# GCN_circulars

GRB_name: GRB221009A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32757
SUBJECT: GRB 221009A: VLA detection
DATE:    22/10/14 20:44:52 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (Utah), K. D. Alexander (Arizona), E. Ayache (Stockholm), E.
Berger (Harvard), R. Chornock (Berkeley), H. van Eerten (Bath), W. Fong
(Northwestern), R. Margutti (Berkeley), C.G. Mundell (Bath), and P. Schady
(Bath) report:

"We observed GRB 221009A (Dichiara et al. GCN 32632) with the Karl G.
Jansky Very Large Array (VLA) beginning on 2022 October 12 23:08 UTC at
multiple frequencies (3.5 d after the burst). In preliminary analysis, we
detect the radio counterpart (Trushkin et al., ATEL 15671; Bright et al.,
GCN 32653; Farah et al., GCN 32655; Rhodes et al., GCN 32700; Leung et al.,
GCN 32836; Laskar et al., GCN 32740) with a flux density of ~ 9.2 mJy at 11
GHz, and position:

RA (J2000) = 19:13:03.50
Dec (J2000) = 19:46:24.23

with a (statistical) uncertainty of 0.01" in each coordinate. This position
is consistent with the optical position (Dichiara et al., GCN 32632;
Lipunov et al., GCN 32634) and the radio position (Laskar et al., GCN
32740). Further observations are planned.

We thank the VLA staff for scheduling and executing these observations"


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32758
SUBJECT: GRB 221009A: Pan-STARRS optical photometry
DATE:    22/10/14 21:35:08 GMT
FROM:    Ken Smith at Queen's University Belfast  <k.w.smith@qub.ac.uk>

M. Huber, A. Schultz, K. C. Chambers (IfA, Hawaii), K. W. Smith,
M. Fulton, S. J. Smartt (QUB), T.-W. Chen (Stockholm), M. Nicholl
(Birmingham), D. R. Young, L. J. Shingles, S. Srivastav, S. Sim (QUB),
T. de Boer, J. Bulger, J. Fairlamb, C.-C. Lin, T. Lowe, E. Magnier,
R. J. Wainscoat, H. Gao (IfA), C. Stubbs (Harvard), A. Rest (STScI)

Daily imaging has been acquired (weather permitting) of the optical
counterpart of Swift J1913.1+1946 (Dichiara et al., GCN 32632;
Lipunov et al.,GCN 32634), the optical afterglow of GRB 221009A
(Kennea & Williams, GCN 32635; Veres et al., GCN 32636) with
Pan-STARRS2 since MJD 59863 (2022-10-11).  The following table
shows the most recent observations.

MJD          filter mag    dmag
59866.22756  r      20.92  0.05
59866.22504  i      19.88  0.02
59866.22371  z      19.21  0.02
59866.22239  y      18.77  0.03

We observed an initial fade of approximately 0.9 mags per day in
i, z and y, slowing to about 0.4 mags per day in these filters
over the last 2 days.


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32759
SUBJECT: GRB 221009A: Large Binocular Telescope Observatory optical afterglow detection
DATE:    22/10/15 00:09:35 GMT
FROM:    Manisha Shrestha at University of Arizona  <mshrestha1@arizona.edu>

GRB 221009A: Large Binocular Telescope Observatory optical afterglow detection



M. Shrestha (Univ. of Arizona),  D. Sand (Univ. of Arizona), K. D. Alexander (Univ. of Arizona), J. Andrews (Gemini), J. Pearson (Univ. of Arizona), N. Smith (Univ. of Arizona), K. Bostroem (Univ. of Arizona)  report on behalf of a wider collaboration:


We observed the field of Swift GRB 221009A (Dichiara et al. GCN 32632 ) with the Large Binocular Telescope Observatory, located in Mount Graham, Arizona, on 2022 October 12 starting at 02:40:10.027 UT (~2.5 days after the trigger) using the MODS instrument in imaging mode in the g, i and z bands.  Data were calibrated with respect to nearby PanSTARRS catalog stars.



We clearly detect the optical counterpart in the i and z bands and obtain an upper limit on the g band. The magnitudes are as follows:

g    > 23

i  = 19.00 +- 0.02 mag

z = 18.26 +- 0.01 mag



These values are not corrected for galactic extinction and are consistent with (Butler et al. GCN 32705, Bikmaev et al. GCN 32743) which were obtained in similar time.



We would like to thank A Cardwell and LBTO staff for obtaining the observations.


GRB_name: GRB221009A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32760
SUBJECT: GRB 221009A: Fermi LAT data rate effects due to extremely high flux
DATE:    22/10/15 07:21:01 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

N. Omodei (Stanford Univ.), P. Bruel (CNRS/IN2P3),
J. Bregeon (CNRS/IN2P3),  M. Pesce-Rollins (INFN Pisa),
D. Horan (CNRS/IN2P3),  E. Bissaldi (Politecnico and INFN Bari),
and R. Pillera (Politecnico and INFN Bari)
report on behalf of the Fermi-LAT team:


We report updated observations of GRB 221009A which was detected by
Swift (Kennea et al. GCN #32635), Fermi-GBM (Veres et al. GCN #32636,
Lesage et al. GCN #32642), Fermi-LAT (Bissaldi et al. GCN #32637,
Pillera et al. #32658), and the IPN (Svinkin et al. GCN #32641).

GRB 221009A triggered Fermi-GBM on October 9, 2022, at 13:16:59.99 UT
(T0, trigger 687014224/221009553).

During some time periods of the main emission episode of GRB 221009A
as seen in GBM, the LAT gamma-ray flux was so high that
more than one photon was recorded at the same time,
which strongly affected event reconstruction.
We are currently investigating the consequences of such a pile-up but,
until further notice, we discourage the use of LAT data in the time
intervals T0+225 to T0+236 seconds and T0+257 to T0+265 seconds
with respect to the GBM trigger time.

The photon with 99 GeV observed 240 seconds
after the GBM trigger is not affected by thesedata rate effects.

The Fermi-LAT point of contact for this burst is
Elisabetta Bissaldi (elisabetta.bissaldi@ba.infn.it).

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


GRB_name: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32761
SUBJECT: GRB 221009A: ALMA and ACA detections
DATE:    22/10/15 10:52:14 GMT
FROM:    Kuiyun Huang at CYCU  <kuiyun@gmail.com>

Y. Urata, K.Y. Huang, S. Covino, K. Wiersema, K. Asada, H. Nagai,S.
Takahashi, K. Yamaoka, M. Tashiro, K.Toma, J. Shimoda, A. Kuwata and J.
Shimoda

We observed the field of GRB 221009A (Dichiara GCN 32632) with ALMAand ACA
at 97.5, 145, and 203 GHz.  The afterglow is significantly detected at all
bands, and the flux at 97.5 GHz was ~7 mJy at 4.3 days after the burst.
Together with the SMA measurements at the
similar epoch (Rhodes et al. GCN 32707), the spectrum seems to be flat
around the mm/submm band.

We thank ALMA staff for rapidly scheduling and supporting these
observations.


GRB_name: GRB221009A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32762
SUBJECT: GRB 221009A: Armchair Energetics
DATE:    22/10/15 13:52:06 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (Goethe Univ.) and J. F. Agui Fernandez (IAA) report:

The ultra-bright, nearby (de Ugarte Postigo et al., GCN #32648) GRB 
221009A (Swift (afterglow) discovery: Dichiara et al., GCN #32632) was 
so intense, it saturated multiple sensitive satellite detectors that 
registered the prompt emission (Fermi GBM: Veres et al., GCN #32636, 
Lesage et al., GCN #32642; Konus-Wind: Frederiks et al., GCN #32668; 
Fermi LAT: Omodei et al. GCN #32760; Agile/MCAL: Ursi et al. GCN #32650; 
INTEGRAL SPI/ACS, Gotz et al., GCN #32660; Insight-HXMT, Tan et al., 
ATel #15660).

Some missions detected GRB 221009A without saturation effects, because 
they are either smaller and less sensitive (GRBAlpha: Ripa et al., GCN 
#32685; SIRI-2: Mitchell et al., GCN #32746) or the burst was off-axis 
and passed through the spacecraft body (SRG ART-XC, Lapshov et al., GCN 
#32663). An especially interesting detection was made by HEBS (Liu et 
al., GCN #32751), which was also not saturated owing to its orbital 
position and environment.

Konus-Wind determined the energetics and spectrum of the first ("onset") 
pulse of the main emission episode (unsaturated, preceding the two 
brightest pulses), from T_0+180 - 200 s, finding a fluence of 8.8E-04 
erg cm^-2 (even this episode alone would be one of the brightest GRBs 
ever detected) and a peak energy of ~1 MeV. Using this spectrum and the 
raw, preliminarily corrected count rates of the other episodes, they 
determined a total fluence of 5.2E-02 erg cm^-2 (Frederiks et al., GCN 
#32668).

We take the count-rate light curve linked in the Konus-Wind GCN and 
determine the counts of the "onset" pulse, thereby determining a 
"fluence per count" conversion. With this value, and assuming the third 
episode of the GRB (from 380 to 610 s) is unsaturated (or corrected 
successfully) and has the same spectrum, we find a fluence of 1.28E-02 
erg cm^-2 for this episode. This is probably an overestimate, as the 
final episode of the GRB is likely softer (see the similar GRB 160625B, 
e.g., B.-B. Zhang et al. 2018, Nature Astronomy, 2, 69). For the HEBS 
data, we derive a significantly lower fluence of ~3E-03 erg cm^-2. A 
potential explanation is that the high background during the time of the 
GRB led to the softer bands being discarded, losing a lot of counts for 
the softer episode.

For the main episode (200 - 300 s), we derive a fluence of 7.65E-02 erg 
cm^-2 from the HEBS light curve, a value somewhat higher than the one 
derived for the entire burst from Konus-Wind. Again, this is dependent 
on the spectrum being the same as during the "onset" pulse. If it is 
even harder, the fluence would increase correspondingly.

Summing all together (the precursor is negligible), we derive, in a 
broad bolometric band from 0.1 keV to 100 MeV (see Agui Fernandez et 
al., 2021, MNRAS, submitted, arXiv:2109.13838), an isotropic energy 
release of log E_iso = 54.77, a value in perfect agreement with GRB 
160625B in the same band. This places GRB 221009A within the very 
highest isotropic energy releases measured so far. On the one hand, this 
implies the GRB is extreme but not an outlier, whereas, on the other 
hand, combined with the very low distance, it makes it an even rarer 
event.


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32763
SUBJECT: GRB 221009A: ATCA detection
DATE:    22/10/15 15:37:33 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

S. Bhandari (ASTRON/JIVE), T. Laskar (Utah), K. D. Alexander (Arizona), E.
Berger (Harvard), R. Chornock (Berkeley), D. Coppejans (Warwick), M. Drout
(Toronto), H. van Eerten (Bath), W. Fong (Northwestern), C. Guidorzi
(Ferrara), R. Margutti (Berkeley), C.G. Mundell (Bath), P. Schady (Bath)
and G. Schroeder (Northwestern) report:

"ATCA observed GRB 221009A (Dichiara et al. GCN 32632) beginning on 2022
October 15 05:00 UTC (5.7 d after the burst) at multiple frequencies. In a
preliminary analysis, we detect the radio counterpart (Trushkin et al.,
ATEL 15671; Bright et al., GCN 32653; Farah et al., GCN 32655; de Ugarte
Postigo et al., GCN 32676; Rhodes et al., GCN 32700; Rhodes et al., GCN
32707; Leung et al., GCN 32836; Laskar et al., GCN 32740; Laskar et al.,
GCN 32757; Urata et al., GCN 32761) with a flux density of ~ 6.8 mJy at
16.7 GHz at a position consistent with the optical position (Dichiara et
al., GCN 32632; Lipunov et al., GCN 32634) and the radio position (Laskar
et al., GCN 32740, Laskar et al., GCN 32757). Further observations are
planned.

We thank the CSIRO staff for approving and carrying out 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: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32765
SUBJECT: GRB 221009A: VLT spectroscopic detection of the host galaxy
DATE:    22/10/15 16:56:06 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

L. Izzo (DARK/NBI), A. Saccardi (GEPI, Observatoire de Paris), J. P. U. 
Fynbo (DAWN/NBI), J. Palmerio (GEPI, Paris obs.), D. B. Malesani 
(Radboud Univ. and DAWN/NBI), J. F. Agui Fernandez (IAA/CSIC), D. A. 
Kann (Goethe Univ.), A. Melandri (INAF/OAR), S. D. Vergani (GEPI, Paris 
obs.), K. Wiersema (Lancaster univ.), report on behalf of the Stargate 
consortium:

We observed the optical counterpart of GRB 221009A (Dichiara et al., GCN 
32632; Veres et al., GCN 32636; and very many other GRB satellites) 
using the ESO VLT UT3 (Melipal) equipped with the X-shooter 
spectrograph. A 40-min spectrum was secured covering the wavelength 
range 3000-25000 AA, with a mean time 2022 October 14.02 UT (4.46 days 
after the Fermi/GBM trigger).

 From the acquisition image, we measure for the optical counterpart a 
magnitude i = 19.89 +- 0.05 (AB; calibrated against Pan-STARRS), 4.45 
days after the Fermi/GBM trigger.

The continuum is still dominated by the afterglow. However, narrow 
emission lines can be seen from the host galaxy. We identify H alpha in 
the optical and Pa alpha in the near-infrared, at redshift z = 0.151, 
consistent with the one measured from the afterglow absorption features 
(de Ugarte Postigo et al., GCN 32648).

The H alpha FWHM is about 110 km s^-1. From the H alpha flux, corrected 
for Galactic extinction (A_V = 4.2 mag), we infer a SFR > 0.25 M_Sun 
yr^-1 (this value is a lower limit due to unaccounted host extinction 
and slit losses).

We acknowledge expert support from the ESO observing staff in Paranal, 
in particular Zahed Wahhaj and Matias Jones.


GRB_name: GRB221009A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32766
SUBJECT: GRB 221009A: ATCA radio spectrum
DATE:    22/10/15 23:15:43 GMT
FROM:    James Leung at U of Sydney/VAST  <jleu9465@uni.sydney.edu.au>

James Leung (University of Sydney/CSIRO), Tara Murphy (University of 
Sydney), Emil Lenc (CSIRO), Gemma Anderson (Curtin)

We report the radio spectrum for the Australia Compact Telescope Array 
(ATCA) observations (Bhandari et al., GCN 32763) taken on 2022 October
15 from 05:00 to 11:30 UTC (5.6 to 5.9d after the Swift/BAT trigger).

ATCA observed at 16.7, 21.2, 33, 35, 45 and 47 GHz. In our preliminary
analysis, we detect the radio counterpart at each frequency (Trushkin 
et al., ATel 15671; Bright et al., GCN 32653; Farah et al., GCN 32655; 
de Ugarte Postigo et al., GCN 32676; Rhodes et al., GCN 32700; Leung
et al., GCN 32836; Laskar et al., GCN 32740; Laskar et al., GCN 32757;
Urata et al., GCN 32761; Bhandari et al., GCN 32763) at a position 
consistent with the Swift/UVOT position (Dichiara et al., GCN 32632). 

The preliminary flux density measurements are reported below, with 
uncertainties being purely statistical:

7.1 +/- 0.1 mJy/beam at 16.7 GHz
6.1 +/- 0.1 mJy/beam at 21.2 GHz
4.8 +/- 0.1 mJy/beam at 33 GHz
4.4 +/- 0.1 mJy/beam at 35 GHz
3.6 +/- 0.2 mJy/beam at 45 GHz
3.5 +/- 0.2 mJy/beam at 47 GHz

Ongoing observations are planned. 

We thank CSIRO staff for rapidly scheduling, supporting and executing
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: GRB221009A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32767
SUBJECT: GRB 221009A: LEIA X-ray Afterglow Detection
DATE:    22/10/16 02:21:05 GMT
FROM:    LEIA Team at NAOC/CAS  <ep_ta@bao.ac.cn>

Y. Liu, C. Zhang, Z.X. Ling, H.Q. Cheng, C.Z. Cui, D.W. Fan, H.B. Hu,

M.H. Huang, C.C. Jin, D.Y. Li, H.Y. Liu, H. Sun, H.W. Pan, W.X. Wang,

Y.F. Xu, M. Zhang, W.D. Zhang, D.H. Zhao, and W. Yuan (NAOC, CAS),

report on behalf of the LEIA and Einstein Probe team:

 

LEIA (Lobster Eye Imager for Astronomy) has performed one

follow-up observation of GRB 221009A detected by Swift/BAT

(Dichiara et al., GCN 32632, Kennea et al., GCN 32635), Fermi-GBM

(Lesage et al., GCN 32642, Veres et al., GCN 32636), Fermi-LAT

(Bissaldi et al. GCN 32637, Pillera et al., GCN 32658), AGILE-MCAL

(Ursi et al., GCN 32650), AGILE-GRID (Piano et al. GCN 32657),

INTEGRAL SPI/ACS (Gotz et al., GCN 32660), Konus-Wind

(Frederiks et al., GCN 32668), HEBS (Liu et al., GCN 32751), at a 

redshift of z = 0.151 (de Ugarte Postigo et al., GCN 32648; 

Castro-Tirado et al., GCN 32686).

 

The pointed observation was conducted from 2022-10-12T05:31:48

to 2022-10-12T05:51:39 with a net exposure of 1012 s. The X-ray

afterglow of GRB 221009A is detected at a significance of 4.9 sigma.

Assuming an absorbed power-law model with a photon index of 2.0,

a Galactic absorption of 5.4 x 10^21 cm^-2 (Willingale et al. 2013;

GCN #32651), and an intrinsic absorption of 1.1 x 10^22 cm^-2 at a

redshift of 0.151 (GCN #32648), the unabsorbed flux in the 0.5 - 4.0 keV

band is (1.8+/-0.4) x 10^-10 ergs/cm^2/s.

 

LEIA (Zhang et al, ApJL submitted) is a soft X-ray monitor (0.5 - 4.0 keV)

with a FoV of 340 square degrees aboard the SATech-01 satellite of the CAS,

launched on July 27, 2022. The above result is preliminary and the final

result will be published elsewhere.


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32769
SUBJECT: GRB 221009A: continued Assy optical afterglow observations, possible SN evidence
DATE:    22/10/16 15:33:29 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI, HSE), V. Kim (FAI), A. Pozanenko (IKI),  M. Krugov 
(FAI), Y. Aimuratov (FAI), N. Pankov (HSE) report on behalf of GRB IKI FuN:

We continue observations of GRB 221009A (Swift J1913.1+1946) (Dichiara 
et al., GCN 32632; Kennea and Williams, GCN  32635; Veres et al., GCN 
32636; Bissaldi et al., GCN  32636; Svinkin et al., GCN 32641; Piano et 
al., GCN 32657; Pillera et al., GCN 32658;  Gotz et al., GCN 32660; 
Frederiks et al., GCN 32668)  with AZT-20 telescope of Assy-Turgen 
observatory.  The observations were carried out  on 2022-10-11 -- 
2022-10-15. The optical afterglow ( GCNs 32632,  32635, 32636, 32641, 
32657, 32658, 32660, 32666, 32668, 32670, 32671, 32676, 32677, 32678, 
32679, 32680, 32683, 32684, 32685, 32686, 32691, 32692, 32693, 32694, 
32695, 32700, 32705, 32707, 32709, 32727, 32729, 32730, 32736, 32738, 
32739, 32740, 32743, 32746, 32749, 32750; 32752; 32753; 32755; 32758; 
32765).

Preliminary photometry of the afterglow on 2022-10-15 is following

Date       UT start  t-T0       Exp.   Filter  OT    Err.   UL(3sigma)
                     (mid, days)  (s)
2022-10-15 15:29:43  6,10259    30*60  g'      22.60  0.12  23.4
2022-10-15 14:25:00  6,05765    30*60  r'      20.96  0.05  22.9
2022-10-15 14:56:19  6,07939    30*60  i'      20.00  0.04  23.2 
2022-10-15 16:01:07  6,11918    15*60  z'      19.31  0.08  21.0
The photometry is based on the nearby PS1 stars.

The light curve based in our photometry can be found in 
http://grb.rssi.ru/GRB221009A/GRB221009A_lc_cc_7_cut.png

The power law (PL) fit parameters are also shown in the figure and do 
not include photometry on 2022-10-15. It can be seen that the color 
change g-i and photometry g, r on October 15, 2022 deviate significantly 
from the PL approximation. We hypothesize that this behaviour may 
indicate a supernova rise.


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32771
SUBJECT: GRB 221009A: Faulkes Telescope North continued optical afterglow follow-up 
DATE:    22/10/16 21:35:11 GMT
FROM:    Manisha Shrestha at University of Arizona  <mshrestha1@arizona.edu>

M. Shrestha (Univ. of Arizona), K. Bostroem (Univ. of Arizona),  D. Sand (Univ. of Arizona), K. D. Alexander (Univ. of Arizona), J. Andrews (Gemini), J. Pearson (Univ. of Arizona), G. Hosseinzadeh (Univ. of Arizona), N. Smith (Univ. of Arizona), D. A. Howell (LCO/UCSB), C. McCully (LCO/UCSB), M. Newsome (LCO/UCSB), E Padilla Gonzalez (LCO/UCSB), C. Pellegrino (LCO/UCSB), G. Terreran (LCO/UCSB), J. Farah (LCO/UCSB) report on behalf of a wider Global Supernova Project collaboration:



We observed the field of Swift GRB 221009A (Dichiara et al. GCN 32632 ) with Faulkes Telescope North, on 2022 October 15 starting at 6:34:12.198 UT (~5.7 days after the trigger) using the MuSCAT3 imager in the r, i, and z bands.  Data were calibrated with respect to nearby PanSTARRS sources for r, i, and z bands .



We clearly detect the optical counterpart in the r, i and z bands and obtain an upper limit on the g band. The magnitudes are as follows:



r  = 21.13 +- 0.06

i  = 20.01 +- 0.05

z = 19.39 +- 0.05



These values are not corrected for galactic extinction and are consistent with the magnitudes reported in Belkin et al. GCN 32769 observed in a similar time frame.


GRB_name: GRB221016A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32773
SUBJECT: GRB 221016A: Fermi GBM Final Real-time Localization
DATE:    22/10/16 23:50:37 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 23:39:22 UT on 16 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221016A (trigger 687656367.709164 / 221016986).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 37.6, Dec = -32.1 (J2000 degrees, equivalent to J2000 02h 30m, -32d 06'), with a statistical uncertainty of 2.2 degrees.

The angle from the Fermi LAT boresight is 98.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221016986/quicklook/glg_skymap_all_bn221016986.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/bn221016986/quicklook/glg_healpix_all_bn221016986.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221016986/quicklook/glg_lc_medres34_bn221016986.gif


GRB_name: GRB221016A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32774
SUBJECT: GRB 221016A: Swift detection of a burst
DATE:    22/10/16 23:53:22 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), J. A. Kennea (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), A. Y. Lien (U Tampa),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
A. Tohuvavohu (U Toronto) and M. A. Williams (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 23:39:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221016A (trigger=1129775).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 38.949, -34.624 which is 
   RA(J2000) = 02h 35m 48s
   Dec(J2000) = -34d 37' 26"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with tail structure with a duration of about 30 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 23:42:24.0 UT, 179.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 38.94479, -34.61039 which is equivalent
to:
   RA(J2000)  = 02h 35m 46.75s
   Dec(J2000) = -34d 36' 37.4"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 50 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.53 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.8
(+3.14/-2.70) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 97 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 0.026. 

Burst Advocate for this burst is K. L. Page (kimlpage1978 AT gmail.com). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB221016A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32775
SUBJECT: GRB 221016A: LCOGT Optical Afterglow Detection
DATE:    22/10/17 03:23:46 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 221016A (Page et al., GCN 32774) field with the LCOGT
1-meter Sinistro instrument at the Cerro Tololo Interamerican Observatory,
Chile site, on October 17, from 01:39 to 02:06 (corresponding to 2.00 to
2.55 hours from the GRB trigger time) with the Bessel I and R filters.

We performed a series of 3x300s exposures in each band.  We detect an
uncataloged optical source within the XRT error region (Page et al., GCN
32774), in R band, and marginally in I-band (2-sigma detection).

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

R = 21.22 +/- 0.18
I = 20.03 +/- 0.17

These magnitudes are not corrected for galactic extinction.  Gemini
imaging+spectroscopic follow up is ongoing.


GRB_name: GRB221016A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32776
SUBJECT: GRB 221016A: Enhanced Swift-XRT position
DATE:    22/10/17 04:07:07 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 165 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 221016A, 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 = 38.94459, -34.61073 which is equivalent
to:

RA (J2000): 02h 35m 46.70s
Dec (J2000): -34d 36' 38.6"

with an uncertainty of 2.4 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB221017A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32777
SUBJECT: GRB 221017A: MAXI/GSC detection
DATE:    22/10/17 07:16:28 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

S. Nawa(Chuo U.), M. Serino(AGU), 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, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, J. Kohara, S. Urabe, 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 (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 2022-10-17T05:39:31 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (116.859 deg, 39.409 deg) = (07 47 26, +39 24 32) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.45 deg and 0.4 deg, respectively.
The roll angle of long axis from the north direction is 83.0 deg counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 109 +- 30 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (115.407, 38.740) deg = (07 41 37, +38 44 24) (J2000)
(R.A., Dec) = (116.206, 38.225) deg = (07 44 49, +38 13 30) (J2000)
(R.A., Dec) = (118.217, 40.060) deg = (07 52 52, +40 03 36) (J2000)
(R.A., Dec) = (117.412, 40.589) deg = (07 49 38, +40 35 20) (J2000)
There was no significant excess flux in the previous transit at 10/17 04:06 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB221016A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32778
SUBJECT: GRB 221016A: z-band upper limit, possible afterglow brightening
DATE:    22/10/17 08:56:18 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Radboud Univ. and DAWN/NBI), D. A. Kann (Goethe Univ.), 
L. Izzo (DARK/NBI), S. Covino, P. D'Avanzo (INAF/OAB), N. R. Tanvir 
(Univ. Leicester), report on behalf of the Stargate consortium:

We observed the field of GRB 221016A (Page et al., GCN 32774) with the 
ESO VLT UT3 (Melipal), using the acquisition camera of the X-shooter 
spectrograph. A single 30 s image is available to us, taken on 2022 Oct 
17.034 UT (1.17 hr after the trigger). The image seeing was rather poor, 
about 2.2".

No source is detected at the position of the optical counterpart 
discovered by Strausbaugh & Cucchiara (GCN 32775), down to a 3-sigma 
limit z > 20.8 (AB; calibrated against one nearby SkyMapper star). 
Comparison between our limit and the magnitudes reported by Strausbaugh 
& Cucchiara (GCN 32775) seems to indicate a brightening of the afterglow 
between ~1 and ~2 hr after the trigger.

We acknowledge the ESO staff for a quick reaction to our request, in 
particular Matias Jones and Felipe Gaete.


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32780
SUBJECT: GRB 221009A: A type I BdHN of exceptional energetics
DATE:    22/10/17 11:16:22 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.
Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:


GRB221009A detected by Swift (Kennea et al. 2022 GCN32635), Fermi-GBM
(Veres et al. 2022, GCN32636, Lesage et al. 2022, GCN32642), Fermi-LAT
(Bissaldi et al. 2022, GCN32637), with redshift of z=0.151 and an isotropic
equivalent energy of Eiso=2x10^54 erg (de Ugarte Postigo et al. 2022,
GCN32648 and GCN32642) is a typical Binary driven Hypernova of type I
(BdHNI), originating from the collapse of a carbon-oxygen core (CO-core) in
presence of a companion neutron star (NS) with common feature with three
BdHNeI: GRB130427A with "pile up" in the prompt phase (Ruffini et al. 2013,
GCN14526); GRB190114C (Ruffini et al. 2019, GCN23715); and GRB180720B
(Ruffini et al. 2018, GCN23019). As the above three sources, GRB221009A
presents: 1) the optical (Lipunov et al. 2022, GCN32634 and GCN32639;
Perley. 2022 GCN32638; Broens. 2022, GCN32640; Hu et al. 2022, GCN32644;
Mondy: Belkin et al. 2022, GCN32645; de Wet et al.2022, GCN32646; Xu et al.
2022 GCN32647; Odeh 2022, GCN32649; Brivio et al. 2022, GCN32652; Izzo et
al. 2022, GCN32765), radio (Bright et al. 2022, GCN32653 and Farah et al.
2022, GCN32655) and X-ray (Kennea et al, 2022, GCN32635, and GCN32651)
synchrotron afterglow emissions as well as the TeV emission (Yong Huang et
al. 2022, GCN32677), which in BdHNI originate from accreting millisecond
spinning newborn NS (Rueda et al. 2022, e-Print: 2204.00579 [astro-ph.HE]);
2) the ultra-relativistic prompt emission (UPE) phase (Moradi et al. 2021,
PRD 104, 063043 and Rastegarnia et al. 2022, EPJC 82, 778) and GeV emission
(Rueda et al 2022 ApJ 929 56) originated from the black hole formed by
hypercritical accretion of the supernova ejecta on the NS companion; and 3)
the optical emission of the nickel decay of the supernova (SN), created by
the collapse of the CO-core. The first evidence of the supernova rise is
reported by S. Belkin et al. 2022, (GCN32769). In this GRB the bolometric
optical peak of SN is expected to be observed at 15.57+/-2.0 days after the
Fermi-GBM trigger (October 24th 2022, uncertainty from October 22nd 2022 to
October 26th 2022, with the bolometric optical luminosity of
L=(9.45+/-2.8)x10^42 erg/s; Aimuratov et al. in preparation).


GRB_name: GRB220926B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32781
SUBJECT: GRB 220926B: Detection by GRBAlpha
DATE:    22/10/17 13:39:57 GMT
FROM:    Jakub Ripa at Masaryk University  <245487@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), F. Munz, N. Husarikova, J.-P. Breuer, M. 
Topinka, 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 220926B (INTEGRAL IBIS/ISGRI detection: Gotz et 
al., GCN 32586) was detected by the GRBAlpha 1U CubeSat (Pal et al. 
Proc. SPIE 2020).

The subthreshold 4.7 sigma detection was confirmed at the peak time 
2022-09-26 10:38:21.2 UTC. The light curve obtained by GRBAlpha is 
temporally consistent with the light curve obtained by INTEGRAL 
IBIS/ISGRI. The GOES X-ray flux does not show any excess, so we exclude 
this detection being a solar flare. Therefore, this event is consistent 
with being a GRB with a duration, as measured by GRBAlpha, of ~8 s.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB220926B_GCN.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a 
future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its 
detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously 
upgrading the on-board data acquisition software stack. 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: GRB221016A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32782
SUBJECT: GRB 221016A: Fermi GBM observation
DATE:    22/10/17 13:58:45 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico and INFN Bari), P. Veres (UAH)
and C. Meegan (UAH) report on behalf of the Fermi GBM Team:


"At 23:39:22.71 UT on 16 October 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221016A (trigger 687656367/221016986),
which was also detected by the Swift/BAT (Page et al. GCN 32774).
The Fermi GBM Final Real-time Localization (GCN 32773)
is consistent with the Swift position.

The angle from the Fermi LAT boresight
at the GBM trigger time is 98 degrees.

The GBM light curve shows a single emission episode
with a duration (T90) of about 13 s (50-300 keV).
The time-averaged spectrum from T0-1.2 s to T0+11 s is
best fit by a Band function with Epeak = 119 +/- 12 keV,
alpha = -0.51 +/- 0.12, and beta = -2.11 +/- 0.11.

The event fluence (10-1000 keV) in this time interval is
(6.3 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.8 s in the 10-1000 keV band
is 7.4 +/- 0.3 ph/s/cm^2.


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

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


GRB_name: GRB221016A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32783
SUBJECT: Konus-Wind detection of GRB 221016A
DATE:    22/10/17 14:06:18 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The long-duration GRB 221016A
(Fermi-GBM detection: Fermi GBM team, GCN#32773,
Bissaldi et al., GCN#32782;
Swift-BAT detection: Page et al., GCN#32774)
triggered Konus-Wind at T0=85166.713 s UT (23:39:26.713).

The burst light curve shows a single emission pulse
which starts at ~T0-1.7 s and has a total duration of ~12.5 s.
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB221016_T85166/

As observed by Konus-Wind, the burst
had a fluence of 5.46(-0.74,+1.07)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.800 s,
of 1.87(-0.73,+0.74)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.02(-0.33,+0.40)
and Ep = 207(-46,+98) keV (chi2 = 60/99 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 = 60/98 dof).

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model
with  alpha = -0.89(-0.30,+0.35)
and Ep = 166(-26,+39) keV (chi2 = 81/96 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 81/95 dof).

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


GRB_name: GRB221016A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32784
SUBJECT: GRB 221016A: Swift-XRT refined Analysis
DATE:    22/10/17 15:15:27 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.2 ks of XRT data for GRB 221016A (Page et al. GCN
Circ. 32774), from 76 s to 44.8 ks after the  BAT trigger. The data
comprise 83 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. 32776).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.20 (+0.22, -0.18), followed by a break at T+254 s to
an alpha of 0.78 (+0.04, -0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.49 (+0.23, -0.21). The
best-fitting absorption column is  7.9 (+4.2, -3.7) x 10^20 cm^-2, in
excess of the Galactic value of 3.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.04 (+0.20, -0.19)
and a best-fitting absorption column of 1.5 (+0.6, -0.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (4.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.5 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 3.5 x 10^20 cm^-2
Excess significance: 3.5 sigma
Photon index:      2.04 (+0.20, -0.19)

If the light curve continues to decay with a power-law decay index of
0.78, the count rate at T+24 hours will be 0.019 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.1 x
10^-13 (8.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01129775.

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


GRB_name: GRB221016A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32785
SUBJECT: GRB 221016A: Swift/UVOT Detection
DATE:    22/10/17 20:13:01 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 221016A
97 s after the BAT trigger (Page et al., GCN Circ. 32774).
A source consistent with the enhanced XRT position (Goad et al. GCN Circ. 32776)
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               97          247          147         20.20 +/- 0.23
b                 3736         3861          123        >19.8
u                  309          349           39        >18.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.026 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221016A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32786
SUBJECT: GRB 221016A: Swift-BAT refined analysis
DATE:    22/10/17 20:42:14 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

S. Laha (GSFC/UMBC), S. D. Barthelmy (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-239 to T+200 sec from the recent telemetry downlink,

we report further analysis of BAT GRB 221016A (trigger #1129775)

(Page, et al., GCN Circ. 32774).  The BAT ground-calculated position is

RA, Dec = 38.938, -34.615 deg which is 

   RA(J2000)  =  02h 35m 45.2s 

   Dec(J2000) = -34d 36' 54.2" 

with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).

The partial coding was 53%.

 

The light curve shows a single peaked pulse. T90 (15-350 keV) is 21.86 +- 5.70 sec 

(estimated error including systematics).

 

The time-averaged spectrum from T-3.18 to T+29.18 sec is best fit by a simple

power-law model.  The power law index of the time-averaged spectrum is

1.28 +- 0.08.  The fluence in the 15-150 keV band is 2.3 +- 0.1 x 10^-06 erg/cm2.

