 | 2022-12-11 11:45:33 |         MASTER-Amur | (11h 01m 07.10s , +56d 17m 25.0s) |   C |    60 | 14.8 |        
   18750 | 2022-12-11 11:46:53 |         MASTER-Amur | (10h 42m 23.34s , +54d 23m 14.1s) |   C |    60 | 14.5 |        
   18829 | 2022-12-11 11:48:13 |         MASTER-Amur | (10h 56m 14.35s , +54d 22m 33.9s) |   C |    60 | 15.1 |        
   18988 | 2022-12-11 11:50:52 |         MASTER-Amur | (10h 02m 28.16s , +52d 27m 47.1s) |   C |    60 | 15.1 |        
   19068 | 2022-12-11 11:52:11 |         MASTER-Amur | (10h 16m 18.76s , +54d 21m 07.3s) |   C |    60 | 14.7 |        
   19148 | 2022-12-11 11:53:31 |         MASTER-Amur | (10h 30m 06.43s , +54d 22m 53.6s) |   C |    60 | 14.5 |        
   19227 | 2022-12-11 11:54:51 |         MASTER-Amur | (11h 13m 59.17s , +56d 17m 53.5s) |   C |    60 | 15.0 |        
   19387 | 2022-12-11 11:57:30 |         MASTER-Amur | (10h 14m 15.77s , +52d 26m 34.8s) |   C |    60 | 14.4 |        
   19467 | 2022-12-11 11:58:50 |         MASTER-Amur | (10h 27m 30.47s , +52d 27m 27.5s) |   C |    60 | 13.9 |        
   19546 | 2022-12-11 12:00:10 |         MASTER-Amur | (10h 46m 37.67s , +56d 17m 04.0s) |   C |    60 | 13.7 |        
   19626 | 2022-12-11 12:01:29 |         MASTER-Amur | (11h 01m 02.19s , +56d 15m 42.7s) |   C |    60 | 14.1 |        
   19705 | 2022-12-11 12:02:49 |         MASTER-Amur | (10h 42m 26.61s , +54d 22m 40.3s) |   C |    60 | 13.9 |        
   19785 | 2022-12-11 12:04:08 |         MASTER-Amur | (10h 56m 06.44s , +54d 22m 11.9s) |   C |    60 | 14.6 |        
   19945 | 2022-12-11 12:06:48 |         MASTER-Amur | (10h 02m 30.25s , +52d 27m 07.7s) |   C |    60 | 14.4 |        
   20024 | 2022-12-11 12:08:07 |         MASTER-Amur | (10h 16m 16.48s , +54d 20m 26.1s) |   C |    60 | 13.4 |        
   20104 | 2022-12-11 12:09:27 |         MASTER-Amur | (10h 40m 33.48s , +54d 21m 04.6s) |   C |    60 | 14.2 |        
   20348 | 2022-12-11 12:13:31 |         MASTER-Amur | (10h 24m 47.95s , +52d 28m 17.0s) |   C |    60 | 13.7 |        
   20428 | 2022-12-11 12:14:51 |         MASTER-Amur | (10h 37m 49.70s , +52d 28m 03.2s) |   C |    60 | 13.5 |        
   20507 | 2022-12-11 12:16:11 |         MASTER-Amur | (10h 57m 04.08s , +56d 17m 09.1s) |   C |    60 | 13.6 |        
   20587 | 2022-12-11 12:17:30 |         MASTER-Amur | (11h 11m 35.61s , +56d 16m 38.5s) |   C |    60 | 14.0 |        
   20667 | 2022-12-11 12:18:50 |         MASTER-Amur | (10h 52m 50.44s , +54d 20m 59.7s) |   C |    60 | 14.1 |        
   20753 | 2022-12-11 12:20:16 |         MASTER-Amur | (11h 06m 39.02s , +54d 21m 48.4s) |   C |    60 | 14.5 |        
   20833 | 2022-12-11 12:21:36 |         MASTER-Amur | (09h 59m 46.78s , +52d 27m 56.5s) |   C |    60 | 14.7 |        
   20912 | 2022-12-11 12:22:56 |         MASTER-Amur | (10h 12m 56.48s , +52d 26m 17.4s) |   C |    60 | 14.6 |        
   20992 | 2022-12-11 12:24:15 |         MASTER-Amur | (10h 49m 41.28s , +52d 27m 47.5s) |   C |    60 | 14.4 |        
   21072 | 2022-12-11 12:25:35 |         MASTER-Amur | (11h 02m 50.65s , +52d 29m 11.4s) |   C |    60 | 14.6 |        
   21311 | 2022-12-11 12:29:34 |         MASTER-Amur | (10h 47m 30.88s , +50d 34m 22.5s) |   C |    60 | 14.6 |        
   21391 | 2022-12-11 12:30:54 |         MASTER-Amur | (11h 00m 07.46s , +50d 33m 24.7s) |   C |    60 | 14.6 |        
   21471 | 2022-12-11 12:32:15 |         MASTER-Amur | (10h 23m 29.73s , +50d 33m 21.5s) |   C |    60 | 14.1 |        
   21551 | 2022-12-11 12:33:34 |         MASTER-Amur | (10h 36m 07.34s , +50d 34m 27.7s) |   C |    60 | 14.4 |        
   21631 | 2022-12-11 12:34:54 |         MASTER-Amur | (11h 14m 39.38s , +52d 27m 12.9s) |   C |    60 | 14.5 |        
   21790 | 2022-12-11 12:37:33 |         MASTER-Amur | (10h 23m 05.66s , +48d 38m 27.2s) |   C |    60 | 14.1 |        
   21869 | 2022-12-11 12:38:52 |         MASTER-Amur | (10h 35m 15.33s , +48d 40m 00.9s) |   C |    60 | 14.1 |        
   21949 | 2022-12-11 12:40:12 |         MASTER-Amur | (10h 49m 40.52s , +52d 27m 48.1s) |   C |    60 | 14.3 |        
   22029 | 2022-12-11 12:41:32 |         MASTER-Amur | (11h 02m 49.31s , +52d 28m 43.1s) |   C |    60 | 14.5 |        
   22108 | 2022-12-11 12:42:51 |         MASTER-Amur | (10h 46m 06.47s , +48d 38m 22.6s) |   C |    60 | 14.0 |        
   22188 | 2022-12-11 12:44:11 |         MASTER-Amur | (10h 58m 19.04s , +48d 38m 44.5s) |   C |    60 | 14.3 |        
   22268 | 2022-12-11 12:45:31 |         MASTER-Amur | (10h 47m 30.84s , +50d 34m 06.7s) |   C |    60 | 14.6 |        
   22347 | 2022-12-11 12:46:51 |         MASTER-Amur | (11h 00m 06.00s , +50d 33m 00.5s) |   C |    60 | 14.4 |        
   22427 | 2022-12-11 12:48:10 |         MASTER-Amur | (10h 23m 34.92s , +50d 33m 43.6s) |   C |    60 | 14.4 |        
   22507 | 2022-12-11 12:49:30 |         MASTER-Amur | (10h 36m 05.92s , +50d 33m 20.1s) |   C |    60 | 14.2 |        
   22586 | 2022-12-11 12:50:50 |         MASTER-Amur | (11h 14m 39.16s , +52d 28m 48.4s) |   C |    60 | 14.3 |        
   22746 | 2022-12-11 12:53:29 |         MASTER-Amur | (10h 23m 02.38s , +48d 37m 38.0s) |   C |    60 | 14.3 |        
   22826 | 2022-12-11 12:54:49 |         MASTER-Amur | (10h 35m 15.53s , +48d 38m 17.7s) |   C |    60 | 14.0 |        
   22905 | 2022-12-11 12:56:08 |         MASTER-Amur | (10h 49m 43.38s , +52d 28m 11.1s) |   C |    60 | 14.4 |        
   22985 | 2022-12-11 12:57:28 |         MASTER-Amur | (11h 02m 52.82s , +52d 26m 38.5s) |   C |    60 | 14.5 |        
   23065 | 2022-12-11 12:58:48 |         MASTER-Amur | (10h 46m 10.19s , +48d 39m 47.2s) |   C |    60 | 14.3 |        
   23144 | 2022-12-11 13:00:08 |         MASTER-Amur | (10h 58m 12.33s , +48d 39m 19.3s) |   C |    60 | 14.4 |        
   23224 | 2022-12-11 13:01:28 |         MASTER-Amur | (10h 47m 27.66s , +50d 34m 05.0s) |   C |    60 | 14.3 |        
   23304 | 2022-12-11 13:02:47 |         MASTER-Amur | (11h 00m 08.87s , +50d 33m 20.7s) |   C |    60 | 14.1 |        
   23384 | 2022-12-11 13:04:07 |         MASTER-Amur | (10h 23m 30.18s , +50d 31m 42.7s) |   C |    60 | 14.1 |        
   23464 | 2022-12-11 13:05:27 |         MASTER-Amur | (10h 36m 11.99s , +50d 32m 13.5s) |   C |    60 | 14.2 |        
   23543 | 2022-12-11 13:06:47 |         MASTER-Amur | (11h 14m 42.64s , +52d 28m 08.6s) |   C |    60 | 14.6 |        
   23703 | 2022-12-11 13:09:26 |         MASTER-Amur | (10h 23m 10.15s , +48d 38m 52.7s) |   C |    60 | 14.1 |        
   23782 | 2022-12-11 13:10:46 |         MASTER-Amur | (10h 35m 09.46s , +48d 38m 37.8s) |   C |    60 | 14.0 |        
   24022 | 2022-12-11 13:14:46 |         MASTER-Amur | (10h 46m 11.48s , +48d 38m 18.2s) |   C |    60 | 13.9 |        
   24102 | 2022-12-11 13:16:05 |         MASTER-Amur | (10h 58m 15.42s , +48d 40m 05.0s) |   C |    60 | 13.7 |        
   24182 | 2022-12-11 13:17:25 |         MASTER-Amur | (11h 11m 29.29s , +50d 33m 51.3s) |   C |    60 | 14.1 |        
   24261 | 2022-12-11 13:18:45 |         MASTER-Amur | (11h 24m 00.91s , +50d 33m 40.8s) |   C |    60 | 14.2 |        
   24342 | 2022-12-11 13:20:05 |         MASTER-Amur | (11h 19m 02.36s , +54d 21m 33.1s) |   C |    60 | 13.8 |        
   24501 | 2022-12-11 13:22:44 |         MASTER-Amur | (10h 45m 31.81s , +46d 45m 47.0s) |   C |    60 | 14.0 |        
   24580 | 2022-12-11 13:24:04 |         MASTER-Amur | (10h 57m 12.57s , +46d 44m 11.0s) |   C |    60 | 14.3 |        
   24660 | 2022-12-11 13:25:23 |         MASTER-Amur | (11h 09m 05.70s , +48d 39m 23.2s) |   C |    60 | 14.0 |        
   25138 | 2022-12-11 13:33:21 |         MASTER-Amur | (11h 11m 29.95s , +50d 34m 21.2s) |   C |    60 | 14.1 |        
   25218 | 2022-12-11 13:34:41 |         MASTER-Amur | (11h 23m 59.75s , +50d 33m 44.2s) |   C |    60 | 14.4 |        
   25298 | 2022-12-11 13:36:01 |         MASTER-Amur | (11h 18m 56.18s , +54d 22m 35.9s) |   C |    60 | 14.3 |        
   25457 | 2022-12-11 13:38:40 |         MASTER-Amur | (10h 45m 28.54s , +46d 43m 38.6s) |   C |    60 | 13.9 |        
   25537 | 2022-12-11 13:40:00 |         MASTER-Amur | (10h 57m 17.27s , +46d 44m 11.7s) |   C |    60 | 14.3 |        
   25616 | 2022-12-11 13:41:19 |         MASTER-Amur | (11h 09m 08.69s , +48d 39m 45.7s) |   C |    60 | 14.2 |        
   26099 | 2022-12-11 13:49:22 |         MASTER-Amur | (11h 11m 25.84s , +50d 32m 03.2s) |   C |    60 | 14.0 |        
   26178 | 2022-12-11 13:50:42 |         MASTER-Amur | (11h 24m 06.08s , +50d 32m 31.0s) |   C |    60 | 14.3 |        
   26258 | 2022-12-11 13:52:02 |         MASTER-Amur | (11h 19m 00.13s , +54d 21m 44.7s) |   C |    60 | 14.3 |        
   26418 | 2022-12-11 13:54:41 |         MASTER-Amur | (10h 45m 35.05s , +46d 44m 42.0s) |   C |    60 | 14.2 |        
   26498 | 2022-12-11 13:56:01 |         MASTER-Amur | (10h 57m 10.70s , +46d 44m 31.3s) |   C |    60 | 14.4 |        
   26577 | 2022-12-11 13:57:20 |         MASTER-Amur | (11h 09m 05.30s , +48d 39m 38.1s) |   C |    60 | 13.8 |        
   26737 | 2022-12-11 14:00:00 |         MASTER-Amur | (10h 23m 22.10s , +46d 42m 59.8s) |   C |    60 | 13.7 |        
   26822 | 2022-12-11 14:01:25 |         MASTER-Amur | (10h 35m 00.83s , +46d 44m 17.3s) |   C |    60 | 13.7 |        
   27698 | 2022-12-11 14:16:01 |         MASTER-Amur | (10h 23m 23.83s , +46d 42m 42.9s) |   C |    60 | 13.7 |        
   27778 | 2022-12-11 14:17:21 |         MASTER-Amur | (10h 35m 01.04s , +46d 44m 00.4s) |   C |    60 | 13.6 |        
   29078 | 2022-12-11 14:39:01 |         MASTER-Amur | (10h 23m 15.78s , +46d 42m 30.2s) |   C |    60 | 16.7 |        
   29157 | 2022-12-11 14:40:20 |         MASTER-Amur | (10h 34m 56.24s , +46d 43m 44.8s) |   C |    60 | 16.8 |        
   43020 | 2022-12-11 18:30:24 |   MASTER-Kislovodsk | (10h 43m 28.47s , +52d 00m 51.5s) |   C |   180 | 16.6 |        
   43021 | 2022-12-11 18:30:24 |   MASTER-Kislovodsk | (10h 49m 47.00s , +51d 36m 00.2s) |   C |   180 | 17.9 |        
   43221 | 2022-12-11 18:33:44 |   MASTER-Kislovodsk | (10h 43m 35.04s , +51d 59m 48.7s) |   C |   180 | 16.6 |        
   43221 | 2022-12-11 18:33:44 |   MASTER-Kislovodsk | (10h 49m 53.44s , +51d 34m 54.7s) |   C |   180 | 18.3 |        
   43421 | 2022-12-11 18:37:04 |   MASTER-Kislovodsk | (10h 51m 28.64s , +51d 58m 39.3s) |   C |   180 | 17.6 |        
   43421 | 2022-12-11 18:37:04 |   MASTER-Kislovodsk | (10h 57m 46.60s , +51d 33m 40.9s) |   C |   180 | 18.3 |        
   43822 | 2022-12-11 18:43:45 |   MASTER-Kislovodsk | (10h 35m 32.53s , +52d 00m 51.4s) |   C |   180 | 16.9 |        
   43822 | 2022-12-11 18:43:45 |   MASTER-Kislovodsk | (10h 41m 51.71s , +51d 35m 58.6s) |   C |   180 | 18.0 |        
   44023 | 2022-12-11 18:47:06 |   MASTER-Kislovodsk | (10h 35m 32.76s , +51d 59m 40.3s) |   C |   180 | 17.0 |        
   44023 | 2022-12-11 18:47:06 |   MASTER-Kislovodsk | (10h 41m 51.97s , +51d 34m 47.6s) |   C |   180 | 17.9 |        
   44223 | 2022-12-11 18:50:26 |   MASTER-Kislovodsk | (10h 35m 37.47s , +54d 01m 04.1s) |   C |   180 | 17.1 |        
   44223 | 2022-12-11 18:50:26 |   MASTER-Kislovodsk | (10h 42m 15.73s , +53d 36m 10.0s) |   C |   180 | 18.1 |        
   44624 | 2022-12-11 18:57:07 |   MASTER-Kislovodsk | (10h 43m 31.23s , +54d 01m 21.3s) |   C |   180 | 17.7 |        
   44624 | 2022-12-11 18:57:07 |   MASTER-Kislovodsk | (10h 50m 09.60s , +53d 36m 26.8s) |   C |   180 | 18.5 |        
   44824 | 2022-12-11 19:00:28 |   MASTER-Kislovodsk | (10h 43m 37.54s , +54d 00m 26.2s) |   C |   180 | 17.7 |        
   44824 | 2022-12-11 19:00:28 |   MASTER-Kislovodsk | (10h 50m 15.91s , +53d 35m 32.7s) |   C |   180 | 18.6 |        
   45025 | 2022-12-11 19:03:48 |   MASTER-Kislovodsk | (10h 51m 31.38s , +53d 59m 17.7s) |   C |   180 | 18.0 |        
   45025 | 2022-12-11 19:03:48 |   MASTER-Kislovodsk | (10h 58m 09.28s , +53d 34m 22.8s) |   C |   180 | 18.7 |        
   45225 | 2022-12-11 19:07:08 |   MASTER-Kislovodsk | (10h 51m 37.28s , +53d 59m 49.2s) |   C |   180 | 17.9 |        
   45225 | 2022-12-11 19:07:09 |   MASTER-Kislovodsk | (10h 58m 15.37s , +53d 34m 54.4s) |   C |   180 | 18.6 |        
   45426 | 2022-12-11 19:10:29 |   MASTER-Kislovodsk | (10h 51m 33.35s , +50d 01m 15.0s) |   C |   180 | 17.6 |        
   45426 | 2022-12-11 19:10:29 |   MASTER-Kislovodsk | (10h 57m 36.55s , +49d 36m 24.2s) |   C |   180 | 18.5 |        
   45626 | 2022-12-11 19:13:49 |   MASTER-Kislovodsk | (10h 51m 33.45s , +49d 59m 46.5s) |   C |   180 | 17.5 |        
   45626 | 2022-12-11 19:13:50 |   MASTER-Kislovodsk | (10h 57m 36.72s , +49d 34m 57.0s) |   C |   180 | 18.3 |        
   46027 | 2022-12-11 19:20:30 |   MASTER-Kislovodsk | (10h 43m 29.79s , +50d 01m 01.8s) |   C |   180 | 17.4 |        
   46027 | 2022-12-11 19:20:30 |   MASTER-Kislovodsk | (10h 49m 34.10s , +49d 36m 15.9s) |   C |   180 | 18.3 |        
   46227 | 2022-12-11 19:23:50 |   MASTER-Kislovodsk | (10h 35m 30.48s , +50d 02m 23.1s) |   C |   180 | 17.5 |        
   46227 | 2022-12-11 19:23:51 |   MASTER-Kislovodsk | (10h 41m 35.50s , +49d 37m 40.8s) |   C |   180 | 18.1 |        
   46628 | 2022-12-11 19:30:31 |   MASTER-Kislovodsk | (10h 35m 30.95s , +48d 00m 38.5s) |   C |   180 | 17.6 |        
   46628 | 2022-12-11 19:30:31 |   MASTER-Kislovodsk | (10h 41m 21.02s , +47d 36m 00.4s) |   C |   180 | 17.9 |        
   46829 | 2022-12-11 19:33:52 |   MASTER-Kislovodsk | (10h 35m 37.08s , +48d 01m 09.4s) |   C |   180 | 17.6 |        
   46829 | 2022-12-11 19:33:52 |   MASTER-Kislovodsk | (10h 41m 27.18s , +47d 36m 32.4s) |   C |   180 | 17.7 |        
   47230 | 2022-12-11 19:40:33 |   MASTER-Kislovodsk | (10h 47m 34.63s , +48d 00m 41.2s) |   C |   180 | 17.5 |        
   47230 | 2022-12-11 19:40:33 |   MASTER-Kislovodsk | (10h 53m 22.74s , +47d 36m 02.9s) |   C |   180 | 18.2 |        
   47430 | 2022-12-11 19:43:53 |   MASTER-Kislovodsk | (10h 47m 43.82s , +55d 02m 09.9s) |   C |   180 | 18.2 |        
   47430 | 2022-12-11 19:43:53 |   MASTER-Kislovodsk | (10h 54m 31.48s , +54d 37m 26.4s) |   C |   180 | 18.7 |        
   47630 | 2022-12-11 19:47:14 |   MASTER-Kislovodsk | (10h 47m 38.94s , +55d 01m 37.4s) |   C |   180 | 18.3 |        
   47631 | 2022-12-11 19:47:14 |   MASTER-Kislovodsk | (10h 54m 26.66s , +54d 36m 55.4s) |   C |   180 | 18.7 |        
   47831 | 2022-12-11 19:50:34 |   MASTER-Kislovodsk | (10h 35m 39.63s , +55d 03m 05.5s) |   C |   180 | 17.8 |        
   47831 | 2022-12-11 19:50:34 |   MASTER-Kislovodsk | (10h 42m 28.32s , +54d 38m 28.5s) |   C |   180 | 18.5 |        
   48219 | 2022-12-11 19:57:03 |   MASTER-Kislovodsk | (10h 15m 30.49s , +50d 04m 01.5s) |   C |   180 | 17.9 |        
   48219 | 2022-12-11 19:57:03 |   MASTER-Kislovodsk | (10h 21m 41.27s , +49d 40m 12.2s) |   C |   180 | 18.3 |        
   48420 | 2022-12-11 20:00:23 |   MASTER-Kislovodsk | (10h 15m 36.59s , +50d 03m 05.8s) |   C |   180 | 18.1 |        
   48420 | 2022-12-11 20:00:23 |   MASTER-Kislovodsk | (10h 21m 47.06s , +49d 39m 17.1s) |   C |   180 | 18.5 |        
   49845 | 2022-12-11 20:25:08 |   MASTER-Kislovodsk | (10h 46m 15.56s , +50d 38m 25.0s) |   C |    60 | 17.5 |        
   49845 | 2022-12-11 20:25:08 |   MASTER-Kislovodsk | (10h 52m 22.27s , +50d 14m 36.9s) |   C |    60 | 18.2 |        
   49925 | 2022-12-11 20:26:28 |   MASTER-Kislovodsk | (10h 48m 59.42s , +52d 32m 18.1s) |   C |    60 | 17.8 |        
   49925 | 2022-12-11 20:26:28 |   MASTER-Kislovodsk | (10h 55m 21.79s , +52d 08m 26.5s) |   C |    60 | 18.2 |        
   50407 | 2022-12-11 20:34:30 |   MASTER-Kislovodsk | (10h 52m 37.54s , +54d 27m 52.2s) |   C |    60 | 18.0 |        
   50407 | 2022-12-11 20:34:31 |   MASTER-Kislovodsk | (10h 59m 16.05s , +54d 03m 48.7s) |   C |    60 | 18.4 |        
   50568 | 2022-12-11 20:37:11 |   MASTER-Kislovodsk | (10h 23m 59.40s , +52d 34m 21.7s) |   C |    60 | 17.0 |        
   50568 | 2022-12-11 20:37:11 |   MASTER-Kislovodsk | (10h 30m 25.89s , +52d 10m 25.4s) |   C |    60 | 17.7 |        
   50743 | 2022-12-11 20:40:06 |   MASTER-Kislovodsk | (10h 46m 19.47s , +50d 39m 12.7s) |   C |    60 | 17.4 |        
   50743 | 2022-12-11 20:40:06 |   MASTER-Kislovodsk | (10h 52m 27.72s , +50d 15m 18.3s) |   C |    60 | 18.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221212A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33044
SUBJECT: GRB 221212A: Fermi GBM Final Real-time Localization
DATE:    22/12/12 06:51:28 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:40:59 UT on 12 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221212A (trigger 692520064.300078 / 221212278).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 142.9, Dec = -19.2 (J2000 degrees, equivalent to J2000 09h 31m, -19d 11'), with a statistical uncertainty of 15.8 degrees.

The angle from the Fermi LAT boresight is 48.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221212278/quicklook/glg_skymap_all_bn221212278.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/bn221212278/quicklook/glg_healpix_all_bn221212278.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221212278/quicklook/glg_lc_medres34_bn221212278.gif


GRB_name: GRB221212A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33045
SUBJECT: Auto: ... (was: GRB 221212A: Fermi GBM Final Real-time Localization)
DATE:    22/12/12 09:43:53 GMT
FROM:    Christian Malacaria at ISSI  <cmalacaria.astro@gmail.com>

This is an OpenPGP/MIME encrypted message (RFC 4880 and 3156)
--------------YCXt72YnZUE0mIKG31zJ46P6
Content-Type: application/pgp-encrypted
Content-Description: PGP/MIME version identification

Version: 1

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Content-Disposition: inline; filename="encrypted.asc"

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=iOjs
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--------------YCXt72YnZUE0mIKG31zJ46P6--


GRB_name: GRB221212A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33046
SUBJECT: Auto: ... (was: GRB 221212A: Fermi GBM Final Real-time Localization)
DATE:    22/12/12 09:43:58 GMT
FROM:    Christian Malacaria at ISSI  <cmalacaria.astro@gmail.com>

This is an OpenPGP/MIME encrypted message (RFC 4880 and 3156)
--------------YCXt72YnZUE0mIKG31zJ46P6
Content-Type: application/pgp-encrypted
Content-Description: PGP/MIME version identification

Version: 1

--------------YCXt72YnZUE0mIKG31zJ46P6
Content-Type: application/octet-stream; name="encrypted.asc"
Content-Description: OpenPGP encrypted message
Content-Disposition: inline; filename="encrypted.asc"

-----BEGIN PGP MESSAGE-----

=iOjs
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--------------YCXt72YnZUE0mIKG31zJ46P6--


GRB_name: GRB221212A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33047
SUBJECT: Auto: ... (was: GRB 221212A: Fermi GBM Final Real-time Localization)
DATE:    22/12/12 09:44:58 GMT
FROM:    Christian Malacaria at ISSI  <cmalacaria.astro@gmail.com>

This is an OpenPGP/MIME encrypted message (RFC 4880 and 3156)
--------------YCXt72YnZUE0mIKG31zJ46P6
Content-Type: application/pgp-encrypted
Content-Description: PGP/MIME version identification

Version: 1

--------------YCXt72YnZUE0mIKG31zJ46P6
Content-Type: application/octet-stream; name="encrypted.asc"
Content-Description: OpenPGP encrypted message
Content-Disposition: inline; filename="encrypted.asc"

-----BEGIN PGP MESSAGE-----

=iOjs
-----END PGP MESSAGE-----

--------------YCXt72YnZUE0mIKG31zJ46P6--


GRB_name: GRB221209A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33049
SUBJECT: GRB 221209A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/12/12 23:03:08 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

Y. Kawakubo (LSU), A. Yoshida, T. Sakamoto, S. Sugita (AGU), 
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),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 221209A (Fermi GBM Final Real-time Localization: 
Fermi GBM team, GCN Circ. 33031; BALROG localization:
Kunzweiler et al., GCN Circ 33032; Fermi GBM observation: 
Bissaldi et al., GCN Circ 33034; AstroSat CZTI detection: 
Gopalakrishnan et al., GCN Circ 33037) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 05:50:25.591 UTC on 9 December 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1354600238/index.html).
The burst signal was seen by all CGBM detectors.
No real-time CGBM GCN notice was distributed about this trigger because
the real-time communication from the ISS was off (loss of signal).

The burst light curve shows a single pulse that starts
at T-2.0 sec, peaks at T+0.9 sec, and ends at T+5.0 sec.
The T90 and T50 durations measured by the SGM data are 3.2 +/- 0.4 sec
and 1.3 +/- 0.1 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1354600238/

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


GRB_name: GRB221215A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33054
SUBJECT: GRB 221215A: Fermi GBM Final Real-time Localization
DATE:    22/12/15 04:25:46 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 04:14:27 UT on 15 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221215A (trigger 692770472.974848 / 221215177).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 156.1, Dec = 38.6 (J2000 degrees, equivalent to J2000 10h 24m, 38d 36'), with a statistical uncertainty of 13.6 degrees.

The angle from the Fermi LAT boresight is 45.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221215177/quicklook/glg_skymap_all_bn221215177.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/bn221215177/quicklook/glg_healpix_all_bn221215177.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221215177/quicklook/glg_lc_medres34_bn221215177.gif


GRB_name: GRB221215B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33058
SUBJECT: GRB 221215B: Fermi GBM Final Real-time Localization
DATE:    22/12/15 16:19:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 16:09:34 UT on 15 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221215B (trigger 692813379.070912 / 221215673).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 23.2, Dec = 32.0 (J2000 degrees, equivalent to J2000 01h 32m, 32d 00'), with a statistical uncertainty of 4.1 degrees.

The angle from the Fermi LAT boresight is 35.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221215673/quicklook/glg_skymap_all_bn221215673.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/bn221215673/quicklook/glg_healpix_all_bn221215673.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221215673/quicklook/glg_lc_medres34_bn221215673.gif


GRB_name: GRB221209A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33059
SUBJECT: IPN triangulation of GRB 221209A (long)
DATE:    22/12/15 16:29:48 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. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,

E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

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

The bright, long-duration GRB 221209A
(Fermi-GBM detection: the Fermi GBM team, GCN Circ. 33031;
Bissaldi, GCN Circ. et al., GCN Circ. 33034;
BALROG localization: Kunzweiler et al., GCN Circ. 33032;
AstroSat-CZTI detection: Gopalakrishnan et al., GCN Circ. 33037;
CALET-CGBM detection: Kawakubo et al., GCN Circ. 33049)
was detected by Fermi(GBM trigger 692257829), Konus-Wind,
INTEGRAL (SPI-ACS), AstroSat (CZTI), CALET (CGBM),
and Mars-Odyssey (HEND) at about 21024 s UT (05:50:24).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   231.643 (15h 26m 34s) +49.850 (+49d 50' 59")
  Corners:
   230.092 (15h 20m 22s) +49.310 (+49d 18' 36")
   230.747 (15h 22m 59s) +49.761 (+49d 45' 38")
   233.222 (15h 32m 53s) +50.361 (+50d 21' 41")
   232.541 (15h 30m 10s) +49.930 (+49d 55' 48")
  ---------------------------------------------
The error box area is 1573 sq. arcmin, and its maximum
dimension is 2.28 deg (the minimum one is 15.5 arcmin).
The Sun distance was 76 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM final localization (GCN 33034) and the BALROG localization 
(33032).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221209_T21024/IPN/

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


GRB_name: GRB221215B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33060
SUBJECT: Fermi GRB 221215B: Global MASTER-Net observations report 
DATE:    22/12/15 16:30:25 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 221215B ( Fermi GBM team, GCN 33058) errorbox  533 sec after notice time and 567 sec after trigger time at 2022-12-15 16:19:02 UT, with upper limit up to  19.9 mag. The observations began at zenith distance = 14 deg. The sun  altitude  is -28.7 deg. 

