# GCN_circulars

GRB_name: GRB220606B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32168
SUBJECT: GRB 220606B: Swift ToO observations
DATE:    22/06/06 13:32:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Swift/BAT-GUANO GRB 220606B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021504

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: GRB220527A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32169
SUBJECT: GRB 220527A: A BdHN I with a clear UPE phase
DATE:    22/06/06 15:33:00 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

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

GRB 220527A is observed by AGILE (Ursi et al. 2022, GCN 32129), Fermi (GCN
32130, Bissaldi et al. 2022, GCN 32131, Mangan et al. 2022, GCN 32133),
Swift (B. Sbarufatti et al. 2022 GCN 32135, A. Tohuvavohu. 2022, GCN
32136), CALET (Yamaoka et al. 2022, GCN 32139), AstroSat (Gopalakrishnan et
al. 2022, GCN 32140), and Konus-Wind (Lysenko et al. 2022, GCN 32152).

With the redshift z = 0.857 of GRB 220527A (D. Xu et al. 2022, GCN 32141),
the isotropic energy of this GRB in 10 keV - 10 MeV, and 20 keV - 16 MeV
ranges are E_iso=(2.60 +\- 0.14)x10^{53} erg, and
E_iso=1.22(-0.06,+0.07)x10^{53} erg, respectively (A. Lysenko et al. 2022,
GCN 32152).

The ultra-relativistic prompt emission phase of this GRB, originating from
the over-criticl electric field around the black hole (Moradi et al 2021,
Phys. Rev. D 104, 063043) extends from rest-frame time of 3.7s to 5.4s. The
UPE phase is best fitted by a cutoff power-law plus blackbody spectrum
(CPL+BB) with best fit parameters of: alpha = -0.57, Ep = 109.5 keV, beta =
-2.36, kT = 47.8 keV.

In addition to the above observations, the following observation of the GeV
emission (E. Bissaldi et al. 2022, GCN 32131), originated from the newborn
black hole (R. Ruffini et al. 2019 ApJ 886 82) and the afterglow emission
(B. Sbarufatti et al. 2022 GCN 32135, A. Tohuvavohu. 2022, GCN 32136)
originated from the newborn neutron star (J.A. Rueda et al. 2020 ApJ 893
148), confirm this GRB is a BDHN I.

Following Ruffini et al. 2021 (MNRAS, 504, 5301,doi:10.1093/mnras/stab724),
we predict the emergence of an optical supernova peak to be detected at
(25.1+/-3.5) days after the trigger (June 21th 2022, uncertainty from June
18th 2022 to June 24th 2022), with the bolometric optical luminosity of
L_SN,b=(9.0+/-2.7)x10^{42} erg/s.

Follow-up optical observations for the SN peak are encouraged.


GRB_name: GRB220606B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32170
SUBJECT: GRB 220606B: GUANO coordinate correction to GCN 32167
DATE:    22/06/06 16:01:12 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

The coordinates for GRB 220606B reported in GCN 32167 were transposed
in the declination, and therefore incorrect.

The correct coordinates of the GRB localization candidate are:

RA, Dec = 28.474, -54.741 deg which is
   RA(J2000)  = 01h 53m 53.76s
   Dec(J2000) = -54d 44â€² 27.6â€³
with an estimated uncertainty of 5 arcmin.

The Swift XRT/UVOT ToO followup is at the correct position.
Sincere apologies for the transcription error.


GRB_name: GRB220606A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32171
SUBJECT: GRB 220606A: Swift/BAT-GUANO detection
DATE:    22/06/06 16:57:44 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 220606A onboard (T0: 2022-02-03T21:15:39.8
 UTC, Fermi/GBM GCN 32164).

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 9.8 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 5.7 and no specific location in the FOV
preferred.

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

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

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

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


GRB_name: GRB220601A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32172
SUBJECT: Konus-Wind detection of GRB 220601A
DATE:    22/06/06 17:24:42 GMT
FROM:    Alexandra Lysenko at Ioffe Institute  <alexandra.lysenko@mail.ioffe.ru>

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

The long-duration GRB 220601A
(IPN triangulation: Kozyrev et al., GCN Circ. 32163)
triggered Konus-Wind at T0=22766.297 s UT (06:19:26.297).

The burst light curve shows a multipeaked structure
which starts at ~T0-42.5 s and has a total duration of ~82.5 s.
The emission is seen up to ~3 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220601_T22766/

As observed by Konus-Wind, the burst
had a fluence of 2.64(-0.16,+0.17)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.056s,
of 6.19(-1.55,+1.57)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+41.216 s)
is best fit in the 28 keV - 5 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.79(-0.17,+0.18)
and Ep = 195(-17,+21) keV (chi2 = 58/71 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 57/70 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 - 5 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.74(-0.16,+0.17),
the high energy photon index beta = -2.81(-2.84,+0.34),
the peak energy Ep = 220(-24,+31) keV
(chi2 = 62/70 dof).

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


GRB_name: GRB220606B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32173
SUBJECT: GRB 220606B: Swift follow-up observations
DATE:    22/06/07 13:36:38 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 220606B (Tohuvavohu et al., GCN
Circ. 32167), collecting 4.9 ks of Photon Counting (PC) mode data
between T0+44.9 ks and T0+68.8 ks. 

No credible X-ray afterglow candidate has been detected within the
BAT-GUANO error circle (Tohuvavohu, GCN Circ. 32170) down to a 0.3 - 10
keV count-rate upper limit of ~ 2e-3 ct/s (3sigma c.l.).

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/00021504.

Swift-UVOT began settled observations 45.1 ks after the trigger. No
optical afterglow consistent with the BAT-GUANO position is detected.
The 3.9 ks exposure in the white filter gives an upper limit of >21.9
mag.


This circular is an official product of the Swift team.


GRB_name: GRB220606B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32174
SUBJECT: GRB 220606B: Fermi GBM Observation
DATE:    22/06/07 16:22:44 GMT
FROM:    Boyan A. Hristov at UAH  <bah0046@uah.edu>

B. Hristov (UAH) and C. Meegan (UAH)

report on behalf of the Fermi GBM Team:


"At 01:03:28.68 UT on 06 June 2022, the Fermi Gamma-Ray Burst Monitor

(GBM) triggered and located GRB 220606B (trigger 676170213 / 220606044),

which was also detected by the Swift/BAT-GUANO (Tohuvavohu et al. 2022,

GCN 32167).


The Fermi GBM Final Real-time Localization (GCN 32165) is consistent

with the GUANO position.


The GBM light curve shows a single peak with a duration (T90) of about

0.9 +/- 0.4 s (50-300 keV).


The time-averaged spectrum from T0-0.256 s to T0+0.768 s is best fit by

a simple power law with index = -1.28 +/- 0.07.


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

(2.9 +/- 0.4)E-7 erg/cm^2. The 0.64-sec peak photon flux measured

starting from T0-0.064 s in the 10-1000 keV band is

2.8 +/- 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: GRB220606B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32177
SUBJECT: GRB 220606B: Gemini South Optical Observations
DATE:    22/06/08 00:14:35 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), E. Troja (Tor Vergata), S. Dichiara (PSU),
on behalf of a larger collaboration:

We performed target of opportunity observations of the short
GRB 220606B (Fermi GBM Team GCN 32165, Tohuvavohu et al. GCN 32167)
with the Gemini Multi Object Spectrograph (GMOS) mounted on the
Gemini-South telescope. We obtained imaging in r-band and z-band
for 630 s in each filter starting at ~1.4 d post-trigger.
The GMOS field of view covers the central ~45% of the BAT error
circle (Tohuvavohu et al. GCN 32170). We note that this includes
a bright nearby galaxy with an estimated distance of 225 Mpc
(GLADE catalog; Dalya et al. 2016).

In comparison to the Dark Energy Survey DR2 catalog (Abbott et al.
2021), we do not identify any uncatalogued sources to a depth
r>25 AB mag and z>24.5 AB mag. This is in agreement with the
previously reported limit from Swift/UVOT (Evans et al. GCNs
32168 and 32173).

Our observations are sensitive to an AT2017gfo-like kilonova
at 225 Mpc. Therefore, either GRB 220606B is not physically
associated with the nearby galaxy or its kilonova is ~25 times
fainter than AT2017gfo at 1.4 d post-merger.

We thank the staff of the Gemini Observatory, in particular
Steve Margheim and Joan Font-Serra, for rapid scheduling of
these observations.


GRB_name: GRB220608A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32178
SUBJECT: GRB 220608A: Fermi GBM Final Real-time Localization
DATE:    22/06/08 05:14:06 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 05:03:44 UT on 8 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220608A (trigger 676357429.750658 / 220608211).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 229.3, Dec = -0.2 (J2000 degrees, equivalent to J2000 15h 17m, 0d 12'), with a statistical uncertainty of 1.2 degrees.

The angle from the Fermi LAT boresight is 86.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220608211/quicklook/glg_skymap_all_bn220608211.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/bn220608211/quicklook/glg_healpix_all_bn220608211.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220608211/quicklook/glg_lc_medres34_bn220608211.gif


GRB_name: GRB220608A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32179
SUBJECT: Fermi GRB 220608A: Global MASTER-Net observations report 
DATE:    22/06/08 05:30:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, 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-OAGH robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Mexico (OAGH National Institute for Astrophysics, Optics and Electronics) started inspect of the Fermi GRB 220608A ( Fermi GBM team, GCN 32178) errorbox  40 sec after notice time and 78 sec after trigger time at 2022-06-08 05:05:03 UT, with upper limit up to  18.1 mag. The observations began at zenith distance = 31 deg. The sun  altitude  is -27.5 deg. 

The galactic latitude b = 45 deg., longitude l =  1 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1999930

We obtain a following upper limits.  

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

      89 | 2022-06-08 05:05:03 |         MASTER-OAGH | (15h 18m 06.15s , +00d 12m 39.1s) |   C |    20 | 18.1 |        
      89 | 2022-06-08 05:05:03 |         MASTER-OAGH | (15h 17m 57.32s , +00d 36m 54.2s) |   C |    20 | 17.3 |        
     130 | 2022-06-08 05:05:44 |         MASTER-OAGH | (15h 17m 52.23s , +00d 36m 07.2s) |   C |    20 | 16.4 |        
     130 | 2022-06-08 05:05:44 |         MASTER-OAGH | (15h 18m 01.03s , +00d 11m 39.2s) |   C |    20 | 17.6 |        
     176 | 2022-06-08 05:06:25 |         MASTER-OAGH | (15h 17m 58.38s , +00d 35m 46.9s) |   C |    30 | 15.6 |        
     176 | 2022-06-08 05:06:25 |         MASTER-OAGH | (15h 18m 07.14s , +00d 11m 45.8s) |   C |    30 | 17.2 |        
     232 | 2022-06-08 05:07:16 |         MASTER-OAGH | (15h 17m 55.44s , +00d 38m 26.1s) |   C |    40 | 14.8 |        
     232 | 2022-06-08 05:07:16 |         MASTER-OAGH | (15h 18m 04.16s , +00d 13m 41.8s) |   C |    40 | 16.8 |        
     298 | 2022-06-08 05:08:17 |         MASTER-OAGH | (15h 17m 55.37s , +00d 36m 37.7s) |   C |    50 | 15.3 |        
     298 | 2022-06-08 05:08:17 |         MASTER-OAGH | (15h 18m 04.07s , +00d 11m 56.5s) |   C |    50 | 17.3 |        
     379 | 2022-06-08 05:09:28 |         MASTER-OAGH | (15h 17m 58.24s , +00d 38m 23.5s) |   C |    70 | 14.9 |        
     379 | 2022-06-08 05:09:28 |         MASTER-OAGH | (15h 18m 06.90s , +00d 13m 38.7s) |   C |    70 | 17.3 |        
     465 | 2022-06-08 05:11:00 |         MASTER-OAGH | (15h 08m 20.46s , +01d 14m 14.4s) |   C |    60 | 15.3 |        
     465 | 2022-06-08 05:11:00 |         MASTER-OAGH | (15h 08m 28.99s , +00d 49m 33.2s) |   C |    60 | 17.0 |        
     804 | 2022-06-08 05:15:53 |         MASTER-OAGH | (15h 17m 10.99s , -00d 11m 35.4s) |   C |   150 | 16.2 |        
     804 | 2022-06-08 05:15:53 |         MASTER-OAGH | (15h 17m 19.75s , -00d 35m 47.3s) |   C |   150 | 17.6 |        
     990 | 2022-06-08 05:18:44 |         MASTER-OAGH | (15h 17m 17.07s , -00d 10m 35.4s) |   C |   180 | 15.7 |        
     990 | 2022-06-08 05:18:44 |         MASTER-OAGH | (15h 17m 25.80s , -00d 35m 21.6s) |   C |   180 | 17.4 |        
    1191 | 2022-06-08 05:22:06 |         MASTER-OAGH | (15h 17m 14.38s , -00d 10m 51.0s) |   C |   180 | 16.1 |        
    1191 | 2022-06-08 05:22:06 |         MASTER-OAGH | (15h 17m 22.89s , -00d 34m 13.3s) |   C |   180 | 17.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220606C
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32180
SUBJECT: GRB 220606C: CALET Gamma-Ray Burst Monitor detection
DATE:    22/06/08 06:20:55 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 220606C triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 13:35:14.394 UTC on 6 June 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1338557524/index.html).
The burst signal was seen by only SGM.

The burst light curve shows a single pulse which starts
at T+3.1 sec, peaks at T+4.1 sec, and ends at T+47.4 sec.
The T90 and T50 durations measured by the SGM data are 30.4 +/- 7.8 sec
and 6.9 +/- 0.6 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1338557524/

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


GRB_name: GRB220606A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32181
SUBJECT: GRB 220606A: Fermi GBM observation
DATE:    22/06/08 14:32:53 GMT
FROM:    Boyan A. Hristov at UAH  <bah0046@uah.edu>

B. Hristov (UAH) and C. Meegan (UAH)

report on behalf of the Fermi GBM Team:


"At 00:35:39.28 UT on 06 June 2022, the Fermi Gamma-Ray Burst Monitor

(GBM) triggered and located GRB 220606A (trigger 676168544 / 220606025,

GCN 32164), which was also detected by the Swift/BAT-GUANO

(A. Tohuvavohu et al. 2022, GCN 32171).


The GBM light curve consists of multiple peaks with a duration (T90)

of about 19.7 +/- 1.6 s (50-300 keV).


The time-averaged spectrum from T0-2.560 s to T0+17.664 s is well fit

by a simple power law with index = -1.37 +/- 0.03.


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

(2.88 +/- 0.17)E-6 erg/cm^2. The 1-sec peak photon flux measured

starting from T0-0.64 s in the 10-1000 keV band is

1.6 +/- 0.2 ph/s/cm^2.


The spectral analysis results presented above are preliminary;

final results will be published in the GBM GRB Catalog:

https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html



For Fermi GBM data and info, please visit the official Fermi GBM Support
Page:

https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"


GRB_name: GRB220609A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32182
SUBJECT: GRB 220609A: Fermi GBM Final Real-time Localization
DATE:    22/06/09 01:42:10 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 01:30:54 UT on 9 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220609A (trigger 676431059.34879 / 220609063).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 225.5, Dec = -33.9 (J2000 degrees, equivalent to J2000 15h 01m, -33d 53'), with a statistical uncertainty of 13.9 degrees.

The angle from the Fermi LAT boresight is 100.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220609063/quicklook/glg_skymap_all_bn220609063.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/bn220609063/quicklook/glg_healpix_all_bn220609063.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220609063/quicklook/glg_lc_medres34_bn220609063.gif


GRB_name: GRB220608A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32183
SUBJECT: GRB 220608A: AstroSat CZTI detection
DATE:    22/06/09 03:23:52 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 detection of a long GRB 220608A which was 
also reported by Fermi GBM (GCN 32178).

The source was clearly detected in the 20-200 keV energy range. The 
light curve showed multiple peaks of emission with the strongest peak at 
2022-06-08 05:03:45.50 UTC. The measured peak count rate associated with 
the burst is 294 (+43, -35) counts/s above the background in the 
combined data of three quadrants, with a total of 2720 (+389, -365) 
counts. The local mean background count rate was 393 (+1, -2) counts/s. 
Using cumulative rates, we measure a T90 of 36 (+11, -3) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve showed multiple peaks 
of emission with the strongest peak at 2022-06-08 05:03:44.45 UTC. The 
measured peak count rate is 483 (+71, -70) counts/s above the background 
in the combined Veto data of four quadrants, with a total of 4040 (+617, 
-645) counts. The local mean background count rate was 1621 (+4, -4) 
counts/s. We measure a T90 of 36 (+5, -10) 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: GRB220609B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32185
SUBJECT: GRB 220609B: CALET Gamma-Ray Burst Monitor detection
DATE:    22/06/10 03:31:48 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 220609B triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 12:21:07.969 UTC on 9 June 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1338812272/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure which starts
at T-6.4 sec, peaks at T+7.9 sec, and ends at T+14.1 sec.
The T90 and T50 durations measured by the SGM data are 9.9 +/- 1.0 sec
and 3.5 +/- 0.2 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1338812272/

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


GRB_name: GRB220609B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32186
SUBJECT: GRB 220609B: AstroSat CZTI detection
DATE:    22/06/10 04:31:26 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 220609B which was 
also detected by CALET GBM (Asaoka et al., GCN Circ. 32185).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-06-09 12:21:15.65 UTC. The measured peak count 
rate associated with the burst is 1230 (+239, -53) counts/s above the 
background in the combined data of four quadrants, with a total of 6095 
(+298, -291) counts. The local mean background count rate was 411 (+3, 
-6) counts/s. Using cumulative rates, we measure a T90 of 11 (+1, -1) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-06-09 
12:21:15.42 UTC. The measured peak count rate is 4988 (+127, -136) 
counts/s above the background in the combined Veto data of four 
quadrants, with a total of 24547 (+545, -597) counts. The local mean 
background count rate was 1421 (+5, -5) counts/s. We measure a T90 of 11 
(+2, -1) s from the cumulative Veto light curve.

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


GRB_name: GRB220610A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32188
SUBJECT: GRB 220610A: Fermi GBM Final Real-time Localization
DATE:    22/06/10 21:54:56 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 21:44:36 UT on 10 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220610A (trigger 676590281.930348 / 220610906).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 160.7, Dec = 24.8 (J2000 degrees, equivalent to J2000 10h 42m, 24d 48'), with a statistical uncertainty of 8.2 degrees.

The angle from the Fermi LAT boresight is 43.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220610906/quicklook/glg_skymap_all_bn220610906.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/bn220610906/quicklook/glg_healpix_all_bn220610906.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220610906/quicklook/glg_lc_medres34_bn220610906.gif


GRB_name: GRB220610A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32189
SUBJECT: Fermi GRB 220610A: Global MASTER-Net observations report 
DATE:    22/06/10 23:45:26 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 220610A ( Fermi GBM team, GCN 32188) errorbox  2670 sec after notice time and 2707 sec after trigger time at 2022-06-10 22:29:44 UT, with upper limit up to  17.2 mag. Observations started at twilight.  The observations began at zenith distance = 55 deg. The sun  altitude  is -10.7 deg. 

The galactic latitude b = 62 deg., longitude l = 211 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2002930

We obtain a following upper limits.  

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

    2737 | 2022-06-10 22:29:44 |         MASTER-OAFA | (10h 42m 50.03s , +23d 26m 38.4s) |   C |    60 | 15.2 |        
    2829 | 2022-06-10 22:31:16 |         MASTER-OAFA | (10h 51m 36.10s , +23d 25m 15.7s) |   C |    60 | 15.7 |        
    3074 | 2022-06-10 22:35:21 |         MASTER-OAFA | (10h 34m 54.77s , +23d 26m 39.4s) |   C |    60 | 15.8 |        
    3166 | 2022-06-10 22:36:53 |         MASTER-OAFA | (10h 33m 45.85s , +21d 30m 39.0s) |   C |    60 | 16.1 |        
    3257 | 2022-06-10 22:38:24 |         MASTER-OAFA | (10h 42m 29.69s , +21d 30m 47.4s) |   C |    60 | 16.7 |        
    3348 | 2022-06-10 22:39:55 |         MASTER-OAFA | (10h 29m 32.50s , +27d 12m 40.3s) |   C |    60 | 16.2 |        
    3440 | 2022-06-10 22:41:26 |         MASTER-OAFA | (10h 38m 39.16s , +27d 14m 30.2s) |   C |    60 | 16.4 |        
    3531 | 2022-06-10 22:42:57 |         MASTER-OAFA | (10h 35m 52.61s , +25d 19m 41.4s) |   C |    60 | 16.4 |        
    3622 | 2022-06-10 22:44:29 |         MASTER-OAFA | (10h 44m 46.99s , +25d 20m 48.3s) |   C |    60 | 16.5 |        
    3850 | 2022-06-10 22:48:16 |         MASTER-OAFA | (10h 51m 33.26s , +23d 24m 53.0s) |   C |    60 | 17.1 |        
    3941 | 2022-06-10 22:49:48 |         MASTER-OAFA | (10h 26m 13.01s , +23d 24m 47.0s) |   C |    60 | 16.8 |        
    4032 | 2022-06-10 22:51:19 |         MASTER-OAFA | (10h 34m 56.90s , +23d 26m 30.4s) |   C |    60 | 16.7 |        
    4217 | 2022-06-10 22:54:24 |         MASTER-OAFA | (10h 42m 30.69s , +21d 32m 27.2s) |   C |    60 | 17.0 |        
    4309 | 2022-06-10 22:55:55 |         MASTER-OAFA | (10h 29m 28.96s , +27d 13m 34.9s) |   C |    60 | 17.0 |        
    4400 | 2022-06-10 22:57:27 |         MASTER-OAFA | (10h 38m 31.69s , +27d 14m 43.4s) |   C |    60 | 16.8 |        
    4938 | 2022-06-10 23:06:24 |         MASTER-OAFA | (10h 51m 35.96s , +23d 26m 50.5s) |   C |    60 | 16.1 |        
    5030 | 2022-06-10 23:07:56 |         MASTER-OAFA | (10h 26m 10.56s , +23d 24m 51.4s) |   C |    60 | 16.2 |        
    5121 | 2022-06-10 23:09:27 |         MASTER-OAFA | (10h 34m 59.53s , +23d 26m 14.3s) |   C |    60 | 16.2 |        
    6113 | 2022-06-10 23:26:00 |         MASTER-OAFA | (10h 42m 26.96s , +21d 32m 24.4s) |   C |    60 | 17.0 |        
    6204 | 2022-06-10 23:27:31 |         MASTER-OAFA | (10h 29m 32.09s , +27d 12m 46.9s) |   C |    60 | 16.0 |        
    6296 | 2022-06-10 23:29:02 |         MASTER-OAFA | (10h 38m 36.86s , +27d 14m 06.7s) |   C |    60 | 15.9 |        
    6387 | 2022-06-10 23:30:33 |         MASTER-OAFA | (10h 46m 40.77s , +27d 14m 38.7s) |   C |    60 | 16.1 |        
    6627 | 2022-06-10 23:34:33 |         MASTER-OAFA | (10h 52m 54.61s , +25d 18m 48.1s) |   C |    60 | 17.2 |        
    6718 | 2022-06-10 23:36:05 |         MASTER-OAFA | (11h 01m 45.03s , +25d 20m 22.4s) |   C |    60 | 17.2 |        
    6810 | 2022-06-10 23:37:36 |         MASTER-OAFA | (10h 50m 15.33s , +21d 32m 23.3s) |   C |    60 | 17.2 |        
    6901 | 2022-06-10 23:39:07 |         MASTER-OAFA | (10h 58m 48.39s , +21d 31m 46.3s) |   C |    60 | 17.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220609B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32190
SUBJECT: IPN triangulation of GRB 220609B
DATE:    22/06/11 17:02:25 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

J. Benkhoff on behalf of the BepiColombo team,

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

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 220609B
(CALET-CGBM detection: Asaoka et al., GCN Circ 32185;
AstroSat-CZTI detection: Gopalakrishnan et al., GCN Circ 32186)
has been detected by Konus-Wind, CALET (CGBM), AstroSat (CZTI),
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), BepiColombo (MGNS),
and GECAM-B, so far, at about 44473 s UT (12:21:13).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  347.791 (23h 11m 10s)  +0.385 ( +0d 23' 05")
 Corners:
  348.003 (23h 12m 01s)  -0.627 ( +0d 37' 39")
  347.702 (23h 10m 49s)  +0.442 ( +0d 26' 31")
  347.634 (23h 10m 32s)  +1.229 ( +1d 13' 46")
  347.880 (23h 11m 31s)  +0.327 ( +0d 19' 37")
 ---------------------------------------------
The error box area is 515 sq. arcmin, and its maximum
dimension is 1.9 deg (the minimum one is 8.4 arcmin).
The Sun distance was 89 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220609_T44473/IPN/

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


GRB_name: GRB220611A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32191
SUBJECT: GRB 220611A: Swift detection of a burst
DATE:    22/06/11 18:36:01 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. B. Cenko (GSFC), E. Ambrosi (INAF-IASFPA), S. D. Barthelmy (GSFC),
V. D'Elia (SSDC & INAF-OAR), J.D. Gropp (PSU), J. A. Kennea (PSU),
S. Laha (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 18:01:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220611A (trigger=1110090).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec  66.526d, -37.289d which is 
   RA(J2000) = 04h 26m 06s
   Dec(J2000) = -37d 17' 20
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Due to a telemetry gap, the BAT onboard
lightcurve is not immediately available.  However, the triggering
algorithm found the source in an 8 second image, indicating a
long GRB. 

The XRT began observing the field at 18:04:20.4 UT, 149.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 66.51418, -37.25899
which is equivalent to:
   RA(J2000)  = 04h 26m 03.40s
   Dec(J2000) = -37d 15' 32.4"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 113 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper.  We cannot determine whether the source
is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 2.66
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 152 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 0.033. 

We note that this source location is ~15 arcsec from the line of sight
to the galaxy MCG-06-10-007, which is described in Simbad
as an S0 galaxy, B=16.3, z~0.049, angular size 18"x16". 

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


GRB_name: GRB220611A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32192
SUBJECT: GRB 220611A: Enhanced Swift-XRT position
DATE:    22/06/11 20:54:10 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 496 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220611A, 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 = 66.51464, -37.26019 which is equivalent
to:

RA (J2000): 04h 26m 3.51s
Dec (J2000): -37d 15' 36.7"

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: GRB220610B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32193
SUBJECT: GRB 220610B: AstroSat CZTI detection
DATE:    22/06/12 04:01:10 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 220610B which was 
also detected by INTEGRAL SPI-ACS (TrigNum 9952.0) and Fermi-GBM 
(TrigNum 676537486).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-06-10 07:04:43.50 UTC. The measured peak count 
rate associated with the burst is 125 (+32, -20) counts/s above the 
background in the combined data of two quadrants (out of four), with a 
total of 969 (+230, -221) counts. The local mean background count rate 
was 226 (+2, -2) counts/s. Using cumulative rates, we measure a T90 of 
20 (+7, -8) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-06-10 
07:04:43.38 UTC. The measured peak count rate is 388 (+69, -71) counts/s 
above the background in the combined Veto data of four quadrants, with a 
total of 2179 (+368, -491) counts. The local mean background count rate 
was 1471 (+5, -5) counts/s. We measure a T90 of 13 (+5, -3) s from the 
cumulative Veto light curve.

CZTI GRB detections are reported regularly on the payload site at 
http://astrosat.iucaa.in/czti/?q=grb. 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: GRB220611A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32194
SUBJECT: GRB 220611A: Swift-XRT refined Analysis
DATE:    22/06/12 08:07:14 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.8 ks of XRT data for GRB 220611A (Cenko et al. GCN
Circ. 32191), from 133 s to 40.2 ks after the  BAT trigger. The data
comprise 270 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 Goad et al.
(GCN Circ. 32192).

The late-time light curve (from T0+5.3 ks) can be modelled with a
power-law decay with a decay index of alpha=0.28 (+0.19, -0.21).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.31 (+/-0.06). The
best-fitting absorption column is  1.04 (+0.13, -0.12) x 10^21 cm^-2,
in excess of the Galactic value of 2.7 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.96 (+0.18, -0.08)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.2 x 10^-11 (3.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+1.8, -0.0) x 10^20 cm^-2
Galactic foreground: 2.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.96 (+0.18, -0.08)

If the light curve continues to decay with a power-law decay index of
0.28, the count rate at T+24 hours will be 0.045 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x
10^-12 (1.6 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/01110090.

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


GRB_name: GRB220611A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32195
SUBJECT: Swift GRB 220611A: Global MASTER-Net observations report 
DATE:    22/06/12 13:10:39 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB 220611A ( S. B. Cenko et al., GCN 32191) errorbox  55433 sec after notice time and 55505 sec after trigger time at 2022-06-12 09:26:56 UT, with upper limit up to  18.6 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -25.6 deg. 

The galactic latitude b = -44 deg., longitude l = 240 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2003639

We obtain a following upper limits.  

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

   55596 |         MASTER-OAFA |   C |   180 | 18.0 |        
   56606 |         MASTER-OAFA |   C |   180 | 18.1 |        
   56950 |         MASTER-OAFA |   C |   180 | 18.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220608B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32196
SUBJECT: GRB 220608B: Detection by VZLUSAT-2
DATE:    22/06/13 10:57:34 GMT
FROM:    Jakub Ripa at Masaryk University  <ripa.jakub@mail.muni.cz>

J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), M. Ohno (Eotvos 
U./Hiroshima U.),  N. Werner  (Masaryk U.),  L. Meszaros (Konkoly 
Observatory), H. Takahashi (Hiroshima U.), B. Csak (Konkoly 
Observatory), M. Topinka, F. Munz, F. Hroch (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 220608B (Fermi/GBM trigger 676366592) was detected 
by a GRB detector on board of the VZLUSAT-2 3U CubeSat 
(https://www.vzlusat2.cz/en/).

The data acquisition was performed by the GRB detector unit no. 1. The 
5.9 sigma detection was confirmed at 2022-06-08 07:36:39 UTC. The GRB 
has the T90 duration of 27 s.

The light curve obtained by VZLUSAT-2 is available here:
https://vzlusat2.konkoly.hu/static/share/GRB220608B_GCN_VZLUSAT2.pdf

The light curve obtained by VZLUSAT-2 with the shape and timing matches 
well the light curve obtained by Fermi/GBM. The GOES X-ray flux does not 
show any excess. Therefore our observation is consistent with this event 
being a GRB.

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: GRB220611A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32197
SUBJECT: GRB 220611A: Swift-BAT refined analysis
DATE:    22/06/13 22:36:11 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
S. B. Cenko (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-239 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220611A (trigger #1110090)
(Cenko et al., GCN Circ. 32191).  The BAT ground-calculated position is
RA, Dec = 66.505, -37.265 deg which is
   RA(J2000)  =  04h 26m 01.2s
   Dec(J2000) = -37d 15' 54.2"
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 70%.

The mask-weighted light curve shows a weak pulse that starts at ~T0
and ends at ~T+60 s. There might be a possible precursor emission
(~ 5 sigma in the 15-350 keV image) from ~T-90 s to ~T-85 s.
T90 (15-350 keV) is 57.00 +- 12.37 sec (estimated error including
systematics).

The time-averaged spectrum from T+0.52 to T+61.52 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.87 +- 0.29.  The fluence in the 15-150 keV band is
6.7 +- 1.3 x 10^-7 erg/cm2. 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/1110090/BA/


GRB_name: GRB220612A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32198
SUBJECT: GRB 220612A: Swift/BAT-GUANO detection
DATE:    22/06/14 21:29:24 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 220612A onboard (T0: 2022-06-12T06:55:22.45
 UTC, CALET trig #1339051922).

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, GUANO sent a command to the Swift Burst Alert Telescope
(BAT) to save 200 seconds of BAT event-mode data from [-45,+45]
seconds around the time of the burst. All the requested event mode
data was delivered to the ground.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 9.3 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, with a
borderline DeltaLLHOut of 7.1 and no specific location in the FOV
preferred.

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

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

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

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


GRB_name: GRB220612A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32199
SUBJECT: GRB 220612A: CALET Gamma-Ray Burst Monitor detection 
DATE:    22/06/15 05:11:25 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

S. Torii (Waseda U), A. Yoshida, T. Sakamoto, S. Sugita (AGU), 
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), 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 220612A (Swift/BAT-GUANO detection: DeLaunay et al.,
GCN Circ. 32198) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 06:55:22.451 UTC on 12 June 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1339051922/index.html).
The burst signal was faintly seen by only the SGM detector.

The light curve of the SGM shows two weak pulses.  The emission starts
at T+2.8 sec, peaks at T+6.2 sec, and ends at T+19.7 sec.
The T90 and T50 durations measured by the SGM data are 15.0 +/- 1.0 sec
and 8.0 +/- 1.4 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1339051922/

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


GRB_name: GRB220611A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32201
SUBJECT: GRB 220611A: Swift/UVOT Upper Limits
DATE:    22/06/15 16:59:08 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 220611A
153 s after the BAT trigger (Cenko et al., GCN Circ. 32191).
No optical afterglow consistent with the XRT position
(Cenko et al. GCN Circ. 32191) 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           153          302          147         >19.5
u_FC               311          561          246         >19.1
white              153          926          245         >19.5
v                  641          835           39         >17.0
b                  566          759           39         >18.2
u                  311          734          265         >19.1
w1                 690          710           19         >17.7
m2                 665          685           19         >17.9
w2                 616          636           19         >18.7

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: GRB220606C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32202
SUBJECT: IPN triangulation of GRB 220606C
DATE:    22/06/15 17:58:12 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

and

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

The long-duration GRB 220606C
(CALET-CGBM detection: Nakahira et al., GCN Circ. 32180)
was detected by CALET (CGBM), INTEGRAL (SPI-ACS trigger 9949),
Konus-Wind, BepiColombo (MGNS), and GECAM-B (trigger tn220606_133517_fb)
at about 48918 s UT (13:35:18).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
   ---------------------------------------------
    RA(2000), deg                 Dec(2000), deg
   ---------------------------------------------
   Center:
    201.004 (13h 24m 01s)  -5.258 ( -5d 15' 29")
   Corners:
    211.181 (14h 04m 43s)  +9.433 ( +9d 25' 59")
    210.801 (14h 03m 12s)  +8.552 ( +8d 33' 07")
    200.664 (13h 22m 39s) -22.171 (-22d 10' 16")
    200.417 (13h 21m 40s) -23.101 (-23d 06' 03")
   ---------------------------------------------
The error box area is 16.3 sq. deg, and its maximum
dimension is 34.2 deg (the minimum one is 28 arcmin).
The Sun distance was 125 deg.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220606_T48919/IPN/

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


GRB_name: GRB220611A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32203
SUBJECT: GRB 220611A: Gemini South Infrared Detection
DATE:    22/06/16 18:57:55 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), E. Troja (Tor Vergata), S. Dichiara (PSU),
on behalf of a larger collaboration:

We performed target of opportunity observations of GRB 220611A
(Cenko et al. GCN 32191) with the FLAMINGOS-2 spectrograph
mounted on the Gemini-South telescope. Observations were carried
out in the Ks filter with a total exposure of 260 s beginning at
3.7 d post-trigger.

We detect a faint source within the XRT position (Goad et al. 32192)
with magnitude Ks = 20.0+/-0.3 AB mag. The object is located at:

RA, DEC = 04:26:03.56, -37:15:34.97

with an uncertainty of 0.5". This source is offset by 6" and 13",
respectively, from two bright galaxies. The latter is located
at redshift z~0.049 (Cenko et al. GCN 32191). Further observations
are planned to determine whether the source is fading or if it
is dominated by the contribution from an underlying host galaxy.

