# GCN_circulars

GRB_name: GRB200608A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27908
SUBJECT: Swift GRB 200608A: Global MASTER-Net observations report 
DATE:    20/06/08 22:28:28 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200608A ( M. J. Moss et al., GCN 27906) errorbox  7027 sec after notice time and 7103 sec after trigger time at 2020-06-08 19:27:01 UT, with upper limit up to  18.0 mag. The observations began at zenith distance = 82 deg. The sun  altitude  is -47.0 deg. 

The galactic latitude b = -36 deg., longitude l = 13 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1376906

We obtain a following upper limits.  

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

    7193 |         MASTER-SAAO |   C |   180 | 14.9 |        
   17386 |         MASTER-SAAO |   C |   180 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200609A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27909
SUBJECT: GRB 200609A: Fermi GBM Final Real-time Localization
DATE:    20/06/09 09:17:24 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 09:06:59 UT on 9 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200609A (trigger 613386424.308736 / 200609380).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 16.3, Dec = 67.4 (J2000 degrees, equivalent to J2000 01h 05m, 67d 24'), with a statistical uncertainty of 1.4 degrees.

The angle from the Fermi LAT boresight is 150.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200609380/quicklook/glg_skymap_all_bn200609380.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200609380/quicklook/glg_healpix_all_bn200609380.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200609380/quicklook/glg_lc_medres34_bn200609380.gif


GRB_name: GRB200605A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27911
SUBJECT: GRB 200605A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/06/09 11:11:36 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

Y. Kawakubo (LSU),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (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 short GRB 200605A (Fermi GBM Localization: the Fermi GBM team,
GCN Circ. 27892; IPN triangulation: Hurley et al., GCN Circ. 27900;
https://gcn.gsfc.nasa.gov/other/200605A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 18:17:42.317 UTC
on 5 June 2020. The burst signal was seen by only the SGM detector.
The source location was outside the FOV of the HXM detectors.
Because of a problem in one of the ground alert processing script,
the GCN notice was not distributed automatically for this event.

The burst light curve shows a double-peaked pulse which starts at
T-0.176 sec, peaks at -0.048 sec and ends at T+0.256 sec. The T90 and T50
durations measured by the SGM data are 0.368 +- 0.062 sec and
0.232 +- 0.051 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1275416255/

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


GRB_name: GRB200605A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27912
SUBJECT: Konus-Wind detection of GRB 200605A
DATE:    20/06/09 12:12:44 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The short-duration GRB 200605A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27892;
IPN triangulation: Hurley et al., GCN Circ. 27900;
CALET-GRBM detection: Kawakubo et al., GCN Circ. 27911)
triggered Konus-Wind at T0=65858.111 s UT (18:17:38.111).

The burst light curve shows a multipeaked structure
which starts at ~T0 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/GRB200605_T65862/

As observed by Konus-Wind, the burst
had a fluence of 3.63(-0.51,+0.60)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.016 s,
of 2.48(-0.69,+0.75)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 = -0.82(-0.20,+0.23)
and Ep = 744(-174,+273) keV (chi2 = 23/28 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 23/27 dof).

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


GRB_name: GRB200608A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27913
SUBJECT: GRB 200608A: Swift-BAT refined analysis
DATE:    20/06/09 19:07:12 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), C. B. Markwardt (GSFC),
M. J. Moss (GWU), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (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 200608A (trigger #976692)
(Moss et al., GCN Circ. 27906).  The BAT ground-calculated position is
RA, Dec = 309.628, -31.194 deg which is
   RA(J2000)  =  20h 38m 30.7s
   Dec(J2000) = -31d 11' 39.4"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 53%.

The mask-weighted light curve shows several overlapping pulses that start
at ~T+20 s and ends at ~T+150 s. The two main peaks occur at
~T+18 s and ~T+70 s, respectively. There may be an additional weak pulse
at ~T-100 s. T90 (15-350 keV) is 119.2 +- 34.7 sec (estimated error
including systematics).

The time-averaged spectrum from T+18.09 to T+147.94 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
2.05 +- 0.22.  The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+70.29 sec in the 15-150 keV band
is 0.7 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/976692/BA/


GRB_name: GRB200609A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27914
SUBJECT: GRB 200609A: Insight-HXMT/HE detection
DATE:    20/06/11 07:19:48 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, S. Xiao, Y. F. Du, Y. G. Zheng, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-06-09T09:06:48.050 (T0), Insight-HXMT/HE detected 
GRB 200609A (trigger ID: HEB200609379) in a routine search of the data, 
which also triggered Fermi/GBM (GCN #27909).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 82.18 s measured from T0-42.67 s. 
The 1-ms peak rate, measured from T0+10.58 s, is 1241 cnts/sec. 
The total counts from this burst is 17682 counts. 
URL_LC:  http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200609379_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
GRB mode with the energy range of about 200-3000 keV (record energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope.  

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200612A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27915
SUBJECT: GRB 200612A: Swift detection of a burst
DATE:    20/06/12 05:06:28 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

E. Sonbas (Adiyaman Univ.), C. Gronwall (PSU), N. J. Klingler (PSU),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 04:39:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200612A (trigger=977310).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 302.681, -45.357 which is 
   RA(J2000) = 20h 10m 43s
   Dec(J2000) = -45d 21' 24"
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.  There is possible lower-level
activity out to T+180s.  The peak count rate was ~1400 counts/sec 
(15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 04:41:04.7 UT, 87.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 302.7017, -45.3343 which is equivalent to:
   RA(J2000)  = 20h 10m 48.41s
   Dec(J2000) = -45d 20' 03.5"
with an uncertainty of 5.1 arcseconds (radius, 90% containment). This
location is 97 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 2.13e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 95 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
0.03. 

We note that Fermi-GBM sees a GRB in a similar location at T+10 minutes,
(trigger  613630183) which may be extended activity of the same source. 
At that time, BAT had slewed away from the source. 

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


GRB_name: GRB200612A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27919
SUBJECT: GRB 200612A: BOOTES-3/YA optical upper limit
DATE:    20/06/12 17:02:23 GMT
FROM:    Youdong HU at IAA-CSIC  <youdong@iaa.es>

Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), I. 
Carrasco and C. Perez del Pulgar (Univ. de Malaga), M. D. 
Caballero-Garcia (ASU-CAS, CZ) and R. Querel (NIWA), on behalf of a 
larger collaboration, report:

The 60cm BOOTES-3/YA robotic telescope at NIWA Lauder in Otago (New 
Zealand) responded to the Swift trigger of GRB 200612A (Sonbas et al. 
GCNC 27915). The first image (clear filter) was obtained starting at 
09:51:32 UT(~ 5.2 hr after trigger). In the co-added image (20 exposures 
60s each), no source is found at the position reported by Swift/XRT 
(Sonbas et al. GCNC 27915) and MASTER-Net (Lipunov et al. GCNC 27917) 
down to 20.3 mag.

We thank the staff at NIWA for its excellent support.


GRB_name: GRB200612A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27920
SUBJECT: GRB 200612A: Late Optical Maximum Deteted by MASTER 
DATE:    20/06/12 18:55:38 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.Tiurina, Lomonosow NSU

We find very late OT (Lipunov et al., GCN 27917) maximum ~17.5 around 
2020-06-12 04:59:09 UT .

This message can be cited.