The galactic latitude b = -30 deg., longitude l = 134 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2184588

We obtain a following upper limits.  

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

     623 | 2022-12-15 16:19:02 |   MASTER-Kislovodsk | (01h 31m 47.44s , +32d 13m 16.9s) |   C |   110 | 19.0 |        
     623 | 2022-12-15 16:19:02 |   MASTER-Kislovodsk | (01h 37m 02.14s , +31d 49m 43.0s) |   C |   110 | 19.7 |        
     769 | 2022-12-15 16:21:13 |   MASTER-Kislovodsk | (01h 31m 52.27s , +32d 13m 24.1s) |   C |   140 | 19.2 |        
     769 | 2022-12-15 16:21:13 |   MASTER-Kislovodsk | (01h 37m 07.18s , +31d 49m 51.9s) |   C |   140 | 19.9 |        
     945 | 2022-12-15 16:23:53 |   MASTER-Kislovodsk | (01h 31m 49.96s , +32d 14m 59.3s) |   C |   170 | 19.3 |        
     945 | 2022-12-15 16:23:53 |   MASTER-Kislovodsk | (01h 37m 05.21s , +31d 51m 29.3s) |   C |   170 | 19.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221209A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33061
SUBJECT: Konus-Wind detection of GRB 221209A
DATE:    22/12/15 16:36:16 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 221209A (Fermi-GBM observation: Bissaldi, GCN 33034;
AstroSat CZTI detection: Gopalakrishnan et al., GCN Circ 33037;
IPN triangulation: Kozyrev et al., GCN 33059)
triggered Konus-Wind (KW) at T0=21024.993 s UT (05:50:24.993).

The burst light curve shows a bright, FRED-like pulse,
which starts at ~T0-0.5 s, peaks at ~T0-0.640 s,
and has a total duration of ~10 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/GRB221209_T21024/

As observed by Konus-Wind, the burst had
a fluence of (6.39 Â± 0.43)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 0.640 s,
of (4.89 Â± 0.28)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+12.302 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.64 (-0.09,+0.10),
the high energy photon index beta = -2.05 (-0.08,+0.07),
the peak energy Ep = 306 (-32,+36) keV,
chi2 = 103/97 dof.

The spectrum near the peak count rate (measured from T0+0.256 to T0+1.280 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.28 (-0.11,+0.12),
the high energy photon index beta = -1.97 (-0.07,+0.06),
the peak energy Ep = 366 (-39,+46) keV,
chi2 = 68/66 dof.

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


GRB_name: GRB221215A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33062
SUBJECT: GRB 221215A: Swift/BAT-GUANO arcminute localization
DATE:    22/12/16 05:48:32 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 221215A onboard (T0:
2022-12-15T04:14:27 UTC, Fermi/GBM GCN 33054).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst in a 4.096 s analysis time bin
with a sqrt(TS) of 11.8.

An arcminute localization is found with DeltaLLHOut of 19.7 and a
DeltaLLHPeak of 7.3.
Cross-correlation imaging also finds this source with SNR 5.5.

See Section 9.1 and Figures 10 and 17 in the NITRATES paper for brief
descriptions and interpretations of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

The BAT position is
RA, Dec = 155.056, +46.873 deg which is
   RA(J2000)  = 10h 20m 13.34s
   Dec(J2000) = +46d 52â€² 21.7â€³
with an estimated uncertainty of 3 arcmin radius.

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: GRB221215A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33063
SUBJECT: GRB 221215A: Swift ToO observations
DATE:    22/12/16 07:17:07 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 221215A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021533

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: GRB221216A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33066
SUBJECT: GRB 221216A: Fermi GBM Final Real-time Localization
DATE:    22/12/16 11:31:45 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 11:21:18 UT on 16 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221216A (trigger 692882483.183742 / 221216473).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 276.3, Dec = -58.1 (J2000 degrees, equivalent to J2000 18h 25m, -58d 06'), with a statistical uncertainty of 5.7 degrees.

The angle from the Fermi LAT boresight is 139.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221216473/quicklook/glg_skymap_all_bn221216473.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/bn221216473/quicklook/glg_healpix_all_bn221216473.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221216473/quicklook/glg_lc_medres34_bn221216473.gif


GRB_name: GRB221216A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33067
SUBJECT: GRB 221216A: Swift detection of a burst
DATE:    22/12/16 11:34:25 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

S. Dichiara (PSU), R. A. J. Eyles-Ferris (U Leicester),
J.D. Gropp (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL) and
B. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 11:21:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221216A (trigger=1144698).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 326.021, -34.405 which is 
   RA(J2000) = 21h 44m 05s
   Dec(J2000) = -34d 24' 17"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of at least 200 sec.  The peak count rate
was ~1640 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 11:22:32.6 UT, 71.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 326.0326, -34.4223 which is equivalent to:
   RA(J2000)  = 21h 44m 7.82s
   Dec(J2000) = -34d 25' 20.3"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). No
event data are yet available to determine the column density using
X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 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
0.042. 

Burst Advocate for this burst is S. Dichiara (simonedichiara55 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: GRB221216A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33068
SUBJECT: GRB 221216A: Nanshan/NEXT optical upper limits
DATE:    22/12/16 13:20:08 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 221216A detected by Swift (Dichiara et al., 
GCN 33067) using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. We obtained a series of frames in the Sloan r-band and z-band, 
starting at 11:23:09 UT on 2022-12-16, i.e., 109s after the BAT trigger.

No optical source is detected in our stacked images at the XRT position 
(Dichiara et al., GCN 33067), with upper limits as follows:

T_mid-T0 (min)    Filter   Upper limit(3-sigma)
     14.26                 r          >17.5
     14.90                 z          >16.5

calibrated with the nearby SkyMapper field and not corrected for 
Galactic extinction.


GRB_name: GRB221216A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33069
SUBJECT: GRB 221216A: Zadko observatory - Gingin optical observations
DATE:    22/12/16 13:45:05 GMT
FROM:    Bruce Gendre at UVI  <bruce.gendre@gmail.com>

B. Gendre, H. Crisp, E. Moore, F. Panther, D. Coward, J. A. Moore
(OzGrav-UWA), A. Klotz (IRAP-CNRS-OMP),
and P. Thierry (AGORA),
report:

We imaged the field of GRB 221216A detected by SWIFT
(trigger 1144698) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 1.39h after the GRB trigger.
The elevation of the field decreased from
35 degrees above horizon and weather conditions
were good.

On individual images taken between t0+4994.4s and t0+7433.4s,
we do not detect any OT with a limiting magnitude of: R > 17.5

On a co-added series of exposures between t0+4993s to t0+6613s,
we estimated a limiting magnitude of R > 19.0

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon= 10.7381 lat=-49.4597
and the galactic extinction in R band is 0.1 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB221216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33070
SUBJECT: Swift GRB 221216A: Global MASTER-Net observations report 
DATE:    22/12/16 14:42:19 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 221216A ( S. Dichiara et al., GCN 33067) errorbox  11435 sec after notice time and 11456 sec after trigger time at 2022-12-16 14:32:17 UT, with upper limit up to  15.4 mag. Observations started at twilight.  The observations began at zenith distance = 79 deg. The sun  altitude  is -9.8 deg. 

The galactic latitude b = -50 deg., longitude l = 11 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2184841

We obtain a following upper limits.  

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

   11546 |   MASTER-Kislovodsk |   C |   180 | 15.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221216A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33071
SUBJECT: GRB 221216A: Enhanced Swift-XRT position
DATE:    22/12/16 15:19:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 1446 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 221216A, 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 = 326.03022, -34.42125 which is equivalent
to:

RA (J2000): 21h 44m 7.25s
Dec (J2000): -34d 25' 16.5"

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: GRB221215A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33072
SUBJECT: GRB 221215A: Swift-XRT observations
DATE:    22/12/16 15:41:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 221215A, collecting 2.8 ks of Photon
Counting (PC) mode data between T0+97.3 ks and T0+113.8 ks. 

No X-ray sources have been detected consistent with being within 296
arcsec of the Swift/BAT-GUANO position. The 3-sigma upper limit in the
field is 0.005 ct  s^-1, corresponding to a 0.3-10 keV observed flux of
1.9e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum).

An uncatalogued was 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/00021533.

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


GRB_name: GRB221216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33073
SUBJECT: GRB 221216A: AKO Upper Limit
DATE:    22/12/16 16:32:07 GMT
FROM:    Mohammad Odeh at Al Khatim Observatory M44  <mshodeh@gmail.com>

Mohammad Odeh of Al-Khatim Observatory (AKO) operated by the International
Astronomical Center, in Abu Dhabi, UAE. 

 

We observed the field of GRB 221216A detected by FERMI (GCN 33066) and Swift
(Dichiara et al., GCN 33067) with our 0.35m f/7.7 robotic telescope. The
observation was done on 16 December 2022 from 15:17:47 to 15:32:55 (UT), 4.1
hours after the GRB trigger. We obtained multiple 180-sec exposures in Ic
filter. We did not detect any afterglow within XRT localization (Evans et
al., GCN 33071). This is consistent with the reported non-detections of (Lu
et al., GCN 33068) and (Gendre et al., GCN 33069).

 

The following upper limit was calculated using Atlas catalogue as a
reference:

----------------------------------------------------------------------------
-

JD (mid), T_mid-T0(hrs), Exposure (sec), Filter, Lim_mag

----------------------------------------------------------------------------
-

2459930.142604, 4.1, 5 x 180 (stacked), Ic, > 17.3

----------------------------------------------------------------------------
-

 

These magnitudes are not corrected for galactic extinction.

 


GRB_name: GRB221216A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33076
SUBJECT: GRB 221216A: Swift-XRT refined Analysis
DATE:    22/12/17 00:12:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

E. Ambrosi  (INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (SSDC &
INAF-OAR), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U.
Leicester) and S. Dichiara report on behalf of the Swift-XRT team:

We have analysed 6.6 ks of XRT data for GRB 221216A (Dichiara et al.
GCN Circ. 33067), from 61 s to 38.7 ks after the  BAT trigger. The data
comprise 249 s in Windowed Timing (WT) mode (the first 10 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. 33071).

The late-time light curve (from T0+4.6 ks) can be modelled with an
initial power-law decay with an index of alpha=0.30 (+0.16, -0.17),
followed by a break at T+12.4 ks to an alpha of 2.2 (+0.4, -0.3).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.58 (+/-0.03). The
best-fitting absorption column is  1.49 (+0.13, -0.12) x 10^21 cm^-2,
in excess of the Galactic value of 2.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.75 (+0.12, -0.11)
and a best-fitting absorption column of 5.1 (+2.9, -2.3) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.7 x 10^-11 (4.0 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.1 (+2.9, -2.3) x 10^20 cm^-2
Galactic foreground: 2.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.75 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
2.2, the count rate at T+24 hours will be 6.3 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/01144698.

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


GRB_name: GRB221216A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33077
SUBJECT: GRB 221216A: Fermi GBM observation
DATE:    22/12/17 09:17:16 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

"At 11:21:18.18 UT on 16 December 2022, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 221216A (trigger 692882483 / 221216473)
which was also detected by the Swift/BAT (Dichiara et al. 2022, GCN 33067)
The Fermi GBM Final Real-time Localization (GCN 33066) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 101
degrees.

The GBM light curve shows multiple peaks
with a duration (T90) of about 184 s (50-300 keV).
The time-averaged spectrum from T0-15 s to T0+173 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.58 +/- 0.18 and
the cutoff energy, parameterized as Epeak, is 94.6 +/- 8.4 keV.
It is fit equally well with a Band function with
Epeak = 82.4 +/- 12.1 keV, alpha = -0.4 +/- 0.3, and beta = -2.5 +/- 0.3.

The event fluence (10-1000 keV) in this time interval is
(6.31 +/- 0.40)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3 s in the 10-1000 keV band
is 3.7 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB221216A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33078
SUBJECT: GRB 221216A: Swift/UVOT Upper Limits
DATE:    22/12/17 16:50:13 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

Paul Kuin (MSSL/UCL) and Simone Dichiara(PSU) report on behalf
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 221116A
113 s after the BAT trigger (Dichiara et al., GCN Circ. 33067).
No optical afterglow consistent with the enhanced XRT position 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              113          263          147         >20.3
white             4797         4997          197         >20.4
u                  325          358           32         >18.3
b                 4592         6041          197         >19.7
uvw1              5618         5818          197         >19.4
uvm2              5413         5613          197         >19.4
uvw2              5003         5203          197         >19.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.042 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221218A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33082
SUBJECT: GRB 221218A: a long GRB detected by INTEGRAL
DATE:    22/12/18 21:56:21 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro.mereghetti@inaf.it>

S.Mereghetti (INAF, IASF-Milano), D.Gotz (CEA, Saclay), C.Ferrigno,
E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC,
Versoix) and J.Borkowski (CAMK, Torun) report:

a gamma ray burst lasting about 140 s has been detected by IBAS in the
IBIS/ISGRI data at 08:14:10  UT of 2022 December 18.

The refined coordinates (J2000) are:
R.A.= 350.6495 deg
DEC.=  -4.2477 deg
with an uncertainty of  1  arcmin (90% c.l.).

The burst had a peak flux of 1 ph/cm2/s (20-200 keV, 1-s integration time)
and a fluence in the same energy range of about 5e-6 erg/cmq.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB221215A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33083
SUBJECT: GRB 221215A: Fermi GBM Detection
DATE:    22/12/19 15:24:17 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

O.J. Roberts (USRA/NASA), J. Wood (NASA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 04:14:27.97 UT on 15 December 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221215A (trigger 692770472 / 221215177)
which was also detected by the Swift/BAT GUANO (DeLaunay et al. 2022, GCN 33062)
The Fermi GBM Final Real-time Localization (GCN 33054) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 53 degrees.

The GBM light curve shows a FRED-like pulse
with a duration (T90) of about 14 s (50-300 keV).
The time-averaged spectrum from T0-2 s to T0+12 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is 1.6 +/- 1.3 and
the cutoff energy, parameterized as Epeak, is 165 +/- 26 keV

The event fluence (10-1000 keV) in this time interval is
(6.8 +/- 1.2)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.7 s in the 10-1000 keV band
is 29.8 +/- 9.4 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: GRB221218A
Detection_method: IBAS
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33085
SUBJECT: GRB 221218A: KAIT Optical Upper Limit
DATE:    22/12/19 18:50:23 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on

behalf of the KAIT GRB team:


The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at

Lick Observatory, responded to INTEGRAL GRB 221218A (Mereghetti et al.,

GCN 33082) starting at 0.78 days after the burst. A total of

23x60s images were obtained in the clear (roughly R) filters.

We do not detect any optical afterglow candidate within the IBAS

position error circle (Mereghetti et al., GCN 33082), neither in

single image, nor in the co-add images. The typical limiting magnitude

of our single clear image is about 18.5 mag calibrated to the PS1 catalog.


GRB_name: GRB221218A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33086
SUBJECT: GRB 221218A: BOOTES-4/MET and OSN optical upper limits
DATE:    22/12/20 08:23:25 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, F. Aceituno, E. Fernandez-Garcia, I. Perez-Garcia, A. J. Castro-Tirado, M. D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga) 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 221218A by INTEGRAL (Mereghetti et al. GCNC 33082), we triggered the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical Observatory (China) to follow up starting on Dec. 19 at 12:52:50 UT (~1.2 day post burst). No new source is detected within the IBAS error region (Mereghetti et al. GCNC 33082) in the co-added image (6 x 60 s, clear filter) down to 19.2 mag.

Later on, we also triggered the 0.9m OSN telescope in Granada (Spain) starting on Dec. 19 at 18:02:59 UT (~1.4 day post burst). Ten images covering the IBAS error region were taken in the I-band. No optical afterglow is detected in the stacked image down to I=20.1. These results are in agreement with the non-detection reported by Lipunov et al. (GCNC 33081) and Zheng et al. (GCNC 33085).

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


GRB_name: GRB221218A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33087
SUBJECT: GRB 221218A: MITSuME Akeno optical upper limits
DATE:    22/12/20 10:21:15 GMT
FROM:    Ichiro Takahashi at Tokyo Tech  <itakahashi@hp.phys.titech.ac.jp>

I. Takahashi, M. Niwano, R. Hosokawa, K. L. Murata, Y. Imai, N. Ito,
S. Sato, N. Higuchi, M. Tateda, M. Sasada, Y. Yatsu, and N. Kawai
(Tokyo Tech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 221218A (S. Mereghetti et al. GCN
Circular #33082, WeiKang Zheng et al. GCN Circular #33085, Y.-D. Hu et
al. GCN Circular #33086) 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
2022-12-18 08:37:35 UT (1405 seconds after the INTEGRAL trigger). We
stacked the images with good conditions. We did not detect any
uncatalogued sources within the error region (S. Mereghetti et al. GCN
Circular #33082). We obtained the 5-sigma limits of the stacked images
as follows.

T0+[sec] | MID-UT | T-EXP[sec] | 5-sigma limits
------------------------------------------------------------------------------------------------
1405 | 2022-12-18 08:51:23 | 1140.0 | g'>19.1, Rc>19.0, Ic>18.4
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time

We used PS1 catalog for flux calibration. The magnitudes are expressed
in the AB system. The images were processed in real-time through the
MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73,
Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire).


GRB_name: GRB221216A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33088
SUBJECT: GRB 221216A: Detection by VZLUSAT-2
DATE:    22/12/20 13:17:55 GMT
FROM:    Jakub Ripa at Masaryk University  <245487@mail.muni.cz>

J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory),  N. Werner (Masaryk 
U.), M. Ohno (Hiroshima U.),  L. Meszaros, B. Csak (Konkoly 
Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. 
Hroch, M. Dafcikova, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, 
J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo 
(Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida 
(ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. 
Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe 
(Rikkyo U.), L. L. Kiss (Konkoly Observatory),  T. Mizuno (Hiroshima 
U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe 
(Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes 
(VZLU), I. Vertat (FEL ZCU) -- the VZLUSAT-2/GRB payload collaboration.

The long-duration GRB 221216A (Fermi/GBM detection: Dunwoody et al., GCN 
Circ. 33077; Dichiara et al., GCN Circ. 33067; GECAM-B trigger num. 105) 
was detected by the GRB detector on board of the VZLUSAT-2 3U CubeSat 
(https://www.vzlusat2.cz/en/).

The data acquisition was performed by GRB detector unit no. 1 and the 
count rate curve shows the peak time at 2022-12-16 11:21:28 UTC. The T90 
duration was measured to be 90 s with the light curve resolution of 1 s. 
The significance during T90 reaches 9.5 sigma.

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB221216A_GCN_VZLUSAT2.pdf

GRB detectors on VZLUSAT-2 are a demonstration payload for a future 
CubeSats constellation (Werner et al. Proc. SPIE 2018). Two GRB modules 
of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 
75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the 
energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 
January 13 from Cape Canaveral.


GRB_name: GRB221218A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33090
SUBJECT: GRB 221218A: 3.6m DOT optical upper limit
DATE:    22/12/21 21:44:51 GMT
FROM:    Rahul Gupta at ARIES, India  <rahulbhu.c157@gmail.com>

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


We observed the field of GRB 221218A detected by INTEGRAL (Mereghetti et al.,
GCN 33082) 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. We have taken multiple frames having an
exposure time of 300 sec in the R filter. We stacked the images after the
alignment. We do not find any evidence of an afterglow candidate inside the
INTEGRAL error circle, consistent with other non-detections (Lipunov et al.,
GCN 33081; Zheng et al., GCN 33085; Hu et al., GCN 33086; and Takahashi et
al., GCN 33087). We obtained the limiting mag of ~ 22.8 mag at ~ 2.3 days
post-detection. Despite early to late time deep optical follow-up
observations, the non-detection of the optical counterpart of GRB 221218A
indicates the dark nature of the burst, although more detailed analysis is
needed to confirm.

The limiting magnitudes quoted are not corrected for the Galactic and host
extinction in the direction of the burst. Photometric calibration is
performed using the standard stars from the USNO-B1.0 catalogue.

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: GRB221221A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33091
SUBJECT: GRB 221221A: Fermi GBM Final Real-time Localization
DATE:    22/12/21 22:49:56 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:39:30 UT on 21 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221221A (trigger 693355175.568406 / 221221944).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 81.8, Dec = 63.4 (J2000 degrees, equivalent to J2000 05h 27m, 63d 23'), with a statistical uncertainty of 2.7 degrees.

The angle from the Fermi LAT boresight is 116.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221221944/quicklook/glg_skymap_all_bn221221944.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/bn221221944/quicklook/glg_healpix_all_bn221221944.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221221944/quicklook/glg_lc_medres34_bn221221944.gif


GRB_name: GRB221221A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33092
SUBJECT: Fermi GRB 221221A: Global MASTER-Net observations report 
DATE:    22/12/22 01:45:20 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 221221A ( Fermi GBM team, GCN 33091) errorbox  889 sec after notice time and 900 sec after trigger time at 2022-12-21 22:54:31 UT, with upper limit up to  19.4 mag. The observations began at zenith distance = 50 deg. The sun  altitude  is -19.6 deg. 

The galactic latitude b = 16 deg., longitude l = 149 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2186194

We obtain a following upper limits.  

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

     931 | 2022-12-21 22:54:31 |        MASTER-Tunka | (05h 13m 04.10s , +62d 00m 46.8s) |   C |    60 | 19.1 |        
     931 | 2022-12-21 22:54:31 |        MASTER-Tunka | (05h 33m 09.63s , +62d 02m 27.4s) |   C |    60 | 19.0 |        
    1021 | 2022-12-21 22:56:01 |        MASTER-Tunka | (04h 59m 40.57s , +63d 52m 33.3s) |   C |    60 | 19.4 |        
    1021 | 2022-12-21 22:56:01 |        MASTER-Tunka | (05h 21m 04.98s , +63d 54m 10.7s) |   C |    60 | 19.4 |        
    1112 | 2022-12-21 22:57:32 |        MASTER-Tunka | (05h 34m 02.96s , +63d 54m 26.5s) |   C |    60 | 19.0 |        
    1206 | 2022-12-21 22:59:06 |        MASTER-Tunka | (05h 21m 31.91s , +65d 47m 31.1s) |   C |    60 | 19.3 |        
    1206 | 2022-12-21 22:59:06 |        MASTER-Tunka | (05h 44m 33.68s , +65d 49m 16.4s) |   C |    60 | 19.4 |        
    1296 | 2022-12-21 23:00:36 |        MASTER-Tunka | (05h 45m 26.07s , +62d 03m 08.6s) |   C |    60 | 19.0 |        
    1296 | 2022-12-21 23:00:36 |        MASTER-Tunka | (06h 05m 34.83s , +62d 04m 53.5s) |   C |    60 | 19.1 |        
    1397 | 2022-12-21 23:02:17 |        MASTER-Tunka | (05h 25m 24.08s , +60d 05m 34.7s) |   C |    60 | 18.9 |        
    1397 | 2022-12-21 23:02:17 |        MASTER-Tunka | (05h 44m 17.59s , +60d 07m 10.0s) |   C |    60 | 18.9 |        
    1488 | 2022-12-21 23:03:48 |        MASTER-Tunka | (05h 32m 12.18s , +67d 42m 58.9s) |   C |    60 | 19.1 |        
    1578 | 2022-12-21 23:05:18 |        MASTER-Tunka | (05h 07m 27.77s , +65d 46m 10.6s) |   C |    60 | 19.4 |        
    1669 | 2022-12-21 23:06:49 |        MASTER-Tunka | (05h 13m 47.63s , +60d 05m 33.9s) |   C |    60 | 18.5 |        
    1759 | 2022-12-21 23:08:19 |        MASTER-Tunka | (05h 00m 55.35s , +61d 57m 06.8s) |   C |    60 | 18.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221221A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33093
SUBJECT: GRB 221221A: AGILE detection
DATE:    22/12/22 15:24:54 GMT
FROM:    Claudio Casentini at INAF-IAPS  <claudio.casentini@inaf.it>

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

The AGILE satellite detected the GRB 221221A at T0 = 2022-12-21 22:39:30 s
(UTC), reported by Fermi/GBM (GCN #33091).

The burst is clearly visible in the AGILE scientific ratemeters of the
MiniCALorimeter, (MCAL; 0.4-100 MeV) detector. The event lasted about 5 s
and it released a total number of 6515 counts in the MCAL detector
(above a background rate of 1145 Hz). The AGILE ratemeters light curves
can be found at http://www.agilescienceapp.it/notices/GRB221221A.png.

At the T0, the event was 108.69 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.
=======================================
Dr. Claudio Casentini, PhD
INAF IAPS - Istituto di Astrofisica e Planetologia Spaziali
Via del Fosso del Cavaliere 100
00133 Roma, Italy
Tel: (+39)3392319601
Email: claudio.casentini@inaf.it
Email: claudio.casentini@roma2.infn.it
Email: claudio.casentini@gmail.com <claudio.casentini@inaf.it>
Email/Skype: clavdio89@hotmail.it


GRB_name: GRB221223A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33096
SUBJECT: GRB 221223A: Fermi GBM Final Real-time Localization
DATE:    22/12/24 00:06:24 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 23:56:06 UT on 23 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221223A (trigger 693532571.759198 / 221223997).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 353.6, Dec = -11.8 (J2000 degrees, equivalent to J2000 23h 34m, -11d 48'), with a statistical uncertainty of 8.2 degrees.

The angle from the Fermi LAT boresight is 82.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221223997/quicklook/glg_skymap_all_bn221223997.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/bn221223997/quicklook/glg_healpix_all_bn221223997.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221223997/quicklook/glg_lc_medres34_bn221223997.gif


GRB_name: GRB221223A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33099
SUBJECT: Fermi GRB 221223A: Global MASTER-Net observations report 
DATE:    22/12/24 20:15:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 221223A ( Fermi GBM team, GCN 33096) errorbox  72801 sec after notice time and 72834 sec after trigger time at 2022-12-24 20:10:01 UT, with upper limit up to  18.2 mag. The observations began at zenith distance = 61 deg. The sun  altitude  is -24.2 deg. 

The galactic latitude b = -67 deg., longitude l = 71 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2186850

We obtain a following upper limits.  

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

   72865 | 2022-12-24 20:10:01 |         MASTER-SAAO | (23h 30m 04.11s , -12d 08m 03.3s) |   C |    60 | 18.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221226A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33104
SUBJECT: GRB 221226A: Fermi GBM Final Real-time Localization
DATE:    22/12/26 16:54:45 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 16:44:27 UT on 26 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221226A (trigger 693765872.056908 / 221226698).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 68.2, Dec = 34.8 (J2000 degrees, equivalent to J2000 04h 32m, 34d 47'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 97.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221226698/quicklook/glg_skymap_all_bn221226698.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/bn221226698/quicklook/glg_healpix_all_bn221226698.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221226698/quicklook/glg_lc_medres34_bn221226698.gif


GRB_name: GRB221226A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33105
SUBJECT: Fermi GRB 221226A: Global MASTER-Net observations report 
DATE:    22/12/26 19:15:18 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 221226A ( Fermi GBM team, GCN 33104) errorbox  6665 sec after notice time and 6700 sec after trigger time at 2022-12-26 18:36:07 UT, with upper limit up to  18.0 mag. Observations started at twilight.  The observations began at zenith distance = 76 deg. The sun  altitude  is -9.8 deg. 

The galactic latitude b = -8 deg., longitude l = 166 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2187618

We obtain a following upper limits.  

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

    6730 | 2022-12-26 18:36:07 |         MASTER-SAAO | (04h 44m 22.09s , +35d 17m 23.9s) |   C |    60 | 15.0 |        
    6810 | 2022-12-26 18:37:27 |         MASTER-SAAO | (04h 28m 26.64s , +33d 24m 58.1s) |   C |    60 | 15.8 |        
    6980 | 2022-12-26 18:40:16 |         MASTER-SAAO | (04h 25m 49.17s , +35d 17m 58.7s) |   C |    60 | 16.1 |        
    7071 | 2022-12-26 18:41:48 |         MASTER-SAAO | (04h 22m 22.24s , +37d 11m 21.9s) |   C |    60 | 16.4 |        
    7162 | 2022-12-26 18:43:19 |         MASTER-SAAO | (04h 32m 21.78s , +37d 12m 39.9s) |   C |    60 | 16.6 |        
    7412 | 2022-12-26 18:47:29 |         MASTER-SAAO | (04h 41m 26.03s , +37d 12m 15.3s) |   C |    60 | 16.8 |        
    7583 | 2022-12-26 18:50:19 |         MASTER-SAAO | (04h 38m 01.88s , +33d 23m 26.3s) |   C |    60 | 17.2 |        
    7674 | 2022-12-26 18:51:51 |         MASTER-SAAO | (04h 34m 37.01s , +35d 19m 08.3s) |   C |    60 | 17.3 |        
    7764 | 2022-12-26 18:53:20 |         MASTER-SAAO | (04h 44m 24.37s , +35d 17m 47.7s) |   C |    60 | 17.2 |        
    7844 | 2022-12-26 18:54:40 |         MASTER-SAAO | (04h 28m 29.31s , +33d 24m 59.4s) |   C |    60 | 17.3 |        
    8014 | 2022-12-26 18:57:30 |         MASTER-SAAO | (04h 25m 46.26s , +35d 19m 15.9s) |   C |    60 | 17.4 |        
    8104 | 2022-12-26 18:59:01 |         MASTER-SAAO | (04h 22m 25.82s , +37d 12m 14.8s) |   C |    60 | 17.8 |        
    8195 | 2022-12-26 19:00:31 |         MASTER-SAAO | (04h 32m 20.32s , +37d 11m 24.2s) |   C |    60 | 17.7 |        
    8444 | 2022-12-26 19:04:41 |         MASTER-SAAO | (04h 41m 26.27s , +37d 11m 56.5s) |   C |    60 | 17.7 |        
    8615 | 2022-12-26 19:07:32 |         MASTER-SAAO | (04h 37m 58.66s , +33d 24m 36.4s) |   C |    60 | 18.0 |        
    8706 | 2022-12-26 19:09:02 |         MASTER-SAAO | (04h 34m 35.73s , +35d 19m 35.3s) |   C |    60 | 18.0 |        
    8785 | 2022-12-26 19:10:22 |         MASTER-SAAO | (04h 44m 29.63s , +35d 18m 45.8s) |   C |    60 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221226B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33107
SUBJECT: GRB 221226B: Fermi GBM Final Real-time Localization
DATE:    22/12/26 22:51:47 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:41:20 UT on 26 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221226B (trigger 693787285.418586 / 221226945).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 16.3, Dec = -53.0 (J2000 degrees, equivalent to J2000 01h 05m, -53d 00'), with a statistical uncertainty of 9.8 degrees.