We thank the staff of the Gemini Observatory, in particular
Steve Margheim and Joan Font-Serra, for rapid scheduling of
these observations. We thank Rodrigo Carrasco for carrying
out the observations.


GRB_name: GRB220613A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32205
SUBJECT: IPN triangulation of GRB 220613A
DATE:    22/06/17 15:55:44 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

J. Benkhoff on behalf of the BepiColombo team,

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

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 220613A
was detected by Konus-Wind, Mars-Odyssey (HEND),
BepiColombo (MGNS), and GECAM-B (trigger tn220613_202337_fb)
at about 73416 s UT (20:23:36).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  189.085 (12h 36m 20s) +14.022 (+14d 01' 21")
 Corners:
  188.733 (12h 34m 56s) +13.688 (+13d 41' 15")
  189.094 (12h 36m 22s) +14.268 (+14d 16' 06")
  189.435 (12h 37m 44s) +14.347 (+14d 20' 49")
  189.077 (12h 36m 19s) +13.776 (+13d 46' 35")
 ---------------------------------------------
The error box area is 584 sq. arcmin, and its maximum
dimension is 57 arcmin (the minimum one is 14.5 arcmin).
The Sun distance was 99 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220613_T73416/IPN/

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


GRB_name: GRB220613A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32206
SUBJECT: Konus-Wind detection of GRB 220613A
DATE:    22/06/17 15:58:15 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 220613A
(IPN triangulation: Kozyrev et al., GCN Circ. 32205)
triggered Konus-Wind at T0=73416.994 s UT (20:23:36.994).

The burst light curve contains two major emission episodes.
The first one, lasting from ~T0-6 s to ~T0+15 s, and
the second episode, from ~T0+89 s to ~T0+133 s.
The total burst duration was ~173 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/GRB220613_T73416/

As observed by Konus-Wind, the burst
had a fluence of 2.61(-0.35,+0.34)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+6.288 s,
of 3.06(-0.48,+0.48)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+170.496 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(-0.12,+0.14),
the high energy photon index beta = -1.88(-0.30,+0.15),
the peak energy Ep = 719(-199,+323) keV
(chi2 = 109/86 dof).

The spectrum near the maximum count rate
(measured from T0+5.888 to T0+7.680 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 = -0.78(-0.08,+0.09),
the high energy photon index beta = -2.32(-0.43,+0.23),
the peak energy Ep = 1106(-187,+221) keV
(chi2 = 73/71 dof).

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


GRB_name: GRB220611A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32208
SUBJECT: GRB 220611A: Gemini Ks counterpart detection
DATE:    22/06/17 17:37:14 GMT
FROM:    Jillian Rastinejad at Northwestern Univ.  <jillianrastinejad2024@u.northwestern.edu>

J. Rastinejad (Northwestern), A. J. Levan (Radboud), D. B. Malesani (Radboud and DAWN/NBI), B. P. Gompertz (Birmingham), W. Fong, C. D. Kilpatrick (Northwestern) report on behalf of a larger collaboration:

We observed the location of GRB 220611A (Cenko et al., GCN 32191) with the FLAMINGOS-2 instrument mounted on the Gemini-South 8-meter telescope on Cerro Pachon, Chile. At a mid-time of 2022 Jun 17.43 UT (~5.7 days post-burst), we obtained 48 x 11 s of K-band imaging at a median airmass of 2.15 and seeing of 1.1 arcsec. A K-band source is detected at the location reported by O'Connor et al. (GCN 32203). Based on calibration to 2MASS, we estimate a preliminary magnitude for the source of K_AB ~ 21.1 +/- 0.2 mag. Compared to the measurement reported by O'Connor et al. (K_AB = 20.0 +/- 0.3 mag), our value is indicative of fading, though we note that the strong, non-uniform background due to the nearby galaxy MCG-06-10-007 and the lack of a common set of calibrators prevent a definitive statement. Furthermore, the source is not detected in archival imaging from the VISTA Hemisphere Survey (VHS; Cross et al. 2012), from which we measure a limiting magnitude K_AB > 20.5 mag. If confirmed, the fading and the non-detection in the VHS images would indicate that this object is transient, thus likely associated with GRB 220611A. 

We also note that a faint optical source is visible in r-band Legacy Source imaging (Dey et al. 2019) at the location reported by O'Connor et al. (GCN 32203). We measure a preliminary magnitude of r_AB ~ 24.5 +/- 0.3 mag for this source (again, uncertain due to the strong, non-uniform background). At present, it is not possible to discern if this source is associated with the z = 0.049 galaxy, or is a fainter, background galaxy. 

Further observations are planned. We thank Jen Andrews, German Gimeno and Ricardo Salinas at Gemini for the rapid planning and execution of these observations.


GRB_name: GRB220617A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32209
SUBJECT: GRB 220617A: Fermi GBM Final Real-time Localization
DATE:    22/06/17 18:41:43 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 SHORT GRB

At 18:31:12 UT on 17 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220617A (trigger 677183477.902462 / 220617772).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 155.8, Dec = 21.2 (J2000 degrees, equivalent to J2000 10h 23m, 21d 11'), with a statistical uncertainty of 2.7 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/bn220617772/quicklook/glg_skymap_all_bn220617772.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/bn220617772/quicklook/glg_healpix_all_bn220617772.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220617772/quicklook/glg_lc_medres34_bn220617772.gif


GRB_name: GRB220617A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32210
SUBJECT: Fermi GRB 220617A: Global MASTER-Net observations report 
DATE:    22/06/17 19:30:35 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) started inspect of the Fermi GRB 220617A ( Fermi GBM team, GCN 32209) errorbox  565 sec after notice time and 600 sec after trigger time at 2022-06-17 18:41:13 UT, with upper limit up to  17.8 mag. The observations began at zenith distance = 72 deg. The sun  altitude  is -37.2 deg. 

The galactic latitude b = 56 deg., longitude l = 216 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2008774

We obtain a following upper limits.  

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

     661 | 2022-06-17 18:41:13 |         MASTER-SAAO | (10h 22m 17.52s , +21d 18m 28.6s) |   C |   120 | 16.9 |        
     826 | 2022-06-17 18:41:13 |         MASTER-SAAO | (10h 22m 18.15s , +21d 18m 33.0s) |   C |   450 | 17.8 |  Coadd 
     843 | 2022-06-17 18:44:01 |         MASTER-SAAO | (10h 22m 23.41s , +21d 20m 08.9s) |   C |   150 | 17.2 |        
    1040 | 2022-06-17 18:47:02 |         MASTER-SAAO | (10h 22m 18.64s , +21d 19m 26.5s) |   C |   180 | 17.1 |        
    1914 | 2022-06-17 19:02:36 |         MASTER-SAAO | (10h 18m 16.82s , +22d 17m 11.7s) |   C |    60 | 15.8 |        
    2005 | 2022-06-17 19:04:08 |         MASTER-SAAO | (10h 26m 56.39s , +22d 16m 07.7s) |   C |    60 | 16.2 |        
    2093 | 2022-06-17 19:05:35 |         MASTER-SAAO | (10h 10m 34.70s , +20d 21m 52.6s) |   C |    60 | 14.0 |        
    2184 | 2022-06-17 19:07:06 |         MASTER-SAAO | (10h 18m 58.19s , +20d 23m 01.3s) |   C |    60 | 16.0 |        
    2884 | 2022-06-17 19:18:46 |         MASTER-SAAO | (10h 26m 42.09s , +20d 21m 46.5s) |   C |    60 | 14.8 |        
    2976 | 2022-06-17 19:20:18 |         MASTER-SAAO | (10h 35m 11.11s , +20d 23m 25.2s) |   C |    60 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220617B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32211
SUBJECT: GRB 220617B: Swift ToO observations
DATE:    22/06/18 01:10:23 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 Fermi/LAT GRB 220617B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021505

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 Fermi/LAT 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: GRB220617A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32212
SUBJECT: GRB 220617A: Fermi-LAT detection
DATE:    22/06/18 01:57:08 GMT
FROM:    Niccolo Di Lalla at Stanford U  <niccolo.dilalla@stanford.edu>

N. Di Lalla (Stanford Univ.), M. Arimoto (Kanazawa Univ.), M. Axelsson 
(KTH & Stockholm Univ.) and
G. Principe (University and INFN Trieste) report on behalf of the 
Fermi-LAT team:

On June 17, 2022, Fermi-LAT detected high-energy emission from GRB 220617A,
which was also detected by Fermi-GBM (trigger 677183477 / 220617772, GCN 
32209).

The best LAT on-ground location is found to be

RA, Dec = 156.96, 15.53 (degrees, J2000)

with an error radius of 0.09 deg (90 % containment, statistical error 
only).
This was 46 deg from the LAT boresight at the time of the GBM trigger:

T0 = 18:31:12 UT.

The data from the Fermi-LAT show a significant increase in the event rate
that is spatially and temporally correlated with the GBM emission with 
high significance.
The photon flux above 100 MeV in the time interval 0-200 s
after the GBM trigger is (4.9 +/- 0.8)E-05 ph/cm2/s.

The estimated photon index above 100 MeV is -1.9 +/- 0.1.

The highest-energy photon is a 8.2 GeV event which is observed 0.9 
seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Giacomo Principe 
(giacomo.principe@ts.infn.it <mailto:giacomo.principe@ts.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: GRB220618A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32214
SUBJECT: GRB 220618A: Swift detection of a burst
DATE:    22/06/18 09:25:56 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

E. Troja (NASA/GSFC/UMCP), C. Gronwall (PSU), K. L. Page (U Leicester)
and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 09:10:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220618A (trigger=1110821).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 38.966, +55.214 which is 
   RA(J2000) = 02h 35m 52s
   Dec(J2000) = +55d 12' 49"
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 ~800 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:12:53.1 UT, 143.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 38.98802, 55.21543
which is equivalent to:
   RA(J2000)  = 02h 35m 57.12s
   Dec(J2000) = +55d 12' 55.5"
with an uncertainty of 4.3 arcseconds (radius, 90% containment). This
location is 45 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 (4.74 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 8.9
(+7.86/-6.18) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 6.79e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 151 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain, extinction expected. 

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: GRB220617A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32215
SUBJECT: GRB 220617A: Swift-XRT observations
DATE:    22/06/18 10:41:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 220617A (Di Lalla et al. GCN Circ. 32212),
collecting 4.9 ks of Photon Counting (PC) mode data between T0+23.9 ks
and T0+37.1 ks. 

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

Please note: due to an error, the original GCN announcing these Swift
observations (GCN 32211) referred to "GRB 220617B", whereas the
observations were of GRB 220617A.

Source 1:
  RA (J2000):  157.1531  =  10:28:36.74
  Dec (J2000): +15.4493  =  +15:26:57.6
  Error: 6.4 arcsec (radius, 90% conf.)
  Count-rate: (2.7 [+1.5, -1.1])e-3 ct s^-1   
  Distance: 730 arcsec from Fermi/LAT position.
  Flux: (5.5 [+3.0, -2.2])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 2:
  RA (J2000):  156.9298  =  10:27:43.15
  Dec (J2000): +15.4059  =  +15:24:21.1
  Error: 6.4 arcsec (radius, 90% conf.)
  Count-rate: (1.45 [+0.92, -0.65])e-3 ct s^-1  
  Distance: 458 arcsec from Fermi/LAT position.

Source 3:
  RA (J2000):  157.0400  =  10:28:9.60
  Dec (J2000): +15.4886  =  +15:29:19.1
  Error: 6.4 arcsec (radius, 90% conf.)
  Count-rate: (1.67 [+0.91, -0.69])e-3 ct s^-1  
  Distance: 314 arcsec from Fermi/LAT position.

Source 4:
  RA (J2000):  156.9896  =  10:27:57.50
  Dec (J2000): +15.4454  =  +15:26:43.4
  Error: 5.7 arcsec (radius, 90% conf.)
  Count-rate: (1.75 [+0.93, -0.70])e-3 ct s^-1  
  Distance: 321 arcsec from Fermi/LAT position.

Source 5:
  RA (J2000):  156.8566  =  10:27:25.60
  Dec (J2000): +15.3577  =  +15:21:27.8
  Error: 6.3 arcsec (radius, 90% conf.)
  Count-rate: 0.0114 [+0.0046, -0.0036] ct s^-1   
  Distance: 716 arcsec from Fermi/LAT position.

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/00021505.

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


GRB_name: GRB220618A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32216
SUBJECT: GRB 220618A: Enhanced Swift-XRT position
DATE:    22/06/18 13:14:20 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 345 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220618A, 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 = 38.98602, +55.21568 which is equivalent
to:

RA (J2000): 02h 35m 56.65s
Dec (J2000): +55d 12' 56.4"

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: GRB220611A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32217
SUBJECT: GRB220611A: Gemini Optical Afterglow Confirmation
DATE:    22/06/18 13:24:01 GMT
FROM:    Eleonora Troja at GSFC  <eleonora.troja@nasa.gov>

B. Oâ€™Connor (UMD/GWU), E. Troja (U Tor Vergata/ASU) , S. Dichiara (PSU),
and S. B. Cenko (NASA/GSFC) report on behalf of a larger collaboration:

We carried out additional target of opportunity observations of GRB220611A
(Cenko et al.
GCN 32191) with the Gemini Multi Object Spectrograph (GMOS) mounted on the
Gemini-South
telescope. The observations began 5.7 d after the GRB trigger, and were
performed in
i-band for a total exposure of 540 s.

We detect the source reported by Oâ€™Connor et al. (GCN 32203) with magnitude
i~21 AB.
This source is not detected in archival images from the Dark Energy Survey
(Abbott et
al. 2021), and is likely the GRB afterglow. We determine that the X-ray,
optical,
and infrared data (Oâ€™Connor et al. GCN 32203, Rastinejad et al. GCN 32208)
can be
modeled by a power-law with spectral index beta~1.

Further observations are planned.

We thank the Gemini staff for rapid scheduling of these observations.


GRB_name: GRB220618A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32218
SUBJECT: GRB 220618A: Swift/UVOT Upper Limits
DATE:    22/06/18 15:40:50 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) 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 220618A
151 s after the BAT trigger (Troja et al., GCN Circ. 32214).
No optical afterglow consistent with the XRT position (Troja et al. GCN
Circ. 32214) 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           151          301          147         >19.8
u_FC               309          559          246         >18.9
white              151          609          167         >19.8
v                  641          649            8         >17.4
b                  565          585           19         >17.9
u                  309          559          246         >18.9
w2                 617          637           19         >18.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.391 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32219
SUBJECT: GRB 220618A: BOOTES-5/JGT early optical upper limit
DATE:    22/06/18 17:16:46 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), D. Hiriart and W. H. Lee (UNAM), C. J. Perez del Pulgar and I. Carrasco (UMA), I. H. Park (SKKU) on behalf of a larger collaboration, report:

Following the detection of GRB 220618A by Swift (Troja et al. GCNC 32214), the BOOTES-5/JGT 0.6m robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) observed the GRB location starting on Jun 18, 09:10:39 UT (~10 s after trigger). In the early co-added image (20 x 10 s exposures in the clear filter), no optical afterglow is detected within the Swift/XRT error region (Osborne et al. GCNC 32216) down to 19.5 mag. This non-detection is consistent with the UVOT results (Kuin et al. GCNC 32218) and MASTER results (Lipunov et al. GCNC 32213).

We thank the staff at Observatorio Astronomico Nacional in San Pedro Martir for their excellent support.


GRB_name: GRB220617A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32220
SUBJECT: IPN triangulation of GRB 220617A (short)
DATE:    22/06/18 18:02:34 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,

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

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 short-duration GRB 220617A
(Fermi-GBM detection: Fermi GBM Team, GCN Circ 32209;
Fermi-LAT detection: Di Lalla et al., GCN Circ 32212)
has been detected by Fermi (GBM trigger 677183477),
INTEGRAL (SPI-ACS), Konus-Wind, and Mars-Odyssey (HEND),
so far, at about 66669 s UT (18:31:09).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  156.882 (10h 27m 32s) +15.600 (+15d 36' 01")
 Corners:
  157.351 (10h 29m 24s) +16.445 (+16d 26' 41")
  157.423 (10h 29m 41s) +16.807 (+16d 48' 25")
  156.369 (10h 25m 29s) +14.606 (+14d 36' 21")
  156.247 (10h 24m 59s) +14.082 (+14d 04' 54")
 ---------------------------------------------
The error box area is 867 sq. arcmin, and its maximum
dimension is 2.9 deg (the minimum one is 5.8 arcmin).
The Sun distance was 66 deg.

This box may be improved.

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220617_T66669/IPN

The Fermi-LAT localization was covered by Swift ToO (GCN Circ 32215)
but none of the X-ray sources detected are inside the box.

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


GRB_name: GRB220618A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32221
SUBJECT: GRB 220618A: Swift-XRT refined Analysis
DATE:    22/06/18 18:35:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.0 ks of XRT data for GRB 220618A (Troja et al. GCN
Circ. 32214), from 131 s to 28.0 ks after the  BAT trigger. The data
comprise 235 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. 32216).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.1 (+/-0.4). At T+399 s  the decay
steepens to an alpha of 4.6 (+3.4, -0.7) before breaking again at
T+1148 s to a final decay with index alpha=0.26 (+0.52, -0.26).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.62 (+/-0.11). The
best-fitting absorption column is  5.9 (+0.6, -0.5) x 10^21 cm^-2, in
excess of the Galactic value of 4.7 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.0 x 10^-11 (8.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      5.9 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 4.7 x 10^21 cm^-2
Excess significance: 3.7 sigma
Photon index:      2.62 (+/-0.11)

If the light curve continues to decay with a power-law decay index of
0.26, the count rate at T+24 hours will be 6.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.1 x
10^-13 (5.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01110821.

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


GRB_name: GRB221106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32222
SUBJECT: GRB 221106A optical counterpart 
DATE:    22/06/18 19:10:23 GMT
FROM:    Giovanna Pugliese at API/UvA  <pugliese@astroduo.org>

D. B. Malesani (Radboud Univ. and DAWN/NBI), G. Pugliese (Amsterdam Univ. and Leiden Observatory), P. Schady (Univ. Bath), A. J. Levan (Radboud Univ.), B. P. Gompertz (Birmingham), report on behalf of the Stargate collaboration:

We observed the candidate counterpart (O'Connor et al., GCN 32203; Rastinejad et al., GCN 32208) of GRB 221106A (Cenko et al., GCN 32191) using  the ESO VLT UT1 (Antu) equipped with the FORS2 imager. Observations were taken in twilight using the I filter, at an average airmass of 2.6, and with a delivered seeing of 1.9". The mean time of the observation (twenty 30-s images) was Jun 18.42 UT (6.67 days after the GRB).

The object noted by O'Connor et al. (GCN 32203) is detected in the stack of our data. Calibrating against three stars from the SkyMapper survey, we measure a preliminary magnitude of i = 23.0 +- 0.2 (AB).

Compared to the archival brightness r = 24.5 from the Legacy Survey (Rastinejad et al., GCN 32208), our measurement favors some transient contribution, consolidating the association of this object to GRB 220611A. Alternatively, the source could be very red, which would however be in contrast with the non-detection in the Legacy Survey z-band image.

We note that the observed magnitude is fainter by ~4.5 mag than what SN 1998bw would look like at z = 0.049, likely ruling out a traditional collapsar GRB in MCG-06-10-007. GRB 221106A might be a background event (consistent with the detection of a potential host galaxy in the Legacy Survey) or, speculatively, originate from a merger event, which would be more consistent with the offset and spectral type of MCG-06-10-007.

We acknowledge support with this difficult observation from the VLT staff at Paranal, in particular Cedric Ledoux and Joseph Anderson. 


GRB_name: GRB220617A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32224
SUBJECT: GRB 220617A: Fermi GBM observation
DATE:    22/06/19 01:54:39 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

J. Wood (NASA/MSFC) reports on behalf of the Fermi GBM Team:

"At 18:31:12.89 UT on 17 June 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220617A (trigger 677183477 / 220617772).
which was also detected by the Fermi-LAT (N. Di Lalla et al. 2022, GCN 32212).

The Fermi GBM Final Real-time Localization (GCN 32209) is consistent with the LAT position.

The GBM light curve consists of a single pulse
with a duration (T90) of about 0.7 s (50-300 keV).
The time-averaged spectrum from T0-0.1 s to T0+0.5 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.7 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 2.3 +/- 0.3 MeV.

The event fluence (10-1000 keV) in this time interval is
(2.3 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.2 s in the 10-1000 keV band is 10 +/- 1 ph/s/cm^2.

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

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


GRB_name: GRB220617A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32227
SUBJECT: GRB 220617A: TNG optical observations
DATE:    22/06/19 12:17:15 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. D'Avanzo (INAF-OAB), S. Piranomonte (INAF-OAR), S. Campana (INAF-OAB), V. D'Elia (ASI/SSDC), 
L. Di Fabrizio, A. Garcia De Gurtubai Escudero (INAF-TNG) on behalf of the CIBO collaboration report:

We observed the field of the short GRB 220617A (Fermi-GBM detection: Fermi GBM Team, GCN Circ 32209; 
Fermi-LAT detection: Di Lalla et al., GCN Circ 32212; IPN detection: Kozyrev et al., GCN Circ. 32220) with the 
Italian 3.6m TNG telescope equipped with the optical camera DOLORES. A series of images were obtained with 
the r-sdss filter on 2022-06-18 from 21:22:18 UT to 22:09:26 UT (i.e. at a mid time of about 1.14 days after the burst).  

The pointing enabled to image the location of the Swift-XRT sources #3 and #4 (Page et al., GCN Circ. 32215), 
both consistent with the Fermi/LAT error circle.

No clear afterglow candidate is detected within the error circles of XRT sources #3 and #4 down to a typical limiting 
magnitude of r ~ 24.5 (AB; calibrated against the SDSS catalogue). 


We note the presence of catalogued galaxies from the SDSS within the error circles of the XRT sources #3 and #4: 

XRT3
- SDSS J102809.40+152924.9 (photo-z = 0.102 +/- 0.031)
- SDSS J102809.54+152915.8 (photo-z = 0.381 +/- 0.083)

XRT4
- SDSS J102757.23+152645.6 (photo-z = 0.714 +/- 0.116)


GRB_name: GRB220611A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32228
SUBJECT: GRB 220611A: Continued Gemini Infrared Observations
DATE:    22/06/19 21:39:00 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD/GWU), E. Troja (U Tor Vergata/ASU), S. Dichiara (PSU),
S. B. Cenko (UMD/GSFC), report on behalf of a larger collaboration:

Additional target of opportunity observations of GRB 220611A
(Cenko et al. GCN 32191) were carried out with the FLAMINGOS-2
spectrograph mounted on the Gemini-South telescope. Observations
began at ~7.7 d in the Ks filter with a total exposure of 912 s.

We detect the GRB afterglow (Oâ€™Connor et al. GCNs 32203 and 32217,
Rastinejad et al. GCN 32208, Malesani et al. GCN 32222) with magnitude
Ks~21.8 AB mag calibrated against stars in the 2MASS catalog. Compared
to earlier Ks data (Oâ€™Connor et al. GCN 32203, Rastinejad et al. GCN
32208), the infrared counterpartâ€™s temporal decay is consistent with the
decay observed in X-rays by Swift/XRT.

We thank the Gemini staff for rapid scheduling of these observations.


GRB_name: GRB220620A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32229
SUBJECT: GRB 220620A: Fermi GBM Final Real-time Localization
DATE:    22/06/20 01:43:22 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 01:32:06 UT on 20 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220620A (trigger 677381531.21551 / 220620064).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 109.4, Dec = 66.9 (J2000 degrees, equivalent to J2000 07h 17m, 66d 54'), with a statistical uncertainty of 2.6 degrees.

The angle from the Fermi LAT boresight is 133.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220620064/quicklook/glg_skymap_all_bn220620064.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/bn220620064/quicklook/glg_healpix_all_bn220620064.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220620064/quicklook/glg_lc_medres34_bn220620064.gif


GRB_name: GRB220619A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32231
SUBJECT: GRB 220619A: AstroSat CZTI detection
DATE:    22/06/20 04:59:25 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 220619A which was 
also detected by Fermi GBM (TrigNum: 677307509).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-06-19 04:58:41.500 UTC. The measured peak 
count rate associated with the burst is 139 (+37, -18) counts/s above 
the background in the combined data of three (out of four) quadrants, 
with a total of 2456 (+577, -573) counts. The local mean background 
count rate was 320 (+2, -3) counts/s. Using cumulative rates, we measure 
a T90 of 47 (+20, -15) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve peaks at 2022-06-19 
04:58:42.035 UTC. The measured peak count rate is 333 (+70, -39) 
counts/s above the background in the combined Veto data of all 
quadrants, with a total of 6930 (+826, -1099) counts. The local mean 
background count rate was 1405 (+3, -3) counts/s. We measure a T90 of 55 
(+15, -18) 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: GRB220620B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32233
SUBJECT: GRB 220620B: Fermi GBM Final Real-time Localization
DATE:    22/06/20 06:26:49 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:16:25 UT on 20 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220620B (trigger 677398590.943632 / 220620261).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 326.9, Dec = -44.6 (J2000 degrees, equivalent to J2000 21h 47m, -44d 36'), with a statistical uncertainty of 8.9 degrees.

The angle from the Fermi LAT boresight is 68.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220620261/quicklook/glg_skymap_all_bn220620261.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/bn220620261/quicklook/glg_healpix_all_bn220620261.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220620261/quicklook/glg_lc_medres34_bn220620261.gif


GRB_name: GRB220620A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32234
SUBJECT: Fermi GRB 220620A: Global MASTER-Net observations report 
DATE:    22/06/20 06:45:20 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev
(Irkutsk State University, API),

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

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

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


MASTER-OAGH robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Mexico (OAGH National Institute for Astrophysics, Optics and Electronics) started inspect of the Fermi GRB 220620A ( Fermi GBM team, GCN 32229) errorbox  13365 sec after notice time and 13402 sec after trigger time at 2022-06-20 05:15:28 UT, with upper limit up to  17.5 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -27.9 deg. 

The galactic latitude b = 28 deg., longitude l = 149 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2010828

We obtain a following upper limits.  

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

   13432 | 2022-06-20 05:15:28 |         MASTER-OAGH | (07h 10m 12.17s , +67d 39m 37.9s) |   C |    60 | 16.4 |        
   13432 | 2022-06-20 05:15:28 |         MASTER-OAGH | (07h 08m 49.08s , +68d 08m 56.2s) |   C |    60 | 16.9 |        
   13652 | 2022-06-20 05:19:08 |         MASTER-OAGH | (07h 30m 01.63s , +68d 09m 43.1s) |   C |    60 | 16.1 |        
   13652 | 2022-06-20 05:19:08 |         MASTER-OAGH | (07h 31m 15.11s , +67d 41m 43.0s) |   C |    60 | 13.9 |        
   13873 | 2022-06-20 05:22:49 |         MASTER-OAGH | (07h 15m 21.49s , +65d 46m 52.9s) |   C |    60 | 13.8 |        
   13873 | 2022-06-20 05:22:49 |         MASTER-OAGH | (07h 14m 04.15s , +66d 16m 23.8s) |   C |    60 | 15.9 |        
   14358 | 2022-06-20 05:30:54 |         MASTER-OAGH | (07h 34m 52.35s , +65d 46m 12.9s) |   C |    60 | 16.1 |        
   14358 | 2022-06-20 05:30:54 |         MASTER-OAGH | (07h 33m 37.45s , +66d 14m 59.2s) |   C |    60 | 16.4 |        
   14439 | 2022-06-20 05:32:15 |         MASTER-OAGH | (07h 10m 14.90s , +67d 41m 06.8s) |   C |    60 | 14.7 |        
   14439 | 2022-06-20 05:32:15 |         MASTER-OAGH | (07h 08m 52.19s , +68d 10m 24.0s) |   C |    60 | 16.4 |        
   14683 | 2022-06-20 05:36:19 |         MASTER-OAGH | (07h 31m 11.72s , +67d 40m 40.9s) |   C |    60 | 17.0 |        
   14683 | 2022-06-20 05:36:19 |         MASTER-OAGH | (07h 29m 50.03s , +68d 09m 26.4s) |   C |    60 | 16.9 |        
   14801 | 2022-06-20 05:38:17 |         MASTER-OAGH | (07h 15m 19.84s , +65d 47m 17.0s) |   C |    60 | 14.6 |        
   14801 | 2022-06-20 05:38:17 |         MASTER-OAGH | (07h 13m 57.08s , +66d 16m 46.3s) |   C |    60 | 16.2 |        
   14882 | 2022-06-20 05:39:38 |         MASTER-OAGH | (07h 04m 41.49s , +69d 33m 11.2s) |   C |    60 | 15.2 |        
   14882 | 2022-06-20 05:39:38 |         MASTER-OAGH | (07h 03m 10.86s , +70d 02m 25.2s) |   C |    60 | 16.6 |        
   15165 | 2022-06-20 05:44:21 |         MASTER-OAGH | (07h 27m 34.36s , +69d 35m 38.5s) |   C |    60 | 17.1 |        
   15165 | 2022-06-20 05:44:21 |         MASTER-OAGH | (07h 26m 08.83s , +70d 04m 14.5s) |   C |    60 | 17.5 |        
   15353 | 2022-06-20 05:47:29 |         MASTER-OAGH | (07h 50m 12.27s , +67d 41m 54.5s) |   C |    60 | 12.6 |        
   15353 | 2022-06-20 05:47:29 |         MASTER-OAGH | (07h 48m 59.51s , +68d 09m 40.1s) |   C |    60 | 13.0 |        
   16276 | 2022-06-20 06:02:51 |         MASTER-OAGH | (07h 48m 52.51s , +68d 09m 08.6s) |   C |    60 | 12.8 |        
   18478 | 2022-06-20 06:39:34 |         MASTER-OAGH | (07h 34m 44.93s , +65d 46m 15.6s) |   C |    60 | 12.9 |        
   18478 | 2022-06-20 06:39:34 |         MASTER-OAGH | (07h 33m 28.49s , +66d 14m 57.2s) |   C |    60 | 15.4 |        
   18560 | 2022-06-20 06:40:55 |         MASTER-OAGH | (07h 04m 45.02s , +69d 33m 39.3s) |   C |    60 | 15.5 |        
   18560 | 2022-06-20 06:40:55 |         MASTER-OAGH | (07h 03m 10.54s , +70d 03m 13.1s) |   C |    60 | 16.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220620B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32235
SUBJECT: Fermi GRB 220620B: Global MASTER-Net observations report 
DATE:    22/06/20 06:45:35 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 220620B ( Fermi GBM team, GCN 32233) errorbox  1110 sec after notice time and 1150 sec after trigger time at 2022-06-20 06:35:36 UT, with upper limit up to  17.0 mag. The observations began at zenith distance = 23 deg. The sun  altitude  is -62.5 deg. 

The galactic latitude b = -50 deg., longitude l = 355 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2011044

We obtain a following upper limits.  

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

    1180 | 2022-06-20 06:35:36 |         MASTER-OAFA | (21h 30m 36.32s , -43d 47m 50.1s) |   C |    60 | 17.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220617A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32237
SUBJECT: Konus-Wind detection of GRB 220617A
DATE:    22/06/20 16:16:01 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 220617A
(Fermi-GBM detection: Fermi GBM Team, GCN Circ 32209;
Wood, GCN Circ 32224;
Fermi-LAT detection: Di Lalla et al., GCN Circ 32212;
IPN triangulation: Kozyrev et al., GCN Circ 32220)
triggered Konus-Wind at T0=66669.24 s UT (18:31:09.240).

The burst light curve shows a multipeaked structure,
which starts at ~T0-0.2 s and has a total duration of ~0.5 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/GRB220617_T66669/

As observed by Konus-Wind, the burst
had a fluence of 6.53(-1.15,+1.34)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.028 s,
of 3.31(-1.27,+1.36)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = 0.02(-0.40,+0.57)
and Ep = 1384(-341,+504) keV (chi2 = 34/40 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 = 33/39 dof).

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


GRB_name: GRB220618A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32238
SUBJECT: GRB 220618A: iTelescope T-19 upper limit
DATE:    22/06/21 00:48:42 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

Y. Koyanagi, K. Hasuda, E. Kiuchi, N. Shimizu, T. Sakamoto (AGU)

We observed the field of GRB 220618A detected by Swift
(Troja et al., GCN Circ. 32214) with the iTelescope.Net
(http://www.itelescope.net) T19 (Planewave 17" CDK) telescope
located at the New Mexico Skies Observatory (NM, USA).
We took 10 images of 120 sec exposures in the Red filter
starting from June 18 at 09:46:36 (UT), about 0.6 hours after
the trigger and stopped at 10:09:40 (UT).

We do not detect the optical afterglow in the individual
images and the stacked image at the XRT position
(Osborne et al., GCN Circ. 32216). The estimated five sigma
upper limits of the combined image (total exposure of 1200 sec)
is 17.8 using the USNO-B1 catalog.


GRB_name: GRB220618A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32239
SUBJECT: GRB 220618A: Swift-BAT refined analysis
DATE:    22/06/21 12:26:59 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

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-239 to T+963 sec from the recent telemetry downlink,

we report further analysis of BAT GRB 220618A (trigger #1110821)

(Troja, et al., GCN Circ. 1110821).  The BAT ground-calculated position is

RA, Dec = 38.986, 55.218 deg which is 

   RA(J2000)  =  02h 35m 56.6s 

   Dec(J2000) = +55d 13' 05.0" 

with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).

The partial coding was 21%.

 

The BAT light curve showed a single peak structure with a duration of about 40 sec. 

T90 (15-350 keV) is 96.00 +- 65.97 sec (estimated error including systematics).

 

The time-averaged spectrum from -15.264 to 128.736 sec is best fit by a power law

with an exponential cutoff.  This fit gives a photon index 0.26 +- 0.85, 

and Epeak of 65.0 +- 16.9 keV (chi squared 53.40 for 56 d.o.f.).  For this

model the total fluence in the 15-150 keV band is 2.2 +- 0.3 x 10^-06 erg/cm2

and the 1-sec peak flux measured from T+8.24 sec in the 15-150 keV band is

0.8 +- 0.4 ph/cm2/sec.  A fit to a simple power law gives a photon index

of 1.61 +- 0.16 (chi squared 63.41 for 57 d.o.f.).  All the quoted errors

are at the 90% confidence level. 

 

The results of the batgrbproduct analysis are available at

http://gcn.gsfc.nasa.gov/notices_s/1110821/BA/

 

 


GRB_name: GRB220618A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32241
SUBJECT: GRB 220618A: Fermi GBM detection
DATE:    22/06/21 16:48:36 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 09:10:19.59 UT on 18 June 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220618A (trigger 677236224 / 220618382)
which was also detected by the Swift/BAT (Troja et al. 2022, GCN 32214).

The angle from the Fermi LAT boresight at the GBM trigger time is 35
degrees.

The GBM light curve consists of a single peak followed
by some extended emission with a duration (T90) of about 44 s (50-300 keV).
The time-averaged spectrum from T0-4.096 s to T0+24.576 s
is best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.30 +/- 0.13  and
the cutoff energy, parameterized as Epeak, is 126 +/- 8 keV.