The 1-sec peak photon flux measured from T+0.03 sec in the 15-150 keV band

is 3.4 +- 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/1129775/BA/

 

 

 

 

 


GRB_name: GRB221017A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32787
SUBJECT: IPN triangulation of GRB 221017A (long)
DATE:    22/10/17 20:49:59 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

A. Ridnaia, D. Frederiks, D. Svinkin, A. Lysenko,
and T. Cline on behalf of the Konus-Wind 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 long-duration GRB 221017A
(MAXI/GSC detection: Nawa et al., GCN 32777)
has been detected by MAXI (GSC), INTEGRAL (SPI-ACS), Konus-Wind,
and Mars-Odyssey (HEND), so far, at about 19789 s UT (05:29:49).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  116.901 (07h 47m 36s) +39.742 (+39d 44' 32")
 Corners:
  116.215 (07h 44m 52s) +41.438 (+41d 26' 15")
  117.708 (07h 50m 50s) +38.402 (+38d 24' 08")
  117.493 (07h 49m 58s) +37.908 (+37d 54' 28")
  116.024 (07h 44m 06s) +40.992 (+40d 59' 30")
 ---------------------------------------------
The error box area is 1.01 sq. deg, and its maximum
dimension is 3.7 deg (the minimum one is 19 arcmin).
The Sun distance was 91 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
MAXI/GSC localization (GCN 32777).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221017_T19789/IPN

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


GRB_name: GRB221009A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32788
SUBJECT: GRB 221009A: Second epoch of NuSTAR data
DATE:    22/10/18 03:28:57 GMT
FROM:    Daniel Brethauer at UC Berkeley  <daniel_brethauer@berkeley.edu>

Daniel Brethauer (UC Berkeley), Raffaella Margutti (UC Berkeley), Judith
Racusin (NASA/GSFC), Brian Grefenstette (Caltech), Kate D. Alexander
(Arizona), Tom Barclay (NASA/GSFC), Edo Berger (Harvard), Eric Burns (LSU),
Brad Cenko (NASA/GSFC), Yvette Cendes (Harvard), Ryan Chornock (UC
Berkeley), Tarraneh Eftekhari (Northwestern), Jamie Kennea (PSU), Tanmoy
Laskar (Utah)


A second epoch of NuSTAR observations of GRB221009A was obtained on October
15, 2022 starting at 05:21:09 UTC (~5.6 days since trigger; Dichiara et
al., GCN 32632; Veres et al., GCN 32636) with an exposure time of 25 ks
(PIs Racusin and Margutti).


The 3-79 keV spectrum is well fit by a power law with a photon index of
Gamma = 1.91 +/- 0.02 (1 sigma c.l.), which suggests spectrally softer
emission than observed during the first NuSTAR epoch (Brethauer et al., GCN
32695). The inferred NuSTAR power-law index is consistent with the value
inferred from contemporaneous Swift-XRT observations, which indicate Gamma=
1.79 +/- 0.11 and a best-fitting intrinsic absorption NHint=(0.46 +/-
0.10)e22 cm-2 at z=0.151 for an assumed Galactic neutral hydrogen column
density NH_mw=0.563e22 cm-2 (Willingale et al., 2013). The corresponding
unabsorbed flux is ~4.5e-11 ergs/cm^2/s  (3-79 keV), indicating a factor
~10 fading with respect to the previous epoch of NuSTAR data (Brethauer et
al., GCN 32695).


Additional epochs of NuSTAR monitoring are planned on October 20th, and
November 2nd. We thank the entire NuSTAR SOC for promptly implementing
these observations.


GRB_name: GRB221017A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32790
SUBJECT: GRB 221017A: Swift ToO observations
DATE:    22/10/18 13:50:15 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the MAXI GRB 221017A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021529

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: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32791
SUBJECT: GRB 221009A: Medicina Radio Telescope observations
DATE:    22/10/18 14:16:50 GMT
FROM:    Marco Marongiu at Ferrara U  <marco.marongiu@unife.it>

M. Marongiu, E. Egron, A. Pellizzoni (INAF/OAC), S. Righini (INAF/IRA), 
C. Guidorzi (UniFe), and S. Mulas (UniCa), report:

We observed GRB 221009A (Dichiara et al. GCN 32632) with the Medicina 
Radio Telescope (www.radiotelescopes.inaf.it) through single-dish 
imaging in X-band (central frequency 8.2 GHz, bandwidth 0.3 GHz) in two 
time intervals: (1) 13:30-19:30 UTC on October 14, 2022 (4.97-5.22 days 
after the burst), and (2) 11:30-19:30 UTC on October 17, 2022 (7.89-8.22 
days after the burst).

In our analysis, at 5.1 days (after the burst) we detected a faint radio 
emission at 8.2 GHz with a flux density of 26 +- 5 mJy at a position 
consistent with the optical position (Dichiara et al., GCN 32632) and 
the radio position (Laskar et al., GCN 32740, Laskar et al., GCN 32757).

We did not detect any significant signal with a 2-sigma upper limit of 
20 mJy at 8.1 days.


We acknowledge the scheduler and the staff of the Medicina Radio 
Telescope for approving and executing these observations.


GRB_name: GRB221009A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32793
SUBJECT: The probability of observing GRB 221009A at z = 0.151
DATE:    22/10/18 14:47:32 GMT
FROM:    Jean-Luc Atteia at IRAP  <jean-luc.atteia@irap.omp.eu>

The prompt emission of the extraordinarily bright GRB 221009A was detected in space by Swift (Dichiara et al. GCNC 32632, Krimm et al. 32688), Fermi (Veres et al. GCNC 32636, Bissaldi et al. GCNC 32637, Lesage et al. GCNC 32642, Pillera et al. GCNC 32658, Omodei et al. GCNC 32760), AGILE (Ursi et al. GCNC 32650, Piano et al. GCNC 32657), INTEGRAL (Gotz et al. GCNC 32660), Solar Orbiter (Xiao et al. GCNC 32661), SRG (Lapshov et al. GCNC 32663), Konus (Frederiks et al. GCNC 32668), GRBAlpha (Ripa 
et al. GCNC 32685), STPSat-6 (Mitchell et al. GCNC 32746), HEBS (Liu et al. GCNC 32751). Various estimates of its prompt isotropic energy ranks it among the most energetic GRBs (Cenko et al. 2011, Atteia et al. 2017):
Gotz et al. GCNC 32660 -      Eiso = 8e53 ergs in [75 keV 1 MeV] ;
Frederiks et al. GCNC 32668 - Eiso = 3e54 ergs in [20 keV - 10 MeV ?] ;
Kann et al. GCNC 32762 -      Eiso = 6e54 ergs in [0.1 keV - 100 MeV] ;

We discuss here the chance to observe such an energetic GRB at redshift z = 0.151 (de Ugarte Postigo GCNC 32648, Castro-Tirado et al. GCNC 32686), considering the rate of such extremely energetic GRBs observed at higher redshifts.

Considering a flat cosmology with H0 = 67.4 km/s/Mpc and Omegam = 0.315 (Planck Collaboration et al. 2020), we extrapolate the rate of â‰ˆ4 extremely energetic GRBs per year derived by Atteia et al. (2017) in the redshift range [1,5], to the volume of the nearby universe enclosed within z = 0.151.

- Assuming a constant GRB formation rate, we obtain 1 extremely energetic GRB per ~130 yr.
- Assuming the GRB formation rate of Palmerio & Daigne (2021), we obtain 1 extremely energetic GRB per ~520 yr.

We conclude that there is a ~10% probability to observe an event like GRB 221009A about 50 years after the discovery of the first GRB.

Bibliography :
- Cenko, S. B., Frail, D. A., Harrison, F. A., et al. 2011, ApJ, 732, 29
- Atteia, J.-L., Heussaff, V., Dezalay, J.-P., et al. 2017, ApJ, 837, 119
- Palmerio, J.T. & Daigne, F. 2021, A&A, 649, 166
- Planck Collaboration, Aghanim, N., Akrami, Y., et al. 2020, A&A, 641, A6


GRB_name: GRB221009A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32795
SUBJECT: GRB 221009A: GRANDMA observations
DATE:    22/10/18 15:32:46 GMT
FROM:    Sarah Antier at OCA  <sarah.antier@oca.eu>

Y. Rajabov, T. Sadibekova (UBAI), Y. Tillayev (UBAI, NUUz),
C. Rinner, Z. Benkhaldoun (OUCA), X. F. Wang (THU/BJP),
J. Zhu (BJP), X. Y. Zeng (CGTU), L. T. Wang, A. Iskandar (XAO),
A. M. Fouad, A. Takey A. Shokry, M. Soliman (NRIAG), P. Hello,
T. Hussenot (IJCLAB), M. Boer, A. de Ugarte Postigo, S. Antier (OCA/Artemis)
D. A. Kann (Goethe Univ.), E. Burns (LSU), A. Simon, A. Baransky
(Kyiv Univ), L. Abe, Ph. Bendjoya, J.-P. Rivet (Lagrange-OCA),
D. Vernet (Galilee-OCA), S. Brunier (KNC), R. Inasaridze, R. Natsvlishvili,
N. Kochiashvili (AbAO), S.Beradze, V. Aivazyan, G. Kapanadze, O.Burkhonov,
J. G. Ducoin (IAP), S.Ehgamberdiev (UBAI, NUUz), A. Klotz (OMP/IRAP),
I. Tosta e Melo (INFN-LNS) report on behalf of GRANDMA collaboration:

The GRANDMA telescope network responded to the alert of the ultra-bright
GRB 221009A (Swift detection: Dichiara et al., GCN 32632; Fermi
GBM detection: Veres et al., GCN 32636).

The first observations started 2.30 h after the Fermi/GBM trigger time
with TAROT-TRE without filter.

Below, we report select observations. We also report our 5-sigma upper
limits. Magnitudes are given in the AB system.

T-T0 (day)| MJD   | Obser.   |Exposure| Filter | Mag +/- err |Upp.Lim. (AB)
___________________________________________________________________________
1.069 |59862.622720|UBAI-ST| 6x180s |R-Bessel| 18.3  +/- 0.1 | 19.2
1.136 |59862.689664| KAO   | 11x100s| sdssr  | 18.57 +/- 0.05| 20.5
1.134 |59862.687523| KAO   | 2x120s | sdssg  | 20.43 +/- 0.2 | 19.8
1.154 |59862.707801| KAO   | 9x80s  | sdssi  | 17.56 +/- 0.05| 20.3
1.166 |59862.719039| KAO   | 2x120s | sdssz  | 16.93 +/- 0.05| 19.7
1.223 |59862.776151|Lisnyky| 10x30s |R-Bessel| 18.15 +/- 0.1 | 19.6
1.258 |59862.811817| MOSS  | 20x60s | clear  | 18.5  +/- 0.1 | 20.3
1.301 |59862.854179|C2PU-O | 2x300s | sdssr  | 18.96 +/- 0.1 | 20
3.027 |59864.580925| SNOVA | 10x150s| clear  |        -      | 19.7
3.047 |59864.600648|UBAI-ST| 5x240s |R-Bessel| 19.85  +/- 0.1| 19.3
4.191 |59865.743981| KAO   | 21x110s| sdssz  | 18.8   +/- 0.1| 19.7

These detections and limits are consistent with the detections and limits
previously reported in Lipunov et al., GCN 32634; Perley, GCN 32638;
Broens, GCN 32640; Hu et al., GCN 32644; Belkin et al., GCN 32645; GCN 32769
; Wet et al., GCN 32646; Xu et al., GCN 32647; de Ugarte Postigo et al., GCN
32648; Odeh, GCN 32649; GCN 32666; Brivio et al., GCN 32652; Kuin et al.,
GCN 32656; Paek et al., GCN 32659; Kumar et al., GCN 32662; Romanov, GCN
32664; 32679; Chen et al., GCN 32667; Vidal et al., GCN 32669; Kim et al.,
GCN 32670; Groot et al., GCN 32678; Castro-Tirado et al., GCN 32686;
Watson et al., GCN 32692; Strausbaugh et al. GCN 32693; Butler et al., GCN
32705; Vinko et al., GCN 32709; Mao et al., GCN 32727; Zaznobin et al.,
GCN 32729; Sasada et al., GCN 32730; Strausbaugh & Cucchiara, GCN 32738;
O'Connor et al., GCN 32739; GCN 32750; Bikmaev et al., GCN 32743; GCN
32752; Rastinejad & Fong, GCN 32749; Schneider et al., GCN 32753;
Dâ€™Avanzo et al., GCN 32755; Huber et al., GCN 32758; Shrestha et al.,
GCN 32759; 32771; Izzo et al., GCN 32765.

The observations were contaminated by the nearly full Moon.

Further analysis are ongoing in GRANDMA especially on
TAROT, ShAO-T60, AbAO-T70 and C2PU-O.

The KAO, UBAI-ST have been calibrated using nearby
stars from the Pan-STARRS catalog in sdss r, g, i and z, measured with
STDpipe (Karpov 2022). Lisnyky-AZT has been calibrated using field
stars from the PanSTARRS-DR1 catalog, measured with the MUPHOTEN pipeline
(Duverne et al. 2022). MOSS and SNOVA data have been calibrated with
Gaia DR2.

We advocate a joint multi-wavelength publication for this event and we are
happy to collaborate with teams that have the same spirit,
to be able to explore the best astrophysical scenario.

GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr)
devoted to the observation of transients in the context of multi-messenger
astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is
the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).


GRB_name: GRB221013B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32798
SUBJECT: GRB 221013B: Swift/BAT-GUANO detection
DATE:    22/10/19 02:04:39 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 221013B onboard (T0: 2022-10-13T02:23:28
 UTC, Fermi/GBM GCN 32726).

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, 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 9.2 in a 1.024
s analysis time bin.

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FOV, with DeltaLLHOut
of 3.3 and DeltaLLHPeak of 0.2.

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

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

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


GRB_name: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32799
SUBJECT: GRB 221009A: Continued LDT Afterglow Monitoring
DATE:    22/10/19 03:59:58 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), S. B. Cenko (NASA/GSFC), E. Troja (UTV/ASU),
S. Dichiara (PSU), A. Kutyrev (NASA/GSFC), S. Veilleux (UMD),
J. Durbak (UMD), on behalf of a larger collaboration:

We performed target of opportunity observations of GRB 221009A
(Dichiara et al., GCN 32632, Veres et al., GCN 32636)
with the 4.3m Lowell Discovery Telescope (LDT) in Happy Jack, AZ.
Observations began on October 13, 2022 at 02:05:29 UT corresponding
to ~9.5 d after the GRB. We obtained images in the riz filters at
an airmass ~1.1 with seeing ~1.7".

The afterglow is clearly detected in each filter. We obtain the
following magnitudes calibrated against the PS1 catalog:

r = 21.68 +/- 0.07 AB mag
i = 20.72 +/- 0.05 AB mag

These magnitudes are not corrected for Galactic extinction.

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


GRB_name: GRB221009A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32800
SUBJECT: GRB 221009A: Spectroscopic detection of emerging SN features
DATE:    22/10/19 11:23:30 GMT
FROM:    Antonio de Ugarte Postigo at OCA  <deugarte@oca.eu>

A. de Ugarte Postigo (OCA), L. Izzo (DARK/NBI), C. C. Thoene
 (ASU-CAS), J. P. U. Fynbo (DAWN/NBI), D. A. Kann (Goethe Univ.), 
J. F. Agui Fernandez (IAA-CSIC), N. R. Tanvir (Leicester Univ.) report:

We have been spectroscopically monitoring the evolution of the 
extremely bright GRB 221009A (Swift detection: Dichiara et al., 
GCN 32632; Fermi GBM detection: Veres et al., GCN 32636) using 
OSIRIS at the 10.4m GTC telescope. In a spectrum combining data 
taken on 16 and 17 October (at an average time of ~8 days after the 
burst), covering the spectral range between 3700 and 10000 AA, the 
emission is still clearly dominated by the afterglow. However, after 
subtracting a model of the continuum, the spectrum shows undulations 
characteristic of a GRB-SN. In particular we identify broad features at 
similar wavelengths (after correcting for the redshift difference) as 
those present in SN 1998bw, with somewhat larger velocities. This is 
indicative of the emergence of the associated supernova. Further 
follow-up observations are planned.


GRB_name: GRB221009A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32802
SUBJECT: GRB 221009A X-ray light-curve and the indication of TeV light-curve
DATE:    22/10/19 15:28:45 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.
Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:

LHAASO observed more than 5000 very high energy (VHE) photons in GRB
221009A, with the highest energy reaching 18 TeV (GCN 32677). Previously,
high energy TeV emissions were also observed in GRB 180720B (Abdalla et al.
2019), 190114C (MAGIC Collaboration 2019), 190829A (H.E.S.S. Collaboration
2021) and 201216C (Blanch et al. GCN 29075). A common feature of these
bursts is that the TeV light-curve follows a power-law decay with a similar
index as the X-ray light-curve, and the TeV luminosity is tens of percent
of the X-ray luminosity (see attached figure 1 and the references of
Abdalla et al. 2019, MAGIC Collaboration 2019 and H.E.S.S. Collaboration
2021, Ruffini et al. 2021, Rueda et al. 2022, Rastegarnia et al. 2022, Wang
et al. 2022). Here we present the X-ray light-curve of GRB 221009A observed
by Swift-XRT (GCN 32651), and the t0 is taken from the Fermi-GBM trigger
time (GCN 32636), see attached figure 2, a power-law of index -1.58 is
fitted. The shadow region shows 20%-60% of the X-ray luminosity, which is
expected to be the 0.3-1 TeV luminosity (17% less luminous for 0.5-18 TeV
assuming a power-law spectrum of photon index -2) of this new burst if it
shares the same behavior as the previous ones. We encourage further
observations, especially the VHE observations, because this burst probably
is more luminous than the previous ones, and it will be precious to have a
late time (after days) VHE luminosity which was never achieved before, as
well as the optical observations for the supernova appearance (GCN 32670,
GCN 32780).

Figure 1: http://www.icranet.org/docs/fig1.png
Figure 2: http://www.icranet.org/docs/fig2.png



http://www.icranet.org

http://www.icranet.org


GRB_name: GRB221009A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32803
SUBJECT: GRB 221009A: BOAO NIR detections
DATE:    22/10/19 15:52:11 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Gregory S.-H. Paek, Gu Lim, Hyeonho Choi, Sophia Kim (SNU),
Hyun-Il Sung (KASI), Yuji Urata (NCU) on behalf of a larger collaboration

We observed the field of GRB 221009A (Swift detection: Dichiara et al., GCN
32632; Fermi GBM detection: Veres et al., GCN 32636), in J and K filters
with the KASINICS instrument on the 1.8 m telescope of the Bohyunsan
Optical Astronomy Observatory (BOAO), Korea. The observation started at
2022-10-18-11:34 (UT) or JD=2459870.98230324, taking a series of images for
about 1.25 hrs.

We identify the afterglow in the KASINICS images, with a rough photometry
of K ~ 18.6 AB mag. Further observations and analysis are being carried out
to obtain more data and refine the photometry.

We thank the staff of BOAO for carrying out the observation.


GRB_name: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32804
SUBJECT: GRB 221009A: TNG NIR detection
DATE:    22/10/19 16:28:04 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

M. Ferro, R. Brivio, P. Dâ€™Avanzo (INAF-OAB), S. Piranomonte (INAF-OAR), V. Lorenzi, G. Mainella (INAF-TNG), 
on behalf of the CIBO collaboration report:

We observed the field of GRB 221009A (Dichiara et al., GCN 32632; Kennea & Williams, GCN 32635; Veres et al., 
GCN 32636; Bissaldi et al., GCN 32637; Svinkin et al., GCN 32641; Ursi et al., GCN Circ. 32650) with the Italian 3.6m 
TNG telescope equipped with the near-infrared camera NICS. A series of images were obtained with the J, H and K filters 
on 2022-01-16 at a mid time of about 7.3 days after the GBM trigger time. 

The NIR afterglow (Brivio et al., GCN Circ. 32652) is clearly detected in all bands. From preliminary photometry we derive 
the following magnitude:

H = 16.45 +/- 0.04

(Vega; calibrated against the 2MASS catalogue).


We acknowledge the TNG visiting astronomers B. Lakeland and B. Nicholson for their support.


GRB_name: GRB221009A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32805
SUBJECT: Improved IPN localization for GRB 221009A (BepiColombo-MGNS light curve)
DATE:    22/10/19 16:43:28 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 team,

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,

and

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

The extremely bright, long-duration GRB 221009A
(GCNs 32632, 32635, 32636, 32637, 32641, 32642, 32650, 32657,
32658, 32668, 32685, 32751; ATels 15650, 15656, 15660)
was detected by the MGNS/BepiColombo interplanetary gamma-ray detector. 
The burst light curves in the energy range 280-460 keV exhibit a 
multi-peaked pulse structure with a total duration of ~6.6 min. The 
source of GRB 221009A was obscured for MGNS by spacecraft structure that 
have limited transparency in the specified above energy range.

The link below provides a plot of the time profile of the gamma-ray 
count rate. The GRB221009A.TXT file, also available at this link,
contains light curve data in three columns: time in UTC, accumulated 
count and accumulation time.

http://l503.iki.rssi.ru/owncloud/index.php/s/HZtqdQ1b9QW3ojv

Using the BepiColombo (MGNS) data we have triangulated GRB 221009A
to the 3 sigma error box whose coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   287.761 (19h 11m 03s) +20.670 (+20d 40' 11")
  Corners:
   283.599 (18h 54m 24s) +27.415 (+27d 24' 54")
   283.634 (18h 54m 32s) +28.133 (+28d 08' 00")
   291.780 (19h 27m 07s) +12.770 (+12d 46' 14")
   291.767 (19h 27m 04s) +11.822 (+11d 49' 20")
  ---------------------------------------------
The error box area is 6.63 sq. deg, and its maximum
dimension is 18 deg (the minimum one is 23 arcmin).
The Sun distance was 92 deg.

This box may be further improved.

The Swift-XRT source (GCN 32632) is inside the box.
The distance between the source and
the Konus-MGNS annulus center line is 1.7 arcmin.

An updated triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221009_T47819/IPN/


GRB_name: GRB221020A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32806
SUBJECT: GRB 221020A: Fermi GBM Final Real-time Localization
DATE:    22/10/20 05:34:08 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:23:52 UT on 20 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221020A (trigger 687936237.82563 / 221020225).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 172.9, Dec = 16.0 (J2000 degrees, equivalent to J2000 11h 31m, 16d 00'), with a statistical uncertainty of 3.0 degrees.

The angle from the Fermi LAT boresight is 36.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221020225/quicklook/glg_skymap_all_bn221020225.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/bn221020225/quicklook/glg_healpix_all_bn221020225.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221020225/quicklook/glg_lc_medres34_bn221020225.gif


GRB_name: GRB221017A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32807
SUBJECT: GRB 221017A: Swift-XRT observations
DATE:    22/10/20 14:42:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 221017A (Nawa et al. GCN Circ. 32777), collecting 1.9 ks of
Photon Counting (PC) mode data between T0+196.7 ks and T0+225.8 ks. 

Two uncatalogued sources are detected:

- Source 1
RA (J2000): 116.8816 = 07:47:31.58
Dec (J2000): 39.3449 = +39:20:41.5
Error: 10.7" (radius, 90% confidence)
Avg. XRT count-rate: 5.4(+2.6,-2.0)x10^(-3) cts/s

- Source 2 
RA (J2000): 116.9220 = 07:47:41.27
Dec (J2000): 39.2614 = +39:15:41.2
Error: 10.0" (radius, 90% confidence)
Avg. XRT count-rate: 3.3(+2.1,-1.5)x10^(-3) cts/s

Both sources lie inside the overlap of the MAXI localization error box
(Nawa et al. GCN Circ. 32777) and the IPN triangulation region (Kozyrev
et al. GCN Circ. 32787).


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/00021529.

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


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32808
SUBJECT: GRB 221009A: Peak luminosity of the supernova vs. synchrotron afterglow
DATE:    22/10/20 14:57:47 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

 Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.
Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:

GRB 221009A appears to be a rare example (Jean-Luc Atteia et al. 2022, GCN
32793) of a particularly energetic and close GRB (de Ugarte Postigo et al.
2022, GCN 32648 and Lesage et al. 2022, GCN 32642 and N.P.M. Kuin et al.
2022, GCN 32656). Within the BdHN model, we have followed the X-ray,
optical, and radio afterglows originating from synchrotron emission powered
by fast spinning newborn neutron stars (vNS) with initial periods of
fraction of a millisecond, accreting the supernova ejecta, created by the
collapse of a carbon-oxygen core (Rueda et al. 2022, arXiv:2204.00579).
Figures 1, 2 and 3 show the afterglows of three type I BdHNe, namely GRB
180720B (Ruffini et al. 2018, GCN 23019), GRB 190114C (Ruffini et al. 2019,
GCN 23715), and GRB 211023A (Aimuratov et al. 2021, GCN 31056), and the
prediction of their associated supernova.
We have indicated the expected time of the occurrence of the supernova in
GRB 221009A (Aimuratov et al. 2022, GCN 32780). The ongoing observations in
optical, radio, and X-ray bands are strongly recommended for allowing the
determination of the spin and magnetic field of the vNS. This will probe as
well if the optical synchrotron emission, at ~ 10^6 s from the Fermi-GBM
trigger, impedes the observations of the optical emission of the supernova
originating from nickel decay (Aimuratov et al. in preparation, see also
data from Ilfan Bikmaev et al. 2022, GCN 32752, and Jia. Ren et al. 2022,
arXiv:2210.10673, reproduced in Fig. 4).

Fig1: http://www.icranet.org/docs/Fig1.pdf
Fig2: http://www.icranet.org/docs/Fig2.pdf
Fig3: http://www.icranet.org/docs/Fig3.pdf
Fig4: http://www.icranet.org/docs/Fig4.pdf


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32809
SUBJECT: GRB221009A: LBT optical imaging
DATE:    22/10/20 15:24:03 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi, E. Maiorano (INAF-OAS), D. B. Malesani (Radboud Univ. and 
DAWN/NBI)on behalf of the CIBO collaboration, F. Cusano (INAF-OAS), and 
D. Paris (INAF-OA Roma), report:

We observed the field of GRB 221009A (Dichiara et al., GCN 32632; Kennea 
& Williams, GCN 32635; Veres et al., GCN 32636; Bissaldi et al., GCN 
32637; Svinkin et al., GCN 32641; Ursi et al., GCN Circ. 32650) 
simultaneously in the blue and red arms with the g'+r' and g'+i' bands 
with the MODS instrument mounted on LBT (Mt Graham, AZ, USA). We 
observed for 22 min per arm at the midtime 03:11 UT on 2022-10-18, 8.58 
days after the burst trigger. Observations were performed under modest 
weather conditions with an average seeing of ~1" but high humidity and 
passing cirrus.

We clearly detect the afterglow and we preliminary measure

r=21.63+-0.02 (AB system),

calibrated against Pan-STARRS field stars.

We acknowledge the excellent support from the LBTO and LBT-INAF staff, 
particularly A. Becker and D. G. Huerta in obtaining these observations.


GRB_name: GRB221013B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32810
SUBJECT: Fermi GBM trigger 687320613 / 221013100 (GRB 221013B) is not a GRB
DATE:    22/10/20 20:25:38 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres  (UAH) reports on behalf of the Fermi GBM Team:

â€œThe Fermi Gamma-ray Burst Monitor (GBM) trigger 687320613 / 221013100  at
02:23:28 UT on 13 October 2022, classified as a GRB (GCN #32726), is in
fact not due to a GRB. This trigger is possibly related to a solar flare.

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


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32811
SUBJECT: GRB 221009A: 1.3m DFOT Optical Observations
DATE:    22/10/21 07:11:24 GMT
FROM:    Rahul Gupta at ARIES, India  <rahulbhu.c157@gmail.com>

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


We performed target of opportunity observations of the extremely bright GRB
221009A (Dichiara et al., GCN 32632; Kennea and Williams, GCN 32635; Veres
et al., GCN 32636; Bissaldi et al., GCN 32637; Svinkin et al., GCN 32641; Ursi
et al., GCN 32650; Piano et al., GCN 32657; Pillera et al., GCN 32658; Gotz
et al., GCN 32660; Xiao et al., GCN 32661; Frederiks et al., GCN 32668; Ripa
et al., GCN 32685) using the 2Kx2K CCD Imager mounted at the 1.3m Devasthal
Fast Optical Telescope (DFOT) located at the Devasthal observatory of
Aryabhatta Research Institute of Observational Sciences (ARIES), India. The
observations were started on 2022-10-16 at 14:41:41 UT, i.e., ~ 7.06 days
after the detection. We have taken multiple frames in the R filter at
different epochs. We clearly detected the optical afterglow of GRB
221009A (GCNs
32632, 32635, 32636, 32641, 32657, 32658, 32660, 32666, 32668, 32670,
32671, 32676, 32677, 32678, 32679, 32680, 32683, 32684, 32685, 32686,
32691, 32692, 32693, 32694, 32695, 32700, 32705, 32707, 32709, 32727,
32729, 32730, 32736, 32738, 32739, 32740, 32743, 32746, 32749, 32750;
32752; 32753; 32755; 32758; 32765; 32769; 32771; 32795; 32799; 32800;
32803; 32804; 32809) in our stacked image. The preliminary photometric
estimate of the afterglow is the following :

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

=========================================================
2022-10-16 14:41:41   ~7.09       R           200*25          21.30 +/- 0.04


Further follow-up observations are planned. The magnitude is not corrected
for the Galactic extinction in the direction of the burst. Photometric
calibration is performed using the standard stars from the USNO-B1.0
catalog.

This circular may be cited.


GRB_name: GRB221021A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32812
SUBJECT: GRB 221021A: Fermi GBM Final Real-time Localization
DATE:    22/10/21 09:28:45 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 09:18:25 UT on 21 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221021A (trigger 688036710.740176 / 221021388).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 218.7, Dec = -68.6 (J2000 degrees, equivalent to J2000 14h 34m, -68d 35'), with a statistical uncertainty of 11.9 degrees.

The angle from the Fermi LAT boresight is 132.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221021388/quicklook/glg_skymap_all_bn221021388.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/bn221021388/quicklook/glg_healpix_all_bn221021388.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221021388/quicklook/glg_lc_medres34_bn221021388.gif


GRB_name: GRB221017A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32813
SUBJECT: GRB 221017A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/10/21 15:48:27 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 221017A (MAXI/GSC detection: Nawa et al., GCN Circ. 32777;
IPN triangulation: Kozyrev et al., GCN Circ 32787)  was detected in the 
ground analysis of the CALET Gamma-ray Burst Monitor (CGBM) data around 
05:29:49 UTC on October 17, 2022 (referenced to GCN Circ 32787). 
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure that starts
at T-20.5 sec, peaks at T+176.6 sec and ends at T+670.4 sec.
The T90 and T50 durations measured by the SGM data are 191.9 +/- 44.4 sec
and 52.7 +/- 0.5 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1350019714/

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


GRB_name: GRB221020A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32815
SUBJECT: GRB 221020A: Detection by GRBAlpha
DATE:    22/10/22 14:20:07 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, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly 
Observatory), M. Dafcikova, F. Munz, N. Husarikova, J.-P. Breuer, M. 
Topinka, 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 221020A (Fermi-GBM detection: Fermi GBM Team, GCN 
Circ. 32806) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. 
SPIE 2020).

The 11.3 sigma detection was confirmed at the peak time 2022-10-20 
05:23:59.8 UTC. The GRB has a T90 duration of 15 s.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221020A_GCN_GRBAlpha.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a 
future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its 
detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously 
upgrading the on-board data acquisition software stack. 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: GRB221022A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32816
SUBJECT: GRB 221022A: Fermi GBM Final Real-time Localization
DATE:    22/10/22 19:41:48 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 19:33:33 UT on 22 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221022A (trigger 688160018.552146 / 221022815).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 126.6, Dec = -17.7 (J2000 degrees, equivalent to J2000 08h 26m, -17d 41'), with a statistical uncertainty of 11.4 degrees.

The angle from the Fermi LAT boresight is 116.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221022815/quicklook/glg_skymap_all_bn221022815.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/bn221022815/quicklook/glg_healpix_all_bn221022815.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221022815/quicklook/glg_lc_medres34_bn221022815.gif


GRB_name: GRB221021A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32817
SUBJECT: GRB 221021A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/10/22 21:47:27 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Gayathri Raman (PSU), Aaron Tohuvavohu (U Toronto), James DeLaunay
(UAlabama), Jamie A. Kennea (PSU), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 220924A onboard (T0:
2022-09-24T21:44:54 UTC, Fermi/GBM GCN 32812, GECAM trig #35).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 20.7 in a
16.384 s analysis time bin.

NITRATES results are consistent with a burst coming from outside the
FOV, with DeltaLLHOut of 0.3.

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

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

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


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32818
SUBJECT: GRB 221009A: optical observations, SN photometric evidence
DATE:    22/10/22 22:47:16 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI, HSE), A. Moskvitin (SAO RAS), V. Kim (FAI), A. Pozanenko 
(IKI),  M. Krugov (FAI), R. Uklein (SAO RAS), N. Pankov (HSE) report on 
behalf of GRB IKI FuN:

We continue observations of GRB 221009A (Swift J1913.1+1946) (Dichiara 
et al., GCN 32632; Kennea and Williams, GCN  32635; Veres et al., GCN 
32636; Bissaldi et al., GCN  32636; Svinkin et al., GCN 32641; Piano et 
al., GCN 32657; Pillera et al., GCN 32658;  Gotz et al., GCN 32660; Xiao 
et al., GCN 32661; Frederiks et al., GCN 32668; GCN 32668; Ripa
et al., GCN 32685; Kozyrev et al., GCN 32805).  Observations  with 
AZT-20 telescope of Assy-Turgen observatory obtained on  October 20, 21 
and TOO photometry with BTA SAO RAS telescope equipped with SCORPIO-2 
was obtained on  October 16 and 18.  The optical afterglow (GCNs 32632, 
  32635, 32636, 32641, 32657, 32658, 32660, 32666, 32668, 32670, 32671, 
32676, 32677, 32678, 32679, 32680, 32683, 32684, 32685, 32686, 32691, 
32692, 32693, 32694, 32695, 32700, 32705, 32707, 32709, 32727, 32729, 
32730, 32736, 32738, 32739, 32740, 32743, 32746, 32749, 32750; 32752; 
32753; 32755; 32758; 32765; 32769; 32771; 32795; 32799; 32803; 32804; 
32809; 32811) is detected in combined images of g',r',i' filters.

Preliminary photometry of the afterglow on 2022-10-20/21 obtained in 
Assy observatory with  AZT-20 telescope is following

Date       UT start  t-T0       Exp.   Filter  OT    Err.   UL(3sigma)
                     (mid, days)  (s)           (AB)
2022-10-20/21 n/d   11.55024    59*60  g'      23.7   0.2   24.5
2022-10-21 14:18:18 12.05299    30*60  r'      21.94  0.07  23.9
2022-10-21 14:49:37 12.08516    30*60  i'      20.72  0.11  23.3

The photometry is based on nearby PS1 stars.