The angle from the Fermi LAT boresight is 46.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221226945/quicklook/glg_skymap_all_bn221226945.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/bn221226945/quicklook/glg_healpix_all_bn221226945.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221226945/quicklook/glg_lc_medres34_bn221226945.gif


GRB_name: GRB221226B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33108
SUBJECT: GRB 221226B: Swift detection of a burst
DATE:    22/12/26 23:00:32 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. B. Cenko (GSFC), J.D. Gropp (PSU), J. A. Kennea (PSU),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and T. M. Parsotan (GSFC/UMBC/CRESSTII) report on
behalf of the Neil Gehrels Swift Observatory Team:

At 22:41:20 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221226B (trigger=1145959).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 22.917, -41.554 which is 
   RA(J2000) = 01h 31m 40s
   Dec(J2000) = -41d 33' 13"
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 10 sec.  The peak count rate
was ~2200 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 22:42:32.4 UT, 72.4 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 22.90890, -41.52648 which
is equivalent to:
   RA(J2000)  = 01h 31m 38.14s
   Dec(J2000) = -41d 31' 35.3"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 101 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.69
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 75 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.017. 

Burst Advocate for this burst is S. B. Cenko (brad.cenko AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB221226B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33109
SUBJECT: GRB 221226B: Enhanced Swift-XRT position
DATE:    22/12/27 03:22:35 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 1173 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 221226B, 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 = 22.90972, -41.52669 which is equivalent
to:

RA (J2000): 01h 31m 38.33s
Dec (J2000): -41d 31' 36.1"

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: GRB221226B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33110
SUBJECT: GRB 221226B: VLT/X-shooter redshift and host galaxy
DATE:    22/12/27 09:26:14 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu (NAOC), A. Chrimes (Radboud Univ.), B. Schneider (MIT),  L. Izzo 
(DARK/NBI), A. Saccardi (GEPI, Observatoire de Paris), Z.P. Zhu (NAOC, 
HUST), N.R. Tanvir (Univ. Leicester) report on behalf of the Stargate 
collaboration:

We observed the field of GRB 221226B detected by Swift (Cenko et al., 
GCN 33108) and Fermi (Fermi GBM team, GCN 33107) using the ESO VLT UT3 
(Melipal) equipped with the X-shooter spectrograph. Our spectra cover 
the wavelength range 3000-21000 AA, and consist of 4 exposures by 1200 s 
each.

The observations started at 01:10:06 UT on 2022-12-27, i.e., ~2.48 hr 
after BAT trigger. The optical afterglow of the burst is detected at 
coordinates

R.A.(J2000) = 01:31:38.036
Dec.(J2000) = - 41:31:37.25

with an uncertainty of ~0.3 arcsec and r = 22.0 +/- 0.1 mag, calibrated 
with Legacy Survey nearby stars.

A broad absorption feature is visible around 4490 AA, which we identify 
as being due to H I. From detection of multiple absorption features, 
which we interpret as being due to S II, Si II, O I, C II, Si IV, Al 
III, NV, and emission features due to [O II] and Hbeta,  we infer a 
common redshift of z = 2.694. We conclude this is the redshift of the burst.

Note that at the optical afterglow position, the Legacy Survey presents 
an extended source with r = 23.82 mag, which is likely the host galaxy 
of the burst, being consistent with the the detection of emission 
features in the X-shooter spectra.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Pascale Hibon and Ditte Slumstrup.


GRB_name: GRB221226B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33111
SUBJECT: GRB 221226B: Swift-XRT refined Analysis
DATE:    22/12/27 11:41:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR), J.A. Kennea
(PSU), A. Tohuvavohu (U. Toronto), D.N. Burrows (PSU), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), V.
D'Elia (SSDC & INAF-OAR) and S.B. Cenko report on behalf of the
Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 221226B (Cenko et al. GCN
Circ. 33108), from 56 s to 40.4 ks after the  BAT trigger. The data
comprise 14 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. 33109).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.58 (+0.13, -0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.5 (+0.4, -0.3). The
best-fitting absorption column is  7 (+23, -7) x 10^21 cm^-2, at a
redshift of 2.694, in addition to the Galactic value of 1.7 x 10^20
cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 4.3 x
10^-11 (4.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.7 x 10^20 cm^-2
Intrinsic column:    7 (+23, -7) x 10^21 cm^-2 at z=2.694
Photon index:      1.5 (+0.4, -0.3)

If the light curve continues to decay with a power-law decay index of
1.58, the count rate at T+24 hours will be 6.9 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x
10^-15 (3.2 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01145959.

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


GRB_name: GRB221226B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33112
SUBJECT: GRB 221226B: Fermi GBM Observation
DATE:    22/12/27 13:16:51 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

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

"At 22:41:20 UT on 26 December 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 221226B (trigger 693787285/221226945),
which was also detected by Swift BAT (S. B. Cenko et al. 2022, GCN 33108)
and has a measured redshift from the VLT/X-Shooter (GCN 33110). The Fermi
GBM Final Real-time Localization (GCN 33107) is consistent with the Swift
BAT position.

The angle from the Fermi LAT boresight is 58 degrees.

The GBM light curve consists of a single emission episode with a duration
(T90)
of about 5 s (50-300 keV). The time-averaged spectrum
from T0+0.002 to T0+2.592 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is 0.2 +/- 0.2 and the cutoff energy,
parameterized as Epeak, is 104 +/- 8 keV.

The event fluence (10-1000 keV) in this time interval is
(7.8 +/- 0.5)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.3 s in the 10-1000 keV band is 4.1 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB221226A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33113
SUBJECT: GRB 221226A: AGILE detection
DATE:    22/12/27 13:57:53 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the GRB 221226A at T0 = 2022-12-26 16:44:27 s
(UTC), reported by Fermi GBM (GCN #33104). The burst is 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 18 s and
it released a total number of 26728 counts in the MCAL detector (above a
background rate of 1222 Hz), and 68254 counts in the AC detector (above a
background rate of 3101 Hz). The AGILE ratemeters light curves can be found
at http://www.agilescienceapp.it/notices/GRB221226A_AGILE_RM_ND.png .
At the T0, the event was 78.3 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: GRB221226B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33114
SUBJECT: GRB 221226B: Swift-UVOT Detection
DATE:    22/12/27 17:23:08 GMT
FROM:    Noel Klingler at NASA-GSFC / UMBC  <njk5441@psu.edu>

N. Klingler (UMBC/NASA-GSFC/CRESST II) reports on behalf of the Swift/UVOT team:

The Swift-UVOT began settled observations of the field of GRB 221226B
76 s after the BAT trigger (Cenko et al., GCN Circ. 33108).  A source
consistent with the XRT position (Goad et al., GCN Circ. 33109) and consistent
with the  optical  counterpart reported by VLT/X-shooter
(Xu et al., GCN Circ. 33110) is detected in the initial UVOT exposures.

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

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

white               76          226          147         20.54 +/- 0.22
v                 4408         4608          197        >19.3
b                 3793         3993          197        >20.0
u                  288         5132          278        >20.1
w1                4818         5018          197        >20.0
m2                4613         4813          197        >19.5
w2                4204         4404          197        >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.017 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221226B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33115
SUBJECT: GRB 221226B Swift-BAT refined analysis
DATE:    22/12/27 22:22:55 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC), S. B. Cenko (GSFC),
H. A. Krimm (NSF), 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-240 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 221226B (trigger #1145959)
(Cenko, et al., GCN Circ. 33108).  The BAT ground-calculated position is
RA, Dec = 22.903, -41.515 deg which is
  RA(J2000)  =  01h 31m 36.7s
   Dec(J2000) = -41d 30' 52.5"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.

The mask-weighted light curve shows a pulse of approximately 4 seconds
total duration and some substructure.   T90 (15-350 keV) is 3.44 +- 0.57 sec
(estimated error including systematics).

The time-averaged spectrum from T+0.22 to T+4.28 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.16 +- 0.13.  The fluence in the 15-150 keV band is 5.4 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.24 sec in the 15-150 keV band
is 2.6 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1145959/BA/


GRB_name: GRB221228A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33116
SUBJECT: GRB 221228A: Fermi GBM Final Real-time Localization
DATE:    22/12/28 05:03:37 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:53:14 UT on 28 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221228A (trigger 693895999.795578 / 221228204).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 290.2, Dec = 13.8 (J2000 degrees, equivalent to J2000 19h 20m, 13d 48'), with a statistical uncertainty of 5.4 degrees.

The angle from the Fermi LAT boresight is 46.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221228204/quicklook/glg_skymap_all_bn221228204.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/bn221228204/quicklook/glg_healpix_all_bn221228204.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221228204/quicklook/glg_lc_medres34_bn221228204.gif


GRB_name: GRB221226B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33119
SUBJECT: GRB 221226B: LCOGT Optical Upper Limits
DATE:    22/12/28 22:28:46 GMT
FROM:    Robert Strausbaugh at University of Minnesota  <rstrausb@umn.edu>

R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on
behalf of a larger collaboration:

We observed the GRB 221226B (Cenko et al., GCN 33108) field with the LCOGT
1-meter Sinistro instrument at the South African Astronomical Observatory
site, on December 27, from 19:40 to 20:07 UT (corresponding to 20.98 to
21.47 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in each band.  We do not detect
any new sources in the XRT error region, in either band.

The following upper limits are calculated using the SkyMapper catalog as
reference:

r > 20.75
i > 20.16

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB221226A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33121
SUBJECT: GRB 221226A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/12/29 01:11:32 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 221126A onboard (T0:
2022-12-26T16:44:27 UTC, Fermi/GBM GCN 33104).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 25.4 in a
8.192 s analysis time bin.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -9.

See Section 9.1 and Figures 10 and 17 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: GRB221226A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33123
SUBJECT: IPN triangulation of GRB 221226A
DATE:    22/12/30 11:32:54 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. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,

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 on behalf of the GRS-Odyssey GRB team,
report:

The long-duration GRB 221226A
(Fermi-GBM detection, the Fermi GBM team, GCN Circ. 33104;
AGILE detection: Panebianco et al., GCN Circ. 33113;
Swift/BAT-GUANO detection: Raman et al., GCN Circ. 33121)
was detected by Fermi(GBM trigger 693765872), AGILE,
Konus-Wind, and INTEGRAL (SPI-ACS), Swift (BAT),
and Mars-Odyssey (HEND) at about 60267 s UT (16:44:27).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    66.901 (04h 27m 36s) +36.975 (+36d 58' 30")
  Corners:
    69.415 (04h 37m 40s) +37.331 (+37d 19' 50")
    64.543 (04h 18m 10s) +37.133 (+37d 07' 58")
    64.358 (04h 17m 26s) +36.223 (+36d 13' 23")
    69.171 (04h 36m 41s) +36.500 (+36d 30' 00")
  ---------------------------------------------
The error box area is 3.3 sq. deg, and its maximum
dimension is 4.2 deg (the minimum one is 51 arcmin).
The Sun distance was 150 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221226_T60271/IPN

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


GRB_name: GRB221226A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33125
SUBJECT: GRB 221226A: Fermi GBM detection
DATE:    22/12/30 16:17:59 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 16:44:27.06 UT on 26 December 2022, the Fermi Gamma-Ray Burst
Monitor (GBM) triggered and located GRB 221226A (trigger 693765872 /
221226698) which was also detected by the AGILE (Panebianco et al.,
GCN 33113) and  Swift/BAT (Raman et al., GCN 33121). The Fermi GBM
Final Real-time Localization was reported in GCN 33104, and it is
consistent with the IPN triangulation (Kozyrev et al., GCN 33123)

The GBM light curve consists of two emission episodes with a duration
(T90) of about 129 s (50-300 keV). The time-averaged spectrum from
T0-3 s to T0+129 s is best fit by a power law function with an
exponential high-energy cutoff.  The power law index is -1.18 +/- 0.03
and the cutoff energy, parameterized as Epeak, is 340 +/- 32 keV.

The event fluence (10-1000 keV) in this time interval is (2.98 +/-
0.10)E-5 erg/cm^2. The 1-sec peak photon flux measured starting from
T0+4.8 s in the 10-1000 keV band is 20.7 +/- 0.4 ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak= 229 +/- 35
keV, alpha = -1.10 +/- 0.05 and beta = -1.90 +/- 0.08.


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

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


GRB_name: GRB221231A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33129
SUBJECT: GRB 221231A: Fermi GBM Final Real-time Localization
DATE:    22/12/31 21:57:19 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 21:46:05 UT on 31 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221231A (trigger 694215970.129412 / 221231907).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 332.7, Dec = 36.5 (J2000 degrees, equivalent to J2000 22h 10m, 36d 30'), with a statistical uncertainty of 5.2 degrees.

The angle from the Fermi LAT boresight is 50.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221231907/quicklook/glg_skymap_all_bn221231907.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/bn221231907/quicklook/glg_healpix_all_bn221231907.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221231907/quicklook/glg_lc_medres34_bn221231907.gif


GRB_name: GRB230101A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33130
SUBJECT: GRB 230101A: Fermi GBM Final Real-time Localization
DATE:    23/01/01 02:26:46 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 02:16:38 UT on 1 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230101A (trigger 694232203.998664 / 230101095).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 206.3, Dec = -21.9 (J2000 degrees, equivalent to J2000 13h 45m, -21d 53'), with a statistical uncertainty of 2.8 degrees.

The angle from the Fermi LAT boresight is 49.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230101095/quicklook/glg_skymap_all_bn230101095.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230101095/quicklook/glg_healpix_all_bn230101095.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230101095/quicklook/glg_lc_medres34_bn230101095.gif


GRB_name: GRB221231A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33132
SUBJECT: GRB 221231A: Swift/BAT-GUANO arcminute localization of a possibly short burst
DATE:    23/01/01 06:08:19 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Swift/BAT did not localize GRB 221231A onboard (T0:
2022-12-31T21:46:05 UTC, Fermi/GBM GCN 33129).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst in a 0.256 s analysis time bin
with a sqrt(TS) of 14.
An arcminute localization is found with DeltaLLHOut of 18.2 and a
DeltaLLHPeak of 7.9.

The burst duration as seen by BAT is less than 0.5 seconds.

See Section 9.1 and Figures 10 and 17 in the NITRATES paper for brief
descriptions and interpretations of sqrt(TS), DeltaLLHPeak, and
DeltaLLHOut.

The BAT position is
RA, Dec = 336.260, +25.138 deg which is
   RA(J2000)  = 22h 25m 02.47s
   Dec(J2000) = +25d 08â€² 18.6â€³
with an estimated uncertainty of 5 arcmin radius.

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: GRB221231A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33133
SUBJECT: GRB 221231A: Swift ToO observations
DATE:    23/01/01 06:37:59 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 221231A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021534

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: GRB221231A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33135
SUBJECT: GRB 221231A: Swift-XRT observations
DATE:    23/01/01 16:54:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (SSDC & INAF-OAR), A. Tohuvavohu (U. Toronto), D.N. Burrows
(PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR),
B. Sbarufatti (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 221231A, collecting 5.0 ks of Photon
Counting (PC) mode data between T0+32.4 ks and T0+44.3 ks. 

Five uncatalogued X-ray sources have been detected, however none of
them is above the RASS limit or shows definitive signs of fading.
Therefore, at the present time we cannot identify which, if any, is the
afterglow. Sources 2 and 5 are inside the error box of Swift/BAT-GUANO,
but source 5 is associated with a known source. Details of these
sources are given below:

Source 1:
  RA (J2000):  336.3458  =  22:25:22.98
  Dec (J2000): +25.1723  =  +25:10:20.3
  Error: 6.5 arcsec (radius, 90% conf.)
  Count-rate: (9.1 [+7.3, -5.4])e-4 ct s^-1   
  Distance: 303 arcsec from Swift/BAT-GUANO position.

Source 2:
  RA (J2000):  336.2560  =  22:25:1.44
  Dec (J2000): +25.1298  =  +25:07:47.2
  Error: 3.1 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.0107 [+0.0022, -0.0020] ct s^-1   
  Distance: 34 arcsec from Swift/BAT-GUANO position.
  Flux: (5.44 [+1.13, -1.00])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 3:
  RA (J2000):  336.2019  =  22:24:48.46
  Dec (J2000): +25.0298  =  +25:01:47.3
  Error: 5.4 arcsec (radius, 90% conf.)
  Count-rate: (1.87 [+0.97, -0.73])e-3 ct s^-1  
  Distance: 435 arcsec from Swift/BAT-GUANO position.
  Flux: (7.8 [+4.0, -3.1])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 4:
  RA (J2000):  336.2146  =  22:24:51.50
  Dec (J2000): +25.2635  =  +25:15:48.7
  Error: 8.9 arcsec (radius, 90% conf.)
  Count-rate: (1.48 [+0.87, -0.64])e-3 ct s^-1  
  Distance: 474 arcsec from Swift/BAT-GUANO position.
  Flux: (2.7 [+1.6, -1.2])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 5:
  RA (J2000):  336.2452  =  22:24:58.84
  Dec (J2000): +25.1872  =  +25:11:14.1
  Error: 5.7 arcsec (radius, 90% conf.)
  Count-rate: (5.6 [+1.8, -1.5])e-3 ct s^-1   
  Distance: 182 arcsec from Swift/BAT-GUANO position.
  Flux: (1.12 [+0.37, -0.30])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021534.

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


GRB_name: GRB221231A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33136
SUBJECT: GRB 221231A: AKO Upper Limit
DATE:    23/01/01 17:47:10 GMT
FROM:    Mohammad Odeh at Al Khatim Observatory M44  <mshodeh@gmail.com>

Mohammad Odeh of Al-Khatim Observatory (AKO) operated by the International
Astronomical Center, in Abu Dhabi, UAE. 

 

As a follow up for the GRB 221231A detected by Fermi/GBM (GCN 33129) and the
observations of the Swift/BAT-GUANO (Perri et al., GCN 33135), we observed
the localization of the five detected uncatalogued X-ray sources mentioned
in GCN 33135. Our observation was done with our 0.36m f/7.7 robotic
telescope on 01 January 2023 around 15:27 (UT), 17.7 hours after the GRB
trigger. We obtained multiple 180-sec exposures in Ic filter. We did not
detect any afterglow within the mentioned locations. 

 

The following upper limit was calculated using Atlas catalogue as a
reference:

----------------------------------------------------------------------------
-

JD (mid), T_mid-T0(hrs), Exposure (sec), Filter, Lim_mag

----------------------------------------------------------------------------
-

2459946.143993, 17.7, 5 x 180 (stacked), Ic, > 18.8

----------------------------------------------------------------------------
-

 

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB230102A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33137
SUBJECT: GRB 230102A: Fermi GBM Final Real-time Localization
DATE:    23/01/02 00:32:32 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 00:22:12 UT on 2 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230102A (trigger 694311737.966744 / 230102015).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 272.8, Dec = -35.1 (J2000 degrees, equivalent to J2000 18h 11m, -35d 06'), with a statistical uncertainty of 4.0 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/2023/bn230102015/quicklook/glg_skymap_all_bn230102015.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230102015/quicklook/glg_healpix_all_bn230102015.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230102015/quicklook/glg_lc_medres34_bn230102015.gif


GRB_name: GRB230102A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33138
SUBJECT: GRB 230102A: AGILE/MCAL detection
DATE:    23/01/02 11:07:23 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE Mini-CALorimeter (MCAL) detected the GRB 230102A at T0 =
2023-01-02 00:22:12.97 +/- 0.01 s (UTC), reported by Fermi GBM (GCN #33137).

The event lasted about 0.16 s and released a total number of 219 counts in
the MCAL detector (in the 0.4-100 MeV energy range), above an average
background rate of 489 Hz. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB230102A_081632_599703732.970000.png
. The time-integrated spectrum of the burst, from T0-0.032 s to T0+0.128 s,
can be fitted in the energy range 0.4-2 MeV with a power-law with ph.ind. =
-2.48 (-0.46,+0.51), resulting in a reduced chi-squared of 0.85 (21 d.o.f.)
and a fluence of 1.07e-06 erg/cm^2 (90% confidence level), in the same
energy range. At the T0, the event was 100 deg off-axis.

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: GRB221231A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33139
SUBJECT: GRB 221231A: Swift-XRT afterglow detection
DATE:    23/01/02 11:54:58 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (SSDC & INAF-OAR), A. Tohuvavohu (U. Toronto), D.N. Burrows
(PSU), J. D. Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR),
B. Sbarufatti (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf
of the Swift-XRT team:

Swift-XRT has conducted further observations of the field of the
Swift/BAT-GUANO-detected burst GRB 221231A. The observations now extend
from T0+32.7 ks to T0+120.0 ks. 

Of the sources reported by Perri et al. (GCN Circ. 33135), "Source 2"
is fading with >3-sigma significance, and is therefore likely the GRB
afterglow. Using 4154 s of PC mode data and 2 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 336.25600, +25.12978
which is equivalent to:

RA (J2000): 22h 25m 01.44s
Dec(J2000): +25d 07' 47.2"

with an uncertainty of 3.0 arcsec (radius, 90% confidence). This
position is 34 arcsec from the Swift/BAT-GUANO position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.1 (+0.6, -0.5).

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/ToO_GRBs/00021534/Source2.php.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021534.

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


GRB_name: GRB230101A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33141
SUBJECT: GRB 230101A: AstroSat CZTI detection
DATE:    23/01/03 10:56:14 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

P. K. Navaneeth (IUCAA), R. Gopalakrishnan (IUCAA), G. Waratkar (IITB), 
A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka 
University/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 the detection of a long GRB 230101A which was 
also detected by Fermi GBM (GCN Circ. 33130).

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 
2023-01-01 02:16:48.5 UTC. The measured peak count rate associated with 
the burst is 183 (+18, -16) counts/s above the background in the 
combined data of all quadrants, with a total of 4974 (+674, -726) 
counts. The local mean background count rate was 435 (+1, -1) counts/s. 
Using cumulative rates, we measure a T90 of 81 (+12, -27) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2023-01-01 
02:16:42.7 UTC. The measured peak count rate is 830 (+65, -61) counts/s 
above the background in the combined Veto data of all quadrants, with a 
total of 14726 (+2045, -2365) counts. The local mean background count 
rate was 7515 (+5, -5) counts/s. We measure a T90 of 27 (+17, -8) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB230102A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33143
SUBJECT: GRB 230102A: Detection by GRBAlpha
DATE:    23/01/03 16:43:28 GMT
FROM:    Marianna Dafcikova at Masaryk University  <500025@mail.muni.cz>

M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal,  A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory),  T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Os
 aka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The short-duration GRB 230102A (Fermi/GBM detection: GCN Circ. 33137; AGILE/MCAL detection: GCN Circ. 33138) was observed by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The detection was confirmed at the peak time 2023-01-02 00:22:13 UTC. The light curve observed by GRBAlpha shows a spike within one 1 s bin. The SNR reaches 5.6.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB230102A_GCN.pdf

All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ 
GRBAlpha is a demonstration mission for a future CubeSats constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. GRBAlpha was launched on 2021 March 22 from Baikonur. After its commissioning phase, the scientific observations are now under way. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.


GRB_name: GRB221230A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33145
SUBJECT: GRB 221230A: CALET Gamma-Ray Burst Monitor detection
DATE:    23/01/04 04:28:35 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

K. Yamaoka (Nagoya U), A. Yoshida, T. Sakamoto,
S. Sugita (AGU), Y. Kawakubo (LSU), 
S. Nakahira (RIKEN), Y. Asaoka (ICRR),
S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 221230A (Wind-KONUS Notice at 03:34:17.508 on 30 December) 
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 03:34:17.34 UTC 
on December 30, 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1356406433/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure that starts
at T+0.6 sec, and peaks at T+16.0 sec and ends at T+21.7 sec.
The T90 and T50 durations measured by the SGM data are 18.6 +/- 0.9 sec
and 13.5 +/- 0.5 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

 http://cgbm.calet.jp/cgbm_trigger/ground/1356406433/index.html

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


GRB_name: GRB221231A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33146
SUBJECT: GRB 221231A: Fermi GBM Observation
DATE:    23/01/04 05:01:54 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 21:46:05 UT on 31 December 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 221231A (trigger 694215970/221231907).
which was also detected by Swift BAT (A. Tohuvavohu et al. 2023, GCN 33132)
and Swift XRT GCN (M. Perri et al. 2023, 33139).
The Fermi GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight is 61 degrees.

The GBM light curve consists of a single emission episode with a duration
(T90)
of about 5 s (50-300 keV). The time-averaged spectrum
from T0-0.06 to T0+4.93 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.2 +/- 0.4 and the cutoff energy,
parameterized as Epeak, is 200 +/- 40 keV.

The event fluence (10-1000 keV) in this time interval is
(4.4 +/- 0.4)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0 s in the 10-1000 keV band is 3.9 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB230102A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33147
SUBJECT: GRB 230102A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    23/01/04 05:32:28 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 230102A onboard (T0:
2022-12-26T00:22:12 UTC, Fermi/GBM GCN 33137, AGILE GCN 33138,
GRBAlpha GCN 33143).

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 2022, ApJ,
941, 169), detects the burst with a sqrt(TS) of 29.2 in a 0.128 s
analysis time bin.

NITRATES results indicate a burst coming from outside the coded FOV,
with DeltaLLHOut of -6.

See Section 9.1 and Figures 10 and 17 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: GRB230104A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33148
SUBJECT: GRB 230104A: AGILE/MCAL detection of a burst
DATE:    23/01/04 09:40:45 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), 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),
A. Addis, L. Baroncelli, A. Bulgarelli, A. Di Piano, V. Fioretti, G.
Panebianco, N. Parmiggiani (INAF/OAS-Bologna), F. Lucarelli, C. Pittori, F.
Verrecchia (SSDC, and INAF/OAR), M. Romani (INAF/OA-Brera), M. Marisaldi
(INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois
(INAF/OA-Cagliari), I. Donnarumma (ASI), A. Giuliani (INAF/IASF-Mi), and P.
Tempesta (TeleSpazio), report on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected a burst at T0 = 2023-01-04
06:03:15.00 +/- 0.01 s (UTC). The event lasted about 1.10 s and released a
total number of 2073 counts in the MCAL detector (in the 0.4-100 MeV energy
range), above an average background rate of 594 Hz. The MCAL light curve
can be found at
http://www.agilescienceapp.it/notices/GRB230104A_081663_599896995.000000.png
.

The burst is also visible in the AGILE scientific ratemeters of the
MiniCALorimeter (MCAL; 0.4-100 MeV), and AntiCoincidence (AC; 50-200 keV)
detectors, where it released a total number of 6525 counts in the MCAL
detector (above a background rate of 1200 Hz), and 13285 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/GRB230104A_AGILE_RM_D.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: GRB221231A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33149
SUBJECT: GRB 221231A: 3.6m DOT optical upper limit
DATE:    23/01/04 13:56:14 GMT
FROM:    Amit Kumar Ror at ARIES  <mitturor77894@gmail.com>

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

We observed the field of GRB 221231A detected by Fermi/GBM (2022, GCN
33129) using the 3.6m Devasthal Optical Telescope of ARIES Nainital. We
have taken multiple frames having an exposure time of 200 sec in the r
filter. We stacked the images after the alignment. We did not find any
evidence of an afterglow candidate inside the Swift XRT error circle (Perri
et al. 2023, GCNs 33135 and 33139). We obtained the limiting mag of ~ 21.7
mag at ~ 1.87 days post-detection. The non-detection of the optical
afterglow is consistent with Odeh 2023, GCN 32876.

The limiting magnitudes quoted are not corrected for the Galactic and host
extinction in the direction of the burst. Photometric calibration is
performed using the standard stars from the Pan-STARRS catalog.

This circular may be cited. 3.6m Devasthal Optical Telescope (DOT) is a
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). The authors of this GCN circular thankfully
acknowledge the consistent support from the staff members to run and
maintain the 3.6m DOT.


GRB_name: GRB230102A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33151
SUBJECT: GRB 230102A: Fermi GBM Observation
DATE:    23/01/05 18:21:17 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

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

"At 00:22:13 UT on 02 January 2023, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 230102A (trigger 694311737/230102015).
which was also detected by Swift/BAT-GUANO (J. DeLaunay et al. 2023, GCN 33147),
GRBAlpha (M. Dafcikova et al 2023, GCN 33143) and AGILE (A. Ursi et al. 2023, GCN 33138).
The Fermi GBM Localization was reported in GCN 33137.

The angle from the Fermi LAT boresight is 65 degrees.

The GBM light curve consists of a single peak with a duration (T90)
of about 0.18 s (50-300 keV). The time-averaged spectrum
from T0-0.06 to T0+0.19 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.94 +/- 0.05 and the cutoff energy,
parameterized as Epeak, is 1508 +/- 260 keV.