GRB_name: GRB200612A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27921
SUBJECT: GRB 200612A: Enhanced Swift-XRT position
DATE:    20/06/12 20:11:58 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 2651 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 200612A, 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 = 302.70204, -45.33550 which is equivalent
to:

RA (J2000): 20h 10m 48.49s
Dec (J2000): -45d 20' 07.8"

with an uncertainty of 1.5 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: GRB200612A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27922
SUBJECT: Konus-Wind observation of ultra-long GRB 200612A
DATE:    20/06/12 20:13:01 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The ultra-long GRB 200612A
(Swift-BAT detection Sonbas et al., GCN 27915;
MASTER OT detection: Lipunov et al., GCN 27917)
was detected by Konus-Wind in the waiting mode.

The burst light curve shows four emission episodes
in the interval from ~T0(BAT) s to ~T0(BAT)+1020 s.

The K-W light curve of this burst is available at
http://www.ioffe.ru/LEA/GRBs/GRB200612A/

As observed by Konus-Wind, the burst had a fluence of
4.08(-0.34,+1.04)x10^-5 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(BAT)+478.8 s, of 2.75(-0.62,+0.85)x10^-7 erg/cm2/s
(both in the 20 - 1500 keV energy band).

The K-W 3-channel time-integrated spectrum
(from ~T0(BAT) s to ~T0(BAT)+1020 s)
is well described by a cutoff power-law model
with alpha = -1.0(-0.2,+0.3) and Ep= 253(-65,+95) keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.


GRB_name: GRB200612A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27923
SUBJECT: GRB 200612A: Swift-XRT refined Analysis
DATE:    20/06/13 00:13:52 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. D'Ai (INAF-IASFPA), J. D. Gropp (PSU), J.A. Kennea (PSU), A.
Tohuvavohu (U. Toronto), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), T.
Sbarrato (INAF-OAB) and E. Sonbas report on behalf of the Swift-XRT
team:

We have analysed 7.4 ks of XRT data for GRB 200612A (Sonbas et al. GCN
Circ. 27915), from 93 s to 63.5 ks after the  BAT trigger. The data
comprise 281 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. 27921).

The late-time light curve (from T0+3.7 ks) can be modelled with a
power-law decay with a decay index of alpha=1.37 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.07 (+/-0.05). The
best-fitting absorption column is  9.1 (+2.3, -2.1) x 10^20 cm^-2, in
excess of the Galactic value of 3.7 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.06 (+0.19, -0.17)
and a best-fitting absorption column of 5.7 (+4.1, -2.0) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.1 x 10^-11 (3.6 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.7 (+4.1, -2.0) x 10^20 cm^-2
Galactic foreground: 3.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.06 (+0.19, -0.17)

If the light curve continues to decay with a power-law decay index of
1.37, the count rate at T+24 hours will be 0.010 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.2 x
10^-13 (3.7 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/00977310.

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


GRB_name: GRB200612A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27924
SUBJECT: GRB 200612A: Swift-BAT refined analysis
DATE:    20/06/13 01:19:49 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
E. Sonbas (Adiyaman Univ.), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 200612A (trigger #977310)
(E. Sonbas et al., GCN Circ. 27915). The BAT ground-calculated position is
RA, Dec = 302.691, -45.354 deg which is
   RA(J2000)  =  20h 10m 45.8s
   Dec(J2000) = -45d 21' 12.7"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The mask weighted light curve shows a complex structure. The
overall structure starts at ~T-20 s and lasts till ~T+200 s.
T90 (15-350 keV) is 171.48 +- 19.74 sec (estimated error including systematics).

The time-averaged spectrum from T-11 to T+193 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.09.  The fluence in the 15-150 keV band is 3.8 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.03 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/977310/BA/


GRB_name: GRB200612A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27925
SUBJECT: Draft Circular for GRB 200612A
DATE:    20/06/13 02:43:08 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

Hey all,

There's very little data to look at here but it's a conclusive
nondetection, so I'll be sending out the upper limits auto-circular shortly
barring any comments.

-Sam


GRB 200612A: Swift/UVOT Upper Limits

S. J. LaPorte (PSU) and E. Sonbas (Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200612A
96 s after the BAT trigger (Sonbas et al., GCN Circ. 27915).
No optical afterglow consistent with the optical position
(Lipunov et al. GCN Circ. 27917)
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            96          245          147         >20.6
white               96          245          147         >20.6
u                  308          375           67         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200613A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27926
SUBJECT: GRB 200613A: Fermi GBM Final Real-time Localization
DATE:    20/06/13 05:40:32 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:30:08 UT on 13 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200613A (trigger 613719013.213684 / 200613229).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 149.1, Dec = 51.1 (J2000 degrees, equivalent to J2000 09h 56m, 51d 06'), with a statistical uncertainty of 1.0 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/2020/bn200613229/quicklook/glg_skymap_all_bn200613229.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200613229/quicklook/glg_healpix_all_bn200613229.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200613229/quicklook/glg_lc_medres34_bn200613229.gif


GRB_name: GRB200612A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27929
SUBJECT: GRB 200612A: Swift/UVOT Upper Limits
DATE:    20/06/13 12:43:45 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

 GRB 200612A: Swift/UVOT Upper Limits

S. J. LaPorte (PSU) and E. Sonbas (Adiyaman Univ.)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200612A
96 s after the BAT trigger (Sonbas et al., GCN Circ. 27915).
No optical afterglow consistent with the optical position
(Lipunov et al. GCN Circ. 27917)
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            96          245          147         >20.6
white               96          245          147         >20.6
u                  308          375           67         >19.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200613A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27930
SUBJECT: GRB 200613A: Fermi GBM observation
DATE:    20/06/13 15:48:47 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

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


"At 05:30:08.21 UT on 13 June 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200613A (trigger 613719013 / 200613229).
The Fermi GBM Final Real-time Localization is reported in GCN #27926.

The angle from the Fermi LAT boresight at the GBM trigger time is 25 degrees.

The GBM light curve shows a bright initial emission episode
followed by a later weaker emission episode
with a duration (T90) of about 470 s (50-300 keV).
The time-averaged spectrum from T0 to T0+50 s is
best fit by a Band function with Epeak = 111 +/- 3 keV,
alpha = -1.08 +/- 0.02, and beta = -2.58 +/- 0.08.

The event fluence (10-1000 keV) in this time interval is
(4.10 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+12.2 s in the 10-1000 keV band
is 27.2 +/- 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: GRB200613A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27931
SUBJECT: GRB 200613A: Fermi-LAT detection
DATE:    20/06/13 17:06:26 GMT
FROM:    Masanori Ohno at Hiroshima University  <ohno@astro.hiroshima-u.ac.jp>

M. Ohno (Hiroshima Univ.), M. Kovacevic (INFN Perugia), E. Bissaldi
(Politecnico & INFN Bari), M. Axelsson (KTH & Stockholm Univ.) and F. Longo
(University and INFN, Trieste) report on behalf of the Fermi-LAT
Collaboration:

On June 13, 2020, Fermi-LAT detected high-energy emission from
GRB 200613A, which was also detected by Fermi-GBM at T0 = 05:30:08 UT (GCN
27926, Bissaldi et al. GCN 27930).

The GRB is detected at high energy (>100 MeV) by Fermi-LAT at a location
of:

RA, Dec = 153.03, 45.85 (degrees, J2000) with an error radius of 0.14 deg
(90% containment, statistical error only).

This was ~29 deg from the LAT boresight when observations started, and is
~5.9 deg from the GBM final ground position.

The photon flux above 100 MeV in the time interval 0 - 10.000 s after the
GBM trigger is 6.6e-07 +/- 3.6e-07 ph/cm2/s.

The estimated photon index above 100 MeV is -1.73 +/- 0.36. The
highest-energy photon is a 7.6 GeV event which is observed ~6.2 ks after
the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Masanori Ohno (
ohno@astro.hiroshima-u.ac.jp).