The light curve based on our observations can be found in 
http://grb.rssi.ru/GRB221009A/GRB221009A_lc_cc_15_cut.png

We observe a bump in the light curve starting on 6th days since trigger. 
The light curve is clearly chromatic at the bump. We  can assume that 
the chromatic bump is a supernova over an afterglow of GRB 221009A 
(Belkin et al., GCN 32769).


GRB_name: GRB221009A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32819
SUBJECT: GRB 221009A: Analysis of the initial episode using data of GBM/Fermi and SPI-ACS/INTEGRAL
DATE:    22/10/22 23:05:12 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We analyze the first episode of GRB 221009A (Dichiara et al., GCN 32632; 
Kennea and Williams, GCN  32635; Veres et al., GCN 32636; Bissaldi et 
al., GCN  32636; Svinkin et al., GCN 32641; Piano et al., GCN 32657; 
Pillera et al., GCN 32658;  Gotz et al., GCN 32660; Xiao et al., GCN 
32661; Frederiks et al., GCN 32668; GCN 32668; Ripa et al., GCN 32685; 
Kozyrev et al., GCN 32805) not affected by dead time and pile-up 
instrumental effects, using publicly available data of GBM/Fermi and 
SPI-ACS/INTEGRAL.

We investigate energy spectrum of the time interval (T0-1, T0+55) s, 
where T0 = 13:16:59 UTC 2022-10-09 is a time of  GBM/Fermi trigger.  The 
spectrum can be fitted by a simple power law model with the spectral 
index of gamma = -1.68 +/- 0.01.

See the spectrum in http://grb.rssi.ru/GRB221009A/GRB221009A_1st_episode.png

It is in a contradiction with CPL (power law with exponential cutoff) 
spectral model for the episode, obtained by Lesage et al., GCN 32642 
using GBM/Fermi data (Epeak = 375 +/- 87 keV) and by Frederiks et al., 
GCN 32668 using Konus/WIND data (Epeak = 975 (-332, +712) keV). The 
value of spectral index is not typical for indexes before the break (in 
CPL or Band model), but it is a rather typical for the index after the 
break in Band model. We hypothesize the actual break to be placed at low 
energies (Epeak < 20 keV). The hypothesis could be supported by placing 
Eiso parameter into Amati correlation diagram.   The Eiso = (3.2 +/- 
0.1)E51 erg is calculated  within our power law model with gamma = -1.68 
and using redshift value of z = 0.151 (de Ugarte Postigo et al., GCN 
32648; Castro-Tirado et al., GCN 32686). The Eiso value corresponds to 2 
sigma range of possible Epeak value of (20, 315) keV for type II (long) 
GRBs (Minaev et al., MNRAS, 492, 2, 1919, 2020).

See the correlation diagram in
http://grb.rssi.ru/GRB221009A/GRB221009_Amati_1st_episode.png

The softness of the spectrum is also confirmed by our analysis of 
SPI-ACS/INTEGRAL data: assuming high values of Epeak (e.g. Epeak = 975 
keV) and using SPI-ACS - GBM cross-calibration method to convert SPI-ACS 
count fluxes to energy units (Minaev et al., in preparation) we obtain 
underestimated value of fluence F_ACS = (1.3 +/- 0.3)E-5 erg/cm^2  for 
Epeak = 975 keV, which is less than reference value of F_GBM = (2.38 +/- 
0.04)E-5 erg/cm^2 in (10, 1000) keV range, calculated within our power 
law model with gamma = -1.68.
Using data of GBM/Fermi we perform cross-correlation analysis of the 
initial episode and find significant spectral lags, typical for type II 
(long) GRBs (e.g. Minaev et al., Astronomy Letters, 40, 5, 235, 2014). 
Spectral lag â€“ energy dependence is fitted satisfactory by logarithmic 
function lag ~ A*log(E) with spectral lag index A = 0.11 +/- 0.03.

The spectral lag and its parameter can be found in 
http://grb.rssi.ru/GRB221009A/GRB221009_GBM_lags_1st_episode.png


GRB_name: GRB221022B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32820
SUBJECT: GRB 221022B: Fermi GBM Final Real-time Localization
DATE:    22/10/22 23:05:54 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 22:55:48 UT on 22 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221022B (trigger 688172153.911872 / 221022955).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 167.4, Dec = 15.4 (J2000 degrees, equivalent to J2000 11h 09m, 15d 24'), with a statistical uncertainty of 1.8 degrees.

The angle from the Fermi LAT boresight is 93.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221022955/quicklook/glg_skymap_all_bn221022955.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/bn221022955/quicklook/glg_healpix_all_bn221022955.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221022955/quicklook/glg_lc_medres34_bn221022955.gif


GRB_name: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32821
SUBJECT: GRB 221009A: James Webb Space Telescope Observations
DATE:    22/10/22 23:17:34 GMT
FROM:    Andrew Levan at U.of Leicester  <a.levan@astro.ru.nl>

A.J. Levan (Radboud Univ.), T. Barclay (NASA/GSFC), E. Burns (LSU), S. B. Cenko (NASA/GSFC), A. A. Chrimes (Radboud Univ.), P. Dâ€™Avanzo (INAF/OABr), V. Dâ€™Elia (INAF/OAR and ASI/SSDC), M. Della Valle (INAF/OAC), A. de Ugarte Postigo (Obs. Cote dâ€™Azur), W. Fong (Northwestern), A. S. Fruchter (STScI), B. P. Gompertz (Birmingham), C. L. Hedges (NASA/GSFC), K. E. Heintz (DAWN/NBI), L. Izzo (DARK/NBI), D. A. Kann (Goethe Univ.), J. A. Kennea (PSU), E. Le Flocâ€™h (CEA Paris-Saclay), D. B. Malesani (Radboud Univ. and DAWN/NBI), A. Melandri (INAF/OAR), B. D. Metzger (Columbia and Flatiron/CCA), S. E. Mullally (STScI), S. Piranomonte (INAF/OAR), M. E. Ravasio (Radboud Univ and INAF/OABr), J. L. Racusin (NASA/GSFC), J. C. Rastinejad (Northwestern), R. Salvaterra (INAF/IASF Milan), B. Sbarufatti (INAF/OABr), B. Schneider (CEA Paris-Saclay), R. L. C. Starling (U. Leicester), N. R. Tanvir (U. Leicester), C. C. Thoene (ASU-CAS), R. A. M. J. Wijers (Amsterdam), D. Xu (NAOC) report:

We observed the afterglow of GRB 221009A (Dichiara et al., GCN 32632; Kennea & Williams, GCN 32635; Bissaldi et al., GCN 32637; Veres et al., GCN 32636) with the James Webb Space Telescope on 22 October 2022, approximately 13 days after the Fermi/GBM trigger. Observations were obtained with the NIRSpec prism, spanning the range 0.6-5.3 microns at low resolution (exposure time 1803 s starting at 13:50 UT), and with MIRI using the Low Resolution Spectroscopy mode, spanning the range 5-12 microns (exposure time 555 s starting at 14:51 UT).

The optical/IR counterpart is well detected in both acquisition and spectral series, providing high signal to noise across the window. Based on provisional NIRSpec data the afterglow appears to be reasonably well described by an absorbed power-law (MW absorption, A_V = 4.2 mag), with a relatively blue spectral slope (nu^-0.4), although we caution that the uncertainty in foreground absorption and photometric calibration means strong statements cannot be made at this stage. 

Further analysis is ongoing. 

We thank the staff of STScI for the rapid assessment of our DDT proposal (GO 2782, PI Levan) and in particular Alison Vick, Greg Sloan and Patrick Ogle for their work to get the observations rapidly into the schedule.


GRB_name: GRB221022B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32822
SUBJECT: GRB 221022B: AGILE detection
DATE:    22/10/23 08:27:48 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the GRB 221022B at T0 = 2022-10-22 22:56:11.76
+/- 0.01 s (UTC), reported by Fermi GBM (#GCN 32820, trigger no. 688172153).

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 15 s and it released a total number of
27380 counts in the MCAL detector (above a background rate of 1070 Hz), and
80780 counts in the AC detector (above a background rate of 2760 Hz). The
AGILE ratemeter light curves can be found at
http://www.agilescienceapp.it/notices/GRB221022B_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, covering the onset of the first episode, from T0-33.15 s to
T0+1.70 s, and released a total number of ~830 counts in the detector,
above an average background rate of 588 Hz. The MCAL light curve can be
found at
http://www.agilescienceapp.it/notices/080607_GRB_MCAL_593564171.767936.png .

The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the
energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress.
Automatic MCAL GRB alert Notices can be found at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.


GRB_name: GRB221022B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32823
SUBJECT: GRB 221022B: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/10/24 00:22:00 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Gayathri Raman (PSU),  Aaron Tohuvavohu (U Toronto), James DeLaunay
(UAlabama), Jamie A. Kennea (PSU), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 221022B onboard (T0:
2022-10-22T22:55:48 UTC, Fermi/GBM GCN 32820, AGILE GCN 32822).

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 44.9 in a
16.384 s analysis time bin.

NITRATES results are consistent with a burst coming from outside the
FOV, with DeltaLLHOut of -17. The best fit sky location is consistent
with the Fermi/GBM position (GCN 32820).

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

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

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


GRB_name: GRB221022A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32824
SUBJECT: GRB 221022A: Swift/BAT-GUANO detection
DATE:    22/10/24 02:41:40 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), Gayathri Raman (PSU), James DeLaunay
(UAlabama), Jamie A. Kennea (PSU), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 221022A onboard (T0: 2022-10-22T19:33:33
 UTC, Fermi/GBM GCN 32816).

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, 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 8.7 in a 4.096
s analysis time bin.

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FOV, with a
borderline DeltaLLHOut of 9.5.

The best fit In FOV position is very weakly preferred over other
positions, with DeltaLLHPeak of 2.1. This position is consistent with
the Fermi/GBM localization (GCN 32816).

The candidate position is
RA, Dec = 118.342, -5.117 which is
   RA(J2000)  = 07h 53m 22.03s
   Dec(J2000) = -5d 07â€² 00.9â€³
with an estimated uncertainty of 5 arcmin.

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

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

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


GRB_name: GRB221023A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32825
SUBJECT: GRB 221023A: AGILE detection of a burst
DATE:    22/10/24 07:33:58 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), C.
Casentini (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata),
A. Argan, M. Cardillo, Y. Evangelista, L. Foffano, E. Menegoni, G. Piano
(INAF/IAPS), A. Bulgarelli, A. Di Piano, V. Fioretti, G. Panebianco, N.
Parmiggiani (INAF/OAS-Bologna), F. Lucarelli (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), F. Longo (Univ. Trieste and INFN Trieste), and P.
Tempesta (TeleSpazio), report on behalf of the AGILE Team:

The AGILE satellite detected a burst at T0 = 2022-10-23 20:41:34 s (UTC).
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 35 s and it released a total number of
115660 counts in the MCAL detector (above a background rate of 1120 Hz),
and 251030 counts in the AC detector (above a background rate of 3010 Hz).
The AGILE ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/GRB221023A_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, from T0+23.34 s to T0+33.35 s (UTC), and released 18196 counts
in the detector, above a background rate of 590 Hz. The MCAL light curve
can be found at
http://www.agilescienceapp.it/notices/GRB221023A_080618_593642494.000000.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: GRB221023A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32826
SUBJECT: GRB 221023A: Fermi GBM Final Localization
DATE:    22/10/24 13:22:51 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

At 20:41:34.92 UT on 23 October 2022, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 221023A (trigger 688250499 / 221023862).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 232.3, Dec = 11.8 (J2000 degrees, equivalent to J2000 15h 29m, 11d 48'),
with a statistical uncertainty of 1 degree.

The angle from the Fermi LAT boresight is 52 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221023862/quicklook/glg_skymap_all_221023862.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/bn221023862/quicklook/glg_healpix_all_bn221023862.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221023862/quicklook/glg_lc_medres34_bn221023862.gif


GRB_name: GRB221024A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32827
SUBJECT: GRB 221024A: Swift detection of a burst
DATE:    22/10/24 13:23:22 GMT
FROM:    Jamie Kennea at Penn State U  <jak51@psu.edu>

R. Brivio (INAF-OAB), P. D'Avanzo (INAF-OAB), M. Ferro (INAF-OAB),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
S. Laha (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), T. Sbarrato (INAF-OAB),
B. Sbarufatti (INAF-OAB), M. H. Siegel (PSU) and M. A. Williams (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 13:00:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221024A (trigger=1131029).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 169.718, +33.041 which is 
   RA(J2000) = 11h 18m 52s
   Dec(J2000) = +33d 02' 28"
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 30 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~3 sec after the trigger. 

The XRT began observing the field at 13:02:36.5 UT, 129.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 169.74060, 33.04207 which is equivalent
to:
   RA(J2000)  = 11h 18m 57.74s
   Dec(J2000) = +33d 02' 31.5"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 68 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.86 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4
(+2.22/-1.98) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the UVW2 filter
starting  127 seconds after the BAT trigger. No credible afterglow
candidate has been  found in the initial data products. The 2.7'x2.7'
sub-image processing failed because there is no aspect solution due
to a nearby very bright star.   Results from the list of  sources
generated on-board are not available at this time. 

Burst Advocate for this burst is R. Brivio (riccardo.brivio 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: GRB221009A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32828
SUBJECT: GRB 221009A: Determination of the black holes mass and spin
DATE:    22/10/24 15:43:08 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

Y. Aimuratov, L. Becerra, C.L. Bianco, C. Cherubini, S. Filippi, M.
Karlica, Liang Li, R. Moradi, F. Rastegar Nia, J.A. Rueda, R. Ruffini, N.
Sahakyan, Y. Wang, S.S. Xue, on behalf of the ICRANet team, report:

In GRB 221009A, as in GRB 130427A (Ackermann et al. 2014, Science, 343, 42;
and Ruffini et al. 2019, ApJ, 886, 82), the Fermi-GBM data in the prompt
phase are piled up (Lesage et al. 2022, GCN 32642). In both cases there are
missing the ultra-relativistic prompt emission (UPE) phases originating
from quantum electrodynamical process around a Kerr BH (Ruffini et al.
2019, ApJ, 886, 82; and Rueda et al. 2022, ApJ, 929, 56), which were well
observed in GRB 190114C (Moradi et al. 2021, Phys Rev D 104, 063043) and
GRB 180720B (Rastegarnia et al. 2022, EPJC 82, 77). Under these conditions,
for GRB 130427A the 0.1-100 GeV data of Fermi-LAT had allowed to determine
only the lower limit on the BH mass, M>2.31 solar masses, and the upper
limit of its spin parameter, Î±<0.4 (Ruffini et al. 2019, ApJ, 886, 82). For
the BDHNI GRB 190114C (Ruffini et al. 2019, GCN 23715), the values of the
BH mass and spin had been determined by taking into account the UPE
contribution: M=4.53 solar masses, Î±=0.54 (Moradi et al. 2021, Phys Rev D
104, 063043). The analysis of GRB 130427A applied to GRB 221009A gives for
the BH mass and spin parameters: M>2.36 solar masses and Î±<0.5.

We identify the spike at 500s as the X-ray flare (see e.g. Ruffini et al.
2021 MNRAS 504, 5301â€“5326 for similar GRBs). We also identify the trigger
in the 10 keV-10 MeV data of Fermi-GBM as the dawn of the supernova
(SN-rise), associated with the gravitational collapse of the progenitor
CO-core. The SN ejecta, accreting on the binary NS companion, give origin
to the BH (BH rise, Rueda & Ruffini 2012, ApJL, 758, L7) and accreting on
the vNS they originate the afterglow (vNS rise, Ruffini et al. 2018, ApJ,
869.101; Becerra, et al. 2022, Phys Rev D 106, 083002).

Additional data analysis from AGILE (GCN 32650), Fermi (GCN 32636, 32637,
32642, 32819), Swift (GCN 32635), LHAASO (GCN 32677), HXMT (Atel 15660) are
needed to relate the SN-rise to the first appearance of the vNS (the
vNS-rise) by the TeV radiation (GCN 32780, 32820, 32808), and also to
relate the appearance of the BH (BH-rise) to the identification of the
first GeV emission.


GRB_name: GRB221021A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32829
SUBJECT: GRB 221021A: Fermi GBM observation
DATE:    22/10/24 17:09:01 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico and INFN Bari) and
C. Meegan (UAH) report on behalf of the Fermi GBM Team:


"At 09:18:25.74 UT on 21 October 2022,
the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221021A
(trigger 688036710 / 221021388),
which was also detected by the Swift/BAT-GUANO
(Raman et al. 2022, GCN 32817).

The GBM position is reported in the Fermi-GBM
Final Real-time Localization (GCN 32812).
The angle from the Fermi LAT boresight
at the GBM trigger time is 132 degrees.

The GBM light curve shows a multipeaked emission
with a duration (T90) of about 68 s (50-300 keV).
The time-averaged spectrum from T0 to T0+60 s is
best fit by a power law function with an exponential
high-energy cutoff.
The power law index is -1.16 +/- 0.03 and the cutoff
energy, parameterized as Epeak, is 2000 +/- 210 keV.

The event fluence (10-1000 keV) in this time interval is
(3.06 +/- 0.07)E-05 erg/cm^2.
The 1-sec peak photon flux measured
starting from T0+34 s in the 10-1000 keV band
is 9.1 +/- 0.5 ph/s/cm^2.


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

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


GRB_name: GRB221022B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32830
SUBJECT: GRB 221022B: Fermi GBM detection
DATE:    22/10/24 17:28:04 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 22:55:48.91 UT on 22 October 2022, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 221022B (trigger 688172153 / 221022955, GCN 32820)
which was also detected by the Swift/BAT- GUANO (Raman et al. 2022, GCN
32823).

The angle from the Fermi LAT boresight at the GBM trigger time is 93
degrees.

The GBM light curve consists of a single peak followed
by some extended emission with a duration (T90) of about 32 s (50-300 keV).
The time-averaged spectrum from T0+7.17 s to T+46.08 s
is best fit by Band function, with Epeak = 265 +/- 6 keV,
alpha = -0.61 +/- 0.02 and beta = -2.61 +/- 0.10.

The event fluence (10-1000 keV) in this time interval is
(7.14 +/- 0.07)E-05  erg/cm^2. The 1-sec peak photon flux measured
starting from T0+22.3 s in the 10-1000 keV band
is 34.3 +/- 0.5 ph/s/cm^2.

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

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


GRB_name: GRB221023A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32831
SUBJECT: GRB 221023A: Fermi-LAT detection
DATE:    22/10/24 18:07:50 GMT
FROM:    Roberta Pillera at Politecnico and INFN Bari  <roberta.pillera@ba.infn.it>

GRB 221023A: Fermi-LAT detection

Pillera R. (Politecnico and INFN Bari), Cutini S. (INFN Perugia), Maheso 
D. (Johannesburg Univ.),
Cheung C. C. (Naval Research Laboratory), Bissaldi E. (Politecnico and 
INFN Bari),
Di Lalla N. (Stanford Univ.) and Khalil T. (Johannesburg Univ.) report 
on behalf of the Fermi-LAT team:

At 20:41:34.92 on October, 23, 2022 Fermi-LAT detected high-energy 
emission
from GRB 221023A, which was reported by AGILE (Ursi et al. GCN 32825) 
and GBM (GBM team 32826).


The best LAT on-ground location is found to be

RA, Dec =  230.30, 15.01 (J2000)

with an error radius of 0.04 deg (90 % containment, statistical error 
only).
This was 48 deg from the LAT boresight at the time of the trigger.

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


  The 100 MeV - 1 GeV photon flux in the time interval 0-1600 s after
the GBM trigger is (7.0 +/- 0.3)E-05 ph/cm2/s.
The estimated photon index above 100 MeV is -2.25 +/- 0.05.
The highest-energy photon is a 17 GeV event with 99% probability
which is observed 576 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.


The Fermi-LAT point of contact for this burst is
Dimakatso Jeannett Maheso (d.j.maheso@gmail.com).

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


GRB_name: GRB221022A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32833
SUBJECT: GRB 221022A: Swift ToO observations
DATE:    22/10/24 19:03:04 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 221022A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021530

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: GRB221022A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32834
SUBJECT: GRB 221022A: Fermi GBM detection
DATE:    22/10/24 21:35:01 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 19:33:33.55 UT on 22 October 2022, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 221022A (trigger 688160018 / 221022815, GCN 32816)
which was also detected by the Swift/BAT- GUANO (Tohuvavohu et al. 2022,
GCN 32824).
The Fermi GBM Final Real-time Localization is consistent
with the Swift-BAT GUANO position.

The angle from the Fermi LAT boresight at the GBM trigger time is 115
degrees.

The GBM light curve consists of a single peak followed
by some extended emission with a duration (T90) of about 7 s (50-300 keV).
The time-averaged spectrum from T0-3.07 s to T0 s
is best fit by a simple power law function with
index -1.39 +/- 0.15.

The event fluence (10-1000 keV) in this time interval is
(3.64 +/- 0.98)E-07  erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.6 s in the 10-1000 keV band
is 3.3 +/- 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: GRB221022B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32837
SUBJECT: GRB 221022B: AstroSat CZTI detection
DATE:    22/10/25 01:57:14 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

R. Gopalakrishnan (IUCAA), V. Prasad (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 221022B which was 
also detected by Fermi GBM (GCN 32820), AGILE (Casentini et al., GCN 
32822) and Swift/BAT-GUANO (Gayathri et al., GCN 32823).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-10-22 22:56:11.50 UTC. The measured peak count 
rate associated with the burst is 1613 (+72, -78) counts/s above the 
background in the combined data of all quadrants, with a total of 14862 
(+774, -850) counts. The local mean background count rate was 494 (+2, 
-3) counts/s. Using cumulative rates, we measure a T90 of 31 (+5, -4) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-10-22 
22:56:10.86 UTC. The measured peak count rate is 2187 (+97, -105) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 18217 (+1046, -1027) counts. The local mean 
background count rate was 1575 (+3, -4) counts/s. We measure a T90 of 27 
(+4, -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: GRB221024A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32838
SUBJECT: GRB 221024A: D50 candidate afterglow
DATE:    22/10/25 04:28:46 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Jan Strobl, Martin Jelinek, Rene Hudec, Cyril Polasek
Astronomical Institute of the Academy of Sciences (ASU CAS), Ondrejov

report

With the 0.5m robotic telescope located in Ondrejov, we observed the
position of the Swift rigger 1131029 or GRB 221024A (Brivio et al, 32827),
starting at October 25, 3:18UT, i.e. 14.25h post GRB. In the series of
unfiltered 60s exposures, we detect an uncatalogued source inside the XRT
error box. The preliminary magnitude of this source is ~19.1+-0.1, the
photometry is complicated by the presence of the star nu UMa in the
proximity of the field.


GRB_name: GRB221024A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32839
SUBJECT: GRB 221024A: Enhanced Swift-XRT position
DATE:    22/10/25 06:08:21 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 3710 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 221024A, 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 = 169.74062, +33.04199 which is equivalent
to:

RA (J2000): 11h 18m 57.75s
Dec (J2000): +33d 02' 31.2"

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: GRB221024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32841
SUBJECT: GRB 221024A: GIT confirmation of the optical afterglow
DATE:    22/10/25 09:04:49 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

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

We observed GRB 221024A detected by Swift-BAT (R. Brivio et al., GCN
#32827) with 0.7m GROWTH-India Telescope (GIT). We obtained multiple 300s
exposures in the r' filter and clearly detected the afterglow in our image
at R.A.= 11:18:57.78  DEC = +33:02:30.64. The photometric results follow as:

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

JD (Start) | T_Start-T0(hrs) | Filter | Magnitude (AB) |

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

2459877.42179 |  9.12 | r' | 18.36 +/- 0.05 |

2459877.45883 | 10.00 | r' | 18.50 +/- 0.1 |

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

GIT photometry and results from Jan Strobl et al. (GCN #32838) conclude
that the source is fading and is an afterglow of GRB 221024A. 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
<https://iopscience.iop.org/article/10.3847/1538-3881/ac7bea>) 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: GRB221022B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32842
SUBJECT: IPN triangulation of GRB 221022B (long)
DATE:    22/10/25 11:38:41 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

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

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

and

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

The long-duration GRB 221022B
(Fermi/GBM detection: Fermi GBM team, GCN 32820;
Poolakkil & Meegan, GCN 32830;
AGILE detection: Casentini et al., GCN 32822;
Swift/BAT-GUANO detection: Raman et al., GCN 32823;
AstroSat CZTI detection: Gopalakrishnan et al., GCN 32837)
has been detected by Fermi (GBM), INTEGRAL (SPI-ACS),
Konus-Wind, AGILE (MCAL, AC), AstroSat (CZTI) and
Swift (BAT), so far, at about 82549 s UT (22:55:49).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  170.477 (11h 21m 55s) +18.413 (+18d 24' 46")
 Corners:
  179.823 (11h 59m 18s) +26.613 (+26d 36' 46")
  161.965 (10h 47m 52s) +10.411 (+10d 24' 38")
  164.336 (10h 57m 21s)  +9.908 ( +9d 54' 28")
  183.830 (12h 15m 19s) +26.171 (+26d 10' 14")
 ---------------------------------------------
The error box area is 52.5 sq. deg, and its maximum
dimension is 26.0 deg (the minimum one is 2.2 deg).
The Sun distance was 43 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM final localization (GCN 32820).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221022_T82557/IPN

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


GRB_name: GRB221025A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32843
SUBJECT: GRB 221025A: Fermi-LAT detection
DATE:    22/10/25 11:43:09 GMT
FROM:    Makoto Arimoto at Tokyo Inst of Tech  <arimoto@hp.phys.titech.ac.jp>

Arimoto M. (Kanazawa University) Pillera R. (Politecnico and INFN
Bari), and Maheso D. (Johannesburg Univ.) report on behalf of the
Fermi-LAT team:

At 00:58:18.42 on October, 25, 2022 Fermi-LAT detected high-energy emission
from GRB 221025A, GBM trigger 221025041 / 688352303 at 00:58:18.42 UT.

The best LAT on-ground location is found to be

RA, Dec =  133.4, 11.0 (J2000)

with an error radius of 1.3 deg (90 % containment, statistical error only).
This was 45 deg from the LAT boresight at the time of the trigger.

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


The 100 MeV - 1 GeV photon flux in the time interval 0-200 s after
the GBM trigger is (2.1 +/- 0.6)E-05 ph/cm2/s.
The estimated integrated photon index above 100 MeV is -2.3 +/- 0.3.
The highest-energy photon is a 1.3 GeV event with 93% probability
which is observed 3 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.


The Fermi-LAT point of contact for this burst is
Dimakatso Jeannett Maheso (d.j.maheso@gmail.com).

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


GRB_name: GRB221022B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32844
SUBJECT: GRB 221022B: Detection by GRBAlpha
DATE:    22/10/25 12:53:55 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), F. Munz, N. Husarikova, J.-P. Breuer, M. Topinka, 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 Metropo
 litan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The long-duration GRB 221022B (Fermi/GBM detection: GCN Circ. 32820; AGILE/MCAL detection: Casentini et al., GCN Circ. 32822; Swift/BAT detection: Raman et al., GCN Circ. 32823; ASTROSAT/CZTI detection: Gopalakrishnan et al. GCN Circ. 32837; Konus/Wind trigger at 2022-10-22 22:55:57 UT; INTEGRAL/SPI-ACS detection at 2022-10-22 22:56:13 UT) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The 23 sigma detection was confirmed at the peak time 2022-10-22 22:56:11.8 UTC. The GRB has a T90 duration of 32 s.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221022B_GCN.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously upgrading the on-board data acquisition software stack. 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: GRB221023A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32845
SUBJECT: GRB 221023A: Fermi GBM Observation
DATE:    22/10/25 14:16:07 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 20:41:34.92 UT on 23 October 2022, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 221023A (trigger 688250499 / 221023862),
this localisation was consistent with the Fermi LAT (GCN 32813). This event
was also observed by AGILE (GCN 32825).

The angle from the Fermi LAT boresight is 48 degrees.

The GBM light curve shows one bright peak with a duration (T90) of about 39
s (50-300 keV). The time-averaged spectrum from T0-2 to T0+58 s is best fit
by a Band function with Epeak = 898 +/- 15 keV, alpha = -1.1 +/- 0.004, and
beta = -2.5 +/- 0.03. It is fit equally well with a power law function with
an exponential high-energy cutoff. The power law index is -1.08 +/- 0.003
and the cutoff energy, parameterized as Epeak, is 997 +/- 14 keV.

The event fluence (10-1000 keV) in this time interval is 0.001 +/-
4.350E-06 erg/cm2. The 1-sec peak photon flux measured starting from T0+20
s in the 10-1000 keV band is 60.9 +/- 0.4 ph/s/cm2.

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: GRB221024A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32846
SUBJECT: GRB 221024A: Swift-XRT refined Analysis
DATE:    22/10/25 14:30:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.0 ks of XRT data for GRB 221024A (Brivio et al. GCN
Circ. 32827), from 114 s to 52.5 ks after the  BAT trigger. The data
comprise 248 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 Osborne et
al. (GCN Circ. 32839).

The late-time light curve (from T0+11.3 ks) can be modelled with a
power-law decay with a decay index of alpha=1.61 (+0.20, -0.21).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.53 (+/-0.04). The
best-fitting absorption column is  5.4 (+/-1.1) x 10^20 cm^-2, in
excess of the Galactic value of 2.9 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.96 (+0.14, -0.13)
and a best-fitting absorption column of 6.0 (+3.2, -2.9) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.3 x 10^-11 (3.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.0 (+3.2, -2.9) x 10^20 cm^-2
Galactic foreground: 2.9 x 10^20 cm^-2
Excess significance: 1.7 sigma
Photon index:      1.96 (+0.14, -0.13)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01131029.

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


GRB_name: GRB221022A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32847
SUBJECT: GRB 221022A: Swift-XRT observations
DATE:    22/10/25 14:45:14 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), E. Ambrosi  (INAF-IASFPA) , M. Capalbi
(INAF-IASFPA), M. Perri (SSDC & INAF-OAR), S. Dichiara (PSU), J.A.
Kennea (PSU), A. Tohuvavohu (U. Toronto), K.L. Page (U. Leicester),
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 221022A (Aaron Tohuvavohu et al. GCN
Circ. 32824), collecting 3.8 ks of Photon Counting (PC) mode data
between T0+170.9 ks and T0+184.2 ks. 

Six uncatalogued X-ray sources have been detected, however none of them
is above the RASS limit or shows definitive signs of fading. None of
the six is inside the GUANO error region. 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):  118.4349  =  07:53:44.38
  Dec (J2000): -5.2165  =  -05:12:59.3
  Error: 7.7 arcsec (radius, 90% conf.)
  Count-rate: (3.1 [+1.5, -1.2])e-3 ct s^-1   
  Distance: 489 arcsec from Swift/BAT-GUANO position.

Source 2:
  RA (J2000):  118.3560  =  07:53:25.45
  Dec (J2000): -5.2797  =  -05:16:47.0
  Error: 5.3 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (4.3 [+1.7, -1.4])e-3 ct s^-1   
  Distance: 588 arcsec from Swift/BAT-GUANO position.
  Flux: (1.12 [+0.45, -0.36])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 3:
  RA (J2000):  118.2368  =  07:52:56.83
  Dec (J2000): -5.2703  =  -05:16:13.1
  Error: 6.1 arcsec (radius, 90% conf.)
  Count-rate: (4.2 [+1.8, -1.4])e-3 ct s^-1   
  Distance: 668 arcsec from Swift/BAT-GUANO position.
  Flux: (2.14 [+0.91, -0.72])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 4:
  RA (J2000):  118.4804  =  07:53:55.29
  Dec (J2000): -5.1253  =  -05:07:31.0
  Error: 6.9 arcsec (radius, 90% conf.)
  Count-rate: (1.65 [+1.13, -0.80])e-3 ct s^-1  
  Distance: 497 arcsec from Swift/BAT-GUANO position.

Source 5:
  RA (J2000):  118.1854  =  07:52:44.49
  Dec (J2000): -5.2601  =  -05:15:36.4
  Error: 4.1 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (5.9 [+2.1, -1.7])e-3 ct s^-1   
  Distance: 761 arcsec from Swift/BAT-GUANO position.
  Flux: (2.22 [+0.79, -0.64])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 6:
  RA (J2000):  118.3078  =  07:53:13.87
  Dec (J2000): -5.2740  =  -05:16:26.4
  Error: 6.6 arcsec (radius, 90% conf.)
  Count-rate: (5.0 [+2.4, -1.8])e-3 ct s^-1   
  Distance: 578 arcsec from Swift/BAT-GUANO position.
  Flux: (1.01 [+0.47, -0.37])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/00021530.

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


GRB_name: GRB221024A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32848
SUBJECT: GRB 221024A: Swift/UVOT UV upper limits
DATE:    22/10/25 14:54:44 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin and R. Brivio report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB221024A
127 seconds after the BAT trigger (Brivio et al., GCN Circ. 32827).
The UVOT could not observe in the u,b,v or white filters due to the
nearby bright star nu uMa (V=3.49, U=6.44).  A source detection has
been reported by Strobl et al. (GCN Circ. 32838) and by Swain et al.
(GCN Circ. 32841) with r' = 18.36 at 9.12 hours after the Trigger.

UVOT obtained images in uvw1, uvm2 and uvw2. Visual inspection shows
no credible source in the initial images with upper limits of 19.7 mag.

In the uvm2 filter which has no red leak we obtained deeper limits:

filter   tstart(s)   tstop(s) exposure 3-sigma UL
uvm2     23992       36065      609      >21.3
uvm2     51885       52503     3306      >20.3

The limits in the UV are about 3 mag. below the reported detections
in r', which may suggest a redshift larger than 1.5.

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221023A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32849
SUBJECT: Konus-Wind detection of GRB 221023A
DATE:    22/10/25 15:49:28 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The long-duration GRB 221023A
(AGILE detection: Ursi et al., GCN 32825;
Fermi-GBM observation: Fermi GBM team, GCN 32826;
Dunwoody et al., GCN 32845;
Fermi-LAT detection: Pillera et al., GCN 32831)
triggered Konus-Wind at T0=74492.216 s UT (20:41:32.216).

The burst light curve shows a multipeaked structure,
which starts at ~T0-0.5 s and has a total duration of ~145.9 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/GRB221023_T74492/

As observed by Konus-Wind, the burst
had a fluence of 6.60(-0.35,+0.35)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+18.928 s,
of 3.84(-0.52,+0.52)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+149.248 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.05(-0.03,+0.03),
the high energy photon index beta = -2.27(-0.17,+0.13),
the peak energy Ep = 760(-64,+68) keV
(chi2 = 128/98 dof).

The spectrum near the maximum count rate
(measured from T0+18.688 to T0+19.200 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.66(-0.12,+0.15),
the high energy photon index beta = -2.32(-0.41,+0.22),
the peak energy Ep = 707(-147,+184) keV
(chi2 = 47/55 dof).