The event fluence (10-1000 keV) in this time interval is
(1.43 +/- 0.05)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0 s in the 10-1000 keV band is 36 +/- 1 ph/s/cm^2.

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

For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
FSSC: Data  Data Access  GBM - Fermi Gamma-ray Space Telescope<https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/>
ID Name Description; GS-106: GBM Burst Catalog Entry: Parameters describing the burst (e.g., durations, fluences). This file is used to create GBM Burst Catalog.: GS-109
fermi.gsfc.nasa.gov


GRB_name: GRB230106A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33155
SUBJECT: GRB 230106: AstroSat LAXPC detection
DATE:    23/01/11 04:54:09 GMT
FROM:    Tilak Katoch at TIFR  <tilak@tifr.res.in>

Tilak Katoch, H. M. Antia and Parag Shah TIFR, Mumbai, India.

Analysis of AstroSat LAXPC data showed the clear detection of a long

GRB 230106. The lightcurve shows the multiple burst profile with the 
peak triggered

at T0 = 00h 55m 22s UT on 06 Jan 2023. The satellite was in a normal 
operating mode

and well before the entry into the SAA region. The lightcurve has a 
burst profile with

T90 =~ 77 sec. The strongest peak measured has a count rate above the 
background

with 876 +/- 35 count/sec in LAXPC10 and 1083 +/- 36 count/sec in 
LAXPC20 at T0+23 sec.

Both LAXPC instruments (LAXPC10 and LAXPC20) have registered this burst 
profile in the

light curve. For LAXPC20, the nominal energy range is 3-100 keV, but due 
to the lower gain

in LAXPC10 the energy range is about 30-400 keV.

The background subtracted lightcurve with 1 sec time-bin is available at 
the website:

https://www.tifr.res.in/~astrosat_laxpc/grb230106lc.jpg

LAXPC was built by TIFR in collaboration with the Indian Space Research 
Organisation.

The Indian Space Research Organisation funded, managed and facilitated 
the project.


GRB_name: GRB230111A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33156
SUBJECT: GRB 230111A: Fermi GBM Final Real-time Localization
DATE:    23/01/11 19:18:06 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 19:07:42 UT on 11 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230111A (trigger 695156867.898656 / 230111797).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 316.1, Dec = -22.5 (J2000 degrees, equivalent to J2000 21h 04m, -22d 30'), with a statistical uncertainty of 8.9 degrees.

The angle from the Fermi LAT boresight is 100.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230111797/quicklook/glg_skymap_all_bn230111797.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230111797/quicklook/glg_healpix_all_bn230111797.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230111797/quicklook/glg_lc_medres34_bn230111797.gif


GRB_name: GRB230111A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33157
SUBJECT: GRB 230111A: MAXI/GSC detection
DATE:    23/01/12 00:28:35 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

K. Setoguchi(Kyoto U.), T. Mihara (RIKEN), M. Serino (AGU),
H. Negoro, M. Nakajima, K. Kobayashi, M. Tanaka, Y. Soejima (Nihon U.),
T. Kawamuro, S. Yamada, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU),
Y. Tsuboi, J. Kohara, S. Urabe, S. Nawa, N. Nemoto (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. Kurihara (JAXA),
Y. Ueda, S. Ogawa, T. Yoshitake, K. Inaba, Y. Nakatani (Kyoto U.),
M. Yamauchi, T. Sato, R. Hatsuda, R. Fukuoka, Y. Hagiwara, Y. Umeki (Miyazaki U.),
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU),
M. Sugizaki (NAOC) ,
W. Iwakiri (Chiba U.)

report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source at 19:07:37 UT on 11 Jan 2023.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (320.188 deg, -30.577 deg) = (21 20 45, -30 34 36) (J2000)
with a 90% C.L. statistical error of 0.22 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius).
Without assumptions on the source constancy, we obtain a rectangular error box for the transient source with the following corners.
(319.214, -30.721) deg = (21 16 51, -30 43 15) (J2000)
(319.406, -31.127) deg = (21 17 37, -31 07 37) (J2000)
(321.653, -30.323) deg = (21 26 36, -30 19 22) (J2000)
(321.454, -29.920) deg = (21 25 48, -29 55 12) (J2000)
The X-ray flux averaged over the scan was 230 +- 30 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at 17:34 UT
and in the next transit at 20:40 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB230112A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33158
SUBJECT: GRB 230112A: Fermi GBM Final Real-time Localization
DATE:    23/01/12 08:23:03 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 08:12:32 UT on 12 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230112A (trigger 695203957.49759 / 230112342).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 62.4, Dec = -3.4 (J2000 degrees, equivalent to J2000 04h 09m, -3d 23'), with a statistical uncertainty of 15.2 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/2023/bn230112342/quicklook/glg_skymap_all_bn230112342.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230112342/quicklook/glg_healpix_all_bn230112342.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230112342/quicklook/glg_lc_medres34_bn230112342.gif


GRB_name: GRB230112A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33160
SUBJECT: Fermi GRB 230112A: Global MASTER-Net observations report 
DATE:    23/01/12 12:15:29 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 230112A ( Fermi GBM team, GCN 33158) errorbox  8076 sec after notice time and 8115 sec after trigger time at 2023-01-12 10:27:47 UT, with upper limit up to  19.1 mag. Observations started at twilight.  The observations began at zenith distance = 71 deg. The sun  altitude  is -9.7 deg. 

The galactic latitude b = -37 deg., longitude l = 196 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2191573

We obtain a following upper limits.  

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

    8145 | 2023-01-12 10:27:47 |        MASTER-Tunka | (05h 08m 15.47s , +04d 53m 17.7s) |   C |    60 | 15.8 |        
    8326 | 2023-01-12 10:30:48 |        MASTER-Tunka | (05h 07m 28.92s , +02d 59m 26.0s) |   C |    60 | 17.2 |        
    8418 | 2023-01-12 10:32:20 |        MASTER-Tunka | (05h 07m 09.16s , +01d 07m 12.6s) |   C |    60 | 17.0 |        
    8599 | 2023-01-12 10:35:21 |        MASTER-Tunka | (04h 51m 50.90s , +01d 07m 37.3s) |   C |    60 | 17.5 |        
    8691 | 2023-01-12 10:36:53 |        MASTER-Tunka | (04h 52m 19.46s , +03d 00m 43.7s) |   C |    60 | 17.7 |        
    8782 | 2023-01-12 10:38:24 |        MASTER-Tunka | (05h 06m 58.53s , -00d 48m 29.0s) |   C |    60 | 17.5 |        
    9096 | 2023-01-12 10:43:38 |        MASTER-Tunka | (05h 00m 31.34s , +06d 43m 49.0s) |   C |    60 | 18.1 |        
    9280 | 2023-01-12 10:46:42 |        MASTER-Tunka | (05h 08m 16.67s , +04d 55m 35.8s) |   C |    60 | 18.2 |        
    9280 | 2023-01-12 10:46:42 |        MASTER-Tunka | (04h 59m 34.83s , +04d 49m 50.9s) |   C |    60 | 18.2 |        
    9463 | 2023-01-12 10:49:45 |        MASTER-Tunka | (05h 07m 26.75s , +03d 02m 08.1s) |   C |    60 | 17.9 |        
    9464 | 2023-01-12 10:49:46 |        MASTER-Tunka | (04h 58m 46.81s , +02d 56m 25.9s) |   C |    60 | 18.0 |        
    9556 | 2023-01-12 10:51:18 |        MASTER-Tunka | (05h 07m 08.33s , +01d 07m 11.3s) |   C |    60 | 17.8 |        
    9556 | 2023-01-12 10:51:18 |        MASTER-Tunka | (04h 58m 29.90s , +01d 01m 30.8s) |   C |    60 | 18.1 |        
    9741 | 2023-01-12 10:54:23 |        MASTER-Tunka | (04h 51m 57.86s , +01d 06m 42.8s) |   C |    60 | 18.4 |        
    9741 | 2023-01-12 10:54:23 |        MASTER-Tunka | (04h 43m 17.97s , +01d 00m 58.8s) |   C |    60 | 18.7 |        
    9832 | 2023-01-12 10:55:54 |        MASTER-Tunka | (04h 52m 16.99s , +03d 02m 23.3s) |   C |    60 | 18.6 |        
    9832 | 2023-01-12 10:55:54 |        MASTER-Tunka | (04h 43m 35.15s , +02d 56m 37.7s) |   C |    60 | 18.7 |        
    9922 | 2023-01-12 10:57:24 |        MASTER-Tunka | (05h 07m 02.90s , -00d 47m 18.8s) |   C |    60 | 18.4 |        
    9922 | 2023-01-12 10:57:24 |        MASTER-Tunka | (04h 58m 25.31s , -00d 52m 58.4s) |   C |    60 | 18.3 |        
   10239 | 2023-01-12 11:02:41 |        MASTER-Tunka | (05h 00m 21.63s , +06d 43m 53.7s) |   C |    60 | 18.7 |        
   10419 | 2023-01-12 11:05:41 |        MASTER-Tunka | (05h 08m 17.85s , +04d 55m 49.1s) |   C |    60 | 18.7 |        
   10419 | 2023-01-12 11:05:41 |        MASTER-Tunka | (04h 59m 30.84s , +04d 50m 02.5s) |   C |    60 | 18.5 |        
   10600 | 2023-01-12 11:08:42 |        MASTER-Tunka | (05h 07m 33.92s , +03d 01m 23.7s) |   C |    60 | 18.6 |        
   10601 | 2023-01-12 11:08:43 |        MASTER-Tunka | (04h 58m 49.72s , +02d 55m 37.5s) |   C |    60 | 18.5 |        
   10691 | 2023-01-12 11:10:13 |        MASTER-Tunka | (05h 07m 06.67s , +01d 08m 44.0s) |   C |    60 | 18.5 |        
   10691 | 2023-01-12 11:10:13 |        MASTER-Tunka | (04h 58m 24.81s , +01d 02m 59.1s) |   C |    60 | 18.5 |        
   10872 | 2023-01-12 11:13:14 |        MASTER-Tunka | (04h 51m 58.31s , +01d 09m 02.7s) |   C |    60 | 19.0 |        
   10873 | 2023-01-12 11:13:15 |        MASTER-Tunka | (04h 43m 15.32s , +01d 03m 15.8s) |   C |    60 | 19.1 |        
   10965 | 2023-01-12 11:14:47 |        MASTER-Tunka | (04h 52m 14.16s , +03d 02m 15.7s) |   C |    60 | 18.9 |        
   10965 | 2023-01-12 11:14:47 |        MASTER-Tunka | (04h 43m 28.99s , +02d 56m 27.4s) |   C |    60 | 18.7 |        
   11055 | 2023-01-12 11:16:17 |        MASTER-Tunka | (05h 07m 00.75s , -00d 44m 50.0s) |   C |    60 | 18.3 |        
   11056 | 2023-01-12 11:16:18 |        MASTER-Tunka | (04h 58m 20.69s , -00d 50m 32.9s) |   C |    60 | 18.3 |        
   11239 | 2023-01-12 11:19:21 |        MASTER-Tunka | (05h 13m 34.42s , -00d 52m 29.3s) |   C |    60 | 18.2 |        
   11420 | 2023-01-12 11:22:22 |        MASTER-Tunka | (05h 13m 38.25s , +01d 03m 33.5s) |   C |    60 | 18.4 |        
   11604 | 2023-01-12 11:25:26 |        MASTER-Tunka | (04h 45m 10.84s , +06d 45m 37.8s) |   C |    60 | 18.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230111A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33162
SUBJECT: GRB 230111A: Fermi GBM Observation
DATE:    23/01/12 17:54:28 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

O.J. Roberts (USRA) and C. Meegan (UAH) report on
behalf of the Fermi Gamma-ray Burst Monitor Team:

"At 19:07:42.90 UT on 11 January 2023, the Fermi
Gamma-ray Burst Monitor (GBM) triggered and located
GRB 230111A (trigger 695156867/230111797), which was
also detected by MAXI (K. Setoguchi et al. 2023, GCN 33157).
The Fermi GBM Localization reported in GCN 33156 is consistent
with the MAXI location.

The angle from the Fermi LAT boresight is 108 degrees.

The GBM light curve consists of a single peak with a duration (T90)
of about 9 s (50-300 keV). The time-averaged spectrum
from T0-3.6 to T0+4.8 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.31 +/- 0.30 and the cutoff energy,
parameterized as Epeak, is 122 +/- 16 keV.

The event fluence (10-1000 keV) in this time interval is
(1.16 +/- 0.12)E-06 erg/cm^2. The measured 1-s peak photon flux
starting from T0-0.9 s in the 10-1000 keV band is 2.6 +/- 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: GRB230114A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33168
SUBJECT: GRB 230114A: Fermi GBM Final Real-time Localization
DATE:    23/01/14 17:09:30 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 16:59:13 UT on 14 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230114A (trigger 695408358.896514 / 230114708).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 236.3, Dec = 3.9 (J2000 degrees, equivalent to J2000 15h 45m, 3d 53'), with a statistical uncertainty of 2.5 degrees.

The angle from the Fermi LAT boresight is 80.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230114708/quicklook/glg_skymap_all_bn230114708.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230114708/quicklook/glg_healpix_all_bn230114708.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230114708/quicklook/glg_lc_medres34_bn230114708.gif


GRB_name: GRB230114A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33170
SUBJECT: GRB 230114A: Detection by VZLUSAT-2
DATE:    23/01/14 22:02:01 GMT
FROM:    Jakub Ripa at Masaryk University  <245487@mail.muni.cz>

J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory),  N. Werner (Masaryk 
U.), M. Ohno (Hiroshima U.),  L. Meszaros, B. Csak (Konkoly 
Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. 
Hroch, M. Dafcikova, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, 
J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo 
(Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida 
(ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. 
Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe 
(Rikkyo U.), L. L. Kiss (Konkoly Observatory),  T. Mizuno (Hiroshima 
U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe 
(Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes 
(VZLU), I. Vertat (FEL ZCU)  -- the VZLUSAT-2/GRB payload collaboration.

The long-duration GRB 230114A (Fermi/GBM detection: The Fermi GBM team, 
GCN Circ. 33168; INTEGRAL/SPI-ACS detection peak at 2023-01-14 ~16:59:14 
UT) was detected by the GRB detector on board of the VZLUSAT-2 3U 
CubeSat (https://www.vzlusat2.cz/en/).

The data acquisition was performed by GRB detector unit no. 1 and the 
detection was confirmed at the peak time 2023-01-14 16:59:17 UTC. The 
T90 duration was measured to be 5 s with the light curve resolution of 1 
s. The significance during T90 reaches 6.7 sigma.

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB230114A_GCN_VZLUSAT2.pdf

All VZLUSAT-2 detections are listed at: 
https://monoceros.physics.muni.cz/hea/VZLUSAT-2/
The GRB detectors on VZLUSAT-2 are a demonstration payload for a future 
constellation of CubeSats (Werner et al. Proc. SPIE 2018). Two GRB 
modules of VZLUSAT-2 are placed in a perpendicular manner and each 
consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, 
covering the energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was 
launched on 2022 January 13 from Cape Canaveral.


GRB_name: GRB230116A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33171
SUBJECT: GRB 230116A: Fermi GBM Final Real-time Localization
DATE:    23/01/16 05:05:00 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:54:34 UT on 16 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230116A (trigger 695537679.288856 / 230116205).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 81.3, Dec = -49.7 (J2000 degrees, equivalent to J2000 05h 25m, -49d 42'), with a statistical uncertainty of 2.1 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/2023/bn230116205/quicklook/glg_skymap_all_bn230116205.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230116205/quicklook/glg_healpix_all_bn230116205.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230116205/quicklook/glg_lc_medres34_bn230116205.gif


GRB_name: GRB230116B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33172
SUBJECT: GRB 230116B: Fermi GBM Final Real-time Localization
DATE:    23/01/16 09:09:37 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 08:59:06 UT on 16 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230116B (trigger 695552351.674084 / 230116374).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 113.6, Dec = -40.4 (J2000 degrees, equivalent to J2000 07h 34m, -40d 23'), with a statistical uncertainty of 2.1 degrees.

The angle from the Fermi LAT boresight is 102.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230116374/quicklook/glg_skymap_all_bn230116374.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230116374/quicklook/glg_healpix_all_bn230116374.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230116374/quicklook/glg_lc_medres34_bn230116374.gif


GRB_name: GRB230116C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33173
SUBJECT: GRB 230116C: Swift detection of a burst
DATE:    23/01/16 15:53:25 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (Adiyaman Univ.), R. A. J. Eyles-Ferris (U Leicester),
C. Gronwall (PSU), J.D. Gropp (PSU), A. Y. Lien (U Tampa),
K. L. Page (U Leicester), D. M. Palmer (LANL),
A. Tohuvavohu (U Toronto) and M. A. Williams (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 15:33:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230116C (trigger=1149250).  Due to an observing constraint,
Swift could not slew to the burst. 
The BAT on-board calculated location is 
RA, Dec 223.463, -16.871 which is 
   RA(J2000) = 14h 53m 51s
   Dec(J2000) = -16d 52' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Although this is an image trigger, the
BAT lightcurve seems to show a complex structure starting around T-50
until a pre-planned slew away from the burst location at T+30, with
a peak of ~300 counts/s (15-350 keV) near the time of the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 09:10 UT on 2023 January 18. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB230116D
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33176
SUBJECT: GRB 230116D: Swift detection of a burst
DATE:    23/01/16 21:23:25 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (Adiyaman Univ.), R. A. J. Eyles-Ferris (U Leicester),
C. Gronwall (PSU), J.D. Gropp (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (AGU) and M. A. Williams (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 21:04:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230116D (trigger=1149293).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 98.594, 49.840d which is 
   RA(J2000) = 06h 34m 23s
   Dec(J2000) =  +49d 50' 24"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Due to a communications gap the BAT
lightcurve before T+8 s is not immediately available, but
the later lightcurve indicates activity out to at least T+30 s. 

The XRT began observing the field at 21:06:54.1 UT, 130.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 98.61709, 49.87257
which is equivalent to:
   RA(J2000)  = 06h 34m 28.10s
   Dec(J2000) = +49d 52' 21.3"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 128 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.65
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 133 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.112. 

Burst Advocate for this burst is E. Sonbas (edasonbas AT yahoo.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33177
SUBJECT: GRB 230116D: Nanshan/NEXT optical afterglow detection
DATE:    23/01/16 22:26:11 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 230116B detected by Swift (Sonbas et al., 
GCN 33176) using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. Observations started at 21:06:37 UT on 2023-01-16, i.e., 114 s 
after the Swift/BAT trigger. A series of frames in the Sloan r- and z- 
filters were obtained.

An uncatalogued and decaying optical transient is detected at the 
Swift/XRT position (Sonbas et al., GCN 33176) at coordinates

R.A. (J2000) = 6:34:28.21
Dec. (J2000) = +49:52:20.38

with a positional uncertainty of ~0.3 arcsec and r ~ 19.1 mag at ~189 s 
after the BAT trigger. We thus conclude that the transient is the 
afterglow of the burst.


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33178
SUBJECT: GRB 230116D: Sintez-Newton/CrAO optical afterglow detection
DATE:    23/01/16 22:42:57 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Nazarov (CrAO), A. Pozanenko (IKI),  S. Belkin (IKI, HSE),  N. Pankov 
(HSE)  report on behalf of IKI GRB FuN:

We observed GRB 230116D (Sonbas et al., GCN 33176)  with Sintez-Newton 
telescope of CrAO observatory.  Observation started on 2023-01-16 (UT) 
21:21:41. The series consists of images with an exposure of 120 s in 
Clear filter.

In the first images we detect an object in coordinates (J2000)
06:34:28.01 +49:52:20.35 (with uncertainties of 0.5 arcsec) which is 
within of the XRT error circle (Sonbas et al., GCN 33176).
Preliminary photometry of the afterglow is 19.5 at (UT) 21:41:56. The 
photometry is based on nearby USNO-B1.0 (R2) stars. There is no object 
in PS1 and DSS2 catalogues at this coordinates. Therefore we suggest the 
object is the afterglow of GRB 230116D. Observation is continuing.


GRB_name: GRB230116D
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33179
SUBJECT: GRB 230116D: SAO RAS observations of OT brightening
DATE:    23/01/16 23:07:21 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

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

We observed the field of the GRB 230116D (Sonbas et al. GCN #33176)
with the SAO RAS 1-m telescope Zeiss-1000 + CCD-photometer in Rc band.

Inside the XRT error circle we detected new transient object
reported by Zhu et al. (GCN #33177) and Nazarov et al. (GCN #33178)
with the coordinates
R.A. = 06:34:28.2
Dec. = +49:52:20.5 (+/- 0".3, J2000) and brightness
R = 19.93 +/- 0.07 (T - T0 = 0.9378h),
R = 19.72 +/- 0.06 (T - T0 = 1.4236h)
Preliminary photometry is based on R2 magnitudes of nearby USNO-B1 stars.

Further observations are ongoing and encouraged.


GRB_name: GRB230116D
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33180
SUBJECT: GRB 230116D: Enhanced Swift-XRT position
DATE:    23/01/17 04:00:15 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 1618 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 230116D, 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 = 98.61719, +49.87240 which is equivalent
to:

RA (J2000): 06h 34m 28.13s
Dec (J2000): +49d 52' 20.6"

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: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33181
SUBJECT: GRB 230116D: GIT optical follow-up
DATE:    23/01/17 04:57:44 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>



GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33182
SUBJECT: GRB 230116D: GIT optical follow-up
DATE:    23/01/17 05:03:49 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

V. Swain (IITB), H. Kumar (IITB), K. Angail (IAO), V. Bhalerao (IITB), G. C. Anupama(IIA), S. Barway (IIA) report on behalf of the GIT team:

[The previous GCN was garbled up, re-posting]

We observed GRB 230116D detected by Swift-BAT (Sonbas et al., GCN 33176) and optical afterglow discovered by Z.P. Zhu et al.(GCN 33177), with 0.7m GROWTH-India Telescope (GIT). We started the observation at 21:39:00 UT on 2023-01-16, i.e., 34.28 min after the Swift/BAT trigger and took multiple exposures in the gâ€™, r' and iâ€™ filters. We clearly detected the afterglow in our stacked image at R.A.= 06:34:28.13, DEC.=+49:52:20.6, within the 2.3 arcsec radius circle (J.P. Osborne et al., GCN 33180). The photometric results follow as:
-------------------------------------------------------------------
 JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Magnitude (AB) |
-------------------------------------------------------------------
 2459961.40208328 | 0.57 | 1 x 20           | r' | >17.63 |
 2459961.41763334 | 0.94 | 8 x 300 (stacked) | gâ€™ | 21.04 +/- 0.07 |
 2459961.44794164 | 1.67 | 8 x 300 (stacked) | râ€™ | 19.99 +/- 0.05 |
 2459961.47255148 | 2.26 | 5 x 300 (stacked) | iâ€™ | >19.84 |
-------------------------------------------------------------------

The results are consistent with S. Nazarov et al.(GCN #33178) and A. S. Moskvitin et al.(GCN #33179).The magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.

The GROWTH India Telescope (GIT; Kumar et al. 2022) 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 the telescopeâ€™s operations. Telescope technical details are available at https://sites.google.com/view/growthindia/.


GRB_name: GRB230117A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33183
SUBJECT: GRB 230117A: Fermi GBM Final Real-time Localization
DATE:    23/01/17 05:14:24 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:04:04 UT on 17 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230117A (trigger 695624649.253766 / 230117211).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 13.6, Dec = 38.2 (J2000 degrees, equivalent to J2000 00h 54m, 38d 12'), with a statistical uncertainty of 6.5 degrees.

The angle from the Fermi LAT boresight is 73.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230117211/quicklook/glg_skymap_all_bn230117211.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230117211/quicklook/glg_healpix_all_bn230117211.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230117211/quicklook/glg_lc_medres34_bn230117211.gif


GRB_name: GRB230117A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33184
SUBJECT: Fermi GRB 230117A: Global MASTER-Net observations report 
DATE:    23/01/17 09:30:16 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 230117A ( Fermi GBM team, GCN 33183) errorbox  14857 sec after notice time and 14892 sec after trigger time at 2023-01-17 09:12:16 UT, with upper limit up to  12.6 mag. Observations started at twilight.  The observations began at zenith distance = 11 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = -24 deg., longitude l = 124 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2192799

We obtain a following upper limits.  

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

   14982 | 2023-01-17 09:12:16 |         MASTER-Amur | (00h 43m 54.98s , +41d 16m 16.5s) |   C |   180 | 12.6 |        
   15402 | 2023-01-17 09:20:15 |         MASTER-Amur | (00h 54m 56.32s , +39d 10m 24.1s) |   C |    60 | 12.1 |        
   15561 | 2023-01-17 09:22:55 |         MASTER-Amur | (00h 53m 28.23s , +37d 17m 23.6s) |   C |    60 | 12.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230116D
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33185
SUBJECT: GRB 230116D: Swift-XRT refined Analysis
DATE:    23/01/17 10:52:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.7 ks of XRT data for GRB 230116D (Sonbas et al. GCN
Circ. 33176), from 113 s to 40.1 ks after the  BAT trigger. The data
comprise 47 s in Windowed Timing (WT) mode (the first 10 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. 33180).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.87 (+0.28, -0.19). At T+559 s  the decay
flattens to an alpha of 0.72 (+0.10, -0.28) before breaking again at
T+11.3 ks to a final decay with index alpha=2.4 (+2.5, -0.8).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.75 (+0.20, -0.09). The
best-fitting absorption column is  consistent with the Galactic value
of 1.6 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.9 x 10^-11 (4.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.75 (+0.20, -0.09)

If the light curve continues to decay with a power-law decay index of
2.4, the count rate at T+24 hours will be 5.1 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-14 (2.4 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01149293.

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


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33187
SUBJECT: GRB 230116D: SAO RAS redshift
DATE:    23/01/17 15:29:14 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Moskvitin (SAO RAS), A. Pozanenko (IKI),  A. Moiseev (SAO RAS), D. 
Oparin  (SAO RAS), S. Belkin (IKI, HSE) report on behalf of larger 
collaboration:

We observed the optical afterglow (Zhu et al., GCN 33177; Nazarov  et 
al., GCN 33178; Moskvitin et al., GCN 33179; Swain et al., GCN 33182) of 
GRB 230116D (Sonbas et al., GCN 33176) with BTA SAO RAS telescope 
equipped with SCORPIO-2. Observation started on 2023-01-16 (UT) 
23:31:38. Spectroscopic observations consists of 10x600 s exposures with 
  940@600 grizm.

We detect a sharp break at 5850 AA and afterglow continuum up to 7200 
AA. We interpret the sharp break due to H I. Over the continuum we 
identified multiple absorption features, which we interpret as due to S 
II, Si II, O I, C II, Si IV at a common redshift of z = 3.81.


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33188
SUBJECT: GRB 230116D: LCOGT Optical Upper Limit
DATE:    23/01/17 15:59:16 GMT
FROM:    Robert Strausbaugh at University of Minnesota  <rstrausb@umn.edu>

R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on
behalf of a larger collaboration:

We observed the GRB 230116D (Sonbas et al., GCN 33176) field with the LCOGT
1-meter Sinistro instrument at the McDonald Observatory, TX, USA site, on
January 17, from 05:24 to 05:56 UT (corresponding to 8.33 to 8.64 hours
from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in each band.  We do not detect a
source in either band within the XRT enhanced error region (Osborne et al.,
GCN 33180).  This suggests fading compared to other optical detections (Zhu
et al., GCN 33177; Nazarov et al., GCN 33178; Moskvitin et al., GCN 33179;
Swain et al., 33182).

The following magnitudes and upper limits are calculated using the
PanSTARRS catalog as reference:

r > 22.2
i > 21.2

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33189
SUBJECT: GRB 230116D: Sintez-Newton/CrAO optical observations
DATE:    23/01/17 19:01:13 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI, HSE), S. Nazarov (CrAO),  A. Pozanenko (IKI),  N. Pankov 
(HSE, IKI) report on behalf of GRB IKI FuN:

We observed the optical afterglow (Zhu et al., GCN 33177; Nazarov  et 
al., GCN 33178; Moskvitin et al. GCNs 33179, 33187; Swain et al., GCN 
33182) of GRB 230116D (Sonbas et al., GCN 33176) with Sintez-Newton 
telescope of CrAO observatory.  Observation started on 2023-01-16 (UT) 
21:21:41. The series consist of images with an exposure of 120 s in 
Clear filter. Preliminary photometry of the stacked images is following

Date UT-start       Exptime Filter t-T0     OT     Err     UL
2023-01-16 21:23:55 35*120  Clear  0.03764  19.82  0.08    22.5
2023-01-16 22:44:52 33*120  Clear  0.09245  19.97  0.16    21.9

Ref.stars
USNO-B1.0
RA DEC R2

06:34:04.9708800 +49:53:05.863200 15.61
06:34:38.7820800 +49:49:22.972800 16.29
06:34:57.9967200 +49:53:01.932000 16.94
06:34:24.5268000 +49:47:49.801200 15.68


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33190
SUBJECT: GRB 230116D: KGO RC-25 optical observations
DATE:    23/01/17 20:01:46 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI, HSE),  A. V. Samokhvalov (citizen scientist, Surgut), 
A. Pozanenko (IKI),  N. Pankov (HSE, IKI) report on behalf of GRB IKI FuN:

We observed the optical afterglow (Zhu et al., GCN 33177; Nazarov  et 
al., GCN 33178; Moskvitin et al. GCNs 33179, 33187; Swain et al., GCN 
33182; Belkin et al., GCN 33189) of GRB 230116D (Sonbas et al., GCN 
33176) with 25cm 1/8 Ritchey-Chretien  telescope of KGO observatory. 
Observation started on 2023-01-16 (UT) 21:21:41. The series consist of 
images with an exposure of 600 s in R-filter. Preliminary photometry of 
the stacked image is following

Date UT-start       Exptime Filter t-T0     OT     Err    UL
2023-01-16 23:36:12 11*600  R      0.16075  20.25  0.20   20.4

Ref.stars
USNO-B1.0
RA DEC R2

06:34:04.9708800 +49:53:05.863200 15.61
06:34:38.7820800 +49:49:22.972800 16.29
06:34:57.9967200 +49:53:01.932000 16.94
06:34:24.5268000 +49:47:49.801200 15.68


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33191
SUBJECT: GRB 230116D: SAO RAS photometry
DATE:    23/01/17 21:39:47 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the optical afterglow (Zhu et al., GCN 33177; Nazarov  et
al., GCN 33178; Moskvitin et al. GCNs 33179, 33187; Swain et al., GCN
33182; Belkin et al., GCNs 33189, 33190)  of GRB 230116D (Sonbas et al., 
GCN 33176) with BTA SAO RAS telescope equipped with SCORPIO-2. 
Observation started on 2023-01-16 (UT) 23:31:38. Photometric 
observations consists of r -filter acquisition imaging and  g,r,i - 
filters after before spectroscopy (Moskvitin et al. GCN 33187). 
Preliminary photometry of stacked images is following


Date       UT-start Exptime Filter t-T0     OT     Err    UL
2023-01-16 23:31:48 2*20    r      0.10951  20.29  0.05   21.4
2023-01-17 01:33:17 2*90    r      0.18859  20.97  0.04   23.2
2023-01-17 01:30:43 3*120   g      0.18935  22.18  0.08   23.1

Ref.stars
PanSTARRS-PS1
RA DEC g r i z
06:34:21.9567816 +49:52:11.318772 16.3946 15.7833 15.5155 15.3912
06:34:23.9012808 +49:51:55.541160 18.8105 18.2189 17.9721 17.8591
06:34:37.7805360 +49:50:45.780468 18.3294 17.6554 17.3783 17.2518

The light curve based on afterglow observations (GCNs 33177,  33178, 
33179, 33187, 33188, 33182, 33189, 33190)   can be found at
http://grb.rssi.ru/GRB230116D/GRB230116D_lc_1.png

The light curve  confirms rebrightening (Moskvitin et al. GCN 33179) or 
plateau at 0.03 - 0.1 days and correlate with XRT LC 
(https://www.swift.ac.uk/xrt_curves/01149293/).