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: GRB200613A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27932
SUBJECT: GRB 200613A: Swift ToO observations
DATE:    20/06/13 17:08:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Fermi/LAT GRB 200613A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021003

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: GRB200613A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27933
SUBJECT: Fermi GRB 200613A: Global MASTER-Net observations report 
DATE:    20/06/13 18:15:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200613A ( Fermi GBM team, GCN 27926) errorbox  44637 sec after notice time and 44665 sec after trigger time at 2020-06-13 17:54:33 UT, with upper limit up to  18.2 mag. Observations started at twilight.  The observations began at zenith distance = 42 deg. The sun  altitude  is -9.8 deg. 

The galactic latitude b = 51 deg., longitude l = 173 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1380771

We obtain a following upper limits.  

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

   44756 | 2020-06-13 17:54:33 |   MASTER-Kislovodsk | (10h 11m 31.91s , +46d 20m 06.9s) |   C |   180 | 17.2 |        
   44756 | 2020-06-13 17:54:33 |   MASTER-Kislovodsk | (10h 11m 44.05s , +45d 51m 37.8s) |   C |   180 | 17.0 |        
   44897 | 2020-06-13 17:57:54 |   MASTER-Kislovodsk | (09h 50m 41.65s , +52d 24m 17.7s) |   C |    60 | 17.4 |        
   44897 | 2020-06-13 17:57:54 |   MASTER-Kislovodsk | (10h 04m 14.80s , +51d 58m 14.9s) |   C |    60 | 17.2 |        
   44977 | 2020-06-13 17:59:15 |   MASTER-Kislovodsk | (09h 50m 35.85s , +50d 23m 21.1s) |   C |    60 | 17.5 |        
   44977 | 2020-06-13 17:59:15 |   MASTER-Kislovodsk | (10h 03m 33.20s , +49d 57m 12.1s) |   C |    60 | 17.5 |        
   45138 | 2020-06-13 18:01:55 |   MASTER-Kislovodsk | (09h 51m 19.61s , +48d 25m 06.7s) |   C |    60 | 17.6 |        
   45138 | 2020-06-13 18:01:55 |   MASTER-Kislovodsk | (10h 03m 45.71s , +47d 58m 51.5s) |   C |    60 | 17.5 |        
   45278 | 2020-06-13 18:03:16 |   MASTER-Kislovodsk | (10h 11m 37.07s , +46d 17m 06.7s) |   C |   180 | 18.2 |        
   45278 | 2020-06-13 18:03:16 |   MASTER-Kislovodsk | (10h 11m 44.14s , +45d 48m 54.3s) |   C |   180 | 18.2 |        
   45419 | 2020-06-13 18:06:37 |   MASTER-Kislovodsk | (09h 50m 42.12s , +52d 24m 34.5s) |   C |    60 | 18.0 |        
   45419 | 2020-06-13 18:06:37 |   MASTER-Kislovodsk | (10h 04m 12.70s , +51d 58m 30.7s) |   C |    60 | 17.8 |        
   45499 | 2020-06-13 18:07:57 |   MASTER-Kislovodsk | (09h 50m 36.32s , +50d 23m 57.5s) |   C |    60 | 18.1 |        
   45499 | 2020-06-13 18:07:57 |   MASTER-Kislovodsk | (10h 03m 31.39s , +49d 57m 48.8s) |   C |    60 | 17.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200612A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27934
SUBJECT: GRB 200612A: Fermi GBM detection
DATE:    20/06/13 20:50:23 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

C. Malacaria (NASA-MSFC/USRA), E. Burns (NASA-GSFC) and C. Meegan (UAH) 
report on behalf of the Fermi GBM Team:

At 04:49:38.68 UT on June 06 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200612A (trigger 613630183/200612201),
which was also detected by the Swift (Osborne et al. 2020, GCN 27921)
and Konus-Wind (Sonbas et al. 2020, GCN 27915; Svinkin et al. 2020, GCN 27922). 
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 50 degrees.

The GBM light curve shows multiple pulses with a 
duration (T90) of about 88 s (50-300 keV).
The GBM light curve also shows evidence of emission preceding the trigger time,
in agreement with the super-long GRB classification by Konus-Wind.

The time-averaged spectrum from T0-214 s to T0+89 s is best-fit
by a power-law with a photon index of -1.80 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(4.187 +/- 0.109)E-05 erg/cm^2.
The 1-sec peak photon flux measured starting from T0+52 s 
in the 10-1000 keV band is 2.8 +/- 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: GRB200613A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27935
SUBJECT: GRB 200613A: Candidate afterglow from OAJ
DATE:    20/06/13 23:06:59 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), M. Blazek, C. Thoene, J. F. Agui Fernandez (all 
HETH/IAA-CSIC), A. Moreno, and H. Vasquez Ramio (both CEFCA) report:

We observed the LAT position of the bright GRB 200613A (Fermi-LAT 
detection: Ohno et al. GCN #27931, Fermi GBM detection: Bissaldi & 
Lesage, GCN #27930) with the T80 0.8m telescope at the Observatorio de 
Javalambre (Teruel, Spain). Observations consisted of 3 x 300 s in g', 3 
x 300 s in r', and 5 x 180 s in i'.

At the position of the second reported XRT source, we detect an optical 
source not seen to several magnitudes deeper in PanSTARRS archival 
imaging. The source is detected in each frame. The position is RA 
(J2000) = 10:12:10.08, Dec. (J2000) = 45:54:14.26 with an estimated 
error of 0".5. There is also a cataloged SDSS source nearby at RA 
(J2000) = 10:12:10.075, Dec. (J2000) = 45:54:12.88, this may be the host 
galaxy of the GRB, though we note nothing is detected here in the 
PanSTARRS image.

Further analysis is in progress. Spectroscopic observations are 
encouraged.


GRB_name: GRB200613A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27936
SUBJECT: GRB 200613A: Swift-XRT afterglow detection
DATE:    20/06/14 04:46:25 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 200613A (Ohno et al. GCN Circ. 27931),
collecting 4.9 ks of Photon Counting (PC) mode data between T0+43.6 ks
and T0+67.6 ks. 

Seven uncatalogued X-ray sources are detected, of which one ("Source
2") is above the RASS limit, and is therefore likely the GRB afterglow.
Using 4079 s of PC mode data and 4 UVOT images, we find an enhanced XRT
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 153.04199, +45.75408 which is
equivalent to:

RA (J2000): 10h 12m 10.08s
Dec(J2000): +45d 45' 14.7"

with an uncertainty of 1.4 arcsec (radius, 90% confidence). This
position is 5.8 arcmin from the Fermi/LAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.6 (+/-0.5).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.89 (+0.14, -0.13). The
best-fitting absorption column is  2.3 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 8.4 x 10^19 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.5 x 10^-11 (4.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 8.4 x 10^19 cm^-2
Excess significance: 7.5 sigma
Photon index:      1.89 (+0.14, -0.13)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021003.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021003.

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


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27937
SUBJECT: GRB 200613A: Kitab and AbAO optical afterglow observations, host galaxy candidate
DATE:    20/06/14 08:21:00 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), S. Belkin (IKI), A. Novichonok (Petrozavodsk State 
University, KIAM), R. Ya. Inasaridze (AbAO), V.R. Ayvazian (AbAO),  G. 
V.  Kapanadze (AbAO),  E. Mazaeva  (IKI), A. Volnova (IKI), I. Molotov 
(KIAM), Sh. Ehgamberdiev (UBAI) report on behalf of IKI-GRB-FuN:

We observed Fermi  GRB 200613A (Fermi GBM team, GCN 27926; Bissaldi et 
al., GCN 27930; Ohno et al., GCN 27931) with Kitab-ISON RC-36  telescope 
starting on 2020-06-13 (UT) 17:58:33 in Clear filter and AS-32 telescope 
of Abastumani observatory in R. Within localization area of XRT 
afterglow (Kennea et al., GCN27936) we  detected the only one object in 
coordinates
(J2000) 10:12:10.02 +45:45:13.7
The object is also visible in SDSS *(SDSS12 J101210.07+454512.8*) as a 
galaxy**with a photometric redshift of z= 0.4745.