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


GRB_name: GRB221009A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32850
SUBJECT: GRB 221009A: spectroscopic confirmation of SN in LBT spectra
DATE:    22/10/25 16:50:09 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

E. Maiorano, E. Palazzi, A. Rossi (INAF-OAS), V. D'Elia (SSDC & 
INAF-OAR), and A. Melandri (INAF-OAR) on behalf of the CIBO 
collaboration, and F. Cusano (INAF-OAS), L. Izzo (DARK/NBI) report:

We report the results of the spectroscopic follow-up observations of the 
afterglow of GRB 221009A (Dichiara et al., GCN 32632; Fermi GBM 
detection: Veres et al., GCN 32636). The optical spectra were obtained 
with the Multi-Object Double Spectrographs (MODS) instrument mounted on 
the 2x8.4-m LBT telescope (Mt. Graham, AZ, USA) at 3 UT on 2022-10-18, 
8.56 days after the burst trigger. The spectra cover the wavelength 
range 3200-10000 AA, and we obtained a total of 6 exposures of 900 s.

After correction for the foreground Galactic extinction (E(B-V)=1.324, 
Schlafly & Finkbeiner 2011), we find that the resulting spectrum is 
clearly dominated by the afterglow. We subtracted the afterglow 
contribution assuming a spectral slope -0.7 (using the convention F_nu ~ 
nu^-beta), anchored to the simultaneous NIR flux. This value has been 
obtained modeling the NIR light curve of the afterglow (Ferro et al., 
GCN 32804; D'Avanzo et al., GCN 32755). The remaining low S/N spectrum 
shows features typical of type Ic-BL supernovae. Therefore, we confirm 
the emerging contribution of SN 2022xiw (de Ugarte Postigo et al. et al. 
TNSCR, 2022-3047) as reported by de Ugarte Postigo et al. (GCN 32800).

We acknowledge the excellent support from the LBTO and LBT-INAF staff, 
particularly A. Becker and D. G. Huerta, in obtaining these observations.


GRB_name: GRB221025A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32851
SUBJECT: GRB 221025A: Fermi GBM Observation
DATE:    22/10/25 16:52:20 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

J. Wood (NASA/MSFC) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:

"At 00:58:18 UT on 25 October 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 221025A (trigger 688352303 / 221025040).
which was also detected by Fermi-LAT (Arimoto M. et al. 2022, GCN 32843).
The Fermi GBM on-ground location is consistent with the Fermi-LAT position.

The on-ground calculated location, using the GBM trigger
data, is RA = 128.9, DEC = +2.2 (J2000 degrees,
equivalent to 08h 36m, +02d 12'), with an uncertainty
of 6.8 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32]).

The angle from the Fermi LAT boresight is 48.5 degrees.

The GBM light curve consists of a single pulse with a duration (T90)
of about 0.4 s (50-300 keV). The time-averaged spectrum
from T0+0.0 to T0+0.8 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.4 +/- 0.1 and the cutoff energy,
parameterized as Epeak, is 1680 +/- 345 keV.

The event fluence (10-1000 keV) in this time interval is
(1.7 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.3 s in the 10-1000 keV band is 13.3 +/- 0.9 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: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32852
SUBJECT: GRB 221009A: SARA-RM 1m Optical Afterglow Detection
DATE:    22/10/26 03:04:37 GMT
FROM:    Kyle Pellegrin at Clemson University  <pelleg2@g.clemson.edu>

K. Pellegrin, K. Rumstay, and D. Hartmann report:


We observed the field of GRB 221009A detected by Swift(Kennea & Williams,
GCN 32635; Veres et al., GCN 32636) Swift BAT (Dichiara et al., GCN 32632),
Fermi LAT (Bissaldi, GCN 32637), Liverpool Telescope (Perley, GCN 32638),
Vereniging Voor Sterrenkunde (Broens, GCN 32640), IPN (Svinkin, GCN 32641),
BOOTES-2/TELMA (Hu et al., GCN 32644), Mondy (Belkin, GCN 32645), MeerLICHT
(Wet et al., GCN 32646), Nanshan/NEXT (Xu et al., GCN 32647), ESO X-shooter
(de Ugarte Postigo, GCN 32648), Al Khatim Observatory M44 (Odeh, GCN 32649
& GCN 32666), AGILE/MCAL (Ursi et al, GCN 32650), REM (Brivio et al., GCN
32652), AMI-LA (Bright et al., GCN 32653), SAAO (Durbak et al., GCN 32654),
ATA (Farah et al., GCN 32655), Swift UVOT (Kuin and Dichiara, GCN 32656),
AGILE/GRID (Piano et al., GCN 32657), LOAO (Paek et al., GCN 32659),
INTEGRAL SPI/ACS (Gotz et al., GCN 32660), GIT (Kumar et al., GCN 32662),
Burke-Gaffney Observatory (Romanov, GCN 32664), SLT-40cm (Chen et al., GCN
32667), Lick/Nickel Telescope (Vidal et al., GCN 32669), Assy (Kim et al.,
GCN 32670 & Belkin et al., GCN 32769), Global MASTER-Net (Lipunov et al.
GCN 32672 & GCN 32673), BlackGEM (Groot et al., GCN 32678), iTelescope
(Romanov, GCN 32679), Sintez-Newton/ CrAO (Belkin et al., GCN 32684),
COATLI (Watson et al. GCN 32692), LCOGT (Strausbaugh et al., GCN 32693 &
GCN 32738), COATLI (Butler et al., GCN 32705), Konkoly Observatory (Vinko
et al., GCN 32709), GMG (Mao et al., GCN 32727), Sayan Observatory
(Zaznobin et al., GCN 32729), MITSuME Okayama (Sasada et al., GCN 32730),
Lowell Discovery Telescope (Oâ€™Connor et al., GCN 32739 & GCN 32799),
RTT-150 (Bikmaev et al., GCN 32743 & GCN 32752), Gemini-South (Rastinejab
and Fong, GCN 32749), Gemini-South (Oâ€™Connor et al., GCN 32750), OHP
(Schneider et al., GCN 32753), REM (Dâ€™Avanzo et al., GCN 32755), Pan-STARRS
(Huber et al., GCN 32758), Large Binocular Telescope (Shrestha et al., GCN
32759), Faulkes Telescope North (Shrestha et al., GCN 32771), GRANDMA
(Rajabov et al., GCN 32795), BOAO (Im et al., GCN 32803), TNG (Ferro et
al., GCN 32804), LBT (Rossi et al., GCN 32809), DFOT (Gupta et al., GCN
32811), AZT-20 (Belkin et al., GCN 32818), and James Webb (Levan et al.,
GCN 32821) using the SARA 1m optical telescope located at the Roque de los
Muchachos Observatory on La Palma, Canary Islands, Spain, equipped with the
Andor Ikon-L camera.



Observations started at 20:50:13 UTC on 2022-10-23 and ended at 22:29:27
UTC on 2022-10-23. We obtained a series of 90 images with an exposure time
of 60s each in the Johnson-Cousins R filter. The afterglow is faintly seen
after stacking all 90 images together. Photometry on the stacked image
found the afterglow to be R=22.19 +/= 0.07 mag at 14.90190 days (midpoint
of stacked observations) after the Swift trigger (GCN 32632).



Photometry based on the PanSTARRS catalog.



The Southeastern Association for Research in Astronomy (SARA) consortium

operates three telescopes: the 0.9-m SARA-KP at Kitt Peak in Arizona,

the 0.6-m SARA-CT at Cerro Tololo in Chile, and the 1.0-m SARA-RM (formerly

the JKT) telescope at Roque de los Muchachos Observatory in the Canary

Islands. For more information see: Keel et al. (2016):

https://iopscience.iop.org/article/10.1088/1538-3873/129/971/015002


GRB_name: GRB221025A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32853
SUBJECT: GRB 221025A: AstroSat CZTI detection
DATE:    22/10/26 13:42:23 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 CIFT framework (Sharma et al., 
2021, JApA, 42, 73) showed the detection of a short GRB 221025A which 
was also detected by Fermi-GBM (Wood et al,. GCN 32851) and Fermi-LAT 
(Arimoto et al,. GCN 32843).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-10-25 00:58:18.6 UTC. The measured peak count 
rate associated with the burst is 904 (+212, -102) counts/s above the 
background in the combined data of all quadrants, with a total of 313 
(+62, -63) counts. The local mean background count rate was 435 (+8, 
-12) counts/s. Using cumulative rates, we measure a T90 of 0.45 (+0.6, 
-0.2) s.

It was also detected in the CsI anticoincidence (Veto) detector in the 
100-500 keV energy range. Due to the intrinsic 1 s binning of veto data, 
we cannot reliably estimate a T90 from it.

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: GRB221024A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32854
SUBJECT: GRB 221024A: Swift-BAT refined analysis
DATE:    22/10/26 14:47:54 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC), R. Brivio (INAF-OAB),
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 221024A (trigger #1131029)
(Brivio, et al., GCN Circ. 32827).  The BAT ground-calculated position is
RA, Dec = 169.702, 33.068 deg which is
   RA(J2000)  =  11h 18m 48.6s
   Dec(J2000) = +33d 04' 04.9"
with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.

The mask-weighted light curve shows a rather weak pulse starting at the trigger
time, peaking around T+5 seconds and decaying to baseline by about T+40 seconds.
There is some low-level emission following this peak, including a possible peak
In the low-energy bands at approximately T+200 seconds. The pipeline-calculated
T90 (15-350 keV) is 120+-111 sec (estimated error including systematics), with the
large stated error due to uncertainty in whether the possible T+200 peak contains
at least 5% of the burst fluence.

The time-averaged spectrum from T+0.00 to T+221.28 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.39 +- 0.25.  The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.93 sec in the 15-150 keV band
is 1.5 +- 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/1131029/BA/


GRB_name: GRB221023A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32856
SUBJECT: GRB 221023A: AGILE/GRID analysis
DATE:    22/10/26 15:16:15 GMT
FROM:    Francesco Verrecchia at SSDC,INAF-OAR  <francesco.verrecchia@ssdc.asi.it>

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

The Gamma-Ray Imaging Detector (GRID) of AGILE detected gamma-ray
transient emission consistent with the long GRB 221023A reported
by AGILE/MCAL (GCN #32825) at T0 = 2022-10-23 20:41:34 s (UTC), also
detected by Fermi/GBM (GCN #32826, #32845), Fermi/LAT (GCN #82831)
and Konus-Wind (GCN #32849).
A refined AGILE/GRID data analysis in the energy range 30 MeV - 10 GeV
shows a detection with a statistical significance of about 4.3 sigma
overa time integration of 50 s starting at the T0 of GRB 221023A,
at a sky position with Galactic coordinates l=28 deg, b=53 deg, with
and an error radius of 4 deg (90% statistical + systematic error;
R.A.= 232 deg, Decl.= 19 deg (J2000)).
The GRID error circle includes the LAT position.
During the 120s integration, we detected a total of 22 events (11
background events estimated through a Li&Ma analysis), 16 events at
energies above 100 MeV, and 2 events above 1 GeV.

These measurements were obtained with AGILE observing a large portion
of the sky in spinning mode. Additional analysis of AGILE data is in
progress.


GRB_name: GRB221022C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32857
SUBJECT: IPN triangulation of GRB 221022C (short)
DATE:    22/10/26 17:33:29 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

A. 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

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

The short-duration GRB 221022C
(Fermi-GBM detection: Poolakkil and Meegan, GCN Circ. 32836)
was detected by Fermi (GBM trigger 688142511), INTEGRAL (SPI-ACS),
Konus-Wind, and Swift (BAT) at about 52906 s UT (14:41:46).
The burst was outside the coded field of view of the BAT.

We have triangulated it to two preliminary, 3 sigma error boxes
whose coordinates are:

Box 1:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   231.382 (15h 25m 32s) -57.938 (-57d 56' 16")
  Corners:
   234.870 (15h 39m 29s) -56.438 (-56d 26' 17")
   235.716 (15h 42m 52s) -56.321 (-56d 19' 17")
   226.200 (15h 04m 48s) -59.592 (-59d 35' 33")
   224.388 (14h 57m 33s) -59.790 (-59d 47' 25")
  ---------------------------------------------

Box 2:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   193.697 (12h 54m 47s) -60.774 (-60d 46' 28")
  Corners:
   189.204 (12h 36m 49s) -59.842 (-59d 50' 33")
   188.243 (12h 32m 58s) -59.852 (-59d 51' 09")
   200.024 (13h 20m 06s) -61.584 (-61d 35' 03")
   201.980 (13h 27m 55s) -61.500 (-61d 29' 58")
  ---------------------------------------------
The error box area is 1.28 sq. deg, and their maximum
dimension is 6.91 deg (the minimum one is 12.4 arcmin).
The Sun distance was 50 deg.

This localization may be improved.

The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM final localization (glg_healpix_all_bn221022612_v00).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221022_T52903/IPN

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


GRB_name: GRB221024A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32859
SUBJECT: GRB 221024A: GRANDMA observations
DATE:    22/10/26 21:06:19 GMT
FROM:    Cristina Andrade at UMN  <andra104@umn.edu>

C. Andrade (UMN), A. Iskandar (XAO), A. Klotz (IRAP-OMP), H. Peng (THU),
T. Sadibekova (AIM-CEA), M.Trevor (UMD), M. Freeberg (KNC),
D. Turpin (CEA), S. Antier (OCA/Artemis), A. Benkhaldoun (HAO),
S. Alishov(ShAO), E. Gurbanov(ShAO), E. Hesenov (ShAO), A. Kaeouach (HAO),
N. Kochiashvili (ShAO) K. Noysena (TRT), F.Guo(THU), Y.Rajabov (UBAI),
N. Sasaki (OPD), Z. Vidadi (ShAO),
report  on behalf of the GRANDMA collaboration:

The GRANDMA telescope network responded to the Swift-BAT alert of
GRB 221024A (R. Brivio et al., GCN 32827, J.P. Osborne et al. GCN 32839,
M. Capalbi et al. GCN 32846, A. Y. Lien et al. GCN 32854),
which is also detected by  Fermi (J. Wood et al. GCN 32835).

The first observations started 22 hours after the BAT trigger time.
The afterglow was reported detected within
the XRT enhanced error region by different teams: J. Strobl et al.
(GCN 32838) D50-telescope from ASU CAS; V. Swain et al. (GCN 32841)
0.7m GROWTH India Telescope; including UVOT observations and
N. P. M. Kuin et al. (GCN 32848).

In the following table we report the preliminary photometry of our
observations. Upper limits are reported at the 5-sigma limit,
in the AB system.

T-T0 (hr)|    MJD    |  Observatory| Filter    | Upp.Mag.
____________________________________________________
22.11   |59877.463197| KNC-NMSkies | ps1/r     | 19.7

Most of the sites were limited by the sky visibility and the weather
conditions. There is also light pollution from the nearby bright star
(Nu UMa, apparent mag (V) +3.490) located at ~6' from the XRT position.
Only one observation was successfully performed in the context of the
Kilonova-Catcher programme (KNC), a professional-amateur collaboration
within the GRANDMA project, by the T21 New Mexico skies iTelescope using
filter ps1/r. The KNC image have been processed using the STDpipe and
photometry was performed using field stars from the PanSTARRS1-r catalogue
as reference.


GRANDMA is a worldwide coordinated telescope network
(grandma.ijclab.in2p3.fr)  devoted to the observation of transients
in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS
497, 5518). Kilonova-Catcher (KNC) is the citizen science program of
GRANDMA (http://kilonovacatcher.in2p3.fr/).


GRB_name: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32860
SUBJECT: GRB 221009A: Further Gemini-South Infrared Observations
DATE:    22/10/27 01:33:55 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), E. Troja (UTV/ASU), S. Dichiara (PSU),
J. Gillanders (UTV), S. B. Cenko (NASA/GSFC):

We performed target of opportunity observations of GRB 221009A
(Dichiara et al., GCN 32632, Veres et al., GCN 32636)
with the FLAMINGOS-2 spectrograph mounted on the Gemini-South
telescope. Observations began on October 26, 2022 at 23:40:44 UT
corresponding to ~17.4 d after the GRB. We obtained images in
JHK with a total exposure of 75 s in each filter.

The afterglow is clearly detected in each filter. We obtain
the following magnitudes calibrated against the 2MASS catalog:

J = 20.1 +/- 0.2 AB mag
H = 19.43 +/- 0.15 AB mag
K = 18.94 +/- 0.08 AB mag

These magnitudes are not corrected for Galactic extinction.

Further infrared observations are planned.

We acknowledge the staff of the Gemini Observatory for assistance
with these observations.


GRB_name: GRB221027A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32861
SUBJECT: GRB 221027A: Fermi GBM Final Real-time Localization
DATE:    22/10/27 04:21:08 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:09:34 UT on 27 Oct 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221027A (trigger 688536579.352978 / 221027173).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 189.4, Dec = -10.0 (J2000 degrees, equivalent to J2000 12h 37m, -10d 00'), with a statistical uncertainty of 1.9 degrees.

The angle from the Fermi LAT boresight is 52.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221027173/quicklook/glg_skymap_all_bn221027173.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/bn221027173/quicklook/glg_healpix_all_bn221027173.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221027173/quicklook/glg_lc_medres34_bn221027173.gif


GRB_name: GRB221027A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32862
SUBJECT: GRB 221027A: Fermi-LAT detection
DATE:    22/10/27 10:28:51 GMT
FROM:    Makoto Arimoto at Tokyo Inst of Tech  <arimoto@hp.phys.titech.ac.jp>

Arimoto M. (Kanazawa University), Bissaldi E. (Politecnico and INFN Bari),
Longo F. (University and INFN Trieste), Scotton L. (CNRS/IN2P3/LUPM)
and Maheso D. (Johannesburg Univ.) report on behalf of the Fermi-LAT
team:

On October, 27, 2022 Fermi-LAT detected high-energy emission from GRB 221027A,
which was also detected by Fermi-GBM (trigger 221027173 / 688536579,
GCN 32861) at 04:09:34.35 UT .

The best LAT on-ground location is found to be

RA, Dec =  185.3, -5.7 (J2000)

with an error radius of 0.4 deg (90 % containment, statistical error only).
This was 51 deg from the LAT boresight at the time of the trigger.

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


The 100 MeV - 1 GeV photon flux in the time interval 0-500 s after
the GBM trigger is (9.1 +/- 2.6)E-06 ph/cm2/s.
The estimated integrated photon index above 100 MeV is -2.2 +/- 0.3.
The highest-energy photon is a 1.1 GeV event with 96% probability
which is observed 26 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.


The Fermi-LAT point of contact for this burst is
Dimakatso Jeannett Maheso (d.j.maheso@gmail.com).

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


GRB_name: GRB221024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32863
SUBJECT: GRB 221024A: Mondy optical observations
DATE:    22/10/27 12:17:13 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), N. Pankov (HSE) report on behalf of IKI-GRB-FuN:
 
We observed the field of GRB 221024A (Swift: Brivio et al., GCN 32827; Fermi: J. Wood et al. GCN 32835 ) with AZT-33IK telescope of Mondy observatory  starting on Oct. 26 (UT) 21:03:08. In the stacked image we detected the optical counterpart (Strobl et al., GCN 32838, Swain et al., GCN 32841, Andrade et al., GCN 32859) in coordinates (J2000) 11:18:57.58,  +33:02:32.1 with uncertainities of 0.14 arcsec in both coordinates. The position of the optical counterpart is 2.3" apart from the center and within of the enhanced XRT position (Osborne et al., GCN 32839). Preliminary photometry of the field is following.
 
Date       UT start t-T0 Filter Exp. OT Err. UL(3sigma)
                    (mid, days) (s)
 
2022-10-26 21:03:08 2.35534 R 29*120 21.0 0.1 22.5
 
Photometry is based on the USNO-B2.0 nearby stars.
USNO-B1.0
RA DEC R2
11:18:51.3907200 +32:59:13.401600 16.52
11:19:04.3800000 +32:58:07.082400 17.00


GRB_name: GRB221022B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32864
SUBJECT: Konus-Wind detection of GRB 221022B
DATE:    22/10/27 12:40:54 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The long-duration GRB 221022B
(Fermi/GBM detection: Fermi GBM team, GCN 32820;
Poolakkil & Meegan, GCN 32830;
AGILE detection: Casentini et al., GCN 32822;
Swift/BAT-GUANO detection: Raman et al., GCN 32823;
AstroSat CZTI detection: Gopalakrishnan et al., GCN 32837;
IPN triangulation: Ridnaia et al., GCN 32842;
GRBAlpha detection: Dafcikova et al., GCN 32844)
triggered Konus-Wind at T0=82557.097 s UT (22:55:57.097).

The burst light curve shows a multipeaked structure
which starts at ~T0-12.1 s and has a total duration of ~51.9 s.
The emission is seen up to ~4 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB221022_T82557/

As observed by Konus-Wind, the burst
had a fluence of 8.19(-0.62,+0.67)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+11.984 s,
of 1.57(-0.24,+0.24)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0+8.448 to T0+43.776 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.68(-0.11,+0.12),
the high energy photon index beta = -2.69(-0.42,+0.23),
the peak energy Ep = 268(-21,+23) keV
(chi2 = 114/98 dof).

The spectrum near the maximum count rate
(measured from T0+8.448 to T0+12.800 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.30(-0.13,+0.15),
the high energy photon index beta = -2.60(-0.24,+0.17),
the peak energy Ep = 299(-24,+27) keV
(chi2 = 104/78 dof).

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


GRB_name: GRB221025A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32865
SUBJECT: IPN triangulation of GRB 221025A (short)
DATE:    22/10/27 14:34:24 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

A. 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,
report:

The short-duration GRB 221025A
(Fermi-LAT detection: Arimoto et al., GCN Circ. 32843;
Fermi-GBM detection: Wood and Meegan, GCN Circ. 32851;
AstroSat-CZTI detection: Gopalakrishnan et al., GCN Circ. 32853)
was detected by Fermi (GBM trigger 688352303), INTEGRAL (SPI-ACS),
Konus-Wind, AstroSat (CZTI), and GECAM-B (trigger tn221025_005818_fb)
at about 3498 s UT (00:58:18).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   134.373 (08h 57m 29s) +13.068 (+13d 04' 07")
  Corners:
   133.601 (08h 54m 24s) +10.772 (+10d 46' 20")
   133.259 (08h 53m 02s) +10.806 (+10d 48' 20")
   135.172 (09h 00m 41s) +15.363 (+15d 21' 46")
   135.522 (09h 02m 05s) +15.330 (+15d 19' 48")
  ---------------------------------------------
The error box area is 1.6 sq. deg, and its maximum
dimension is 5.03 deg (the minimum one is 19.44 arcmin).
The Sun distance was 78 deg.

This localization may be improved.

The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM final localization (glg_healpix_all_bn221025040_v00).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221025_T03498/IPN/

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


GRB_name: GRB221027A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32866
SUBJECT: GRB 221027A: Fermi GBM detection
DATE:    22/10/27 14:45:08 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

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

"At 04:09:34.35 UT on 27 October 2022, the Fermi
Gamma-Ray Burst Monitor (GBM) triggered and located
GRB 221027A (trigger 688536579 / 221027173), which was
also detected by Fermi-LAT (M. Arimoto et al. 2022, GCN 32862).

The Fermi GBM Final Real-time Localization (GCN 32861) is
consistent with the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger
time is 51 degrees.

The GBM light curve consists of a bright pulse
with a duration (T90) of about 7 s (50-300 keV).
The time-averaged spectrum from T0-1.5s to T0+9.7 s is
best fit by a Band function with Epeak = 341 +/- 37 keV,
alpha = -0.75 +/- 0.06, and beta = -2.09 +/- 0.14.

The event fluence (10-1000 keV) in this time interval is
(9.2 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+1.2 s in the 10-1000 keV band
is 8.5 +/- 0.3 ph/s/cm^2.

A power law function with an exponential high-energy cutoff
fits the spectrum equally well. The power law index
is -0.81 +/- 0.04 and the cutoff energy, parameterized as
Epeak, is 411 +/- 29 keV

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: GRB221027B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32867
SUBJECT: GRB 221027B: Swift detection of a burst
DATE:    22/10/27 19:32:47 GMT
FROM:    Jamie Kennea at Penn State U  <jak51@psu.edu>

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

At 19:13:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221027B (trigger=1131397).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 225.603, +47.448 which is 
   RA(J2000) = 15h 02m 25s
   Dec(J2000) = +47d 26' 53"
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 15 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 19:15:44.9 UT, 126.2 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 225.62105,
47.44193 which is equivalent to:
   RA(J2000)  = 15h 02m 29.05s
   Dec(J2000) = +47d 26' 30.9"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 49 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.88 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.4
(+1.76/-1.55) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 130 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 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
0.033. 

Burst Advocate for this burst is A. Y. Lien (yarleen 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: GRB221027B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32868
SUBJECT: GRB 221027B: Enhanced Swift-XRT position
DATE:    22/10/27 23:17:15 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 1519 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 221027B, 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 = 225.62095, +47.44205 which is equivalent
to:

RA (J2000): 15h 02m 29.03s
Dec (J2000): +47d 26' 31.4"

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: GRB221027B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32869
SUBJECT: GRB 221027B: BOOTES-1 optical upper limit
DATE:    22/10/28 00:02:43 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado, M. D. Caballero-Garcia, R. Sanchez-Ramirez, I. Perez-Garcia (IAA-CSIC),  C. Perez del Pulgar,  A. Castellon, I. Carrasco, A. Reina (Univ. de Malaga) and F. Rendon (IAA-CSIC and INTA-CEDEA) on behalf of a larger collaboration, report:

Following the detection of GRB 221027B by Swift (Lien et al., GCNC 32867), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst on Oct 27 at 19:19:30 UT (~6 min after trigger). In the co-added frame (20 x 10 s, clear filter), no source is detected within the enhanced XRT error position (Beardmore et al., GCNC 32868) down to 17.3 mag, which is consistent with the non-detection reported by UVOT (Lien et al., GCNC 32867).

We thank the staff at INTA-CEDEA for their excellent support.


GRB_name: GRB221027B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32870
SUBJECT: GRB 221027B: Swift-XRT refined Analysis
DATE:    22/10/28 04:26:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.1 ks of XRT data for GRB 221027B (Lien et al. GCN
Circ. 32867), from 109 s to 24.9 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.
32868).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.77 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.95 (+/-0.16). The
best-fitting absorption column is  1.3 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 2.9 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (4.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 2.9 x 10^20 cm^-2
Excess significance: 3.7 sigma
Photon index:      1.95 (+/-0.16)

If the light curve continues to decay with a power-law decay index of
0.77, the count rate at T+24 hours will be 0.015 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.2 x
10^-13 (6.5 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/01131397.

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


GRB_name: GRB221027B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32871
SUBJECT: Swift GRB 221027B: Global MASTER-Net observations report 
DATE:    22/10/28 07:12:31 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-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 221027B ( A. Y. Lien et al., GCN 32867) errorbox  21757 sec after notice time and 22094 sec after trigger time at 2022-10-28 01:21:53 UT, with upper limit up to  18.5 mag. The observations began at zenith distance = 79 deg. The sun  altitude  is -31.2 deg. 

The galactic latitude b = 57 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=2136676

We obtain a following upper limits.  

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

   22185 |      MASTER-Tavrida |   C |   180 | 17.6 |        
   22185 |      MASTER-Tavrida |   C |   180 | 15.2 |        
   22376 |      MASTER-Tavrida |   C |   180 | 17.9 |        
   22376 |      MASTER-Tavrida |   C |   180 | 15.1 |        
   22662 |      MASTER-Tavrida |   C |   180 | 18.3 |        
   22662 |      MASTER-Tavrida |   C |   180 | 15.4 |        
   23028 |      MASTER-Tavrida |   C |   180 | 18.3 |        
   23028 |      MASTER-Tavrida |   C |   180 | 16.0 |        
   23985 |      MASTER-Tavrida |   C |   180 | 18.5 |        
   23985 |      MASTER-Tavrida |   C |   180 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221017A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32872
SUBJECT: Konus-Wind detection of GRB 221017A
DATE:    22/10/28 12:04:43 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The long-duration GRB 221017A
(MAXI/GSC detection: Nawa et al., GCN 32777;
IPN triangulation: Kozyrev et al., GCN 32787;
CALET/CGBM detection: Cherry et al., GCN 32813)
triggered Konus-Wind at T0=19789.594 s UT (05:29:49.594).

The burst light curve shows a multipeaked structure
which starts at ~T0-19.1 s and has a total duration of ~332 s.
The emission is seen up to ~6 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB221017_T19789/

As observed by Konus-Wind, the burst
had a fluence of 3.90(-0.32,+0.32)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+175.872 s,
of 9.62(-1.55,+1.56)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+312.320 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.99(-0.06,+0.07),
the high energy photon index beta = -2.75(-0.46,+0.23),
the peak energy Ep = 237(-15,+16) keV
(chi2 = 119/98 dof).

The spectrum near the maximum count rate
(measured from T0+151.552 to T0+182.016 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.92(-0.04,+0.04),
the high energy photon index beta = -2.98(-0.35,+0.22),
the peak energy Ep = 288(-13,+13) keV
(chi2 = 137/98 dof).

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


GRB_name: GRB221027B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32873
SUBJECT: GRB 221027B: FRAM-ORM and Ondrejov SBT optical limits
DATE:    22/10/28 12:45:08 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

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

report:

The 2x20cm robotic telescope BART-SBT in Ondrejov (CZ) reacted robotically
to the Swift alert of GRB221027B (Lien et al., GCNC 32867 and Perri et al.
GCNC 32870, GCNC 29119 and 29124), obtaining a series of 12s unfiltered
frames at 19:19:46 UT, i.e. 367s post trigger.

The 25cm robotic telescope FRAM-ORM at La Palma (Spain) reacted to the same
alert, providing a series of 60s unfiltered images from 19:28:20 UT, i.e.
882s post trigger.

Similarly to Hu et al. (GCNC 32869) and Lipunov et al. (GCNC 32871), we do
not detect any new or strongly variable source neither in single or in
combined frames with the following limits:

Tel.    T-T0[mid,s]  Texp[s]  Limit[ABmag]  Note
SBT     374          12       <15.5         (similar during the following
30 min)
SBT     494          240      <17.0
SBT     674          600      <17.3
SBT     1574         2400     <17.7
FRAM    912          60       <17.0         (similar next 60 minutes)
FRAM    1238         10x60    <18.0


GRB_name: GRB221028A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32874
SUBJECT: GRB 221028A: Swift detection of a burst
DATE:    22/10/28 13:32:46 GMT
FROM:    Jamie Kennea at Penn State U  <jak51@psu.edu>

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

At 13:16:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221028A (trigger=1131910).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 314.206, +41.066 which is 
   RA(J2000) = 20h 56m 49s
   Dec(J2000) = +41d 03' 56"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 40 sec.  The peak count rate
was ~2300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 13:18:03.7 UT, 96.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 314.20310,
41.08996 which is equivalent to:
   RA(J2000)  = 20h 56m 48.74s
   Dec(J2000) = +41d 05' 23.9"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 86 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (7.76 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 2.3
(+2.57/-1.47) x 10^22 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 8.64e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT data is unavailable at this time. 

Burst Advocate for this burst is A. Y. Lien (yarleen 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: GRB221027B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32875
SUBJECT: GRB 221027B: Swift/UVOT Upper Limits
DATE:    22/10/28 15:11:15 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and A. Y. Lien (U. Tampa)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 221027B
131 s after the BAT trigger (Lien et al., GCN Circ. 32867).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 32868)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC           131          281          147         >21.1
u_FC               344          594          246         >20.2
white              131         1544          392         >21.5
v                  673         1594          117         >19.2
b                  599         1520           97         >19.4
u                  344         1661          335         >20.4
w1                 722         1644           97         >18.8
m2                 698          718           19         >17.6
w2                 111          841           30         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.033 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32876
SUBJECT: GRB 221028A: GIT optical upper limit
DATE:    22/10/28 15:26:09 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

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

We observed GRB 221028A detected by Swift (A. Y. Lien et al. GCN # 32874)
with 0.7m GROWTH-India Telescope (GIT). We obtained two 300-sec exposures
in the r' filter. We did not detect any new source within a 5-arcsec radius
uncertainty circle around the Swift-XRT position (A. Y. Lien et al. GCN #
32874) in our stacked image. The upper limit follows as:

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

 JD (mid) | T_mid-T0(hrs) | Filter | Lim_Mag (5-sigma) |

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

 2459881.102968 | 1.2 | r' | > 20.24 |

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

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
<https://iopscience.iop.org/article/10.3847/1538-3881/ac7bea>) 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: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32877
SUBJECT: LIGO-Virgo-KAGRA and GEO600 statement on GRB 221009A
DATE:    22/10/28 15:30:08 GMT
FROM:    Francesco Pannarale at LIGO-Virgo-KAGRA Collaboration  <francesco.pannarale@ligo.org>

None of the LIGO, Virgo, or KAGRA detectors were in observing operation
at the time of GRB 221009A. The detectors are currently being prepared
for the O4 observing run, which is expected to begin in March 2023. The
observing run planning can be viewed here:
https://observing.docs.ligo.org/plan/

GEO600 was taking data at the time of GRB 221009A. However, its
sensitivity is insufficient to detect any viable GRB progenitor at the 
estimated z=0.151 (de Ugarte Postigo et al. GCNC 32648), and the data
show no evidence of an astrophysical transient at the time of GRB 221009A.


GRB_name: GRB221028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32878
SUBJECT: GRB 221028A: BOOTES-4/MET optical upper limit
DATE:    22/10/28 16:03:30 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, E. Fernandez-Garcia, I. Perez-Garcia, A. J. Castro-Tirado, M. D. Caballero-Garcia, R. Sanchez-Ramirez (IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga), S. Guziy (Univ. of Nikolaev) and D. R. Xiong, Y. F. Fan, J. M. Bai, C. J. Wang, Y. X. Xin, X. H. Zhao (Yunnan Observatories of CAS) on behalf of a larger collaboration, report:

Following the detection of GRB 221028A by Swift (Lien et al. GCNC 32874), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical Observatory (China) automatically responded to this burst starting on Oct. 28 at 13:24:22 UT (~8 min after trigger). No new source is detected within the XRT error region (Lien et al. GCNC 32874) in the co-added image (33 x 10 s, clear filter) down to 19.9 mag, which is consistent with the non-detection reported by GIT (Kumar et al., GCNC 32876).

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


GRB_name: GRB221028A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32879
SUBJECT: Swift GRB 221028A: Global MASTER-Net observations report 
DATE:    22/10/28 18:16:35 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 221028A ( A. Y. Lien et al., GCN 32874) errorbox  17090 sec after notice time and 17113 sec after trigger time at 2022-10-28 18:01:41 UT, with upper limit up to  18.7 mag. Observations started at twilight.  The observations began at zenith distance = 74 deg. The sun  altitude  is -13.0 deg. 

The galactic latitude b = -3 deg., longitude l = 83 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2137317

We obtain a following upper limits.  