The event fluence (10-1000 keV) in this time interval is
(3.6 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+10.05 s in the 10-1000 keV band
is 2.3 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB220623A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32243
SUBJECT: GRB 220623A: Swift detection of a burst
DATE:    22/06/23 07:20:12 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

B. Sbarufatti (PSU), K. L. Page (U Leicester),
T. M. Parsotan (GSFC/UMBC/CRESSTII), M. H. Siegel (PSU) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 07:04:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220623A (trigger=1111672).  Swift did not slew immediately 
to the burst. 
The BAT on-board calculated location is 
RA, Dec 145.462, +75.828 which is 
   RA(J2000) = 09h 41m 51s
   Dec(J2000) = +75d 49' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 25 sec. One peak occurred before 
the trigger and another occurred at the trigger time.  The peak count 
rate was ~9000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+61.4
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB220623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32244
SUBJECT: GRB 220623A: Swift-XRT observations
DATE:    22/06/23 08:35:46 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), G. Cusumano (INAF-IASF PA), M. Perri (SSDC &
INAF-OAR), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester) and
D.N. Burrows (PSU) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 220623A at 08:11:23.5 UT,
4029.1 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 145.39717,
75.82155 which is equivalent to:
   RA(J2000)  = 09h 41m 35.32s
   Dec(J2000) = +75d 49' 17.6"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 61 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 (2.49 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.4
(+2.74/-2.39) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB220623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32245
SUBJECT: GRB 220623A: iTelescope optical upper limit
DATE:    22/06/23 10:17:01 GMT
FROM:    Filipp Dmitrievich Romanov at Amateur astronomer  <filipp.romanov.27.04.1997@gmail.com>

I observed the field of GRB 220623A (Sbarufatti et al., GCN Circ.
32243) remotely using telescope T24 (0.61-m f/6.5 reflector + CCD) of
iTelescope.Net in Sierra Remote Observatory (Auberry, California, USA)
on 2022-06-23. Three images (exposures 300 seconds, BINx1) were
obtained with Ic filter with mid time 09:26:42 UTC (8548 seconds after
the trigger). I did not detect any optical afterglow in the BAT and
the XRT (Kennea et al., GCN Circ. 32244) positions. The magnitude
limit is about 18 mag, compared to the magnitudes of nearby stars from
the USNO-B1.0 Catalog (Monet et al., 2003).
F. D. Romanov.


GRB_name: GRB220623A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32246
SUBJECT: GRB 220623A: AstroSat CZTI detection
DATE:    22/06/23 11:15:23 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 220623A which was 
also detected by Swift-BAT (Sbarufatti et al., GCN 32243), Swift-XRT 
(Kennea et al., GCN 32244) and INTEGRAL SPI-ACS (TrigNum: 9966).

The source was clearly detected in the 20-200 keV energy range. The 
light curve showed multiple peaks of emission with the strongest peak at 
2022-06-23 07:04:14.500 UTC. The measured peak count rate associated 
with the burst is 127 (+38, -17) counts/s above the background in the 
combined data of three (out of four) quadrants, with a total of 738 
(+204, -207) counts. The local mean background count rate was 360 (+2, 
-2) counts/s. Using cumulative rates, we measure a T90 of 9 (+9, -2) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve showed multiple peaks 
of emission with the strongest peak at 2022-06-23 07:04:13.771 UTC. The 
measured peak count rate is 570 (+74, -60) counts/s above the background 
in the combined Veto data of all quadrants, with a total of 2919 (+440, 
-459) counts. The local mean background count rate was 1502 (+5, -5) 
counts/s. We measure a T90 of 8 (+4, -1) s from the cumulative Veto 
light curve.

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


GRB_name: GRB220623A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32247
SUBJECT: GRB 220623A: AGILE detection
DATE:    22/06/23 11:41:48 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), F. Lucarelli, C. Pittori, F. Verrecchia (SSDC, and
INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M.
Cardillo, C. Casentini, Y. Evangelista, L. Foffano, E. Menegoni, G. Piano
(INAF/IAPS), A. Bulgarelli, A. Di Piano, V. Fioretti, N. Parmiggiani
(INAF/OAS-Bologna), 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 the GRB 220623A at T0 = 2022-06-23 07:04:14 s
(UTC), reported by Swift BAT (GCN #32243), Swift XRT (GCN #32244), and
AstroSat CZTI (GCN #32246). The burst is clearly visible in the AGILE
scientific ratemeters of the SuperAGILE (SA; 20-60 keV), MiniCALorimeter
(MCAL; 0.4-100 MeV), and AntiCoincidence (AC; 50-200 keV) detectors. The
event lasted about 25 s and it released a total number of 1950 counts in
the SA detector (above a background rate of 85 Hz), 29800 counts in the
MCAL detector (above a background rate of 1050 Hz), and 72370 counts in the
AC detector (above a background rate of 2770 Hz). The AGILE ratemeters
light curves can be found at
http://www.agilescienceapp.it/notices/GRB220623A_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, from T1 = 2022-06-23 07:04:09.65 s (UTC) to T2 = 2022-06-23
07:04:16.15 s (UTC), and released 4200 counts in the detector, above a
background rate of 530 Hz. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB220623A_078852_583052654.000000.png
. At the T0, the event was 35 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: GRB220623A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32248
SUBJECT: GRB 220623A: Enhanced Swift-XRT position
DATE:    22/06/23 15:39:19 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 1568 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 220623A, 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 = 145.39376, +75.82100 which is equivalent
to:

RA (J2000): 09h 41m 34.50s
Dec (J2000): +75d 49' 15.6"

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: GRB220623B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32249
SUBJECT: GRB 220623B: Fermi GBM Final Real-time Localization
DATE:    22/06/23 15:44:25 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 15:33:56 UT on 23 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220623B (trigger 677691241.431566 / 220623649).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 216.1, Dec = 50.2 (J2000 degrees, equivalent to J2000 14h 24m, 50d 12'), with a statistical uncertainty of 4.1 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/bn220623649/quicklook/glg_skymap_all_bn220623649.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/bn220623649/quicklook/glg_healpix_all_bn220623649.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220623649/quicklook/glg_lc_medres34_bn220623649.gif


GRB_name: GRB220609B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32250
SUBJECT: Konus-Wind detection of GRB 220609B
DATE:    22/06/23 16:56:10 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220609B (CALET-CGBM detection: Asaoka et al., GCN Circ 32185;
AstroSat-CZTI detection: Gopalakrishnan et al., GCN Circ 32186;
IPN localization: Kozyrev et al., GCN 32190)
triggered Konus-Wind (KW) at T0=44473.865 s UT (12:21:13.865).

The burst light curve shows a single emission pulse
which starts at ~T0-1.5 s and has a total duration of ~18 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/GRB220609_T44473/

As observed by Konus-Wind, the burst had
a fluence of (1.0 Â± 0.1)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 4.544 s,
of (2.7 Â± 0.2)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+14.592 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.79 (-0.11,+0.13),
the high energy photon index beta = -2.02 (-0.14,+0.10),
the peak energy Ep = 537 (-86,+112) keV,
chi2 = 113/98 dof.

The spectrum near the peak count rate (measured from T0 to T0+6.400 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.83 (-0.06,+0.07),
the high energy photon index beta = -2.04 (-0.17,+0.12),
the peak energy Ep = 748 (-145,+170) keV,
chi2 = 88/97 dof.

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


GRB_name: GRB220623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32251
SUBJECT: GRB 220623A: BOOTES-5/JGT optical afterglow detection
DATE:    22/06/23 17:57:34 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), D. Hiriart and W. H. Lee (UNAM), C. J. Perez del Pulgar and I. Carrasco (UMA), I. H. Park (SKKU) on behalf of a larger collaboration, report:

Following the detection of GRB 220623A by both Swift (Sbarufatti et al. GCNC 32243), AstroSat (Gopalakrishnan et al. GCNC 32246) and AGILE (Ursi et al. GCNC 32247), the 60cm BOOTES-5/JGT robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) automatically responded to the burst on June 23 at 07:05:03 UT (i.e. ~ 47 s after trigger). In the first 1 s exposure image, an optical afterglow is detected at the enhanced Swift-XRT position (Beardmore et al. GCNC 32248) with a preliminary magnitude of 17.1 +- 0.2 mag (clear filter). Further observations are ongoing and encouraged.

We thank the staff at San Pedro Martir Observatory for their excellent support.


GRB_name: GRB220623A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32252
SUBJECT: GRB 220623A: Swift/UVOT Upper Limits
DATE:    22/06/23 18:32:09 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 220623A
4034 s after the BAT trigger (Sbarufatti et al., GCN Circ. 32243).
No optical afterglow consistent with the XRT position
(Kennea et al. GCN Circ. 32244)
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          4034         4184          147         >19.9
white             4034         5415          344         >20.1
v                 4190         9642          326         >18.9
b                 5010         5210          197         >19.4
u                 4805         5005          197         >19.0
w1                4600         4800          197         >19.3
m2                4395         4595          197         >19.9
w2                5421         5621          197         >19.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.036 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32253
SUBJECT: GRB 220623A: NOT optical observations
DATE:    22/06/23 23:43:30 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Radboud Univ. and DAWN/NBI), L. Izzo (DARK/NBI), J. S. 
Thomsen (NOT), R. Clavero (IAC) report on behalf of a larger collaboration:

We observed the field of GRB 220623A (Sbarufatti et al., GCN 32243) 
using the Nordic Optical Telescope (NOT) equipped with the ALFOSC 
imager. Two sets of observations were acquired in the r and z filters, 
with mid times 2022 Jun 23.890 and 23.903 UT (14.3 and 14.6 hr after the 
trigger, respectively). The exposure times were 3x300 and 5x200 s in r 
and z, respectively.

No source is detected in our images within or close to the GRB XRT 
position (Evans et al., GCN 32248), down to the following 3-sigma limits:

r > 23.4 (AB);
z > 22.5 (AB).

Flux calibration was carried out against nearby stars from the 
Pan-STARRS catalog.


GRB_name: GRB220623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32254
SUBJECT: GRB 220623A: Swift-XRT refined Analysis
DATE:    22/06/24 01:14:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.4 ks of XRT data for GRB 220623A (Sbarufatti et al.
GCN Circ. 32243), from 4.0 ks to 57.1 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN Circ.
32248).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.85 (+0.14, -0.13).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.92 (+0.19, -0.18). The
best-fitting absorption column is  2.0 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 2.5 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 3.7 x 10^-11 (4.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.0 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 2.5 x 10^20 cm^-2
Excess significance: 4.7 sigma
Photon index:      1.92 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
1.85, the count rate at T+24 hours will be 1.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.0 x
10^-14 (9.3 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/01111672.

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


GRB_name: GRB220623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32255
SUBJECT: GRB 220623A: AbAO optical upper limit
DATE:    22/06/24 01:50:04 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 220623A detected by Swift (Sbarufatti et 
al., GCN 32243; Kennea et al., GCN 32244), AstroSat (Gopalakrishnan et 
al., GCN 32246) and AGILE (Ursi et al., GCN 32247) with AS-32 telescope 
of Abastumani Observatory (AbAO). We do not detect any optical sources 
within enhanced XRT position (Beardmore et al., GCN 32248). In 
particular we do not detect the source reported by Y.-D. Hu et al. (GCN 
32251). Preliminary upper limit of a stacked image is following:

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

2022-06-23 17:53:02  0.47313  65*60  R      n/d    n/d    21.5

The photometry is based on nearby USNO-B1.0 stars, R2 magnitude
USNO-B1.0_id R2
1658-0059467 15.40
1658-0059509 15.39


GRB_name: GRB220624A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32256
SUBJECT: GRB 220624A: Fermi GBM Final Real-time Localization
DATE:    22/06/24 03:08:52 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 02:58:35 UT on 24 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220624A (trigger 677732320.15865 / 220624124).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 179.0, Dec = 20.4 (J2000 degrees, equivalent to J2000 11h 56m, 20d 23'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 83.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220624124/quicklook/glg_skymap_all_bn220624124.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/bn220624124/quicklook/glg_healpix_all_bn220624124.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220624124/quicklook/glg_lc_medres34_bn220624124.gif


GRB_name: GRB220624B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32257
SUBJECT: GRB 220624B: Fermi GBM Final Real-time Localization
DATE:    22/06/24 10:30:39 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 10:20:24 UT on 24 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220624B (trigger 677758829.234126 / 220624431).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 97.8, Dec = 41.6 (J2000 degrees, equivalent to J2000 06h 31m, 41d 36'), with a statistical uncertainty of 4.1 degrees.

The angle from the Fermi LAT boresight is 92.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220624431/quicklook/glg_skymap_all_bn220624431.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/bn220624431/quicklook/glg_healpix_all_bn220624431.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220624431/quicklook/glg_lc_medres34_bn220624431.gif


GRB_name: GRB220623A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32258
SUBJECT: Konus-Wind detection of GRB 220623A
DATE:    22/06/24 12:32:17 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220623A (Swift detection: Sbarufatti et al., GCN Circ. 32243;
AstroSat-CZTI detection: Gopalakrishnan et al., GCN Circ 32246;
AGILE detection: Ursi et al., GCN Circ 32247)
triggered Konus-Wind (KW) at T0=25447.564 s UT (07:04:07.564).

The burst light curve shows a bright, double-peaked structure
which starts at ~T0-0.2 s and has a total duration of ~15 s.
A weaker emission in visible in the KW lc until ~T0+50 s.
The emission at the bright phase of the event is seen up to ~2.5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB220623_T25447/

As observed by Konus-Wind, the burst had
a fluence of (2.5 Â± 0.3)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 0.064 s,
of (8.8 Â± 0.8)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+49.408 s)
is best fit in the 20 keV - 15 MeV range
by a power law with exponential cutoff (CPL) model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.13(-0.11,+0.12) and Ep = 869(-224,+363) keV (chi2 = 93/98 dof).
Fitting this spectrum by a Band function yields the same values of alpha and Ep,
and an upper limit on the high energy photon index beta of -2.6 (chi2 = 93/97 dof).

The spectrum near the peak count rate (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range by a CPL function
with  alpha = -0.82(-0.09,+0.10) and Ep = 910(-136,+177) keV (chi2 = 86/98 dof).
Fitting this spectrum by a Band function yields the same values of alpha and Ep,
and an upper limit on the high energy photon index beta of -2.9 (chi2 = 86/97 dof).

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


GRB_name: GRB220624A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32259
SUBJECT: GRB 220624A: AGILE detection
DATE:    22/06/24 14:47:15 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the long GRB 220624A at T0 = 2022-06-24
02:58:35 s (UTC), reported by Fermi GBM (GCN #32256). The burst is clearly
visible in the AGILE scientific ratemeters of the SuperAGILE (SA; 20-60
keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and AntiCoincidence (AC; 50-200
keV) detectors. The event lasted about 57 s and it released a total number
of 5930 counts in the SA detector (above a background rate of 70 Hz), 88920
counts in the MCAL detector (above a background rate of 1135 Hz), and
212145 counts in the AC detector (above a background rate of 3195 Hz). The
AGILE ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/GRB220624A_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, from T1 = 2022-06-24 02:58:34.36 s (UTC) to T2 = 2022-06-24
02:58:46.85 s (UTC), and released 14630 counts in the detector, above a
background rate of 620 Hz. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB220624A_078864_583124315.000000.png
. At the T0, the event was 20 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: GRB220624A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32261
SUBJECT: GRB 220624A: AGILE/GRID analysis
DATE:    22/06/24 17:36:04 GMT
FROM:    Francesco Verrecchia at SSDC,INAF-OAR  <francesco.verrecchia@ssdc.asi.it>

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

The Gamma-Ray Imaging Detector (GRID) of AGILE detected a gamma-ray 
transient
temporally coincident with the long  GRB 220624A reported by Fermi/GBM in
GCN #32256 and also detected by AGILE/MCAL (Ursi et al., GCN #32259).

A preliminary GRID analysis shows a detection with a statistical 
significance
above 8 sigma over a time integration of 20 s starting from the T0 of GRB
220624A, at a sky position compatible with that of the GRB.
We obtained 25 events 2 of which are notably above 1 GeV.

The GRB position was about 30 deg off-axis from the GRID boresight.

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: GRB220611A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32262
SUBJECT: GRB 220611A: X-ray afterglow Chandra sub-arcsecond localization
DATE:    22/06/24 18:10:44 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

A. J. Levan (Radboud Univ.), D. B. Malesani (Radboud Univ. and 
DAWN/NBI), B. P. Gompertz (Birmingham) report on behalf of a larger 
collaboration:

The Chandra X-ray observatory imaged the X-ray afterglow of GRB 220611A 
(Cenko et al., GCN 32191). Observations started on 2022 Jun 23.92 UT 
(12.15 days after the GRB), using the ACIS-S instrument, for a total 
exposure time of 15 ks.

We detect a single object consistent with the Swift X-ray position (Goad 
et al., GCN 32192), with a total of ~30 source counts. Its coordinates 
are (J2000):

RA = 04:26:03.57
Dec = -37:15:35.1

with an uncertainty of ~0.5". This position is consistent with the 
optical and near-infrared source reported by Gemini-S (Oâ€™Connor et al., 
GCN 32203, 32217; Rastinejad et al., GCN 32208) and VLT (Malesani et 
al., GCN 32222), as well as with the source seen in archival images from 
the Legacy Survey. This detection thus cements the nature of this object 
as the mutli-wavelength afterglow of GRB 220611A.

We thank the Chandra director, Pat Slane, for awarding discretionary 
time to this project, and the observatory staff for rapidly planning and 
scheduling these observations.


GRB_name: GRB220624A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32263
SUBJECT: GRB 220624A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/06/24 18:45:57 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 220624A onboard (T0:
2022-06-24T02:58:35 UTC, Fermi/GBM GCN 32256, CALET trig # 1340074490,
AGILE GCN 32259,32261).

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

Upon trigger 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 75 in a 16.384
s analysis time bin.
The burst episode as seen by BAT is ~50 s long.

NITRATES results indicate a burst coming from outside of the coded
FoV, with DeltaLLHOut of -427. The NITRATES maximum likelihood sky
position is consistent with the Fermi/GBM localization region.

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: GRB220623A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32264
SUBJECT: GRB 220623A: Swift-BAT refined analysis
DATE:    22/06/24 18:49:10 GMT
FROM:    Tyler Parsotan at UMBC/GSFC/CRESST II  <parsotat@umbc.edu>

ï»¿
T. Parsotan (GSFC/UMBC), S. D. Barthelmy (GSFC), 
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), (i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+842 sec from the recent telemetry downlink, we report further analysis of BAT GRB 220623A (trigger #1111672) (Sbarufatti, et al., GCN Circ. 32243).  The BAT ground-calculated position is
RA, Dec = 145.459, 75.823 deg which is 
   RA(J2000)  =  09h 41m 50.1s 
   Dec(J2000) = +75d 49' 22.9" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 94%.
 
The BAT light curve showed a triple-peaked structure. One possible precursor peak occurred prior to the trigger, another occurred at the trigger time, and the final occurred 10 s post trigger. At ~40 s there may be broad emission as well.  T90 (15-350 keV) is 57.11 +- 8.53 sec (estimated error including systematics).
 
The time-averaged spectrum from -3.84 to 73.652 sec is best fit by a simple power-law model.  The power law index of the time-averaged spectrum is 1.33 +- 0.07.  The fluence in the 15-150 keV band is 3.5 +- 0.1 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T-0.15 sec in the 15-150 keV band is 4.5 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence level. 
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1111672/BA/
 


GRB_name: GRB220624A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32265
SUBJECT: IPN triangulation of GRB 220624A
DATE:    22/06/24 22:08:37 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

J. Benkhoff on behalf of the BepiColombo team,

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

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

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

and

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

The long-duration GRB 220624A
(Fermi/GBM detection: Fermi GBM Team, GCN 32256;
AGILE detection: Ursi et al., GCN 32259;
AGILE/GRID detection: Verrecchia et al., GCN 32261;
Swift/BAT-GUANO detection: Tohuvavohu et al., GCN 32263)
has been detected by Fermi (GBM trigger 677732320),
Konus-Wind, Mars-Odyssey (HEND), BepiColombo (MGNS),
CALET (CGBM), AGILE (SA, MCAL, AC), and Swift (BAT),
so far, at about 10715 s UT (02:58:35).
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:
  179.348 (11h 57m 24s) +16.691 (+16d 41' 27")
 Corners:
  179.501 (11h 58m 00s) +16.922 (+16d 55' 18")
  179.357 (11h 57m 26s) +16.791 (+16d 47' 29")
  179.194 (11h 56m 47s) +16.456 (+16d 27' 20")
  179.339 (11h 57m 21s) +16.590 (+16d 35' 25")
 ---------------------------------------------
The error box area is 91 sq. arcmin, and its maximum
dimension is 33 arcmin (the minimum one is 4 arcmin).
The Sun distance was 80 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM final localization (GCN 32256).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220624_T10712/IPN

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


GRB_name: GRB220624A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32267
SUBJECT: Fermi GRB 220624A: Global MASTER-Net observations report 
DATE:    22/06/25 00:15:21 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 220624A ( Fermi GBM team, GCN 32256) errorbox  73147 sec after notice time and 73182 sec after trigger time at 2022-06-24 23:18:17 UT, with upper limit up to  16.8 mag. The observations began at zenith distance = 53 deg. The sun  altitude  is -20.2 deg. 

The galactic latitude b = 76 deg., longitude l = 240 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2014237

We obtain a following upper limits.  

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

   73212 | 2022-06-24 23:18:17 |         MASTER-OAFA | (11h 46m 48.60s , +19d 37m 00.6s) |   C |    60 | 16.8 |        
   73488 | 2022-06-24 23:22:52 |         MASTER-OAFA | (11h 55m 57.05s , +21d 32m 42.9s) |   C |    60 | 16.0 |        
   73599 | 2022-06-24 23:24:44 |         MASTER-OAFA | (12h 04m 29.08s , +21d 31m 52.7s) |   C |    60 | 15.5 |        
   73710 | 2022-06-24 23:26:35 |         MASTER-OAFA | (11h 54m 38.45s , +17d 43m 50.5s) |   C |    60 | 16.4 |        
   74306 | 2022-06-24 23:36:31 |         MASTER-OAFA | (11h 46m 41.60s , +19d 37m 49.0s) |   C |    60 | 16.0 |        
   74397 | 2022-06-24 23:38:02 |         MASTER-OAFA | (11h 55m 14.99s , +19d 38m 51.1s) |   C |    60 | 15.5 |        
   74671 | 2022-06-24 23:42:35 |         MASTER-OAFA | (11h 54m 39.68s , +17d 43m 02.0s) |   C |    60 | 16.2 |        
   75428 | 2022-06-24 23:55:13 |         MASTER-OAFA | (11h 46m 48.65s , +19d 36m 57.2s) |   C |    60 | 12.3 |        
   75520 | 2022-06-24 23:56:44 |         MASTER-OAFA | (11h 55m 16.98s , +19d 38m 15.4s) |   C |    60 | 14.0 |        
   75611 | 2022-06-24 23:58:16 |         MASTER-OAFA | (11h 55m 54.10s , +21d 31m 13.9s) |   C |    60 | 13.8 |        
   75702 | 2022-06-24 23:59:47 |         MASTER-OAFA | (12h 04m 34.80s , +21d 32m 30.2s) |   C |    60 | 12.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220623B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32268
SUBJECT: Fermi GRB 220623B: Global MASTER-Net observations report 
DATE:    22/06/25 03:15:44 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 220623B ( Fermi GBM team, GCN 32249) errorbox  1 days 36625 sec after notice time and 1 days 36660 sec after trigger time at 2022-06-25 01:44:57 UT, with upper limit up to  15.2 mag. The observations began at zenith distance = 79 deg. The sun  altitude  is -51.2 deg. 

The galactic latitude b = 61 deg., longitude l = 91 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2013845

We obtain a following upper limits.  

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

  123091 | 2022-06-25 01:44:57 |         MASTER-OAFA | (14h 18m 37.96s , +46d 12m 54.9s) |   C |    60 | 13.2 |        
  123182 | 2022-06-25 01:46:28 |         MASTER-OAFA | (14h 30m 27.39s , +46d 11m 45.4s) |   C |    60 | 14.3 |        
  123365 | 2022-06-25 01:49:31 |         MASTER-OAFA | (14h 22m 37.30s , +44d 17m 08.1s) |   C |    60 | 15.1 |        
  123456 | 2022-06-25 01:51:02 |         MASTER-OAFA | (14h 40m 59.56s , +46d 12m 28.2s) |   C |    60 | 13.9 |        
  123547 | 2022-06-25 01:52:33 |         MASTER-OAFA | (14h 32m 42.08s , +44d 18m 51.9s) |   C |    60 | 15.0 |        
  124384 | 2022-06-25 02:06:30 |         MASTER-OAFA | (14h 40m 59.88s , +46d 12m 07.3s) |   C |    60 | 15.0 |        
  125523 | 2022-06-25 02:25:29 |         MASTER-OAFA | (14h 32m 47.38s , +44d 16m 53.1s) |   C |    60 | 15.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220624A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32269
SUBJECT: GRB 220624A: Fermi GBM Detection
DATE:    22/06/25 15:25:40 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

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

"At 02:58:35 UT on 24 June 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220624A (trigger 677732320/220624124)
which was also detected by AGILE (A. Ursi, et al. 2022, GCN 32259),
Swift/BAT-GUANO (A. Tohuvavohu et al., GCN 32263),
and localized by IPN (A. S. Kozyrev et al. 2022, GCN 32265).
The Fermi GBM Final Real-time Localization (GCN 32256) is consistent with
the IPN triangulation.

The angle from the Fermi LAT boresight is 86 degrees.

The GBM light curve shows two bright emission episodes
and one faint emission episode with a duration (T90)
of about 285 s (10-1000 keV).

The time-averaged spectrum for the first emission episode
from T0-0.5 to T0+59.9 s is best fit by
a Band function with Epeak = 486 +/- 12 keV,
alpha = -0.75 +/- 0.01, and beta = -2.39 +/- 0.06.
The event fluence (10-1000 keV) in this time interval is
(1.550 +/- 0.001)E-04 erg/cm^2.

The time-averaged spectrum for the second emission episode
from T0+137.7 to T0+172.5 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.23 +/- 0.06 and the cutoff energy,
parameterized as Epeak, is 132 +/- 8 keV.
The event fluence (10-1000 keV) in this time interval is
(1.19 +/- 0.04)E-05 erg/cm^2.
A Band function fits the spectrum equally well
with Epeak= 124 +/- 11 keV, alpha = -1.19 +/- 0.07 and beta = -2.8 +/- 0.5.

The time-averaged spectrum for the third emission episode
from T0+285.2 to T0+333.3 s is best fit by
a Band function with Epeak = 61 +/- 10 keV,
alpha = 1.3 +/- 1.0, and beta = -2.0 +/- 0.1.
The event fluence (10-1000 keV) in this time interval is
(7.3 +/- 0.5)E-06 erg/cm^2.

The 1-sec peak photon flux measured starting from T0+6.0 s
in the 10-1000 keV band is 39.1 +/- 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: GRB220623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32271
SUBJECT: GRB 220623A: T193-OHP optical upper limit
DATE:    22/06/26 16:43:42 GMT
FROM:    Benjamin Schneider at CEA  <benjamin.schneider@cea.fr>

B. Schneider, D. Turpin, E. Le Flocâ€™h (CEA), C. Adami, 
S. Basa (LAM), S. Vergani, J. Palmerio (GEPI) 
report on behalf of a larger collaboration:

We observed the field of GRB 220623A (Sbarufatti et al. GCN 32243; 
Gopalakrishnan et al. GCN 32246; Ursi et al. GCN 32247) using 
the T193cm telescope at Observatoire de Haute-Provence (France) 
equipped with the MISTRAL spectro-imager. Six exposures 
(1x300s + 5x600s) were obtained in the i band using the red MISTRAL 
set-up from 2022 23 Jun 21:32:10 UT to 2022 23 Jun 23:05:49 UT 
(mid time ~15.2h after trigger). Data reduction is still preliminary. 
In the combined frame, we do not detect any source within the 2.2 arsec
error circle of the enhanced XRT position (Evans et al. GCN 32248; 
Beardmore et al. GCN 32248) down to the following 3-sigma limit:

i > 21.5 mag (AB)

The photometric calibration was performed using nearby stars 
from the PanSTARRS catalog.

We acknowledge the support from Observatoire de Haute-Provence, 
in particular Jean-Pierre Troncin and Jerome Schmidt.


GRB_name: GRB220624A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32272
SUBJECT: GRB 220624A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/06/27 03:03:19 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

Y. Akaike (Waseda U), A. Yoshida, T. Sakamoto, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), S. Torii, 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 220624A (Fermi GBM Final Real-time Localization: Fermi GBM team,
GCN Circ. 32256; AGILE detection: Ursi et al., GCN Circ. 32259; AGILE/GRID analysis:
Verrecchia et al., GCN Circ: 32261; Swift/BAT-GUANO detection: Tohuvavohu et al., 
GCN Circ. 32263; IPN triangulation: Kozyrev et al., GCN Circ. 32265; Fermi-GBM 
Detection: Lesage et al., GCN Circ. 32269) triggered the CALET Gamma-ray Burst 
Monitor (CGBM) at 02:58:32.538 UTC on 24 June 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1340074490/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure which starts at T+2.5 sec.
The whole episode was not seen by CGBM because the sequence of the HV
turn-off started from T+20 sec.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1340074490/

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


GRB_name: GRB220623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32273
SUBJECT: GRB 220623A: GIT optical upper limits.
DATE:    22/06/27 08:51:40 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

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

We observed GRB 220623A detected by Swift (Sbarufatti et al., GCN 32243;
Kennea et al., GCN 32244), AstroSat (Gopalakrishnan et al., GCN 32246) and
AGILE (Ursi et al., GCN 32247), with the 0.7m GROWTH-India Telescope (GIT).
The observations started at 15:05:15 UT on 2022-06-23, 8.02 hours 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 2.1
arcsec radius circle around R.A.= 09h 41m 34.50s, Dec.= +75d 49' 15.6â€ (Phil
Evans et al. GCN #32248). The obtained upper limits follow as:

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

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

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

 2459754.132298985 | 8.10 | 3 x 300 (stacked) | r' | > 21.10 |

 2459754.141603815 | 8.32 | 2 x 300 (stacked) | g' | > 21.01 |

 2459754.149142145 | 8.50 | 2 x 300 (stacked) | i' | > 20.23 |

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

These upper limits are consistent with Benjamin et al.(GCN #32271), Alexei
et al.(GCN #32255), Daniele et al.(GCN #32253), Alexander et al.(GCN
#32252), Filipp et al.(GCN #32245). The magnitudes are calibrated against
PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic
extinction.


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree
field of view, set up by the Indian Institute of Astrophysics (IIA) and the
Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and
IUSSTF. It is located at the Indian Astronomical Observatory (Hanle),
operated by IIA. We acknowledge funding by the IITB alumni batch of 1994,
which partially supports operations of the telescope. Telescope technical
details are available at https://sites.google.com/view/growthindia/.


GRB_name: GRB220627A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32278
SUBJECT: GRB 220627A: Fermi GBM Final Real-time Localization
DATE:    22/06/27 21:31:11 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 21:21:00 UT on 27 Jun 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220627A (trigger 678057665.085772 / 220627890).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 211.5, Dec = -35.1 (J2000 degrees, equivalent to J2000 14h 05m, -35d 06'), with a statistical uncertainty of 4.2 degrees.

The angle from the Fermi LAT boresight is 20.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220627890/quicklook/glg_skymap_all_bn220627890.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/bn220627890/quicklook/glg_healpix_all_bn220627890.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220627890/quicklook/glg_lc_medres34_bn220627890.gif


GRB_name: GRB220627A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32280
SUBJECT: Fermi GRB 220627A: Global MASTER-Net observations report 
DATE:    22/06/27 22:00:31 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-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 220627A ( Fermi GBM team, GCN 32278) errorbox  579 sec after notice time and 592 sec after trigger time at 2022-06-27 21:30:52 UT, with upper limit up to  19.9 mag. The observations began at zenith distance = 39 deg. The sun  altitude  is -72.1 deg. 

The galactic latitude b = 25 deg., longitude l = 320 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2016919

We obtain a following upper limits.  

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

     653 | 2022-06-27 21:30:52 |         MASTER-SAAO | (14h 04m 14.66s , -35d 01m 06.7s) |   C |   120 | 19.9 |        
     802 | 2022-06-27 21:33:12 |         MASTER-SAAO | (14h 04m 12.35s , -34d 59m 11.6s) |   C |   140 | 19.9 |        
    1231 | 2022-06-27 21:41:01 |         MASTER-SAAO | (14h 06m 01.84s , -34d 45m 29.2s) |   C |    60 | 19.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32281
SUBJECT: GRB 220627A: MeerLICHT detection of two afterglow candidates
DATE:    22/06/28 02:12:29 GMT
FROM:    Paul Groot at Radboud University Nijmegen  <p.groot@astro.ru.nl>

P.J. Groot (Radboud/UCT/SAAO), S. de Wet (UCT/SAAO), P.M. Vreeswijk
(Radboud) report on behalf of the MeerLICHT consortium:

Following the detection of GRB220627A by Fermi (Fermi GBM team, GCN
32278) the MeerLICHT 0.6m wide-field optical telescope, located at
SAAO Sutherland, South Africa, started scanning the error box at
2022-06-27 21:43 UT (T0+23 minutes and 3 minutes after the alert was
received). Observations were obtained in the q-band (440-720nm), using
52 tiles (146 square degrees) to cover a 71% cumulative
probabilty. Before the observability limit of HA=+4.5 hr was reached
32.4 square degrees were covered at least twice, covering a cumulative
probability of 7.5% of the Fermi error box.

Automatic data processing using BlackBOX/ZOGY resulted in 7 new
transients that were observed at least twice and were detected with a
significance >12 in the difference images. Five of these candidates
can be associated to known asteroids. 

The remaining two candidates are uncataloged and are both detected
three times: 

Candidate 1 is MLTJ143615.50-360417.3,
at RA,Dec (ICRS) 14:36:15.50, -36:04:17.3 (219.06459,-36.07149),
first detected at q_AB = 18.13+/-0.03 on 2022-06-27 22:50:22/05 (MJD
59757.95164). Last non-detection was on MJD 58971.02.19 at q_AB > 20.35
(for a transient source).  

Candidate 2 is MLTJ143614.90-373629.0,
at RA,Dec (ICRS) 14:36:14.90. -37:36:29.0 (219.06217,-37.60809),
first detected at q_AB = 19.62+/-0.10, on 2022-06-27 22:53:20.54 (MJD
59757.95371). Last non-detection was on MJD 59737.8835 at q_AB > 20.82

Candidate 1 shows the presence of an underlying object in the MeerLICHT
reference image at q_AB = 20.72, possibly a host galaxy. 
Candidate 2 shows no underlying source in the MeerLICHT reference image
with a limiting magnitude of q_AB > 20.28. 

During the three MeerLICHT observations Candidate 1 evolved to q_AB =
18.21 +/-0.02 at 2022-06-27 23:16:51 (MJD 59757.97004). Candidate 2
brightened to q_AB = 19.43 +/- 0.10 at 2022-06-27 23:18:14 (MJD
59757.97100).

Follow-up observations of both candidates are encouraged. 

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: GRB220627A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32283
SUBJECT: GRB 220627A: Fermi-LAT detection
DATE:    22/06/28 07:00:40 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

N. Di Lalla (Stanford Univ.), M. Axelsson (KTH & Stockholm Univ.), M. Arimoto (Kanazawa Univ.), N. Omodei (Stanford Univ.) and M. Crnogorevi (Univ. of Maryland & NASA/GSFC) report on behalf of the Fermi-LAT team:

On June 27, 2022, Fermi-LAT detected high-energy emission from GRB 220627A, which was also detected by Fermi-GBM (trigger 678057665 / 220627890, GCN 32278).