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33192
SUBJECT: GRB 230116D: SAO RAS further observations
DATE:    23/01/18 04:08:32 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

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

We observed the field of the GRB 230116D (Sonbas et al. GCN #33176)
with the SAO RAS 1-m telescope Zeiss-1000 + CCD-photometer in Rc band
on January 16/17 (21:55:22--00:36:40 UT) and 17/18 (21:42:43--23:31:38).

During the first night the optical afterglow (Zhu et al., GCN #33177;
Nazarov et al., GCN #33178; Moskvitin et al. GCNs #33179, #33187;
Swain et al., GCN #33182; Belkin et al., GCNs #33189, #33190, #33191)
was clearly detected in individual frames and shows complex behaviour.

t-T0, h    R_mag  +/- err     exp, s
0.844      19.967 +/- 0.070   300
0.948      19.888 +/- 0.068   300
1.045      19.874 +/- 0.066   300
1.138      19.818 +/- 0.063   300
1.233      19.674 +/- 0.057   300
1.332      19.595 +/- 0.051   300
1.432      19.701 +/- 0.055   300
1.526      19.668 +/- 0.056   300
1.623      19.779 +/- 0.062   300
1.717      19.764 +/- 0.063   300
1.820      19.728 +/- 0.058   300
1.924      19.626 +/- 0.055   300
2.022      19.539 +/- 0.052   300
2.130      19.709 +/- 0.064   300
2.226      19.798 +/- 0.070   300
2.346      19.870 +/- 0.078   300
2.444      19.976 +/- 0.083   300
2.644      20.021 +/- 0.086   300
2.835      20.065 +/- 0.066   2 x 300
3.041      20.032 +/- 0.063   2 x 300
3.241      20.138 +/- 0.062   2 x 300
3.441      20.223 +/- 0.075   2 x 300

We also obtained 17 x 300 images in Rc band during the second night.
The OT is detected in the stacked frame with the brightness of
R = 22.9 +/- 0.2 (t-T0 = 25.541h = 1.064d) which is in agreement with
upper limit reported by Strausbaugh & Cucchiara (GCN #33188).
Preliminary photometry is based on R2 magnitudes of nearby USNO-B1 stars.


GRB_name: GRB230116C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33193
SUBJECT: GRB 230116C: Swift-BAT refined analysis
DATE:    23/01/18 22:23:03 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

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 230116C (trigger #1149250)
(Sonbas et al., GCN Circ. 33173).  The BAT ground-calculated position is
RA, Dec = 223.467, -16.883 deg which is
   RA(J2000)  =  14h 53m 52.0s
   Dec(J2000) = -16d 52' 57.5"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 65%.

The BAT light curve showed a complex structure with a duration of about 400 sec.
T90 (15-350 keV) is 316.77 +- 52.50 sec (estimated error including systematics).

The time-averaged spectrum from T-35.86 to T+346.68 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.72 +- 0.14.  The fluence in the 15-150 keV band is 6.1 +- 0.5 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+247.71 sec in the 15-150 keV band
is 0.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1149250/BA/


GRB_name: GRB230116D
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33194
SUBJECT: GRB 230116D: Swift-BAT refined analysis
DATE:    23/01/18 22:24:27 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

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 230116D (trigger #1149293)
(Sonbas et al., GCN Circ. 33176).  The BAT ground-calculated position is
RA, Dec = 98.584, 49.831 deg which is
   RA(J2000)  =  06h 34m 20.1s
   Dec(J2000) = +49d 49' 50.3"
with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 98%.

The BAT light curve showed a complex structure with a duration of about 40 sec.
T90 (15-350 keV) is 41.00 +- 11.18 sec (estimated error including systematics).

The time-averaged spectrum from T+1.14 to T+53.144 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.38 +- 0.22.  The fluence in the 15-150 keV band is 8.12 +- 1.2 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+12.14 sec in the 15-150 keV band
is 0.6 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1149293/BA/


GRB_name: GRB230118A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33195
SUBJECT: GRB 230118A: Fermi GBM Final Real-time Localization
DATE:    23/01/19 00:04:31 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 23:54:10 UT on 18 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230118A (trigger 695778855.155984 / 230118996).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 330.8, Dec = 20.0 (J2000 degrees, equivalent to J2000 22h 03m, 20d 00'), with a statistical uncertainty of 11.0 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/2023/bn230118996/quicklook/glg_skymap_all_bn230118996.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230118996/quicklook/glg_healpix_all_bn230118996.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230118996/quicklook/glg_lc_medres34_bn230118996.gif


GRB_name: GRB230118A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33196
SUBJECT: Fermi GRB 230118A: Global MASTER-Net observations report 
DATE:    23/01/19 10:30:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 230118A ( Fermi GBM team, GCN 33195) errorbox  35156 sec after notice time and 35189 sec after trigger time at 2023-01-19 09:40:39 UT, with upper limit up to  12.4 mag. Observations started at twilight.  The observations began at zenith distance = 55 deg. The sun  altitude  is -15.4 deg. 

The galactic latitude b = -28 deg., longitude l = 78 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2193130

We obtain a following upper limits.  

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

   35220 | 2023-01-19 09:40:39 |         MASTER-Amur | (22h 07m 46.55s , +20d 14m 59.6s) |   C |    60 | 12.4 |        
   35299 | 2023-01-19 09:41:59 |         MASTER-Amur | (22h 16m 19.39s , +20d 15m 48.0s) |   C |    60 | 12.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230119A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33197
SUBJECT: GRB 230119A: Fermi GBM Final Real-time Localization
DATE:    23/01/19 13:34:04 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 13:23:36 UT on 19 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230119A (trigger 695827421.318578 / 230119558).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 332.4, Dec = -20.1 (J2000 degrees, equivalent to J2000 22h 09m, -20d 06'), with a statistical uncertainty of 3.1 degrees.

The angle from the Fermi LAT boresight is 90.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230119558/quicklook/glg_skymap_all_bn230119558.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230119558/quicklook/glg_healpix_all_bn230119558.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230119558/quicklook/glg_lc_medres34_bn230119558.gif


GRB_name: GRB230116D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33198
SUBJECT: GRB 230116D: 3.6m DOT optical upper limit
DATE:    23/01/20 05:06:14 GMT
FROM:    Rahul Gupta at ARIES, India  <rahulbhu.c157@gmail.com>

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

We observed the field of GRB 230116D detected by Swift (Sonbas et al., GCN
33176) using the 3.6m Devasthal Optical Telescope of ARIES Nainital. We
have taken multiple frames having an exposure time of 300 sec in the r
filter. We stacked the images after the alignment. We do not detect the
optical afterglow (Zhu et al., GCN 33177; Nazarov et al., GCN 33178;
Moskvitin et al., GCNs 33179, 33187, 33192; Swain et al., GCN 33182; and
Belkin et al., GCNs 33189, 33190, 33191). We obtained the limiting mag of ~
22.7 mag at ~ 1.04 days post-detection.

The limiting magnitudes quoted are not corrected for the Galactic and host
extinction in the direction of the burst. Photometric calibration is
performed using the standard stars from the Pan-STARRS catalog.

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: GRB230119A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33199
SUBJECT: GRB 230119A: CALET Gamma-Ray Burst Monitor detection
DATE:    23/01/20 12:20:10 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

S. Nakahira (RIKEN), A. Yoshida, T. Sakamoto, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), Y. Asaoka (ICRR),
S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu,
T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 230119A (Fermi GBM Final Real-time Localization: 
Fermi GBM team, GCN Circ. 33197) triggered the CALET 
Gamma-ray Burst Monitor (CGBM) at 13:23:33.64 UTC on 19 Jan 2023
(http://cgbm.calet.jp/cgbm_trigger/flight/1358169750/).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure that starts
at T-0.4 sec, peaks at T+3.0 sec, and ends at T+91.0 sec.
The T90 and T50 durations measured by the SGM data are 79.6 +/- 4.6 sec
and 45.4 +/- 1.2 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1358169750/index.html

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


GRB_name: GRB230116B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33200
SUBJECT: IPN triangulation of GRB 230116B (short)
DATE:    23/01/20 17:53:22 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. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,

E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

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

The bright, short-duration GRB 230116B
(Fermi-GBM detection: the Fermi GBM team, GCN Circ. 33172)
has been detected by Fermi(GBM trigger 695552351),
Konus-Wind, INTEGRAL (SPI-ACS), and Mars-Odyssey (HEND), so far,
at about 32347 s UT (08:59:07).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   115.533 (07h 42m 08s) -43.027 (-43d 01' 39")
  Corners:
   115.712 (07h 42m 51s) -42.983 (-42d 58' 59")
   115.582 (07h 42m 20s) -43.076 (-43d 04' 34")
   115.353 (07h 41m 25s) -43.071 (-43d 04' 17")
   115.483 (07h 41m 56s) -42.979 (-42d 58' 44")
  ---------------------------------------------
The error box area is 58 sq. arcmin, and its maximum
dimension is 17 arcmin (the minimum one is 5.8 arcmin).
The Sun distance was 116 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM final localization (GCN 33172).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB230116_T32349/IPN

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


GRB_name: GRB230120A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33201
SUBJECT: GRB 230120A: AstroSat CZTI detection
DATE:    23/01/20 19:29:55 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

  G. Waratkar (IITB), A. Ahmad (IITB), A. Vibhute (IUCAA), V. Bhalerao 
(IITB), D. Bhattacharya (Ashoka University/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 the detection of GRB 230120A which was also 
detected by GECAM-B (TrigNum 135).

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 
2023-01-20 10:53:13.5 UTC, followed by another strong peak about 100 s 
later. The measured peak count rate associated with the burst is 139.8 
(+28.1 -15.4) counts/s above the background in the combined data of all 
four quadrants, with a total of 1853 (+441 -318) counts. The local mean 
background count rate was 124.9 (+0.7 -1.2) counts/s. Using cumulative 
rates, we measure a T90 of 114.95 (+20.59 -8.86) 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 strong peak at 2023-01-20 10:53:11.6 UTC, 
followed by another peak about 100 s later. The measured peak count rate 
is 778.6 (+73.8 -60.0) counts/s above the background in the combined 
Veto data of all four quadrants, with a total of 12139 (+1359 -1526) 
counts. The local mean background count rate was 1325.6 (+3.0 -3.3) 
counts/s. We measure a T90 of 120.35 (+11.00 -11.32) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB230116B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33203
SUBJECT: GRB 230116B: Fermi GBM observation
DATE:    23/01/21 17:53:00 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

R. Hamburg (CNRS/IJCLab) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 08:59:06.67 UT on 16 January 2023, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 230116B (trigger 695552351 / 230116374), which
was
also localized by the IPN network (Kozyrev et al. 2023, GCN 33200).
The GBM on-ground location is consistent with the IPN position.

The angle from the Fermi LAT boresight at the GBM trigger time is 104
degrees.

The GBM light curve consists of a single pulse with a duration (T90) of
about 64 ms (50-300 keV). The time-averaged spectrum from T0-0.064 s to
T0+0.128 is best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.07 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 733 +/- 53 keV.

The event fluence (10-1000 keV) in this time interval is
(3.7 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.0 s in the 10-1000 keV band is 75.5 +/- 3.0 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: GRB230123A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33206
SUBJECT: GRB 230123A: Swift detection of a burst
DATE:    23/01/23 10:36:16 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

M. A. Williams (PSU), R. A. J. Eyles-Ferris (U Leicester),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (U Tampa) and K. L. Page (U Leicester) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 10:19:44 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230123A (trigger=1150429).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 40.937, -65.676 which is 
   RA(J2000) = 02h 43m 45s
   Dec(J2000) = -65d 40' 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 10 sec.  The peak count rate 
was ~800 counts/sec (15-350 keV), at ~1 sec after the trigger. 
The immediately available BAT light curve does not include data 
from ~T+8 s to ~T+100 s. There might be additional burst emission 
in that time interval. 

The XRT began observing the field at 10:21:13.6 UT, 88.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 40.85977, -65.68672
which is equivalent to:
   RA(J2000)  = 02h 43m 26.34s
   Dec(J2000) = -65d 41' 12.2"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 120 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper.  We cannot determine whether the source
is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.95 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 1.3
(+1.44/-1.26) x 10^22 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 92 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 12% 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
0.022. 

Burst Advocate for this burst is M. A. Williams (mjw6837 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB230116C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33207
SUBJECT: GRB 230116C: Swift-XRT observations
DATE:    23/01/23 13:54:57 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J. D. Gropp (PSU), S. Dichiara (PSU), A.P. Beardmore (U. Leicester),
J.P. Osborne (U. Leicester), B. Sbarufatti (INAF-OAB), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU) and A. Y. Lien
(U Tampa) report on behalf of the Swift-XRT team:

We have analysed 9.4 ks of Photon Counting (PC) mode XRT data for the
Swift-BAT-detected burst GRB 230116C (Lien et al. GCN Circ. 33193),
collected between T0+159.6 ks and T0+537.9 ks. 

Six uncatalogued X-ray sources have been detected consistent with being
within 296 arcsec of the Swift-BAT 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):  223.47316  =  14:53:53.56
  Dec (J2000): -16.91649  =  -16:54:59.4
  Error: 2.7 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.0102 +/- 0.0013 ct s^-1   
  Distance: 167 arcsec from Swift-BAT position.
  Flux: (3.43 [+0.44, -0.43])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 2:
  RA (J2000):  223.4729  =  14:53:53.49
  Dec (J2000): -16.8864  =  -16:53:11.2
  Error: 6.4 arcsec (radius, 90% conf.)
  Count-rate: (2.80 [+1.09, -0.88])e-3 ct s^-1  
  Distance: 65 arcsec from Swift-BAT position.

Source 3:
  RA (J2000):  223.4516  =  14:53:48.38
  Dec (J2000): -16.9158  =  -16:54:56.8
  Error: 6.8 arcsec (radius, 90% conf.)
  Count-rate: (3.15 [+0.84, -0.69])e-3 ct s^-1  
  Distance: 165 arcsec from Swift-BAT position.
  Flux: (1.45 [+0.39, -0.32])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 8:
  RA (J2000):  223.4602  =  14:53:50.44
  Dec (J2000): -16.8420  =  -16:50:31.2
  Error: 6.3 arcsec (radius, 90% conf.)
  Count-rate: (1.79 [+0.90, -0.70])e-3 ct s^-1  
  Distance: 104 arcsec from Swift-BAT position.

Source 9:
  RA (J2000):  223.4090  =  14:53:38.16
  Dec (J2000): -16.9156  =  -16:54:56.0
  Error: 8.1 arcsec (radius, 90% conf.)
  Count-rate: (8.7 [+5.4, -4.3])e-4 ct s^-1   
  Distance: 245 arcsec from Swift-BAT position.

Source 15:
  RA (J2000):  223.4391  =  14:53:45.37
  Dec (J2000): -16.8309  =  -16:49:51.2
  Error: 8.7 arcsec (radius, 90% conf.)
  Count-rate: (5.7 [+4.3, -3.4])e-4 ct s^-1   
  Distance: 166 arcsec from Swift-BAT position.

Eleven uncatalogued sources were also detected too far from the GRB
position to be likely afterglow candidates.

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/01149250.

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


GRB_name: GRB230123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33208
SUBJECT: GRB 230123A: Zadko observatory - Gingin optical observations
DATE:    23/01/23 14:31:21 GMT
FROM:    Bruce Gendre at UVI  <bruce.gendre@gmail.com>

B. Gendre (UWA/OzGrav), G. Stratta (INAF/Goethe University Frankfurt),
E. Moore (UWA/OzGrav), F. Panther (UWA/OzGrav), D. Coward (UWA/OzGrav),
J. A. Moore (OzGrav-UWA), A. Klotz (IRAP-CNRS-OMP), and P. Thierry (AGORA)
report:

We imaged the field of GRB 230123A detected by SWIFT
(trigger 1150429, GCN 33206, Williams et al. 2023)
with the Zadko robotic telescope (D=100cm)
located at the Zadko observatory - Gingin, Australia.

The observations started 2.56h after the GRB trigger (t0+9213.4s).
The elevation of the field decreased from
51 degrees above horizon and weather conditions
were good.

We observed the field for one hour, and have not detected any afterglow
down to magnitude 18.7 in individual images. On a stack of 6 images, we reached
an upper limit of R = 19.0 with no detection of the afterglow.
Further observations are planned.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=286.2098 lat=-47.6419
and the galactic extinction in R band is 0.0 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.
======================================================================


GRB_name: GRB230123A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33209
SUBJECT: GRB 230123A: Enhanced Swift-XRT position
DATE:    23/01/23 16:43:36 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 1184 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 230123A, 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 = 40.85842, -65.68648 which is equivalent
to:

RA (J2000): 02h 43m 26.02s
Dec (J2000): -65d 41' 11.3"

with an uncertainty of 4.1 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: GRB230123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33210
SUBJECT: GRB 230123A: Swift-XRT refined Analysis
DATE:    23/01/23 17:57:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.4 ks of XRT data for GRB 230123A (Williams et al.
GCN Circ. 33206), from 73 s to 18.4 ks after the  BAT trigger. The data
comprise 8 s in Windowed Timing (WT) mode (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.
33209).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.68 (+0.08, -0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+0.4, -0.3). The
best-fitting absorption column is  1.4 (+1.0, -0.8) x 10^21 cm^-2, in
excess of the Galactic value of 3.0 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.2 x 10^-11 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.4 (+1.0, -0.8) x 10^21 cm^-2
Galactic foreground: 3.0 x 10^20 cm^-2
Excess significance: 2.2 sigma
Photon index:      2.1 (+0.4, -0.3)

If the light curve continues to decay with a power-law decay index of
0.68, the count rate at T+24 hours will be 3.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (1.4 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/01150429.

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


GRB_name: GRB230123A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33211
SUBJECT: GRB 230123A: Swift/UVOT Upper Limits
DATE:    23/01/23 19:25:47 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and M. Williams (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 230123A
93 s after the BAT trigger (Williams et al., GCN Circ. 33206).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 33209)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC            93          243          147         >20.6
u_FC               305          555          246         >20.6
white               93         1704          412         >21.0
v                  637         1754          136         >19.4
b                  562         1679          117         >20.0
u                  305         1825          359         >20.5
w1                 686         1804          117         >20.8
m2                1412         1605           39         >18.7
w2                 612         1209           78         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.022 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB230122A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33213
SUBJECT: GRB 230122A: Swift/BAT-GUANO detection
DATE:    23/01/24 00:54:25 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 230122A onboard (T0:
2023-01-22T13:43:24 UTC, INTEGRAL/SPI-ACS trig #10169).

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 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 2022, ApJ,
941, 169), detects the burst with a sqrt(TS) of 12.1 in a 1.024 s
analysis time bin.
The burst duration is ~2 seconds.

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FOV.

See Section 9.1 and Figures 10 and 17 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: GRB230123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33214
SUBJECT: GRB 230123A: Swift-BAT refined analysis
DATE:    23/01/24 05:08:44 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),
T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU),
M. Stamatikos (OSU), M. A. Williams (PSU) (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 230123A (trigger #1150429)
(Williams et al., GCN Circ. 33206).  The BAT ground-calculated position is
RA, Dec = 40.905, -65.661 deg which is
   RA(J2000)  =  02h 43m 37.3s
   Dec(J2000) = -65d 39' 39.9"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.

The mask-weighted light curve shows a single-peaked structure
that starts at ~T-2 s, peaks at ~T+1, and ends at ~T+6 s.
T90 (15-350 keV) is 5.37 +- 1.03 sec (estimated error including
systematics).

The time-averaged spectrum from T-1.25 to T+4.75 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 2.06 +- 0.24.  The fluence in the 15-150 keV band
is 2.7 +- 0.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from
T+0.12 sec in the 15-150 keV band is 1.1 +- 0.2 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1150429/BA/


GRB_name: GRB230124A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33215
SUBJECT: GRB 230124A: Fermi GBM Final Real-time Localization
DATE:    23/01/24 15:28:54 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 15:18:46 UT on 24 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230124A (trigger 696266331.698466 / 230124638).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 67.2, Dec = -1.4 (J2000 degrees, equivalent to J2000 04h 28m, -1d 23'), with a statistical uncertainty of 3.3 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/2023/bn230124638/quicklook/glg_skymap_all_bn230124638.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230124638/quicklook/glg_healpix_all_bn230124638.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230124638/quicklook/glg_lc_medres34_bn230124638.gif


GRB_name: GRB230124A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33216
SUBJECT: Fermi GRB 230124A: Global MASTER-Net observations report 
DATE:    23/01/24 15:45:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 230124A ( Fermi GBM team, GCN 33215) errorbox  521 sec after notice time and 554 sec after trigger time at 2023-01-24 15:28:00 UT, with upper limit up to  19.0 mag. Observations started at twilight.  The observations began at zenith distance = 51 deg. The sun  altitude  is -13.9 deg. 

The galactic latitude b = -31 deg., longitude l = 197 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2194256

We obtain a following upper limits.  

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

     609 | 2023-01-24 15:28:00 |   MASTER-Kislovodsk | (04h 24m 10.16s , -01d 16m 01.3s) |   C |   110 | 18.1 |        
     754 | 2023-01-24 15:28:00 |   MASTER-Kislovodsk | (04h 24m 10.17s , -01d 16m 01.3s) |   C |   400 | 19.0 |  Coadd 
     749 | 2023-01-24 15:30:10 |   MASTER-Kislovodsk | (04h 24m 10.23s , -01d 17m 43.1s) |   C |   130 | 18.3 |        
     913 | 2023-01-24 15:32:39 |   MASTER-Kislovodsk | (04h 24m 12.35s , -01d 15m 53.2s) |   C |   160 | 18.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33217
SUBJECT: GRB 230123A: LCOGT Optical Upper Limits
DATE:    23/01/24 17:19:20 GMT
FROM:    Robert Strausbaugh at University of Minnesota  <rstrausb@umn.edu>

R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on
behalf of a larger collaboration:

We observed the GRB 230123A (Williams et al., GCN 33206) field with the
LCOGT 1-meter Sinistro instrument at the Cerro Tololo Interamerican
Observatory, Chile site, on January 24, from 02:06 to 02:38 UT
(corresponding to 15.78 to 16.32 hours from the GRB trigger time) with the
Bessel R and I filters.

We performed a series of 3x300s exposures in each band.  We do not detect a
source in either band within the XRT enhanced error region (Beardmore et
al., GCN 33209), consistent with other optical upper limits (Gendre et al.,
GCN 33208; Belles et al., 33211).

The following upper limits are calculated using the USNO-B1.0 catalog as
reference:

R > 20.8
I > 20.1

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB230114B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33218
SUBJECT: GRB 230114B: Detection by VZLUSAT-2
DATE:    23/01/24 21:32:32 GMT
FROM:    Jakub Ripa at Masaryk University  <245487@mail.muni.cz>

J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory),  N. Werner (Masaryk 
U.), M. Ohno (Hiroshima U.),  L. Meszaros, B. Csak (Konkoly 
Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. 
Hroch, M. Dafcikova, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, 
J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo 
(Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida 
(ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. 
Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe 
(Rikkyo U.), L. L. Kiss (Konkoly Observatory),  T. Mizuno (Hiroshima 
U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe 
(Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes 
(VZLU), I. Vertat (FEL ZCU)  -- the VZLUSAT-2/GRB payload collaboration.

The short-duration GRB 230114B (Konus-Wind detection trigger time at 
2023-01-14 20:40:57.752 UT; INTEGRAL/SPI-ACS detection peak at 
~2023-01-14 20:40:56 UT) was detected by the GRB detector on board of 
the VZLUSAT-2 3U CubeSat (https://www.vzlusat2.cz/en/).

The data acquisition was performed by GRB detector unit no. 1 and the 
detection was confirmed at the peak time 2023-01-14 20:40:54 UTC. The 
duration was measured to be 1 s with the light curve resolution of 1 s. 
The significance is 4.9 sigma.

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB230114B_GCN_VZLUSAT2.pdf

All VZLUSAT-2 detections are listed at: 
https://monoceros.physics.muni.cz/hea/VZLUSAT-2/
The GRB detectors on VZLUSAT-2 are a demonstration payload for a future 
CubeSats constellation (Werner et al. Proc. SPIE 2018). Two GRB modules 
of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 
75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the 
energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 
January 13 from Cape Canaveral.


GRB_name: GRB230124A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33220
SUBJECT: GRB 230124A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    23/01/25 02:49:23 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 230124A onboard (T0:
2023-01-24T15:18:46 UTC, Fermi/GBM GCN 33215).

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 2022, ApJ,
941, 169), detects the burst with a sqrt(TS) of 9.5 in a 4.096 s
analysis time bin.

NITRATES results are consistent with a burst coming from outside the
FOV, as suggested by the Fermi/GBM localization.

See Section 9.1 and Figures 10 and 17 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: GRB230124A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33222
SUBJECT: GRB 230124A: Fermi GBM Observation
DATE:    23/01/26 01:00:42 GMT
FROM:    Sarah Dalessi at UAH  <sd0104@uah.edu>

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

"At 15:18:46.70 UT on 24 January 2023, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 230124A (trigger 696266331 / 230124638)
which was also detected by the Swift/BAT-GUANO (J. A. Kennea et al.
2023, GCN 33220).
The Fermi GBM Final Real-time Localization was reported in GCN 33215.

The angle from the Fermi LAT boresight at the GBM trigger time is 32 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 12 s (50-300 keV).
The time-averaged spectrum from T0-2.56 s to T0+12.8 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.36 +/- 0.13 and
the cutoff energy, parameterized as Epeak, is 77.41 +/- 3.34 keV.

The event fluence (10-1000 keV) in this time interval is
(2.248 +/- 0.077)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7.1 s in the 10-1000 keV band
is 4.6 +/- 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: GRB230126A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33225
SUBJECT: GRB 230126A: Fermi GBM Final Real-time Localization
DATE:    23/01/26 18:31:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 18:20:44 UT on 26 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230126A (trigger 696450049.448062 / 230126764).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 96.9, Dec = -27.0 (J2000 degrees, equivalent to J2000 06h 27m, -27d 00'), with a statistical uncertainty of 11.8 degrees.

The angle from the Fermi LAT boresight is 91.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230126764/quicklook/glg_skymap_all_bn230126764.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230126764/quicklook/glg_healpix_all_bn230126764.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230126764/quicklook/glg_lc_medres34_bn230126764.gif


GRB_name: GRB230128A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33231
SUBJECT: GRB 230128A: Fermi GBM Final Real-time Localization
DATE:    23/01/28 22:57:57 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 22:47:49 UT on 28 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230128A (trigger 696638874.07722 / 230128950).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 197.6, Dec = 61.7 (J2000 degrees, equivalent to J2000 13h 10m, 61d 42'), with a statistical uncertainty of 6.3 degrees.

The angle from the Fermi LAT boresight is 90.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230128950/quicklook/glg_skymap_all_bn230128950.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230128950/quicklook/glg_healpix_all_bn230128950.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230128950/quicklook/glg_lc_medres34_bn230128950.gif


GRB_name: GRB230129A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33232
SUBJECT: GRB 230129A: Fermi GBM Final Real-time Localization
DATE:    23/01/29 06:16:36 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:05:21 UT on 29 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230129A (trigger 696665126.147626 / 230129254).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 111.9, Dec = 2.4 (J2000 degrees, equivalent to J2000 07h 27m, 2d 23'), with a statistical uncertainty of 22.6 degrees.