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

   17203 |         MASTER-SAAO |   C |   180 | 18.4 |        
   17414 |         MASTER-SAAO |   C |   180 | 18.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221027B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32880
SUBJECT: GRB 221027B: COATLI Upper Limits
DATE:    22/10/28 18:36:57 GMT
FROM:    Rosa Leticia Becerra Godinez at Inst. de Astronoma,UNAM  <rbecerra@astro.unam.mx>

Rosa L. Becerra (UNAM), Alan M. Watson (UNAM), Nat Butler (ASU), Simone
Dichiara (PSU), Tzveti Dimitrova (ASU), OcÃ©lotl LÃ³pez (UNAM), Diego
GonzÃ¡lez (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita
Pereyra (UNAM), Eleonora Troja (UTV/ASU) and report:

We observed the field of the GRB 221027B (Lien et al., GCN Circ. 32867)
with the COATLI 50-cm telescope and HUITZI f/8 imager at the Observatorio
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir (
http://coatli.astroscu.unam.mx) from 2022-10-28 01:47 UTC to 02:13 UTC (6.6
hours after the trigger), obtaining a total of 750 seconds of exposure in
the r filter.

We do not detect any uncataloged sources within the XRT error region
(Beardmore et al., GCN Circ. 32868) to a 3-sigma limit of r > 21.4 mag.

Our photometry is calibrated against the Pan-STARRS1 catalog, is on an
approximate AB system, and is not corrected for Galactic extinction in the
direction of the GRB.

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


GRB_name: GRB221028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32881
SUBJECT: GRB 221028A: LCOGT Optical Upper Limits
DATE:    22/10/28 20:43:59 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 221028A (Lien et al., GCN 32874) field with the LCOGT
1-meter Sinistro instrument at the Teide Observatory, on Tenerife, on
October 28, from 19:17 to 19:44 (corresponding to 6.02 to 6.45 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 uncatalouged sources in the XRT error region, in either band,
consistent with other optical upper limits (Kumar et al., GCN 32876; Hu et
al., GCN 32878; Lipunov et al., GCN 32879).

The following upper limits are calculated using the Pan-STARRS catalog as
reference:

r > 21.80
i > 21.62

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB221028B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32882
SUBJECT: GRB 221028B: MAXI/GSC detection
DATE:    22/10/29 00:31:06 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

H. Negoro (Nihon U.), M. Serino (AGU), M. Shidatsu (Ehime U.), 
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, W. Iwakiri, J. Kohara, S. Urabe, S. Nawa, N. Nemoto (Chuo U.), 
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 (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 2022-10-28T20:57:52 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (215.098 deg, -36.880 deg) = (14 20 23, -36 52 48) (J2000)
with a 90% C.L. statistical error of 0.23 deg and an additional systematic 
uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 159 +- 26 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(214.489, -35.809) deg = (14 17 57, -35 48 32) (J2000)
(214.045, -36.075) deg = (14 16 10, -36 04 30) (J2000)
(215.717, -37.852) deg = (14 22 52, -37 51 07) (J2000)
(216.165, -37.579) deg = (14 24 39, -37 34 44) (J2000)
There was no significant excess flux in the previous transit at 19:24 UT
and in the next transit at 22:09 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB221028A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32883
SUBJECT: GRB 221028A: MITSuME Okayama optical upper limits
DATE:    22/10/29 07:02:15 GMT
FROM:    Masafumi Niwano at Tokyo Institute of Tech  <niwano@hp.phys.titech.ac.jp>

M. Niwano, R. Hosokawa, I.Takahashi, 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 221028A (A. Y. Lien et al. GCN Circular 
#32874, H. Kumar et al. GCN Circular #32876, Y.-D. Hu et al. GCN 
Circular #32878, V. Lipunov et al. GCN Circular #32879, R. Strausbaugh 
et al. GCN Circular #32881) with the optical three color (g', Rc, and 
Ic) CCD cameras attached to the MITSuME 50 cm telescope Okayama.

The observation with a series of 60 sec exposures started at 2022-10-28 
13:17:23 UT (59 seconds after the Swift/BAT trigger). We stacked the 
images with good conditions. We did not detect any uncatalogued sources 
within the Swift/XRT error region (A. Y. Lien et al. GCN Circular 
#32874). We obtained the 5-sigma limits of the stacked images as follows.

T0+[sec] | MID-UT | T-EXP[sec] | 5-sigma limits
------------------------------------------------------------------------------------------------
59 | 2022-10-28 14:17:10 | 5790.0 | g'>18.7, Rc>19.5, Ic>18.7
------------------------------------------------------------------------------------------------
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: GRB221027A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32884
SUBJECT: GRB 221027A: AGILE detection
DATE:    22/10/29 08:43:17 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi, F. Longo (Univ. Trieste and INFN Trieste), C. Pittori, F.
Verrecchia (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor
Vergata), A. Argancc, M. Cardillo, C. Casentini, Y. Evangelista, L.
Foffano, E. Menegoni, G. Piano (INAF/IAPS), A. Bulgarelli, A. Di Piano, V.
Fioretti, G. Panebianco, N. Parmiggiani (INAF/OAS-Bologna), F. Lucarelli
(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 satellite detected the GRB 221027A at T0 = 2022-10-27 04:09:34 s
(UTC), reported by Fermi GBM (GCNs #32861, #32866) and Fermi LAT (GCN
#32862). 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 10 s and it released a total number
of 11040 counts in the MCAL detector (above a background rate of 1180 Hz),
and 30890 counts in the AC detector (above a background rate of 3250 Hz).
The AGILE ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/GRB221027A_AGILE_RM.png .

The event also triggered a high time resolution MCAL data acquisition, from
T0-22.42 s to T0+7.94 s (UTC), and released 5086 counts in the detector,
above a background rate of 472 Hz. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB221027A_080667_593928574.000000.png
. The time-integrated spectrum of the burst between T0 and T0+3s be fitted
in the energy range 0.4-10 MeV with a power-law with ph. ind. = -2.31
(-0.69/+1.26), resulting in a reduced chi-squared of 1.44 (48 d.o.f.) and a
fluence of 1.8e-06 ergs/cm^2 (90% confidence level), in the same energy
range. At the T0, the event was 67 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: GRB221028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32885
SUBJECT: GRB 221028A: AGILE detection
DATE:    22/10/29 08:43:27 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi, F. Longo (Univ. Trieste and INFN Trieste), C. Pittori, F.
Verrecchia (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor
Vergata), A. Argan, M. Cardillo, C. Casentini, Y. Evangelista, L. Foffano,
E. Menegoni, G. Piano (INAF/IAPS), A. Bulgarelli, A. Di Piano, V. Fioretti,
G. Panebianco, N. Parmiggiani (INAF/OAS-Bologna), F. Lucarelli (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 satellite detected the GRB 221028A at T0 = 2022-10-28 13:16:27 s
(UTC), reported by Swift BAT (GCN #32874). 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 2 s
and it released a total number of 3155 counts in the MCAL detector (above a
background rate of 1180 Hz), and 7270 counts in the AC detector (above a
background rate of 3410 Hz). The AGILE ratemeters light curves can be found
at http://www.agilescienceapp.it/notices/GRB221028A_AGILE_RM.png .

The event also triggered a high time resolution MCAL data acquisition, from
T0-4.31 s to T0+33.35 s (UTC), and released 1924 counts in the detector,
above a background rate of 477 Hz. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB221028A_080686_594047787.000000.png
. The time-integrated spectrum of the burst between T0-2s and T0+7s be
fitted in the energy range 0.4-10 MeV with a power-law with ph. ind. =
-2.65 (-0.39/+0.50), resulting in a reduced chi-squared of 0.78 (48 d.o.f.)
and a fluence of 3.1e-06 ergs/cm^2 (90% confidence level), in the same
energy range. At the T0, the event was 49 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: GRB221028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32886
SUBJECT: GRB 221028A: HCT optical upper limit
DATE:    22/10/29 08:49:36 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar (IITB), A. Dutta (IIA), D.K. Sahu (IIA), G. C. Anupama (IIA), S.
Barway (IIA), V. Bhalerao (IITB), R. Gupta (ARIES), K. Misra (ARIES), D.
Panchal (ARIES), S.B. Pandey (ARIES), report on behalf of the HCT team:

We observed GRB 221028A detected by Swift-BAT (A. Y. Lien et al. GCN #
32874) with the 2.0m Himalayan Chandra Telescope (HCT) of the Indian
Astronomical Observatory (IAO). We obtained exposures in the Bessel V, Rc
and Ic filters and did not detect any afterglow within the Swift-XRT
uncertainty circle (A. Y. Lien et al. GCN # 32874). The obtained upper
limits follow as:

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

 JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Lim_mag (5-sigma) |

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

 2459881.075085 | 0.52 | 60  | Rc | > 19.94 |

 2459881.091424 | 0.92 | 300 | Rc | > 22.06 |

 2459881.1037215| 1.21 | 300 | Ic | > 20.74 |

 2459881.108775 | 1.33 | 420 | V | > 22.30 |

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

The upper limits are consistent with Kumar et al., GCN #32876; Hu et al.,
GCN #32878; Lipunov et al., GCN #32879, R. Strausbaugh et al., GCN #32881.
The reported magnitudes are in the AB system of magnitude, calibrated
against PanSTARRS DR1 (Chambers et al., 2016) using Lupton's transformation
equations available at
http://classic.sdss.org/dr4/algorithms/sdssUBVRITransform.html#Lupton2005
and not corrected for Galactic extinction.

These observations were carried out under the ToO program HCT-2022-C3-P12.
We thank the HCT staff for their support during the observations. The
Indian Astronomical Observatory is operated by the Indian Institute of
Astrophysics, Bengaluru, India.


GRB_name: GRB221028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32888
SUBJECT: GRB 221028A: COATLI Upper Limits
DATE:    22/10/29 17:43:28 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Rosa Becerra (UNAM), Simone
Dichiara (PSU), Tzveti Dimitrova (ASU), OcÃ©lotl LÃ³pez (UNAM), Diego
GonzÃ¡lez (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita
Pereyra (UNAM), Eleonora Troja (UTV/ASU) and report:

We observed the field of the GRB 221028A (Lien et al., GCN Circ. 32874)
with the COATLI 50-cm telescope and HUITZI f/8 imager at the Observatorio
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir (
http://coatli.astroscu.unam.mx) from 2022-10-29 02:13 UTC to 08:03 UTC
(13.5 to 19.3 hours after the trigger), obtaining a total of 244 minutes of
exposure in the r filter.

At the position of the XRT afterglow (Lien et al., GCN Circ. 32874), we do
not detect a source to the following 3-sigma upper limit:

r > 23.4

Our photometry is calibrated against the Pan-STARRS1 catalog, is on an
approximate AB system, and is not corrected for Galactic extinction in the
direction of the GRB.

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


GRB_name: GRB221028A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32889
SUBJECT: GRB 221028A: CrAO/ZTSh optical upper limit
DATE:    22/10/29 20:04:27 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the GRB 221028A  (Lien et al., GCN 32874; Ursi et al., GCN 
32885) with ZTSh 2.6m telescope of CrAO observatory starting on Oct. 28 
(UT) 19:38:37.  We do not detect any optical object within XRT 
localization (Lien et al., GCN 32874). This is consistent with reported 
  non-detections   (Hu et al., GCN 32878; Kumar et al., GCN 32876; 
Lipunov et al., GCN 32879; Strausbaugh et al., GCN 32881; Niwano et al., 
GCN 32883; Kumar  et al., GCN 32886;  Watson   et al., GCN 32888).

Preliminary photometry of the field in a combined image is following

Date       UT start   t-T0    Filter Exp.     OT      err    UL(3sigma)
                      (mid, days)       (s)
2022-10-28 19:38:37   0.27233 R      10*120   n/d     n/d    20.7

The photometry is based on several nearby USNO-B1.0 (R2) stars
USNO-B1.0
RA DEC R2
20:56:40.7621 +41:04:57.000 15.60
20:56:51.9768 +41:04:22.922 17.21
20:57:00.0629 +41:02:55.072 16.04


GRB_name: GRB221029A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32890
SUBJECT: GRB 221029A: Detection by GRBAlpha
DATE:    22/10/29 21:48:23 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, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly 
Observatory), M. Dafcikova, F. Munz, N. Husarikova, J.-P. Breuer, M. 
Topinka, 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 221029A (Fermi-GBM detection trigger 
688698332/221029045; INTEGRAL/SPI-ACS detection peak at about 2022-10-29 
01:05:28) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 
2020).

The 9.8 sigma detection was confirmed at the peak time 2022-10-29 
01:05:27.8 UTC. The GRB has the T90 duration of 36 s.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221029A_GCN_GRBAlpha.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a 
future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its 
detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously 
upgrading the on-board data acquisition software stack. 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: GRB221029A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32891
SUBJECT: GRB 221029A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/10/29 22:42:43 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), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 221029A onboard (T0:
2022-10-29T01:05:27 UTC, GECAM trig 49, Fermi/GBM trig 688698332,
GRBAlpha GCN 32890).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 51.6 in a
2.048 s analysis time bin.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -60.
The NITRATES best fit sky location is consistent with the Fermi/GBM
localization.

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

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

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


GRB_name: GRB221027B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32892
SUBJECT: GRB 221027B: Swift-BAT refined analysis
DATE:    22/10/30 16:03:48 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@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 221027B (trigger #1131397)
(Lien et al., GCN Circ. 32867).  The BAT ground-calculated position is
RA, Dec = 225.601, 47.451 deg which is
   RA(J2000)  =  15h 02m 24.2s
   Dec(J2000) = +47d 27' 04.4"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 45%.

The mask-weighted light curve shows a structure with two pulses that start
at ~T-6 s and end at ~T+4 s. The first weaker peak occurs at ~T-5 s,
followed by the main peak that occurs at ~T0. T90 (15-350 keV)
is 8.66 +- 1.10 sec (estimated error including systematics).

The time-averaged spectrum from T-5.98 to T+4.20 sec is best fit
by a simple power-law model.  The power law index of the
time-averaged spectrum is 2.39 +- 0.19.  The fluence in
the 15-150 keV band is 5.8 +- 0.6 x 10^-7 erg/cm2. The 1-sec peak
photon flux measured from T-0.08 sec in the 15-150 keV band
is 3.4 +- 0.4 ph/cm2/sec.  All the quoted errors are at
the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1131397/BA/


GRB_name: GRB221028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32893
SUBJECT: GRB 221028A, Swift-BAT refined analysis
DATE:    22/10/30 16:04:53 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) (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 221028A (trigger #1131910)
(Lien et al., GCN Circ. 32874).  The BAT ground-calculated position is
RA, Dec = 314.198, 41.082 deg which is
   RA(J2000)  =  20h 56m 47.5s
   Dec(J2000) = +41d 04' 56.0"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 53%.

The mask-weighted light curve shows a short pulse that starts and peaks
at ~T0 and ends at ~T+2, followed by several overlapping pulses that lasts
till ~T+84 s. The structure resembles those of short GRBs with extended
emission.
T90 (15-350 keV) is 57.1 +- 15.0 sec (estimated error including
systematics).

Due to current detector issues, data below ~50 keV are inaccurate. Thus,
only data above 50 keV are used for spectral analysis. The time-averaged
spectrum from T-0.1 to T+84.0 sec is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 1.367 +- 0.325.
The fluence in the 15-150 keV band is 1.51 +- 0.14 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.56 sec in the 15-150 keV band
is 0.8 +- 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/1131910/BA/


GRB_name: GRB221028A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32894
SUBJECT: GRB 221028A: AKO Optical Upper Limit
DATE:    22/10/30 20:24:14 GMT
FROM:    Mohammad Odeh at Al Khatim Observatory M44  <mshodeh@gmail.com>

Mohammad Odeh at Al-Khatim Astronomical Observatory (AKO), operated by the
International Astronomical Center (IAC), in Abu Dhabi, the United Arab
Emirates.



We observed the GRB 221028A  (Lien et al., GCN 32874) with our 0.36m
telescope on 30 October from 15:39 to 16:44 (UT). We obtained exposures in
the B, V, and Ic filters and did not detect any afterglow within XRT
localization (Lien et al., GCN 32874). This is consistent with the reported
non-detections of (Hu et al., GCN 32878; Lipunov et al., GCN 32879;
Strausbaugh et al., GCN 32881; Niwano et al., GCN 32883; Kumar et al., GCN
32886; Watson et al., GCN 32888; Belkin et al., GCN 32889).



Each image consists of seven stacked frames, each frame is a 3-minute
exposure. The obtained upper limits are as follows:



Mid Time (UT), Filter, Lim. Mag.

2022-10-30T16:16:06Z, B, > 18.3

2022-10-30T16:13:03Z, V, > 19.6

2022-10-30T16:09:22Z, Ic, > 20.2


GRB_name: GRB221028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32895
SUBJECT: GRB 221028A: Correction to GCN 32893 - Fluence and flux are for 50-150 keV
DATE:    22/10/31 01:55:30 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

The fluence for the time averaged spectrum and the 1-s peak
flux quoted in the BAT refined analysis for GRB 221028A
(Palmer et al., GCN Circ. #32893) should be for the energy
range of 50-150 keV, instead of the 15-150 keV written in
the original circular.

In other words, it should be
"The fluence in the 50-150 keV band is 1.51 +- 0.14 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.56 sec in the 50-150 keV band
is 0.8 +- 0.2 ph/cm2/sec."

We apologize for the typos and any confusion this may cause.


GRB_name: GRB221028A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32896
SUBJECT: GRB 221028A: NUTTelA-TAO / BSTI Early Optical Limits
DATE:    22/10/31 02:35:10 GMT
FROM:    Toktarkhan Komesh at Nazarbayev University  <toktarkhan.komesh@nu.edu.kz>

T. Komesh (NU), B. Grossan (UCB, NU), Z. Maksut (NU), M. Krugov (FAI), 
report on behalf of the Energetic Cosmos Laboratory: The Nazarbayev 
University Transient Telescope at Assy-Turgen Astrophysical Observatory 
(NUTTelA-TAO) observed the field of GRB 221028A on receipt of an 
automated GCN / BAT position alert, observing in Sloan g', r' and i' 
bands, with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan, 
Kumar & Smoot 2019, JHEA, 32, 14).We started observations at UT 
2022-10-28 13:47:19, 1852 s after the BAT trigger. Observations were 
made under partially cloudy conditions, beginning with the target at an 
altitude of 82 deg. No new or changing sources consistent with the XRT 
position (Lien 2022, GCN 32874) were detected. Note that these 
observations provide essentially full-time coverage, simultaneous in all 
three bands. We report the following results: start time t-t0(s) end 
time UL g' UL r' ULi' exposure_time (s) ------------ -------- 
----------- ------ ------ ----- ------ 13:47:19 1852 13:48:19 19.3 18.9 
18.7 60 13:48:19 1912 13:58:19 20.3 19.4 20.0 600 start time is in UT. 
t-t0(s) gives the time since trigger, in seconds. UL gives the 5 sigma 
upper limit sensitivity in magnitudes for an image withindividual 
exposure time (first row) and for images co-added to the given exposure 
time (second row). The given upper limit values are derived from the 
average calibration with only 2-4 standard stars per co-added frame, and 
no other analysis or corrections. ---------------------------------- NU 
= Nazarbayev University, Nur-Sultan, Kazakhstan UCB = University of 
California, Berkeley, USA FAI = Fesenkov Astrophysical Institute, 
Kazakhstan This research has been funded by the Science Committee of the 
Ministry of Science and Higher Education of the Republic of Kazakhstan 
(Grant No. AP14870504). The NUTTelA-TAO Team acknowledges the support of 
the staff of the Assy-Turgen Astrophysical Observatory, Almaty, 
Kazakhstan, and the Fesenkov Astrophysical Institute, Almaty, Kazkhstan.


GRB_name: GRB221028A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32897
SUBJECT: GRB 221028A: NUTTelA-TAO / BSTI Early Optical Limits
DATE:    22/10/31 02:47:47 GMT
FROM:    Toktarkhan Komesh at Nazarbayev University  <toktarkhan.komesh@nu.edu.kz>

T. Komesh (NU), B. Grossan (UCB, NU), Z. Maksut (NU), M. Krugov (FAI), report on behalf of the Energetic Cosmos Laboratory:

The Nazarbayev University Transient Telescope at Assy-Turgen Astrophysical Observatory (NUTTelA-TAO) observed the field of GRB 221028A on receipt of an automated GCN / BAT position alert, observing in Sloan g', r' and i' bands, with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan, Kumar & Smoot 2019, JHEA, 32, 14).

We started observations at UT 2022-10-28 13:47:19, 1852 s after the BAT trigger. Observations were made under partially cloudy conditions, beginning with the target at an altitude of 82 deg. No new or changing sources consistent with the XRT position (Lien 2022, GCN 32874) were detected. Note that these observations provide essentially full-time coverage, simultaneous in all three bands. We report the following results:

start time   t-t0(s)     end time      UL g'    UL r'  ULi'   exposure_time (s)
------------ --------  -----------     ------  ------  -----   ------
13:47:19      1852      13:48:19        19.3    18.9    18.7 60
13:48:19      1912      13:58:19        20.3    19.4    20.0    600

start time is in UT. t-t0(s) gives the time since trigger, in seconds. UL gives the 5 sigma upper limit sensitivity in magnitudes for an image with individual exposure time (first row) and  for images co-added to the given exposure time (second row). The given upper limit values are derived from the average calibration with only 2-4 standard stars per co-added frame, and no other analysis or corrections.

----------------------------------
NU = Nazarbayev University, Nur-Sultan, Kazakhstan
UCB = University of California, Berkeley, USA
FAI = Fesenkov Astrophysical Institute, Kazakhstan

This research has been funded by the Science Committee of the Ministry of Science and Higher Education of the Republic of Kazakhstan (Grant No. AP14870504). The NUTTelA-TAO Team acknowledges the support of the staff of the Assy-Turgen Astrophysical Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical Institute, Almaty, Kazkhstan.


GRB_name: GRB221028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32898
SUBJECT: GRB 221028A: 1.3m DFOT Optical upper limit
DATE:    22/10/31 07:20:02 GMT
FROM:    Amit Kumar Ror at ARIES  <mitturor77894@gmail.com>

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


We observed Swift-BAT detected GRB 221028A (Lien et al. GCN 32874) using
the 2Kx2K CCD Imager mounted on the 1.3m Devasthal Fast Optical Telescope
(DFOT) located at the Devasthal observatory of Aryabhatta Research
Institute of Observational Sciences (ARIES), India. The observations were
started on 2022-10-28 at 15:17:46, i.e., around 2 hours after the BAT
trigger. We have taken multiple frames, each having an exposure time of 300
sec in the R filter. We did not detect any new source within the XRT error
circle in our stacked image. We obtain the following 3-sigma upper limit in
the stacked image.


Date Start (UT)  T_start-T0 (hours) Filter  Exp time (sec)  Limiting
magnitude

===============================================================

2022-10-28 15:17:46    ~2        R        300x6   > 21.5

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

The non-detection of the optical afterglow is consistent with Kumar et al.
GCNs 32876, 32886; Hu et al. GCN 32878; Lipunov et al. GCN 32879;
Strausbaugh et al. GCN 32881; Niwano et al. GCN 32883; Watson et al. GCN
no. 32888; Belkin et al. GCN 32889; Odeh GCN 32894; and Komesh et al. GCN
32897.

This circular may be cited.


GRB_name: GRB221028A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32899
SUBJECT: GRB 221028A: Swift-XRT refined Analysis
DATE:    22/10/31 07:29:01 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 5.6 ks of XRT data for GRB 221028A (Lien et al. GCN
Circ. 32874), from 92 s to 28.1 ks after the  BAT trigger. The data
comprise 23 s in Windowed Timing (WT) mode (the first 2 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The refined XRT position is RA, Dec = 314.2027, +41.0898 which is
equivalent to:

RA (J2000): 20 56 48.64
Dec(J2000): +41 05 23.3

with an uncertainty of 3.5 arcsec (radius, 90% confidence).

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.04 (+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 (+0.5, -0.4). The
best-fitting absorption column is  2.4 (+1.0, -0.8) x 10^22 cm^-2, in
excess of the Galactic value of 7.8 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 8.2 x 10^-11 (1.3 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.4 (+1.0, -0.8) x 10^22 cm^-2
Galactic foreground: 7.8 x 10^21 cm^-2
Excess significance: 3.3 sigma
Photon index:      1.5 (+0.5, -0.4)

If the light curve continues to decay with a power-law decay index of
2.04, the count rate at T+24 hours will be 8.3 x 10^-6 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.8 x
10^-16 (1.1 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/01131910.

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


GRB_name: GRB221029A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32900
SUBJECT: GRB 221029A: Fermi GBM Final Localization
DATE:    22/10/31 13:42:50 GMT
FROM:    Joe Mangan at UCD  <joseph.mangan@ucdconnect.ie>

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

"At 01:05:27.31 UT on 29 October 2022, the Fermi Gamma-Ray Burst
Monitor (GBM) triggered and located GRB221029A (trigger 688698332 /
221029045).

The on-ground calculated location, using the GBM trigger data, is RA =
53.3, DEC = -44.9 (J2000 degrees, equivalent to 3h 33m, -44d 54'),
with a statistical uncertainty of 1 degrees (radius, 1-sigma
containment, statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90%
of GRBs having a 3.7 deg error and a small tail suffering a larger
than 10 deg systematic error. [Connaughton et al. 2015, ApJS, 216, 32]
).

The angle from the Fermi LAT boresight at the GBM trigger time is 72 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221029045/quicklook/glg_skymap_all_bn221029045.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/bn221029045/quicklook/glg_healpix_all_bn221029045.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221029045/quicklook/glg_lc_medres34_bn221029045.gif


GRB_name: GRB221022C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32901
SUBJECT: Konus-Wind detection of GRB 221022C
DATE:    22/10/31 14:54:50 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The short-duration GRB 221022C
(IPN triangulation: Svinkin et al., GCN Circ. 32857)
triggered Konus-Wind at T0=52903.608 s UT (14:41:43.608).

The burst light curve shows a multipeaked structure,
which starts at T0-88 ms and has a total duration of ~128 ms.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB221022_T52903/

As observed by Konus-Wind, the burst
had a fluence of 8.55(-1.23,+1.68)x10^-7 erg/cm2,
and a 16-ms peak flux, measured from T0-0.012 s,
of 2.01(-0.39,+0.47)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Since the main fraction of the burst emission was detected
before the trigger, the spectral analysis was performed using
the KW 3-channel light curve data.

Modelling the KW 3-channel time-integrated spectrum
(measured from T0-0.088 s to T0+0.040 s)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep),
yields alpha = -0.09(-0.28,+0.40) and Ep = 548(-86,+121) keV.

All the quoted errors are at the 68% confidence level.
All the quoted values are preliminary.


GRB_name: GRB221027C
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32902
SUBJECT: GRB 221027C: AstroSat CZTI detection
DATE:    22/11/01 11:39:51 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

M. Dixit (IITB), R. Gopalakrishnan (IUCAA), G. Waratkar (IITB), V. 
Prasad (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 a long GRB 221027C.

It was clearly detected in the CsI anticoincidence (Veto) detector in 
the 100-500 keV energy range. The light curve peaks at 2022-10-27 
11:01:02.643 UTC. The measured peak count rate is 430.9 (+76.5, -42.7) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 1296 (+366, -418) counts. The local mean 
background count rate was 1406.0 (+6.2, -6.7) counts/s. We measure a T90 
of 5.3 (+5.9, -3.0) s from the cumulative Veto light curve.

The source was also faintly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-10-27 11:01:04.500 UTC. The measured peak 
count rate associated with the burst is 96.1 (+45.0, -6.1) counts/s 
above the background in the combined data of three quadrants, with a 
total of 368 (+128, -149) counts. The local mean background count rate 
was 349.1 (+2.7, -2.7) counts/s. Using cumulative rates, we measure a 
T90 of 6.4 (+0.6, -3.9) s.

CZTI GRB detections are reported regularly on the payload site at 
http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led 
consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, 
and PRL. The Indian Space Research Organisation funded, managed, and 
facilitated the project.


GRB_name: GRB221029A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32903
SUBJECT: GRB 221029A: Fermi GBM observation
DATE:    22/11/01 13:34:55 GMT
FROM:    Joe Mangan at UCD  <joseph.mangan@ucdconnect.ie>

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

At 01:05:27.31 UT on 29 October 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221029A (trigger 688698332 / 21029045). The
Fermi GBM Final Real-time Localization is reported in GCN 32900.

The GBM light curve consists of three emission episodes
with a duration (T90) of about 27.7 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+28.416 s is
best fit by a Band function with Epeak = 130.7 +/- 6.3 keV,
alpha = -1.12 +/- 0.03, and beta = -2.15 +/- 0.04

The event fluence (10-1000 keV) in this time interval is
(2.69 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.32 s in the 10-1000 keV band
is 35.5 +/- 0.5 ph/s/cm^2.

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

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


GRB_name: GRB221028A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32904
SUBJECT: GRB 221028A: Detection by VZLUSAT-2
DATE:    22/11/01 18:05:11 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.

A long-duration GRB 221028A (Swift/BAT detection: Lien et al., GCN Circ. 
32874; AGILE detection: Ursi et al., GCN Circ. 32885; KONUS-Wind 
detection: trig. time 2022-10-28 13:16:29.550 UT; INTEGRAL/SPI-ACS 
detection peak at 2022-10-28 13:16:28.3 UT) was detected by both GRB 
detector units on board of the VZLUSAT-2 3U CubeSat 
(https://www.vzlusat2.cz/en/).

The data acquisition was performed by GRB detector units no. 0 and no. 
1. The 7.1 (6.1) sigma detection significance was confirmed at detector 
unit no. 0 (no. 1) at 2022-10-28 13:16:26 UTC. The T90 duration was 
measured to be 23 s (26 s) for detector unit no. 0 (no. 1).

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB221028A_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: GRB221027B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32905
SUBJECT: GRB 221027B: GRANDMA observations
DATE:    22/11/03 14:53:01 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

N. Kochiashvili (AbAO), Z. Vidadi (ShAO), D. A. Kann (Goethe Univ.),
P. Gokuldass (Florida Tech.), S. Beradze (AbAO), Sh. Aghayeva (ShAO),
R. Le Montagner (IJCLab), C. Rinner, Z. Benkhaldoun (OUCA),
S. Antier (OCA/Artemis), J. Ali, A. Kaouech (OUCA/KNC), and Sergey 
Karpov
(FZU) report on behalf of the GRANDMA collaboration:

The GRANDMA telescope network responded to the Swift-BAT alert of
GRB 221027B (Lien et al., GCN 32867, Beardmore et al., GCN 32868,
Perri et al., GCN 32870, Markwardt et al., GCN 32892). No optical
afterglow consistent with the XRT position (Beardmore et al., GCN
32868) is detected by Swift in the initial UVOT exposures (Belles &
Lien, GCN 32875).

The first observations started 23.8 hours after the BAT trigger time.
The optical counterpart of the afterglow was not detected in our
observations.

In the following table we report the preliminary photometry of our
observations. Upper limits are reported at the 5-sigma limit,
in the AB system.

T-T0 (hr)| MJD       | Obser.   |Exposure    | Filter | Upp.Lim.
-----------------------------------------------------------------
23.7956 | 59880.79262 | KNC-HAO | 15 x 120 s | L      | 20.5

HAO data have been calibrated with PS1 catalog. Values are
not corrected for the Galactic extinction E(B-V) = 0.0262 mag
(Schlafly & Finkbeiner 2011).

Our upper limits are in agreement with other non-detections from
Swift UVOT (Belles & Lien, GCN 32875), BOOTES-1 (Hu et al., GCN
32869), MASTER (Lipunov et al., GCN 32871), BART-SBT and FRAM-ORM
(Jelinek et al., GCN 32873), and COATLI (Becerra et al., GCN 32880).

GRANDMA is a worldwide coordinated telescope network
(grandma.ijclab.in2p3.fr) devoted to the observation of transients
in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS
497, 5518). Kilonova-Catcher (KNC) is the citizen science program of
GRANDMA (http://kilonovacatcher.in2p3.fr/).


GRB_name: GRB221028A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32906
SUBJECT: GRB 221028A: GRANDMA observations
DATE:    22/11/03 14:55:19 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

N. Kochiashvili (AbAO), Z. Vidadi (ShAO), D. A. Kann (Goethe Univ.),
P. Gokuldass (Florida Tech.), S. Beradze (AbAO), Sh. Aghayeva (ShAO),
R. Le Montagner (IJCLab), C. Rinner, Z. Benkhaldoun (OUCA), A.Janati
(HAO), S. Antier (OCA/Artemis), J. Ali, A. Kaeouach (KNC), and Sergey
Karpov (FZU) report on behalf of the GRANDMA collaboration:

The GRANDMA telescope network responded to the Swift-BAT alert of
GRB 221028A (Lien et al., GCN 32874, Palmer et al., GCN 32893,
D'Elia et al., GCN 32899), which was also detected by AGILE (Ursi
et al., GCN 32885) and VZLUSAT-2 (Ripa et al., GCN 32904).

The first observations started 5.43 hours after the BAT trigger time.
The optical counterpart of the afterglow was not detected in our
observations.

In the following table we report the preliminary photometry of our
observations. Upper limits are reported at the 5-sigma limit,
in the AB system.

T-T0 (hr)| MJD       | Obser.   |Exposure    | Filter| Upp.Lim. (AB)
--------------------------------------------------------------------
5.4341   |59880.77951| MOSS     | 60 x 60 s  | Clear | 21.5
5.8778   |59880.79591| KNC-HAO  | 47 x 180 s |   L   | 22.0

MOSS data has been calibrated with the Gaia DR2 catalog.
HAO data has been calibrated with PS1 catalog.
Values are not corrected for the very large Galactic extinction
E(B-V) = 1.8573 mag (Schlafly & Finkbeiner 2011).

Our upper limits are in agreement with other non-detections from
Swift UVOT (Lien et al., GCN 32874), GIT (Kumar et al., GCN 32876),
BOOTES-4/MET (Hu et al., GCN 32878), MASTER (Lipunov et al., GCN 32879),
LCOGT (Strausbaugh et al., GCN 32881), MITSuME (Niwano et al., GCN 
32883),
HCT (Kumar et al., GCN 32886), COATLI (Watson et al., GCN 32888),
ZTSh 2.6m (Belkin et al., GCN 32889), AKO (Odeh et al., GCN 32894),
NUTTelA-TAO/BSTI (Komesh et al., GCN 32896, 32897), and DFOT (Kumar et
al., GCN 32898).

GRANDMA is a worldwide coordinated telescope network
(grandma.ijclab.in2p3.fr)  devoted to the observation of transients
in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS
497, 5518). Kilonova-Catcher (KNC) is the citizen science program of
GRANDMA (http://kilonovacatcher.in2p3.fr/).


GRB_name: GRB221009A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32907
SUBJECT: High-precision position of the compact radio counterpart to GRB221009A
DATE:    22/11/03 15:45:05 GMT
FROM:    Dr. Pikky Atri at ASTRON  <atri@astron.nl>

P. Atri (ASTRON), T. An (SHAO), M. Giroletti (INAF-IRA), Y.-K. Zhang (SHAO), J. Bright (Oxford), W. Farah (SETI Institute), Rob Fender (Oxford, UCT), J.-J. Geng (PMO), G. Ghirlanda (INAF - OAB), S. Giarratana (University of Bologna, INAF-IRA), Alexander van der Horst (GWU), Y. Li (PMO), Y. Liu (SHAO), B. Marcote (JIVE), J. C. A. Miller-Jones (ICRAR-Curtin), Sara E. Motta (INAF-OAB, Oxford), M. Prez-Torres (IAA-CSIC), L. Rhodes (Oxford), O.S. Salafia (INAF - OAB), A. Wang (SHAO), X.-F. Wu (PMO), Z. Xu (SHAO), J. Yang (OSO)

The Very Long Baseline Array (VLBA) observed GRB221009A on 14-15th October 2022 at 2cm (15.2 GHz) to measure the position of the radio counterpart of the GRB with high accuracy (Project code TG015). These were done ~5 days after the GRB was first reported by the Swift Burst Alert Telescope on 9th October 2022 (ATel #15650).