The best LAT on-ground location is found to be

RA, Dec = 201.2, -32.5 (degrees, J2000)

with an error radius of 0.2 deg (90 % containment, statistical error only). This was 27 deg from the LAT boresight at the time of the GBM trigger:

T0 = 21:21:00.9 UT.

The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The 100 MeV - 1 GeV photon flux in the time interval 0-600 s after the GBM trigger is (1.8 +/- 0.3)E-05 ph/cm2/s, and the photon flux above 1 GeV is (1.3 +/- 0.4)E-06 ph/cm2/s. The estimated photon index above 100 MeV is -2.2 +/- 0.15. The highest-energy photon is a 15.7 GeV event which is observed 176 seconds after the GBM trigger.


A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is Milena Crnogorevi (mcrnogor@astro.umd.edu<mailto:mcrnogor@astro.umd.edu>).

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


GRB_name: GRB220627A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32284
SUBJECT: GRB 220627A: Swift ToO observations
DATE:    22/06/28 09:37:08 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 Fermi/LAT GRB 220627A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021506

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 Fermi/LAT 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: GRB220624A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32286
SUBJECT: Konus-Wind detection of GRB 220624A
DATE:    22/06/28 12:44:56 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220624A (Fermi-GBM detection: Fermi GBM Team, GCN 32256; Lesage & Meegan, GCN Circ 32269;
AGILE detection: Ursi et al., GCN Circ 32259;
Swift/BAT-GUANO detection outside the coded FOV: Tohuvavohu et al., GCN Circ 32263;
IPN triangulation: Kozyrev et al., GCN 32265;
CALET-CGBM detection: Akaike et al., GCN Circ 32272)
triggered Konus-Wind (KW) at T0=10712.946 s UT (02:58:32.946).

The burst light curve shows three major emission episodes.
The first episode lasts from ~T0-3 s to ~T0+54 s,
the second - from ~T0-135 s to ~T0+168 s,
and the third - from ~T0-291 s to ~T0+365 s.
The total duration of the burst is ~370 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/GRB220624_T10712/

As observed by Konus-Wind, the burst had
a fluence of (3.15 Â± 0.49)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 5.760 s,
of (2.22 Â± 0.15)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+340.224 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.89 (-0.14,+0.17),
the high energy photon index beta = -2.11 (-0.28,+0.17),
the peak energy Ep = 379 (-71,+86) keV,
chi2 = 65/97 dof.

The spectrum near the peak count rate (measured from T0 to T0+14.336 s)
is best fit in the 20 keV - 15 MeV range
by a GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.51 (-0.06,+0.06),
the high energy photon index beta = -2.17 (-0.06,+0.06),
the peak energy Ep = 439 (-25,+27) keV,
chi2 = 89/97 dof.

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


GRB_name: GRB220627A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32287
SUBJECT: GRB 220627A: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/06/28 19:37:07 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 220627A onboard (T0:
2022-06-27T21:21:00 UTC, Fermi/GBM GCN 32278, INTEGRAL trig #9970, ).

The INTEGRAL and Fermi/GBM 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 90 seconds of BAT event-mode data from
[-45,+45] seconds around the time of the burst. All the requested
event mode data was delivered to the ground.

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 31 in a 16.384
s analysis time bin.

NITRATES results indicate a burst coming from outside of the coded
FoV, with DeltaLLHOut of -70. The NITRATES maximum likelihood sky
position is consistent with the Fermi GBM and LAT localization region.

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: GRB220627A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32288
SUBJECT: GRB 220627A: Fermi GBM Detection of a possible Lensed or Ultra-long GRB
DATE:    22/06/28 20:22:56 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

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

"At 21:21:00.09 UT on 27 June 2022, the Fermi Gamma-ray Burst Monitor
(GBM) triggered and located GRB 220627A (trigger 678057665/220627890)
which was also detected by the LAT (N. Di Lalla, et al. 2022, GCN 32283)
and observed by Swift-BAT-GUANO (G. Raman, et al. 2022, GCN 32287).

The Fermi GBM Final Real-time Localization (GCN 32278) is consistent
with the LAT position.

The angle from the Fermi LAT boresight is 27 degrees.

The GBM light curve shows multiple bursts over a duration (T90) of
about 138 s (10-1000 keV).

The time-averaged spectrum for the this burst from T0-5 s to T0+289 s
is best fit by a power law function with an exponential high-energy
cutoff. The power law index is -0.83 +/- 0.02 and the cutoff energy,
parameterized as Epeak, is 410 +/- 16 keV. The event fluence (10-1000 keV)
in this time interval is (7.88 +/- 0.13)E-05 erg/cm^2.

A Band function fits the spectrum equally well with Epeak= 390 +/- 20 keV,
alpha = -0.81 +/- 0.03 and beta = -2.68 +/- 0.31.

The 1-sec peak photon flux measured starting from T0+171.1 s in the
10-1000 keV band is 5.1 +/- 0.2 ph/s/cm^2.

Separately, about 1000 s later at 21:36:56.39 UT, GBM triggered on
678058621/220627901, which localized to a similar location of
RA: 207.02 deg. Dec: -28.48 deg. (J2000 degrees, equivalent to
J2000 13h 48m, +/- 28d 28'), with a statistical uncertainty of 1.2 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] ).

We find the T90 of this multiple pulsed burst of similar shape, to be
127 s (10-1000 keV). The time-averaged spectrum for the this burst
from T0-47 s to T0+122 s is best fit by a power law function with an
exponential high-energy cutoff. The power law index is -1.12 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 227 +/- 15 keV. The event
fluence (10-1000 keV) in this time interval is (2.47 +/- 0.08)E-05 erg/cm^2.

The 1-sec peak photon flux measured starting from T0+113.2 s in the
10-1000 keV band is 3.5 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB220627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32289
SUBJECT: GRB 220627A: MeerLICHT candidate optical afterglow
DATE:    22/06/28 22:59:47 GMT
FROM:    Simon de Wet at UCT  <dwtsim002@myuct.ac.za>

S. de Wet (UCT), P.J. Groot (Radboud/UCT/SAAO), D.B. Malesani (Radboud and
DAWN/NBI), A.J. Levan (Radboud) and D. Pieterse (Radboud) report on behalf
of the MeerLICHT consortium:

Following the Fermi/LAT detection and localisation of GRB 220627A (Di Lalla
et al., GCN 32283), also proposed to be a lensed or ultra-long GRB
candidate by Fermi/GBM (Roberts et al., GCN 32288), the 0.6 m wide-field
MeerLICHT optical telescope obtained 2x300s observations in the q-band of
two fields encompassing the LAT error box starting at 17:12:15 UT on 2022
June 28, approximately 1.17 days after the GBM trigger. We note that these
two fields were not observed during observations of the Fermi/GBM error box
from the previous night (Groot et al., GCN 32281). We also note that the
two transient candidates from those observations are not consistent with
the Fermi/LAT errorbox, therefore we exclude their association with GRB
220627A.

Within the error box of the uncatalogued X-ray Source 3 discovered by
Swift/XRT through ToO observations (Evans, GCN 32284), we detect a new
transient candidate at the following coordinates:

RA (J2000) = 13:25:28.49 (201.36872d)
Dec (J2000) = -32:25:33.31 (-32.42592d)

calibrated against Gaia DR2, with a positional uncertainty of 0.1" in each
coordinate. The same object is detected in a further 2x300s observations ~1
hour later. The source is detected with an AB magnitude of

q = 21.25 +/- 0.09

in the first exposure. We detect no source at the transient location in an
archival image of the same field down to a 3-sigma limiting magnitude of q
> 21.71. We suggest this may be the afterglow of GRB 220627A. Further
follow-up is encouraged.

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: GRB220627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32291
SUBJECT: GRB 220627A: VLT MUSE redshift
DATE:    22/06/29 13:06:24 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

L. Izzo (DARK/NBI), V. D'Elia (ASI/SSDC, INAF/OAR), A. de Ugarte Postigo 
(OCA), J. P. U. Fynbo (DAWN/NBI), D. A. Kann (IAA-CSIC), A. J. Levan 
(Radboud Univ.), D. B. Malesani (Radboud Univ. and DAWN/NBI), A. 
Saccardi (GEPI/Paris Obs.), C. C. Thoene (ASU-CAS), J. F. Agui Fernandez 
(IAA-CSIC), S. de Wet (UCT), P. J. Groot (Radboud Univ., UCT, SAAO), 
report on behalf of the Stargate consortium:

We observed the candidate optical afterglow (de Wet et al., GCN 32289) 
of the Fermi GBM and LAT GRB 220627A (Roberts et al., GCN 32288; Di 
Lalla et al., GCN 32283) using the ESO VLT equipped with the MUSE 
integral-field spectrograph. Observations were carried out starting on 
2022 June 29.06 UT (1.17 days after the trigger), and cover the 
wavelength range 4800-9300 AA.

A broad trough is detected centered around 4960 AA, which we interpret 
as due to DLA HI absorption. A number of metal lines are also detected, 
which we identify as, among others, O I, O I*, Si II, Si II*, C II, C 
II*, Si IV, C IV, Al II, at a common redshift z = 3.084. We also note 
the presence of a (rich) intervening system at z = 2.665 (as identified 
by, e.g., S IV, Si II, C IV, Fe II, Al II).

The redshift and luminosity of this object, together with its X-ray 
emission (Evans et al., GCN 32284), make it very likely to be the 
afterglow of GRB 220627A. Using the preliminary GBM fluence and spectral 
parameters (Roberts et al., GCN 32288), we derive an 
isotropic-equivalent quasi-bolometric gamma-ray energy of 3.6*10^54 erg 
(0.1 keV - 100 MeV rest frame).

We thank the ESO staff at Paranal for carrying out or observations, in 
particular Jonathan Smoker, Camila Navarrete, Rodrigo Palominos, and 
Marco Berton.


GRB_name: GRB220627A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32295
SUBJECT: Konus-Wind detection of GRB 220627A
DATE:    22/06/29 17:44:21 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The ultra-long (or possible lensed) GRB 220627A
(Fermi-GBM detection: Roberts et al., GCN 32288;
Fermi-LAT detection: Di Lalla et al., GCN 32283;
Swift/BAT-GUANO detection: Raman et al., GCN 32287)
was detected by Konus-Wind (KW) in the waiting mode.

A Bayesian analysis of the burst light curve (lc) reveals
two separated, multi-peaked emission episodes.
The first episode starts at ~T0-140 s and ends at ~T0+290 s;
the second, weaker episode starts at ~T0+915 s and ends at ~T0+1150 s;
where T0 = T0(GBM) = 21:21:00 UT.

Although the described structure of the burst lc is consistent with that reported by GBM (GCN 32288),
a weak emission tail that can be traced in the KW soft energy band (~20-100 keV) till ~T0+3700 s.
We note that this extended emission is visible in the same KW detector,
i.e., it came from the same (southern) ecliptic hemisphere,
however its attribution to GRB 220627A cannot be unambiguously confirmed from the KW data alone.

The KW light curve of this burst is available
at http://www.ioffe.ru/LEA/GRBs/GRB220627A/

Modeling a time-integrated spectrum of the burst (measured from T0-140 s to T0+1150 s)
by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.23 (-0.14, + 0.19) and Ep = 250 (-49,+60) keV.
In the 10 keV -10 MeV band, standard for the KW analysis,
the total burst fluence is (1.07 Â± 0.12)x10^-4 erg/cm^2
and the 2.944 s peak energy flux is (9.7 Â± 0.7)x10^-7 erg/cm^2/s.

The spectrum of the first episode alone can be described by a CPL
with alpha = -0.85 (-0.09, + 0.09) and Ep = 324 (-19,+21) keV;
and the spectrum of the second, weaker episode -  by a CPL
with alpha = -1.61 (-0.11, + 0.14) and Ep = 301 (-87,+233) keV.
 From these fits, fluences in two individual episodes
are estimated to (7.2 Â± 0.7)x10^-5 erg/cm^2 and (3.2 Â± 1.2)x10^-5 erg/cm^2, respectively.

Assuming the redshift z=3.084 (Izzo et al., GCN 32291)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the burst isotropic energy release E_iso to (2.3 Â± 0.3)x10^54 erg,
the isotropic peak luminosity L_iso on the (1+z)*64ms scale to (1.3 Â± 0.1)x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum Ep,z to 1020(-200,+250) keV.
With the obtained estimates, GRB 220627A is inside 68% prediction bands
for both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW GRBs
with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021),
see http://www.ioffe.ru/LEA/GRBs/GRB220627A/GRB220627A_rest_frame.pdf


GRB_name: GRB220627A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32296
SUBJECT: GRB 220627A: Swift-XRT afterglow detection
DATE:    22/06/30 00:29:37 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 220627A (Di Lalla et al. GCN Circ. 32283),
collecting 4.9 ks of Photon Counting (PC) mode data between T0+44.3 ks
and T0+148.8 ks. 

Fourteen uncatalogued X-ray sources are detected, of which one ("Source
3") is fading with >3-sigma significance, and is therefore likely the
GRB afterglow. Using 1679 s of PC mode data and 1 UVOT image, we find
an enhanced XRT position (using the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue): RA, Dec = 201.36878,
-32.42624 which is equivalent to:

RA (J2000): 13h 25m 28.51s
Dec(J2000): -32d 25' 34.5"

with an uncertainty of 3.1 arcsec (radius, 90% confidence). This
position is 9.6 arcmin from the Fermi/LAT position and is consistent
with the previously detected candidate afterglow (GCN Circ 32289).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.4 (+0.8, -0.5).

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021506.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021506.

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


GRB_name: GRB220627A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32302
SUBJECT: GRB 220627A: Swift/UVOT Upper Limits
DATE:    22/06/30 12:59:59 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 220627A
130224 s after the LAT trigger (Di Lalla, et al., GCN Circ. 32283).
No optical afterglow consistent with the optical position (de Wet et al., 
GCN Circ. 32289, Izzo et al., GCN Circ. 33391) or X-ray afterglow
(Gropp et al., GCN Circ. 32296) is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are:

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

u               130224       148828         4854         >22.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.047 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220624A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32303
SUBJECT: GRB 220624A: AGILE/GRID refined analysis
DATE:    22/06/30 14:30:05 GMT
FROM:    Francesco Verrecchia at SSDC,INAF-OAR  <francesco.verrecchia@ssdc.asi.it>

F. Verrecchia (SSDC, and INAF/OAR), A. Ursi (INAF/IAPS), A. Giuliani
(INAF/IASF-Mi), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata),
F. Longo (Univ. Trieste and INFN Trieste), L. Foffano (INAF/IAPS),
F. Lucarelli, C. Pittori (SSDC, and INAF/OAR), M. Romani
(INAF/OA-Brera), G. Piano, A. Argan, M. Cardillo, C. Casentini,
Y. Evangelista, E. Menegoni (INAF/IAPS), A. Bulgarelli, A. Di Piano,
V. Fioretti, 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:

he Gamma-Ray Imaging Detector (GRID) of AGILE detected gamma-ray
transient emission consistent with the long GRB 220624A reported
by Fermi/GBM (GCN #32256) at T0 = 2022-06-24 02:58:35 s (UTC),
as already reported in Verrecchia et al. GCN #32261 and also
detected by AGILE/MCAL (Ursi et al., GCN #32259).
An improved localization has been reported by the IPN (Kozyrev
et al. GCN #32265).

A refined AGILE/GRID data analysis in the energy range 30 MeV - 10
GeV shows a detection with a statistical significance of about 10
sigma over a time integration of 20 s starting at the T0 of GRB
220624A, at a sky position with Galactic coordinates l=260 deg,
b=75 deg, with and an error radius of 4 deg (90% statistical +
systematic error; R.A.= 182 deg, Decl.= 16 deg (J2000)).

The GRID error circle includes the IPN position.
During the 20s integration, we detected a total of 41 events (3
background events estimated through a Li&Ma analysis), 17 events at
energies above 100 MeV, and 3 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: GRB220627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32304
SUBJECT: GRB 220627A, GROND observations
DATE:    22/06/30 15:07:56 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

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

We observed the field of GRB 220627A (Fermi GBM team, GCN 32278) with 
GROND mounted at the 2.2m MPG telescope at La Silla Observatory (Chile).

Observations started at 01:30 UT on June 30, 2022, about 2.2 days after 
the GRB trigger and were on target for 20 minutes. They were performed at 
an average seeing of 0.8 arcsec and at an airmass of 1.1.

The reported optical transient (de Wet et al., GCN 32289; Izzo et al., GCN 
32291) is detected in the optical but not in the NIR bands with the 
following (preliminary) magnitudes and upper limits (AB mags; 3 sigma):

g' = 23.31 +/- 0.11,
r' = 22.70 +/- 0.06,
i' = 22.50 +/- 0.12,
z' = 22.23 +/- 0.21,
J  > 21.4,
H  > 20.6,
K  > 19.7.

The given limits are derived based on calibrating the optical images 
against the SM catalog and the JHK data against 2MASS stars.

We thank Regis Lachaume and Paul Eigenthaler for excellent support and for 
performing the observations.


GRB_name: GRB220701A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32306
SUBJECT: GRB 220701A: Swift detection of a burst
DATE:    22/07/01 05:12:33 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

P. A. Evans (U Leicester), S. Dichiara (PSU), H. A. Krimm (NSF),
K. L. Page (U Leicester), T. M. Parsotan (GSFC/UMBC/CRESSTII) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 04:52:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220701A (trigger=1114034).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 242.478, +55.420 which is 
   RA(J2000) = 16h 09m 55s
   Dec(J2000) = +55d 25' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 16 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:56:06.0 UT, 187.9 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 242.50589, 55.40679 which is equivalent
to:
   RA(J2000)  = 16h 10m 01.41s
   Dec(J2000) = +55d 24' 24.4"
with an uncertainty of 4.2 arcseconds (radius, 90% containment). This
location is 74 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.03
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 175 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 85% 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
0.008. 

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


GRB_name: GRB200701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32307
SUBJECT: GRB 200701A: KAIT Optical Upper Limit
DATE:    22/07/01 05:43:36 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 200701A (Evans al.,
GCN 32306) starting at 04:57:09 UT, 251 s after the burst.
Observations were performed with an automatic sequence in the
clear (roughly R), V, and I filters, and the exposure time was 20 s
per image. Our first few images were out-focused, and the first useful
focused image started at 05:07:57 UT. In the aftward focused images,
we do not detect any optical afterglow candidate within
the reported XRT position error circle (Evans et al., GCN 32306),
neither in single image, nor in the co-add images.
The typical limiting magnitude of our single clear image is about
18.5 mag calibrated to the Pan-STARRS1 catalog.


GRB_name: GRB220701A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32308
SUBJECT: GRB 220701A: Enhanced Swift-XRT position
DATE:    22/07/01 06:34:49 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 962 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220701A, 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 = 242.50501, +55.40820 which is equivalent
to:

RA (J2000): 16h 10m 1.20s
Dec (J2000): +55d 24' 29.5"

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: GRB220701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32309
SUBJECT: GRB 220701A: Lowell Discovery Telescope Optical Observations
DATE:    22/07/01 09:46:37 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

B. O'Connor (UMD, GWU), S.B. Cenko (UMD, NASA-GSFC), E. Troja (UTV),
S. Dichiara (PSU), A. Kutyrev (UMD, NASA-GSFC), S. Veilleux (UMD):

We observed GRB 220701A (Evans et al. GCN 32306) with the Large
Monolithic Imager (LMI) on the 4.3-m Lowell Discovery Telescope (LDT).
Observations began on July 1, 2022 at 08:01:14 UT in r-band (~3.1 hr
after the GRB) for a total exposure of 1000 s at airmass 1.3 and
seeing 1.2". Within the XRT enhanced position (Evans et al. GCN 32308)
we do not detect a source to depth r > 24.3 AB mag.

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

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


GRB_name: GRB220701A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32310
SUBJECT: GRB 220701A: Swift/UVOT Upper Limits
DATE:    22/07/01 11:27:13 GMT
FROM:    Samantha Oates at MSSL  <samantha.oates@alumni.ucl.ac.uk>

S. R. Oates (U. Birmingham) and P. A. Evans (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220701A
175 s after the BAT trigger (Evans et al., GCN Circ. 32306).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 32308)
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           175          325          147         >21.0
u_FC               333          583          246         >20.2
white              175         1884          424         >21.6
v                  665         1758          136         >19.2
b                  589         1858          136         >20.2
u                  333         1833          363         >20.5
w1                 714         1808          117         >19.4
w2                 640         1906           55         >18.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.008 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32311
SUBJECT: GRB 220701A: BOOTES-5/JGT early optical upper limit
DATE:    22/07/01 14:37:07 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado, I. Perez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), C. J. Perez del Pulgar and I. Carrasco (UMA), I. H. Park (SKKU) on behalf of a larger collaboration, report:

Following the detection of GRB 220701A by Swift (Evans et al. GCNC 32306), the BOOTES-5/JGT 0.6m robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) observed the GRB location starting on Jul 01, 04:55:30 UT (~152 s after trigger). In the early co-added image (20 x 10 s exposures in the clear filter), no optical afterglow is detected within the Swift/XRT error region (Evans et al. GCNC 32306, GCNC 32308) down to 20.4 mag. This non-detection is consistent with those results from KAIT (Zheng et al. GCNC 32307), LDT (O'Connor et al. GCNC 32309) and UVOT (Oates et al. GCNC 32310).

We thank the staff at Observatorio Astronomico Nacional in San Pedro Martir for their excellent support.


GRB_name: GRB220701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32313
SUBJECT: GRB 220701A: LCO Optical Upper Limits
DATE:    22/07/02 01:37:45 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration:

We observed the Swift GRB 220701A (Evans et al., GCN 32306) field with the LCO 1-m Sinistro instrument at the Teide Observatory, on Tenerife, on July 1, from 21:07 to 21:34 UT (corresponding to 16.25 to 16.70 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in r and i bands. We do not detect an optical counterpart within the XRT enhanced error region (Evans et al., GCN 32308) in either band, consistent with other non-detections (O'Connor et al., GCN 32309; Oates et al., GCN 32310; Hu et al., GCN 32311). The following upper limits are calculated using the PanSTARRS catalog as reference:

r>22.9
i>21.9

These magnitudes are not corrected for galactic extinction.

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


GRB_name: GRB220701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32314
SUBJECT: GRB 220701A: Swift-XRT refined Analysis
DATE:    22/07/02 02:45:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.2 ks of XRT data for GRB 220701A (Evans et al. GCN
Circ. 32306), from 178 s to 52.7 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN Circ. 32308).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.03 (+0.15, -0.12).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.7, -0.6). The
best-fitting absorption column is  1.2 (+0.7, -0.5) x 10^22 cm^-2, in
excess of the Galactic value of 1.0 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.4 x 10^-11 (1.1 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.2 (+0.7, -0.5) x 10^22 cm^-2
Galactic foreground: 1.0 x 10^20 cm^-2
Excess significance: 4.0 sigma
Photon index:      2.3 (+0.7, -0.6)

If the light curve continues to decay with a power-law decay index of
1.03, the count rate at T+24 hours will be 5.6 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.4 x
10^-14 (6.3 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/01114034.

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


GRB_name: GRB220701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32315
SUBJECT: GRB 220701A: Keck/LRIS Optical Upper Limit
DATE:    22/07/02 10:47:23 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

WeiKang Zheng, Yi Yang, Thomas G. Brink and Alexei V. Filippenko
(UC Berkeley) report on behalf of the KAIT GRB team:

We observed the field of GRB 200701A (Evans al., GCN 32306) with the
Low Resolution Imaging Spectrometer (LRIS) mounted on the 10-m Keck I
telescope, started at 10:41 UT on July 1st (5.82 hours after the burst).
We obtained 5x180s exposure in g and RG850 (close to z) filter
simultaneously,
under the averaged seeing ~1.2". We do not detect any optical afterglow
candidate within the enhanced XRT position error circle (Evans al., GCN
32308)
with the following upper limit, calibrated to the Pan-STARRS1 catalog in
g and z filter:

g > 24.5
z > 22.8

Our result is consistent with other non-detections (Zheng et al. GCNC 32307;
O'Connor et al., GCN 32309; Oates et al., GCN 32310; Hu et al., GCN 32311,
Strausbaugh et al., GCN 32313).


GRB_name: GRB220627A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32316
SUBJECT: GRB 220627A: AstroSat CZTI detection
DATE:    22/07/02 11:42:11 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

A. Suresh (IITB), G. Waratkar (IITB), R. Gopalakrishnan (IUCAA), 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 the long (or possibly 
lensed) GRB 220627A which was also detected by Fermi GBM (Fermi GBM 
team, GCN 32278; Roberts et al., GCN 32288), Fermi-LAT (Lalla et al., 
GCN 32283), Swift-BAT-GUANO (Raman et al., GCN 32287), Konus-Wind 
(Frederiks et al., GCN 32295), and Swift-XRT (Gropp et al. GCN 32302).

AstroSat CZTI was in the South Atlantic Anomaly (SAA) region during the 
first burst episode. About 1000s after the first burst, CZTI detected 
the second burst episode that was also reported by Fermi-GBM (GCN 
32288), and Konus-Wind (GCN 32295). This burst was clearly detected in 
the 20-200 keV energy range. The light curve peaks at 2022-06-27 
21:38:49.500 UTC. The measured peak count rate associated with the burst 
is 233 (+43, -41) counts/s above the background in the combined data of 
all four quadrants, with a total of 2707 (+454, -447) counts. The local 
mean background count rate was 500 (+3, -4) counts/s. Using cumulative 
rates, we measure a T90 of 43 (+2, -12) 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: GRB220701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32317
SUBJECT: GRB 220701A: AbAO optical upper limit
DATE:    22/07/02 14:30:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 220701A detected by Swift (Evans et al., 
GCN 32306;) with AS-32 telescope of Abastumani Observatory (AbAO) 
starting on 2022-07-01 (UT) 17:54:12. We do not detect any optical 
sources within enhanced XRT position (Evans et al., GCN 32308). This 
upper limit is consistent with earlier and later non detection 
(O'Connor  et al. GCN 32309; Oates  et al. GCN 32310; Hu et al. GCN 
32311; Strausbaugh et al. GCN 32313; Zheng et al. GCN 32315). 
Preliminary upper limit of a stacked image is following:

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

2022-07-01 17:54:12  0.55016  22*60  R      n/d    n/d    21.0

The photometry is based on nearby USNO-B1.0 stars, R2 magnitude
RA DEC R2
16:10:21.85344 +55:26:18.9924 15.49
16:10:42.83688 +55:25:01.9920 17.38
16:10:59.99544 +55:21:15.1020 16.08
16:10:33.30600 +55:17:14.3520 16.76


GRB_name: GRB220701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32318
SUBJECT: GRB 220701A: COATLI Optical Upper Limit
DATE:    22/07/02 17:50:14 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

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

We observed the field of GRB 220701A (Evans et al., GCN Circ. 32306) with the
COATLI 50-cm telescope and interim imager at the Observatorio AstronÃ³mico
Nacional on the Sierra de San Pedro MÃ¡rtir (http://coatli.astroscu.unam.mx) from
2022-07-02 03:45 UTC to 11:21 UTC (22.81 to 30.41 hours after the trigger),
obtaining a total of 21405 seconds of exposure in the r filter.

We do not detect any uncataloged sources in the XRT error region (Evans et al.,
GCN Circ. 32306) to a 3-sigma limit of r = 23.7.

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

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


GRB_name: GRB220701A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32320
SUBJECT: GRB 220701A: MITSuME Akeno optical upper limits
DATE:    22/07/04 06:38:32 GMT
FROM:    Yutaka Takamatsu at Tokyotech  <takamatsu@hp.phys.titech.ac.jp>

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

We observed the field of GRB 220701A (P. A. Evans et al. GCN Circular
#32306 & #32308, B. O'Connor et al. GCN Circular #32309, S. R. Oates
et al. GCN Circular #32310, Y.-D. Hu et al. GCN Circular #32311, R.
Strausbaugh et al. GCN Circular #32313, J. D. Gropp et al. GCN
Circular #32314, WeiKang Zheng et al. GCN Circular #32315, S. Belkin
et al. GCN Circular #32317, Alan M. Watson et al. GCN Circular #32318)
with the optical three color (g', Rc, and Ic) CCD cameras attached to
the MITSuME 50 cm telescope Akeno.

The observation with a series of 60 sec exposures started at
2022-07-01 19:37:09 UT (884 minutes after the Swift/BAT trigger). We
stacked the images with good conditions. We did not detect any
uncatalogued sources within the enhanced Swift/BAT error region (Evans
et al. GCN Circular #32306). We obtained the 5-sigma limits of the
stacked images as follows.

T0+[days] | MID-UT | T-EXP[sec] | 5-sigma limits
------------------------------------------------------------------------------------------------
0.6 | 2022-07-01 14:31:19 | 9060 | g'>19.4, Rc>20.1, Ic>20.9
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time

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


GRB_name: GRB220705A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32322
SUBJECT: GRB 220705A: Fermi GBM Final Localization
DATE:    22/07/05 14:42:48 GMT
FROM:    Joe Mangan at UCD  <joseph.mangan@ucdconnect.ie>

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

At 06:45:53.34 UT on 5 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220705A (trigger 678696358 / 220705282).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 149.8, Dec = -10.7 (J2000 degrees, equivalent to J2000 9h 59m, -10d 43'),
with a statistical uncertainty of 11.2 degrees.

The angle from the Fermi LAT boresight is 46 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220705282/quicklook/glg_skymap_all_bn220705282.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/bn220705282/quicklook/glg_healpix_all_bn220705282.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220705282/quicklook/glg_lc_medres34_bn220705282.gif


GRB_name: GRB220702A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32323
SUBJECT: GRB 220702A: Fermi GBM Final Localization
DATE:    22/07/05 16:48:18 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

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

At 13:39:35.74 UT on 2 July 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220702A (trigger 678461980 / 220702569).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 160.0, Dec = 6.5 (J2000 degrees, equivalent to J2000 10h 40m, 6d 30'),
with a statistical uncertainty of 11.5 degrees.

The angle from the Fermi LAT boresight is 75 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220705282/quicklook/glg_skymap_all_bn220702569.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/bn220705282/quicklook/glg_healpix_all_bn220702569.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220705282/quicklook/glg_lc_medres34_bn220702569.gif


GRB_name: GRB220702B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32324
SUBJECT: GRB 220702B: Fermi GBM Final Localization
DATE:    22/07/05 16:53:14 GMT
FROM:    Oliver J Roberts at USRA/NASA  <oliver.roberts@nasa.gov>

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

At 20:12:46.60 UT on 2 July 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220702B (trigger 678485571 / 220702842).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 170.7, Dec = 46.8 (J2000 degrees, equivalent to J2000 11h 22m, 46d 48'),
with a statistical uncertainty of 5.5 degrees.

The angle from the Fermi LAT boresight is 65 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220705282/quicklook/glg_skymap_all_bn220702842.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/bn220705282/quicklook/glg_healpix_all_bn220702842.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220705282/quicklook/glg_lc_medres34_bn220702842.gif


GRB_name: GRB220701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32325
SUBJECT: GRB220701A: VIRT Optical Upper Limit
DATE:    22/07/05 17:51:12 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

P. Gokuldass (Florida Institute of Technology), N. Orange (OrangeWave
Innovative Science, LLC), K. Noonan (UVI), R. Querrard (UVI), K. Smith
(UVI), D. Morris (UVI) report:

We observed the field of GRB220701A (Evans et al., GCN 32306) with the 0.5m
Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 07-01-2022 starting at 05:16:18.64 UT (T+24
min). We performed a series of exposures in the R filter with a total
exposure of 3300 s. The weather conditions were partly cloudy during the
hours of observation with an average airmass of 2.

We detect no new source within the enhanced XRT position error circle
(Evans et al., 32308), consistent with other non-detections (Zheng et al.
GCN 32307;  O'Connor  et al. GCN 32309; Oates  et al. GCN 32310; Hu et al.
GCN 32311; Strausbaugh et al. GCN 32313; Belkin et al. GCN 32317) and
report the following 5-sigma upper limit:


T_mid            ||Exposure     ||Filter      ||Limit

T+ 1.5 hrs      ||3300s         ||R          ||>19.8


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 80NSSC19M0060, and NSF EiR award 1901296.This message can be
cited.


GRB_name: GRB220412A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32326
SUBJECT: GRB220412A: VIRT Optical Upper Limit
DATE:    22/07/05 17:53:31 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

K. Noonan (UVI), P. Gokuldass (Florida Institute of Technology), N. Orange
(OrangeWave Innovative Science, LLC), K. Smith (UVI), D. Morris (UVI)
report:

We observed the field of GRB220412A (N. J. Klingler et al., GCN 31881) with
the 0.5m Virgin Island Robotic Telescope (VIRT) at the University of the
Virgin Islands' Etelman Observatory on 04-13-2022 starting at 00:11:58.73
UT (T+17.30 hrs). We performed a series of exposures in the R filter with a
total exposure of 4000 s. The weather conditions were partly cloudy during
the hours of observation with an average airmass of 1.25.

We find no new source within the enhanced XRT position error circle (P. A.
Evans et al., 31887) and report the following 5-sigma upper limit:

T_mid            ||Exposure     ||Filter      ||Limit

T+ 18.2 hrs    ||4000s          ||R            ||>20.8

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 80NSSC19M0060, and NSF EiR award 1901296.This message can be
cited.


GRB_name: GRB220408A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32327
SUBJECT: GRB220408A: VIRT Optical Upper Limit
DATE:    22/07/05 17:55:28 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

K. Noonan (UVI), P. Gokuldass (Florida Institute of Technology), N. Orange
(OrangeWave Innovative Science, LLC), K. Smith (UVI), D. Morris (UVI)
report:

We observed the field of GRB220408A (Caputo et al., GCN 31848) with the
0.5m Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 04-08-2022 starting at 23:53:07.963 UT
(T+18.7 hrs). We performed a series of exposures in the R filter with a
total exposure of 6180 s. The weather conditions were partly cloudy during
the hours of observation with an average airmass of 1.5.

We detect no new source within the enhanced XRT position error circle (A.P.
Beardmore et al., 31852), consistent with other non-detections  ( Zheng &
Filippenko, GCN 31850; Jiang et al., GCN 31853; Kumar et al., GCN 31857;
and Gregory et al., GCN 31867)  and report the following 5-sigma upper
limit:

T_mid            ||Exposure     ||Filter      ||Limit

T+ 19.5 hrs    ||6180s          ||R            ||>20.8

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 80NSSC19M0060, and NSF EiR award 1901296.This message can be
cited.


GRB_name: GRB220701A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32328
SUBJECT: GRB 220701A: Swift-BAT refined analysis
DATE:    22/07/06 13:57:34 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),  P. A. Evans (U Leicester),
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 220701A (trigger #1114034)
(Evans, et al., GCN Circ. 32306).  The BAT ground-calculated position is
RA, Dec = 242.474, 55.436 deg which is
   RA(J2000)  =  16h 09m 53.7s
   Dec(J2000) = +55d 26' 08.9"
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 56%.

The BAT mask-weighted light curve shows a fairly weak peak extending from
Roughly T-2 to T+8 seconds. T90 (15-350 keV) is 5.77 +- 1.13 sec (estimated
error including systematics).