The angle from the Fermi LAT boresight is 76.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230129254/quicklook/glg_skymap_all_bn230129254.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230129254/quicklook/glg_healpix_all_bn230129254.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230129254/quicklook/glg_lc_medres34_bn230129254.gif


GRB_name: GRB230130A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33234
SUBJECT: GRB 230130A: Fermi GBM Final Real-time Localization
DATE:    23/01/30 05:04:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:53:48 UT on 30 Jan 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230130A (trigger 696747233.90504 / 230130204).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 204.2, Dec = 55.8 (J2000 degrees, equivalent to J2000 13h 36m, 55d 47'), with a statistical uncertainty of 6.3 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/2023/bn230130204/quicklook/glg_skymap_all_bn230130204.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230130204/quicklook/glg_healpix_all_bn230130204.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230130204/quicklook/glg_lc_medres34_bn230130204.gif


GRB_name: GRB230128A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33235
SUBJECT: GRB 230128A: AstroSat CZTI detection
DATE:    23/01/30 09:22:07 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

P K. Navaneeth (IUCAA), R. Gopalakrishnan (IUCAA), G. Waratkar (IITB), 
A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka 
University/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 the detection of a long GRB230128A which was 
also detected by Fermi GBM (GCN Circ. 33231).

It was clearly detected in the CsI anticoincidence (Veto) detector in 
the 100-500 keV energy range. The light curve peaks at 2023-01-28 
22:48:33.09 UTC. The measured peak count rate is 669 (+68, -52) counts/s 
above the background in the combined Veto data of all quadrants, with a 
total of 9446 (+1558, -2165) counts. The local mean background count 
rate was 2912 (+3, -5) counts/s. We measure a T90 of 53 (+12, -16) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB230129A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33236
SUBJECT: GRB 230129A: AstroSat CZTI detection
DATE:    23/01/30 16:18:48 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

P K. Navaneeth (IUCAA), R. Gopalakrishnan (IUCAA), G. Waratkar (IITB), 
A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka 
University/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 the detection of short GRB 230129A which was 
also detected by Fermi GBM (GCN Circ. 33232).

The source was faintly detected in the 20-200 keV energy range. The 
light curve peaks at 2023-01-29 06:05:21.15 UTC. The measured peak count 
rate associated with the burst is 300 (+148, -38) counts/s above the 
background in the combined data of all quadrants, with a total of 161 
(+48, -54) counts. The local mean background count rate was 319 (+7, 
-12) counts/s. Using cumulative rates, we measure a T90 of 0.78 (+0.37, 
-0.36) s. We note that the T90 measurement may be a slight underestimate 
due to the limited number of photons detected from the burst.

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

CZTI GRB detections are reported regularly on the payload site at 
http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led 
consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB230201A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33242
SUBJECT: GRB 230201A: Fermi GBM Final Real-time Localization
DATE:    23/02/01 05:50:01 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:39:33 UT on 1 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230201A (trigger 696922778.405158 / 230201236).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 346.5, Dec = 43.8 (J2000 degrees, equivalent to J2000 23h 06m, 43d 47'), with a statistical uncertainty of 9.7 degrees.

The angle from the Fermi LAT boresight is 126.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230201236/quicklook/glg_skymap_all_bn230201236.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230201236/quicklook/glg_healpix_all_bn230201236.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230201236/quicklook/glg_lc_medres34_bn230201236.gif


GRB_name: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33243
SUBJECT: GRB 221009A: radio afterglow detection with the EVN
DATE:    23/02/01 10:41:25 GMT
FROM:    Stefano Giarratana at University of Bologna  <s.giarratana@ira.inaf.it>

S. Giarratana (University of Bologna, INAF-IRA), M. Giroletti 
(INAF-IRA), T. An (Shanghai A.O.), G. Anderson (Curtin University), P. 
Atri (ASTRON), J. S. Bright (University of Oxford), R. Fender 
(University of Oxford), G. Ghirlanda (INAF-OAB), J. K. Leung (University 
of Sydney, CSIRO), B. Marcote (JIV-ERIC), M. PÃ©rez-Torres (IAA-CSIC), L. 
Rhodes (University of Oxford), O. S. Salafia (INAF-OAB), J. Yang (OSO)

On UT 2022 November 18 and 21 (40 and 43 days post-burst) we observed 
the radio counterpart of GRB 221009A (Dichiara et al, GCN 32632; Veres 
et al., GCN 32636) with the European VLBI Network (EVN) at a central 
frequency of 8.3 and 5 GHz, respectively.

 From a preliminary analysis, the source is clearly detected at both 
frequencies with >30 sigma significance. The 8.3 GHz surface brightness 
peak is ~1.3 mJ/beam. The synthesized beam is 0.9 x 0.5 mas (PA = 7.7 
deg). The 5 GHz surface brightness peak is ~1.4 mJy/beam. The 
synthesized beam is 1.7 x 0.9 mas (PA = 9.25 deg).

The source is found at a position within ~1 mas of the one previously 
reported by Atri et al., GCN 32907 with the VLBA at 15.2 GHz. The offset 
is most likely accounted for by systematics.

All the results presented here are preliminary. Further analysis is in 
progress. We will report the final results in a forthcoming publication.

We would like to thank the directors and staff of all the EVN telescopes 
for approving, executing, and processing these out-of-session ToO 
observations.

The European VLBI Network is a joint facility of independent European, 
African, Asian, and North American radio astronomy institutes. 
Scientific results from data presented in this publication are derived 
from the following EVN project code: RG013.


GRB_name: GRB230201A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33245
SUBJECT: Fermi GRB 230201A: Global MASTER-Net observations report 
DATE:    23/02/01 14:15:17 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 230201A ( Fermi GBM team, GCN 33242) errorbox  30102 sec after notice time and 30143 sec after trigger time at 2023-02-01 14:01:57 UT, with upper limit up to  16.6 mag. The observations began at zenith distance = 69 deg. The sun  altitude  is -51.3 deg. 

The galactic latitude b = -15 deg., longitude l = 104 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2195907

We obtain a following upper limits.  

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

   30174 | 2023-02-01 14:01:57 |         MASTER-Amur | (23h 26m 10.17s , +46d 56m 59.1s) |   C |    60 | 16.5 |        
   30253 | 2023-02-01 14:03:16 |         MASTER-Amur | (23h 37m 52.83s , +46d 57m 45.0s) |   C |    60 | 16.5 |        
   30333 | 2023-02-01 14:04:36 |         MASTER-Amur | (23h 43m 41.80s , +45d 01m 42.1s) |   C |    60 | 16.6 |        
   30413 | 2023-02-01 14:05:56 |         MASTER-Amur | (23h 55m 06.14s , +45d 01m 50.0s) |   C |    60 | 16.5 |        
   30492 | 2023-02-01 14:07:15 |         MASTER-Amur | (23h 32m 04.89s , +48d 49m 45.5s) |   C |    60 | 16.5 |        
   30572 | 2023-02-01 14:08:35 |         MASTER-Amur | (23h 44m 15.31s , +48d 51m 13.9s) |   C |    60 | 16.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230126A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33246
SUBJECT: GRB 230126A: Detection by VZLUSAT-2
DATE:    23/02/01 18:29:36 GMT
FROM:    Marianna Dafcikova at Masaryk University  <500025@mail.muni.cz>

M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory),  N.
Werner  (Masaryk U.), M. Ohno (Hiroshima U.),  L. Meszaros, B. Csak
(Konkoly Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka,
F. Hroch, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, J. Kapus, M.
Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo (Needronix), G. Galgoczi
(Wigner Research Center/Eotvos U.), N. Uchida (ISAS/JAXA), T. Enoto (Kyoto
U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. Hirose, H. Matake (Hiroshima
U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), L. L. Kiss (Konkoly
Observatory),  T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka
(Univ of Tokyo), K. Torigoe (Hiroshima U.), P. Svoboda, V. Daniel, J.
Dudas, M. Junas, J. Gromes (VZLU), I. Vertat (FEL ZCU)  -- the
VZLUSAT-2/GRB payload collaboration.

The long duration GRB 230126A (Fermi/GBM detection: GCN Circ. 33225) was
detected by the GRB detector on board of the VZLUSAT-2 3U CubeSat (
https://www.vzlusat2.cz/en/).

The data acquisition was performed by the GRB detector unit no. 0 and the
detection was confirmed at the peak time 2023-01-26 18:20:46 UTC. The T90
duration was measured to be 14 s with the light curve resolution of 1 s.
The significance during T90 reaches 5.1 sigma.

The light curve obtained by VZLUSAT-2 is available here:

https://vzlusat2.konkoly.hu/static/share/GRB230126A_GCN_VZLUSAT2.pdf

All VZLUSAT-2 detections are listed at:
https://monoceros.physics.muni.cz/hea/VZLUSAT-2/

The GRB detectors on VZLUSAT-2 are a demonstration payload for a future
CubeSat constellation (Werner et al. Proc. SPIE 2018). Two GRB modules of
VZLUSAT-2 are placed in a perpendicular manner and each consists of a 75 x
75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy
range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 January 13
from Cape Canaveral.


GRB_name: GRB230201B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33247
SUBJECT: GRB 230201B: Fermi GBM Final Real-time Localization
DATE:    23/02/01 20:07:10 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 19:56:48 UT on 1 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230201B (trigger 696974213.104426 / 230201831).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 27.4, Dec = 16.5 (J2000 degrees, equivalent to J2000 01h 49m, 16d 30'), with a statistical uncertainty of 2.2 degrees.

The angle from the Fermi LAT boresight is 49.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230201831/quicklook/glg_skymap_all_bn230201831.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230201831/quicklook/glg_healpix_all_bn230201831.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230201831/quicklook/glg_lc_medres34_bn230201831.gif


GRB_name: GRB230201B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33249
SUBJECT: Fermi GRB 230201B: Global MASTER-Net observations report 
DATE:    23/02/02 09:45:19 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 230201B ( Fermi GBM team, GCN 33247) errorbox  48850 sec after notice time and 48883 sec after trigger time at 2023-02-02 09:31:32 UT, with upper limit up to  16.6 mag. Observations started at twilight.  The observations began at zenith distance = 36 deg. The sun  altitude  is -10.9 deg. 

The galactic latitude b = -44 deg., longitude l = 143 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2196085

We obtain a following upper limits.  

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

     656 | 2023-02-01 20:06:43 |             MASTER- | (01h 49m 58.81s , +16d 29m 53.9s) |   C |   120 | 16.7 |        
     810 | 2023-02-01 20:09:03 |             MASTER- | (01h 50m 03.58s , +16d 29m 05.6s) |   C |   150 | 16.6 |        
    1007 | 2023-02-01 20:12:04 |             MASTER- | (01h 49m 56.20s , +16d 28m 21.1s) |   C |   180 | 16.7 |        
    1206 | 2023-02-01 20:15:24 |             MASTER- | (01h 50m 01.17s , +16d 28m 39.3s) |   C |   180 | 16.6 |        
   48914 | 2023-02-02 09:31:32 |         MASTER-Amur | (01h 47m 36.09s , +16d 24m 48.5s) |   C |    60 | 16.1 |        
   48993 | 2023-02-02 09:32:51 |         MASTER-Amur | (01h 55m 52.14s , +16d 26m 10.9s) |   C |    60 | 16.3 |        
   49232 | 2023-02-02 09:36:50 |         MASTER-Amur | (01h 46m 34.64s , +14d 31m 51.4s) |   C |    60 | 16.3 |        
   49312 | 2023-02-02 09:38:09 |         MASTER-Amur | (01h 54m 45.72s , +14d 30m 46.2s) |   C |    60 | 16.5 |        
   49393 | 2023-02-02 09:39:31 |         MASTER-Amur | (01h 48m 40.42s , +18d 20m 14.0s) |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33254
SUBJECT: GRB 221216A: Swift-BAT refined analysis
DATE:    23/02/02 22:03:51 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC), S. Dichiara (PSU),
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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT  GRB 221216A (trigger #1144698)
(Dichiara, et al., GCN Circ. 33067).  The BAT ground-calculated position is
RA, Dec = 326.023, -34.394 deg which is
   RA(J2000)  =  21h 44m 05.6s
   Dec(J2000) = -34d 23' 37.4"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows two broad peaks, one centered around T+0,
and the other at T+165 seconds.  There is a third, more narrow and weaker peak
at T+50 seconds and some possible subsidiary peaks.  Note that not all of the event
data is available, so it is possible that the burst extended before or after this period.
T90 (15-350 keV) is 174.48 +- 5.26 sec (estimated error including systematics).

The time-averaged spectrum from -9.68 to T+175.22 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.02 +- 0.36,
and Epeak of 91.0 +- 44.0 keV (chi squared 37.14 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 4.6 +- 0.3 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.23 sec in the 15-150 keV band is
1.8 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.56 +- 0.08 (chi squared 44.55 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/1144698/BA/


GRB_name: GRB230201B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33259
SUBJECT: GRB 230201B: TURBO Optical Upper Limits
DATE:    23/02/03 22:21:28 GMT
FROM:    Robert Strausbaugh at University of Minnesota  <rstrausb@umn.edu>

R. Strausbaugh (UMN), D. Warshofsky (UMN), P. L. Kelly (UMN) report on
behalf of a larger collaboration:

We observed the GRB 230201B (Fermi GBM Team, GCN 33247) field with the
Total-Coverage Ultrafast Response to Binary-Mergers Observatory (TURBO)
prototype telescope in St. Paul, Minnesota on February 2, from 02:58 to
03:14 UT (corresponding to 7.03 to 7.30 hours after GRB trigger) in SDSS g
and r-band filters.

We acquired a series of 10x90s exposures in each band.  We do not detect
any fading sources in the GBM error region in either band, consistent with
available optical upper limits (Lipunov et al., GCN 33249).

The following 3-sigma upper limits in AB magnitudes are calculated using
the Pan-STARRS catalog as reference:

g > 17.95

r > 17.84

These magnitudes are not corrected for foreground Galactic extinction.

The TURBO prototype in St. Paul consists of two co-mounted 11-inch
telescopes each with a 6.6 square degree field of view. TURBO will consist
of two arrays of 8 pairs of co-mounted 11-inch telescopes at two dark-sky
sites: Magdalena Ridge Observatory, New Mexico, USA and Skinakas
Observatory, Crete, Greece.


GRB_name: GRB230204A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33260
SUBJECT: GRB 230204A: Swift detection of a possible burst (or possible transient Swift J1552.8-5055)
DATE:    23/02/04 03:45:02 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA),
V. D'Elia (SSDC & INAF-OAR), J. A. Kennea (PSU), A. Y. Lien (U Tampa),
A. Melandri (INAF-OAB), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB),
M. H. Siegel (PSU), A. Tohuvavohu (U Toronto) and M. A. Williams (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 02:56:57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230204A (trigger=1152509).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 238.164d, -50.858d which is 
   RA(J2000) = 15h 52m 39s
   Dec(J2000) = -50d 51' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Due to a telemetry gap, the BAT lightcurve
before T+8s is not immediately available, and no obvious variation is
visible in the remainder of the lightcurve, as is typical for an
image trigger. 

The XRT began observing the field at 02:59:24.1 UT, 146.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 238.1950, -50.9167 which is equivalent to:
   RA(J2000)  = 15h 52m 46.80s
   Dec(J2000) = -50d 55' 00.1"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). 

The initial flux in the 2.5 s image was 2.77e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 156 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the large, but
uncertain, extinction expected. 

We note that this source is near the Galactic plane (lat=2.38 deg)
and was detected as a 64 s image trigger, which raises the possibility
that this is a Galactic transient.  We would name this source
Swift J1552.8-5055 if it is not a GRB. 

Further analysis of the nature of this source will require the
full downlinked dataset. 

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


GRB_name: GRB230204A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33261
SUBJECT: GRB 230204A: Enhanced Swift-XRT position
DATE:    23/02/04 07:39:42 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 1193 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 230204A, 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 = 238.19965, -50.91653 which is equivalent
to:

RA (J2000): 15h 52m 47.91s
Dec (J2000): -50d 54' 59.5"

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: GRB230204A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33264
SUBJECT: GRB 230204A: Swift-XRT refined Analysis
DATE:    23/02/04 18:03:23 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), A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB), P.
D'Avanzo (INAF-OAB), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto),
D.N. Burrows (PSU) and A. D'Ai report on behalf of the Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 230204A (D'Ai et al. GCN
Circ. 33260), from 136 s to 46.9 ks after the  BAT trigger. The data
comprise 250 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 33261).

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.37 (+0.16, -0.14).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.64 (+/-0.10). The
best-fitting absorption column is  2.61 (+0.21, -0.20) x 10^22 cm^-2,
in excess of the Galactic value of 1.0 x 10^22 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.5 (+/-0.4) and a
best-fitting absorption column of 2.1 (+0.7, -0.6) x 10^22 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 7.6 x 10^-11 (1.2 x 10^-10) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.1 (+0.7, -0.6) x 10^22 cm^-2
Galactic foreground: 1.0 x 10^22 cm^-2
Excess significance: 2.8 sigma
Photon index:      1.5 (+/-0.4)

If the light curve continues to decay with a power-law decay index of
2.37, the count rate at T+24 hours will be 1.2 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.2 x
10^-16 (1.4 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01152509.

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


GRB_name: GRB230204B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33265
SUBJECT: GRB 230204B: MAXI/GSC detection
DATE:    23/02/04 22:51:17 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

M. Serino (AGU), W. Iwakiri (Chiba U.),
H. Negoro, M. Nakajima, K. Kobayashi, M. Tanaka, Y. Soejima (Nihon U.),
T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU),
Y. Tsuboi, J. Kohara, S. Urabe, S. Nawa, N. Nemoto (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. Kurihara (JAXA),
Y. Ueda, S. Ogawa, K. Setoguchi, T. Yoshitake, K. Inaba, Y. Nakatani (Kyoto U.),
M. Yamauchi, T. Sato, R. Hatsuda, R. Fukuoka, Y. Hagiwara, Y. Umeki (Miyazaki U.),
K. Yamaoka (Nagoya U.),
Y. Kawakubo (LSU),
M. Sugizaki (NAOC) 
report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source 
at 21:47:51 UT on 4 Feb 2023.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (197.581 deg, -21.752 deg) = (13 10 19, -21 45 07) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.12 deg and 0.1 deg, respectively.
The roll angle of long axis from the north direction is 156.0 deg counterclockwise.
Without assumptions on the source constancy, we obtain a rectangular error box 
for the transient source with the following corners.
(196.900, -21.911) deg = (13 07 36, -21 54 39) (J2000)
(196.998, -22.143) deg = (13 07 59, -22 08 34) (J2000)
(198.373, -21.637) deg = (13 13 29, -21 38 13) (J2000)
(198.273, -21.406) deg = (13 13 05, -21 24 21) (J2000)
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 628 +- 49 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at 20:15 UT
with an upper limit of 20 mCrab.


GRB_name: GRB230204A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33266
SUBJECT: GRB 230204A: Swift/UVOT Upper Limits
DATE:    23/02/04 23:36:26 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

 S. J. LaPorte (PSU) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 230204A
156 s after the BAT trigger (D'Ai et al., GCN Circ. 33260).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 33261)
is detected in the initial UVOT exposures.
A known source with no significant signs of fading
is detected 2.88 arcsec from the XRT position at:

RA (J2000): 15h 52m 47.83s
Dec (J2000): -50d 54' 56.74"

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           156            306          147          >17.5
u_FC                  314            564          246         >19.1
white                  156          1372          373         >17.8
v                         645          1596          117         >15.9
b                         570          1521            97         >17.9
u                         314          5553          382         >19.1
w1                      695           5489          274         >19.1
m2                      670          1446            97         >18.8
w2                       621          1571          117         >18.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 2.516 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB230204B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33267
SUBJECT: GRB 230204B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    23/02/05 02:56:17 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 230204B onboard (T0:
2023-02-04T21:44:25.2 UTC, CALET trig CALET 1359582171, Fermi/GBM trig
697239872, INTEGRAL trig 10188, MAXI GCN 33265).

The CALET, INTEGRAL, and Fermi 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 2022, ApJ,
941, 169), detects the burst with a sqrt(TS) of 21.5 in a 4.096 s
analysis time bin.
The burst duration as seen by BAT is ~65 s.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -4.
The OFOV localization is consistent with the MAXI position for this burst.

See Section 9.1 and Figures 10 and 17 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: GRB230204B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33268
SUBJECT: GRB 230204B: AstroSat CZTI detection
DATE:    23/02/05 05:39:45 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

G. Waratkar (IITB), P K. Navaneeth (IUCAA), P. Shetty (IITB), A. Ahmad 
(IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka 
University/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 the detection of the bright long GRB 230204B 
which was also detected by MAXI-GSC (GCN Circ. 33265), SWIFT/BAT-GUANO 
(GCN Circ. 33267), along with CALET, INTEGRAL and FERMI notices.

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 
2023-02-04 21:45:19.5 UTC. The measured peak count rate associated with 
the burst is 175.4 (+27.7 -26.6) counts/s above the background in the 
combined data of all four quadrants, with a total of 7611 (+557 -740) 
counts. The local mean background count rate was 131.2 (+0.7 -0.9) 
counts/s. Using cumulative rates, we measure a T90 of 216.64 (+5.13 
-22.56) s. In the preliminary analysis, we find 3240 Compton events 
associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve showed multiple peaks 
of emission with the strongest peak at 2023-02-04 21:45:18.7 UTC. The 
measured peak count rate is 1315.9 (+79.7 -88.8) counts/s above the 
background in the combined Veto data of all four quadrants, with a total 
of 48625 (+1487 -1923) counts. The local mean background count rate was 
1273.2 (+2.4 -1.8) counts/s. We measure a T90 of 212.32 (+2.94 -7.75) 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, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33269
SUBJECT: GRB 230204B: GIT discovery of the likely optical afterglow
DATE:    23/02/05 05:46:49 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

V. Swain (IITB), H. Kumar (IITB), G. Waratkar(IITB), V. Bhalerao (IITB), G.
C. Anupama(IIA), S. Barway (IIA) and K. Angail (IAO) report on behalf of
the GIT team:

We observed the field of GRB 230204B detected by MAXI (Serino et al., GCN
33265) with 0.7m GROWTH-India Telescope (GIT). We started observations at
23:22:37.597 UT, i.e., 1.57 hrs after the Swift/BAT trigger. We obtained 10
frames in the r' band of 300 sec each. We detected an uncatalogued source
at RA 13:10:34.96, Dec: -21:43:05.31 with an uncertainty of 0.67 arcsec.
There is no minor planet present at this position. The photometric results
follow as:

----------------------------------------------------------------------

 JD (mid) | T_mid-T0 (hrs) | Filter | Magnitude (AB) |

----------------------------------------------------------------------

 2459980.47404 | 1.57  | r' | 15.50 +/- 0.04  |

 2459980.50774 | 2.38  | r' | 16.45 +/- 0.05  |

----------------------------------------------------------------------

The candidate decayed by 0.95 magnitude during our observations, separated
by a time span of 48 mins. The fast decay suggests that the candidate is
likely an afterglow of GRB 230204B. We encourage photometric for further
confirmation and spectroscopic follow-up for redshift measurement. The
magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and
not corrected for Galactic extinction.

The GROWTH India Telescope (GIT; Kumar et al. 2022) 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 the operations
of the telescope. Telescope technical details are available at
https://sites.google.com/view/growthindia/.


GRB_name: GRB230205A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33271
SUBJECT: GRB 230205A: Swift detection of a burst
DATE:    23/02/05 11:01:42 GMT
FROM:    Elena Ambrosi at INAF-IASF  <elena.ambrosi@inaf.it>

E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), A. Y. Lien (U Tampa),
A. Melandri (INAF-OAB), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB)
and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 10:29:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230205A (trigger=1152764).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 202.072d, +46.684d which is 
   RA(J2000) = 13h 28m 17s
   Dec(J2000) = +46d 41' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Due to a telemetry gap, the BAT light curve
before T+8s is not immediately available, and after that time shows 
no obvious variability.  The BAT rate trigger was on a 3 s timescale,
consistent with the lack of variation at later times. 

The XRT began observing the field at 10:31:40.0 UT, 108.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 202.07147, 46.72613
which is equivalent to:
   RA(J2000)  = 13h 28m 17.15s
   Dec(J2000) = +46d 43' 34.1"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 151 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper.  We cannot determine whether the source
is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.09 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 1.2
(+0.71/-0.56) x 10^22 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 100 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers none of
the XRT error circle. The 8'x8' region for the list of sources generated
on-board covers 100% of the XRT error circle. The list of sources is typically
complete to about 18 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.036. 

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


GRB_name: GRB230204B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33272
SUBJECT: GRB 230204B: AGILE detection
DATE:    23/02/05 11:56:28 GMT
FROM:    Claudio Casentini at INAF-IAPS  <claudio.casentini@inaf.it>

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

The AGILE satellite detected the bright and long GRB 230204B at
T0 = 2023-02-04 21:44:25.2 s (UTC), reported by MAXI/GSC, Swift/BAT-GUANO,
AstroSAT CZTI, GIT (GCNs #33265, #33267, #33268 and #33269), CALET trig
1359582171, Fermi/GBM trig 697239872 and INTEGRAL trig 10188.

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 145 s and it released a total number of 170125
counts
in the MCAL detector (above a background rate of 1418 Hz), and 468843
counts in the AC
detector (above a background rate of 3197 Hz). The AGILE ratemeters light
curves
can be found at
http://www.agilescienceapp.it/notices/GRB230204B_AGILE_RM_A.png .

The event also triggered a partial high-time resolution MCAL data
acquisition,
from T0-20 s to T0+25 s (UTC). The multi-peaked MCAL light curve can be
found
at
http://www.agilescienceapp.it/notices/GRB230204B_082123_602631919.000000.png
.

At the T0, the event was 72 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: GRB230204B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33273
SUBJECT: GRB 230204B: Detection by GRBAlpha
DATE:    23/02/05 16:58:49 GMT
FROM:    Marianna Dafcikova at Masaryk University  <500025@mail.muni.cz>

M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner
(Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak
(Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P.
Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal,  A. Povalac (Brno U.
of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo,
M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U.
of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H.
Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos
U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G.
Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi
(Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss
(Konkoly Observatory),  T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.),
H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima
U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U.
Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The long-duration GRB 230204B (MAXI/GSC detection: GCN Circ. 33265;
Swift/BAT-GUANO detection: GCN Circ. 33267; AstroSat detection: GCN Circ.
33268; AGILE/MCAL detection: GCN Circ. 33272; Fermi/GBM detection: trigger
no. 697239872; CALET/GCBM detection: trigger no. 1359582171; INTEGRAL/SPI-ACS
detection: trigger no. 10188) was observed by the GRBAlpha 1U CubeSat (Pal
et al. Proc. SPIE 2020).

The detection was confirmed at the peak time 2023-02-04 21:47:03 UTC. The
T90 duration measured by GRBAlpha is 207 s and the maximum significance
during T90 reaches 25 sigma in the 110-370 keV band.

The light curve obtained by GRBAlpha is available here:

https://grbalpha.konkoly.hu/static/share/GRB230204B_GCN.pdf

All GRBAlpha detections are listed at:
https://monoceros.physics.muni.cz/hea/GRBAlpha/

GRBAlpha is a demonstration mission for a future CubeSats constellation
(Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75
x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy
range from ~50 keV to ~1000 keV. GRBAlpha was launched on 2021 March 22
from Baikonur. After its commissioning phase, the scientific observations
are now under way. To increase the duty cycle and the downlink rate, the
upgrade of the on-board data acquisition software stack is in progress. The
ground segment is also supported by the radio amateur community and it
takes advantage of the SatNOGS network for increased data downlink volume.


GRB_name: GRB230205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33274
SUBJECT: GRB 230205A: BOOTES-5/JGT early optical upper limit
DATE:    23/02/05 17:16:06 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado, I. Perez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), C. J. Perez del Pulgar (UMA) and I. Carrasco (SMA), I. H. Park (SKKU) on behalf of a larger collaboration, report:

Following the detection of GRB 230205A by Swift (Ambrosi et al. GCNC 33271), the BOOTES-5/JGT 0.6m robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) observed the GRB location starting on Feb. 5, 10:30:47 UT (~ 56 s after trigger). In the co-added image (20 x 60 s exposures in the clear filter), no optical afterglow is detected within the enhanced Swift/XRT error region (Ambrosi et al. GCNC 33271) down to 20.4 mag, which is consistent with the limit reported by UVOT (Ambrosi et al. GCNC 33271).

We thank the staff at Observatorio Astronomico Nacional in San Pedro Martir for their excellent support.


GRB_name: GRB230205A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33275
SUBJECT: GRB 230205A: Enhanced Swift-XRT position
DATE:    23/02/05 17:46:40 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 2803 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 230205A, 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 = 202.07096, +46.72520 which is equivalent
to:

RA (J2000): 13h 28m 17.03s
Dec (J2000): +46d 43' 30.7"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB230204B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33276
SUBJECT: GRB 230204B: Swift ToO observations
DATE:    23/02/05 20:06:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the MAXI GRB 230204B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021535

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 MAXI 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: GRB230205A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33277
SUBJECT: GRB 230205A: Swift-XRT refined Analysis
DATE:    23/02/05 21:29:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.9 ks of XRT data for GRB 230205A (Ambrosi et al. GCN
Circ. 33271), from 80 s to 30.1 ks after the  BAT trigger. The data
comprise 10 s in Windowed Timing (WT) mode (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. 33275).

The late-time light curve (from T0+5.1 ks) can be modelled with a
power-law decay with a decay index of alpha=0.85 (+0.29, -0.27).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.84 (+0.23, -0.22). The
best-fitting absorption column is  6.0 (+1.6, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 2.1 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.6 x 10^-11 (7.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.0 (+1.6, -1.4) x 10^21 cm^-2
Galactic foreground: 2.1 x 10^20 cm^-2
Excess significance: 6.8 sigma
Photon index:      1.84 (+0.23, -0.22)

If the light curve continues to decay with a power-law decay index of
0.85, the count rate at T+24 hours will be 5.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.6 x
10^-13 (4.0 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01152764.