A compact radio source was detected with a >10sigma significance (rms of 0.06 mJy/beam). Fitting a Gaussian elliptical model to the target shows that the peak emission is from the position:

RA 19h13m03s.500792 (2)
Dec 19d46m24s.22891 (7)

Note that the uncertainties here are purely from a fit to the image plane. Due to a 2 arcminutes offset between the pointing position of the VLBA and the position of the GRB, there was a ~25% drop in sensitivity at the location of the GRB. The systematic uncertainties could be of the order of ~0.1mas based on the beamsize of the VLBA and the uncertainties due to the target-calibrator throw are smaller than this. Follow-up observations of GRB221009A will be conducted with the VLBA.

We would like to thank the VLBA schedulers for conducting these service observations for a quick first-epoch look at the GRB.


GRB_name: GRB221029A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32908
SUBJECT: GRB 221029A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/11/04 04:08:43 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 221029A (Detection by GRBAlpha: Ripa et al., GCN Circ. 32890;
Swift/BAT-GUANO detection: DeLaunay et al., GCN Circ. 32891;
Fermi GBM Final Localization: Fermi GBM team, GCN Circ. 32900;
Fermi GBM observation: Mangan et al., GCN Circ. 32903) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 01:05:26.60 UTC on 29 October 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1351040741/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 multi-peaked structure that starts
at T+0.2 sec, peaks at T+1.6 sec, and ends at T+32.4 sec.
The T90 and T50 durations measured by the SGM data are 27.6 +/- 0.8 sec
and 12.7 +/- 1.4 sec (40-1000 keV), respectively.

The ground-processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1351040741/

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


GRB_name: GRB221009A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32912
SUBJECT: Correction to GCN 32852 (GRB 221009A: SARA-RM 1m Optical Afterglow Detection)
DATE:    22/11/05 19:13:51 GMT
FROM:    Kyle Pellegrin at Clemson University  <pelleg2@g.clemson.edu>

K. Pellegrin,  K. Rumstay, and D. Hartmann report:

The midpoint of observations since the swift trigger stated in GCN 32852
was incorrectly stated at 14.90190 days. The midpoint of observations
occurred on 2022-10-23 at 21:38:42 UTC which makes it 14.3114 days since
the swift trigger on 2022-10-09 at 14:10:17 UTC.

We apologize for any inconvenience this may have caused.


GRB_name: GRB221107A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32913
SUBJECT: GRB 221107A: Fermi GBM Final Localization
DATE:    22/11/07 14:24:08 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

At 01:22:52.46 UT on 7 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 221107A (trigger 689476977 / 221107058).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 146.15, Dec = -45.40 (J2000 degrees, equivalent to J2000 09h 45m, -45d
24'), with a statistical uncertainty of 2.06 degrees.

The angle from the Fermi LAT boresight is 54 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221107058/quicklook/glg_skymap_all_bn221107058.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/bn221107058/quicklook/glg_healpix_all_bn221107058.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221107058/quicklook/glg_lc_medres34_bn221107058.gif


GRB_name: GRB221107A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32915
SUBJECT: GRB 221107A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/11/07 17:36:42 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), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 221107A onboard (T0:
2022-11-07T01:22:54.55 UTC, GECAM trig 53, Fermi/GBM trig 689476977).

The GECAM 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,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 23.8 in a
8.192 s analysis time bin.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -45.6.
The NITRATES best fit sky location is consistent with the Fermi/GBM
localization (GCN 32193).

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

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

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


GRB_name: GRB221009A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32916
SUBJECT: GRB 221009A: Extended Bad Time Intervals for Fermi LAT data 
DATE:    22/11/07 17:38:36 GMT
FROM:    Nicola Omodei at Stanford U.  <nicola.omodei@slac.stanford.edu>

N. Omodei (Stanford Univ.), P. Bruel (CNRS/IN2P3), J. Bregeon (CNRS/IN2P3), M. Pesce-Rollins (INFN Pisa), D. Horan (CNRS/IN2P3),  E. Bissaldi (Politecnico and INFN Bari), and R. Pillera (Politecnico and INFN Bari) 
report on behalf of the Fermi-LAT team: 

Further investigation of the low-level data has shown that X-ray and soft gamma-ray pile-up, multiple photons being recorded at the same time, impacted a larger time interval than reported in the first GCN (Omodei et al. GCN #32760). 
This very high level of pile-up means that the LAT data cannot be analyzed with the standard tools. 
We have thus extended the Bad Time Interval (BTI) to cover the time between T0+203 and T0+294, where T0 is the Fermi-GBM trigger time, October 9, 2022, at 13:16:59.99 UT.

We are currently working on analysis methods that would allow us to reduce the duration of these BTIs.

The signals in the instrument produced by the 99 GeV photon observed 240 seconds after the GBM trigger were well above the noise due to the GRB induced pile-up. Because the extra energy deposited in the instrument at that time was much less than 99 GeV, we are confident that the photon energy was well reconstructed.

The Fermi-LAT point of contact for this burst is 
Elisabetta Bissaldi (elisabetta.bissaldi@ba.infn.it).

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


GRB_name: GRB221107A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32917
SUBJECT: GRB 221107A: Detection by GRBAlpha
DATE:    22/11/07 18:50:11 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), F. Munz, N. Husarikova, J.-P. Breuer, M. Topinka, 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 Metropo
 litan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The long-duration GRB 221107A (Fermi/GBM detection: GCN Circ. 32913, Swift/BAT detection: GCN Circ. 32915) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The 9.3 sigma detection was confirmed at the peak time 2022-11-07 01:22:58.2 UTC. The light curve shows a double-peak structure with a T90 duration of 265 s.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221107A_GCN.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously upgrading the on-board data acquisition software stack. 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: GRB221107A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32918
SUBJECT: GRB 221107A: Fermi GBM Observation
DATE:    22/11/08 14:30:30 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

"At 01:22:52.46 UT on 07 November 2022, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 221107A (trigger 689476977 / 221107058.
This event was also observed by Swift/BAT-GUANO (GCN 32915) and GRBAlpha
(GCN 32917).

The GBM position is reported in the Fermi-GBM Final on-ground Localization
(GCN 32913). The angle from the Fermi LAT boresight is 54 degrees.

The GBM light curve shows numerous peaks with a duration (T90) of about 231
s (50-300 keV). The time-averaged spectrum from T0-2 to T0+235 s is best
fit by a Band function with Epeak = 47 +/- 2 keV, alpha = 0.32 +/- 0.17,
and beta = -2.00 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is (7.464 +/-
0.261)E-05 erg/cm2. The 1-sec peak photon flux measured starting from
T0+9.5 s in the 10-1000 keV band is 10.3 +/- 0.4 ph/s/cm2.

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: GRB221108A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32919
SUBJECT: GRB 221108A: Fermi GBM Final Localization
DATE:    22/11/08 16:06:58 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

At 11:19:33.13 UT on 8 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 221108A (trigger 689599178 / 221108472).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 346.7, Dec = -54.7 (J2000 degrees, equivalent to J2000 23h 07m, -54d
42'), with a statistical uncertainty of 12.8 degrees.

The angle from the Fermi LAT boresight is 133 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221108472/quicklook/glg_skymap_all_bn221108472.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/bn221108472/quicklook/glg_healpix_all_bn221108472.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221108472/quicklook/glg_lc_medres34_bn221108472.gif


GRB_name: GRB221104A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32920
SUBJECT: GRB 221104A: Fermi GBM Final Localization
DATE:    22/11/08 17:29:08 GMT
FROM:    Christian Malacaria at ISSI  <cmalacaria.astro@gmail.com>

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

At 11:19:44.36 UT on 4 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) 
triggered and located GRB 221104A (trigger 689253589 / 221104472).
The on-ground calculated location, using the Fermi GBM trigger data, is 
RA = 180.2, Dec = -22.7
(J2000 degrees, equivalent to J2000 12h 01m, -22d 42'), with a 
statistical uncertainty of 11.7 degrees.

The angle from the Fermi LAT boresight is 101 degrees.


The skymap can be found here: 
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221104472/quicklook/glg_skymap_all_bn221104472.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/bn221104472/quicklook/glg_healpix_all_bn221104472.fit

The GBM light curve can be found here: 
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221104472/quicklook/glg_lc_medres34_bn221104472.gif


GRB_name: GRB221009A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32921
SUBJECT: GRB 221009A: Hubble Space Telescope observations
DATE:    22/11/08 21:17:06 GMT
FROM:    Andrew Levan at U.of Leicester  <a.levan@astro.ru.nl>

A.J. Levan (Radboud Univ.), T. Barclay (NASA/GSFC), K. Bhirombhakdi (STScI), E. Burns (LSU), S. B. Cenko (NASA/GSFC), A. A. Chrimes (Radboud Univ.), P. Dâ€™Avanzo (INAF/OABr), V. Dâ€™Elia (INAF/OAR and ASI/SSDC), M. Della Valle (INAF/OAC), A. de Ugarte Postigo (Obs. Cote dâ€™Azur), W. Fong (Northwestern), A. S. Fruchter (STScI), B. P. Gompertz (Birmingham), D. Hartmann (Clemson University), C. L. Hedges (NASA/GSFC), K. E. Heintz (DAWN/NBI), L. Izzo (DARK/NBI), P. Jakobsson (U. Iceland), P.G. Jonker (Radboud Univ. & SRON), D. A. Kann (Goethe Univ.), J. A. Kennea (PSU), E. Le Flocâ€™h (CEA Paris-Saclay), D. B. Malesani (Radboud Univ. and DAWN/NBI), A. Melandri (INAF/OAR), B. D. Metzger (Columbia and Flatiron/CCA), S. E. Mullally (STScI), E. Pian (INAF, Bologna), S. Piranomonte (INAF/OAR), G. Pugliese (Amsterdam Univ.), J. L. Racusin (NASA/GSFC), J. C. Rastinejad (Northwestern), M. E. Ravasio (Radboud Univ and INAF/OABr), A. Rossi (INAF/OAS), R. Salvaterra (INAF/IASF Milan), B. Sbarufatti (INAF/OABr), B. Schneider (CEA Paris-Saclay), R. L. C. Starling (U. Leicester), N. R. Tanvir (U. Leicester), C. C. Thoene (ASU-CAS), S. D. Vergani (CNRS - Paris Obs.), R. A. M. J. Wijers (Amsterdam), D. Xu (NAOC) report:

We observed the afterglow of GRB 221009A (Dichiara et al., GCN 32632; Kennea & Williams, GCN 32635; Bissaldi et al., GCN 32637; Veres et al., GCN 32636) with the Hubble Space Telescope on 8 November 2022, approximately 30 days after the Fermi/GBM trigger. Observations were obtained in five filters spanning the optical and NIR region (F625W, F775W, F098M, F125W and F160W). 

The optical/IR counterpart is well detected in all images, with provisional AB magnitudes of F625W = 23.61 +/- 0.04, F775W = 22.43 +/- 0.04, F098M = 21.21 +/- 0.01, F125W = 20.63 +/- 0.01, F160W = 20.37 +/- 0.01 mag, based on small apertures around the source location (errors statistical only). After correction for foreground extinction the spectral shape is indicative of a peak around 1 micron, which could be due to the contribution from the associated supernova (de Ugarte Postigo et al. GCN 32800, Belkin et al. GCN 32818, Maiorano et al. GCN 32850).

Inspection of the images reveals faint emission to the NE which is only visible in the NIR bands, and which extends for approximately 1" (2.6 kpc at z = 0.151; de Ugarte Postigo et al., GCN 32648; Castro-Tirado et al. GCN 32686). We suggest this extension is the host galaxy of GRB 221009A and is only visible in the NIR due to foreground extinction. 

Analysis is ongoing, and further observations are planned in late November and early December. 

We thank the staff of STScI, in particular Claus Leitherer, William Januszewski and Joel David Green for their work in rapidly implementing the related DDT proposal (GO 17264, PI Levan).


GRB_name: GRB221110A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32925
SUBJECT: GRB 221110A: Swift detection of a burst with an optical counterpart
DATE:    22/11/10 02:57:59 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. A. Williams (PSU), S. Dichiara (PSU), J. A. Kennea (PSU),
S. Laha (GSFC/UMBC), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 02:28:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221110A (trigger=1136936).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 29.119, -27.314 which is 
   RA(J2000) = 01h 56m 29s
   Dec(J2000) = -27d 18' 50"
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 ~1400 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 02:29:32.8 UT, 75.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 29.09928, -27.29435 which
is equivalent to:
   RA(J2000)  = 01h 56m 23.83s
   Dec(J2000) = -27d 17' 39.7"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 94 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.46 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.2
(+3.14/-2.70) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 01:56:23.90 =  29.09958
  DEC(J2000) = -27:17:36.9  = -27.29355
with a 90%-confidence error radius of about 0.5 arc sec. This position is 3.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.62 with a 1-sigma error of about  0.07. 

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: GRB221110A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32926
SUBJECT: GRB 221110A: LCOGT Optical Afterglow Detection
DATE:    22/11/10 04:44:32 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 221110A (Williams et al., GCN 32925) field with the
LCOGT 1-meter Sinistro instrument at the Cerro Tololo Interamerican
Observatory, Chile site, on November 10, from 03:12 to 03:40 (corresponding
to 0.73 to 1.20 hours from the GRB trigger time) with the SDSS r and i
filters.

We performed a series of 3x300s exposures in each band.  We detect an
uncataloged source in the Swift error region, in both bands, consistent
with the optical counterpart candidate (Lipunov et al., GCN 32924).

The following magnitudes are calculated using the Pan-STARRS catalog as
reference:

r = 19.45 +/- 0.06
i = 18.19 +/- 0.08

These magnitudes are not corrected for galactic extinction.  Imaging and
spectroscopic follow-up has been conducted with Gemini and analysis is
ongoing.


GRB_name: GRB221110A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32927
SUBJECT: GRB 221110A: COATLI Afterglow detection
DATE:    22/11/10 04:49:36 GMT
FROM:    Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada  <mpereyra@astro.unam.mx>

*Margarita Pereyra (UNAM),  Alan M. Watson (UNAM), Nat Butler (ASU), Rosa
Becerra (UNAM), Simone Dichiara (PSU), Tzveti Dimitrova (ASU), OcÃ©lotl
LÃ³pez (UNAM), Diego GonzÃ¡lez (UNAM), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Eleonora Troja (UTV/ASU) and report:We observed the field of
the GRB 221110A (Williams et al., GCN Circ. 32925) with the COATLI 50-cm
telescope and HUITZI f/8 imager at the Observatorio AstronÃ³mico Nacional on
the Sierra de San Pedro MÃ¡rtir (http://coatli.astroscu.unam.mx
<http://coatli.astroscu.unam.mx/>) from 2022-11-10 03:26 UTC to 03:59 UTC
(0.96hrs to 1.5 hours after the trigger), obtaining a total of 29 minutes
of exposure in the r filter.At the position of the UVOT afterglow (Williams
et al., GCN Circ. 32925), we detect a source with the following magnitude
and 1-sigma uncertainty:r = 19.7 +/- 0.15Our photometry is calibrated
against the Pan-STARRS1 catalog, is on an approximate AB system, and is not
corrected for Galactic extinction in the direction of the GRB.Observations
and reductions will continue. Further observations are planned.We thank the
COATLI/HUITZI technical team and the staff of the Observatorio AstronÃ³mico
Nacional.*

-- 
*Dr. Margarita Pereyra *

*FFTF, Schlumberger Foundation Alumnae*
----------------------------------------------------------------------------------------------------------------

*CatedrÃ¡tica Conacyt*

*Instituto de AstronomÃ­a de la UNAM,*

*Km. 107 Carretera Tijua**na-Ensenada, *

*Ensenada Baja California, MÃ©xico. C.P. 22860*

Oficina: 405

Skype: margarita-pereyra


GRB_name: GRB221110A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32928
SUBJECT: GRB 221110A: VLT/X-shooter redshift
DATE:    22/11/10 05:18:41 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

L. Izzo (DARK/NBI), D. B. Malesani (Radboud Univ. and DAWN/NBI), S. 
Vejlgaard Nielsen (DAWN/NBI), N. R. Tanvir (Univ. Leicester), J. P. U. 
Fynbo (DAWN/NBI), D. Xu (NAOC) report on behalf of the Stargate 
collabaration:

We observed the optical afterglow of GRB 221110A (Williams et al., GCN 
32925; Lipunov et al., GCN 32924; Strausbaugh & Cucchiara, GCN 32926; 
Pereyra et al., GCN 32927) using the ESO VLT UT3 (Melipal) equipped with 
the X-shooter spectrograph. Our spectra cover the wavelength range 
3000-25000 AA, and consist of 2 exposures by 600 s each. The observation 
mid time was 2022 Nov 10.158 UT (1.33 hr after the GRB).

We clearly detect continuum over the wavelength range 6200-25000 AA. A 
sharp break is visible around 6200 AA, which we identify as due to H I. 
 From detection of multiple absorption features, which we interpret as 
due to Si IV, C IV, Fe II, O I, Si II, Al II, Al III, and many others, 
we infer a redshift of z = 4.06. An intervening system is also detected 
from Fe II and Mg II at z = 2.724.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Michael Marsset and Florian Rodler.


GRB_name: GRB221110A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32929
SUBJECT: GRB 221110A: Enhanced Swift-XRT position
DATE:    22/11/10 06:08:06 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 1662 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 221110A, 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 = 29.09871, -27.29519 which is equivalent
to:

RA (J2000): 01h 56m 23.69s
Dec (J2000): -27d 17' 42.7"

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: GRB221110A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32930
SUBJECT: GRB 221110A: Swift-XRT refined Analysis
DATE:    22/11/10 16:24:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.4 ks of XRT data for GRB 221110A (Williams et al.
GCN Circ. 32925), from 64 s to 40.0 ks after the  BAT trigger. The data
comprise 55 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 Evans et
al. (GCN Circ. 32929).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.971 (+0.028, -0.027).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.88 (+/-0.15). The
best-fitting absorption column is  8 (+14, -8) x 10^21 cm^-2, at a
redshift of 4.06, in addition to the Galactic value of 1.5 x 10^20
cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.4 x
10^-11 (3.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.5 x 10^20 cm^-2
Intrinsic column:    8 (+14, -8) x 10^21 cm^-2 at z=4.06
Photon index:      1.88 (+/-0.15)

If the light curve continues to decay with a power-law decay index of
0.971, the count rate at T+24 hours will be 9.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-13 (3.3 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/01136936.

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


GRB_name: GRB221110A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32931
SUBJECT: GRB 221110A: Swift-BAT refined analysis
DATE:    22/11/10 18:59:32 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Parsotan (GSFC/UMBC), S. D. Barthelmy (GSFC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), 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+600 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 221110A (trigger #1136936)
(Williams et al., GCN Circ. 32925).  The BAT ground-calculated position is
RA, Dec = 29.106, -27.298 deg which is
   RA(J2000)  =  01h 56m 25.5s
   Dec(J2000) = -27d 17' 51.4"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.

The mask-weighted light curve shows a single-pulse structure
that starts at ~T0, peaks at ~T+1 s, and ends at ~T+10 s.
T90 (15-350 keV) is 8.98 +- 2.11 sec (estimated error including
systematics).

The time-averaged spectrum from T-0.41 to T+9.74 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.41 +- 0.16.  The fluence in the 15-150 keV band
is 5.1 +- 0.5 x 10^-7 erg/cm2. The 1-sec peak photon flux measured
from T+0.52 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/1136936/BA/


GRB_name: GRB221110A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32932
SUBJECT: GRB 221110A: Swift/UVOT Detection and Corrected UVOT Position
DATE:    22/11/11 04:27:28 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

 GRB 221110A: Swift/UVOT Detection and Corrected UVOT Position

S. J. LaPorte (PSU) and M. Williams (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 221110A
83 s after the BAT trigger (Williams et al., GCN Circ. 32925).
A fading source is detected at
RA (J2000) = 01:56:23.72 = 29.09882
Dec (J2000): = -27:17:45.09 = -27.29586
which is consistent with the XRT position (Evans et al. GCN Circ. 32929).

The UVOT position reported in the initial detection circular
(Williams et al., GCN Circ. 32925)
was incorrect, and differs from the updated position presented here by 8.45
arcsec.
We apologize for any inconvenience this discrepancy may cause.

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

b                     3773          3973          196        >19.91
m2                  4593          4793          196        >19.35
u                       326            439          110        >19.33
v                      4357          4557          197        >19.5
w1                   4798          4998          196        >19.48
w2                   4184          4383          196         >19.55
white_FC            114            264          147          18.68+-0.08
white                3978          4178          196         >20.66

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.013 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221110A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32933
SUBJECT: GRB 221110A: GMG upper limit
DATE:    22/11/11 11:22:24 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, J.-J. Zhang, and J.-M. Bai (YNAO) report:We observed the field of GRB 221110A (Williams et al. GCN 32925) by the GMG telescope in Yunnan observatories.The observation began from UT 17:06:28 Nov 10, 2022, about 15 hours from the trigger. We could not observe the opticalafterglow down to a magnitude limit of r~20.8. 


GRB_name: GRB221009A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32934
SUBJECT: GRB 221009A: GRANDMA/Kilonova-Catcher observations 
DATE:    22/11/11 17:01:38 GMT
FROM:    Damien Turpin at NAOC (CAS)  <dturpin-astro@hotmail.com>

O. Aguerre, F. Bayard, E. Broens, H-B. Eggenstein, M. Freeberg, 
R. Kneip (KNC), A. Lekic, B. Delaveau, E. Durand (KNC/IPSA), 
S. Leonini, D. Marchais, E. Maris, R. Mnard, G. Parent, 
M. Richmond, F. Romanov, M. Serrau, S. Vanaverbeke (KNC), 
S. Antier (OCA/Artemis), D. A. Kann (Goethe Univ.),
S. Karpov (FZU), A. Klotz (OMP/IRAP), T. Midavaine (SAF),
D. Turpin (CEA) report on behalf of GRANDMA and
Kilonova-Catcher collaborations:

The Kilonova-Catcher telescope network responded to the alert of 
the ultra-bright GRB 221009A (Swift detection: Dichiara et al.,
GCN 32632; Fermi GBM detection: Veres et al., GCN 32636). 

In total, 220 science images sent by the KNC amateur astronomers
were analyzed. The KNC observations cover the period from 6.3h 
to about 17.5 days after the Fermi/GBM trigger time.

Below, we report a subset of these observations. Magnitudes are given 
in the AB system and we also report our 5-sigma upper limits.

T-T0 (day)| MJD  | Obser.  |Exposure| Filter | Mag +/- err |Upp.Lim. (AB)
___________________________________________________________________________
0.285 | 59861.838073 | T-BRO | 5 x 180s | Ic | 15.65 +/- 0.03 | 18.0
0.578 | 59862.131620 | BGO | 60s | I | 16.58 +/- 0.07 | 17.8
1.241 | 59862.794004 | Astrolab IRIS | 14 x 180s | I | 17.47 +/- 0.07 | 18.5
1.365 | 59862.918754 | Ch-Perdrix | 10 x 180s | Clear | 18.76 +/- 0.14 | 19.2
1.447 | 59863.000000 | Ste-Sophie | 16 x 360s | TR-rgb | 18.89 +/- 0.06 | 20.4
1.531 | 59863.084675 | HVO | 59 x 120s | R | 18.93 +/- 0.09 | 19.8
1.703 | 59863.256925 | SRO Auberry | 300s | I | 17.85 +/- 0.13 | 18.1
2.217 | 59863.770555 | Montarrenti | 2 x 30s | Clear | 18.65 +/- 0.24 | 18.5
2.229 | 59863.782465 | EHEA-WL | 199 x 32s | I | 18.64 +/- 0.21 | 18.7
2.267 | 59863.820289 | CO-K26 | 8884s | Lum | -- | 19.7
2.308 | 59863.861789 | GPO | 5700s | Clear | -- | 19.8
2.522 | 59864.075696 | LCO-MDO | 7 x 180s | sdss-r | 19.56 +/- 0.12 | 20.2
2.555 | 59864.108314 | NMSkies | 11 x 300s | Ic | 18.74 +/- 0.13 | 19.3
3.250 | 59864.803399 | Atlas | 30 x 120s | R | -- | 18.4
5.323 | 59866.876810 | Crous Gats | 180 x 32s | TR-rgb | 20.46 +/- 0.14 | 21.0

These detections and limits are consistent with the detections and limits
previously reported in Lipunov et al., GCN 32634; Perley, GCN 32638;
Broens, GCN 32640; Hu et al., GCN 32644; Belkin et al., GCN 32645; GCN 32769
; Wet et al., GCN 32646; Xu et al., GCN 32647; de Ugarte Postigo et al., GCN
32648, 32800; Odeh, GCN 32649; GCN 32666; Brivio et al., GCN 32652; Kuin et al.,
GCN 32656; Paek et al., GCN 32659; Kumar et al., GCN 32662; Romanov, GCN
32664; 32679; Chen et al., GCN 32667; Vidal et al., GCN 32669; Kim et al.,
GCN 32670; Groot et al., GCN 32678; Castro-Tirado et al., GCN 32686;
Watson et al., GCN 32692; Strausbaugh et al. GCN 32693; Butler et al., GCN
32705; Vinko et al., GCN 32709; Mao et al., GCN 32727; Zaznobin et al.,
GCN 32729; Sasada et al., GCN 32730; Strausbaugh & Cucchiara, GCN 32738;
O'Connor et al., GCN 32739; GCN 32750, GCN 32799, GCN 32860; Bikmaev et al.,
GCN 32743; GCN 32752; Rastinejad & Fong, GCN 32749; Schneider et al., GCN
32753; DAvanzo et al., GCN 32755; Huber et al., GCN 32758; Shrestha et al.,
GCN 32759; 32771; Izzo et al., GCN 32765; Levan et al., GCN 32821, GCN 32921;
Maiorano et al., GCN 32850; Pellegrin et al., GCN 32852.

The GRANDMA/Kilonova-Cacther images have been calibrated using field
stars from the PanSTARRS-DR1 catalog using the STDpipe pipeline
(Karpov 2022).

We advocate a joint multi-wavelength publication for this event and we are 
happy to collaborate with teams that have the same spirit, 
to be able to explore the best astrophysical scenario.

GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr)
devoted to the observation of transients in the context of multi-messenger
astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is
the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).


GRB_name: GRB221110A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32935
SUBJECT: GRB 221110A: COATLI Second-Epoch Upper Limits
DATE:    22/11/11 21:03:17 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Rosa Becerra (UNAM), Simone
Dichiara (PSU), Tzveti Dimitrova (ASU), OcÃ©lotl LÃ³pez (UNAM), Diego
GonzÃ¡lez (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita
Pereyra (UNAM), and Eleonora Troja (UTV/ASU) report:

We observed the field of the GRB 221110A (Williams et al., GCN Circ. 32925)
with the COATLI 50-cm telescope and HUITZI f/8 imager at the Observatorio
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir (
http://coatli.astroscu.unam.mx) from 2022-11-11 03:28 UTC to 09:01 UTC
(25.0 to 30.6 hours after the trigger), obtaining a total of 270 minutes of
exposure in the r filter.

The source detected in our earlier observations (Pereyra et al., GCN Circ.
32927 has now faded and is not detected to a 3-sigma limit of

r > 22.6

Our photometry is calibrated against the Pan-STARRS1 catalog, is on an
approximate AB system, and is not corrected for Galactic extinction in the
direction of the GRB.

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


GRB_name: GRB221112A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32936
SUBJECT: GRB 221112A: Fermi GBM Final Real-time Localization
DATE:    22/11/12 06:25:54 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 06:18:04 UT on 12 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221112A (trigger 689926689.355394 / 221112263).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 91.8, Dec = -52.6 (J2000 degrees, equivalent to J2000 06h 07m, -52d 36'), with a statistical uncertainty of 5.7 degrees.

The angle from the Fermi LAT boresight is 41.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221112263/quicklook/glg_skymap_all_bn221112263.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/bn221112263/quicklook/glg_healpix_all_bn221112263.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221112263/quicklook/glg_lc_medres34_bn221112263.gif


GRB_name: GRB221112A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32937
SUBJECT: GRB 221112A: Detection by GRBAlpha
DATE:    22/11/13 09:46:13 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), F. Munz, N. Husarikova, J.-P. Breuer, M. Topinka, 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 Metropo
 litan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The long-duration GRB 221112A (Fermi/GBM detection: GCN Circ. 32936) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The subthreshold 3.4 sigma detection was confirmed at the peak time 2022-11-12 06:18:04 UTC. The light curve in the 110-370 keV band obtained by GRBAlpha is consistent with the light curve obtained by Fermi/GBM. The GRB has a T90 duration of 15 s.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221112A_GCN.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously upgrading the on-board data acquisition software stack. 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: GRB221110A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32939
SUBJECT: GRB 221110A: GRANDMA observations
DATE:    22/11/15 13:57:43 GMT
FROM:    Iara Tosta e Melo at INFN  <tostaemelo@lns.infn.it>

Content:
M. Coughlin (UMN), E. Gurbanov (ShAO), F. Navarete (SOAR/NOIRLab),
N. Kochiashvili (AbAO), M. Masek (FZU), Y. Rajabov (UBAI),
T. Sadibekova (AIM-CEA), M. Freeberg (KNC), A. Klotz (OMP/IRAP),
M. Boer, A. de Ugarte Postigo, S. Antier (OCA/Artemis), D. Turpin (CEA),
R.W. Kiendrebeogo (OCA/Artemis, LPCE/UJKZ), I. Tosta e Melo (INFN-LNS),
M. Lamoureux, K. Kruiswijk (UCLouvain), J.-G. Ducoin (IAP),
C. Rinner, Z. Benkhaldoun (OUCA), J. Ali, A. Kaouech (OUCA/KNC),
A. M. Fouad, A. Takey, A. Hamed, M. Abdel-Sabour, A. Shokry,
M. Soliman (NRIAG),  X. F. Wang (THU/BJP), J. Zhu (BJP), X. Y. Zeng 
(CGTU),
L. T. Wang, A. Iskandar (XAO), K. Smith (UVI), P. Gokuldass (Florida 
Tech)
N. Orange (OrangeWave Innovative Science, LLC), T. Hussenot (IJCLab),
A. M. Fouad (NRIAG), A. Takey(NRIAG), H. A. Ismail, M. Abdel-Sabour 
(NRIAG),
D. A. Kann (Goethe Univ.) report on behalf of the GRANDMA collaboration:

The GRANDMA telescope network responded to the Swift-BAT alert of
GRB 221110A (M. A. Williams et al., GCN 32925, P.A. Evans et al. GCN 
32929)
detected at 02:28:17.62 UT. An afterglow was immediately detected by 
UVOT with
the estimated magnitude of 18.62 with a 1-sigma error of ~0.07 at XRT
(not refined) position RA, Dec: 29.09928, -27.29435. The VLT/X-shooter
spectroscopic observations (L. Izzo et al., GCN 32928) reported a high-z
candidate at z=4.06.

The first GRANDMA observations started 40 s after the BAT trigger time
with TCH telescope at La Silla, Chile.

Below, we report selected observations. We also report our 5-sigma upper
limits. Magnitudes are given in the AB system.

T-T0(hr)|    MJD     | Obser.  | Exposure | Filter | Mag +/- err|Upp.Lim
_______________________________________________________________________________
  0.06   |59893.105660| TCH     | 5x30s    |  clear | 15.9+/-0.1 | 17.2
  3.3    |59893.242788| SOAR    | 1x300s   |  sdssr | 21.7+/-0.2 | -
  3.3    |59893.246601| SOAR    | 1x300s   |  sdssi | 19.8+/-0.1 | -
  3.3    |59893.238496| SOAR    | 1x300s   |  sdssz | 19.4+/-0.2 | -
  8.1    |59893.440510| KNC-SSO | 5x300s   |   Ic   |       -    | 19.0
  17.6   |59893.835694| KAO     | 10x250s  | sdssz  |       -    | 19.9
  18.7   |59893.881065| KNC-HAO | 20x180s  |    R   |       -    | 19.8
  19.3   |59893.905405| MOSS    | 60x60s   |  clear |       -    | 20.4
  25.1   |59894.149306| VIRT    | 400x10s  |    R   |       -    | 20.1

These observations are consistent with previous reports by LCOGT
(R. Strausbaugh et al GCN 32926) and COATLI (M. Pereyra et al. GCN 
32927).

TCH and MOSS data have been calibrated using nearby
stars from the Pan-STARRS catalogue in sdss-r measured with
STDpipe (Karpov 2022).

KNC-HAO data have been calibrated with respect to
field stars from the Pan-STARRS and APASS catalogues, using the MUPHOTEN
pipeline (Duverne et al. 2022).

The upper limit derived for KAO data was defined with the faintest 
detected
star in the field and the images were processed with IRAF.

SOAR used the "Goodman Spectroscopic Pipeline" for imaging processing
and IRAF for getting the astrometric solution. The photometric 
calibration
was done by comparison with SkyMapper sources in the field in SDSS.

The images of iTelescope 32 (Siding Spring Observatory, Australia)
have been processed using the STDpipe and photometry was performed
using field stars from the PanSTARRS1-i catalogue as a reference.

VIRT data was processed with the in-house pipeline which uses the
USNO.B1 catalogue.

The nearly full Moon contaminated the observations.

GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr)
devoted to the observation of transients in the context of 
multi-messenger
astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher 
(KNC) is
the citizen science program of GRANDMA 
(http://kilonovacatcher.in2p3.fr/).


GRB_name: GRB221115A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32940
SUBJECT: GRB 221115A: Swift/BAT-GUANO detection
DATE:    22/11/15 22:49:14 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), Gayathri Raman (PSU), James DeLaunay
(UAlabama), Jamie A. Kennea (PSU), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 221115A onboard (T0: 2022-11-15T00:25:28
 UTC, Fermi/GBM trig 690164733).

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, 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 8.4 in a
16.384 s analysis time bin.

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FoV.
The Fermi/GBM localization places this burst outside the
contemporaneous BAT FoV.

See Section 9.1 and Figure 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: GRB221115B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32941
SUBJECT: GRB 221115B: Swift/BAT-GUANO arcminute localization
DATE:    22/11/15 23:40:37 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), Tyler Parsotan (GSFC/UMBC) report:

Swift/BAT did not localize GRB 221115B onboard (T0:
2022-11-15T09:46:15 UTC, CALET trig 1352540756).

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

Upon trigger by this notice, GUANO sent a command to the Swift Burst
Alert Telescope (BAT) to save 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 2.048 s analysis time bin
with a sqrt(TS) of 27.7.
The duration of the burst as seen by BAT is ~5 seconds.

A confident arcminute localization is found with DeltaLLHPeak of 49.