The time-averaged spectrum from T-1.40 to T+4.83 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.37 +- 0.34.  The fluence in the 15-150 keV band is 1.8 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.65 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/1114034/BA/


GRB_name: GRB220706A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32329
SUBJECT: GRB 220706A: Swift detection of a burst
DATE:    22/07/06 16:27:19 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@inaf.it>

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

At 16:09:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220706A (trigger=1114937).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 0.587, -16.391 which is 
   RA(J2000) = 00h 02m 21s
   Dec(J2000) = -16d 23' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex structure
 with a duration of about 50 sec.  The peak count rate
was ~1400 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 16:10:57.0 UT, 102.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 0.60368, -16.41065 which is equivalent
to:
   RA(J2000)  = 00h 02m 24.88s
   Dec(J2000) = -16d 24' 38.3"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 91 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 (2.40 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 6.6
(+4.12/-3.33) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 107 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
0.025. 

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


GRB_name: GRB220706A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32330
SUBJECT: GRB 220706A: Prompt enhanced Swift-XRT position
DATE:    22/07/06 16:57:59 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 220706A, we find an
enhanced XRT position of the afterglow: RA, Dec: 0.60455, -16.41107
which is equivalent to:
   RA (J2000)  = 00 02 25.09
   Dec (J2000) = -16 24 39.9
with an uncertainty of 1.9 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/1114937.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB220706A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32331
SUBJECT: GRB 220706A: Zadko observatory - Gingin optical observations
DATE:    22/07/06 17:57:05 GMT
FROM:    Bruce Gendre at UVI  <bruce.gendre@gmail.com>

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

We imaged the field of GRB 220706A detected by SWIFT
(trigger 1114937, D'Ai et al. GCN 32329) with the Zadko
robotic telescope (D=100cm) located at the observatory -
Gingin, Australia.

The observations started 157.6s after the GRB trigger
(123.9s after the notice). The elevation of the field
increased from 18 degrees above horizon and weather
conditions were good.
At the position of the X-ray afterglow reported by
Evans et al. (GCN 32330), we do not detect any source
using a clear filter.
t0+157.6s to t0+167.6s : R > 14.5

We co-added a series of long exposures:
t0+1414s to t0+1962s : R > 17.0

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

N.B. Galactic coordinates are lon= 73.7767 lat=-74.3612

This message may be cited.


GRB_name: GRB220706A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32332
SUBJECT: Swift GRB 220706A: Global MASTER-Net observations report 
DATE:    22/07/06 22:45:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev
(Irkutsk State University, API),

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

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 220706A ( A. D'Ai et al., GCN 32329) errorbox  22935 sec after notice time and 22975 sec after trigger time at 2022-07-06 22:32:09 UT, with upper limit up to  18.2 mag. The observations began at zenith distance = 71 deg. The sun  altitude  is -80.3 deg. 

The galactic latitude b = -75 deg., longitude l = 76 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2023835

We obtain a following upper limits.  

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

   23065 |         MASTER-SAAO |   C |   180 | 18.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220706A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32333
SUBJECT: GRB 220706A: Enhanced Swift-XRT position
DATE:    22/07/06 23:58:49 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 822 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220706A, 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 = 0.60427, -16.41121 which is equivalent
to:

RA (J2000): 00h 02m 25.03s
Dec (J2000): -16d 24' 40.4"

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: GRB220706A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32335
SUBJECT: GRB 220706A: Nanshan/NEXT optical upper limits
DATE:    22/07/07 02:45:18 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 220706A detected by Swift (D'Ai et al., GCN 
32329) using the NEXT-0.6m telescope located at Nanshan, Xinjiang, 
China. We obtained 7x200 s frames in the Sloan r-band and 5x200 s frames 
in the Sloan z-band, starting at 20:21:09 UT on 2022-07-06, i.e., 4.2 hr 
after the BAT trigger.

No optical source is detected in our stacked images at the enhanced XRT 
position (Goad et al., GCN 32333), with upper limits as follows:

T_mid-T0 (hr)    Filter   Upper limit(3-sigma)
    4.41                 r          >20.7
    4.79                 z          >18.8

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


GRB_name: GRB220702B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32336
SUBJECT: GRB 220702B: AstroSat CZTI detection
DATE:    22/07/07 03:05:30 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

A. Suresh (IITB), 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 220702B which was 
also detected by Fermi-GBM (Fermi GBM Team, GCN 32324).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-07-02 20:12:46.500 UTC. The measured peak 
count rate associated with the burst is 117 (+47 -12) counts/s above the 
background in the combined data of all four quadrants, with a total of 
988 (+222 -248) counts. The local mean background count rate was 474 (+4 
-5) counts/s. Using cumulative rates, we measure a T90 of 16 (+1 -4) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve showed multiple peaks 
of emission with the strongest peak at 2022-07-02 20:12:47.671 UTC. The 
measured peak count rate is 208 (+67 -40) counts/s above the background 
in the combined Veto data of all quadrants, with a total of 1533 (+352 
-382) counts. The local mean background count rate was 1405 (+5 -6) 
counts/s. We measure a T90 of 18 (+1 -5) s from the cumulative Veto 
light curve.

CZTI GRB detections are reported regularly on the payload site at 
http://astrosat.iucaa.in/czti/?q=grb. 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: GRB220706A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32337
SUBJECT: GRB 220706A: MAXI/GSC detection 84 minutes after the Swift Trigger
DATE:    22/07/07 05:18:45 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

M. Serino, T. Sakamoto (AGU), W. Iwakiri (Chuo U.),  H. Negoro (Nihon U.), Y. Kawakubo (LSU),
N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), 
M. Nakajima, K. Kobayashi, M. Tanaka, Y. Soejima (Nihon U.), 
T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, M. Matsuoka (RIKEN), 
S. Sugita, H. Hiramatsu, A. Yoshida (AGU), 
Y. Tsuboi, J. Kohara (Chuo U.), 
M. Shidatsu, M. Iwasaki (Ehime U.),
S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka, T. Kurihara (JAXA), 
Y. Ueda, S. Ogawa, K. Setoguchi, T. Yoshitake, K. Inaba (Kyoto U.), 
H. Tsunemi (Osaka U.), 
M. Yamauchi, T. Sato, R. Hatsuda, R. Fukuoka, Y. hagiwara, Y. Umeki (Miyazaki U.), 
K. Yamaoka (Nagoya U.),
M. Sugizaki (NAOC)

report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray 
transient source at 17:33:25 UT on 2022 July 6 at
(R.A., Dec) = (0.219 deg, -16.471 deg) (J2000)
This position was consistent with GRB 220607A (GCN #32329) and the scan transit
was 5051 sec after the BAT trigger time (T0).
The scan was not completed because the GSC HV turned off due to the high 
latitude constraint. The preliminary observed flux was about 200 mCrab in 
the 2 - 10 keV band.
The transient was also observed at the next scan transit (17:53, T0+6260s) and 
the flux decayed to about 60 mCrab in the same energy band.
We note that Swift/XRT also detected bright X-ray flare around T0+5400s.
There was no significant excess flux in the previous transit at 16:00 UT
and in the third transit at 19:26 UT with an upper limit of 20 mCrab for each.
Since the X-ray flaring activity of this GRB was unusual, we encourage 
multi-wavelength observations.


GRB_name: GRB220706A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32338
SUBJECT: GRB 220706A: Optical observations from NOT
DATE:    22/07/07 07:06:31 GMT
FROM:    Antonio de Ugarte Postigo at OCA  <deugarte@oca.eu>

A. de Ugarte Postigo, (OCA), D.B. Malesani (Radboud Univ. and DAWN/NBI),
and A. Kasikov (NOT, Aarhus Univ, Univ. of Tartu) report on behalf of a larger
collaboration,

We observed the field of GRB 220706A (Dâ€™Ai et al. GCN 32329) with AlFOSC 
on the 2.5m NOT telescope at Roque de los Muchachos Observatory (La 
Palma, Spain). The observation started at 04:33 UT (11.68 hrs after the burst) 
and consisted on 3x300s imaging in r-band and 5x200s in z-band.

No new object is detected within the refined XRT error box (Evans et al. GCN 
32330) in neither of the bands. The 3-signa detection limit in the r-band is 
24.5 mag and 23.6 in z-band, calibrated with respect to Pan-STARRS field 
stars. Our non detection is consistent with previous reports (Gendre et al. 
GCN 32331, Lipunov et al. GCN 32332, Jiang et al. GCN 32335).

We do note that there is a faint source at the Northern edge of the error box, 
at a distance of ~2.9â€œ from the centre of the XRT position, which is also 
marginally detected in the Pan-STARRS images, and for which we measure 
a magnitude of 24.1+/-0.3, with coordinates (J2000):

R.A.: 00:02:25.01
Dec.: -16:24:37.0


GRB_name: GRB220706A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32339
SUBJECT: GRB 220706A, GROND observations
DATE:    22/07/07 13:17:52 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

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

We observed the field of GRB 220706A (DAi et al., GCN 32329) with
GROND mounted at the 2.2m MPG telescope at La Silla Observatory
(Chile).

Observations started at a midtime of 09:40 UT on July 07, 2022, about
17.5 hours after the GRB trigger and were on target for 20 minutes.
They were performed at an average seeing of 1.2 arcsec and at an
airmass close to 1.0.

Inside the enhanced Swift/XRT error circle (Goad et al., GCN 32333),
we do not detect an optical/NIR transient in any band down to the
following upper limits (AB mags; 3 sigma):

g' > 25.2,
r' > 24.9,
i' > 24.2,
J  > 21.7,
H  > 21.0,
K  > 19.9.

Combining the GROND optical (g'r'i') and NIR (JHK) bands, no object is
detected inside the enhanced XRT error circle either.

Our measurements add to previousely reported results (Gendre et al.,
GCN 32331; Lipunov et al., GCN 32332; Jiang et al., GCN 32335; de
Ugarte-Postigo et al., GCN 32338).

The source at the northern border of the enhanced XRT error circle
reported by de Ugarte Postigo et al. (GCN 32338) is clearly detected
in our combined gri images. At present we cannot decide whether this
is a galaxy or not.

The given limits are derived based on calibrating the optical images
against the Pan-STARRS catalog and the JHK data against 2MASS stars.
We thank Sam Kim for excellent support and for performing the
observations.


GRB_name: GRB220706A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32340
SUBJECT: GRB 220706A: Swift-XRT refined Analysis
DATE:    22/07/07 13:36:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.6 ks of XRT data for GRB 220706A (D'Ai et al. GCN
Circ. 32329), from 87 s to 67.9 ks after the  BAT trigger. The data
comprise 578 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 Goad et al.
(GCN Circ. 32330).

The late-time light curve (from T0+4.4 ks) can be modelled with a
power-law decay with a decay index of alpha=1.3 (+/-0.4).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.33 (+0.15, -0.14). The
best-fitting absorption column is  6.0 (+/-0.8) x 10^21 cm^-2, in
excess of the Galactic value of 2.4 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (7.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.0 (+/-0.8) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 12.4 sigma
Photon index:      2.33 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
1.3, the count rate at T+24 hours will be 0.016 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.6 x
10^-13 (1.2 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/01114937.

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


GRB_name: GRB220627A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32341
SUBJECT: GRB 220627A: ATCA detection of radio counterpart
DATE:    22/07/07 14:26:05 GMT
FROM:    James Leung at U of Sydney/VAST  <jleu9465@uni.sydney.edu.au>

James Leung (U. Sydney, CSIRO), Ziteng Wang (U. Sydney, CSIRO), Tao
An (SHAO), Adam Deller (Swinburne), Giancarlo Ghirlanda (INAF/Brera),
Stefano Giarratana (U. Bologna, INAF/IRA), Marcello Giroletti
(INAF/IRA), David L. Kaplan (UWM), Emil Lenc (CSIRO), Tara Murphy
(U. Sydney), Lauren Rhodes (U. Oxford), Om Sharan Salafia
(U. Milano-Bicocca, INAF/Brera), Cristiana Spingola (INAF/IRA)

The Australia Telescope Compact Array (ATCA) observed GRB 220627A
(Fermi GBM team, GCN Circ. 32278) at multiple frequencies starting at
04:00 UT on 2022 July 5 (7.3 days post-burst). We detected a radio
source with a preliminary flux density of ~0.4 mJy at a central
frequency of 17 GHz at

RA = 13:25:28.48
Dec = -32:25:32.14
              
with positional uncertainty of ~1.5 arcsec. The position of the radio
source is consistent with the candidate optical (de Wet et al., GCN
Circ. 32289) and X-ray afterglow (Gropp et al., GCN Circ. 32296)
positions. 

Further observations with several facilities at different frequencies
are ongoing.

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


GRB_name: GRB220706A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32342
SUBJECT: GRB 220706A: LCO Optical Upper Limits
DATE:    22/07/08 01:42:44 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration:

We observed the Swift GRB 220706A (D'Ai et al., GCN 32329) field with the Siding Spring Observatory, Australia site, on July 6, from 18:15 to 18:52 (corresponding to 2.10 to 2.72 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in i and 2x300 and 1x135 r bands (the last r-band observation was interrupted).  We do not detect an optical counterpart within the XRT enhanced error region (Goad et al., GCN 32333) in either band, consistent with other non-detections (Gendre et al., GCN 32331; Lipunov et al., GCN 32332; Jiang et al., GCN 32335; de Ugarte-Postigo et al., GCN 32338; Guelbenzu et al., GCN 32339).

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

r>23.0
i>22.5

We also observed with the LCO 1-m Sinistro instrument at the Teide Observatory, on Tenerife, on July 7, from 04:25 to 04:52 UT (corresponding to 12.27 to 12.72 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in i and r bands.

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

r>22.4
i>22.4

These magnitudes are not corrected for galactic extinction.

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


GRB_name: GRB220708A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32343
SUBJECT: GRB 220708A: Swift detection of a burst
DATE:    22/07/08 04:54:20 GMT
FROM:    Valerio D'Elia at ASDC  <valerio.delia@ssdc.asi.it>

V. D'Elia (SSDC & INAF-OAR), A. D'Ai (INAF-IASFPA), T. Sakamoto (AGU)
and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 04:39:29 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220708A (trigger=1115156).  Swift did not slew immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 103.118, +72.191 which is 
   RA(J2000) = 06h 52m 28s
   Dec(J2000) = +72d 11' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed several peaks 
with a duration of about 40 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~2 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+36.8
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is V. D'Elia (valerio.delia AT ssdc.asi.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: GRB220708A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32344
SUBJECT: GRB 220708A: Swift-XRT observations
DATE:    22/07/08 06:02:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 220708A at 05:20:39.0 UT,
2469.3 seconds after the BAT trigger. No source was detected in 767 s
of promptly downlinked data, which covered 94% of the BAT error circle.
We are waiting for the full dataset to detect and localise the XRT
counterpart.


GRB_name: GRB220708B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32345
SUBJECT: GRB 220708B: Swift/BAT-GUANO arcminute localization
DATE:    22/07/08 10:11:30 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 220708B onboard (T0:
2022-07-08T02:06:67 UTC, CALET trig #1341281218).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst in a 4.096 s analysis time bin
with a sqrt(TS) of 41.4.
The duration of the burst as seen by BAT is ~7 seconds.

A confident arcminute localization is found with DeltaLLHOut of 150
and a DeltaLLHPeak of 68.

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

The BAT position is
RA, Dec = 248.652, 36.338 deg which is
   RA(J2000)  = 16h 34m 36.48s
   Dec(J2000) = +36d 20â€² 16.8â€³
with an estimated uncertainty of 5 arcmin.

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

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

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


GRB_name: GRB220708B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32346
SUBJECT: GRB 220708B: Swift ToO observations
DATE:    22/07/08 11:50:47 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 220708B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021508

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: GRB220708A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32347
SUBJECT: GRB 220708A: Enhanced Swift-XRT position
DATE:    22/07/08 13:27:53 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 1178 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 220708A, 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 = 103.12570, +72.14111 which is equivalent
to:

RA (J2000): 06h 52m 30.17s
Dec (J2000): +72d 08' 28.0"

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: GRB220706A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32348
SUBJECT: GRB 220706A: Swift-BAT refined analysis
DATE:    22/07/08 14:07:29 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU),
(i.e. the Swift-BAT team):
  
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 220706A (trigger #1114937)
(D'Ai, et al., GCN Circ. 32329).  The BAT ground-calculated position is
RA, Dec = 0.577, -16.411 deg which is
    RA(J2000)  =  00h 02m 18.5s
    Dec(J2000) = -16d 24' 38.8"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
  
The BAT mask-weighted light curve shows a bright peak starting from
T-3 s to T+30 s.  The weak emission is evident in the 10-s binned
light curve starting from T-80 s to T+70 s.  T90 (15-350 keV) is
86.9 +- 18.0 sec (estimated error including systematics).
  
The time-averaged spectrum from T-71.84 to T+36.15 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.75 +- 0.17.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+3.72 sec in the 15-150 keV band
is 0.9 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.
  
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1114937/BA/


GRB_name: GRB220708A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32349
SUBJECT: GRB 220708A: BOOTES-5/JGT early optical upper limit
DATE:    22/07/08 14:25:49 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado, I. Perez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM), C. J. Perez del Pulgar and I. Carrasco (UMA), I. H. Park (SKKU) on behalf of a larger collaboration, report:

Following the detection of GRB 220708A by Swift (D'Elia et al. GCNC 32343), the BOOTES-5/JGT 0.6m robotic telescope at Observatorio Astronomico Nacional in San Pedro Martir (Mexico) observed the GRB location starting on Jul 08, 04:40:14 UT (~ 45 s after trigger). In the early co-added image (30 x 10 s exposures in the clear filter), no optical afterglow is detected within the enhanced Swift/XRT error region (Osborne et al. GCNC 32347) down to 20.5 mag.

We thank the staff at Observatorio Astronomico Nacional in San Pedro Martir for their excellent support.


GRB_name: GRB220708B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32350
SUBJECT: GRB 220708B: Swift-XRT afterglow detection
DATE:    22/07/08 14:27:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 220708B, collecting 1.7 ks of Photon
Counting (PC) mode data between T0+35.1 ks and T0+36.8 ks. 

An uncatalogued X-ray source is detected and is above the RASS 3-sigma
upper limit at this position, and is therefore likely the GRB
afterglow.  The position of this source is RA, Dec=248.5790, +36.3478
which is equivalent to:

RA (J2000): 16:34:18.97
Dec(J2000): +36:20:52.0

with an uncertainty of 4.0 arcsec (radius, 90% confidence).  This
position is 3.6 arcmin from the Swift/BAT-GUANO position.  The light
curve is consistent with a constant source of mean count rate 6.5e-02
ct/sec. A power-law fit gives an index of 0.0 (+0.0, -3.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.3 (+0.6, -0.5). The
best-fitting absorption column is  3.2 (+2.2, -1.7) x 10^21 cm^-2, in
excess of the Galactic value of 1.4 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.2 x 10^-11 (5.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+2.2, -1.7) x 10^21 cm^-2
Galactic foreground: 1.4 x 10^20 cm^-2
Excess significance: 2.9 sigma
Photon index:      2.3 (+0.6, -0.5)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021508.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021508.

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


GRB_name: GRB220706A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32351
SUBJECT: GRB 220706A: Swift/UVOT Upper Limits
DATE:    22/07/08 20:06:11 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

 GRB 220706A: Swift/UVOT Upper Limits

S. J. LaPorte (PSU) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220706A
107 s after the BAT trigger (D'Ai et al., GCN Circ. 32329).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 32333)
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           107          257          147         >20.5
u_FC               320          570          246         >20.0
white              107         1025          334         >20.5
b                  751          771           19         >18.5
u                  320          570          246         >20.0
w1                 701          720           19         >17.8
m2                 849          869           19         >18.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.025 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220708A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32352
SUBJECT: GRB 220708A: Swift-XRT refined Analysis
DATE:    22/07/08 20:22:18 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.3 ks of XRT data for GRB 220708A (D'Elia et al. GCN
Circ. 32343), from 2.5 ks to 49.4 ks after the BAT trigger. The data
comprise 257 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN Circ. 32347).

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

If the light curve continues to decay with a power-law decay index of
1.1, the count rate at T+24 hours will be 8.8 x 10^-4 count s^-1

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01115156.

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


GRB_name: GRB220706A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32353
SUBJECT: GRB 220706A : NICER detection of re-brightening 1 day after the Swift trigger
DATE:    22/07/09 00:07:58 GMT
FROM:    Motoko Serino at Aoyama Gakuin U.  <serino@phys.aoyama.ac.jp>

W. Iwakiri (Chuo U.), M. Shidatsu (Ehime.U), M. Serino (AGU), K. C. Gendreau, Z. Arzoumanian (NASA/GSFC), 
T. Enoto, T. Mihara (RIKEN)

We report on initial NICER observations of GRB 220706A (GCN #32329) carried out on 2022 July 7. 
The observations were carried out in two parts. The first epoch began at 01:36 UT, approximately a half-day 
after the Swift/BAT trigger (GCN #32329), and ended at 03:34 UT, with ~1.5 ksec of exposure across two 
successive orbits of the International Space Station (ISS). The lightcurve shows a slow decay: 
the NICER-measured X-ray flux decreased from 8 x 10-13 to 6 x 10-13 erg/cm2/s in the 0.3-10 keV band. 
The emission overall was soft, with hardness ratio of 0.1 between the 0.3-2.0 and 2.0-10.0 keV bands. 
The second epoch was from 17:08 to 22:09 UT (~1 day after the Swift/BAT detection), with 3.4 ksec exposure 
in total. We found re-brightening of the afterglow: the NICER average flux during the second epoch 
was 6.5 x 10-12 erg/cm2/s in 0.3-10 keV, with a hardness ratio of 0.6. The result suggests that the spectrum 
has significantly hardened compared with the first-epoch results, unlike typical GRBs. 

NICER will continue to monitor this source. Multi-wavelength followup observations are strongly encouraged.

Note: Because the nature of the source is unknown, this message is cross-posted to ATel and GCN.


GRB_name: GRB220708A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32354
SUBJECT: GRB 220708A: Swift/UVOT Upper Limits
DATE:    22/07/09 03:01:38 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

A. Belles (PSU) and V. D'Elia (SSDC & INAF-OAR)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220708A
2473 s after the BAT trigger (D'Elia et al., GCN Circ. 32343).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 32347)
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          2473         2622          147         >19.8
white             2473         8325          402         >20.2
v                 2934         3134          197         >18.9
b                 2680         3954          216         >20.1
u                 2655         3749          216         >19.9
w1                2630         3544          216         >19.3
m2                3139         3339          197         >19.3
w2                2730         2930          197         >19.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.169 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220708B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32355
SUBJECT: GRB 220708B: Nanshan/NEXT optical upper limits
DATE:    22/07/09 03:18:20 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 220708B detected by Swift/BAT-GUANO 
(Tohuvavohu et al., GCN 32345) using the NEXT-0.6m telescope located at 
Nanshan, Xinjiang, China. We obtained 10x200 s frames in the Sloan 
r-band and 9x200 s frames in Sloan z-band, starting at 19:15:57.859 UT 
on 2022-07-08,i.e.,17.15 hr after the BAT trigger.

No optical source is detected in our stacked images at the  XRT 
afterglow position (Osborne et al., GCN 32350), with upper limits as 
follows:

T_mid-T0 (hr)    Filter   Upper limit(3-sigma)
    17.42               r         >21.60
    17.96               z         >19.54

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


GRB_name: GRB220708B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32356
SUBJECT: GRB 220708B: CALET Gamma-Ray Burst Monitor detection
DATE:    22/07/09 04:25:21 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

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

The long GRB 220708B (Swift/BAT-GUANO arcminute localization: 
Tohuvavohu et al., GCN Circ. 32345) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 02:06:55.120 UTC on 8 July 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1341281218/index.html).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a single pulse which starts
at T+2.6 sec, peaks at T+4.8 sec, and ends at T+6.5 sec.
The T90 and T50 durations measured by the SGM data are 3.4 +/- 0.3 sec
and 1.4 +/- 0.2 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1341281218/

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


GRB_name: GRB220708B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32358
SUBJECT: Konus-Wind detection of GRB 220708B
DATE:    22/07/09 16:57:15 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 220708B (Swift/BAT-GUANO arcminute localization:
Tohuvavohu et al., GCN Circ 32345;
CALET-CGBM detection: Kobayashi et al., GCN Circ 32356)
triggered Konus-Wind (KW) at T0=7620.140 s UT (02:07:00.140).

The burst light curve shows two separated emission episodes.
The first episode (reported in GCNs 32345, 32356)
starts at ~T0-1 s and has a duration of ~4 s.
The second, much longer episode starts at ~T0-380 s and lasts to ~T0+450 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/GRB220708_T07620/

As observed by Konus-Wind, the burst had
a total fluence of (1.23 Â± 0.44)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0 + 0.832 s,
of (2.03 Â± 0.39)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the first episode (measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range by a power law with exponential
cutoff (CPL) model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.68(-0.22,+0.44) and Ep = 90(-9,+11) keV (chi2 = 77/97 dof).
Fitting this spectrum by a Band function yields the same values of alpha and Ep,
and an upper limit on the high energy photon index beta of -2.8 (chi2 = 76/96 dof).
The fluence in this time interval is (2.8 Â± 0.5)E-06 erg/cm^2.

The time-averaged spectrum of the second episode (measured from T0+377.088 to T0+450.816 s)
is best fit in the 20 keV - 15 MeV range by a CPL model
with alpha = -1.48(-0.31,+0.42) and Ep = 146(-45,+66) keV (chi2 = 90/98 dof).
A Band function fits the spectrum equally well with alpha = -1.20 (-0.56,+0.57),
beta = -2.29(-7.71, + 0.34), and Ep = 107 (-32, +68) keV (chi2 = 90/97 dof).
The fluence in this time interval is (9.5 Â± 3.9)E-06 erg/cm^2.


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


GRB_name: GRB220708B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32359
SUBJECT: Konus-Wind detection of GRB 220708B (Correction to GCN 32358)
DATE:    22/07/10 16:26:21 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

D. Frederiks, on behalf of the Konus-Wind team:

The correct start time of the second episode of GRB 220708B reported in the KW GCN 32358 is T0+380 s.
We apologize for the typo and thank Jean-Luc Atteia for pointing this out.


GRB_name: GRB220708B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32360
SUBJECT: GRB 220708B: T193-OHP optical upper limit
DATE:    22/07/10 20:54:34 GMT
FROM:    Damien Turpin at NAOC (CAS)  <dturpin-astro@hotmail.com>

D. Turpin (CEA), C. Adami (LAM), B. Schneider,
E. Le Floch (CEA), S. Basa (LAM) report on behalf of
a larger collaboration:

We observed the field of GRB 220708B (Tohuvavohu et al. GCN 32345,
Kobayashi et al. GCN 32356, Frederiks et al. GCN 32358) using the T193cm
telescope at Observatoire de Haute-Provence (France) equipped with the 
MISTRAL spectro-imager. Six exposures (6x600s) were obtained in the r band
using the bleu MISTRAL set-up from 2022 08 Jul 20:55:39 UT to 2022 08 Jul
22:14:27 UT (mid time ~19.5h after trigger). In the combined frame, we do not
detect any source within the 4 arcsec error circle of the XRT position 
(Osborne et al. GCN 32350) down to the following 3-sigma limit:

r > 22.3 mag (AB)

The photometric calibration was performed using nearby stars 
from the PanSTARRS catalog. The magnitude is not corrected 
for Galactic extinction and it is consistent with the non-detections 
reported by Jiang et al. (GCN 32355).

We express our deepest thanks to the Observatoire de Haute-Provence for its
support, in particular to Stphane Favard and Jrme Schmitt.


GRB_name: GRB220708A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32361
SUBJECT: GRB 220708A: Swift-BAT refined analysis
DATE:    22/07/10 21:10:28 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

S. D. Barthelmy (GSFC), D'Elia (SSDC & INAF-OAR),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):
  
Using the data set from T-239 to T+1566 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 220708A (trigger #1115156)
(D'Elia, et al., GCN Circ. 32343).  The BAT ground-calculated position is
RA, Dec = 103.038, 72.199 deg which is
    RA(J2000)  =  06h 52m 09.1s
    Dec(J2000) = +72d 11' 57.4"
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
  
The BAT mask-weighted light curve shows a peak starting from T-1 s to T+3 s.
T90 (15-350 keV) is 4.4 +- 1.0 sec (estimated error including systematics).
  
The time-averaged spectrum from T-1.55 to T+3.44 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.31 +- 0.32.  The fluence in the 15-150 keV band is 1.3 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+1.54 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/1115156/BA/


GRB_name: GRB220711A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32362
SUBJECT: GRB 220711A: Fermi GBM Final Real-time Localization
DATE:    22/07/11 06:52:23 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:41:07 UT on 11 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220711A (trigger 679214472.628158 / 220711279).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 96.1, Dec = 33.9 (J2000 degrees, equivalent to J2000 06h 24m, 33d 53'), with a statistical uncertainty of 16.9 degrees.

The angle from the Fermi LAT boresight is 50.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711279/quicklook/glg_skymap_all_bn220711279.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/bn220711279/quicklook/glg_healpix_all_bn220711279.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711279/quicklook/glg_lc_medres34_bn220711279.gif


GRB_name: GRB220708B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32363
SUBJECT: GRB 220708B: GIT optical upper limits
DATE:    22/07/11 11:45:05 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

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

We observed GRB 220708B detected by Swift (Tohuvavohu et al., GCN 32345; Evans et at., GCN 32350), CALET GBM (Kawakubo et al., GCN 32356) and Konus-Wind (Frederiks et al., GCN 32358), with the 0.7m GROWTH-India Telescope (GIT). The observations started at 21:04:33 UT on 2022-07-08, 18.96 hours after the Swift trigger. We obtained multiple 300-sec exposures in the gâ€™, r' and iâ€™ filters. We did not detect any new source in our stacked images within the 4 arcsec radius circle around R.A.= 16h 34m 18.97s, Dec.= +36d 20' 52.0â€ (Osborne et al. GCN #32350). The obtained upper limits follow as:
-------------------------------------------------------------------
 JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Lim_mag (5-sigma) |
-------------------------------------------------------------------
 2459769.38578312 | 19.14 | 4 x 300 (stacked) | g' | > 21.03 |
 2459769.39333163 | 19.32 | 4 x 300 (stacked) | r' | > 20.99 |
 2459769.41415129 | 19.82 | 4 x 300 (stacked) | i' | > 19.83 | 
-------------------------------------------------------------------

These upper limits are consistent with Jiang et al.(GCN #32355), Turpin et al.(GCN #32360). The magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.


GRB_name: GRB220707A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32364
SUBJECT: GRB 220707A: AstroSat CZTI detection
DATE:    22/07/11 15:34:31 GMT
FROM:    Gaurav Waratkar at IIT,Bombay  <gauravwaratkar@iitb.ac.in>

A. Suresh (IITB), 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 220707A. It was 
also reported by INTEGRAL (Notice 9976,0).

The source was clearly detected in the 20-200 keV energy range. The 
light curve peaks at 2022-07-07 20:37:31.0 UTC. The measured peak count 
rate associated with the burst is 73 (+10 -9) counts/s above the 
background in the combined data of three quadrants, with a total of 3687 
(+409 -429) counts. The local mean background count rate was 332 (+1 -1) 
counts/s. Using cumulative rates, we measure a T90 of 75 (+11 -11) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve showed multiple peaks 
of emission with the strongest peak at 2022-07-07 20:37:29.6 UTC. The 
measured peak count rate is 380 (+82 -10) counts/s above the background 
in the combined Veto data of all quadrants, with a total of 15340 (+1048 
-1023)  counts. The local mean background count rate was 1343 (+3 -4) 
counts/s. We measure a T90 of 81 (+7 -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: GRB220711B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32365
SUBJECT: GRB 220711B: Fermi GBM Final Real-time Localization
DATE:    22/07/11 18:27:45 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 18:16:28 UT on 11 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220711B (trigger 679256193.06458 / 220711761).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 267.8, Dec = 31.5 (J2000 degrees, equivalent to J2000 17h 51m, 31d 30'), with a statistical uncertainty of 4.6 degrees.

The angle from the Fermi LAT boresight is 109.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711761/quicklook/glg_skymap_all_bn220711761.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/bn220711761/quicklook/glg_healpix_all_bn220711761.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711761/quicklook/glg_lc_medres34_bn220711761.gif


GRB_name: GRB220711B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32366
SUBJECT: GRB 220711B: Swift detection of a burst
DATE:    22/07/11 18:36:05 GMT
FROM:    Jamie Kennea at Penn State U  <jak51@psu.edu>

A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA),
V. D'Elia (SSDC & INAF-OAR), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (U Tampa), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester) and A. Tohuvavohu (U Toronto) report on
behalf of the Neil Gehrels Swift Observatory Team:

At 18:16:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220711B (trigger=1115766).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 261.993, +24.669 which is 
   RA(J2000) = 17h 27m 58s
   Dec(J2000) = +24d 40' 10"
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 100 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 18:18:12.3 UT, 103.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 262.02020,
24.67997 which is equivalent to:
   RA(J2000)  = 17h 28m 04.85s
   Dec(J2000) = +24d 40' 47.9"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 97 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 (7.40 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2
(+2.26/-2.02) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 113 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
0.067. 

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


GRB_name: GRB220711B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32367
SUBJECT: GRB 220711B: LCO Optical Upper Limits
DATE:    22/07/11 22:19:28 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration:

We observed the Fermi/Swift GRB 220711B (Fermi GBM Team, GCN 32365; D'Ai et al., GCN 32366) field with the Teide Observatory, Tenerife site, on July 11, from 21:05 to 21:23 (corresponding to 2.82 to 3.12 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 2x335s exposures in i and r bands.  We do not detect an optical counterpart within the XRT error region (D'Ai et al., GCN 32366) in either band.

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

r>21.54
i>21.34

These magnitudes are not corrected for galactic extinction.

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


GRB_name: GRB220711B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32368
SUBJECT: GRB 220711B: NOT optical observations
DATE:    22/07/11 23:20:15 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Radboud Univ. and DAWN/NBI), D. Alexander Kann 
(IAA/CSIC), S. D. Vergani (CNRS - Paris Obs./GEPI), L. Izzo (DARK/NBI), 
O. Durfeldt Pedros (NOT and DTU Space), and T. Pursimo (NOT), report on 
behalf of a larger collaboration:

We observed the field of GRB 220711B (D'Ai et al., GCN 32366) with the 
Nordic Optical Telescope (NOT) equipped with the ALFOSC imager. 
Observations started in twilight in the r band, so that the first images 
are not especially deep. A further set of five 200-s z-band images 
started on 2022 Jul 11.90 UT (3.23 hr after the trigger).

Close to the currently available XRT position, we see three sources in 
the stack of the z-band images (astrometry and photometry are calibrated 
against the Gaia and Pan-STARRS catalogs, respectively):

1)
RA = 17:28:04.49
Dec = +24:40:50.8
z = 21.78 +- 0.13 AB

2)
RA = 17:28:04.44
Dec = +24:40:46.7
z = 22.09 +- 0.15 AB

3)
RA = 17:28:04.97
Dec = +24:40:44.7
z = 22.60 +- 0.19 AB

Sources 2) and 3) are visible in archival images from the Pan-STARRS 
survey, while source 1) is not, which makes it a viable afterglow 
candidate. However, sources 1), and 2) are slightly outside (5.6" and 
5.7" away) the currently available (unenhanced) XRT position (which has 
a 3.6" 90% error radius).

Sources 2) and 3) are also detected in our NOT r-band images, while 
source 1) is not.