(We believe that Kann et al. (GCN 27935) observed and reported the same 
object).

We suggest the SDSS galaxy *J101210.07+454512.8* is a host galaxy of GRB 
200613A.
Preliminary photometry of the source is following

Date,      UT start, t-T0,   Exp.,  Filter,  OT,   Err., UL
                     (mid, days)
2020-06-13  17:58:33  0.54057 60*60 CR      19.39  0.20  19.8
2020-06-13  18:16:59  0.55024 50*60  R      19.27  0.07  22.1

The photometry is based on nearby SDSS DR12 stars
SDSS-DR12_id        R(Lupton)
J101149.76+454320.7 12.404
J101245.45+455119.1 13.328


GRB_name: GRB200613A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27938
SUBJECT: GRB 200613A: OAJ Afterglow: Error in Coordinates
DATE:    20/06/14 08:39:36 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC) corrects:

The source reported in Kann et al., GCN #27935, lies at coordinates:

RA (J2000) = 10:12:10.08
Dec. (J2000) = 45:45:14.26

and is therefore coincident with the XRT afterglow (Kennea et al., GCN 
#27936) and the source detected earlier by Pozanenko et al. (GCN #27937) 
as well as the potential host galaxy also mentioned by the latter GCN 
(coordinates in GCN #27935 suffer the same error).

I'm sorry for any inconvenience I may have caused.


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27939
SUBJECT: GRB 200613A: Liverpool Telescope observations
DATE:    20/06/14 10:46:42 GMT
FROM:    Luca Izzo at DARK/NBI  <luca.izzo@gmail.com>

We observed the field of GRB 200613A (Bissaldi and Lesage, GCN #27930; Ohno et al., GCN #27931) with the IO:O camera mounted on the 2-m Liverpool Telescope located in La Palma, Spain. Observations started on June 13th at 22:20:26 UT (0.701 days after the GRB trigger) and we obtained a series of 60s images in the r filter.

We clearly detect in the stacked image the optical afterglow at the position reported by the Swift-XRT (Kennea et al., GCN #27936) and by OAJ, Kitab and AbAO (Kann et al., GCN #27935, GCN #27938; Pozanenko et al., GCN #27937). We measure a preliminary AB magnitude for the afterglow of r = 19.45 +- 0.20 mag (t_mid = 0.705 d) calibrated against Pan-STARRS catalogue stars.


GRB_name: GRB200614A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27940
SUBJECT: GRB 200614A: Fermi GBM Final Real-time Localization
DATE:    20/06/14 14:45:17 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:34:55 UT on 14 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200614A (trigger 613838100.238884 / 200614608).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 115.7, Dec = 60.8 (J2000 degrees, equivalent to J2000 07h 42m, 60d 47'), with a statistical uncertainty of 6.5 degrees.

The angle from the Fermi LAT boresight is 82.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200614608/quicklook/glg_skymap_all_bn200614608.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200614608/quicklook/glg_healpix_all_bn200614608.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200614608/quicklook/glg_lc_medres34_bn200614608.gif


GRB_name: GRB200614A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27942
SUBJECT: Fermi GRB 200614A: Global MASTER-Net observations report 
DATE:    20/06/14 15:45:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200614A ( Fermi GBM team, GCN 27940) errorbox  2103 sec after notice time and 2142 sec after trigger time at 2020-06-14 15:10:37 UT, with upper limit up to  17.1 mag. Observations started at twilight.  The observations began at zenith distance = 58 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = 30 deg., longitude l = 152 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1381664

We obtain a following upper limits.  

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

    2172 | 2020-06-14 15:10:37 |        MASTER-Tunka | (04h 29m 28.78s , +70d 07m 54.4s) |   C |    60 | 16.0 |        
    2590 | 2020-06-14 15:17:35 |        MASTER-Tunka | (04h 25m 19.49s , +69d 36m 27.1s) |   C |    60 | 15.9 |        
    2686 | 2020-06-14 15:19:11 |        MASTER-Tunka | (04h 52m 44.81s , +70d 08m 40.6s) |   C |    60 | 16.0 |        
    2783 | 2020-06-14 15:20:48 |        MASTER-Tunka | (04h 53m 37.47s , +71d 37m 21.8s) |   C |    60 | 16.5 |        
    2881 | 2020-06-14 15:22:26 |        MASTER-Tunka | (05h 23m 50.40s , +72d 07m 52.6s) |   C |    60 | 16.7 |        
    2976 | 2020-06-14 15:24:01 |        MASTER-Tunka | (04h 31m 21.86s , +73d 35m 32.9s) |   C |    60 | 16.9 |        
    3074 | 2020-06-14 15:25:39 |        MASTER-Tunka | (05h 05m 13.03s , +74d 09m 03.4s) |   C |    60 | 17.1 |        
    3170 | 2020-06-14 15:27:15 |        MASTER-Tunka | (04h 27m 52.81s , +71d 35m 54.7s) |   C |    60 | 15.8 |        
    3266 | 2020-06-14 15:28:51 |        MASTER-Tunka | (04h 52m 54.51s , +70d 08m 13.6s) |   C |    60 | 16.1 |        
    3365 | 2020-06-14 15:30:30 |        MASTER-Tunka | (05h 19m 19.13s , +71d 38m 10.9s) |   C |    60 | 16.2 |        
    3464 | 2020-06-14 15:32:09 |        MASTER-Tunka | (05h 05m 13.37s , +74d 09m 02.8s) |   C |    60 | 16.4 |        
    3704 | 2020-06-14 15:36:09 |        MASTER-Tunka | (05h 12m 00.45s , +69d 38m 43.6s) |   C |    60 | 16.0 |        
    3801 | 2020-06-14 15:37:46 |        MASTER-Tunka | (05h 31m 13.21s , +68d 10m 00.0s) |   C |    60 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27943
SUBJECT: GRB 200613A: Xinglong-2.16m optical observations
DATE:    20/06/14 15:46:06 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu, X. Liu, S.Y. Fu, D. Xu, J. Zheng, A.Y. Zhou (NAOC) report:

We observed the field of GRB 200613A (Fermi GBM team, GCN 27926; 
Bissaldi et al., GCN 27930; Ohno et al., GCN 27931) using the 
Xinglong-2.16m telescope equipped with the BFOSC camera. Observations 
were carried out starting at 12:44:18 UT on 2020-06-14, and 5x300s 
R-band frames were obtained.

The previously reported afterglow (e.g., Kann et al., GCN 27935; Kennea 
et al., GCN 27936; Pozanenko et al., GCN 27937; Izzo et al., GCN 27939) 
is clearly detected in our stacked image, with R = 19.45 +/- 0.05 mag 
(at Tmid-T0 = 1.266 days post-burst), calibrated with nearby Pan-STARRS1.