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


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33278
SUBJECT: GRB 230204B: ATLAS detection of the optical afterglow and a projected location in a nearby galaxy group
DATE:    23/02/05 23:27:16 GMT
FROM:    Stephen Smartt at Queen's U/Belfast  <s.smartt@qub.ac.uk>

S. J. Smartt (Oxford), K. W. Smith, S. Srivastav, D. R. Young,,
M. Fulton, M. McCollum, T. Moore, J. Weston (Queen's University
Belfast), L. Shingles (GSI/QUB), L. Rhodes (Oxford), L. Denneau, J.
Tonry, H. Weiland, A. Lawrence, R. Siverd (IfA, University of Hawaii),
N. Erasmus, W. Koorts (South African Astronomical Observatory), A.
Jordan, V. Suc (UAI, Obstech), A. Rest (STScI), T.-W. Chen (TUM/MPA),
M. Nicholl (Birmingham), C. Stubbs (Harvard), J. Sommer (LMU/QUB)

We report early optical observations of the afterglow of the Maxi/GSC
discovered GRB 230204B (Serino et al. GCN 33265). The optical
afterglow was discovered by Kumar et al. (GCN 29233) at r=15.50 +/-
0.04 with a decline rate of 1.2 mag per hr. Kumar et al. reported this
optical transient discovery as AT2023bic to the Transient Name Server.

We observed the field with the ATLAS system in normal survey mode.
ATLAS is a quadruple 0.5m telescope system with two units in Hawaii,
and one each in Chile and South Africa (see Tonry et al. 2018,
PASP,130:064505). Our transient science server (Smith et al. 2020,
PASP, 132:085002) independently detected AT2023bic on the ATLAS
(Sutherland) images at coordinates RA = 13:10:34.93, Declination =
-21:43:05.1 (J2000).

Forced photometry at those coordinates results in the following AB
magnitudes in the o-band filter (a broad r+i composite filter) :

MJD                   Date                             mag   dmag
59980.05525005 2023-02-05 01:19:33 17.05 0.04
59980.05708335 2023-02-05 01:22:12 17.18 0.05
59980.07028305 2023-02-05 01:41:12 17.33 0.05
59980.07343935 2023-02-05 01:45:45 17.32 0.05

We measure a decline rate of 0.6 mag per hr, approximately 2hrs after
the Kumar et al. measurement. The decline may be slowing.

We note that AT2023bic is located 108.60" N, 10.90" W from the nearby
galaxy ESO 576- G 003, at z = 0.009873 (approximately 40Mpc). This
galaxy sits within the PGC1 0045721 galaxy group (NED and Kourkchi &
Tully 2017, ApJ 843, 16). While this is likely a line of sight
coincidence, a spectroscopic redshift of AT2023bic is needed. If it
were at a distance of 40Mpc, it would be 22kpc projected offset from
ESO 576- G 003. There is no source in the Pan-STARRS 3Pi images at
this positon (Chambers et al. arXiv:1612.05560).


GRB_name: GRB230204A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33279
SUBJECT: GRB 230204A: Swift-BAT refined analysis
DATE:    23/02/06 03:46:38 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Parsotan (GSFC/UMBC), S. D. Barthelmy (GSFC),
A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. 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 230204A (trigger #1152509)
(D'Ai et al., GCN Circ. 33260).  The BAT ground-calculated position is
RA, Dec = 238.166, -50.848 deg which is
   RA(J2000)  =  15h 52m 39.8s
   Dec(J2000) = -50d 50' 52.8"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 48%.

The mask-weighted light curve shows a multi-peaked structure that
starts at ~T-10 and ends at ~T+200 s. The most prominent peak
occurs at ~T+148 s. T90 (15-350 keV) is 182.05 +- 16.73 sec
(estimated error including systematics).

The time-averaged spectrum from T-6.81 to T+195.62 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.72 +- 0.13.  The fluence in the 15-150 keV band is 3.7 +- 0.3 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+148.12 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1152509/BA/


GRB_name: GRB230205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33280
SUBJECT: GRB 230205A: Swift-BAT refined analysis (T90 = 2.3 s)
DATE:    23/02/06 04:14:03 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-240 to T+962 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 230205A (trigger #1152764)
(Ambrosi et al., GCN Circ. 33271).  The BAT ground-calculated position is
RA, Dec = 202.057, 46.686 deg which is
   RA(J2000)  =  13h 28m 13.7s
   Dec(J2000) = +46d 41' 08.1"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a short pulse that starts at ~T0,
peaks at ~T+2 s, and ends at ~T+3 s. In addition, there may be some
hint of extended emission that lasts till ~T+80 s. T90 (15-350 keV)
is 2.30 +- 0.36 sec (estimated error including systematics).

The time-averaged spectrum from T+0.32 to T+2.87 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.44 +- 0.29.  The fluence in the 15-150 keV band is 1.6 +- 0.3 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+1.74 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1152764/BA/


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33281
SUBJECT: GRB 230204B: VLT/X-shooter redshift
DATE:    23/02/06 11:18:58 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

A. Saccardi (GEPI, Paris obs.), D. A. Kann (Goethe Univ.), J. Palmerio 
(GEPI, Paris obs. and IAP), V. Dâ€™Elia (SSDC and INAF-OAR), B. Schneider 
(MIT), L. Izzo (DARK/NBI), A. de Ugarte Postigo (OCA), D. B. Malesani 
(Radboud Univ. and DAWN/NBI) report on behalf of the Stargate collaboration:

We observed the optical afterglow of GRB 230204B (Serino et al., GCN 
33265; Swain et al., GCN 33269), also known as AT 2023bic (Smartt et 
al., GCN 33278), using the ESO VLT UT3 (Melipal) equipped with the 
X-shooter spectrograph. Our spectra cover the wavelength range 
3000-25000 AA, and consist of 4 exposures by 600 s each. The observation 
mid time was 2023 Feb 6.22 UT (31.4 hr after the GRB).

In a 30 s image taken with the acquisition camera on Feb 6.19 UT, we 
detect the optical afterglow, for which we measure a magnitude r = 21.55 
+- 0.18 AB (calibrated against a single nearby star from the Pan-STARRS 
catalog).

A faint continuum is the detected in the visible and near-infrared arms. 
Several, weak absorption features can be identified, which we interpret 
as due to Mg II, Mg I and Fe II at a common redshift of z = 2.142. While 
individual lines have low S/N, the combined detection of multiple 
features provides a convincing measurement of the redshift of this 
absorption system.

The association with the PGC1 0045721 galaxy group is thus a chance 
superposition, as already suggested by Smartt et al. (GCN 33278).

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Claudia Paladini and Heidi Korhonen.


GRB_name: GRB230205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33282
SUBJECT: GRB 230205A: OHP/T193 optical observations
DATE:    23/02/06 11:57:33 GMT
FROM:    Damien Turpin at NAOC (CAS)  <dturpin-astro@hotmail.com>

D. Turpin (CEA Paris-Saclay), C. Adami (LAM), E. Le Floc'h,
D. Gotz, C. Plasse (CEA Paris-Saclay), B. Schneider (MIT),
S. D. Vergani, A. Saccardi (GEPI, Observatoire de Paris), 
S. Basa, M. Ferrari, A. Le Van Suu (LAM) report 
on behalf of a larger collaboration:

We observed the field of the possible short GRB 230205A (Ambrosi et al.,
GCN 33271; Page et al., GCN 33277, Sakamoto et al., GCN 33280) using the 
T193cm telescope equipped with MISTRAL at Observatoire de Haute-Provence 
(France). 
Six exposures were obtained in the R-band (5x20s + 1x60s + 1x120s +
2x180s) under poor weather conditions from 2023 06 Feb. 03:37:06 UT to
2023 06 Feb 04:07:34 UT. 
In the combined last two frames (mid time ~17.57h after trigger), 
we do not detect the source and obtain the following upper limit:

R > 20.95 mag (AB)

The photometric calibration was performed using nearby stars from 
the PanSTARRS catalog.

No further observations using the MISTRAL instrument mounted on the 
T193-OHP are planned.

We acknowledge the excellent support from Observatoire de Haute Provence, 
in particular Stephane Favard, Jerome Schmitt.


GRB_name: GRB230205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33283
SUBJECT: GRB 230205A: SVOM/C-GFT optical upper limit
DATE:    23/02/06 13:09:38 GMT
FROM:    Chao Wu at NAOC  <wuchao.lamost@gmail.com>

Chao Wu (NAOC),  Zhe Kang (CHO), Liping Xin (NAOC), Xuhui Han (NAOC),
Xiaomeng Lu (NAOC),  Damien Turpin(CEA),  Zhenwei Li (CHO)ï¼ŒPinpin
Zhang (NAOC)ï¼ŒRuosong Zhang (NAOC)ï¼ŒYulei Qiu (NAOC)ï¼ŒYou  Lv (CHO)ï¼ŒJing
Wang(GXU), Cordier Bertrand (CEA)  and Jianyan Wei (NAOC) on behalf of
SVOM GRB team

We observed the burst GRB230205A (Ambrosi et al. GCN 33271) on
14:02:03 UT, Feb. 5th, 2023, about 3.5 hours after the Swift trigger
with C-GFT (Chinese Ground Follow-up Telescope in SVOM mission) in
System Test Mode (STM). C-GFT is located at Jilin (long.=126.33 deg,
lat.= 43.8243778 deg), Changchun Observatory, National Astronomical
Observatories, CAS. It has FOV of 1.5 deg X 1.5 deg with a 4k*4k CMOS
detector mounted on the primary focus of  1.2-meter-aperure telescope.

A series of g and r band images were obtained. The exposure time was
30 seconds for each frame.

No optical afterglow was detected within the enhanced XRT error box
(Goad et al., GCN 33275) down to a limit magnitude of 17.0 mag in each
r-band single frame (in STM).  The photometry was calibrated with
nearby UCAC 4 catalogs. The upper limit is consistent with the limit
reports (Ambrosi et al. GCN 33271;  Hu et al., GCN 33274).

More detailed analysis is continuing.

We thank the observation assistant Bowen Li at Jilin observatory for
their excellent support.


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33284
SUBJECT: GRB 230204B: 3.6m DOT optical observation
DATE:    23/02/06 13:35:11 GMT
FROM:    Amit Kumar Ror at ARIES  <mitturor77894@gmail.com>

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

We observed the field of GRB 230204B detected by MAXI/GSC (Serino et al.
2023, GCN 33265) using the 3.6m Devasthal Optical Telescope located at the
Devasthal observatory of the Aryabhatta Research Institute of Observational
Sciences (ARIES), Nainital, India.

We have taken multiple frames having an exposure time of 180 sec each in
the r filter. We stacked the images after the alignment. We clearly detect
the optical transient discovered by Swain and Kumar et al. 2023 (GCN 33269)
in the stacked images. The estimated preliminary magnitude is the following:

Date Start_UT T_start-T0 (days) Filter  Exp time (sec)       magnitude
==============================================================
2023-02-06 01:49:47.93   ~1.168          r        180 sec*10
 21.04 +/- 0.04

The detection of the optical transient is consistent with the observation
of Swain and Kumar et al. 2023 (GCN 33269), Smartt et al. 2023 (GCN 33278),
and Saccardi et al. 2023 (GCN 33281)

The limiting magnitude quoted is not corrected for the galactic and host
extinctions in the direction of the transient. Photometric calibration is
performed using the standard stars from the Pan-STARRS catalog.

This circular may be cited. The 3.6m Devasthal Optical Telescope (DOT) is a
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). The authors of this GCN circular thankfully
acknowledge the consistent support from the staff members to run and
maintain the 3.6m DOT.


GRB_name: GRB230204B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33285
SUBJECT: GRB 230204B: Swift-XRT afterglow detection
DATE:    23/02/06 15:16:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 230204B (Serino et al. GCN Circ. 33265). A possible optical
counterpart was reported by GIT (Swain et al. GCN Circ. 33269).
Swift-XRT observations consist of 4.2 ks of Photon Counting (PC) mode
data between T0+80.5 ks and T0+97.9 ks.

One uncatalogued X-ray source has been detected consistent with the GIT
position. The source is below the RASS limit but does not show
definitive signs of fading. This is most likely the afterglow, given
also the reported redshift of z=2.14 (Saccardi et al. GCN Circ. 33281)
but further observations are required to assess for fading. Details of
this source are given below:

Source 3:
  RA (J2000):  197.6441  =  13:10:34.58
  Dec (J2000): -21.7164  =  -21:42:58.9
  Error: 7.4 arcsec (radius, 90% conf.)
  Count-rate: (5.6 +/- 1.5)e-3 ct s^-1  
  Distance: 8 arcsec from MAXI position.
  Flux: (3.8 +/- 1.0)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021535.

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


GRB_name: GRB230205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33286
SUBJECT: GRB 230205A: LCOGT Optical Upper Limits
DATE:    23/02/06 16:21:38 GMT
FROM:    Robert Strausbaugh at University of Minnesota  <rstrausb@umn.edu>

R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on
behalf of a larger collaboration:

We observed the GRB 230205A (Ambrosi et al., GCN 33271) field with the
LCOGT 1-meter Sinistro instrument at the McDonald Observatory, TX, USA
site, on February 6, from 11:51 to 12:23 UT (corresponding to 25.20 to
25.52 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in each band.  We do not detect a
source in either band within the XRT enhanced error region (Goad et al.,
GCN 33275) consistent with other optical upper limits (Hu et al., GCN
33274; Turpin et al., GCN 33282; Wu et al., GCN 33283).

The following magnitudes and upper limits are calculated using the
PanSTARRS catalog as reference:

r > 21.2
i > 20.8

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB230204B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33288
SUBJECT: GRB 230204B: Fermi GBM detection
DATE:    23/02/06 20:28:18 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

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

"At 21:44:27.20 UT on 4 February 2023, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 230204B (trigger 697239872 / 230204906)
which was also detected by the Swift/BAT-GUANO (Kennea et al. 2023, GCN
33267),
Swift-XRT (D'Elia et al. 2023, GCN 33285), MAXI/GS (Serino et al. 2023, GCN
33265),
AGILE (Casentini et al. 2023, GCN 33272), ATLAS (Smartt et al. 2023, GCN
33278),
and VLT/X-shooter (Saccardi et al. 2023, GCN 33281).

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

The GBM light curve consists of multiple peaks followed
by some extended emission with a duration (T90) of about 216 s (50-300 keV).
The time-averaged spectrum from T0-1.024 s to T0+228.4 s
is best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.97 +/- 0.02  and
the cutoff energy, parameterized as Epeak, is 783 +/- 40 keV.
A Band function fits equally well, with Epeak = 763 +/- 45 keV,
alpha = -0.97 +/- 0.02 and beta = -2.73 +/- 0.29.

The event fluence (10-1000 keV) in this time interval is
(138.9 +/- 1.5)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+156 s in the 10-1000 keV band
is 7.3 +/- 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: GRB230205A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33289
SUBJECT: GRB 230205A: Swift/UVOT Upper Limits
DATE:    23/02/06 20:44:18 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M.H. Siegel (PSU) and E/ Ambrosi (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 230205A
100 s after the BAT trigger (Ambrosi et al., GCN Circ. 33271).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 33275)
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           100          250          147         >21.3
u_FC               258          508          246         >20.3
white              100         5198          526         >21.5
v                  588         1581          117         >19.5
b                  514         1680          117         >20.1
u                  258         1481          343         >20.2
w1                 638          657           19         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.036 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB230204B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33292
SUBJECT: GRB 230204B: Swift/UVOT Upper Limits
DATE:    23/02/06 20:50:39 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) and V. Dâ€™Elia (SSDC & INAF-OAR)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 230204B
80 ks after the MAXI trigger (Serino et al., GCN Circ. 33265).
No optical afterglow consistent with the optical or XRT positions
(Swain et al., GCN Circ. 33269, Smartt et al., GCN Circ. 33278, Dâ€™Elia et al.,
GCN Circ. 33285) 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

v                81062       109630          314         >19.1
b                80652       109220          314         >20.1
u                80567       109136          314         >19.8
w1               80403       109052          629         >20.1
m2               81146       109877         2154         >20.9
w2               80737       109546         1259         >20.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.109 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33293
SUBJECT: GRB 230204B: LCOGT Optical Upper Limits
DATE:    23/02/06 21:29:51 GMT
FROM:    Robert Strausbaugh at University of Minnesota  <rstrausb@umn.edu>

R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on
behalf of a larger collaboration:

We observed the GRB 230204B (Serino et al., GCN 33265) field with the LCOGT
1-meter Sinistro instrument at the Siding Spring Observatory, Australia
site, on February 6, from 15:27 to 16:24 UT (corresponding to 38.33 to 39.3
hours from the GRB trigger time) with the SDSS g, r, and i filters.

We performed a series of 3x300s exposures in each band.  We do not detect a
source in any band at the GIT optical counterpart location (Swain et al.,
GCN 33269), evidence for additional fading compared to early optical
detections (Swain et al., GCN 33269; Smartt et al., GCN 33278; Saccardi et
al., GCN 33281; Ror et al., GCN 33284).

The following upper limits are calculated using the PanSTARRS catalog as
reference:
g > 22.0
r > 21.9
i > 21.1
These magnitudes are not corrected for galactic extinction.


GRB_name: GRB230207A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33294
SUBJECT: GRB 230207A: Fermi GBM Final Real-time Localization
DATE:    23/02/07 00:42:00 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 00:30:44 UT on 7 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230207A (trigger 697422649.274452 / 230207021).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 234.3, Dec = -32.5 (J2000 degrees, equivalent to J2000 15h 37m, -32d 30'), with a statistical uncertainty of 4.9 degrees.

The angle from the Fermi LAT boresight is 82.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230207021/quicklook/glg_skymap_all_bn230207021.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230207021/quicklook/glg_healpix_all_bn230207021.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230207021/quicklook/glg_lc_medres34_bn230207021.gif


GRB_name: GRB230207A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33295
SUBJECT: Fermi GRB 230207A: Global MASTER-Net observations report 
DATE:    23/02/07 01:00:23 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 230207A ( Fermi GBM team, GCN 33294) errorbox  614 sec after notice time and 647 sec after trigger time at 2023-02-07 00:41:32 UT, with upper limit up to  18.8 mag. The observations began at zenith distance = 52 deg. The sun  altitude  is -35.8 deg. 

The galactic latitude b = 18 deg., longitude l = 339 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2197290

We obtain a following upper limits.  

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

     713 | 2023-02-07 00:41:32 |         MASTER-SAAO | (15h 17m 05.81s , -31d 23m 31.7s) |   C |   130 | 18.5 |        
     713 | 2023-02-07 00:41:32 |         MASTER-SAAO | (15h 16m 03.20s , -31d 22m 38.3s) |   C |   130 | 18.4 |        
     889 | 2023-02-07 00:44:13 |         MASTER-SAAO | (15h 17m 00.65s , -31d 24m 30.0s) |   C |   160 | 18.8 |        
     889 | 2023-02-07 00:44:13 |         MASTER-SAAO | (15h 15m 57.97s , -31d 23m 36.8s) |   C |   160 | 18.6 |        
    1090 | 2023-02-07 00:47:24 |         MASTER-SAAO | (15h 16m 04.72s , -31d 23m 24.9s) |   C |   180 | 18.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230207B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33296
SUBJECT: GRB 230207B: AGILE detection of a burst
DATE:    23/02/07 11:50:36 GMT
FROM:    Claudio Casentini at INAF-IAPS  <claudio.casentini@inaf.it>

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

The AGILE satellite detected the long GRB 220307B at
T0 = 2023-02-07 04:40:48 s (UTC) (CALET trig. 1359779945).

The burst is clearly visible in the AGILE scientific ratemeters of the
MiniCALorimeter (MCAL; 0.4-100 MeV) and in all the five panels of the
AntiCoincidence
system (AC Top, 50-200 keV; AC Lat, 80-200 keV). The event lasted about 14
s and it
released a total number of 15515 counts in the MCAL detector (above a
background rate of 996 Hz),
and 49298 counts in the AC Top detector (above a background rate of 2674
Hz).
The AGILE ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/GRB230207B_AGILE_RM_ND.png .

The event also triggered a (partial) high-time resolution MCAL data
acquisition,
from T0-1 s to T0+5 s (UTC), and released 116 counts in the detector, above
a background rate of 67 Hz. The MCAL light curve can be found
at
http://www.agilescienceapp.it/notices/GRB230207B_082154_602829648.000000.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: GRB230207B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33298
SUBJECT: GRB 230207B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    23/02/07 17:30:03 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 230207B onboard (T0:
2023-02-07T04:40:48 UTC, CALET trig 1359779945, INTEGRAL 10190, AGILE
GCN 33296)

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ,
941, 169), detects the burst with a sqrt(TS) of 27.8 in a 8.192 s
analysis time bin.
The burst duration as seen by BAT is ~15 s.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -36.

See Section 9.1 and Figures 10 and 17 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: GRB230208A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33300
SUBJECT: GRB 230208A: Fermi GBM Final Real-time Localization
DATE:    23/02/08 09:20:32 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 09:10:08 UT on 8 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230208A (trigger 697540213.924094 / 230208382).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 81.0, Dec = 54.7 (J2000 degrees, equivalent to J2000 05h 24m, 54d 42'), with a statistical uncertainty of 26.7 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/2023/bn230208382/quicklook/glg_skymap_all_bn230208382.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230208382/quicklook/glg_healpix_all_bn230208382.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230208382/quicklook/glg_lc_medres34_bn230208382.gif


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33301
SUBJECT: GRB 230204B: MASTER early OT detection
DATE:    23/02/08 11:22:06 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V.Lipunov (Lomonosov MSU), D.A.H.Buckley (SAAO), A.Chasovnikov, Ya.Kechin, A.Kuznetsov, 
N.Tiurina, O.Gress, E.Gorbovskoy, G.Antipov, P.Balanutsa, K.Zhirkov, D.Vlasenko, V.Senik, D.Kuvshinov,
V.Topolev, Yu.Tselik, D.Cheryasov, I.Gorbunov (Lomonosov Moscow State University, SAI, Physics Department),
C.Francile, R. Podesta, F. Podesta (Observatorio Astronomico Felix Aguilar of San Juan National University of Argentina),
R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.Corella,L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory),
N.M.Budnev (ISU,API),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational State University)

MASTER OT J131034.94-214304.8 early detection of MAXI GRB 230204B optical 
counterpart (Swain et al. GCN 33269, Smartt et al. GCN 33278, Saccardi et al. GCN 33281, Ror et al. GCN 33284, Siegel et al. GCN 33292, Strausbaugh et al. GCN 33293)

MASTER-SAAO robotic telescope  (Global MASTER-Net http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, v.2010, 30L)
located in South African Astronomical Observatory,
started inspect of the MAXI GRB230204.91 (trigger 979708795, 13h10m14.88s, -22d02m13.2s, R=1deg, Serino et al. GCN 33265; 
Kennea et al. GCN 33267, Waratkar et al. GCN 33268, Casentini et al. GCN 33272, Dafcikova et al. GCN 33273, D'Elia et al. GCN 33285, Poolakkil et al. GCN 33288)
errorbox 85 sec after notice time (1075 sec after trigger time) at 2023-02-04 22:06:06 UT
with upper limit  to  19.4m ( unfiltered ) .

Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2196693

The observations began at zenith distance = 63 deg. The sun  altitude: -40.5 deg., the distance to Moon (alt=12 deg.) was 89 deg., the Moon phase 0.99). The galactic latitude b = 40 deg., longitude l = 309 deg.

MASTER-SAAO auto-detection system ( Lipunov et al., 2010 )
detected OT source at (RA, Dec) = 13h 10m 34.94s -21d 43m 04.8s at 2023-02-04.92090 UT.
The OT unfiltered magnitude at first image is 12.9m (mlim=17.6). Automatic light curve decay has pecularity.
We have reference image on 2020-04-24.82001 UT with  unfiltered mlim=20.6m.

We observed this field also in very wide field cameras (MASTER-VWFC).
The reduction will be continued.


GRB_name: GRB230205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33302
SUBJECT: GRB 230205A: possible host galaxy detection with the Schmidt - Asiago telescope
DATE:    23/02/08 14:42:11 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

L. Tomasella (INAF-OAPd), P. Dâ€™Avanzo, (INAF-OAB), E. Cappellaro (INAF-OAPd) on behalf of a larger collaboration report:

We observed the field of the possibly short GRB 230205A (Ambrosi et al, GCN Circ. 33271; Sakamoto et al., GCN Circ. 33280) 
with the Schmidt telescope of the INAF - Padova Astronomical Observatory located in Asiago (Italy). Observations were carried 
out in imaging mode with the r and i filters about 2.5 days after the burst T0. 

No clear afterglow candidate is detected within the enhanced XRT position (Goad et al., GCN Circ. 33275) down to the following 
magnitude limits: r > 21.2 mag, i > 21.0 mag (AB; 3sigma c.l.). 

In our i-band image we detect a source at the SW edge of the XRT error circle at the following position (J2000):
RA = 13:28:16.87
Dec = +46:43:29.3 

For this source we measure a magnitude of i = 21.1 +/- 0.3 (AB). 

We note that this source is detected also in archival SDSS and Pan-STARRS images. In the SDSS the source is named as 
SDSS J132816.81+464329.8 and is flagged as a galaxy with a photometric redshift of z = 0.484 +/- 0.090 and a magnitude 
i = 21.19 +/- 0.11 mag (AB; consistent with our measurement). 

This object is therefore a candidate host galaxy for GRB 230205A. 

As a further note, we report that the position of the X-ray afterglow of GRB 230205A lies at about 3.5 arminutes (in projection) 
to the galaxy NGC 5169 (whose luminosity distance is ~ 33 Mpc). 


GRB_name: GRB230207B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33303
SUBJECT: GRB 230207B: Detection by GRBAlpha
DATE:    23/02/08 14:52:24 GMT
FROM:    Marianna Dafcikova at Masaryk University  <500025@mail.muni.cz>

M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner
(Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak
(Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P.
Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal,  A. Povalac (Brno U.
of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo,
M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U.
of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H.
Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos
U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G.
Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi
(Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss
(Konkoly Observatory),  T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.),
H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima
U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U.
Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The long-duration GRB 230207B (AGILE/MCAL detection: GCN Circ. 33296;
Swift/BAT-GUANO detection: GCN Circ. 33298; CALET/GCBM detection: trigger
no. 1359779945; INTEGRAL/SPI-ACS detection: trigger no. 10190) was observed
by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The detection was confirmed at the peak time 2023-02-07 04:40:48 UTC. The
T90 duration measured by GRBAlpha is 10 s and the overall significance
during T90 reaches 25 sigma.

The light curve obtained by GRBAlpha is available here:

https://grbalpha.konkoly.hu/static/share/GRB230207B_GCN.pdf

All GRBAlpha detections are listed at:
https://monoceros.physics.muni.cz/hea/GRBAlpha/

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a
future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector
of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a
SiPM array, covering the energy range from ~50 keV to ~1000 keV. To
increase the duty cycle and the downlink rate, the upgrade of the on-board
data acquisition software stack is in progress. The ground segment is also
supported by the radio amateur community and it takes advantage of the
SatNOGS network for increased data downlink volume.


GRB_name: GRB221009A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33305
SUBJECT: GRB 221009A: Continued Swift Observations
DATE:    23/02/08 18:41:45 GMT
FROM:    Maia Williams at Penn State  <mjw6837@psu.edu>

M. Williams (PSU) reports on behalf of the Swift Team:

Swift resumed observations of GRB 221009A on February 7 at 00:51 UTC after the end of Sun constraint, ~10 Ms after the Fermi/GBM trigger (Veres et al., GCN Circ. 32636). The X-ray afterglow is still faintly detectable (1.9 x 10^-3 counts s^-1) in a 9.4 ks XRT exposure.

Further observations are planned for this weekend.


GRB_name: GRB230209A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33306
SUBJECT: GRB 230209A: Fermi GBM Final Real-time Localization
DATE:    23/02/09 04:38:55 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 04:28:40 UT on 9 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230209A (trigger 697609725.271226 / 230209187).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 227.8, Dec = -18.6 (J2000 degrees, equivalent to J2000 15h 11m, -18d 36'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 1.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230209187/quicklook/glg_skymap_all_bn230209187.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230209187/quicklook/glg_healpix_all_bn230209187.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230209187/quicklook/glg_lc_medres34_bn230209187.gif


GRB_name: GRB230205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33307
SUBJECT: GRB 230205A: SUBARU HSC pre-imaging for host galaxy search
DATE:    23/02/09 16:31:10 GMT
FROM:    Kuiyun Huang at CYCU  <kuiyun@gmail.com>

Y. Urata, K.Y. Huang on behalf of a larger collaboration

We processed pre-imaging data for the field of the possible short GRB
230205A (Ambrosi et al., GCN Circ. 33271; Sakamoto et al., GCN Circ. 33280)
obtained by SUBRU Hyper-Suprime-Cam with i-band filter on June 6, 2019.
No clear source is identified within the enhanced XRT position (Goad et
al., GCN Circ. 33275).
The host galaxy candidate suggested by Tomasella et al. (GCN Circ. 33302)
is clearly detected.
In addition to this source, there is a source with i = 22.1 +/- 0.1
at the NW edge of the XRT error circle at RA = 13:28:16.92 Dec =
+46:43:32.73.

The image is available at the following link.
https://lh3.googleusercontent.com/VfQ2VhB3PtkCkwrfTVEKX0M0ARJ4bMKJk5g8vnVejx2Onx5CO5HamxaU6h34PDI1m0_MYmf3s-QSkacCSJYbEIMLV57-NkLBpnrVQCxVrMatuUvc4uf0euvRk9m65tiY7A=w1280


GRB_name: GRB230209A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33308
SUBJECT: GRB 230209A is not a GRB
DATE:    23/02/09 17:19:49 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

J. Wood (NASA/MSFC) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:

"The Fermi Gamma-ray Burst Monitor (GBM) trigger 697609725/230209187 at 04:28:40 UT
on 09 February 2023, tentatively classified as GRB 230209A (GCN 33306), is in fact not due
to a GRB. This trigger is likely due to local particles."


GRB_name: GRB230205A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33309
SUBJECT: GRB 230205A: 6 GHz VLA observations
DATE:    23/02/09 22:07:28 GMT
FROM:    Genevieve Schroeder at Northwestern University  <genevieveschroeder2023@u.northwestern.edu>

G. Schroeder, J. C. Rastinejad, W. Fong, C. D. Kilpatrick, A. E. Nugent
(Northwestern), E. Berger (Harvard), T. Laskar (Utah) report:

"We observed the position of the possibly short GRB 230205A (Ambrosi et al,
GCN 33271; Sakamoto et al., GCN 33280) with the Karl G. Jansky Very Large
Array (VLA) under program 23A-296 (PI: Schroeder) beginning on 2023
February 8.25 UT (2.81 days post-burst) at a mean frequency of 6 GHz.