The relation of these sources to GRB 220711B is still under 
investigation. Further NOT observations are planned.


GRB_name: GRB220711B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32369
SUBJECT: GRB 220711B: Fermi GBM Detection
DATE:    22/07/12 00:49:33 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

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

"At 18:16:28.06 UT on 11 July 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220711B (trigger 679256193/220711761)
which was also detected by Swift-BAT (A. D'Ai et al. 2022, GCN 32366).
The Fermi GBM Final Real-time Localization (GCN 32365) is consistent
with the Swift-BAT position.

The angle from the Fermi LAT boresight is 101 degrees.

The GBM light curve consists of a multipeaked emission episode with a
duration (T90)
of about 82 s (10-1000 keV). The time-averaged spectrum
from T0-40 to T0+61 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.39 +/- 0.07 and the cutoff energy,
parameterized as Epeak, is 81 +/- 6 keV.

The event fluence (10-1000 keV) in this time interval is
(1.02 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.4 s in the 10-1000 keV band is 6.0 +/- 0.4 ph/s/cm^2.
A Band function fits the spectrum equally well
with Epeak= 79 +/- 8 keV, alpha = -1.37 +/- 0.09 and beta = -2.93 +/- 0.71.

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: GRB220711B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32370
SUBJECT: GRB 220711B: Enhanced Swift-XRT position
DATE:    22/07/12 02:09:51 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 3094 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 220711B, 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 = 262.01900, +24.68096 which is equivalent
to:

RA (J2000): 17h 28m 4.56s
Dec (J2000): +24d 40' 51.5"

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: GRB220711B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32371
SUBJECT: GRB 220711B: Swift/UVOT Upper Limits
DATE:    22/07/12 05:02:33 GMT
FROM:    Noel Klingler at NASA-GSFC / UMBC  <njk5441@psu.edu>

N. J. Klingler (GSFC/UMBC/CRESTII) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220711B
114 s after the BAT trigger (D'Ai et al., GCN Circ. 32366).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 32370)
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           114          264          147         >21.0
u_FC               326          576          246         >20.2
white              114          915          221         >21.0
v                  655         4601          236         >19.7
b                  581          773           39         >19.7
u                  326         5120          368         >20.4
w1                 704         5011          216         >20.5
m2                 852         4806          216         >19.4
w2                 631         4396          216         >20.4

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.067 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220711B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32372
SUBJECT: GRB 220711B: Swift-XRT refined Analysis
DATE:    22/07/12 12:14:06 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), E. Ambrosi 
(INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR),
D.N. Burrows (PSU), J. D. Gropp (PSU), J.A. Kennea (PSU), P.A. Evans
(U. Leicester) and A. D'Ai report on behalf of the Swift-XRT team:

We have analysed 6.3 ks of XRT data for GRB 220711B (D'Ai et al. GCN
Circ. 32366), from 93 s to 44.7 ks after the  BAT trigger. The data
comprise 414 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. 32370).

The late-time light curve (from T0+4.2 ks) can be modelled with a
power-law decay with a decay index of alpha=0.91 (+/-0.11).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+/-0.04). The
best-fitting absorption column is  2.59 (+/-0.16) x 10^21 cm^-2, in
excess of the Galactic value of 7.4 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.08 (+/-0.18) and a
best-fitting absorption column of 2.3 (+0.7, -0.6) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (4.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 7.4 x 10^20 cm^-2
Excess significance: 4.4 sigma
Photon index:      2.08 (+/-0.18)

If the light curve continues to decay with a power-law decay index of
0.91, the count rate at T+24 hours will be 0.016 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.4 x
10^-13 (7.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01115766.

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


GRB_name: GRB220711C
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32373
SUBJECT: IPN triangulation of GRB 220711C (short)
DATE:    22/07/12 15:50:56 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, 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 short-duration GRB 220711C
was detected by Fermi (GBM trigger 679248723),
INTEGRAL (SPI-ACS), Konus-Wind, and Swift (BAT)
at about 58318 s UT (16:11:58).
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:
    79.625         -47.309
   Corners:
    64.292         -35.777
    64.270         -36.123
    94.188         -53.124
    93.862         -52.805
   ------------------------------
The error box area is 5.5 sq. deg, and its maximum
dimension is 27 deg (the minimum one is 12 arcmin).
The Sun distance was 72 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM final localization (glg_healpix_all_bn220711675_v00).

A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB220711_T58317/IPN

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


GRB_name: GRB220711B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32374
SUBJECT: GRB 220711B: Swift-BAT refined analysis
DATE:    22/07/12 16:35:07 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
A. D'Ai (INAF-IASFPA), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220711B (trigger #1115766)
(D'Ai et al., GCN Circ. 32366).  The BAT ground-calculated position is
RA, Dec = 262.018, 24.674 deg which is
   RA(J2000)  =  17h 28m 04.3s
   Dec(J2000) = +24d 40' 27.1"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.

The mask-weighted light curve shows a multi-peaked structure that
starts at ~T-40 s and ends at ~T+100 s. The main peak occurs at ~T0.
T90 (15-350 keV) is 88.64 +- 19.96 sec (estimated error including
systematics).

The time-averaged spectrum from T-37.72 to T+98.89 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.75 +- 0.08.  The fluence in the 15-150 keV band
is 6.0 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T-0.02 sec in the 15-150 keV band is 3.0 +- 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/1115766/BA/


GRB_name: GRB220710A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32375
SUBJECT: GRB 220710A: Swift/BAT-GUANO arcminute localization
DATE:    22/07/12 20:58:22 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 220710A onboard (T0:
2022-07-10T03:29:34 UTC, GECAM trig utn220710_032932_GECAMb).

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 burst is detected in BAT with a duration of ~25 seconds.
The burst occurred during a Swift slew.
The burst position is found with an image SNR of 20.

The BAT position is
RA, Dec = 221.592, 20.657 deg which is
   RA(J2000)  = 14h 46m 22.08s
   Dec(J2000) =  20d 39â€² 25.2â€³
with an uncertainty of 2 arcmin.

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

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


GRB_name: GRB220710A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32376
SUBJECT: GRB 220710A: Swift ToO observations
DATE:    22/07/12 22:50:11 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 220710A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021509

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: GRB220712B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32377
SUBJECT: GRB 220712B: NOT optical afterglow confirmation
DATE:    22/07/12 23:18:47 GMT
FROM:    Daniele B Malesani at Radboud U  <d.malesani@astro.ru.nl>

D. B. Malesani (Radboud Univ. and DAWN/NBI), Z.P. Zhu (NAOC, HUST), M. 
A. Keniger (NOT), O. Durfeldt Pedros (NOT and DTU Space) report on 
behalf of a larger collaboration:

We observed again the field of GRB 220711B (D'Ai et al., GCN 32366) with 
the Nordic Optical Telescope equipped with the ALFOSC camera. 
Observations were carried out in the z band for a total of 25 min 
exposure. The mid time of the observation was 2022 Jul 12.92 UT (27.71 
hr after the GRB).

Object 1) identified by Malesani et al. (GCN 32368) has faded and is no 
longer detected in our images down to a limiting magnitude z > 23.5 AB 
(calibrated against nearby Pan-STARRS sources). We also note that the 
UVOT-enhanced XRT position (Beardmore et al., GCN 32370) has shifted and 
is fully consistent with the optical position.

We thus conclude that this object is the optical afterglow of GRB 220711B.

We note the red color of the afterglow: as measured in our images from 
last night (Malesani et al., GCN 32368), the afterglow had r-z > 2.2. As 
such, it is a potential high-redshift candidate (r dropout), though the 
large column density measured in the X-ray spectrum favors dust 
extinction as the explanation of the red color.


GRB_name: GRB220711B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32378
SUBJECT: Fermi GRB 220711B: Global MASTER-Net observations report 
DATE:    22/07/13 00:30:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev
(Irkutsk State University, API),

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

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 220711B ( Fermi GBM team, GCN 32365) errorbox  1 days 20192 sec after notice time and 1 days 20226 sec after trigger time at 2022-07-12 23:53:34 UT, with upper limit up to  17.0 mag. The observations began at zenith distance = 75 deg. The sun  altitude  is -71.6 deg. 

The galactic latitude b = 25 deg., longitude l = 57 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2028449

We obtain a following upper limits.  

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

    9098 | 2022-07-11 20:47:36 |             MASTER- | (17h 52m 34.45s , +31d 27m 32.4s) |   C |    60 | 18.1 |        
    9173 | 2022-07-11 20:48:51 |             MASTER- | (18h 02m 05.30s , +31d 27m 48.8s) |   C |    60 | 18.0 |        
    9320 | 2022-07-11 20:51:18 |             MASTER- | (17h 58m 24.11s , +29d 35m 23.4s) |   C |    60 | 18.0 |        
    9395 | 2022-07-11 20:52:32 |             MASTER- | (17h 57m 18.45s , +33d 21m 21.6s) |   C |    60 | 18.3 |        
    9529 | 2022-07-11 20:54:47 |             MASTER- | (18h 06m 54.95s , +33d 23m 15.9s) |   C |    60 | 18.1 |        
    9603 | 2022-07-11 20:56:01 |             MASTER- | (18h 06m 41.33s , +29d 33m 13.2s) |   C |    60 | 17.9 |        
    9960 | 2022-07-11 21:01:58 |             MASTER- | (18h 15m 59.80s , +29d 34m 09.9s) |   C |    60 | 18.0 |        
   10371 | 2022-07-11 21:08:49 |             MASTER- | (17h 52m 33.12s , +31d 28m 51.2s) |   C |    60 | 18.1 |        
   10445 | 2022-07-11 21:10:03 |             MASTER- | (18h 02m 02.64s , +31d 27m 49.2s) |   C |    60 | 17.5 |        
   87628 | 2022-07-12 18:36:25 |             MASTER- | (17h 44m 54.03s , +35d 17m 39.5s) |   C |    60 | 17.1 |        
   87703 | 2022-07-12 18:37:40 |             MASTER- | (17h 54m 49.30s , +35d 17m 32.4s) |   C |    60 | 17.6 |        
   87835 | 2022-07-12 18:39:53 |             MASTER- | (17h 34m 51.34s , +31d 31m 06.4s) |   C |    60 | 17.6 |        
   87909 | 2022-07-12 18:41:06 |             MASTER- | (17h 44m 09.20s , +31d 29m 54.8s) |   C |    60 | 17.6 |        
   88045 | 2022-07-12 18:43:22 |             MASTER- | (17h 39m 13.60s , +33d 24m 50.7s) |   C |    60 | 17.8 |        
   88119 | 2022-07-12 18:44:36 |             MASTER- | (17h 48m 43.86s , +33d 23m 37.4s) |   C |    60 | 17.9 |        
   88258 | 2022-07-12 18:46:56 |             MASTER- | (18h 04m 17.54s , +27d 42m 49.8s) |   C |    60 | 17.6 |        
   88332 | 2022-07-12 18:48:10 |             MASTER- | (18h 13m 13.60s , +27d 41m 39.0s) |   C |    60 | 15.8 |        
   88469 | 2022-07-12 18:50:27 |             MASTER- | (18h 03m 39.99s , +35d 18m 02.0s) |   C |    60 | 18.1 |        
   88544 | 2022-07-12 18:51:41 |             MASTER- | (18h 13m 29.75s , +35d 16m 52.5s) |   C |    60 | 17.8 |        
   88680 | 2022-07-12 18:53:58 |             MASTER- | (17h 44m 55.34s , +35d 19m 28.8s) |   C |    60 | 17.9 |        
   88755 | 2022-07-12 18:55:13 |             MASTER- | (17h 54m 50.22s , +35d 18m 15.6s) |   C |    60 | 18.2 |        
   88893 | 2022-07-12 18:57:31 |             MASTER- | (17h 34m 46.75s , +31d 31m 50.7s) |   C |    60 | 18.0 |        
   88967 | 2022-07-12 18:58:45 |             MASTER- | (17h 44m 15.51s , +31d 30m 40.0s) |   C |    60 | 18.0 |        
   89105 | 2022-07-12 19:01:02 |             MASTER- | (17h 39m 08.40s , +33d 25m 37.7s) |   C |    60 | 18.0 |        
   89179 | 2022-07-12 19:02:17 |             MASTER- | (17h 48m 51.01s , +33d 24m 26.3s) |   C |    60 | 18.2 |        
   89255 | 2022-07-12 19:03:32 |             MASTER- | (18h 04m 14.10s , +27d 41m 34.0s) |   C |    60 | 17.8 |        
   89388 | 2022-07-12 19:05:45 |             MASTER- | (18h 13m 15.43s , +27d 43m 22.9s) |   C |    60 | 17.9 |        
   89464 | 2022-07-12 19:07:02 |             MASTER- | (18h 03m 39.10s , +35d 17m 57.1s) |   C |    60 | 18.3 |        
   89602 | 2022-07-12 19:09:20 |             MASTER- | (18h 13m 29.70s , +35d 17m 42.4s) |   C |    60 | 18.1 |        
   89678 | 2022-07-12 19:10:35 |             MASTER- | (17h 44m 54.93s , +35d 17m 19.4s) |   C |    60 | 18.2 |        
   89813 | 2022-07-12 19:12:51 |             MASTER- | (17h 54m 44.11s , +35d 19m 07.0s) |   C |    60 | 18.3 |        
   89888 | 2022-07-12 19:14:06 |             MASTER- | (17h 34m 50.97s , +31d 30m 35.0s) |   C |    60 | 18.1 |        
   90076 | 2022-07-12 19:17:14 |             MASTER- | (17h 44m 10.26s , +31d 31m 24.1s) |   C |    60 | 18.2 |        
   90150 | 2022-07-12 19:18:28 |             MASTER- | (17h 39m 13.33s , +33d 24m 23.1s) |   C |    60 | 18.1 |        
   90288 | 2022-07-12 19:20:46 |             MASTER- | (17h 48m 44.63s , +33d 25m 12.3s) |   C |    60 | 18.2 |        
   90364 | 2022-07-12 19:22:02 |             MASTER- | (18h 04m 20.94s , +27d 42m 14.5s) |   C |    60 | 17.8 |        
   90523 | 2022-07-12 19:24:41 |             MASTER- | (18h 13m 17.06s , +27d 43m 04.0s) |   C |    60 | 17.9 |        
   90600 | 2022-07-12 19:25:57 |             MASTER- | (18h 03m 38.78s , +35d 17m 46.6s) |   C |    60 | 18.3 |        
   90785 | 2022-07-12 19:29:02 |             MASTER- | (18h 13m 21.62s , +35d 18m 32.9s) |   C |    60 | 17.9 |        
   90860 | 2022-07-12 19:30:18 |             MASTER- | (18h 10m 27.72s , +31d 28m 46.9s) |   C |    60 | 18.0 |        
   91048 | 2022-07-12 19:33:26 |             MASTER- | (18h 19m 51.93s , +31d 30m 34.1s) |   C |    60 | 18.1 |        
   91123 | 2022-07-12 19:34:41 |             MASTER- | (18h 15m 36.84s , +33d 22m 32.1s) |   C |    60 | 12.4 |        
   91337 | 2022-07-12 19:38:14 |             MASTER- | (17h 31m 41.85s , +29d 35m 08.8s) |   C |    60 | 18.1 |        
   91524 | 2022-07-12 19:41:21 |             MASTER- | (17h 40m 55.44s , +29d 36m 59.9s) |   C |    60 | 18.1 |        
   91598 | 2022-07-12 19:42:36 |             MASTER- | (17h 47m 05.69s , +27d 40m 57.4s) |   C |    60 | 18.0 |        
   91785 | 2022-07-12 19:45:43 |             MASTER- | (17h 56m 07.99s , +27d 42m 48.1s) |   C |    60 | 17.9 |        
   91860 | 2022-07-12 19:46:58 |             MASTER- | (18h 10m 33.38s , +31d 29m 29.1s) |   C |    60 | 17.9 |        
   92048 | 2022-07-12 19:50:05 |             MASTER- | (18h 19m 51.50s , +31d 30m 18.0s) |   C |    60 | 18.0 |        
   92122 | 2022-07-12 19:51:20 |             MASTER- | (18h 15m 41.53s , +33d 23m 16.4s) |   C |    60 | 18.0 |        
   92335 | 2022-07-12 19:54:53 |             MASTER- | (17h 31m 48.72s , +29d 35m 45.3s) |   C |    60 | 18.0 |        
   92521 | 2022-07-12 19:57:58 |             MASTER- | (17h 40m 53.67s , +29d 36m 37.9s) |   C |    60 | 18.0 |        
   92595 | 2022-07-12 19:59:13 |             MASTER- | (17h 47m 11.12s , +27d 41m 34.8s) |   C |    60 | 17.8 |        
   92782 | 2022-07-12 20:02:20 |             MASTER- | (17h 56m 07.69s , +27d 42m 26.6s) |   C |    60 | 17.8 |        
   92856 | 2022-07-12 20:03:34 |             MASTER- | (18h 10m 33.09s , +31d 29m 13.3s) |   C |    60 | 17.0 |        
  106657 | 2022-07-12 23:53:34 |         MASTER-SAAO | (17h 45m 25.60s , +31d 37m 42.4s) |   C |    60 | 16.7 |        
  106737 | 2022-07-12 23:54:54 |         MASTER-SAAO | (17h 54m 53.08s , +31d 37m 30.4s) |   C |    60 | 16.8 |        
  106827 | 2022-07-12 23:56:24 |         MASTER-SAAO | (17h 42m 12.38s , +29d 44m 25.4s) |   C |    60 | 16.8 |        
  106906 | 2022-07-12 23:57:44 |         MASTER-SAAO | (17h 51m 25.02s , +29d 45m 10.9s) |   C |    60 | 16.9 |        
  106997 | 2022-07-12 23:59:15 |         MASTER-SAAO | (17h 50m 05.59s , +33d 33m 46.5s) |   C |    60 | 16.6 |        
  107087 | 2022-07-13 00:00:45 |         MASTER-SAAO | (17h 59m 44.94s , +33d 32m 11.4s) |   C |    60 | 16.8 |        
  107170 | 2022-07-13 00:02:07 |         MASTER-SAAO | (17h 59m 41.66s , +29d 43m 34.7s) |   C |    60 | 17.0 |        
  107260 | 2022-07-13 00:03:38 |         MASTER-SAAO | (18h 08m 50.39s , +29d 44m 05.3s) |   C |    60 | 17.0 |        
  107340 | 2022-07-13 00:04:57 |         MASTER-SAAO | (17h 57m 22.60s , +27d 51m 15.7s) |   C |    60 | 16.9 |        
  107432 | 2022-07-13 00:06:30 |         MASTER-SAAO | (18h 06m 18.27s , +27d 49m 45.4s) |   C |    60 | 17.0 |        
  107512 | 2022-07-13 00:07:50 |         MASTER-SAAO | (17h 27m 56.18s , +31d 40m 35.1s) |   C |    60 | 14.9 |        
  107814 | 2022-07-13 00:12:52 |         MASTER-SAAO | (17h 37m 16.91s , +31d 39m 31.8s) |   C |    60 | 15.8 |        
  107905 | 2022-07-13 00:14:23 |         MASTER-SAAO | (17h 45m 37.78s , +31d 40m 12.6s) |   C |    60 | 16.1 |        
  107996 | 2022-07-13 00:15:53 |         MASTER-SAAO | (17h 54m 57.41s , +31d 38m 25.7s) |   C |    60 | 16.3 |        
  108075 | 2022-07-13 00:17:13 |         MASTER-SAAO | (17h 42m 25.20s , +29d 46m 22.8s) |   C |    60 | 16.1 |        
  108166 | 2022-07-13 00:18:44 |         MASTER-SAAO | (17h 51m 26.66s , +29d 45m 13.2s) |   C |    60 | 16.3 |        
  108246 | 2022-07-13 00:20:03 |         MASTER-SAAO | (17h 59m 51.64s , +33d 32m 54.3s) |   C |    60 | 16.3 |        
  108336 | 2022-07-13 00:21:34 |         MASTER-SAAO | (17h 59m 42.45s , +29d 43m 45.6s) |   C |    60 | 16.4 |        
  108416 | 2022-07-13 00:22:54 |         MASTER-SAAO | (18h 08m 57.21s , +29d 43m 34.7s) |   C |    60 | 16.5 |        
  108507 | 2022-07-13 00:24:24 |         MASTER-SAAO | (17h 57m 25.77s , +27d 51m 33.7s) |   C |    60 | 16.4 |        
  108586 | 2022-07-13 00:25:44 |         MASTER-SAAO | (18h 06m 25.29s , +27d 49m 33.4s) |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220711B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32380
SUBJECT: GRB 220711B: GIT optical upper limits
DATE:    22/07/13 02:48:45 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

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

We observed GRB 220711B detected by Fermi (Fermi GBM Team, GCN 32365; Lesage, GCN 32369), Swift (D'Ai et al., GCN 32366) and NOT optical (Malesani et al., GCN 32368), with the 0.7m GROWTH-India Telescope (GIT). The observations started at 18:22:15 UT on 2022-07-11, 5.78 mins after the Fermi 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 2.1 arcsec radius circle around R.A.= 17h 28m 4.56s, Dec.= +24d 40' 51.5" (Beardmore et al. GCN #32370). The obtained upper limits follow as:
-------------------------------------------------------------------
 JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Lim_mag (5-sigma) |
-------------------------------------------------------------------
 2459772.307085455 | 1.09 | 10 x 300 (stacked) | r' | > 21.03 |
 2459772.313860030 | 1.25 | 5 x 300 (stacked) | g' | > 20.50 |
 2459772.330168085 | 1.65 | 5 x 300 (stacked) | i' | > 20.34 | 
-------------------------------------------------------------------

While the first image was observed within just 6 minutes of the burst, the observing conditions were suboptimal and the first r' image has a limiting magnitude of ~19. No source is detected in that single 300-s exposure either. 

These upper limits are consistent with Strausbaugh et al.(GCN #32367), and Klingler et al.(GCN #32371), and with detection by Malesani et al (GCN #32368, 32377) given the high r-z colour they have inferred. The magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.


GRB_name: GRB220711B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32381
SUBJECT: GRB 220711B: NUTTelA-TAO / BSTI Early Optical Limits (Preliminary)
DATE:    22/07/13 06:42:29 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 220711B 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 received the alert at UT 
2022-07-11 18:16:50, 22 seconds after  the BAT trigger time, and started 
observations at UT 18:17:02, 12 s after receipt, 34 s after the BAT 
trigger. Observations were made under partially cloudy conditions. No 
new or changing sources consistent with the XRT position (Beardmore 
2022, GCN 32370) were detected. The observations fully cover the 
UVOT/XRT observation time interval and partly cover the prompt emission 
time (D'Ai 2022, GCN 32366). 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) ------------ -------- ----------- ------ ------ 
----- ------ 18:17:02 34 18:18:02 18.3 18.1 17.7 60 18:18:17 109 
18:23:17 19.2 18.9 18.7 300 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 images co-added to the given exposure time. The first 
row in the table corresponds to co-adds of an initial short exposure 
image sequence of 0.3 s (these sub-second exposures are read-noise 
suppressed by our EMCCD cameras, with high gain electron multiplication 
active; other images are taken in conventional CCD operation mode) for 
g' and r', and 7.5 s for i'. The second row corresponds to co-adds from 
a continuing series of 3 s exposures for g' and r', and 15 s exposures 
for i'.  Calibration was done with 4 bright Pan-STARRS catalog stars on 
our images. We caution the reader that these are preliminary results, 
without color or other corrections. Please also note that times are 
approximate. ---------------------------------- NU = Nazarbayev 
University, Nur-Sultan, Kazakhstan UCB = University of California, 
Berkeley, USA HKUST = Hong Kong University of Science and Technology FAI 
= Fesenkov Astrophysical Institute, Kazakhstan The NUTTelA-TAO Team 
acknowledges the support of the staff of the Assy-Turgen Astrophysical 
Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical 
Institute, Almaty, Kazkhstan.


GRB_name: GRB220711C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32382
SUBJECT: Konus-Wind detection of GRB 220711C
DATE:    22/07/13 14:24:59 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 220711C
(IPN triangulation: Svinkin et al., GCN Circ 32373)
triggered Konus-Wind at T0=58317.557 s UT (16:11:57.557).

The burst light curve shows a single emission pulse,
which starts at T0-0.3 s and has a total duration of ~0.4 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/GRB220711_T58317/

As observed by Konus-Wind, the burst
had a fluence of 2.01(-0.37,+0.43)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.066 s,
of 1.27(-0.49,+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+0.128 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = 0.06(-0.41,+0.55)
and Ep = 736(-169,+251) keV (chi2 = 19/26 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 = 19/25 dof).

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


GRB_name: GRB220711B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32383
SUBJECT: GRB 220711B, GROND observations
DATE:    22/07/13 14:52:45 GMT
FROM:    Ana Nicuesa at TLS Tautenburg  <ana@tls-tautenburg.de>

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

We observed the field of GRB 220711B (D'Ai et al., GCN 32366;
Beardmore et al. GCN 32370) with GROND mounted at the 2.2m MPG
telescope at La Silla Observatory (Chile).

Observations started at 01:53 UT on July 13, 2022, about 32 hr after
the GRB trigger and were on target for  40 minutes. They were performed
at an average seeing of 1.0 arcsec and at an airmass of 1.7.

The fading source discovered by Malesani et al. (GCN 32377) is
detected in the combined JHK images. For the individual bands we can
only provide the following preliminary upper limits (midtime of 2:20
UT):

  g' > 23.0,
  r' > 23.5,
  i' > 23.2,
  z' > 19.8,
  J  > 21.7,
  H  > 21.1,
  K  > 20.1  (AB mag; 3 sigma).

The given limits are derived based on calibrating the optical images
against the SDSS catalog and the JHK data against 2MASS stars.
We thank Sam Kim and Regis Lachaume for excellent support and for
performing the observations.


GRB_name: GRB220711C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32384
SUBJECT: GRB 220711C: Swift/BAT-GUANO detection outside the coded FOV
DATE:    22/07/13 15:42:38 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not localize GRB 220711C onboard (T0:
2022-07-11T16:11:58 UTC, IPN GCN 32373, KONUS GCN 32382).

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

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

The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu,
arXiv:2111.01769), detects the burst with a sqrt(TS) of 10.9 in a
0.256 s analysis time bin.

NITRATES results are consistent with a burst coming from outside the
FOV, with DeltaLLHOut of 6.

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

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: GRB220710A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32385
SUBJECT: GRB 220710A: Swift-XRT afterglow detection
DATE:    22/07/13 16:37:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-GUANO-detected burst GRB 220710A, collecting 4.4 ks of Photon
Counting (PC) mode data between T0+242.5 ks and T0+287.4 ks. 

An uncatalogued X-ray source is detected consistent with being within
197 arcsec of the Swift/BAT-GUANO position and is above the 2SXPS
3-sigma upper limit at this position, and is therefore likely the GRB
afterglow.  The position of this source is RA, Dec=221.5668, +20.6576
which is equivalent to:

RA (J2000): 14:46:16.03
Dec(J2000): +20:39:27.3

with an uncertainty of 8.3 arcsec (radius, 90% confidence).  This
position is 83 arcsec from the Swift/BAT-GUANO position.  We cannot
determine at the present time whether the source is fading.

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/ToO_GRBs/00021509/Source3.php.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021509.

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


GRB_name: GRB220711B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32386
SUBJECT: GRB 220711B: 10.4 m GTC(+EMIR) observations
DATE:    22/07/13 18:24:32 GMT
FROM:    RubÃ©n SÃ¡nchez-RamÃ­rez at IAA-CSIC  <ruben@iaa.es>

R. Sanchez-Ramirez, Y.-D. Hu, I. Perez-Garcia, M.D. Caballero-Garcia, A.J. Castro-Tirado (IAA-CSIC) report on behalf of a larger collaboration:
We observed the field of GRB220711B (Fermi GBM team GCNc 32365, D'Ai et al. GCNc 32366) with the Espectrografo Multiobjeto Infra-Rojo (EMIR), mounted on the 10.4m Gran Telescopio de Canarias (GTC) in La Palma (Spain).
Imaging observations started on Jul 12 at 00:32:14 (~4.3 hrs after the GRB) and were carried out in the J and Ks bands for a total exposure time of 1260s in each filter.
The afterglow reported by Malesani et al. (GCNc 32368 and 32377) is clearly detected in a preliminary reduction of both filters, measuring J~21.3 AB.

A second epoch was obtained on Jul 12 at 23:31:10 in the J band, observing a decay of about 1 magnitude between both epochs.

Further observations are planned.

We thank the excellent support from the GTC staff.


GRB_name: GRB220711B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32387
SUBJECT: GRB 220711B: 10.4 m GTC(+EMIR) observations
DATE:    22/07/13 18:43:53 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

R. Sanchez-Ramirez, Y.-D. Hu, I. Perez-Garcia, M.D. Caballero-Garcia, A.J. Castro-Tirado (IAA-CSIC) report on behalf of a larger collaboration:

We observed the field of GRB220711B (Fermi GBM team GCNC 32365, D'Ai et al. GCNC 32366) with the Espectrografo Multiobjeto Infra-Rojo (EMIR), mounted on the 10.4m Gran Telescopio de Canarias (GTC) in La Palma (Spain). Imaging observations started on Jul 12 at 00:32:14 (~4.3 hrs after the GRB) and were carried out in the J and Ks bands for a total exposure time of 1260s in each filter. The afterglow reported by Malesani et al. (GCNC 32368 and 32377) is clearly detected in a preliminary reduction of both filters, measuring J~21.3 AB.

A second epoch was obtained on Jul 12 at 23:31:10 in the J band, observing a decay of about 1 magnitude between both epochs. Further observations are planned.

We thank the excellent support from the GTC staff.


GRB_name: GRB220711B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32388
SUBJECT: Retraction of GRB 220711B: 10.4 m GTC(+EMIR) observations (GCN 32387) 
DATE:    22/07/13 21:19:03 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu report:

GCNC 32387 is a repeated submittion of GCNC 32386 by mistake. Please ignore it and pay attention to GCNC 32386. Sorry for this mistake and I apologize for any confusion this mistake may have caused.


GRB_name: GRB220711C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32389
SUBJECT: GRB 220711C: Fermi GBM Observation
DATE:    22/07/13 21:56:21 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

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

"At 16:11:58.54 UT on 11 July 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220711C (trigger 679248723/220711675)
which was also detected by Konus-Wind (A. Ridnaia, et al. 2022, GCN 32382),
Swift/BAT-GUANO (G. Raman et al. 2022, GCN 32384),
and localized by IPN (D. Svinkin et al. 2022, GCN 32373).

The on-ground calculated location, using the GBM trigger data,
is RA = 81.06, DEC = -48.16 (J2000 degrees, equivalent
to 05h 24m, -48d 10'), with an uncertainty of 3.5 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 Fermi GBM on-ground location is consistent with the IPN triangulation.

The angle from the Fermi LAT boresight is 130 degrees.

The GBM light curve consists of a single emission episode with a duration (T90)
of about 0.3 s (10-1000 keV). The time-averaged spectrum
from T0-0.06 to T0+0.26 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -0.1 +/- 0.2 and the cutoff energy,
parameterized as Epeak, is 972.6 +/- 136.0 keV.

The event fluence (10-1000 keV) in this time interval is
(1.51 +/- 0.08)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0 s in the 10-1000 keV band is 13.6 +/- 1.4 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: GRB220710A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32390
SUBJECT: GRB 220710A: Swift/UVOT Upper Limits
DATE:    22/07/14 06:28:25 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A.A. Breeveld (UCL-MSSL) and N. J. Klingler (GSFC/UMBC/CRESTII) report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220710A 242493 s after the GECAM/GUANO 
trigger (Tohuvavohu et al., GCN Circ. 32375).
No optical afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 32385) is detected 
in the UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. 
Proc. 1358, 373) for the initial exposures are:

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

white           242493       287404         4429         >22.9

The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of 
E(B-V) = 0.030 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB220714A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32391
SUBJECT: GRB 220714A: Possible Swift detection of a burst
DATE:    22/07/14 06:45:18 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

S. Laha (GSFC/UMBC), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), S. Dichiara (PSU), M. Ferro (INAF-OAB),
N. J. Klingler (GSFC/UMBC/CRESSTII), H. A. Krimm (NSF),
K. L. Page (U Leicester) and T. Sbarrato (INAF-OAB) report on behalf
of the Neil Gehrels Swift Observatory Team:

At 05:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located a possible GRB 220714A (trigger=1116172). Swift slewed immediately. 
The BAT on-board calculated location is 
RA, Dec  which is 171.904, -59.342
  RA(J2000)  =  11h 27m 37s
  Dec(J2000) = -59d 20' 32"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty). 

No source was detected in 270 s of promptly downlinked data. We are
waiting for the full dataset to detect and localise the XRT
counterpart. 

Some of the TDRSS notices, including all of the BAT notices, have been
lost, so we have no prompt information about the possible GRB
light-curve or duration. Therefore, such information will only be
available when the data have been dumped to the ground around 09 UT. 

Burst Advocate for this burst is S. Laha (sib.laha 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: GRB220714B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32392
SUBJECT: GRB 220714B: Fermi GBM Final Real-time Localization
DATE:    22/07/14 14:08:37 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 13:58:06 UT on 14 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220714B (trigger 679499891.272708 / 220714582).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 45.9, Dec = -22.6 (J2000 degrees, equivalent to J2000 03h 03m, -22d 36'), with a statistical uncertainty of 2.8 degrees.

The angle from the Fermi LAT boresight is 124.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220714582/quicklook/glg_skymap_all_bn220714582.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/bn220714582/quicklook/glg_healpix_all_bn220714582.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220714582/quicklook/glg_lc_medres34_bn220714582.gif


GRB_name: GRB220714B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32393
SUBJECT: GRB 220714B: Swift detection of a burst
DATE:    22/07/14 14:10:18 GMT
FROM:    Kim Page at U.of Leicester  <kimlpage1978@gmail.com>

S. Laha (GSFC/UMBC), R. Brivio (INAF-OAB), P. D'Avanzo (INAF-OAB),
S. Dichiara (PSU), M. Ferro (INAF-OAB), J.D. Gropp (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), 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 13:58:04 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220714B (trigger=1116221).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 47.072, -19.334 which is 
   RA(J2000) = 03h 08m 17s
   Dec(J2000) = -19d 20' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 40 sec.  The peak count rate
was ~5500 counts/sec (15-350 keV), at ~13 sec after the trigger. 

The XRT began observing the field at 13:59:20.9 UT, 76.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 47.0803, -19.3269 which is equivalent to:
   RA(J2000)  = 03h 08m 19.27s
   Dec(J2000) = -19d 19' 36.8"
with an uncertainty of 5.2 arcseconds (radius, 90% containment). This
location is 38 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 1.70e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of  56 seconds with the White filter
starting 121 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 position. 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 0.032. 

Burst Advocate for this burst is S. Laha (sib.laha 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: GRB220713A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32394
SUBJECT: GRB 220713A: Fermi GBM Final Localization
DATE:    22/07/14 16:14:51 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

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

At 16:35:42.06 UT on 13 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220713A (trigger 679422947 / 220713691).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 25.0, Dec = 34.5 (J2000 degrees, equivalent to J2000 01h 40m, +34d 30'), with a statistical uncertainty of 4.6 degrees.