GRB_name: GRB200613A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27944
SUBJECT: GRB 200613A: Swift/UVOT Detection
DATE:    20/06/14 17:02:42 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC)
reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200613A
43621 s after the FERMI/LAT trigger (Ohno et al., GCN Circ. 27931).
A source consistent with the XRT position (Kennea et al., GCN Circ. 27936)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  10:12:10.03 = 153.04178 (deg.)
    Dec (J2000) = +45:45:14.1  =  45.75391 (deg.)
with an estimated uncertainty of 0.46 arc sec. (radius, 90% confidence).
This position is consistent with the optical counterparts
reported by Kann et al. (GCN Circ. 27935 & 27938) and
Pozanenko (GCN Circ. 27937).

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

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

white            44416        45204         775         19.65 +/- 0.07
v                45211        45427         213        >18.6
u                43621        44409         775         19.02 +/- 0.12

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200615A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27947
SUBJECT: GRB 200615A: Fermi GBM Final Real-time Localization
DATE:    20/06/15 06:10:23 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 LONG GRB

At 06:00:05 UT on 15 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200615A (trigger 613893610.082594 / 200615250).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 48.1, Dec = 5.4 (J2000 degrees, equivalent to J2000 03h 12m, 5d 24'), with a statistical uncertainty of 6.0 degrees.

The angle from the Fermi LAT boresight is 62.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200615250/quicklook/glg_skymap_all_bn200615250.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200615250/quicklook/glg_healpix_all_bn200615250.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200615250/quicklook/glg_lc_medres34_bn200615250.gif


GRB_name: GRB200615A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27948
SUBJECT: Fermi GRB 200615A: Global MASTER-Net observations report 
DATE:    20/06/15 10:45:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200615A ( Fermi GBM team, GCN 27947) errorbox  13375 sec after notice time and 13402 sec after trigger time at 2020-06-15 09:43:27 UT, with upper limit up to  19.1 mag. The observations began at zenith distance = 77 deg. The sun  altitude  is -22.4 deg. 

The galactic latitude b = -42 deg., longitude l = 175 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1382183

We obtain a following upper limits.  

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

   13433 | 2020-06-15 09:43:27 |         MASTER-OAFA | (03h 39m 17.15s , +01d 56m 03.2s) |   C |    60 | 17.8 |        
   13524 | 2020-06-15 09:44:59 |         MASTER-OAFA | (03h 39m 37.24s , +03d 56m 02.4s) |   C |    60 | 17.8 |        
   13798 | 2020-06-15 09:49:33 |         MASTER-OAFA | (03h 39m 10.24s , +01d 55m 41.9s) |   C |    60 | 17.8 |        
   13981 | 2020-06-15 09:52:35 |         MASTER-OAFA | (03h 39m 37.53s , +03d 57m 28.7s) |   C |    60 | 18.1 |        
   15194 | 2020-06-15 10:11:49 |         MASTER-OAFA | (03h 07m 07.28s , +01d 56m 33.9s) |   C |   180 | 19.1 |        
   15406 | 2020-06-15 10:15:21 |         MASTER-OAFA | (03h 07m 01.99s , +01d 56m 01.1s) |   C |   180 | 19.1 |        
   15558 | 2020-06-15 10:18:53 |         MASTER-OAFA | (03h 06m 59.90s , +03d 57m 00.7s) |   C |    60 | 18.5 |        
   15649 | 2020-06-15 10:20:24 |         MASTER-OAFA | (03h 07m 06.53s , +03d 56m 01.9s) |   C |    60 | 18.3 |        
   15740 | 2020-06-15 10:21:55 |         MASTER-OAFA | (02h 59m 00.18s , +03d 54m 52.2s) |   C |    60 | 18.3 |        
   15832 | 2020-06-15 10:23:26 |         MASTER-OAFA | (02h 59m 05.64s , +03d 55m 00.4s) |   C |    60 | 18.5 |        
   15923 | 2020-06-15 10:24:57 |         MASTER-OAFA | (03h 15m 03.47s , +03d 57m 01.2s) |   C |    60 | 18.0 |        
   16014 | 2020-06-15 10:26:29 |         MASTER-OAFA | (03h 15m 03.40s , +03d 55m 27.9s) |   C |    60 | 17.9 |        
   16105 | 2020-06-15 10:27:59 |         MASTER-OAFA | (03h 15m 06.22s , +01d 56m 57.7s) |   C |    60 | 17.8 |        
   16196 | 2020-06-15 10:29:30 |         MASTER-OAFA | (03h 15m 02.07s , +01d 56m 13.8s) |   C |    60 | 17.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27949
SUBJECT: GRB 200613A: Continued Xinglong-2.16m optical observations
DATE:    20/06/15 15:23:05 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

X. Liu, Z.P. Zhu, S.Y. Fu, D. Xu, J. Zheng, A.Y. Zhou (NAOC) report:

We continued to observe the field of GRB 200613A (Fermi GBM team, GCN 
27926; Bissaldi et al., GCN 27930; Ohno et al., GCN 27931) using the 
Xinglong-2.16m telescope equipped with the BFOSC camera. Observations 
were carried out starting at 12:43:45 UT on 2020-06-15, and 5x300s 
R-band frames were obtained.

The previously reported afterglow (e.g., Kann et al., GCN 27935; Kennea 
et al., GCN 27936; Pozanenko et al., GCN 27937; Izzo et al., GCN 27939; 
Zhu et al., GCN 27943) is still clearly detected in our stacked image, 
with R = 20.0 +/- 0.1 mag (at Tmid-T0 = 2.311 days post-burst), 
calibrated with nearby Pan-STARRS1.

Further observations are planned.


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27958
SUBJECT: GRB 200613A: continued AbAO optical afterglow observations
DATE:    20/06/15 21:49:44 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), R. Ya. Inasaridze (AbAO), V. R. 
Ayvazian (AbAO),  G. V. Kapanadze (AbAO),  E. Mazaeva  (IKI), A. Volnova 
(IKI), I. Molotov (KIAM)  report on behalf of IKI-GRB-FuN:

We continue observations of Fermi  GRB 200613A (Fermi GBM team, GCN 
27926; Bissaldi et al., GCN 27930; Ohno et al., GCN 27931) with  AS-32 
telescope of Abastumani observatory in R-filter. The afterglow (e.g., 
Kann et al., GCN 27935; Kennea et al., GCN 27936; Pozanenko et al., GCN 
27937; Izzo et al., GCN 27939; Zhu et al., GCN 27943) is detected in a 
stacked image. Preliminary photometry of the afterglow is following

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

2020-06-15  17:44:15 2.53029 49*60  R       20.47  0.11  21.9

The photometry is based on nearby SDSS DR12 stars
SDSS-DR12_id        R(Lupton)
J101149.76+454320.7 12.404
J101245.45+455119.1 13.328


GRB_name: GRB200616A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27959
SUBJECT: GRB 200616A: Fermi GBM Final Real-time Localization
DATE:    20/06/16 01:19:37 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 01:09:15 UT on 16 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200616A (trigger 613962560.630758 / 200616048).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 116.2, Dec = -72.2 (J2000 degrees, equivalent to J2000 07h 44m, -72d 12'), with a statistical uncertainty of 4.6 degrees.