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

The BAT position is
RA, Dec = 54.788, -16.701 deg which is
   RA(J2000)  = 03h 39m 09.16s
   Dec(J2000) = -16d 42â€² 03.5â€³
with an estimated uncertainty of 3 arcmin.

XRT and UVOT follow-up has been requested, but will be significantly
delayed due to operational constraints.
We encourage followup from other facilities.

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

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


GRB_name: GRB221115A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32942
SUBJECT: GRB 221115A: Fermi GBM detection
DATE:    22/11/16 15:43:45 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 00:25:28.80 UT on 15 November 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221115A (trigger 690164733 / 221115018)
which was also detected by the Swift/BAT-GUANO (Tohuvavohu et al. GCN 32940).

The on-ground calculated location, using the GBM trigger data, is RA =
37.7, DEC = -3.1 (J2000 degrees, equivalent to 02 h 31 m, -03 d 06 '),
with a statistical uncertainty of 2.1 degrees (radius, 1-sigma
containment, statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90%
of GRBs having a 3.7 deg error and a small tail suffering a larger
than 10 deg systematic error. [Connaughton et al. 2015, ApJS, 216, 32]
).

The angle from the Fermi LAT boresight at the GBM trigger time is 84 degrees.



The GBM light curve consists of two emission episodes with a duration
(T90) of about 147 s (50-300 keV). The time-averaged spectrum from
T0-12.5 s to T0+151.3 s is best fit by
a power law function with an exponential high-energy cutoff.  The
power law index is -0.83 +/- 0.08 and the cutoff energy, parameterized
as Epeak, is 283 +/- 30 keV.


The event fluence (10-1000 keV) in this time interval is (2.26 +/-
0.12)E-5 erg/cm^2. The 1-sec peak photon flux measured starting from
T0+32.1 s in the 10-1000 keV band is 3.50 +/- 0.24 ph/s/cm^2.



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

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


GRB_name: GRB221115B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32943
SUBJECT: GRB 221115B : MeerLICHT upper limits
DATE:    22/11/17 11:07:15 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

S. de Wet (UCT), P.J. Groot (Radboud/UCT/SAAO) report on behalf of the
MeerLICHT consortium:

We observed the Swift/BAT-GUANO localisation of GRB 221115B (DeLaunay et
al., GCN 32941) with the 0.6m wide-field MeerLICHT optical telescope
situated in Sutherland, South Africa, obtaining 2x300s observations in the
q-band (roughly g+r) fully encompassing the 3' error box. Observations
began at 21:21:30 UT on 2022 November 16, 1.48 days post-trigger.

Employing our transient detection pipeline along with an archival reference
image, we detect no new transients within the GUANO error box down to a
5-sigma transient limiting magnitude of q > 20.80. Our new images had
full-frame 5-sigma limiting magnitudes of q = 22.10 and q = 22.18, while
our archival reference image had a limiting magnitude of q = 21.10. All
magnitudes are in the AB system.

MeerLICHT is built and run by a consortium consisting of Radboud
University, the University of Cape Town, the South African Astronomical
Observatory, the University of Oxford, the University of Manchester and the
University of Amsterdam.


GRB_name: GRB221009A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32944
SUBJECT: Correction to GCN 32646 (GRB 221009A (Swift J1913.1+1946): MeerLICHT observations)
DATE:    22/11/17 11:39:27 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

S. de Wet (UCT) reports on behalf of the MeerLICHT consortium:

The r-band magnitude for the afterglow of GRB 221009A reported in GCN 32646
was incorrectly reported as r = 17.76 +/- 0.08 at 18:23:59 UT. The correct
magnitude is r = 16.76 +/- 0.08.

We apologize for any inconvenience this may have caused.


GRB_name: GRB221115B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32945
SUBJECT: GRB 221115B: LCOGT Optical Upper Limits
DATE:    22/11/17 21:13:24 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 221115B (DeLaunay et al., GCN 32941) field with the
LCOGT 1-meter Sinistro instrument at the South African Astronomical
Observatory site, on November 16, from 19:40 to 20:08 (corresponding to
34.15 to 34.62 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 fading uncatalogued sources in the BAT error region, in either band,
consistent with other optical upper limits (de Wet et al., GCN 32943).

The following upper limits are calculated using the Pan-STARRS catalog as
reference:

r > 22.4
i > 21.5

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB221118A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32946
SUBJECT: GRB 221118A: Fermi GBM Final Real-time Localization
DATE:    22/11/18 13:58:58 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 13:48:19 UT on 18 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221118A (trigger 690472104.534408 / 221118575).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 276.5, Dec = -45.3 (J2000 degrees, equivalent to J2000 18h 26m, -45d 17'), with a statistical uncertainty of 6.3 degrees.

The angle from the Fermi LAT boresight is 112.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221118575/quicklook/glg_skymap_all_bn221118575.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/bn221118575/quicklook/glg_healpix_all_bn221118575.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221118575/quicklook/glg_lc_medres34_bn221118575.gif


GRB_name: GRB221114A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32947
SUBJECT: GRB 221114A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/11/18 18:23:28 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 221114A (GECAM GCN Notice #67) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 15:19:37.44 UTC on 14 November  2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1352474360/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a single pulse which starts
at T+1.4 sec, peaks at T+17.6 sec, and ends at T+20.1 sec.
The T90 and T50 durations measured by the SGM data are 15.9 +/- 1.0 sec
and 8.5 +/- 0.5 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1352474360/

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


GRB_name: GRB221115B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32948
SUBJECT: GRB 221115B: CALET Gamma-Ray Burst Monitor detection
DATE:    22/11/18 19:06:45 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 221115B (Swift/BAT-GUANO arcminute localization: DeLaunay et al.,
GCN Circ. 32941) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 09:46:15.63 UTC on 15 November 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1352540756/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows two pulses.  
The first faint pulse is around T-12 s, and the second main pulse starts
at T+0.0 sec, peaks at T+0.6, sec, and ends at T+2.4 sec.
The T90 and T50 durations measured by the SGM data are 2.1 +/- 0.2 sec
and 0.9 +/- 0.3 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1352540756/

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


GRB_name: GRB221009A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32949
SUBJECT: GRB 221009A: Japanese VLBI Network observation
DATE:    22/11/19 04:37:23 GMT
FROM:    Kotaro Niinuma at Yamaguchi University  <niinuma@yamaguchi-u.ac.jp>

=========================================================================

K. Niinuma (Yamaguchi Univ.), Y. Yonekura (Ibaraki Univ.), K. Fujisawa, 
K. Motogi (Yamaguchi Univ.), and W. Iwakiri (Chiba Univ.)

We carried out the very long baseline interferometry (VLBI) observations 
of GRB221009A/Swift J1913.1+1946 (Dichiara et al. GCN 32632, ATel 15650) 
at 9:00 - 10:15 UT on October 11, at 8:00 - 9:15 on October 25 and 26, 
2022 (1.82 days, 15.78 days, and 16.78 days after the Fermi-GBM trigger 
(Veres et al. GCN 32632), respectively).

The observation was performed in both C-band (center frequency of 6856 
MHz with a bandwidth of 512 MHz) and X-band (center frequency of 8448 
MHz with a bandwidth of 512 MHz), simultaneously by single baseline 
interferometry consisting of Yamaguchi-34m radio telescope operated by 
Yamaguchi University and Hitachi-32m radio telescope operated by Ibaraki 
University. Both telescopes recorded only left-circular polarization. 
This array is a part of the Japanese VLBI Network and the baseline 
length is of 873 km.

GRB221009A/Swift J1913.1+1946 was successfully detected on October 11, 
and its VLBI flux densities were 13+/â€“3 mJy at 6.86 GHz and of 11+/-3 
mJy at 8.45 GHz. On the other hand, it was not detected on October 25 
and 26, and the 5-sigma upper limits of VLBI flux density were 3mJy at 
both 6.86GHz and 8.45GHz. The bright quasar J1905+1943 was also observed 
to determine the VLBI flux density of GRB221009A/Swift J1913.1+1946. The 
radio emission from the very compact component detected by our VLBI 
observation showed slightly steep spectrum in radio band on 1.82 days 
after the Fermi-GBM trigger.

=========================================================================



-- 
NIINUMA Kotaro
Graduate School of Sciences and Technology for Innovation,
Yamaguchi Univ., Yoshida 1677-1, Yamaguchi 753-8512, Japan
Phone: +81-(0)83-933-5759
E-mail:niinuma@yamaguchi-u.ac.jp

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GRB_name: GRB221119A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32950
SUBJECT: GRB 221119A: Fermi GBM Final Real-time Localization
DATE:    22/11/19 15:13:22 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 15:02:53 UT on 19 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221119A (trigger 690562978.639846 / 221119627).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 147.0, Dec = -12.9 (J2000 degrees, equivalent to J2000 09h 48m, -12d 54'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 89.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221119627/quicklook/glg_skymap_all_bn221119627.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/bn221119627/quicklook/glg_healpix_all_bn221119627.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221119627/quicklook/glg_lc_medres34_bn221119627.gif


GRB_name: GRB221119A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32952
SUBJECT: GRB 221119A: Fermi-LAT detection
DATE:    22/11/20 14:15:17 GMT
FROM:    Francesco Longo at U of Trieste,INFN Trieste  <franzlongo1969@gmail.com>

Longo F. (University and INFN Trieste), Pillera R. (Politecnico and INFN, Bari)
and Palatiello M. (University of Udine and INFN Trieste) report
on behalf of the Fermi-LAT team:

On November, 19, 2022 Fermi-LAT detected high-energy emission
from GRB 221119A, which was also detected by Fermi-GBM
(trigger 221119627 / 690562978, GCN 32950) at 15:02:53 UT .

The best LAT on-ground location is found to be

RA, Dec = 144.6, -14.5 (J2000)

with an error radius of 0.6 deg (90 % containment, statistical error only).
This was at 85 deg from the LAT boresight at the time of the trigger.

The GRB entered in the LAT field of view only after 3.5 ks from
the trigger time.

The 100 MeV - 1 GeV photon flux in the time interval 3500-5000 s
after the GBM trigger is (2.1 +/- 0.8) E-06 ph/cm2/s.
The estimated integrated photon index above 100 MeV is -1.9 +/- 0.3.
The highest-energy photon is a 2.6 GeV event with 99% probability
which is observed around 4600 seconds after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is
Michele Palatiello (michele.palatiello@gmail.com).

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


GRB_name: GRB221119A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32953
SUBJECT: GRB 221119A: Detection by GRBAlpha
DATE:    22/11/20 15:07:20 GMT
FROM:    Andras Pal at Konkoly Observatory  <apal@konkoly.hu>

A. Pal (Konkoly Observatory), J. Ripa, M. Dafcikova, N. Werner (Masaryk 
U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly 
Observatory), F. Munz, N. Husarikova, J.-P. Breuer, M. Topinka, 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 221119A (Fermi/GBM detection: GCN Circ. 32950; 
GECAM-B detection at 2022-11-19 15:02:54.65 UT, trigg. num. 72; also 
detected by INTEGRAL/SPI-ACS) was detected by the GRBAlpha 1U CubeSat (Pal 
et al. Proc. SPIE 2020). The first double-peaked signal, acquired with a 
1-second cadence was confirmed with a ~14 sigma detection at the peak 
times of 2022-11-19 15:02:55 and 15:02:58 UTC, respectively. In addition, 
the presence, duration and amplitude of the second peak is also confirmed 
by the GRBAlpha light curve 40-50 seconds after the double peaks. The T90 
duration of this GRB is 54 seconds and the overall significance during T90 
reaches 23.5.

The light curve obtained by GRBAlpha is available here: 
https://grbalpha.konkoly.hu/static/share/GRB221119A_GCN.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a 
future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its detector 
consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously upgrading the 
on-board data acquisition software stack. The ground segment is also 
supported by the radio amateur community, and it takes advantage of the 
SatNOGS network for increased data downlink volume, also allowing us the 
retrieval with a small latency. We would like to thank the support of the 
operators of the individual receiver stations as well as the maintenance 
of the network itself.


GRB_name: GRB221119A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32954
SUBJECT: GRB 221119A: Fermi GBM detection
DATE:    22/11/20 16:31:02 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 15:02:53.64 UT on 19 November 2022, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 221119A (trigger 690562978 / 221119627)
which was also detected by the Fermi-LAT (Longo et al. 2022, GCN 32952).
The Fermi GBM Final Real-time Localization (GCN 32950) is consistent with
the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger time is 90
degrees.

The GBM light curve consists of multiple peaks followed
by some extended emission with a duration (T90) of about 66 s (50-300 keV).
The time-averaged spectrum from T0 s to T+74.75 s
is best fit by Band function, with Epeak = 132 +/- 11 keV,
alpha = -1.18 +/- 0.04 and beta = -1.97 +/- 0.04.

The event fluence (10-1000 keV) in this time interval is
(4.02 +/- 0.07)E-05  erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.84 s in the 10-1000 keV band
is 18.0 +/- 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: GRB221120A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32955
SUBJECT: GRB 221120A: Swift detection of a likely short burst
DATE:    22/11/20 21:57:40 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

R. A. J. Eyles-Ferris (U Leicester), J.D. Gropp (PSU),
J. A. Kennea (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 21:29:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221120A (trigger=1141030). Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 41.3225  43.1970 which is 
   RA(J2000) = 02h 45m 17s
   Dec(J2000) = 43d 11' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT trigger duration was 0.256 s, suggesting
a possible short burst.  Due to a telemetry gap, no further BAT information
will be available until ground contact. 

Using promptly downlinked data we find an uncatalogued X-ray source
with an enhanced position: RA, Dec 41.33852, 43.24280 which is
equivalent to:
   RA(J2000)  = 02h 45m 21.24s
   Dec(J2000) = +43d 14' 34.1"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). 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 does not constrain the column density. 

UVOT took a finding chart exposure of 150 seconds with the White
filter. No credible afterglow candidate has been found in the initial
data products. The 2.7'x2.7' sub-image covers 0% 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. 

Burst Advocate for this burst is R. A. J. Eyles-Ferris (raje1 AT leicester.ac.uk). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB221120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32956
SUBJECT: GRB 221120A: GIT upper limits on optical afterglow
DATE:    22/11/21 01:24:33 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

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

We observed the short GRB 221120A detected by Swift (R. A. J. Eyles-Ferris et al., GCN 32955), with the 0.7m GROWTH-India Telescope (GIT). The observations started at 22:31:28 UT on 2022-11-20, 62 mins after the Swift trigger. We obtained multiple 300-sec exposures in the g', r' and i' filters. We did not detect any new source in our stacked images within the 1.9 arcsec radius circle around R.A.= 02h 45m 21.24s, Dec.= +43d 14' 34.1". The obtained upper limits follow as:
-------------------------------------------------------------------
JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Lim_mag (5-sigma) |
-------------------------------------------------------------------
2459904.44036416 | 1.08 | 3 x 300 (stacked) | g' | > 21.24 |
2459904.46842522 | 1.75 | 8 x 300 (stacked) | r' | > 21.37 |
2459904.46658235 | 1.70 | 3 x 300 (stacked) | i' | > 20.44 | 
-------------------------------------------------------------------

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 <https://iopscience.iop.org/article/10.3847/1538-3881/ac7bea <https://iopscience.iop.org/article/10.3847/1538-3881/ac7bea>>) 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/ <https://sites.google.com/view/growthindia/>.


GRB_name: GRB221120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32957
SUBJECT: GRB 221120A: LDT Optical Afterglow Candidate
DATE:    22/11/21 02:57:19 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), I. Andreoni (UMD), S. B. Cenko (NASA/GSFC),
E. Troja (UTV/ASU), S. Dichiara (PSU), A. Kutyrev (NASA/GSFC),
S. Veilleux (UMD), J. Durbak (UMD), on behalf of a larger collaboration:

We performed target of opportunity observations of GRB 221120A
(Eyles-Ferris et al., GCN 32955) with the 4.3m Lowell Discovery
Telescope in Happy Jack, AZ. Observations began on October 21,
2022 at 01:32:08.76 UT corresponding to ~4 hr after the GRB.
We obtained 8x150 s exposures in r-band under good conditions.

At the North-East edge of the XRT localization we detect a faint
source with magnitude r~24.1 AB mag. The source position is:

RA, DEC (J2000) = 02:45:21.36, 43:14:34.9 +/- 0.5"

No other sources are detected within 5" of the GRB localization to
depth r>24.5 AB mag. At present we cannot evaluate whether this
source is the counterpart to GRB 221120A. These results are consistent
with previous upper limits (Swain et al., GCN 32956).

We note the presence of a nearby bright galaxy at an offset of
~16.5" from the center of the XRT localization (Eyles-Ferris et al.,
GCN 32955). The galaxy has a photometric redshift from SDSS of z~0.12.
At this redshift, the offset from the XRT position is ~37 kpc. The
probability of chance coincidence is Pcc<0.05. Therefore. this is a
plausible host galaxy of GRB221120A.

Magnitudes are calibrated against nearby SDSS stars.

These magnitudes are not corrected for Galactic interstellar
reddening E(B-V)~0.08 mag.

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

Further observations are planned.


GRB_name: GRB221120A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32958
SUBJECT: GRB 221120A: Swift/UVOT Upper Limits
DATE:    22/11/21 04:53:00 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

Paul Kuin (MSSL/UCL) and Rob Eyles-Ferris (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 221120A
208 s after the BAT trigger (Eyles-Ferris et al., GCN Circ. 32955).
An optical detection in r' has been reported by O'Connor et al.
(GCN Circ. 32957).
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

u_FC               208          458          246         >19.9
white              761          911          295         >21.0
u                  208          458          246         >19.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.093 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221120A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32959
SUBJECT: GRB 221120A is a short burst
DATE:    22/11/21 05:30:03 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Confirming the "likely" classification from GCN 32955, GRB 221120A has a
measured T90 duration of ~0.8 seconds (15-195 keV) in the Swift/BAT data.
Followup is encouraged.


GRB_name: GRB221121A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32960
SUBJECT: GRB 221121A: Fermi GBM Final Real-time Localization
DATE:    22/11/21 06:45:10 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 06:34:49 UT on 21 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221121A (trigger 690705294.743784 / 221121274).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 168.8, Dec = 71.1 (J2000 degrees, equivalent to J2000 11h 15m, 71d 05'), with a statistical uncertainty of 1.1 degrees.

The angle from the Fermi LAT boresight is 18.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221121274/quicklook/glg_skymap_all_bn221121274.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/bn221121274/quicklook/glg_healpix_all_bn221121274.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221121274/quicklook/glg_lc_medres34_bn221121274.gif


GRB_name: GRB221120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32961
SUBJECT: GRB221120A: Montarrenti Observatory Upper Limit
DATE:    22/11/21 07:30:57 GMT
FROM:    Simone Leonini at Monarrenti Obs  <s.leonini@iol.it>

<!doctype html>
<html>
 <head> 
  <meta charset="UTF-8"> 
 </head>
 <body>
  <p class="default-style"></p>
  <p dir="ltr">Simone Leonini, M. Conti, P. Rosi and L.M. Tinjaca Ramirez (Montarrenti Observatory, Siena, Italy) report:</p>
  <p dir="ltr">We observed the field of the short GRB221120<a href="tel:221120"></a>A (Trigger 1141030, R.A.J. Eyles-Ferris et al., GCN Circ. 32955) with the automatic 0.53m RC telescope + U47 detector at Montarrenti Observatory (Siena, Italy, IAU code C88).</p>
  <p dir="ltr">The observations were started under good weather conditions at 2022-11-20 22:35:10 UT (2.240s after notice) stacking 10x30s clear filter CCD exposures.</p>
  <p dir="ltr">We have not found optical transient within the error-box of the Neil Gehrels Swift Observatory position (RA 02h 45m 17.00s, Dec +43d 11m 49.0s - J2000).<br> Mag. upper limit R = 19.86+/-0.14</p>
  <p dir="ltr">Magnitudes were obtained from USNO-B1 catalogue and are not corrected for galactic extinction.</p>
  <p dir="ltr">Observations are consistent with previous upper limits (Swain et al., GCN 32956).<br></p>
 </body>
</html>


GRB_name: GRB221120A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32962
SUBJECT: GRB 221120A: Enhanced Swift-XRT position
DATE:    22/11/21 08:24:43 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 1363 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 221120A, 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 = 41.33982, +43.24315 which is equivalent
to:

RA (J2000): 02h 45m 21.56s
Dec (J2000): +43d 14' 35.4"

with an uncertainty of 2.4 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB221120A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32963
SUBJECT: GRB 221120A: Swift-XRT refined Analysis
DATE:    22/11/21 12:45:58 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 8.4 ks of XRT data for GRB 221120A (Eyles-Ferris et
al. GCN Circ. 32955), from 103 s to 47.0 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Goad et al. (GCN Circ. 32962).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.6 (+/-0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+1.1, -0.9). The
best-fitting absorption column is  3.2 (+2.4, -1.7) x 10^22 cm^-2, in
excess of the Galactic value of 1.2 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 7.9 x 10^-11 (1.8 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+2.4, -1.7) x 10^22 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 3.0 sigma
Photon index:      1.9 (+1.1, -0.9)

If the light curve continues to decay with a power-law decay index of
1.6, the count rate at T+24 hours will be 8.2 x 10^-6 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.5 x
10^-16 (1.5 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01141030.

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


GRB_name: GRB221120A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32964
SUBJECT: GRB 221120A: Fermi GBM observation
DATE:    22/11/21 15:15:14 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 21:29:27.85 UT on 20 November 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 221120A (trigger 690672572 / 221120895)
which was also detected by the Swift/BAT (Eyles-Ferris et al., GCN 32955).
The GBM on-ground location is consistent with the Swift position.


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


The GBM light curve consists of two pulses
with a duration (T90) of about 0.64 s (50-300 keV).
The time-averaged spectrum from T0-0.13 s to T0+0.58 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is 0.11 +/- 0.31 and
the cutoff energy, parameterized as Epeak, is 379 +/- 65 keV.

The event fluence (10-1000 keV) in this time interval is
(7.8 +/- 0.9)E-7 erg/cm^2. The 64 ms peak photon flux measured
starting from T0+0.38 s in the 10-1000 keV band
is 7.45 +/- 0.91 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: GRB221120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32965
SUBJECT: GRB 221120A: Archival PS1 Imaging of Faint Source near XRT position
DATE:    22/11/21 19:18:20 GMT
FROM:    Jillian Rastinejad at Northwestern Univ.  <jillianrastinejad2024@u.northwestern.edu>

J. Rastinejad, C. D. Kilpatrick, A. E. Nugent and W. Fong  (Northwestern) report:

We analyzed stacked images from the Pan-STARRS 3pi Data Release 1 image archive (Flewelling et al. 2016) of the location of the short-duration GRB 221120A (Eyles-Ferris et al., GCN 32955, Tohuvavohu et al., GCN 32959).  We detect a faint source in multiple bands centered at

RA (J2000): 02:45:21.31
Dec (J2000): +43:14:35.35

This source is just outside the enhanced XRT position (90% confidence, Goad et al., GCN 32962) and marginally consistent with the optical source reported by O'Connor et al. (GCN 32957) using their reported 0.5'' uncertainty. Performing forced aperture photometry of the source with an aperture approximately equal to the FWHM size (0.9 - 2.0''), we measure the following magnitudes:

g > 23.8 mag
r = 23.2 +/- 0.5 mag
i = 23.1 +/- 0.3 mag
z = 23.5 +/- 0.5 mag
y = 22.0 +/- 0.4 mag

All magnitudes are in the AB system. The source appears extended although the low S/N precludes a firm conclusion. Using the i-band magnitude and an offset of 2.7'' between the centers of this possible galaxy and the XRT position, we calculate a probability of chance coincidence (Pcc; Bloom et al. 2002) of 0.05. The bright, offset galaxy previously reported by O'Connor et al. (GCN 32957), PSO J041.3414+43.242, is also apparent in the PS1 imaging, and for which we measure r_AB = 17.6 mag (similar to the tabulated SDSS magnitude for this source). At an angular offset of 13.2'', we find a Pcc of 0.02.

Thus, it is possible that the optical afterglow candidate reported by GCN 32957 is actually the galaxy apparent in PS1 imaging. Given the comparable Pcc values of both sources, it is difficult to make a clear host association with present information. Confirmation of a fading counterpart is critical to refining the position of the counterpart and determining the true host.


GRB_name: GRB221120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32966
SUBJECT: GRB 221120A: Liverpool Telescope Upper Limits
DATE:    22/11/21 22:03:04 GMT
FROM:    Ben Gompertz at U of Birmingham  <b.gompertz@bham.ac.uk>

B. P. Gompertz, M. Nicholl (U. Birmingham), N. Tanvir, G. Lamb, P. O'Brien (U. Leicester) and K. Wiersema (U. Lancaster) report:
 
We observed short GRB 221120A (Eyles-Ferris et al., GCN 32955) with the IO:O optical camera on the 2m robotic Liverpool Telescope. Observations began on November 20, 2022 at 23:50:33 UT (~2.5h after the Swift trigger) and consist of a series of 10x150s exposures in each of the SDSS r' and i' filters.

We place the following 3-sigma upper limits on an optical source at the location of the the X-ray afterglow (Goad et al., GCN 31962) at the time of observation:
 
r' > 21.82
i' > 21.88
 
Magnitudes are in the AB system, calibrated against nearby PS1 stars, and are not corrected for the Galactic reddening of E(B-V) = 0.08 magnitudes along the line of sight (Schlafly & Finkbeiner 2011). Our observations are only weakly constraining to any evolution in the afterglow candidate identified by O'Connor et al. (GCN 32957), precluding power-law decays steeper than ~t^-4 between the two epochs.


GRB_name: GRB221120A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32967
SUBJECT: GRB221120A: WIRC near-IR imaging of the afterglow candidate
DATE:    22/11/22 00:37:56 GMT
FROM:    Viraj Karambelkar at Indian Inst of Tech,Bombay  <karambelkarvraj21197@gmail.com>

Viraj Karambelkar (Caltech), Zach Vanderbosch (Caltech), Mansi Kasliwal
(Caltech), Igor Andreoni (U. of Maryland)

We observed the location of the short duration GRB 221120A (Eyles-Ferris et
al., GCN 32955, Tohuvavohu et al., GCN 32959) in the NIR J-band with the
Wide-Field Infrared Camera (WIRC, Wilson et al. 2003) on the 200-inch Hale
telescope at Palomar Observatory. Observations began on November 21, 2022
at 06:22:07 UT (approx. 9 hours since the Swift detection), and comprise a
series of 30x45 second exposures.

We detect a faint source centered at RA = 02:45:21.3, Dec = +43:14:35.2
(J2000).

Performing forced aperture photometry at the location of this source
suggests a J-band magnitude of

m_J = 22.0 +/- 0.3 mag (AB).


This source is spatially coincident with that reported by Rastinejad et al.
(GCN 32965) from archival PS1 images, and also consistent with the position
of the LDT afterglow candidate (O'Connor et al., GCN 32957).

The magnitude reported above is not corrected for Galactic interstellar
reddening E(B-V)~0.08 mag


GRB_name: GRB221120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32968
SUBJECT: GRB 221120A: AKO Telescope Upper Limits
DATE:    22/11/22 04:39:10 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. 

 

We observed the short GRB 221120A detected by Swift (R. Eyles-Ferris et al.,
GCN 32955), with our 0.35m telescope. The observation was done on 21
November 2022 from 15:36:06 to 15:48:28 (UT), 18.2 hours after the Swift
trigger. We obtained multiple 180-sec exposures in Ic filter. We did not
detect any afterglow within XRT localization (M.R. Goad et al., GCN 32962).

 

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

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

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

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

2459905.155422, 18.2, 5 x 180 (stacked), Ic, > 19.5

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

 

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB221121A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32969
SUBJECT: GRB221121A: AstroSat CZTI detection
DATE:    22/11/22 10:53:13 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 CIFT framework (Sharma et al., 
2021, JApA, 42, 73) showed the detection of a long GRB221121A which was 
also detected by Fermi GBM (GCN Circ. 32960).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-11-21 06:34:50.5 UTC. The measured peak count 
rate associated with the burst is 173 (+42, -40) counts/s above the 
background in the combined data of all quadrants, with a total of 1531 
(+490, -529) counts. The local mean background count rate was 532 (+3, 
-4) counts/s. Using cumulative rates, we measure a T90 of 22 (+15, -9) 
s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-11-21 
06:34:53.9 UTC. The measured peak count rate is 283 (+79, -30) counts/s 
above the background in the combined Veto data of all quadrants, with a 
total of 3488 (+696, -662) counts. The local mean background count rate 
was 1746 (+6, -6) counts/s. We measure a T90 of 22 (+10, -4) s from the 
cumulative Veto light curve.

CZTI GRB detections are reported regularly on the payload site at 
http://astrosat.iucaa.in/czti/?q=grb. 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: GRB221120A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32970
SUBJECT: GRB 221120A: Swift-BAT refined analysis
DATE:    22/11/22 18:45:41 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

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

Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 221120A (trigger #1141030)
(Eyles-Ferris et al., GCN Circ. 32955). The BAT ground-calculated position is
RA, Dec = 41.363, 43.241 deg which is
   RA(J2000)  =  02h 45m 27.1s
   Dec(J2000) = +43d 14' 26.5"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.

The BAT  light curve shows several peaks within a duration of ~1 sec
T90 (15-350 keV) is 0.79 +- 0.16 sec (estimated error including systematics).

The time-averaged spectrum from T-0.60 to T+0.27 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.85 +- 0.27.  The fluence in the 15-150 keV band is 1.1 +- 0.2 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T-0.67 sec in the 15-150 keV band
is 1.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1141030/BA/


GRB_name: GRB221121A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32971
SUBJECT: IPN triangulation of GRB 221121A (long)
DATE:    22/11/22 21:00:17 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

J. Benkhoff on behalf of the BepiColombo team,

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

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

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

and

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

The long-duration GRB 221121A
(Fermi-GBM detection: Fermi GBM Team, GCN Circ. 32960;
AstroSat-CZTI detection: Gopalakrishnan et al., GCN Circ. 32969)
has been detected by Fermi (GBM trigger 690705294), Konus-Wind,
INTEGRAL (SPI-ACS), AstroSat (CZTI), CALET (CGBM), GECAM-B
(trigger tn221121_063449_fb), Swift (BAT), and BepiColombo (MGNS),
so far, at about 23690 s UT (06:34:50).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  163.104 (10h 52m 25s) +69.356 (+69d 21' 22")
 Corners:
  164.660 (10h 58m 38s) +69.887 (+69d 53' 12")
  164.681 (10h 58m 43s) +70.133 (+70d 08' 00")
  161.617 (10h 46m 28s) +68.809 (+68d 48' 31")
  161.623 (10h 46m 30s) +68.558 (+68d 33' 29")
 ---------------------------------------------
The error box area is 952 sq. arcmin, and its maximum
dimension is 1.9 deg (the minimum one is 9 arcmin).
The Sun distance was about 103 deg.

This localization may be improved.

The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM final localization (GCN Circ. 32960).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221121_T23691/IPN

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


GRB_name: GRB221120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32972
SUBJECT: GRB 221120A: GTC Confirmation of an Underlying Galaxy
DATE:    22/11/22 23:02:37 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), N. Butler (ASU), A. Watson (UNAM),
E. Troja (UTV/ASU), S. Dichiara (PSU), on behalf of a
larger collaboration:

We observed the short GRB 221120A (Eyles-Ferris et al., GCN 32955,
Tohuvavohu et al., GCN 32959) using OSIRIS at the 10.4m Gran Telescopio
Canarias (GTC). The observation started on November 22, 2022 at
00:44:32 UTC (~1.13 d) for a total exposure of 540 s in r-band.

At the location of the source reported by O'Connor et al. (GCN 32957)
we detect a source with magnitude r~24.38+/-0.08 AB mag calibrated using
nearby SDSS stars. This serves as confirmation of the underlying galaxy
(Rastinejad et al., GCN 32965) and demonstrates a lack of fading of the
source found by O'Connor et al. (GCN 32957). While the host association
is unclear, if this galaxy is associated to GRB 221120A, the observed
r-J color (Karambelkar et al., GCN 32967) suggests that GRB 221120A was
a distant event (see, e.g., O'Connor et al. 2022, MNRAS, 515, 4890).

We thank the GTC staff for rapidly scheduling and executing these
observations.


GRB_name: GRB221009A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32973
SUBJECT: GRB 221009Aï¼šDAMPE observed a 34.7 GeV p
DATE:    22/11/23 01:26:16 GMT
FROM:    Kai-Kai Duan at Purple Mountain Observatory  <duankk@pmo.ac.cn>

Kai-Kai Duan (Purple Mountain Observatory), Zun-Lei Xu (PMO), Zhao-Qiang Shen (PMO), Wei Jiang (PMO), Lu-Yao Jiang (PMO), Dong-Ya Guo (Institute of High Energy Physics), Wen-Xi Peng (IHEP), Fabio Gargano (Istituto Nazionale di Fisica Nucleare) and Xiang Li (PMO), report on behalf of the DAMPE collaboration: We report the observation of GRB 221009A with DAMPE, which has been reported by Swift (Kennea et al. GCN #32635, Krimm et al. GCN #32688), Fermi-GBM (Veres et al. GCN #32636, Lesage et al. GCN #32642), Fermi-LAT (Bissaldi et al. GCN #32637, Pillera et al. GCN #32658, Xia et al. GCN #32748), LHAASO (Huang et al. GCN #32677) and so on. Though the GRB is about 90 deg from the boresight of DAMPE at the moment of Fermi-GBM trigger (out of the normal FOV), the Unbiased-Trigger counts of DAMPE increased significantly from 227 to 233 seconds after the Fermi-GBM trigger. We believe that about 21 out of 35 events during the 6-second timespan were from the GRB, and the highest deposit energy is 2.4 GeV for these events.  The FOV of DAMPE began to cover the GRB position about one hour later, and it observed a 34.7 GeV (RA = 289.93 deg, DEC = 19.96 deg) photon at 1.58 deg (with the 95% containment of the PSF as ~ 2 deg) from the swift localization of this GRB (RA = 288.265 deg, Dec = 19.774 deg, from Dichiara et al. GCN #32632) 4896 seconds after the Fermi-GBM trigger. The p-value of this photon emitted from background is 0.0003, corresponding to 3.6-sigma significance locally. During the past 6-year observation, DAMPE observed only one photon with energy above 30 GeV within 2 deg around this GRB position. At 9.37 and 16.26 days after the Fermi-GBM trigger, DAMPE observed 8.33 GeV (RA = 287.82 deg, DEC = 20.35 deg) and 10.74 GeV (RA = 287.48 deg, DEC = 19.88 deg) photons around 0.71 deg and 0.75 deg from the LAT localization of GRB 221009A. The local significance of these two photons are 3.10 and 3.22 sigma, respectively. The 95% containment of the PSF above 10 GeV is about 2 deg.  The detailed data analysis is still on going. DAMPE is a satellite for dark matter detection indirectly, cosmic-ray physics and gamma-ray astronomy by detection of the high-energy electrons, cosmic rays and gamma rays.