The angle from the Fermi LAT boresight is 69.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220713691/quicklook/glg_skymap_all_bn220713691.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/bn220713691/quicklook/glg_healpix_all_bn220713691.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220713691/quicklook/glg_lc_medres34_bn220713691.gif


GRB_name: GRB220714B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32395
SUBJECT: GRB 220714B: Enhanced Swift-XRT position
DATE:    22/07/14 18:41:13 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 1471 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 220714B, 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 = 47.08386, -19.32962 which is equivalent
to:

RA (J2000): 03h 08m 20.13s
Dec (J2000): -19d 19' 46.6"

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: GRB220714B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32396
SUBJECT: GRB 220714B: UVOT afterglow discovery
DATE:    22/07/14 18:53:03 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and S. Laha (GSFC/UMBC) report on behalf of the Swift team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3552 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  =     03:08:20.18 =  47.08409
  DEC(J2000) = -19:19:45.3  = -19.32925
with a 90%-confidence error radius of about 0.61 arc sec. This position is 1.5
arc sec. from the center of the XRT error circle (Evans et al. GCN Circ. 32395). The estimated magnitude is
16.52 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.032.


GRB_name: GRB220714A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32397
SUBJECT: Swift/BAT Trigger 1116172 (=GRB 220714A) is not a real astrophysical event
DATE:    22/07/14 20:16:29 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

S. Laha (GSFC/UMBC),  K. L. Page (U Leicester), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII),
report on behalf of the Neil Gehrels Swift Observatory Team:

After analysis of the full dataset, we have determined that trigger=1116172 (reported as possible GRB 220714A in GCN#32391)
is not an astrophysical event.  Instead, a known race condition in the onboard software caused the currently-active source Cen X-3 to be misidentified.


GRB_name: GRB220714B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32398
SUBJECT: GRB 220714B: Swift-XRT refined Analysis
DATE:    22/07/15 04:20:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.0 ks of XRT data for GRB 220714B (Laha et al. GCN
Circ. 32393), from 71 s to 45.6 ks after the  BAT trigger. The data
comprise 135 s in Windowed Timing (WT) mode (the first 4 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. 32395).

The late-time light curve (from T0+3.5 ks) can be modelled with a
power-law decay with a decay index of alpha=1.22 (+/-0.04).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.95 (+0.19, -0.18). The
best-fitting absorption column is  2.7 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 3.2 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.03 (+/-0.10) and a
best-fitting absorption column of 1.47 (+0.28, -0.27) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (4.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.47 (+0.28, -0.27) x 10^21 cm^-2
Galactic foreground: 3.2 x 10^20 cm^-2
Excess significance: 7.0 sigma
Photon index:      2.03 (+/-0.10)

If the light curve continues to decay with a power-law decay index of
1.22, the count rate at T+24 hours will be 0.059 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 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/01116221.

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


GRB_name: GRB220715A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32399
SUBJECT: GRB 220715A: Fermi GBM Final Real-time Localization
DATE:    22/07/15 08:59:57 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 08:49:40 UT on 15 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220715A (trigger 679567785.342096 / 220715368).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 171.2, Dec = -31.1 (J2000 degrees, equivalent to J2000 11h 24m, -31d 06'), with a statistical uncertainty of 7.5 degrees.

The angle from the Fermi LAT boresight is 108.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220715368/quicklook/glg_skymap_all_bn220715368.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/bn220715368/quicklook/glg_healpix_all_bn220715368.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220715368/quicklook/glg_lc_medres34_bn220715368.gif


GRB_name: GRB220714B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32400
SUBJECT: GRB 220714B: LCO Optical Observations
DATE:    22/07/15 12:51:28 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration:

We observed the Swift GRB 220714B (Laha et al., GCN 32393) field with the LCO 1-meter Sinistro instrument at the South African Astronomical Observatory site, on July 15, from 02:32 to 02:59 UT (corresponding to 13.57 to 14.02 hours from the GRB trigger time) with the SDSS r and i filters.

We performed a series of 3x300s exposures in i and r bands.  We detect an optical counterpart at the same position as the UVOT afterglow (Marshall et al., GCN 32396) in both bands.

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

r = 19.77 +/- 0.07
i = 19.44 +/- 0.07

These magnitudes are not corrected for galactic extinction.

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


GRB_name: GRB220715A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32401
SUBJECT: GRB 220715A: AGILE/MCAL detection
DATE:    22/07/15 15:24:26 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE Mini-CALorimeter (MCAL) detected the GRB 220715A at T0 =
2022-07-15 08:49:40.23 +/- 0.01 s (UTC), reported by Fermi GBM (GCN #32399).

The event lasted about 0.40 s and released a total number of 300 counts in
the MCAL detector (in the 0.4-100 MeV energy range), above an average
background rate of 480 Hz. The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/079170_GRB_MCAL_584959780.229917.png
. The time-integrated spectrum of the burst, from T0-0.10 s to T0+0.30 s,
can be fitted in the energy range 0.4-10 MeV with a power-law with ph.ind.
= -2.06 (-0.367,+0.49), resulting in a reduced chi-squared of 0.86 (24
d.o.f.) and a fluence of 6.20e-07 erg/cm^2 (90% confidence level), in the
same energy range. At the T0, the event was 65 deg off-axis.

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


GRB_name: GRB220714B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32402
SUBJECT: GRB 220714B: Fermi GBM observation
DATE:    22/07/15 17:26:22 GMT
FROM:    Sarah Dalessi at UAH  <sd0104@uah.edu>

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

"At 13:58:06.27 UT on 14 July 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220714B (trigger 679499891 / 220714582)
which was also detected by the Swift/BAT (S. Laha et al. 2022, GCN 32393)
The Fermi GBM Final Real-time Localization (GCN 32392) is consistent
with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 121 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 28 s (50-300 keV).
The time-averaged spectrum from T0-3.07 s to T0+26.6 s is
well by a power law function with an exponential
high-energy cutoff.  The power law index is -1.63 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 139 +/- 24 keV

The event fluence (10-1000 keV) in this time interval is
(8.0 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+11.0 s in the 10-1000 keV band
is 6.5 +/- 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: GRB220714B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32403
SUBJECT: GRB 220714B: Swift-BAT refined analysis
DATE:    22/07/15 19:47:40 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

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-173 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 220714B (trigger #1116221)
(Laha, et al., GCN Circ. 32393).  The BAT ground-calculated position is
RA, Dec = 47.086, -19.321 deg which is
   RA(J2000)  =  03h 08m 20.7s
   Dec(J2000) = -19d 19' 13.8"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 88%.

The mask-weighted light curve shows a complex structure.  The main period of
emission starts around T-5 sec and continues to T+35 seconds with three main
overlapping pulses.  There is some precursor activity starting as early as T-45
seconds and low-level emission extending to T+60 seconds.  The spacecraft
slewed away from the burst location at around T+275 seconds.
T90 (15-350 keV) is 50.10 +- 7.96 sec (estimated error including systematics).

The time-averaged spectrum from -48.27 to +45.75 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.92 +- 0.07.  The fluence in the 15-150 keV band is 4.4 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+12.89 sec in the 15-150 keV band
is 3.8 +- 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/1116221/BA/


GRB_name: GRB220715B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32404
SUBJECT: GRB 220715B: Fermi GBM Final Real-time Localization
DATE:    22/07/15 22:35:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:24:42 UT on 15 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220715B (trigger 679616687.73956 / 220715934).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 221.7, Dec = -36.4 (J2000 degrees, equivalent to J2000 14h 46m, -36d 23'), with a statistical uncertainty of 16.5 degrees.

The angle from the Fermi LAT boresight is 87.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220715934/quicklook/glg_skymap_all_bn220715934.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/bn220715934/quicklook/glg_healpix_all_bn220715934.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220715934/quicklook/glg_lc_medres34_bn220715934.gif


GRB_name: GRB220715B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32405
SUBJECT: GRB 220715B: Swift detection of a burst
DATE:    22/07/15 22:39:06 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Troja (NASA/GSFC/UMCP), P. D'Avanzo (INAF-OAB), S. Dichiara (PSU),
M. Ferro (INAF-OAB), J.D. Gropp (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), T. Sbarrato (INAF-OAB) and
M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 22:24:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220715B (trigger=1116441).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 254.889, -33.597 which is 
   RA(J2000) = 16h 59m 33s
   Dec(J2000) = -33d 35' 48"
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 50 sec.  The peak count rate
was ~2400 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 22:26:20.9 UT, 98.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 254.87520, -33.59766 which is
equivalent to:
   RA(J2000)  = 16h 59m 30.05s
   Dec(J2000) = -33d 35' 51.6"
with an uncertainty of 5.7 arcseconds (radius, 90% containment). This
location is 41 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.58
x 10^21 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 102 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. Because of the density of
catalogued stars, further analysis is required to report an upper limit for any
afterglow in the region. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.525. 

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: GRB220715B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32406
SUBJECT: GRB 220715B: Prompt enhanced Swift-XRT position
DATE:    22/07/15 23:08:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using  promptly downlinked XRT event data for GRB 220715B, we find an
enhanced XRT position of the afterglow: RA, Dec: 254.87517, -33.59793
which is equivalent to:
   RA (J2000)  = 16 59 30.04
   Dec (J2000) = -33 35 52.5
with an uncertainty of 1.9 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/1116441.

Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).

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


GRB_name: GRB220715B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32407
SUBJECT: Swift GRB 220715B: Global MASTER-Net observations report 
DATE:    22/07/16 00:10:43 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB 220715B ( E. Troja et al., GCN 32405) errorbox  3230 sec after notice time and 3257 sec after trigger time at 2022-07-15 23:18:59 UT, with upper limit up to  15.1 mag. The observations began at zenith distance = 34 deg. The sun  altitude  is -18.7 deg. 

The galactic latitude b =  5 deg., longitude l = 351 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2032406

We obtain a following upper limits.  

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

    3347 |         MASTER-OAFA |   C |   180 | 13.0 |        
    3746 |         MASTER-OAFA |   C |   180 | 14.5 |        
    3957 |         MASTER-OAFA |   C |   180 | 14.3 |        
    4168 |         MASTER-OAFA |   C |   180 | 13.5 |        
    4379 |         MASTER-OAFA |   C |   180 | 14.8 |        
    5784 |         MASTER-OAFA |   C |   180 | 15.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220715B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32408
SUBJECT: GRB 220715B: BOOTES-network optical upper limits
DATE:    22/07/16 00:34:30 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, M. A. Castro Tirado (Univ. de Malaga), R. Fernandez-Munoz (IHSM/UMA-CSIC), M. Jelinek (ASU-CAS) and F. Rendon (IAA-CSIC and INTA-CEDEA) on behalf of a larger collaboration, report:

Following the detection of GRB 220715B by both Swift (Troja et al., GCNC 32405) and Fermi (GBM team., GCNC 32404), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva, Spain) automatically responded to this burst on Jul. 15 at 22:25:39 UT (i.e. ~57 s after trigger). In the co-added frame (30 x 10 s, clear filter), no source is detected within the enhanced XRT position (Evans et al., GCNC 32406) down to 16.1 mag.

Later on, the 0.6m BOOTES-2/TELMA robotic telescope at IHSM La Mayora (UMA-CSIC) in Algarrobo Costa (Malaga, Spain) automatically pointed to the burst position at 22:26:07 UT (i.e. ~85 s after trigger). In the co-added image (25 x 10 s, clear filter), no optical afterglow is detected within the enhanced XRT position (Evans et al., GCNC 32406) down to 18.4 mag.

We note the expected high galactic extinction towards the burst location, in the direction of the Galactic Bulge.

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


GRB_name: GRB220715B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32409
SUBJECT: GRB 220715B: Enhanced Swift-XRT position
DATE:    22/07/16 02:27:16 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 1379 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 220715B, 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 = 254.87532, -33.59775 which is equivalent
to:

RA (J2000): 16h 59m 30.08s
Dec (J2000): -33d 35' 51.9"

with an uncertainty of 2.5 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: GRB220715B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32410
SUBJECT: GRB 220715B: Swift/UVOT Upper Limits
DATE:    22/07/16 08:26:04 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) 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 220715B
103 s after the BAT trigger (Troja et al., GCN Circ. 32405).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 32409)
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           103          253          147         >20.1
u_FC               316          565          246         >20.0
white              103         1369          373         >20.4
v                  645         1419           97         >18.9
b                  571         5005          274         >20.8
u                  316         1488          319         >20.1
w1                 695         1468           78         >18.8
m2                 670         1443           97         >19.8
w2                 621         5144          227         >19.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.525 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB220715B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32411
SUBJECT: GRB 220715B: Swift-XRT refined Analysis
DATE:    22/07/16 09:05:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.4 ks of XRT data for GRB 220715B (Troja et al. GCN
Circ. 32405), from 106 s to 29.2 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. 32406).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.75 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.6 (+0.5, -0.4). The
best-fitting absorption column is  1.0 (+0.4, -0.3) x 10^22 cm^-2, in
excess of the Galactic value of 3.6 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.7 x 10^-11 (1.1 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.0 (+0.4, -0.3) x 10^22 cm^-2
Galactic foreground: 3.6 x 10^21 cm^-2
Excess significance: 3.2 sigma
Photon index:      2.6 (+0.5, -0.4)

If the light curve continues to decay with a power-law decay index of
0.75, the count rate at T+24 hours will be 4.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x
10^-13 (5.3 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/01116441.

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


GRB_name: GRB220715B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32412
SUBJECT: GRB 220715B: Fermi GBM detection
DATE:    22/07/16 23:23:20 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

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

"At 22:24:42.74 UT on 15 July 2022, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 220715B (trigger 679616687 / 220715934), which was
also detected by the Swift/BAT (E. Troja et al. 2022, GCN 32405)

The Fermi GBM Final Real-time Localization (GCN 32404) is consistent with
the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 69
degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 40 s (50-300 keV).
The time-averaged spectrum from T0-1.024 s to T0+43.008 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.09 +/- 0.23  and
the cutoff energy, parameterized as Epeak, is 118 +/- 28 keV.

The event fluence (10-1000 keV) in this time interval is
(2.2 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.8 s in the 10-1000 keV band
is 2.5 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB220714B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32413
SUBJECT: GRB220714B: UVOT detections
DATE:    22/07/18 18:49:00 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and S. Laha (NASA/UMCP) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 220714B
3628 s after the BAT trigger (Laha et al, GCN Circ. 32393) and
detected a bright afterglow (Marshall & Laha, GCN Circ. 32396).
Marshal and Laha provided the UVOT position of GRB 220714B.
Perhaps due to a bright nearby star in the field, there were some
exposures which were cut short, but in this report we include those
using the UVOT photometric system (Breeveld et al. 2011, AIP Conf.
Proc. 1358, 373):

Filter            Time        Exp(s)         Mag

white              150           55          18.0 +/- 0.1
white             3628          147          16.53+/- 0.03
v                 3810          197          16.79+/- 0.09
m2                4115          197          16.42+/- 0.08
w1                4220          197          16.41+/- 0.06
u                 4425          197          16.33+/- 0.04
b                 4630          197          17.26+/- 0.05
white             4835          197          16.86+/- 0.03
w2                4992          102          17.16+/- 0.12
v                 5897           18          17.4 +/- 0.6

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.032 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB220715B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32414
SUBJECT: GRB 220715B: Swift-BAT refined analysis
DATE:    22/07/18 20:12:06 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

A. Y. Lien (U Tampa), S. D. Barthelmy (GSFC), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC/UMBC), T. Sakamoto (AGU), M. Stamatikos (OSU),
E. Troja (NASA/GSFC/UMCP), (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 220715B (trigger #1116441)
(Troja, et al., GCN Circ. 32405).  The BAT ground-calculated position is
RA, Dec = 254.860, -33.586 deg which is
   RA(J2000)  =  16h 59m 26.5s
   Dec(J2000) = -33d 35' 10.3"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 95%.
The mask-weighted light curve shows an initial pulse with a FRED shape,
Beginning at just before T+0 and extending to about T+20.  There is a second
weaker, softer pulse centered just after T+40 sec.  There are a few gaps in the
light curve data, but none appear to correspond to burst activity.
T90 (15-350 keV) is 40.40 +- 1.24 sec (estimated error including systematics).
The time-averaged spectrum from T-0.15 to T+42.17 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.36 +- 0.11.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T-0.08 sec in the 15-150 keV band
is 1.3 +- 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/1116441/BA/


GRB_name: GRB220719A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32415
SUBJECT: GRB 220719A: Fermi GBM Final Real-time Localization
DATE:    22/07/19 14:15:59 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:05:31 UT on 19 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220719A (trigger 679932336.585264 / 220719587).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 258.6, Dec = -68.6 (J2000 degrees, equivalent to J2000 17h 14m, -68d 35'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 169.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220719587/quicklook/glg_skymap_all_bn220719587.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/bn220719587/quicklook/glg_healpix_all_bn220719587.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220719587/quicklook/glg_lc_medres34_bn220719587.gif


GRB_name: GRB220711B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32416
SUBJECT: GRB 220711B: CALET Gamma-Ray Burst Monitor detection
DATE:    22/07/19 14:35:42 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

Y. Shimizu, (Kanagawa U) 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 (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 220711B (Fermi GBM Final Real-time Localization: Fermi GBM team,
GCN Circ. 32365; Fermi GBM Detection: Lesage et al., GCN Circ 32369; 
Swift detection: D'Ai et al., GCN Circ 32366, Swift-BAT refined analysis: 
Krimm et al.,  GCN Circ 32374) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 18:16:31.192 UTC on 11 July 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1341598587/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 which starts
at T-39.5 sec, peaks at T-2.4 sec, and ends at T+93.7 sec.
The T90 and T50 durations measured by the SGM data are 82.7 +/- 3.8 sec
and 15.7 +/- 4.0 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1341598587/

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


GRB_name: GRB220715A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32417
SUBJECT: GRB 220715A: CALET Gamma-Ray Burst Monitor detection
DATE:    22/07/19 14:41:00 GMT
FROM:    Yuta Kawakubo at Louisiana State U./CALET  <kawakubo1@lsu.edu>

T. Tamura (Kanagawa U), 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 (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 220715A (Fermi GBM Final Real-time Localization: Fermi GBM team,
GCN Circ. 32399; AGILE/MCAL detection: Ursi et al., GCN Circ 32401) triggered the 
CALET Gamma-ray Burst Monitor (CGBM) at 08:49:37.333 UTC on 15 July 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1341910167/index.html).
The burst signal was seen by only SGM detector.

The burst light curve shows a weak signal which starts
at T+0.8 sec, peaks at T+3.8 sec, and ends at T+12.7 sec.
The T90 and T50 durations measured by the SGM data are 10.0 +/- 2.0 sec
and 6.0 +/- 2.0 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1341910167/

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


GRB_name: GRB220721A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32420
SUBJECT: GRB 220721A: Fermi GBM Final Real-time Localization
DATE:    22/07/21 00:41:52 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 00:30:25 UT on 21 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220721A (trigger 680056230.386204 / 220721021).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 356.6, Dec = -39.5 (J2000 degrees, equivalent to J2000 23h 46m, -39d 30'), with a statistical uncertainty of 9.1 degrees.

The angle from the Fermi LAT boresight is 25.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220721021/quicklook/glg_skymap_all_bn220721021.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/bn220721021/quicklook/glg_healpix_all_bn220721021.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220721021/quicklook/glg_lc_medres34_bn220721021.gif


GRB_name: GRB220721A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32421
SUBJECT: Fermi GRB 220721A: Global MASTER-Net observations report 
DATE:    22/07/21 01:00:47 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev
(Irkutsk State University, API),

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

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 220721A ( Fermi GBM team, GCN 32420) errorbox  360 sec after notice time and 409 sec after trigger time at 2022-07-21 00:37:15 UT, with upper limit up to  19.6 mag. The observations began at zenith distance = 29 deg. The sun  altitude  is -62.5 deg. 

The galactic latitude b = -72 deg., longitude l = 346 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2036832

We obtain a following upper limits.  

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

     440 | 2022-07-21 00:37:15 |         MASTER-SAAO | (00h 12m 27.53s , -33d 12m 32.0s) |   C |    60 | 19.5 |        
     466 | 2022-07-21 00:37:41 |             MASTER- | (00h 14m 27.09s , -30d 58m 08.1s) |   C |    60 | 17.3 |        
     520 | 2022-07-21 00:38:35 |         MASTER-SAAO | (00h 21m 56.34s , -33d 13m 09.2s) |   C |    60 | 19.6 |        
     610 | 2022-07-21 00:40:05 |         MASTER-SAAO | (00h 12m 48.29s , -35d 07m 04.3s) |   C |    60 | 19.4 |        
     690 | 2022-07-21 00:41:25 |         MASTER-SAAO | (00h 22m 30.15s , -35d 08m 07.7s) |   C |    60 | 19.5 |        
     780 | 2022-07-21 00:42:55 |         MASTER-SAAO | (00h 30m 35.98s , -33d 12m 29.3s) |   C |    60 | 19.6 |        
     989 | 2022-07-21 00:46:23 |             MASTER- | (23h 35m 25.55s , -35d 04m 35.1s) |   C |    60 | 16.0 |        
     989 | 2022-07-21 00:46:24 |             MASTER- | (23h 25m 57.69s , -34d 56m 37.5s) |   C |    60 | 16.3 |        
    1122 | 2022-07-21 00:48:37 |             MASTER- | (23h 58m 00.11s , -33d 05m 39.6s) |   C |    60 | 15.3 |        
    1122 | 2022-07-21 00:48:37 |             MASTER- | (23h 48m 44.79s , -32d 57m 41.4s) |   C |    60 | 15.9 |        
    1151 | 2022-07-21 00:49:06 |         MASTER-SAAO | (23h 35m 37.49s , -38d 53m 31.0s) |   C |    60 | 19.5 |        
    1199 | 2022-07-21 00:49:54 |             MASTER- | (23h 40m 23.19s , -33d 10m 30.2s) |   C |    60 | 16.2 |        
    1199 | 2022-07-21 00:49:54 |             MASTER- | (23h 31m 07.63s , -33d 02m 31.0s) |   C |    60 | 16.5 |        
    1280 | 2022-07-21 00:51:15 |             MASTER- | (23h 46m 29.29s , -31d 16m 47.4s) |   C |    60 | 16.2 |        
    1280 | 2022-07-21 00:51:15 |             MASTER- | (23h 37m 24.93s , -31d 08m 47.3s) |   C |    60 | 16.6 |        
    1547 | 2022-07-21 00:55:42 |         MASTER-SAAO | (00h 12m 25.62s , -33d 13m 54.3s) |   C |    60 | 19.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220715B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32422
SUBJECT: GRB 220715B: VIRT Optical Upper Limit
DATE:    22/07/24 02:17:46 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

K. Noonan (UVI), P. Gokuldass (Florida Institute of Technology), N. Orange
(OrangeWave Innovative Science, LLC), K. Smith (UVI), R. Querrard (UVI), D.
Morris (UVI) report:

We observed the field of GRB220715B (Fermi GRB team, GCN 32404; and Troja
et al., GCN 32405) with the 0.5m Virgin Island Robotic Telescope (VIRT) at
the University of the Virgin Islands' Etelman Observatory on 07-16-2022
starting at 00:06:54 UT (T+1.7 hrs). We performed a series of exposures in
the R filter with a total exposure of 3910 s. The weather conditions were
partly cloudy during the hours of observation with an average airmass of
1.6.

We detect no new source within the enhanced XRT position error circle
(Evans et al., GCNC 32406), consistent with other non-detections (Lipunov
et al. GCN 32407, Hu et al, GCN 33408; and Kuin et al., GCN 32410) and
report the following 5-sigma upper limit:

T_mid            ||Exposure     ||Filter      ||Limit

T+ 3.1  hrs     ||3910s          ||R            ||>19.1

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 80NSSC19M0060, and NSF EiR award 1901296.This message can
be cited.


GRB_name: GRB220724A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32423
SUBJECT: GRB 220724A: Fermi GBM Final Real-time Localization
DATE:    22/07/24 23:53:28 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 23:43:03 UT on 24 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220724A (trigger 680398988.456506 / 220724988).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 238.5, Dec = -19.2 (J2000 degrees, equivalent to J2000 15h 54m, -19d 11'), with a statistical uncertainty of 8.0 degrees.

The angle from the Fermi LAT boresight is 86.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220724988/quicklook/glg_skymap_all_bn220724988.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/bn220724988/quicklook/glg_healpix_all_bn220724988.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220724988/quicklook/glg_lc_medres34_bn220724988.gif


GRB_name: GRB220724A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32424
SUBJECT: Fermi GRB 220724A: Global MASTER-Net observations report 
DATE:    22/07/25 05:30:21 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, D. Vlasenko, 
G.Antipov, D.Zimnukhov, V.Senik, 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-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 220724A ( Fermi GBM team, GCN 32423) errorbox  16981 sec after notice time and 17018 sec after trigger time at 2022-07-25 04:26:41 UT, with upper limit up to  17.9 mag. The observations began at zenith distance = 58 deg. The sun  altitude  is -78.3 deg. 

The galactic latitude b = 28 deg., longitude l = 352 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2040301

We obtain a following upper limits.  

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

   17108 | 2022-07-25 04:26:41 |         MASTER-OAFA | (15h 46m 13.07s , -19d 21m 40.3s) |   C |   180 | 17.6 |        
   17742 | 2022-07-25 04:37:15 |         MASTER-OAFA | (15h 46m 12.83s , -19d 19m 22.9s) |   C |   180 | 17.9 |        
   17987 | 2022-07-25 04:42:20 |         MASTER-OAFA | (15h 55m 41.17s , -22d 23m 42.3s) |   C |    60 | 16.7 |        
   18078 | 2022-07-25 04:43:51 |         MASTER-OAFA | (15h 52m 36.37s , -14d 42m 48.9s) |   C |    60 | 17.1 |        
   18445 | 2022-07-25 04:49:58 |         MASTER-OAFA | (15h 36m 33.55s , -15d 43m 53.3s) |   C |    60 | 17.6 |        
   18811 | 2022-07-25 04:56:04 |         MASTER-OAFA | (15h 47m 09.28s , -20d 53m 04.9s) |   C |    60 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB220726A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32426
SUBJECT: GRB 220726A: Fermi GBM Final Real-time Localization
DATE:    22/07/26 09:53:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 09:42:47 UT on 26 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220726A (trigger 680521372.015932 / 220726405).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 196.9, Dec = -61.8 (J2000 degrees, equivalent to J2000 13h 07m, -61d 47'), with a statistical uncertainty of 5.3 degrees.

The angle from the Fermi LAT boresight is 54.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220726405/quicklook/glg_skymap_all_bn220726405.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/bn220726405/quicklook/glg_healpix_all_bn220726405.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220726405/quicklook/glg_lc_medres34_bn220726405.gif


GRB_name: GRB220728A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32427
SUBJECT: GRB 220728A: Fermi GBM Final Real-time Localization
DATE:    22/07/28 16:30:57 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 16:20:39 UT on 28 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220728A (trigger 680718044.343708 / 220728681).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 5.4, Dec = 36.2 (J2000 degrees, equivalent to J2000 00h 21m, 36d 12'), with a statistical uncertainty of 15.2 degrees.

The angle from the Fermi LAT boresight is 77.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220728681/quicklook/glg_skymap_all_bn220728681.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/bn220728681/quicklook/glg_healpix_all_bn220728681.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220728681/quicklook/glg_lc_medres34_bn220728681.gif


GRB_name: GRB220728A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  32429
SUBJECT: Fermi GRB 220728A: Global MASTER-Net observations report 
DATE:    22/07/29 00:45:18 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

R. Podesta, C.Lopez, F. Podesta, C.Francile 
(Observatorio Astronomico Felix Aguilar OAFA),

R. Rebolo, M. Serra 
(The Instituto de Astrofisica de Canarias),

D. Buckley 
(South African Astronomical Observatory),

O.A. Gres, N.M. Budnev
(Irkutsk State University, API),

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

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

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


MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 220728A ( Fermi GBM team, GCN 32427) errorbox  20937 sec after notice time and 20969 sec after trigger time at 2022-07-28 22:10:09 UT, with upper limit up to  18.2 mag. The observations began at zenith distance = 77 deg. The sun  altitude  is -74.7 deg. 

The galactic latitude b = -26 deg., longitude l = 117 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=2043520

We obtain a following upper limits.  