The angle from the Fermi LAT boresight is 17.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200616048/quicklook/glg_skymap_all_bn200616048.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200616048/quicklook/glg_healpix_all_bn200616048.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200616048/quicklook/glg_lc_medres34_bn200616048.gif


GRB_name: GRB200615B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27960
SUBJECT: GRB 200615B: MAXI/GSC detection 
DATE:    20/06/16 01:40:27 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro.hitoshi@nihon-u.ac.jp>

K. Miike (Miyazaki U.), H. Negoro (Nihon U.), Y. Kawakubo (LSU), 
M. Nakajima, M. Aoki, K. Kobayashi, R. Takagi, K, Asakura, 
K, Seino, S. Mokumoto (Nihon U.), 
T. Mihara, C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN), 
T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), 
M. Shidatsu (Ehime U.), N. Kawai, R. Adachi, M. Niwano (Tokyo Tech), 
S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), 
Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), 
H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi (Miyazaki U.), 
T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), M. Sugizaki (NAOC) 
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered on an uncatalogued X-ray transient source 
at 10:30:18 UT on 2020 June 15.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (153.421 deg, -5.158 deg) = (10 13 41, -05 09 28) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.34 deg and 0.3 deg, respectively. 
The roll angle of the long axis from the north direction is 180.0 deg counterclockwise. 
Without assumptions on the source flux constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (152.024, -3.311) deg = (10 08 05, -03 18 39) (J2000) 
(R.A., Dec) = (151.564, -3.753) deg = (10 06 15, -03 45 10) (J2000) 
(R.A., Dec) = (153.538, -5.793) deg = (10 14 09, -05 47 34) (J2000) 
(R.A., Dec) = (153.998, -5.350) deg = (10 15 59, -05 20 59) (J2000) 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius)
in both error regions.

The X-ray flux averaged over the scan was 85 +- 19 mCrab
(4.0-10.0keV, 1 sigma error).

There was no significant excess flux in the previous transit at 08:57 UT
and in the next transit at 12:03 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB200616A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27961
SUBJECT: Fermi GRB 200616A: Global MASTER-Net observations report 
DATE:    20/06/16 01:45:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200616A ( Fermi GBM team, GCN 27959) errorbox  304 sec after notice time and 338 sec after trigger time at 2020-06-16 01:14:54 UT, with upper limit up to  19.6 mag. The observations began at zenith distance = 72 deg. The sun  altitude  is -54.7 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200616A errorbox  601 sec after notice time and 635 sec after trigger time at 2020-06-16 01:19:51 UT, with upper limit up to  17.5 mag. The observations began at zenith distance = 65 deg. The sun  altitude  is -46.2 deg. 

The galactic latitude b = -21 deg., longitude l = 293 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1382729

We obtain a following upper limits.  

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

     369 | 2020-06-16 01:14:54 |         MASTER-SAAO | (07h 30m 34.93s , -75d 53m 38.2s) |   C |    60 | 19.2 |        
     369 | 2020-06-16 01:14:54 |         MASTER-SAAO | (07h 58m 43.08s , -75d 52m 05.2s) |   C |    60 | 19.4 |        
     449 | 2020-06-16 01:16:14 |         MASTER-SAAO | (07h 33m 20.18s , -73d 54m 44.7s) |   C |    60 | 19.3 |        
     449 | 2020-06-16 01:16:14 |         MASTER-SAAO | (07h 58m 04.22s , -73d 53m 20.9s) |   C |    60 | 19.4 |        
     529 | 2020-06-16 01:17:34 |         MASTER-SAAO | (07h 27m 18.60s , -77d 52m 49.4s) |   C |    60 | 19.4 |        
     529 | 2020-06-16 01:17:34 |         MASTER-SAAO | (07h 59m 58.51s , -77d 51m 07.7s) |   C |    60 | 19.5 |        
     639 | 2020-06-16 01:18:54 |         MASTER-SAAO | (07h 34m 37.50s , -72d 09m 47.5s) |   C |   120 | 19.1 |        
     639 | 2020-06-16 01:18:54 |         MASTER-SAAO | (07h 56m 59.49s , -72d 08m 32.7s) |   C |   120 | 19.3 |        
     666 | 2020-06-16 01:19:51 |         MASTER-OAFA | (07h 36m 21.01s , -69d 59m 29.3s) |   C |    60 | 17.1 |        
     789 | 2020-06-16 01:21:14 |         MASTER-SAAO | (07h 34m 44.80s , -72d 09m 15.4s) |   C |   140 | 19.2 |        
     789 | 2020-06-16 01:21:14 |         MASTER-SAAO | (07h 57m 06.26s , -72d 08m 01.5s) |   C |   140 | 19.4 |        
     848 | 2020-06-16 01:22:53 |         MASTER-OAFA | (07h 39m 19.14s , -67d 58m 00.7s) |   C |    60 | 16.9 |        
     963 | 2020-06-16 01:23:53 |         MASTER-SAAO | (07h 34m 41.75s , -72d 07m 44.3s) |   C |   170 | 19.3 |        
     963 | 2020-06-16 01:23:53 |         MASTER-SAAO | (07h 57m 01.51s , -72d 06m 30.2s) |   C |   170 | 19.4 |        
     939 | 2020-06-16 01:24:24 |         MASTER-OAFA | (08h 23m 06.72s , -69d 57m 46.3s) |   C |    60 | 17.5 |        
    1158 | 2020-06-16 01:27:03 |         MASTER-SAAO | (07h 34m 40.92s , -72d 09m 17.0s) |   C |   180 | 19.4 |        
    1158 | 2020-06-16 01:27:03 |         MASTER-SAAO | (07h 57m 02.85s , -72d 08m 03.5s) |   C |   180 | 19.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200613A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27962
SUBJECT: GRB 200613A: MITSuME Akeno optical upper limits
DATE:    20/06/16 01:48:34 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

K. L. Murata, N. Ito, R. Hosokawa, R. Adachi, M. Niwano, F. Ogawa, N.
Nakamura, S. Ogata, H. Takamatsu, H. Hara, Y. Yatsu, and N.
Kawai(TokyoTech) report on behalf of the MITSuME collaboration:

We observed the field of GRB 200613A (Fermi GBM team, GCN 27926; Bissaldi
et al., GCN 27930; Ohno et al., GCN 27931) with the optical three color
(g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of
Akeno Observatory, Yamanashi, Japan.

The observation started on 2020-06-15 11:33. We did not detect the optical
afterglow (Kann et al., GCN 27935; Kennea et al., GCN 27936; Pozanenko et
al., GCN 27937; Izzo et al., GCN 27939; Zhu et al., GCN 27943; Marshall et
al., GCN 27944; Liu et al., GCN 27949; Belkin et al., GCN 27958) in the
stacked image. We obtained the 5-sigma limits as follows.

T0+[hour] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
54 2020-06-15T12:29:27 2040 g'>19.3, Rc>19.5, Ic>18.6
------------------------------------------------------------------------------------------------
T0+: Elapsed time after the burst
T-EXP: Total Exposure time

We used the 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., submitted;
https://github.com/MNiwano/Eclair)


GRB_name: GRB200613A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27964
SUBJECT: GRB 200613A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/06/16 12:34:45 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

K. Yamaoka (Nagoya U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), S. Nakahira (RIKEN),
Y. Asaoka, S. Torii (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 very long GRB 200613A (Fermi GBM observation: Bissaldi and Lesage,
GCN Circ. 27930; Fermi-LAT detection: Ohno et al., GCN Circ. 27931;
https://gcn.gsfc.nasa.gov/other/200613A.gcn3) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 05:30:08.657 UTC on 13 June 2020.
The burst signal was seen by all CGBM detectors.
Because of a problem in one of the ground alert processing script,
the GCN notice was not distributed automatically for this event.

The burst light curve shows the main emission episode which starts at
T-1 sec, peaks at T+11 sec and ends at T+35 sec, followed by a much weaker
emission episode which starts at ~T+278 sec and ends at ~T+423 sec.
The T90 and T50 durations measured by the SGM data are 381 +- 34 sec and
268 +- 237 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1276061388/

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


GRB_name: GRB200616B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27967
SUBJECT: GRB 200616B: Fermi GBM Final Real-time Localization
DATE:    20/06/16 15:52:06 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 15:41:47 UT on 16 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200616B (trigger 614014912.725084 / 200616654).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 148.2, Dec = -42.2 (J2000 degrees, equivalent to J2000 09h 52m, -42d 12'), with a statistical uncertainty of 1.6 degrees.