Key Laboratory of Dark Matter and Space Astronomy
Purple Mountain Observatory
Chinese Academy of Sciences
Nanjing 210008
P.R.China
email: duankk@pmo.ac.cn


GRB_name: GRB221121A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32974
SUBJECT: GRB 221121A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/11/23 07:05:35 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 221121A (Fermi GBM Final Real-time Localization:
Fermi GBM team, GCN Circ. 32960; AstroSat CZTI detection:
Gopalakrishnan et al., GCN Circ 32969; IPN triangulation: 
Kozyrev etc al., GCN Circ. 32971) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 06:34:47.10 UTC on 21 November 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1353047657/index.html).
The burst signal was seen by only SGM detector.

The burst light curve shows a single pulse which starts
at T+2.6 sec, peaks at T+3.1 sec, and ends at T+30.2 sec.
The T90 and T50 durations measured by the SGM data are 24.1 +/- 0.8 sec
and 10.1 +/- 1.7 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1353047657/

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


GRB_name: GRB221120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32976
SUBJECT: GRB 221120A: VIRT Optical Upper Limit
DATE:    22/11/23 18:55:14 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

R. Querrard (UVI), P. Gokuldass (Florida Institute of Technology), N.
Orange (OrangeWave Innovative Science, LLC), K. Noonan (UVI), K. Smith
(UVI), D. Morris (UVI) report:

We observed the field of GRB221120A (R. A. J. Eyles-Ferris et al., GCN
32955) with the 0.5m Virgin Island Robotic Telescope (VIRT) at the
University of the Virgin Islands' Etelman observatory on 11-21-2022
starting at 01:20:09 UT (T+3.8 hrs). We performed a series of exposures in
the R filter with a total exposure of 4000 s. The weather conditions were

partly cloudy to cloudy during the hours of observation with an average
airmass of 1.1.

We detect no new source within the enhanced XRT position error circle (Goad
et al., GCNC 32962) consistent with other non-detections (Swain et al., GCN
32956, O'Connor

et al., GCN 32957, Leonini et al. GCN 32961, Gompertz et al, GCN 32966; and
Odeh et al., GCN 32968) and report the following 5-sigma upper limit:

T_mid            ||Exposure     ||Filter      ||Limit

T+ 4.3  hrs     ||4000s          ||R            ||>20.34

The limit is estimated from comparison to nearby USNO B1 stars and is not
corrected for Galactic extinction. The VIRT is still in the commissioning
phase.

We acknowledge financial support from NASA MUREP MIRO award 80NSSC21M0001,
NASA EPSCoR award 80NSSC22M0063, and NSF EiR award 1901296. R.Q. and N.B.O.
also acknowledge financial support from South Carolina Space Grant award
80NSSC20M0054. This message can be cited.


GRB_name: GRB221122A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32977
SUBJECT: GRB 221122A: Detection by GRBAlpha
DATE:    22/11/23 19:58:52 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), F. Munz, N. Husarikova, J.-P. Breuer, M. Topinka, 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 Metropo
 litan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The short-duration GRB 221122A (GECAM-B detection at 2022-11-22 02:43:26.65 UT, trigger no. 77) was detected by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The subthreshold detection was confirmed at the peak time 2022-11-22 02:43:26 UTC. The GRB has a T90 duration of 2 s and the overall significance during T90 reaches 4.3. The duration and the detection time of the event are consistent with the GRB reported by the GECAM-B instrument.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221122A_GCN.pdf

GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Its detector consists of a 75 x 75 x 5 mm^3 CsI(Tl) 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, we are continuously upgrading the on-board data acquisition software stack. 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: GRB221120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32978
SUBJECT: GRB 221120A: TURBO Optical Upper Limit
DATE:    22/11/23 21:10:38 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 221120A (Eyles-Ferris et al., GCN 32955) field with the
Total-Coverage Ultrafast Response to Binary-Mergers Observatory (TURBO)
prototype telescope in St. Paul, Minnesota on November 21, from 01:34 to
01:36 UT (corresponding to 4.08 hours after GRB trigger) in SDSS g-band and
from 02:45 to 02:47 UT (5.25 hours after GRB trigger) in SDSS r-band
filters.

We acquired a series of 5x30s exposures in each band.  We do not detect any
fading uncatalogued sources in the XRT error region in either band, which
is consistent with available optical upper limits (Swain et al., GCN 32956;
Kuin et al., GCN 32958; Gompertz et al., GCN 32966; Odeh et al., GCN 32968;
Querrard et al., GCN 39276).

The following 3-sigma upper limits in AB magnitudes are calculated using
the Pan-STARRS catalog as reference:

g > 16.0

r > 15.4

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: GRB221124A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32981
SUBJECT: GRB 221124A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/11/25 03:33:01 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 221124A (GECAM Trigger #79; IPN RAW Notice at
02:00:24.17 on 24 November) triggered the CALET Gamma-ray Burst
Monitor (CGBM) at 02:00:24.88 UTC on 24 November 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1353290389/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure that starts 
at T-58 sec and ends at T+~350 sec. We are not able to obtain 
the duration because of the scheduled HV turn-off started just 
after the end of the emission. 

The ground-processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1353290389/

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


GRB_name: GRB221120A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32982
SUBJECT: GRB 221120A: Detection by VZLUSAT-2
DATE:    22/11/25 13:43:19 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.

A short-duration GRB 221120A (Swift/BAT detection: Eyles-Ferris et al., 
GCN Circ. 32955; Fermi/GBM detection: Veres and Meegan et al., GCN Circ. 
32964; GECAM-B detection trig. num. 75; INTEGRAL/SPI-ACS detection peak 
at 2022-11-20 21:29:28 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 
subthreshold detection was confirmed at the peak time 2022-11-20 
21:29:27 UTC. The T90 duration was measured to be 2 s with the light 
curve cadence of 1 s. The overall significance during T90 reaches 4.4 sigma.

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB221120A_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: GRB221124A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32984
SUBJECT: GRB 221124A: Swift/BAT-GUANO detection
DATE:    22/11/26 07:55:10 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 221124A onboard (T0:
2022-11-24T02:00:24 UTC, CALET trig 1353290389, GECAM trig 79).

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

Upon trigger, 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 8 in a 1.024 s
analysis time bin.

NITRATES results, independently, are ambiguous with respect to whether
this burst originates from in or outside the BAT FOV.
The GECAM localization places this burst outside the contemporaneous 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: GRB221126A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32985
SUBJECT: GRB 221126A: Fermi GBM Final Real-time Localization
DATE:    22/11/26 13:18:03 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 13:07:29 UT on 26 Nov 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221126A (trigger 691160854.94316 / 221126547).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 143.5, Dec = 13.1 (J2000 degrees, equivalent to J2000 09h 33m, 13d 05'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 22.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221126547/quicklook/glg_skymap_all_bn221126547.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/bn221126547/quicklook/glg_healpix_all_bn221126547.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221126547/quicklook/glg_lc_medres34_bn221126547.gif


GRB_name: GRB221124A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32986
SUBJECT: IPN triangulation of GRB 221124A (long)
DATE:    22/11/27 15:01:15 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

S. Xiao, S.-L. Xiong, X.-Q. Li, X.-Y. Wen, L.-M. Song, S.-J. Zheng,
W.-X. Peng, and F. Zhang on behalf of the GECAM team,

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

and

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

The long-duration GRB 221124A
(CALET-CGBM detection: Sugita et al., GCN Circ. 32981;
Swift/BAT-GUANO detection: Tohuvavohu et al., GCN Circ. 32984;
GECAM-B detection: Huang et al., ATel 15777)
has been detected by CALET (CGBM), Konus-Wind, INTEGRAL (SPI-ACS),
GECAM-B (GRD), and Swift (BAT), so far,
at about 7224 s UT (02:00:24).
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:
   310.423 (20h 41m 42s) +34.999 (+34d 59' 56")
  Corners:
   317.972 (21h 11m 53s) +25.823 (+25d 49' 21")
   314.677 (20h 58m 42s) +33.947 (+33d 56' 49")
   299.731 (19h 58m 56s) +43.400 (+43d 24' 01")
   305.508 (20h 22m 02s) +36.238 (+36d 14' 17")
  ---------------------------------------------
The error box area is 50 sq. deg, and its maximum
dimension is 23 deg (the minimum one is 3.3 deg).
The Sun distance was about 84 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB221124_T07224/IPN

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


GRB_name: GRB221126A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32987
SUBJECT: GRB 221126A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/11/27 18:14:59 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:
2022-11-26T13:07:29 UTC, Fermi/GBM GCN 32985).

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 11.9 in a
4.096 s analysis time bin.

NITRATES results indicate a burst coming from outside the FOV, with
DeltaLLHOut of -1.

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: GRB221126A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32990
SUBJECT: GRB 221126A: AstroSat CZTI detection
DATE:    22/11/28 13:58:27 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

M. Dixit (IITB), V. Prasad (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 long GRB 221126A which was 
also detected by Fermi-GBM (GCN Cir. 32985) and Swift/BAT-GUANO (GCN 
Cir. 32987).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-11-26 13:07:28.950 UTC. The measured peak 
count rate associated with the burst is 590.6 (+51.2, -55.0) counts/s 
above the background in the combined data of all quadrants, with a total 
of 2093 (+254, -271) counts. The local mean background count rate was 
433.4 (+2.7, -3.0) counts/s. Using cumulative rates, we measure a T90 of 
4.89 (+4.45, -1.03) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-11-26 
13:07:28.640 UTC. The measured peak count rate is 663.6 (+72.1, -79.1) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 1770 (+234, -259) counts. The local mean 
background count rate was 1410.0 (+4.9, -5.4) counts/s. We measure a T90 
of 4.18 (+1.11, -1.24) 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: GRB221127A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32991
SUBJECT: GRB 221127A: Detection by GRBAlpha
DATE:    22/11/28 16:42:39 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, J.-P. Breuer, F. Munz , M. Topinka, 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 Metrop
 olitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.

The GRB 221127A (Fermi-GBM detection at 2022-11-27 08:27:10.52 UT, trigger no. 691230435) was observed by the GRBAlpha 1U CubeSat (Pal et al. Proc. SPIE 2020).

The subthreshold detection was confirmed at the peak time 2022-11-27 08:27:10 UTC. The T90 duration measured by GRBAlpha is 3 s and the overall significance during T90 reaches 3.0. The time of the event is consistent with the GRB reported by Fermi-GBM.

The light curve obtained by GRBAlpha is available here:
https://grbalpha.konkoly.hu/static/share/GRB221127A_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: GRB221126A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32992
SUBJECT: GRB 221126A: AGILE detection
DATE:    22/11/28 17:26:49 GMT
FROM:    Claudio Casentini at INAF-IAPS  <claudio.casentini@inaf.it>

C. Casentini, A. Ursi (INAF/IAPS), F. Lucarelli (SSDC, and INAF/OAR),
M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), C. Pittori, 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),
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 221126A at T0 = 2022-11-26 13:07:29 s
(UTC), reported by Fermi/GBM (GCN #32985), Swift/BAT (GCN #32987) and
AstroSat CZTI (GCN #32990).

The burst is clearly visible in the AGILE scientific ratemeters of the
AntiCoincidence, (AC-Top; 50-200 keV) detector. The event lasted about 6 s
and it released a total number of 25792 counts in the AC-Top detector
(above a background rate of 3388 Hz). The AGILE ratemeters light curves
can be found at http://www.agilescienceapp.it/notices/GRB221126A.png.

At the T0, the event was 51.82 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: GRB221126A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32994
SUBJECT: GRB 221126A: Fermi GBM observation
DATE:    22/11/29 11:59:03 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) and C. Meegan (UAH) report on behalf of the Fermi GBM
Team:

"At 13:07:29.94 UT on 26 November 2022, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 221126A (trigger 691160854 / 221126547).

This event was also observed by Swift/BAT-GUANO (GCN 32987), AstroSat CZTI
(GCN 32990) 
and AGILE (GCN 32992).

The GBM position is reported in the Fermi-GBM Final on-ground Localization
(GCN 32985). 
The angle from the Fermi LAT boresight is 22 degrees.

The GBM light curve shows a structured pulse with a duration (T90) of about
7 s (50-300 keV).
The time-averaged spectrum from T0-0.90 s to T0+8.32 s is best fit by a
power law function 
with an exponential high-energy cutoff.  The power law index is -0.94 +/-
0.03 and the cutoff energy, 
parameterized as Epeak, is 194 +/- 8 keV

The event fluence (10-1000 keV) in this time interval is (9.29 +/- 0.02)E-06
erg/cm^2. The 1.024-sec 
peak photon flux measured starting from T0+4.224 s in the 10-1000 keV band
is 15.7 +/- 0.4 ph/s/cm^2.

A Band function fits the spectrum equally well with Epeak= 190 +/- 10 keV,
alpha = -0.92 +/- 0.04 
and beta = -3.1 +/- 0.6.

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: GRB221009A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32995
SUBJECT: Optical polarization observation of GRB 221009A
DATE:    22/11/30 22:48:23 GMT
FROM:    Ioannis Liodakis at Finnish Centre for Astronomy with ESO  <jliodakis@gmail.com>

E. Lindfors (FINCA), K. Nilsson (FINCA), I. Liodakis (FINCA), A. Kasikov 
(NOT, Aarhus University, Tartu Observatory), I. Negueruela (University 
of Alicante)

We observed gamma-ray burst GRB221009A following the GCN alert #32632 
(Dichiara et al., 2022) in optical polarization. The source was observed 
with the Nordic Optical Telescope (NOT) and the ALFOSC instrument in the 
R-band using the standard setup for linear polarization observations 
(lambda/2 retarder followed by a calcite). The observations started 
2022-10-12 at 20:15UT, i.e. approximately 3 days and 6 hours after the 
trigger (2022-10-09 14:10:17 UT). The observations were performed with 
clear sky with seeing 1.2 arcseconds. As the GRB occurred in crowded 
galactic field the ordinary beam image of the GRB221009A ended up behind 
the extraordinary beam of the nearby bright star. Therefore, we had to 
perform careful modelling of the PSF using the second bright star in the 
field of view and subtracted the modeled PSF from the image. We repeated 
this for each image separately. As the PSF subtraction can result in 
some artifacts to the background, we measured the resulting images with 
small aperture of 1.5 arcsec radius. Using the standard formulas, we 
derived a 2 sigma upper limit of 5.1% percent on the polarization degree.


GRB_name: GRB221201A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32997
SUBJECT: GRB 221201A: Fermi GBM Final Real-time Localization
DATE:    22/12/01 12:35:06 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 12:24:45 UT on 1 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221201A (trigger 691590290.314944 / 221201517).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 263.4, Dec = -70.4 (J2000 degrees, equivalent to J2000 17h 33m, -70d 24'), with a statistical uncertainty of 1.5 degrees.

The angle from the Fermi LAT boresight is 130.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221201517/quicklook/glg_skymap_all_bn221201517.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/bn221201517/quicklook/glg_healpix_all_bn221201517.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221201517/quicklook/glg_lc_medres34_bn221201517.gif


GRB_name: GRB221201A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32998
SUBJECT: GRB 221201A: Swift detection of a burst
DATE:    22/12/01 12:47:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

E. Troja (NASA/GSFC/UMCP), M. G. Bernardini (INAF-OAB),
R. Brivio (INAF-OAB), P. D'Avanzo (INAF-OAB), S. Dichiara (PSU),
P. A. Evans (U Leicester), R. A. J. Eyles-Ferris (U Leicester),
M. Ferro (INAF-OAB), J.D. Gropp (PSU), J. A. Kennea (PSU),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB),
K. L. Page (U Leicester), D. M. Palmer (LANL),
C. Salvaggio (INAF-OAB), T. Sbarrato (INAF-OAB) and
B. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 12:25:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221201A (trigger=1142847).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 266.933, -68.260 which is 
   RA(J2000) = 17h 47m 44s
   Dec(J2000) = -68d 15' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 40 sec.  The peak count rate 
was ~5000 counts/sec (15-350 keV), at ~-13 sec after the trigger. 
(The peak occurred during a pre-planned slew and the nominal trigger
time is the start of the first post-slew image.)

The XRT began observing the field at 12:27:56.2 UT, 170.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 266.9228, -68.2510 which is equivalent to:
   RA(J2000)  = 17h 47m 41.47s
   Dec(J2000) = -68d 15' 03.6"
with an uncertainty of 5.7 arcseconds (radius, 90% containment). This
location is 35 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 0.1 s image was 2.34e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 202 seconds with the U filter starting
337 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. Data
from the list of sources generated on-board are not available at this time. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.065. 

Burst Advocate for this burst is E. Troja (nora.gsfc 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: GRB221124A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32999
SUBJECT: Konus-Wind detection of GRB 221124A
DATE:    22/12/01 18:06:09 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The long-duration GRB 221124A
(CALET-CGBM detection: Sugita et al., GCN Circ. 32981;
Swift/BAT-GUANO detection: Tohuvavohu et al., GCN Circ. 32984;
GECAM-B detection: Huang et al., ATel 15777)
triggered Konus-Wind at T0=7224.17 s UT (02:00:24.170).

The burst light curve shows a multipeaked structure
which starts at ~T0-64 s and has a total duration of ~425 s.
The emission is seen up to 5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB221124_T07224/

As observed by Konus-Wind, the burst
had a fluence of 4.71(-0.98,+1.92)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0-0.006 s,
of 2.17(-0.76,+0.82)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+360.704 s)
is best fit in the 20 keV - 5 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.80(-0.30,+0.38),
the high energy photon index beta = -2.96(-7.04,+0.70),
the peak energy Ep = 172(-35,+47) keV
(chi2 = 74/74 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.70(-0.36,+0.45)
and Ep = 275(-59,+106) keV (chi2 = 47/60 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 47/59 dof).

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


GRB_name: GRB221201A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33000
SUBJECT: Swift GRB 221201A: Global MASTER-Net observations report 
DATE:    22/12/01 18:36:55 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 221201A ( E. Troja et al., GCN 32998) errorbox  21718 sec after notice time and 21801 sec after trigger time at 2022-12-01 18:28:26 UT, with upper limit up to  16.2 mag. Observations started at twilight.  The observations began at zenith distance = 64 deg. The sun  altitude  is -11.5 deg. 

The galactic latitude b = -20 deg., longitude l = 325 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2172144

We obtain a following upper limits.  

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

   21891 |         MASTER-SAAO |   C |   180 | 16.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB221201A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33001
SUBJECT: GRB 221201A: Enhanced Swift-XRT position
DATE:    22/12/01 19:58:22 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 1465 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 221201A, 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 = 266.92463, -68.24884 which is equivalent
to:

RA (J2000): 17h 47m 41.91s
Dec (J2000): -68d 14' 55.8"

with an uncertainty of 2.1 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB221201A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33002
SUBJECT: GRB 221201A: Swift-XRT refined Analysis
DATE:    22/12/01 22:31:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), T.
Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), A. Tohuvavohu (U.
Toronto), D.N. Burrows (PSU) and E. Troja report on behalf of the
Swift-XRT team:

We have analysed 6.4 ks of XRT data for GRB 221201A (Troja et al. GCN
Circ. 32998), from 159 s to 30.1 ks after the  BAT trigger. The data
comprise 375 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. 33001).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=5.33 (+0.28, -0.27). At T+214 s  the decay
steepens to an alpha of 6.37 (+0.24, -0.17) before breaking again at
T+368 s to a final decay with index alpha=0.907 (+/-0.026).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.18 (+/-0.06). The
best-fitting absorption column is  3.41 (+0.17, -0.16) x 10^21 cm^-2,
in excess of the Galactic value of 7.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.93 (+0.13, -0.12)
and a best-fitting absorption column of 2.7 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (5.3 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 7.5 x 10^20 cm^-2
Excess significance: 6.5 sigma
Photon index:      1.93 (+0.13, -0.12)

If the light curve continues to decay with a power-law decay index of
0.907, the count rate at T+24 hours will be 0.049 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-12 (2.6 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01142847.

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


GRB_name: GRB221201A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33003
SUBJECT: GCN: GRB 221201A: Swift/UVOT Upper Limits
DATE:    22/12/02 13:27:29 GMT
FROM:    Samantha Oates at MSSL  <samantha.oates@alumni.ucl.ac.uk>

S. R. Oates (U.Birmingham) and E. Troja (NASA/GSFC/UMCP)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 221201A
179 s after the BAT trigger (Troja et al., GCN Circ. 32998).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 33001)
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           179          329          147         >20.1
white              179         1970          225         >20.2
v                 1479         2020           78         >17.8
b                 1404         2107           85         >18.8
u                  337         2094          277         >19.2
w1                1529         2069           78         >18.4
m2                1504         2045           78         >18.5
w2                1454         1996           78         >18.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.066 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221202A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33005
SUBJECT: GRB 221202A: Swift detection of a burst
DATE:    22/12/02 20:20:01 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

R. Caputo (GSFC), M. G. Bernardini (INAF-OAB), R. Brivio (INAF-OAB),
P. D'Avanzo (INAF-OAB), S. Dichiara (PSU),
R. A. J. Eyles-Ferris (U Leicester), M. Ferro (INAF-OAB),
J.D. Gropp (PSU), N. J. Klingler (GSFC/UMBC/CRESSTII),
H. A. Krimm (NSF), A. Y. Lien (U Tampa), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. M. Parsotan (GSFC/UMBC/CRESSTII),
C. Salvaggio (INAF-OAB), A. Tohuvavohu (U Toronto) and
M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 20:06:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221202A (trigger=1142997).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 77.095, -59.806 which is 
   RA(J2000) = 05h 08m 23s
   Dec(J2000) = -59d 48' 21"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 20 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 20:07:48.2 UT, 97.6 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 77.08221,
-59.83213 which is equivalent to:
   RA(J2000)  = 05h 08m 19.73s
   Dec(J2000) = -59d 49' 55.7"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 96 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.11
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 101 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
0.027. 

Burst Advocate for this burst is R. Caputo (regina.caputo 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: GRB221202B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33006
SUBJECT: GRB 221202B: Fermi GBM Final Real-time Localization
DATE:    22/12/02 21:52:14 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 21:41:52 UT on 2 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221202B (trigger 691710117.068684 / 221202904).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 346.4, Dec = -3.1 (J2000 degrees, equivalent to J2000 23h 05m, -3d 06'), with a statistical uncertainty of 1.2 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/bn221202904/quicklook/glg_skymap_all_bn221202904.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/bn221202904/quicklook/glg_healpix_all_bn221202904.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221202904/quicklook/glg_lc_medres34_bn221202904.gif


GRB_name: GRB221202A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33007
SUBJECT: GRB 221202A: MeerLICHT upper limits
DATE:    22/12/02 22:14:11 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

S. de Wet (UCT) and P.J. Groot (Radboud/UCT/SAAO) report on behalf of the
MeerLICHT consortium:

Following the detection by Swift of GRB 221202A and its X-ray counterpart
(Caputo et al., GCN 33005), the 0.6m wide-field MeerLICHT telescope,
located at Sutherland, South Africa, obtained 5x300s observations in the
q,z,i,r,g bands beginning at 21:14:34 UT on 2022 December 2, approximately
1.14 hours after the Swift trigger.

We detect no new source at the XRT position (Caputo et al., GCN 33005) in
any of our images down to the following 3-sigma upper limits, in the AB
magnitude system:

q > 21.80 at 21:17:27 UT
z > 20.01 at 21:22:34 UT
i > 21.02 at 21:28:03 UT
r > 21.53 at 21:33:25 UT
g > 21.58 at 21:38:54 UT

MeerLICHT is built and run by a consortium consisting of Radboud
University, University of Cape Town, the South African Astronomical
Observatory, the University of Oxford, the University of Manchester and the
University of Amsterdam.


GRB_name: GRB221202A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33008
SUBJECT: GRB 221202A: Enhanced Swift-XRT position
DATE:    22/12/02 22:47:18 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 864 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 221202A, 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 = 77.08299, -59.83246 which is equivalent
to:

RA (J2000): 05h 08m 19.92s
Dec (J2000): -59d 49' 56.9"

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: GRB221202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33009
SUBJECT: GRB 221202A: LCOGT Optical Upper Limits
DATE:    22/12/02 22:51:53 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 221202A (Caputo et al., GCN 33005) field with the LCOGT
1-meter Sinistro instrument at the South African Astronomical Observatory
site, on December 2, from 21:09 to 21:36 (corresponding to 1.05 to 1.5
hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 3x280s exposures in each band.  We do not detect
any  sources in the XRT error region, in either band, consistent with other
optical upper limits (de Wet et al., GCN 33007).

The following upper limits are calculated using the USNO-B.1 catalog as
reference:

R > 20.0
I > 19.0

These magnitudes are not corrected for galactic extinction.


GRB_name: GRB221202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33010
SUBJECT: GRB 221202A: Swift-XRT refined Analysis
DATE:    22/12/03 07:45:52 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.1 ks of XRT data for GRB 221202A (Caputo et al. GCN
Circ. 33005), from 82 s to 27.6 ks after the  BAT trigger. The data
comprise 185 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN Circ. 33008).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.45 (+0.08, -0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.25 (+0.11, -0.10). The
best-fitting absorption column is  3.94 (+0.29, -0.28) x 10^21 cm^-2,
in excess of the Galactic value of 2.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.77 (+0.32, -0.29)
and a best-fitting absorption column of 2.1 (+0.8, -0.7) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 2.5 x 10^-11 (5.3 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.1 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 2.1 x 10^20 cm^-2
Excess significance: 4.6 sigma
Photon index:      2.77 (+0.32, -0.29)

If the light curve continues to decay with a power-law decay index of
1.45, the count rate at T+24 hours will be 4.0 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-14 (2.1 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01142997.

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


GRB_name: GRB221201A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33011
SUBJECT: GRB 221201A: Fermi GBM observation
DATE:    22/12/03 08:49:40 GMT
FROM:    Christian Malacaria at ISSI  <cmalacaria.astro@gmail.com>

GRB 221201A: Fermi GBM observation

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

"At 12:24:45.31 UT on 01 December 2022, the Fermi Gamma-Ray Burst 
Monitor (GBM)
triggered and located GRB 221201A (trigger 691590290 / 221201517).

This event was also observed by Swift/BAT and  Swift/XRT (GCN 32998).

The GBM position is reported in the Fermi-GBM Final on-ground 
Localization (GCN 32997)
and is consistent with the Swift position.
The angle from the Fermi LAT boresight is 125 degrees.

The GBM light curve shows a single pulse with a duration (T90) of about 
29 s (50-300 keV).
The time-averaged spectrum from T0-0 s to T0+15 s is best fit by a Band 
function
with Epeak = 144 +/- 7 keV, alpha = -0.57 +/- 0.07, and beta = -2.5 +/- 0.1

The event fluence (10-1000 keV) in this time interval is (1.59 +/- 
0.03)E-05 erg/cm^2.
The 1-sec peak photon flux measured starting from T0+6.8 s in the 
10-1000 keV band
is 20.5 +/- 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: GRB221203A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33012
SUBJECT: GRB 221203A: Fermi GBM Final Real-time Localization
DATE:    22/12/03 13:03:36 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 LONG GRB

At 12:52:59 UT on 3 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221203A (trigger 691764784.454144 / 221203537).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 355.1, Dec = -69.0 (J2000 degrees, equivalent to J2000 23h 40m, -69d 00'), with a statistical uncertainty of 4.6 degrees.

The angle from the Fermi LAT boresight is 60.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221203537/quicklook/glg_skymap_all_bn221203537.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/bn221203537/quicklook/glg_healpix_all_bn221203537.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221203537/quicklook/glg_lc_medres34_bn221203537.gif


GRB_name: GRB221201A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33013
SUBJECT: GRB 221201A: Swift-BAT refined analysis
DATE:    22/12/03 15:01:15 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),

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

A. Y. Lien (U Tampa),, C. B. Markwardt (GSFC),

D. M. Palmer (LANL),, T. Parsotan (GSFC/UMBC),

T. Sakamoto (AGU), (i.e. the Swift-BAT team):



Using the data set from T-239 to T+941 sec from the recent telemetry
downlink,

we report further analysis of BAT GRB 221201A (trigger #1142847)

(Troja et al., GCN Circ. 32998).  The BAT ground-calculated position is

RA, Dec = 266.903, -68.230 deg which is

   RA(J2000)  =  17h 47m 36.6s

   Dec(J2000) = -68d 13' 48.2"

with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).

The partial coding was 51%.



The mask-weighted light curve shows a single peaked pulse.

T90 (15-350 keV) is 33.71 +- 2.03 sec (estimated error including
systematics).



The time-averaged spectrum from T-20.88 to T+22.92 sec is best fit by a
simple

power-law model.  The power law index of the time-averaged spectrum is

1.63 +- 0.05.  The fluence in the 15-150 keV band is 8.6 +- 0.2 x 10^-06
erg/cm2.

The 1-sec peak photon flux measured from T-13.51 sec in the 15-150 keV band

is 11.2 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence

level.



The results of the batgrbproduct analysis are available at

http://gcn.gsfc.nasa.gov/notices_s/1142847/BA/


GRB_name: GRB221202A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33014
SUBJECT: GRB 221202A: VLT/FORS2 Afterglow Discovery
DATE:    22/12/03 17:28:59 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi (INAF), G. Pugliese (API, Amsterdam university), D. A. Kann 
(Goethe Univ.), B. Schneider (CEA Paris-Saclay), and V. D'Elia (INAF/OAR 
and ASI/SSDC) report on behalf of the Stargate collaboration:

We performed photometric observations of the afterglow of GRB 221202A 
detected by the Swift Burst Alert Telescope (BAT) at 20:06:10.56 UT 
(Caputo et al., GCN 33005; De Wet et al., GCN 33007; Beardmore et al., 
GCN 33008;  Strausbaugh et al., GCN 33009; Evans et al., GCN 33010) with 
the FORS2 instrument at the ESO VLT-UT1 in the R_Special, I_Bessel and 
z_Gunn filters (in the following RIz). The observation started at 
06:50:29 UT (about 10.73 hours after the BAT detection), and consisted 
of 500 s in R, 800 s in I, and 1320 s in z.

We detect a source in the XRT error circle in all filters at position 
RA, Dec. (J2000) = 05:08:19.94,-59:49:58.6, astrometrized against Gaia 
DR3 field stars. We measure the following photometry, consistent with 
the upper limits of MeerLICHT (S. de Wet et al., GCN 33007) and LCOGT 
(R. Strausbaugh et al., GCN 33009):

R = 23.10 +/- 0.05 mag,
I = 22.68 +/- 0.06 mag,
z = 22.52 +/- 0.07 mag.

Magnitudes are calibrated against SkyMapper field stars and are in the 
AB system. For the R and I bands we use the Lupton formulas to convert 
the standard stars to the BVRI photometric system, then convert the 
measured magnitudes back to the AB system.

A source at the same position is visible in r'-band images downloaded 
and stacked from the Legacy Imaging Survey, with r' ~ 24.3 mag (AB). 
Therefore, we conclude that the detected source is dominated by the 
afterglow of GRB 221202A and slightly contaminated by the GRB host 
galaxy. We derive an X-ray to optical slope beta_OX ~ 0.8, therefore the 
afterglow is not dark, just faint.

We acknowledge the support provided by T. C. Emy and the Paranal staff, 
in particular Ana Escorza, Ricardo Arrue, Marcela Espinoza, and Michael 
Abdul-Masih.


GRB_name: GRB221202A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33015
SUBJECT: GRB 221202A: Swift-BAT refined analysis
DATE:    22/12/03 19:01:10 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

S. D. Barthelmy (GSFC),  H. A. Krimm (NSF),

S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),

C. B. Markwardt (GSFC), D. M. Palmer (LANL),

T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU),

M. Stamatikos (OSU) (i.e. the Swift-BAT team):



Using the data set from T-240 to T+962 sec from the recent telemetry
downlink,

we report further analysis of BAT GRB 221202A (trigger #1142997)

(Caputo et al. GCN Circ. 33005).  The BAT ground-calculated position is

RA, Dec = 77.002, -59.836 deg which is

   RA(J2000)  =  05h 08m 00.5s

   Dec(J2000) = -59d 50' 09.0"

with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).

The partial coding was 85%.



The mask-weighted light curve shows a single peaked pulse.

T90 (15-350 keV) is 10.34 +- 1.21 sec (estimated error including
systematics).



The time-averaged spectrum from T+1.03 to T+12.44 sec is best fit by a
simple

power-law model.  The power law index of the time-averaged spectrum is

1.64 +- 0.25.  The fluence in the 15-150 keV band is 3.2 +- 0.6 x 10^-07
erg/cm2.

The 1-sec peak photon flux measured from T+3.31 sec in the 15-150 keV band

is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence

level.



The results of the batgrbproduct analysis are available at

http://gcn.gsfc.nasa.gov/notices_s/1142997/BA/


GRB_name: GRB221202A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33016
SUBJECT: GRB 221202A: Swift/UVOT Detection
DATE:    22/12/03 21:07:48 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

Paul Kuin (MSSL-UCL) and R. Caputo (GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 221202A
102 s after the BAT trigger (Caputo et al., GCN Circ. 33005).
A source consistent with the XRT position (Beardmore et al. GCN Circ. 33008)
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              102          733          186         20.66 +/- 0.20
v                  590         4820          216        >19.9
b                  516          709           39        >19.8
u                  260          857          285        >19.7
w1                 640          832           39        >20.8
m2                 615          808           39        >18.1
w2                 566         4635          235        >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.027 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB221203B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33017
SUBJECT: GRB 221203B: Fermi GBM Final Real-time Localization
DATE:    22/12/03 21:26:43 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 21:16:22 UT on 3 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221203B (trigger 691794987.572292 / 221203886).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 287.5, Dec = 34.1 (J2000 degrees, equivalent to J2000 19h 10m, 34d 06'), with a statistical uncertainty of 11.3 degrees.

The angle from the Fermi LAT boresight is 65.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221203886/quicklook/glg_skymap_all_bn221203886.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/bn221203886/quicklook/glg_healpix_all_bn221203886.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221203886/quicklook/glg_lc_medres34_bn221203886.gif


GRB_name: GRB221202B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33019
SUBJECT: GRB 221202B: Detection by VZLUSAT-2
DATE:    22/12/04 13:08:54 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.

A long-duration GRB 221202B (Fermi/GBM detection: The Fermi GBM team, 
GCN Circ. 33006; Konus-Wind detection trigger time at 2022-12-02 
21:41:58.66 UT; INTEGRAL/SPI-ACS detection peak at ~2022-12-02 21:42:00 
UT) was marginally 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 
marginal detection shows the peak time 2022-12-02 21:42:03 UTC. The T90 
duration was measured to be 20 s with the light curve resolution of 1 s. 
The significance during T90 reaches 5.4 sigma.

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB221202B_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: GRB221205A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  33021
SUBJECT: GRB 221205A: Fermi GBM Final Real-time Localization
DATE:    22/12/05 00:42:21 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 00:31:56 UT on 5 Dec 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 221205A (trigger 691893121.981046 / 221205022).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 220.1, Dec = 54.5 (J2000 degrees, equivalent to J2000 14h 40m, 54d 30'), with a statistical uncertainty of 7.7 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/2022/bn221205022/quicklook/glg_skymap_all_bn221205022.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/bn221205022/quicklook/glg_healpix_all_bn221205022.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn221205022/quicklook/glg_lc_medres34_bn221205022.gif