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

    7539 | 2022-07-28 18:25:48 |             MASTER- | (00h 10m 58.27s , +39d 20m 52.3s) |   C |    60 | 16.8 |        
    7540 | 2022-07-28 18:25:48 |             MASTER- | (00h 20m 54.46s , +39d 13m 29.2s) |   C |    60 | 16.7 |        
    7615 | 2022-07-28 18:27:04 |             MASTER- | (00h 11m 25.61s , +41d 13m 52.5s) |   C |    60 | 17.0 |        
    7615 | 2022-07-28 18:27:04 |             MASTER- | (00h 21m 38.47s , +41d 06m 32.5s) |   C |    60 | 16.9 |        
    7691 | 2022-07-28 18:28:19 |             MASTER- | (00h 10m 39.36s , +37d 24m 41.9s) |   C |    60 | 16.9 |        
    7691 | 2022-07-28 18:28:19 |             MASTER- | (00h 20m 19.84s , +37d 17m 14.7s) |   C |    60 | 16.9 |        
    7828 | 2022-07-28 18:30:37 |             MASTER- | (00h 30m 35.03s , +39d 20m 44.9s) |   C |    60 | 17.2 |        
    7828 | 2022-07-28 18:30:37 |             MASTER- | (00h 40m 29.87s , +39d 13m 30.2s) |   C |    60 | 17.0 |        
    7903 | 2022-07-28 18:31:52 |             MASTER- | (00h 11m 48.68s , +43d 07m 36.0s) |   C |    60 | 17.2 |        
    7903 | 2022-07-28 18:31:52 |             MASTER- | (00h 22m 18.93s , +43d 00m 29.1s) |   C |    60 | 17.6 |        
    8037 | 2022-07-28 18:34:06 |             MASTER- | (00h 29m 46.66s , +37d 26m 36.9s) |   C |    60 | 17.2 |        
    8037 | 2022-07-28 18:34:06 |             MASTER- | (00h 39m 26.17s , +37d 19m 17.1s) |   C |    60 | 17.0 |        
    8112 | 2022-07-28 18:35:21 |             MASTER- | (00h 31m 33.88s , +41d 13m 43.2s) |   C |    60 | 17.6 |        
    8112 | 2022-07-28 18:35:21 |             MASTER- | (00h 41m 45.65s , +41d 06m 31.9s) |   C |    60 | 17.4 |        
    8249 | 2022-07-28 18:37:37 |             MASTER- | (00h 10m 25.16s , +35d 32m 18.0s) |   C |    60 | 17.4 |        
    8249 | 2022-07-28 18:37:38 |             MASTER- | (00h 19m 50.50s , +35d 24m 59.5s) |   C |    60 | 17.1 |        
    8324 | 2022-07-28 18:38:53 |             MASTER- | (23h 51m 31.92s , +39d 19m 25.6s) |   C |    60 | 17.8 |        
    8325 | 2022-07-28 18:38:53 |             MASTER- | (00h 01m 26.76s , +39d 12m 14.2s) |   C |    60 | 17.0 |        
    8459 | 2022-07-28 18:41:08 |             MASTER- | (00h 11m 00.52s , +39d 20m 27.4s) |   C |    60 | 17.7 |        
    8460 | 2022-07-28 18:41:08 |             MASTER- | (00h 20m 55.46s , +39d 13m 16.9s) |   C |    60 | 17.6 |        
    8534 | 2022-07-28 18:42:23 |             MASTER- | (00h 11m 26.42s , +41d 13m 29.9s) |   C |    60 | 17.8 |        
    8534 | 2022-07-28 18:42:23 |             MASTER- | (00h 21m 38.23s , +41d 06m 21.2s) |   C |    60 | 17.7 |        
    8670 | 2022-07-28 18:44:39 |             MASTER- | (00h 10m 42.34s , +37d 26m 22.0s) |   C |    60 | 17.7 |        
    8670 | 2022-07-28 18:44:39 |             MASTER- | (00h 20m 21.82s , +37d 19m 08.4s) |   C |    60 | 17.4 |        
    8745 | 2022-07-28 18:45:54 |             MASTER- | (00h 30m 40.99s , +39d 19m 33.2s) |   C |    60 | 17.9 |        
    8745 | 2022-07-28 18:45:54 |             MASTER- | (00h 40m 35.87s , +39d 12m 22.0s) |   C |    60 | 17.8 |        
    9036 | 2022-07-28 18:50:45 |             MASTER- | (00h 11m 43.68s , +43d 08m 28.6s) |   C |    60 | 17.8 |        
    9036 | 2022-07-28 18:50:45 |             MASTER- | (00h 22m 14.50s , +43d 01m 23.5s) |   C |    60 | 17.9 |        
    9112 | 2022-07-28 18:52:01 |             MASTER- | (00h 29m 52.43s , +37d 25m 26.0s) |   C |    60 | 17.8 |        
    9112 | 2022-07-28 18:52:01 |             MASTER- | (00h 39m 31.84s , +37d 18m 12.5s) |   C |    60 | 17.6 |        
    9247 | 2022-07-28 18:54:15 |             MASTER- | (00h 31m 29.14s , +41d 14m 33.0s) |   C |    60 | 18.0 |        
    9247 | 2022-07-28 18:54:15 |             MASTER- | (00h 41m 41.15s , +41d 07m 26.7s) |   C |    60 | 17.6 |        
    9322 | 2022-07-28 18:55:31 |             MASTER- | (00h 10m 29.64s , +35d 31m 13.4s) |   C |    60 | 17.8 |        
    9322 | 2022-07-28 18:55:31 |             MASTER- | (00h 19m 54.98s , +35d 23m 59.1s) |   C |    60 | 17.3 |        
    9452 | 2022-07-28 18:57:41 |             MASTER- | (00h 11m 03.49s , +35d 31m 13.5s) |   C |    60 | 17.8 |        
    9452 | 2022-07-28 18:57:41 |             MASTER- | (00h 20m 28.75s , +35d 23m 59.4s) |   C |    60 | 17.3 |        
    9528 | 2022-07-28 18:58:57 |             MASTER- | (00h 11m 05.18s , +39d 19m 23.5s) |   C |    60 | 18.0 |        
    9528 | 2022-07-28 18:58:57 |             MASTER- | (00h 21m 00.19s , +39d 12m 14.4s) |   C |    60 | 17.7 |        
    9658 | 2022-07-28 19:01:06 |             MASTER- | (00h 11m 19.85s , +41d 14m 26.8s) |   C |    60 | 18.1 |        
    9658 | 2022-07-28 19:01:07 |             MASTER- | (00h 21m 32.00s , +41d 07m 18.9s) |   C |    60 | 17.9 |        
    9732 | 2022-07-28 19:02:21 |             MASTER- | (00h 20m 27.75s , +37d 18m 07.3s) |   C |    60 | 17.7 |        
    9940 | 2022-07-28 19:05:48 |             MASTER- | (00h 11m 41.90s , +43d 08m 28.1s) |   C |    60 | 18.1 |        
   10015 | 2022-07-28 19:07:04 |             MASTER- | (00h 29m 51.93s , +37d 25m 23.0s) |   C |    60 | 18.0 |        
   10015 | 2022-07-28 19:07:04 |             MASTER- | (00h 39m 31.42s , +37d 18m 10.7s) |   C |    60 | 17.2 |        
   10151 | 2022-07-28 19:09:19 |             MASTER- | (00h 31m 27.98s , +41d 14m 30.5s) |   C |    60 | 18.3 |        
   10151 | 2022-07-28 19:09:19 |             MASTER- | (00h 41m 40.06s , +41d 07m 24.1s) |   C |    60 | 14.5 |        
   10226 | 2022-07-28 19:10:35 |             MASTER- | (00h 10m 30.46s , +35d 31m 13.5s) |   C |    60 | 18.0 |        
   10226 | 2022-07-28 19:10:35 |             MASTER- | (00h 19m 56.04s , +35d 24m 01.0s) |   C |    60 | 17.2 |        
   10356 | 2022-07-28 19:12:44 |             MASTER- | (00h 11m 04.27s , +35d 31m 14.4s) |   C |    60 | 18.0 |        
   10356 | 2022-07-28 19:12:45 |             MASTER- | (00h 20m 29.90s , +35d 24m 01.6s) |   C |    60 | 17.4 |        
   10432 | 2022-07-28 19:14:01 |             MASTER- | (00h 01m 29.34s , +41d 06m 22.2s) |   C |    60 | 12.4 |        
   10561 | 2022-07-28 19:16:10 |             MASTER- | (00h 12m 06.53s , +45d 02m 32.5s) |   C |    60 | 17.9 |        
   10637 | 2022-07-28 19:17:25 |             MASTER- | (00h 32m 34.22s , +43d 07m 33.2s) |   C |    60 | 16.3 |        
   10637 | 2022-07-28 19:17:25 |             MASTER- | (00h 43m 05.09s , +43d 00m 29.3s) |   C |    60 | 12.1 |        
   10774 | 2022-07-28 19:19:43 |             MASTER- | (00h 29m 00.82s , +35d 32m 16.7s) |   C |    60 | 18.1 |        
   10774 | 2022-07-28 19:19:43 |             MASTER- | (00h 38m 26.52s , +35d 25m 04.6s) |   C |    60 | 17.2 |        
   10851 | 2022-07-28 19:21:00 |             MASTER- | (23h 51m 40.81s , +37d 25m 26.6s) |   C |    60 | 18.1 |        
   10978 | 2022-07-28 19:23:06 |             MASTER- | (23h 52m 14.50s , +37d 25m 26.7s) |   C |    60 | 18.0 |        
   11055 | 2022-07-28 19:24:24 |             MASTER- | (00h 10m 14.12s , +33d 37m 11.5s) |   C |    60 | 14.0 |        
   11055 | 2022-07-28 19:24:24 |             MASTER- | (00h 19m 27.28s , +33d 29m 58.5s) |   C |    60 | 16.8 |        
   11125 | 2022-07-28 19:25:34 |             MASTER- | (00h 10m 14.06s , +33d 37m 11.2s) |   C |    60 | 18.0 |        
   11125 | 2022-07-28 19:25:34 |             MASTER- | (00h 19m 27.20s , +33d 29m 58.5s) |   C |    60 | 16.5 |        
   11266 | 2022-07-28 19:27:55 |             MASTER- | (23h 43m 13.20s , +39d 20m 36.0s) |   C |    60 | 18.3 |        
   11266 | 2022-07-28 19:27:55 |             MASTER- | (23h 53m 09.46s , +39d 13m 24.7s) |   C |    60 | 12.6 |        
   11477 | 2022-07-28 19:31:25 |             MASTER- | (00h 12m 04.74s , +45d 02m 35.6s) |   C |    60 | 12.4 |        
   11553 | 2022-07-28 19:32:42 |             MASTER- | (00h 32m 33.49s , +43d 07m 35.4s) |   C |    60 | 14.0 |        
   11553 | 2022-07-28 19:32:42 |             MASTER- | (00h 43m 04.80s , +43d 00m 29.4s) |   C |    60 | 14.2 |        
   11686 | 2022-07-28 19:34:55 |             MASTER- | (00h 29m 00.49s , +35d 32m 19.4s) |   C |    60 | 18.0 |        
   11686 | 2022-07-28 19:34:55 |             MASTER- | (00h 38m 26.53s , +35d 25m 07.7s) |   C |    60 | 17.2 |        
   11763 | 2022-07-28 19:36:12 |             MASTER- | (23h 51m 40.58s , +37d 25m 31.7s) |   C |    60 | 18.2 |        
   11891 | 2022-07-28 19:38:20 |             MASTER- | (23h 52m 12.59s , +37d 25m 32.9s) |   C |    60 | 18.2 |        
   11967 | 2022-07-28 19:39:36 |             MASTER- | (00h 10m 13.23s , +33d 37m 17.8s) |   C |    60 | 18.1 |        
   11967 | 2022-07-28 19:39:36 |             MASTER- | (00h 19m 26.53s , +33d 30m 03.7s) |   C |    60 | 16.9 |        
   12091 | 2022-07-28 19:41:40 |             MASTER- | (00h 10m 45.47s , +33d 37m 18.9s) |   C |    60 | 18.2 |        
   12091 | 2022-07-28 19:41:40 |             MASTER- | (00h 19m 58.78s , +33d 30m 05.4s) |   C |    60 | 15.3 |        
   12292 | 2022-07-28 19:45:01 |             MASTER- | (23h 43m 50.27s , +39d 19m 42.8s) |   C |    60 | 18.4 |        
   12367 | 2022-07-28 19:46:16 |             MASTER- | (23h 53m 35.00s , +41d 06m 37.1s) |   C |    60 | 14.1 |        
   12498 | 2022-07-28 19:48:27 |             MASTER- | (00h 12m 03.57s , +45d 02m 40.1s) |   C |    60 | 12.4 |        
   12574 | 2022-07-28 19:49:43 |             MASTER- | (00h 32m 32.56s , +43d 07m 38.4s) |   C |    60 | 13.1 |        
   12574 | 2022-07-28 19:49:43 |             MASTER- | (00h 43m 04.03s , +43d 00m 33.1s) |   C |    60 | 14.1 |        
   12707 | 2022-07-28 19:51:56 |             MASTER- | (00h 29m 01.26s , +35d 32m 25.3s) |   C |    60 | 18.2 |        
   12784 | 2022-07-28 19:53:12 |             MASTER- | (23h 51m 39.00s , +37d 25m 40.1s) |   C |    60 | 18.5 |        
   12911 | 2022-07-28 19:55:20 |             MASTER- | (23h 52m 12.76s , +37d 25m 40.8s) |   C |    60 | 18.4 |        
   12987 | 2022-07-28 19:56:36 |             MASTER- | (00h 10m 11.84s , +33d 37m 25.8s) |   C |    60 | 18.2 |        
   13112 | 2022-07-28 19:58:41 |             MASTER- | (00h 10m 44.83s , +33d 37m 26.9s) |   C |    60 | 18.2 |        
   13188 | 2022-07-28 19:59:57 |             MASTER- | (23h 43m 15.37s , +39d 19m 49.3s) |   C |    60 | 12.4 |        
   13318 | 2022-07-28 20:02:07 |             MASTER- | (23h 43m 14.14s , +41d 14m 53.2s) |   C |    60 | 18.4 |        
   13394 | 2022-07-28 20:03:23 |             MASTER- | (00h 33m 35.37s , +45d 01m 42.1s) |   C |    60 | 18.8 |        
   13530 | 2022-07-28 20:05:38 |             MASTER- | (00h 50m 09.30s , +39d 20m 37.8s) |   C |    60 | 18.3 |        
   13530 | 2022-07-28 20:05:38 |             MASTER- | (01h 00m 05.30s , +39d 13m 31.8s) |   C |    60 | 15.9 |        
   13608 | 2022-07-28 20:06:57 |             MASTER- | (23h 44m 42.69s , +37d 25m 52.5s) |   C |    60 | 13.2 |        
   13734 | 2022-07-28 20:09:03 |             MASTER- | (23h 45m 16.52s , +37d 25m 53.0s) |   C |    60 | 12.6 |        
   13734 | 2022-07-28 20:09:03 |             MASTER- | (23h 54m 57.66s , +37d 18m 41.2s) |   C |    60 | 13.8 |        
   13809 | 2022-07-28 20:10:18 |             MASTER- | (23h 55m 33.03s , +43d 00m 50.1s) |   C |    60 | 14.0 |        
   13936 | 2022-07-28 20:12:25 |             MASTER- | (23h 45m 35.46s , +43d 07m 59.4s) |   C |    60 | 18.2 |        
   13936 | 2022-07-28 20:12:25 |             MASTER- | (23h 56m 07.94s , +43d 00m 49.9s) |   C |    60 | 13.9 |        
   14013 | 2022-07-28 20:13:42 |             MASTER- | (00h 28m 25.33s , +33d 37m 29.0s) |   C |    60 | 18.1 |        
   14220 | 2022-07-28 20:17:08 |             MASTER- | (23h 53m 31.84s , +41d 06m 52.7s) |   C |    60 | 14.3 |        
   14431 | 2022-07-28 20:20:39 |             MASTER- | (00h 48m 55.63s , +37d 25m 39.2s) |   C |    60 | 18.3 |        
   14431 | 2022-07-28 20:20:39 |             MASTER- | (00h 58m 36.10s , +37d 18m 31.0s) |   C |    60 | 16.9 |        
   14562 | 2022-07-28 20:22:51 |             MASTER- | (00h 50m 07.34s , +39d 20m 41.7s) |   C |    60 | 18.6 |        
   14640 | 2022-07-28 20:24:09 |             MASTER- | (23h 44m 42.33s , +37d 26m 00.2s) |   C |    60 | 12.8 |        
   14640 | 2022-07-28 20:24:09 |             MASTER- | (23h 54m 23.58s , +37d 18m 49.3s) |   C |    60 | 14.3 |        
   14760 | 2022-07-28 20:26:09 |             MASTER- | (23h 45m 14.78s , +37d 26m 00.8s) |   C |    60 | 18.2 |        
   14836 | 2022-07-28 20:27:25 |             MASTER- | (23h 44m 58.05s , +43d 08m 04.9s) |   C |    60 | 18.5 |        
   14961 | 2022-07-28 20:29:30 |             MASTER- | (23h 45m 31.51s , +43d 08m 06.1s) |   C |    60 | 18.4 |        
   14961 | 2022-07-28 20:29:30 |             MASTER- | (23h 56m 04.25s , +43d 00m 58.2s) |   C |    60 | 14.9 |        
   15038 | 2022-07-28 20:30:47 |             MASTER- | (00h 28m 23.66s , +33d 37m 37.5s) |   C |    60 | 18.3 |        
   15247 | 2022-07-28 20:34:16 |             MASTER- | (00h 47m 41.25s , +35d 31m 39.2s) |   C |    60 | 18.6 |        
   15457 | 2022-07-28 20:37:46 |             MASTER- | (00h 48m 52.86s , +37d 25m 44.9s) |   C |    60 | 18.4 |        
   15664 | 2022-07-28 20:41:12 |             MASTER- | (23h 44m 34.13s , +37d 27m 09.2s) |   C |    60 | 18.7 |        
   15664 | 2022-07-28 20:41:12 |             MASTER- | (23h 54m 15.90s , +37d 19m 57.4s) |   C |    60 | 14.4 |        
   15740 | 2022-07-28 20:42:28 |             MASTER- | (00h 01m 29.49s , +44d 55m 02.5s) |   C |    60 | 13.9 |        
   15872 | 2022-07-28 20:44:40 |             MASTER- | (23h 44m 49.20s , +43d 09m 13.2s) |   C |    60 | 18.6 |        
   15872 | 2022-07-28 20:44:40 |             MASTER- | (23h 55m 22.64s , +43d 02m 04.2s) |   C |    60 | 13.9 |        
   15948 | 2022-07-28 20:45:57 |             MASTER- | (23h 51m 53.45s , +33d 38m 06.4s) |   C |    60 | 18.7 |        
   16164 | 2022-07-28 20:49:33 |             MASTER- | (00h 28m 14.80s , +33d 38m 49.1s) |   C |    60 | 18.6 |        
   16241 | 2022-07-28 20:50:50 |             MASTER- | (00h 12m 30.43s , +46d 56m 05.8s) |   C |    60 | 12.5 |        
   16241 | 2022-07-28 20:50:50 |             MASTER- | (00h 23m 47.01s , +46d 49m 01.7s) |   C |    60 | 14.0 |        
   16375 | 2022-07-28 20:53:04 |             MASTER- | (00h 47m 34.73s , +35d 32m 49.7s) |   C |    60 | 18.7 |        
   16449 | 2022-07-28 20:54:18 |             MASTER- | (00h 48m 52.18s , +37d 25m 52.6s) |   C |    60 | 18.3 |        
   16597 | 2022-07-28 20:56:46 |             MASTER- | (23h 56m 55.60s , +35d 26m 02.9s) |   C |    60 | 14.7 |        
   16759 | 2022-07-28 20:59:28 |             MASTER- | (23h 48m 11.26s , +45d 01m 17.8s) |   C |    60 | 18.5 |        
   16759 | 2022-07-28 20:59:28 |             MASTER- | (23h 59m 05.41s , +44d 54m 10.9s) |   C |    60 | 14.5 |        
   17043 | 2022-07-28 21:04:12 |             MASTER- | (00h 09m 51.76s , +31d 44m 06.4s) |   C |    60 | 18.5 |        
   17043 | 2022-07-28 21:04:12 |             MASTER- | (00h 18m 54.89s , +31d 36m 53.4s) |   C |    60 | 14.2 |        
   17229 | 2022-07-28 21:07:18 |             MASTER- | (00h 27m 37.30s , +31d 44m 57.3s) |   C |    60 | 18.4 |        
   17229 | 2022-07-28 21:07:18 |             MASTER- | (00h 36m 40.36s , +31d 37m 48.1s) |   C |    60 | 13.7 |        
   17305 | 2022-07-28 21:08:34 |             MASTER- | (00h 47m 38.57s , +35d 31m 54.8s) |   C |    60 | 18.9 |        
   17440 | 2022-07-28 21:10:49 |             MASTER- | (00h 34m 33.11s , +46d 57m 06.3s) |   C |    60 | 19.1 |        
   17440 | 2022-07-28 21:10:49 |             MASTER- | (00h 45m 50.01s , +46d 50m 06.9s) |   C |    60 | 14.0 |        
   17518 | 2022-07-28 21:12:07 |             MASTER- | (23h 47m 31.47s , +35d 32m 20.8s) |   C |    60 | 18.9 |        
   17518 | 2022-07-28 21:12:07 |             MASTER- | (23h 56m 59.66s , +35d 25m 09.0s) |   C |    60 | 14.0 |        
   17645 | 2022-07-28 21:14:14 |             MASTER- | (23h 48m 04.44s , +35d 32m 21.3s) |   C |    60 | 18.9 |        
   17721 | 2022-07-28 21:15:30 |             MASTER- | (23h 48m 15.75s , +45d 02m 19.2s) |   C |    60 | 18.6 |        
   17721 | 2022-07-28 21:15:30 |             MASTER- | (23h 59m 10.42s , +44d 55m 14.5s) |   C |    60 | 14.0 |        
   17854 | 2022-07-28 21:17:43 |             MASTER- | (00h 51m 27.96s , +41d 15m 05.5s) |   C |    60 | 12.3 |        
   18064 | 2022-07-28 21:21:13 |             MASTER- | (00h 09m 43.36s , +31d 45m 14.3s) |   C |    60 | 18.5 |        
   18064 | 2022-07-28 21:21:13 |             MASTER- | (00h 18m 46.73s , +31d 38m 03.7s) |   C |    60 | 13.8 |        
   18140 | 2022-07-28 21:22:29 |             MASTER- | (00h 27m 41.30s , +31d 44m 05.7s) |   C |    60 | 13.8 |        
   18352 | 2022-07-28 21:26:01 |             MASTER- | (00h 34m 37.09s , +46d 56m 13.3s) |   C |    60 | 19.1 |        
   18487 | 2022-07-28 21:28:16 |             MASTER- | (23h 56m 53.26s , +35d 26m 17.3s) |   C |    60 | 14.0 |        
   18564 | 2022-07-28 21:29:33 |             MASTER- | (00h 01m 30.53s , +46d 49m 19.7s) |   C |    60 | 14.2 |        
   18773 | 2022-07-28 21:33:01 |             MASTER- | (00h 51m 33.50s , +41d 14m 15.9s) |   C |    60 | 18.6 |        
   18906 | 2022-07-28 21:35:15 |             MASTER- | (00h 53m 01.38s , +43d 09m 15.6s) |   C |    60 | 12.3 |        
   18983 | 2022-07-28 21:36:32 |             MASTER- | (00h 09m 49.37s , +31d 44m 25.2s) |   C |    60 | 18.5 |        
   18983 | 2022-07-28 21:36:32 |             MASTER- | (00h 18m 53.07s , +31d 37m 12.9s) |   C |    60 | 13.9 |        
   19119 | 2022-07-28 21:38:48 |             MASTER- | (00h 27m 32.84s , +31d 45m 17.6s) |   C |    60 | 13.7 |        
   19119 | 2022-07-28 21:38:48 |             MASTER- | (00h 36m 36.54s , +31d 38m 07.9s) |   C |    60 | 13.9 |        
   19330 | 2022-07-28 21:42:19 |             MASTER- | (00h 34m 27.64s , +46d 57m 20.7s) |   C |    60 | 19.1 |        
   19330 | 2022-07-28 21:42:19 |             MASTER- | (00h 45m 45.62s , +46d 50m 21.1s) |   C |    60 | 14.2 |        
   19408 | 2022-07-28 21:43:36 |             MASTER- | (23h 51m 56.14s , +31d 44m 35.4s) |   C |    60 | 18.7 |        
   19408 | 2022-07-28 21:43:36 |             MASTER- | (00h 01m 00.34s , +31d 37m 22.4s) |   C |    60 | 14.2 |        
   19543 | 2022-07-28 21:45:52 |             MASTER- | (00h 46m 24.29s , +33d 39m 16.3s) |   C |    60 | 12.5 |        
   19620 | 2022-07-28 21:47:09 |             MASTER- | (00h 09m 35.34s , +29d 50m 28.2s) |   C |    60 | 18.6 |        
   19620 | 2022-07-28 21:47:09 |             MASTER- | (00h 18m 28.59s , +29d 43m 17.0s) |   C |    60 | 13.7 |        
   19807 | 2022-07-28 21:50:16 |             MASTER- | (00h 26m 59.87s , +29d 51m 22.0s) |   C |    60 | 18.6 |        
   19807 | 2022-07-28 21:50:16 |             MASTER- | (00h 35m 53.13s , +29d 44m 12.2s) |   C |    60 | 14.2 |        
   19883 | 2022-07-28 21:51:31 |             MASTER- | (00h 45m 29.23s , +31d 44m 16.6s) |   C |    60 | 18.6 |        
   19883 | 2022-07-28 21:51:32 |             MASTER- | (00h 54m 32.94s , +31d 37m 08.3s) |   C |    60 | 13.8 |        
   20097 | 2022-07-28 21:55:06 |             MASTER- | (00h 24m 33.17s , +48d 43m 24.9s) |   C |    60 | 14.1 |        
   20424 | 2022-07-28 22:00:33 |             MASTER- | (23h 23m 27.15s , +41d 14m 43.3s) |   C |    60 | 12.8 |        
   20503 | 2022-07-28 22:01:52 |             MASTER- | (00h 46m 26.85s , +33d 38m 27.7s) |   C |    60 | 12.3 |        
   20503 | 2022-07-28 22:01:52 |             MASTER- | (00h 55m 43.18s , +33d 31m 19.6s) |   C |    60 | 14.1 |        
   20579 | 2022-07-28 22:03:08 |             MASTER- | (00h 09m 28.15s , +29d 49m 38.5s) |   C |    60 | 18.5 |        
   20579 | 2022-07-28 22:03:08 |             MASTER- | (00h 18m 22.26s , +29d 42m 25.5s) |   C |    60 | 13.7 |        
   20711 | 2022-07-28 22:05:20 |             MASTER- | (00h 26m 56.72s , +29d 51m 33.2s) |   C |    60 | 18.7 |        
   20711 | 2022-07-28 22:05:20 |             MASTER- | (00h 35m 50.74s , +29d 44m 21.3s) |   C |    60 | 14.4 |        
   20786 | 2022-07-28 22:06:35 |             MASTER- | (00h 45m 27.75s , +31d 44m 28.1s) |   C |    60 | 18.6 |        
   20786 | 2022-07-28 22:06:35 |             MASTER- | (00h 54m 32.21s , +31d 37m 18.9s) |   C |    60 | 14.1 |        
   21000 | 2022-07-28 22:10:09 |         MASTER-SAAO | (23h 23m 16.11s , +27d 32m 56.4s) |   C |    60 | 17.5 |        
   21003 | 2022-07-28 22:10:12 |             MASTER- | (01h 05m 42.99s , +44d 55m 29.7s) |   C |    60 | 14.2 |        
   21080 | 2022-07-28 22:11:28 |         MASTER-SAAO | (23h 32m 11.68s , +27d 32m 06.7s) |   C |    60 | 17.5 |        
   21127 | 2022-07-28 22:12:16 |             MASTER- | (00h 55m 19.35s , +45d 02m 31.8s) |   C |    60 | 19.3 |        
   21127 | 2022-07-28 22:12:16 |             MASTER- | (01h 06m 15.30s , +44d 55m 29.6s) |   C |    60 | 14.0 |        
   21176 | 2022-07-28 22:13:05 |         MASTER-SAAO | (23h 14m 05.40s , +29d 26m 18.8s) |   C |    60 | 17.8 |        
   21206 | 2022-07-28 22:13:35 |             MASTER- | (23h 33m 10.08s , +41d 07m 27.4s) |   C |    60 | 14.1 |        
   21256 | 2022-07-28 22:14:24 |         MASTER-SAAO | (23h 23m 09.49s , +29d 25m 13.9s) |   C |    60 | 17.8 |        
   21329 | 2022-07-28 22:15:37 |             MASTER- | (23h 23m 25.61s , +41d 14m 39.6s) |   C |    60 | 12.1 |        
   21329 | 2022-07-28 22:15:37 |             MASTER- | (23h 33m 43.27s , +41d 07m 27.7s) |   C |    60 | 14.2 |        
   21406 | 2022-07-28 22:16:55 |             MASTER- | (00h 46m 26.31s , +33d 38m 35.4s) |   C |    60 | 13.8 |        
   21406 | 2022-07-28 22:16:55 |             MASTER- | (00h 55m 42.96s , +33d 31m 26.5s) |   C |    60 | 14.0 |        
   21439 | 2022-07-28 22:17:27 |         MASTER-SAAO | (23h 25m 37.64s , +25d 37m 45.3s) |   C |    60 | 18.1 |        
   21518 | 2022-07-28 22:18:47 |         MASTER-SAAO | (23h 31m 25.72s , +29d 26m 12.6s) |   C |    60 | 17.5 |        
   21536 | 2022-07-28 22:19:05 |             MASTER- | (00h 09m 25.37s , +29d 51m 43.1s) |   C |    60 | 18.6 |        
   21536 | 2022-07-28 22:19:05 |             MASTER- | (00h 18m 19.98s , +29d 44m 30.0s) |   C |    60 | 14.1 |        
   21608 | 2022-07-28 22:20:17 |         MASTER-SAAO | (23h 40m 37.57s , +29d 27m 07.2s) |   C |    60 | 17.3 |        
   21613 | 2022-07-28 22:20:21 |             MASTER- | (00h 27m 01.85s , +29d 50m 39.4s) |   C |    60 | 18.8 |        
   21613 | 2022-07-28 22:20:21 |             MASTER- | (00h 35m 56.16s , +29d 43m 27.5s) |   C |    60 | 15.0 |        
   21688 | 2022-07-28 22:21:37 |         MASTER-SAAO | (23h 33m 39.79s , +25d 38m 17.1s) |   C |    60 | 17.8 |        
   21747 | 2022-07-28 22:22:36 |             MASTER- | (00h 45m 18.91s , +31d 45m 35.5s) |   C |    60 | 18.7 |        
   21747 | 2022-07-28 22:22:36 |             MASTER- | (00h 54m 23.80s , +31d 38m 26.7s) |   C |    60 | 14.1 |        
   21779 | 2022-07-28 22:23:08 |         MASTER-SAAO | (23h 42m 27.29s , +25d 37m 13.8s) |   C |    60 | 17.6 |        
   21859 | 2022-07-28 22:24:27 |         MASTER-SAAO | (23h 23m 52.46s , +31d 21m 07.3s) |   C |    60 | 17.4 |        
   21949 | 2022-07-28 22:25:58 |         MASTER-SAAO | (23h 33m 14.24s , +31d 19m 24.6s) |   C |    60 | 17.5 |        
   21961 | 2022-07-28 22:26:10 |             MASTER- | (01h 05m 34.32s , +44d 56m 34.5s) |   C |    60 | 14.0 |        
   22045 | 2022-07-28 22:27:34 |         MASTER-SAAO | (23h 23m 16.55s , +27d 32m 54.8s) |   C |    60 | 18.0 |        
   22125 | 2022-07-28 22:28:54 |         MASTER-SAAO | (23h 32m 12.51s , +27d 32m 18.4s) |   C |    60 | 17.7 |        
   22221 | 2022-07-28 22:30:30 |         MASTER-SAAO | (23h 14m 01.07s , +29d 27m 29.7s) |   C |    60 | 18.0 |        
   22247 | 2022-07-28 22:30:56 |             MASTER- | (00h 35m 45.05s , +48d 50m 36.1s) |   C |    60 | 18.9 |        
   22301 | 2022-07-28 22:31:50 |         MASTER-SAAO | (23h 23m 16.96s , +29d 26m 23.4s) |   C |    60 | 17.9 |        
   22383 | 2022-07-28 22:33:12 |             MASTER- | (23h 33m 21.73s , +33d 39m 48.0s) |   C |    60 | 19.1 |        
   22383 | 2022-07-28 22:33:12 |             MASTER- | (23h 42m 39.86s , +33d 32m 33.6s) |   C |    60 | 13.9 |        
   22481 | 2022-07-28 22:34:50 |         MASTER-SAAO | (23h 25m 41.13s , +25d 37m 22.8s) |   C |    60 | 18.2 |        
   22578 | 2022-07-28 22:36:26 |         MASTER-SAAO | (23h 31m 31.05s , +29d 26m 54.3s) |   C |    60 | 17.8 |        
   22673 | 2022-07-28 22:38:02 |         MASTER-SAAO | (23h 40m 42.37s , +29d 25m 35.7s) |   C |    60 | 17.6 |        
   22753 | 2022-07-28 22:39:22 |         MASTER-SAAO | (23h 33m 40.30s , +25d 39m 19.2s) |   C |    60 | 17.9 |        
   22808 | 2022-07-28 22:40:16 |             MASTER- | (23h 31m 07.65s , +46d 57m 20.9s) |   C |    60 | 18.8 |        
   22844 | 2022-07-28 22:40:53 |         MASTER-SAAO | (23h 42m 28.55s , +25d 38m 16.4s) |   C |    60 | 17.7 |        
   22886 | 2022-07-28 22:41:35 |             MASTER- | (00h 56m 33.69s , +45d 02m 34.3s) |   C |    60 | 12.8 |        
   22925 | 2022-07-28 22:42:14 |         MASTER-SAAO | (23h 23m 51.49s , +31d 21m 27.3s) |   C |    60 | 17.1 |        
   23016 | 2022-07-28 22:43:45 |         MASTER-SAAO | (23h 33m 19.46s , +31d 20m 20.9s) |   C |    60 | 17.5 |        
   23018 | 2022-07-28 22:43:46 |             MASTER- | (23h 36m 20.11s , +43d 02m 23.5s) |   C |    60 | 14.0 |        
   23092 | 2022-07-28 22:45:01 |             MASTER- | (23h 25m 17.04s , +39d 21m 19.0s) |   C |    60 | 19.0 |        
   23093 | 2022-07-28 22:45:01 |             MASTER- | (23h 35m 17.27s , +39d 13m 24.9s) |   C |    60 | 14.0 |        
   23097 | 2022-07-28 22:45:06 |         MASTER-SAAO | (23h 23m 12.52s , +27d 31m 25.3s) |   C |    60 | 18.1 |        
   23192 | 2022-07-28 22:46:41 |         MASTER-SAAO | (23h 32m 19.30s , +27d 31m 37.4s) |   C |    60 | 17.6 |        
   23240 | 2022-07-28 22:47:28 |             MASTER- | (00h 37m 35.02s , +48d 52m 20.6s) |   C |    60 | 12.4 |        
   23317 | 2022-07-28 22:48:46 |             MASTER- | (23h 35m 24.36s , +33d 39m 20.9s) |   C |    60 | 14.8 |        
   23317 | 2022-07-28 22:48:46 |             MASTER- | (23h 44m 41.70s , +33d 31m 25.3s) |   C |    60 | 13.9 |        
   23521 | 2022-07-28 22:52:10 |             MASTER- | (23h 30m 39.52s , +35d 33m 13.8s) |   C |    60 | 19.1 |        
   23658 | 2022-07-28 22:54:27 |             MASTER- | (23h 41m 21.42s , +31d 46m 18.1s) |   C |    60 | 18.9 |        
   23658 | 2022-07-28 22:54:27 |             MASTER- | (23h 50m 27.23s , +31d 38m 22.3s) |   C |    60 | 14.4 |        
   24024 | 2022-07-28 23:00:33 |             MASTER- | (23h 51m 08.76s , +46d 35m 48.3s) |   C |    60 | 18.6 |        
   24099 | 2022-07-28 23:01:48 |             MASTER- | (23h 42m 49.15s , +42d 46m 54.3s) |   C |    60 | 18.9 |        
   24175 | 2022-07-28 23:03:04 |             MASTER- | (23h 41m 12.86s , +38d 58m 02.7s) |   C |    60 | 18.9 |        
   24331 | 2022-07-28 23:05:40 |             MASTER- | (00h 37m 30.53s , +48d 51m 56.6s) |   C |    60 | 14.8 |        
   24410 | 2022-07-28 23:06:58 |             MASTER- | (23h 35m 20.94s , +33d 38m 46.3s) |   C |    60 | 16.4 |        
   24410 | 2022-07-28 23:06:58 |             MASTER- | (23h 44m 39.91s , +33d 31m 27.0s) |   C |    60 | 13.9 |        
   24542 | 2022-07-28 23:09:10 |             MASTER- | (23h 27m 05.87s , +37d 27m 34.4s) |   C |    60 | 14.0 |        
   24542 | 2022-07-28 23:09:10 |             MASTER- | (23h 36m 52.29s , +37d 20m 16.6s) |   C |    60 | 13.8 |        
   24753 | 2022-07-28 23:12:42 |             MASTER- | (23h 41m 18.52s , +31d 45m 42.2s) |   C |    60 | 14.6 |        
   24753 | 2022-07-28 23:12:42 |             MASTER- | (23h 50m 25.96s , +31d 38m 21.4s) |   C |    60 | 14.0 |        
   24829 | 2022-07-28 23:13:58 |             MASTER- | (23h 53m 53.83s , +29d 50m 46.6s) |   C |    60 | 18.8 |        
   24829 | 2022-07-28 23:13:58 |             MASTER- | (00h 02m 50.20s , +29d 43m 26.9s) |   C |    60 | 14.1 |        
   25265 | 2022-07-28 23:21:14 |             MASTER- | (23h 42m 42.24s , +42d 45m 57.8s) |   C |    60 | 18.8 |        
   25396 | 2022-07-28 23:23:25 |             MASTER- | (23h 41m 12.14s , +39d 00m 04.6s) |   C |    60 | 18.9 |        
   25471 | 2022-07-28 23:24:40 |             MASTER- | (23h 42m 50.67s , +37d 05m 08.4s) |   C |    60 | 19.1 |        
   25607 | 2022-07-28 23:26:55 |             MASTER- | (23h 45m 44.06s , +35d 12m 13.9s) |   C |    60 | 14.5 |        
   25682 | 2022-07-28 23:28:11 |             MASTER- | (23h 55m 55.97s , +31d 23m 34.2s) |   C |    60 | 18.8 |        
   25683 | 2022-07-28 23:28:11 |             MASTER- | (23h 46m 47.67s , +31d 31m 57.3s) |   C |    60 | 13.9 |        
   25863 | 2022-07-28 23:31:12 |             MASTER- | (23h 56m 29.62s , +31d 23m 32.3s) |   C |    60 | 18.8 |        
   25863 | 2022-07-28 23:31:12 |             MASTER- | (23h 47m 21.27s , +31d 31m 55.4s) |   C |    60 | 14.0 |        
   25959 | 2022-07-28 23:32:48 |             MASTER- | (01h 11m 25.34s , +39d 21m 11.3s) |   C |    60 | 12.2 |        
   25959 | 2022-07-28 23:32:48 |             MASTER- | (01h 21m 25.52s , +39d 14m 06.3s) |   C |    60 | 14.1 |        
   26069 | 2022-07-28 23:34:37 |             MASTER- | (01h 09m 30.82s , +37d 28m 10.0s) |   C |    60 | 18.7 |        
   26069 | 2022-07-28 23:34:37 |             MASTER- | (01h 19m 15.38s , +37d 21m 02.8s) |   C |    60 | 14.1 |        
   26359 | 2022-07-28 23:39:28 |             MASTER- | (01h 06m 27.10s , +33d 39m 08.7s) |   C |    60 | 12.3 |        
   26359 | 2022-07-28 23:39:28 |             MASTER- | (01h 15m 44.83s , +33d 31m 55.6s) |   C |    60 | 13.9 |        
   26492 | 2022-07-28 23:41:41 |             MASTER- | (00h 46m 15.91s , +29d 51m 57.9s) |   C |    60 | 18.8 |        
   26492 | 2022-07-28 23:41:41 |             MASTER- | (00h 55m 11.41s , +29d 44m 43.3s) |   C |    60 | 14.0 |        
   26568 | 2022-07-28 23:42:57 |             MASTER- | (01h 07m 57.80s , +35d 33m 03.1s) |   C |    60 | 18.9 |        
   26568 | 2022-07-28 23:42:57 |             MASTER- | (01h 17m 28.49s , +35d 25m 52.7s) |   C |    60 | 13.8 |        
   26705 | 2022-07-28 23:45:14 |             MASTER- | (00h 11m 04.53s , +27d 57m 33.8s) |   C |    60 | 15.6 |        
   26705 | 2022-07-28 23:45:14 |             MASTER- | (00h 19m 50.63s , +27d 50m 17.6s) |   C |    60 | 13.8 |        
   26781 | 2022-07-28 23:46:30 |             MASTER- | (23h 53m 51.25s , +29d 50m 19.1s) |   C |    60 | 13.9 |        
   26970 | 2022-07-28 23:49:39 |             MASTER- | (01h 21m 17.86s , +39d 14m 50.5s) |   C |    60 | 14.1 |        
   27045 | 2022-07-28 23:50:53 |             MASTER- | (01h 09m 33.67s , +37d 27m 00.6s) |   C |    60 | 12.0 |        
   27254 | 2022-07-28 23:54:23 |             MASTER- | (01h 13m 21.39s , +41d 15m 01.6s) |   C |    60 | 14.4 |        
   27254 | 2022-07-28 23:54:23 |             MASTER- | (01h 23m 39.92s , +41d 07m 52.7s) |   C |    60 | 14.2 |        
   27390 | 2022-07-28 23:56:39 |             MASTER- | (01h 15m 39.07s , +33d 32m 49.7s) |   C |    60 | 13.9 |        
   27466 | 2022-07-28 23:57:55 |             MASTER- | (00h 46m 19.35s , +29d 50m 53.1s) |   C |    60 | 12.2 |        
   27466 | 2022-07-28 23:57:55 |             MASTER- | (00h 55m 15.41s , +29d 43m 35.9s) |   C |    60 | 14.3 |        
Filter C is a clear (unfiltred) band. 


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