The angle from the Fermi LAT boresight is 17.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200616654/quicklook/glg_skymap_all_bn200616654.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200616654/quicklook/glg_healpix_all_bn200616654.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200616654/quicklook/glg_lc_medres34_bn200616654.gif


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27971
SUBJECT: GRB 200613A: Jet-break from Xinglong-2.16m optical observations
DATE:    20/06/17 01:39:34 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

S.Y. Fu, Z.P. Zhu, X. Liu, D. Xu, J. Zheng, A.Y. Zhou (NAOC) report:

We continued to observe the field of GRB 200613A (Fermi GBM team, GCN 
27926; Bissaldi et al., GCN 27930; Ohno et al., GCN 27931) using the 
Xinglong-2.16m telescope equipped with the BFOSC camera. Observations 
were carried out starting at 12:55:02 UT on 2020-06-16, and 5x300s 
R-band frames were obtained.

The optical afterglow (e.g., Kann et al., GCN 27935; Kennea et al., GCN 
27936; Pozanenko et al., GCN 27937; Izzo et al., GCN 27939; Zhu et al., 
GCN 27943; Marshall, GCN 27944; Liu et al., GCN 27949; Belkin et al., 
GCN 27958) is still well detected in our stacked image, with R = 21.07 
+/- 0.21 mag (at Tmid-T0 = 3.3175 days post-burst), calibrated with 
nearby Pan-STARRS1.

Compared with our previous measurements, the afterglow now has turned to 
decay quickly, with a temporal decay index of  \alpha ~ 2.5 and a break 
time of ~ 2.3 days post-burst. This break can be interpreted as a jet break.

Further observations are planned.


GRB_name: GRB200615B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27974
SUBJECT: GRB 200615B: CALET Gamma-Ray Burst Monitor detection
DATE:    20/06/17 12:04:33 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

S. Nakahira (RIKEN),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U),
Y. Asaoka, S. Torii (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:

At 10:26:46.325 UTC on 15 June 2020, the CALET Gamma-ray Burst Monitor
(CGBM) triggered on the long weak GRB 200615B (trigger 1276251981:
http://cgbm.calet.jp/cgbm_trigger/flight/1276251981/index.html),
which was also detected by the MAXI/GSC at T0(CGBM)+213 sec
(Miike et al. 2020, GCN Circ. 27960).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure which starts at
T+3.8 sec and ends at T+48.8 sec. The T90 and T50 durations measured
by the SGM data are 40.0 +- 6.3 sec and 28.0 +- 9.5 sec (40-1000 keV),
respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1276251981/

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


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27978
SUBJECT: GRB 200613A: Mondy optical observations
DATE:    20/06/18 10:44:12 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI),  A. Pozanenko (IKI), E. Klunko (ISTP),  M. Eselevich 
(ISTP), E. Mazaeva (IKI), A. Volnova (IKI) report on behalf of IKI-GRB FuN:

We observed the  GRB 200613A (Fermi GBM team, GCN 27926; Bissaldi et 
al., GCN 27930; Ohno et al., GCN 27931; Yamaoka Ohno et al., GCN 27964) 
with with AZT-33IK 1.5-m telescope of Sayan observatory (Mondy) starting 
on 2020-06-17 (UT) 16:30:12.

The optical afterglow (e.g., Kann et al., GCN 27935; Pozanenko et al., GCN 27937; Izzo et al., GCN 27939; Zhu et al., GCN 27943; Marshall, GCN 27944; Liu et al., GCN 27949; Belkin et al., GCN 27958) is detected in a stacked image. Preliminary photometry of the afterglow is following

Date       UT start  t-T0    Filter Exp.   OT    Err. UL
                     (mid, days)     (s)
2020-06-17 16:30:12  4.47365 R      22*120 20.94 0.14 22.1

The photometry is based on nearby SDSS stars
SDSS-DR12_id      R(Lupton)
J101206.52+454606.4 14.962
J101207.75+454443.4 17.877
J101206.50+454322.2 15.151


GRB_name: GRB200617A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27981
SUBJECT: GRB 200617A: Insight-HXMT/HE detection
DATE:    20/06/18 15:29:35 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, Y. G. Zheng, C. Cai, Y. F. Du, W. C. Xue, 
Q. Luo, Q. B. Yi, Y. Huang, C. K. Li, G. Li, 
X. B. Li, J. Y. Liao, S. L. Xiong,C. Z. Liu, 
X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, 
X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), 
T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-06-17T16:18:05.80 (T0), Insight-HXMT/HE detected 
GRB 200617A (trigger ID: HEB200617679) in a routine search of the data.

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 1.89 s measured from T0-1.65 s. 
The 1-ms peak rate, measured from T0+0.09 s, is 2209 cnts/sec. 
The total counts from this burst is 1309 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200617679_lc.jpg

All measurements above are made with the CsI detectors operating in the 
normal mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27982
SUBJECT: GRB 200613A: SAO RAS optical observations
DATE:    20/06/18 18:15:13 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

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

We observed the field of the GRB 200613A (Fermi GBM team, GCN 27926;
Bissaldi et al., GCN 27930; Ohno et al., GCN 27931; Ohno et al.,
GCN 27964) with the 1m telescope of SAO RAS, Zeiss-1000,
equipped with the Multi-Mode Photometer-Polarimeter (MMPP).
We obtained 6 x 300 sec. images in Rc band on 2020.06.16
19:05:00--19:45:16 UT, T_mid - T0 = 3.5799 days.

The optical afterglow (Kann et al., GCN 27935; Pozanenko et al.,
GCN 27937; Izzo et al., GCN 27939; Zhu et al., GCN 27943;
Marshall, GCN 27944; Liu et al., GCN 27949; Belkin et al., GCN 27958;
Fu et al., GCN 27971; Belkin et al., GCN 27978) is clearly visible
in individual images and stacked frame with the brightness of
R = 20.58 +/- 0.05.

The photometry is based on nearby SDSS DR12 stars
SDSS_id        R(Lupton)
J101206.52+454606.4 14.962
J101207.75+454443.4 17.877
J101220.88+454613.5 16.508
J101211.59+454721.5 18.659
J101209.58+454817.4 18.076


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27983
SUBJECT: GRB 200613A: continued Kitab optical observations
DATE:    20/06/18 22:04:59 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Novichonok (Petrozavodsk State University, KIAM), A. 
Pozanenko (IKI),  E. Mazaeva  (IKI), A. Volnova (IKI), I. Molotov 
(KIAM), Sh. Ehgamberdiev (UBAI) report on behalf of IKI-GRB-FuN:

We continued observations of GRB 200613A (Fermi GBM team, GCN 27926; 
Bissaldi et al., GCN 27930; Ohno et al., GCN 27931; Yamaoka Ohno et al., 
GCN 27964) with  Kitab-ISON RC-36 telescope in Clear filter. The optical 
afterglow (e.g., Kann et al., GCN 27935; Pozanenko et al., GCN 27937; 
Izzo et al., GCN 27939; Zhu et al., GCN 27943) is detected in a stacked 
image. Preliminary photometry of the afterglow is following

Date,      UT start, t-T0,   Exp.,  Filter, OT,    Err., UL
                     (mid, days)
2020-06-14  16:56:58 1.5086  5460   CR      19.68  0.13  21.2
2020-06-15  16:54:39 2.4997  4200   CR      20.4   0.3   20.4
2020-06-16  16:30:51 3.5005  7200   CR      n/d    n/d   20.5