We detect a radio source with a flux of ~40 microJy at the position:


RA(J2000) = 13:28:16.838

Dec(J2000) = +46:43:32.87


with an uncertainty of ~0.5" in each coordinate. This position is on the
outskirts of the XRT position (Goad et al. GCN 33275), on the NW edge. The
radio source position is consistent with the position of the optical source
reported by Urata et al. GCN 33307, although with a slight offset of
~0.85". If we assume this optical source is the host galaxy of GRB 230205A
and the radio source is afterglow, we find a probability of chance
coincidence of Pcc ~ 0.003 (Bloom et al. 2002). Alternatively, the detected
radio emission could originate from the host. In contrast, the radio source
is offset by ~3.6" from the center of the cataloged optical source (SDSS
J132816.81+464329.8) mentioned by Tomasella et al. GCN 33302. If we instead
assume that SDSS J132816.81+464329.8 is the host galaxy of GRB 230205A, we
find Pcc ~ 0.02.


Further observations are planned to determine the variability of the radio
source. We thank the VLA staff for quickly approving and executing these
observations."


GRB_name: GRB230209B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33310
SUBJECT: GRB 230209B: Fermi GBM Final Real-time Localization
DATE:    23/02/09 22:43:06 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 22:32:36 UT on 9 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230209B (trigger 697674761.889546 / 230209939).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 87.2, Dec = 23.5 (J2000 degrees, equivalent to J2000 05h 48m, 23d 30'), with a statistical uncertainty of 1.8 degrees.

The angle from the Fermi LAT boresight is 82.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230209939/quicklook/glg_skymap_all_bn230209939.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230209939/quicklook/glg_healpix_all_bn230209939.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230209939/quicklook/glg_lc_medres34_bn230209939.gif


GRB_name: GRB230209B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33311
SUBJECT: Fermi GRB 230209B: Global MASTER-Net observations report 
DATE:    23/02/09 23:30:19 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 230209B ( Fermi GBM team, GCN 33310) errorbox  78 sec after notice time and 112 sec after trigger time at 2023-02-09 22:34:29 UT, with upper limit up to  17.6 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -43.2 deg. 

The galactic latitude b = -2 deg., longitude l = 185 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2197905

We obtain a following upper limits.  

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

     123 | 2023-02-09 22:34:29 |         MASTER-SAAO | (05h 48m 38.85s , +23d 25m 41.1s) |   C |    20 | 17.3 |        
     123 | 2023-02-09 22:34:29 |         MASTER-SAAO | (05h 47m 42.98s , +23d 26m 01.2s) |   C |    20 | 16.6 |        
     167 | 2023-02-09 22:35:09 |         MASTER-SAAO | (05h 48m 43.58s , +23d 26m 01.0s) |   C |    30 | 17.5 |        
     167 | 2023-02-09 22:35:09 |         MASTER-SAAO | (05h 47m 47.64s , +23d 26m 21.7s) |   C |    30 | 16.9 |        
     233 | 2023-02-09 22:36:09 |         MASTER-SAAO | (05h 48m 41.95s , +23d 27m 14.2s) |   C |    40 | 17.6 |        
     233 | 2023-02-09 22:36:10 |         MASTER-SAAO | (05h 47m 46.01s , +23d 27m 36.0s) |   C |    40 | 17.0 |        
     298 | 2023-02-09 22:37:09 |         MASTER-SAAO | (05h 48m 42.43s , +23d 25m 55.7s) |   C |    50 | 17.6 |        
     298 | 2023-02-09 22:37:09 |         MASTER-SAAO | (05h 47m 46.50s , +23d 26m 18.0s) |   C |    50 | 17.0 |        
     389 | 2023-02-09 22:38:30 |         MASTER-SAAO | (05h 48m 45.87s , +23d 27m 28.8s) |   C |    70 | 17.5 |        
     389 | 2023-02-09 22:38:30 |         MASTER-SAAO | (05h 47m 49.96s , +23d 27m 51.9s) |   C |    70 | 16.9 |        
     649 | 2023-02-09 22:42:26 |         MASTER-SAAO | (05h 48m 40.23s , +23d 31m 32.5s) |   C |   120 | 17.1 |        
     649 | 2023-02-09 22:42:26 |         MASTER-SAAO | (05h 47m 43.59s , +23d 32m 07.7s) |   C |   120 | 16.5 |        
     810 | 2023-02-09 22:44:56 |         MASTER-SAAO | (05h 48m 36.07s , +23d 30m 39.6s) |   C |   140 | 16.9 |        
     810 | 2023-02-09 22:44:56 |         MASTER-SAAO | (05h 47m 39.45s , +23d 31m 15.3s) |   C |   140 | 16.2 |        
    1000 | 2023-02-09 22:47:47 |         MASTER-SAAO | (05h 48m 43.26s , +23d 30m 46.1s) |   C |   180 | 17.1 |        
    1000 | 2023-02-09 22:47:47 |         MASTER-SAAO | (05h 47m 46.69s , +23d 31m 22.6s) |   C |   180 | 16.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230210A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33312
SUBJECT: GRB 230210A: Fermi GBM Final Real-time Localization
DATE:    23/02/10 06:24:28 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:14:06 UT on 10 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230210A (trigger 697702451.965266 / 230210260).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 278.0, Dec = 73.0 (J2000 degrees, equivalent to J2000 18h 32m, 73d 00'), with a statistical uncertainty of 8.9 degrees.

The angle from the Fermi LAT boresight is 137.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230210260/quicklook/glg_skymap_all_bn230210260.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230210260/quicklook/glg_healpix_all_bn230210260.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230210260/quicklook/glg_lc_medres34_bn230210260.gif


GRB_name: GRB230209B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33315
SUBJECT: GRB 230209B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    23/02/11 00:37:33 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 230209B onboard (T0:
2023-02-09T22:32:36 UTC, Fermi/GBM GCN 33310, INTEGRAL trig 10198).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ,
941, 169), detects the burst with a sqrt(TS) of 42.1 in a 2.048 s
analysis time bin.
The burst duration as seen by BAT is ~60 s.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -53.
The NITRATES best fit OFOV position is consistent with the Fermi/GBM
localization (GCN 33310).

See Section 9.1 and Figures 10 and 17 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: GRB230211A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33316
SUBJECT: GRB 230211A: Fermi GBM Final Real-time Localization
DATE:    23/02/11 17:46:37 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 17:36:11 UT on 11 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230211A (trigger 697829776.865304 / 230211733).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 59.2, Dec = 51.7 (J2000 degrees, equivalent to J2000 03h 56m, 51d 42'), with a statistical uncertainty of 14.6 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/2023/bn230211733/quicklook/glg_skymap_all_bn230211733.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230211733/quicklook/glg_healpix_all_bn230211733.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230211733/quicklook/glg_lc_medres34_bn230211733.gif


GRB_name: GRB230211A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33317
SUBJECT: 230211A is not a GRB
DATE:    23/02/11 20:05:44 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

S. Poolakkil (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor
Team:

"The Fermi Gamma-ray Burst Monitor (GBM) trigger 697829776/230211733 at
17:36:11.87 UT
on 11 February 2023, tentatively classified as GRB 230211A (GCN 33316), is
in fact not due
to a GRB. This trigger is likely due to LS V +44 17 / RX J0440.9+4431."
-- 
Suraj Poolakkil
Fermi GBM Graduate Research Assistant
Dept. of Space Science
University of Alabama in Huntsville


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33321
SUBJECT: GRB 230204B: ATCA radio detection
DATE:    23/02/14 04:42:11 GMT
FROM:    Tara Murphy at U of Sydney  <tara.murphy@sydney.edu.au>

Ashna Gulati (U. Sydney, CSIRO), James Leung (U. Sydney, CSIRO), David Kaplan (UWM), Tara Murphy (U. Sydney)

We observed GRB 230204B (Serino et al., GCN 33265) with the Australia Telescope Compact Array (ATCA), on 2023 February 8 from 13:00 to 23:00 UT (3.6 days after the MAXI/GSC trigger) at 5.5, 9.0, 16.7, 21.2, 33.0 and 35.0 GHz. In our preliminary analysis, we detect the radio counterpart at 16.7 GHz at a position consistent with the GIT optical counterpart position (Swain et al., GCN 33269).

Radio emission has not been detected within 1â€™ of the GRB position in previous radio surveys: National Radio Astronomy Observatory VLA Sky Survey (NVSS; Condon et al., 1998), Sydney University Molonglo Sky Survey (SUMSS; Mauch et al., 2003), the Rapid ASKAP Continuum Survey (RACS; McConnell et al., 2020) or the Very Large Array Sky Survey (VLASS; Lacy et al., 2019). We measured a VLASS 5-sigma upper limit of 0.69 mJy at 3GHz.

We report the ATCA detection and 5-sigma upper limits below:

Freq (GHz) |  Flux Density (mJy)
â€”----------------------------------------
5.5              | <0.56
9.0              | <0.25
16.7            | 0.19 +/- 0.03
21.2            | <0.14
33.0            | <0.12
35.0            | <0.13

Further analysis of this data is ongoing.

We thank CSIRO staff for supporting these observations.

The Australia Telescope Compact Array is part of the Australia Telescope National Facility which is funded by the Australian Government for operation as a National Facility managed by CSIRO. We acknowledge the Gomeroi people as the traditional owners of the Observatory site.


GRB_name: GRB230204B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33322
SUBJECT: GRB 230204B: CALET Gamma-Ray Burst Monitor detection 
DATE:    23/02/14 06:18:39 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

Y. Asaoka (ICRR), A. Yoshida, T. Sakamoto, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 230204B (MAXI/GSC Detection: Serino et al., GCN Circ. 33265;
Swift/BAT-GUANO detection: Kennea et al., GCN Circ. 33267; AstroSat CZTI
detection: Waratkar et al., GCN Circ. 33268; AGILE detection: Casentini et al.,
GCN Circ. 33272; Detection by GRBAlpha: Dafcikova et al., GCN Circ. 33273;
Fermi-GBM Detection: Poolakkil et al., GCN Circ. 33288) triggered
the CALET Gamma-ray Burst Monitor (CGBM) at 21:44:25.20 UTC 
on February 4, 2023
(http://cgbm.calet.jp/cgbm_trigger/flight/1359582171/index.html).
The burst signal was seen by only the SGM detector.

The burst light curve shows a double-peaked structure that starts
at T+2.3 sec, peaks at T+54.1 sec and ends at T+65.0 sec.
The T90 and T50 durations measured by the SGM data are 59.5 +/- 0.9 sec
and 11.6 +/- 0.8 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1359582171/

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


GRB_name: GRB230209B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33323
SUBJECT: IPN triangulation of GRB 230209B
DATE:    23/02/14 13:25:05 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. Goldstein, M. S. Briggs, C. Wilson-Hodge,
and E. Burns on behalf of the Fermi GBM team,

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 on behalf of the GRS-Odyssey GRB team,
report:

The long-duration GRB 230209B
(Fermi-GBM detection: the Fermi GBM team, GCN Circ. 33310;
Swift/BAT-GUANO detection: Raman et al., GCN Circ. 33315)
was detected by Fermi (GBM trigger 697674761), Konus-Wind,
INTEGRAL (SPI-ACS), Swift (BAT), Mars-Odyssey (HEND),
and BepiColombo (MGNS) at about 81157 s UT (22:32:37).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    89.366 (05h 57m 28s) +29.199 (+29d 11' 57")
  Corners:
    89.445 (05h 57m 47s) +29.700 (+29d 41' 58")
    89.336 (05h 57m 21s) +30.139 (+30d 08' 22")
    89.289 (05h 57m 09s) +28.600 (+28d 35' 59")
    89.401 (05h 57m 36s) +27.754 (+27d 45' 15")
  ---------------------------------------------
The error box area is 674 sq. arcmin, and its maximum
dimension is 2.4 deg (the minimum one is 6.6 arcmin).
The Sun distance was 128 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB230209_T81161/IPN

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


GRB_name: GRB230209B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33324
SUBJECT: GRB 230209B: Fermi GBM Observation
DATE:    23/02/14 21:51:53 GMT
FROM:    Sarah Dalessi at UAH  <sd0104@uah.edu>

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

"At 22:32:36.89 UT on 09 February 2023, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 230209B (trigger 697674761 / 230209939)
which was also detected by the Swift/BAT-GUANO (G. Raman et al. 2023,
GCN 33315).
The Fermi GBM Final Real-time Localization (GCN #33310) is consistent with the
localization by the IPN network (Kozyrev et al. 2023, GCN 33323).

The angle from the Fermi LAT boresight at the GBM trigger time is 76 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 67 s (50-300 keV).
The time-averaged spectrum from T0-2.82 s to T0+68.87 s is best fit by
a Band function with Epeak = 183 +/- 6 keV,
alpha = -0.34 +/- 0.04, and beta = -2.44 +/- 0.09.

The event fluence (10-1000 keV) in this time interval is
(3.669 +/- 0.052)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.83 s in the 10-1000 keV band
is 16.4 +/- 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: GRB230209B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33325
SUBJECT: GRB 230209B: AGILE detection
DATE:    23/02/15 10:57:52 GMT
FROM:    Claudio Casentini at INAF-IAPS  <claudio.casentini@inaf.it>

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

The AGILE satellite detected the GRB 230209B at T0 = 2023-02-09 22:32:37 s
(UTC),
reported by Fermi/GBM (GCN #33310, GCN #33324), Swift/BAT (GCN #33315),
IPN network (GCN #33323) and Global MASTER-Net (GCN #33311).

The burst is clearly visible in the AGILE scientific ratemeters of the
MiniCALorimeter
(MCAL; 0.4-100 MeV) and in four out of five panels of the AntiCoincidence
system
(AC Top, 50-200 keV; AC Lat, 80-200 keV). The event lasted about 6.2 s and
it
released a total number of 4642 counts in the MCAL detector (above a
background rate
of 656 Hz), and 25551 counts in the AC Top detector (above a background
rate of
3547 Hz). The AGILE ratemeters light curves can be found at:
http://www.agilescienceapp.it/notices/GRB230209B_AGILE_RM_ND.png.

The event also triggered a high-time resolution MCAL data acquisition, from
T0-4 s
to T0+9 s (UTC), and released 2587 counts in the detector, above a
background rate
of 579.10 Hz. The MCAL light curve can be found at:
http://www.agilescienceapp.it/notices/GRB230209B_082193_603066757.789296.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: GRB230215A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33326
SUBJECT: GRB 230215A: Fermi GBM Final Real-time Localization
DATE:    23/02/15 14:51:43 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:41:18 UT on 15 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230215A (trigger 698164883.649682 / 230215612).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 353.0, Dec = -5.1 (J2000 degrees, equivalent to J2000 23h 32m, -5d 05'), with a statistical uncertainty of 10.1 degrees.

The angle from the Fermi LAT boresight is 73.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230215612/quicklook/glg_skymap_all_bn230215612.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230215612/quicklook/glg_healpix_all_bn230215612.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230215612/quicklook/glg_lc_medres34_bn230215612.gif


GRB_name: GRB230215A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33327
SUBJECT: Fermi GRB 230215A: Global MASTER-Net observations report 
DATE:    23/02/15 19:30:36 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 230215A ( Fermi GBM team, GCN 33326) errorbox  14520 sec after notice time and 14555 sec after trigger time at 2023-02-15 18:43:53 UT, with upper limit up to  16.7 mag. Observations started at twilight.  The observations began at zenith distance = 79 deg. The sun  altitude  is -15.6 deg. 

The galactic latitude b = -61 deg., longitude l = 80 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2199216

We obtain a following upper limits.  

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

   14585 | 2023-02-15 18:43:53 |         MASTER-SAAO | (00h 04m 31.32s , -13d 59m 38.8s) |   C |    60 | 16.1 |        
   14677 | 2023-02-15 18:45:25 |         MASTER-SAAO | (00h 11m 40.88s , -08d 17m 17.6s) |   C |    60 | 16.7 |        
   15025 | 2023-02-15 18:51:14 |         MASTER-SAAO | (00h 11m 48.89s , -10d 12m 52.2s) |   C |    60 | 16.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230216A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33328
SUBJECT: GRB 230216A: Swift detection of a burst
DATE:    23/02/16 15:05:20 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

N. J. Klingler (GSFC/UMBC/CRESSTII), P. A. Evans (U Leicester),
R. A. J. Eyles-Ferris (U Leicester), J.D. Gropp (PSU),
J. A. Kennea (PSU), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), B. Sbarufatti (INAF-OAB) and
M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 14:48:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230216A (trigger=1154815).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 113.966, -8.015 which is 
   RA(J2000) = 07h 35m 52s
   Dec(J2000) = -08d 00' 53"
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 ~700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 14:50:15.1 UT, 100.3 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 113.95924, -8.01160
which is equivalent to:
   RA(J2000)  = 07h 35m 50.22s
   Dec(J2000) = -08d 00' 41.8"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 27 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.17
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 105 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
0.197. 

The XRT position is 3.8" from the galaxy WISEA J073550.15-080045.2

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: GRB230216A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33329
SUBJECT: GRB 230216A: Zadko observatory - Gingin optical observations
DATE:    23/02/16 15:54:22 GMT
FROM:    Bruce Gendre at UVI  <bruce.gendre@gmail.com>

B. Gendre, E. Moore, F. Panther, D. Coward, J. A. Moore (OzGrav-UWA),
A. Klotz (IRAP-CNRS-OMP), and P. Thierry (AGORA), report:

We imaged the field of GRB 230216A detected by SWIFT (trigger 1154815,
Klingler et al. GCN #33328) with the Zadko robotic telescope (D=100cm)
located at the observatory - Gingin, Australia.

The observations started 164.1s after the GRB trigger
(130.9s after the notice). The elevation of the field decreased from
64 degrees above horizon and weather conditions
were good.

The field is crowded and the star USNO-B1 0819-0175793 lies within the XRT
error box of the possible counterpart, making the analysis complex.
However, on a serie of exposures taken between T0+164s and T0+3006s,
the PSF of USNO-B1 0819-0175793 increases toward the North axis before
returning to a value compatible with the other nearby stars.

We would tentatively conclude that the optical afterglow is located
behind that star.
The coordinates of the afterglow would then be
RA = 07h35m50.1s (J2000)
DEC = -08d00m42.5s (J2000)

At the moment it is impossible to estimate the magnitude of the
afterglow; the limiting
magnitude of the images is R ~ 19. Further observations are planned.

N.B. Galactic coordinates are lon=225.1876 lat= +6.0956
and the galactic extinction in R band is 0.0 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.
======================================================================


GRB_name: GRB230216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33330
SUBJECT: GRB 230216A: AKO Upper Limit
DATE:    23/02/16 17:17:11 GMT
FROM:    Mohammad Odeh at Al Khatim Observatory M44  <mshodeh@gmail.com>

Mohammad Odeh of Al-Khatim Observatory (AKO) operated by the International
Astronomical Center, in Abu Dhabi, UAE. 

 

As a follow up for the GRB 230216A detected by Swift (GCN 33328), we
observed the field of the GRB with our 0.35m f/7.7 robotic telescope. The
observation was done on 16 February 2023 from 16:39:17 to 16:51:39 (UT), 1.8
hours after the GRB trigger. We obtained multiple 180-sec exposures in Ic
filter. We did not detect any afterglow within XRT localization. Though, the
star USNO-B1 0819-0175793 lies within the XRT error box, which might hide a
possible afterglow. This is consistent with the report of (Gendre et al.,
GCN 33329).

 

The following upper limit was calculated using Atlas catalogue as a
reference:

----------------------------------------------------------------------------
-

JD (mid), T_mid-T0(hrs), Exposure (sec), Filter, Lim_mag

----------------------------------------------------------------------------
-

2459992.199329, 1.8, 3 x 180 (stacked), Ic, > 19.3

----------------------------------------------------------------------------
-

 

These magnitudes are not corrected for galactic extinction.

 


GRB_name: GRB230216A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33331
SUBJECT: GRB 230216A: Enhanced Swift-XRT position
DATE:    23/02/16 17:54:51 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 1108 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 230216A, 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 = 113.95906, -8.01133 which is equivalent
to:

RA (J2000): 07h 35m 50.17s
Dec (J2000): -08d 00' 40.8"

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

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

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


GRB_name: GRB230216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33332
SUBJECT: Swift GRB 230216A: Global MASTER-Net observations report 
DATE:    23/02/16 18:25:15 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov,  D.Cheryasov, Ya.Kechin
(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),

L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez 
(INAOE, Guillermo Haro Astrophysics Observatory),

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 230216A ( N. J. Klingler et al., GCN 33328) errorbox  12295 sec after notice time and 12332 sec after trigger time at 2023-02-16 18:14:07 UT, with upper limit up to  16.9 mag. Observations started at twilight.  The observations began at zenith distance = 40 deg. The sun  altitude  is -10.1 deg. 

The galactic latitude b =  7 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=2199464

We obtain a following upper limits.  

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

   12423 |         MASTER-SAAO |   C |   180 | 16.4 |        
   12423 |         MASTER-SAAO |   C |   180 | 16.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB230204B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33333
SUBJECT: GRB 230204B: Lowell Discovery Telescope Observations
DATE:    23/02/17 00:41:17 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD, GWU), E. Hammerstein (UMD), S.B. Cenko (UMD,
NASA-GSFC), E. Troja (UTV, ASU), S.Dichiara (PSU),
J. Durbak (UMD, NASA-GSFC), A. Kutyrev (UMD, NASA-GSFC),
S. Veilleux (UMD), I. Andreoni (UMD, NASA-GSFC), and
G. Srinivasaragavan (UMD):

We observed the field of GRB 230204B (Serino et al. GCN 33265;
Kennea et al. GCN 33267) using the Large Monolithic Imager (LMI)
on the 4.3m Lowell Discovery Telescope (LDT) at Happy Jack, AZ.
Observations began on February 13th, 2023 at 11:05:48 UT at
airmass 1.8 under seeing of ~2" with total exposure 2400 s
in i-band.

At the location of the optical counterpart (Swain et al. GCN 33269),
we do not detect any source to depth i>23.7 AB mag.

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

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


GRB_name: GRB230205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33334
SUBJECT: GRB 230205A: Lowell Discovery Telescope Observations
DATE:    23/02/17 00:43:14 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD, GWU), E. Hammerstein (UMD), S.B. Cenko (UMD,
NASA-GSFC), E. Troja (UTV, ASU), S.Dichiara (PSU),
J. Durbak (UMD, NASA-GSFC), A. Kutyrev (UMD, NASA-GSFC),
S. Veilleux (UMD), I. Andreoni (UMD, NASA-GSFC), and
G. Srinivasaragavan (UMD):

We observed the field of GRB 230205A (Ambrosi et al. GCN 33271;
Sakamoto et al. GCN 33280) using the Large Monolithic Imager (LMI)
on the 4.3m Lowell Discovery Telescope (LDT) at Happy Jack, AZ.
We began observations on February 13, 2023 at 12:54:52 UT in
r-band and i-band for 600 s each. The target was at airmass
1.1 with seeing ~2".

We do not detect any source within the XRT enhanced position
(Goad et al. GCN 33275) to depth r>23.8 AB mag. The host
galaxy candidate (Tomasella et al. GCN 33302), hereafter S1,
is clearly detected in both filters. We likewise detect
the source (S2) reported by Urata et al. (GCN 33307).

We measure the following magnitudes for S1 and S2:

S1: r ~ 22.0 +/- 0.1 AB mag
S1: i ~ 21.20 +/- 0.05 AB mag

S2: r ~ 23.7 +/- 0.3 AB mag
S2: i ~ 22.7 +/- 0.2 AB mag

The magnitudes of S1 are consistent with the earlier report
of Tomasella et al. (GCN 33302) and the SDSS catalog. For S2,
we derive a slightly fainter i-band magnitude compared to
Urata et al. (GCN 33307). However, as their images were obtained
prior to the explosion, this is not an indication of fading.
Thus, both these sources are candidate host galaxies to
GRB 230205A  (Schroeder et al. GCN 33309).

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

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


GRB_name: GRB230216A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33335
SUBJECT: GRB 230216A: Swift-XRT refined Analysis
DATE:    23/02/17 02:22:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

E. Ambrosi  (INAF-IASFPA) , M. Capalbi (INAF-IASFPA), S. Dichiara
(PSU), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M.
Perri (SSDC & INAF-OAR) and N.J. Klingler report on behalf of the
Swift-XRT team:

We have analysed 7.3 ks of XRT data for GRB 230216A (Klingler et al.
GCN Circ. 33328), from 84 s to 34.1 ks after the  BAT trigger. The data
comprise 8 s in Windowed Timing (WT) mode (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.
33331).

The late-time light curve (from T0+4.5 ks) can be modelled with a
power-law decay with a decay index of alpha=1.82 (+0.17, -0.15).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.00 (+0.19, -0.09). The
best-fitting absorption column is  consistent with the Galactic value
of 3.2 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.7 x 10^-11 (5.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+/-0.7) x 10^21 cm^-2
Galactic foreground: 3.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.00 (+0.19, -0.09)

If the light curve continues to decay with a power-law decay index of
1.82, the count rate at T+24 hours will be 1.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.7 x
10^-14 (8.6 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01154815.

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


GRB_name: GRB230216A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33336
SUBJECT: GRB 230216A: Swift-BAT refined analysis
DATE:    23/02/17 19:01:37 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

M. Stamatikos (OSU), 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),
T. Sakamoto (AGU), (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 230216A (trigger #1154815)
(Klingler, et al., GCN Circ. 33328).  The BAT ground-calculated position is
RA, Dec = 113.966, -7.993 deg which is
   RA(J2000)  =  07h 35m 51.9s
   Dec(J2000) = -07d 59' 36.2"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 85%.

The mask-weighted light curve shows a trio of peaks at approximately T-80 sec,
T-20 sec and T+0 sec, with some possible substructure and other, smaller
peaks. T90 (15-350 keV) is 91.20 +- 7.31 sec (estimated error including systematics).

The time-averaged spectrum from T-81.07 to T+16.40 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.90 +- 0.23.  The fluence in the 15-150 keV band is 1.3 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.13 sec in the 15-150 keV band
is 1.2 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1154815/BA/


Dr. Hans A. Krimm, Program Officer
Divisional of Astronomical Sciences
National Science Foundation
2415 Eisenhower Avenue, Room W9158
Alexandria, VA  22314
Tel: 703-292-2761


GRB_name: GRB230217A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33338
SUBJECT: GRB 230217A: Fermi GBM Final Real-time Localization
DATE:    23/02/17 22:04:27 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 21:53:10 UT on 17 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230217A (trigger 698363595.689472 / 230217912).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 278.8, Dec = -27.4 (J2000 degrees, equivalent to J2000 18h 35m, -27d 23'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 56.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230217912/quicklook/glg_skymap_all_bn230217912.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230217912/quicklook/glg_healpix_all_bn230217912.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230217912/quicklook/glg_lc_medres34_bn230217912.gif


GRB_name: GRB230217A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33339
SUBJECT: GRB 230217A: Swift detection of a short burst
DATE:    23/02/17 22:07:41 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

M. J. Moss (GWU), R. A. J. Eyles-Ferris (U Leicester),
J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB) and
M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 21:53:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 230217A (trigger=1154967).  Swift did not slew to the burst
due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 280.771, -28.856 which is 
   RA(J2000) = 18h 43m 05s
   Dec(J2000) = -28d 51' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single short
peak with a duration of about 1 sec.  The peak count rate
was ~15000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Moon observing constraint, Swift cannot slew to the BAT
position until 10:09 UT on 2023 February 18. There will thus be no 
XRT or UVOT data for this trigger before this time. 

Burst Advocate for this burst is M. J. Moss (mikejmoss3 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: GRB230216A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33340
SUBJECT: GRB 230216A: SVOM/C-GFT optical upper limit
DATE:    23/02/18 04:38:35 GMT
FROM:    Chao Wu at NAOC  <wuchao.lamost@gmail.com>

  Zhe Kang (CHO), Liping Xin (NAOC), Chao Wu (NAOC), Xuhui Han (NAOC),
 Xiaomeng Lu (NAOC),  Damien Turpin(CEA),  Zhenwei Li (CHO)ï¼ŒPinpin Zhang
(NAOC)ï¼ŒRuosong Zhang (NAOC)ï¼ŒYulei Qiu (NAOC)ï¼ŒYou  Lv (CHO)ï¼ŒJing Wang(GXU),
Cordier Bertrand (CEA)  and Jianyan Wei (NAOC) on behalf of SVOM GRB team

We observed the burst GRB230216A (Klingler et al. GCN Circ. 33328) on
14:50:01 UT, Feb. 16th, 2023, about  87 seconds after the Swift trigger
with C-GFT (Chinese Ground Follow-up Telescope in SVOM mission) in System
Test Mode (STM). C-GFT is located at Jilin (long.=126.33 deg, lat.=
43.8243778 deg), Changchun Observatory, National Astronomical
Observatories, CAS. It has FOV of 1.5 deg X 1.5 deg with a 4k*4k CMOS
detector mounted on the primary focus of  1.2-meter-aperure telescope.

A series of g and r band images were obtained. The exposure time was 10-30
seconds for each frame.

The bright star USNO-B1 0819-0175793 is located within the XRT enhanced
error box (Osborne et al., GCN 33331) which has been reported (Gendre et
al.,GCN 33329;  Mohammad Odeh GCN 33330). No optical afterglow was detected
with an image subtraction by the first r band image with an image obtained
43 minutes after.  A limit magnitude of 18.5 mag is derived for r-band
single frame (in STM) after calibration with nearby UCAC 4 catalogs.

More detailed analysis is continuing.

We thank the observation assistant Bowen Li at Jilin observatory for their
excellent support.

This message may be cited.