The photometry is based on nearby SDSS DR12 stars
SDSS-DR12_id        R(Lupton)
J101149.76+454320.7 12.404
J101245.45+455119.1 13.328


GRB_name: GRB200619A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27985
SUBJECT: GRB 200619A: Insight-HXMT/HE detection
DATE:    20/06/19 11:52:34 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, Y. G. Zheng, C. Cai, Y. F. Du, W. C. Xue, 
Q. Luo, Q. B. Yi, Y. Huang, C. K. Li, G. Li, 
X. B. Li, J. Y. Liao, S. L. Xiong,C. Z. Liu, 
X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang, 
X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), 
T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-06-19T02:36:11.60 (T0), Insight-HXMT/HE detected 
GRB 200619A (trigger ID: HEB200619108) in a routine search of the data, 
which also triggered Fermi/GBM and INTEGRAL (EXB 200619108).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 18.49 s measured from T0+0.35 s. 
The 1-ms peak rate, measured from T0-0.04 s, is 2889 cnts/sec. 
The total counts from this burst is 14248 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200619108_lc.jpg

All measurements above are made with the CsI detectors operating in the 
normal mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200619B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27986
SUBJECT: GRB 200619B: Fermi GBM Final Real-time Localization
DATE:    20/06/19 11:59:03 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 11:48:43 UT on 19 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200619B (trigger 614260128.085724 / 200619492).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 200.4, Dec = -45.1 (J2000 degrees, equivalent to J2000 13h 21m, -45d 06'), with a statistical uncertainty of 5.1 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/2020/bn200619492/quicklook/glg_skymap_all_bn200619492.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200619492/quicklook/glg_healpix_all_bn200619492.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200619492/quicklook/glg_lc_medres34_bn200619492.gif


GRB_name: GRB200619A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27991
SUBJECT: GRB 200619A: AGILE detection
DATE:    20/06/19 14:02:02 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the GRB 200619A reported by Insight-HXMT/HE
(Xiao et al., GCN #27985), occurring at T0 = 2020-06-19T02:36:11.60 +/-
0.01 s (UTC).

The event is visible in the scientific ratemeters (RMs) of the
Anti-Coincidence (AC, 80-200 keV) and Mini-Calorimeter (MCAL, 0.4-100 MeV)
detectors. Their light curves show a FRED profile, lasting ~15 s and
releasing ~54380 counts in the AC RMs and ~22675 counts in the MCAL RMs.
The ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/RM_GRB200619A.png .

Additional analysis of AGILE data is in progress.


GRB_name: GRB200619A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27993
SUBJECT: GRB 200619A: Fermi GBM observation
DATE:    20/06/19 21:15:01 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

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

"At 02:36:11.67 UT on 19 June 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200619A (trigger 614226976 / 200619108).
This burst was also detected by the AGILE satellite (A. Ursi et al. 2020, GCN 27991)
and Insight-HXMT/HE (S. Xiao et al. 2020, GCN 27985).

The on-ground calculated location, using the GBM trigger
data, is RA = 101.4, DEC = 56.7 (J2000 degrees,
equivalent to 06h 45m, 56d 44'), with a statistical uncertainty
of 4.0 degrees (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).

The angle from the Fermi LAT boresight at the GBM trigger time is 103 degrees.

The GBM light curve consists of a single bright peak
with a duration (T90) of about 29 s (50-300 keV).
The time-averaged spectrum from T0+0.003 s to T0+29.120 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.82 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 1268 +/- 199 keV.

The event fluence (10-1000 keV) in this time interval is
(1.42 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.064 s in the 10-1000 keV band
is 4.8 +/- 0.4 ph/s/cm^2.

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

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


GRB_name: GRB200619B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27994
SUBJECT: GRB 200619B: AstroSat CZTI detection
DATE:    20/06/19 21:25:55 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 200619B, which was also detected by Fermi GBM (GCN #27986).

The source was clearly detected in the 40-200 keV energy range. The light curve showed a single peak of emission peaking at 2020-06-19 11:48:43.617 UT. The measured peak count rate associated with the burst is 188 +/- 23 cts/s above the background in the combined data of four quadrants, with a total of 917 +/- 11 cts. The local mean background count rate was 520 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 8.182 +/- 0.028 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, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.


GRB_name: GRB200619B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27995
SUBJECT: Fermi GRB 200619B: Global MASTER-Net observations report 
DATE:    20/06/19 21:30:24 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 200619B ( Fermi GBM team, GCN 27986) errorbox  33291 sec after notice time and 33333 sec after trigger time at 2020-06-19 21:04:16 UT, with upper limit up to  17.6 mag. Observations started at twilight.  The observations began at zenith distance = 73 deg. The sun  altitude  is -12.6 deg. 

The galactic latitude b = 18 deg., longitude l = 303 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1385756

We obtain a following upper limits.  

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

   33364 | 2020-06-19 21:04:16 |          MASTER-IAC | (13h 02m 42.95s , -43d 52m 47.7s) |   C |    60 | 16.8 |        
   33364 | 2020-06-19 21:04:16 |          MASTER-IAC | (12h 51m 30.58s , -43d 48m 31.7s) |   C |    60 | 16.5 |        
   33479 | 2020-06-19 21:06:11 |          MASTER-IAC | (12h 40m 35.18s , -43d 53m 58.8s) |   C |    60 | 17.1 |        
   33479 | 2020-06-19 21:06:11 |          MASTER-IAC | (12h 29m 22.82s , -43d 49m 45.5s) |   C |    60 | 16.6 |        
   33599 | 2020-06-19 21:08:11 |          MASTER-IAC | (12h 59m 07.07s , -41d 55m 02.4s) |   C |    60 | 17.1 |        
   33599 | 2020-06-19 21:08:11 |          MASTER-IAC | (12h 48m 15.92s , -41d 50m 44.5s) |   C |    60 | 16.7 |        
   33717 | 2020-06-19 21:10:10 |          MASTER-IAC | (13h 02m 47.52s , -43d 55m 04.7s) |   C |    60 | 17.4 |        
   33717 | 2020-06-19 21:10:10 |          MASTER-IAC | (12h 51m 34.98s , -43d 50m 47.5s) |   C |    60 | 17.0 |        
   33835 | 2020-06-19 21:12:07 |          MASTER-IAC | (12h 40m 32.80s , -43d 53m 38.4s) |   C |    60 | 17.4 |        
   33835 | 2020-06-19 21:12:07 |          MASTER-IAC | (12h 29m 20.63s , -43d 49m 25.0s) |   C |    60 | 16.9 |        
   33956 | 2020-06-19 21:14:08 |          MASTER-IAC | (12h 59m 10.12s , -41d 54m 43.7s) |   C |    60 | 17.6 |        
   33956 | 2020-06-19 21:14:08 |          MASTER-IAC | (12h 48m 19.17s , -41d 50m 26.5s) |   C |    60 | 17.1 |        
   34075 | 2020-06-19 21:16:08 |          MASTER-IAC | (12h 37m 44.18s , -41d 53m 32.1s) |   C |    60 | 17.4 |        
   34075 | 2020-06-19 21:16:08 |          MASTER-IAC | (12h 26m 53.44s , -41d 49m 18.4s) |   C |    60 | 17.0 |        
   34193 | 2020-06-19 21:18:05 |          MASTER-IAC | (12h 56m 39.20s , -39d 54m 15.7s) |   C |    60 | 17.6 |        
   34193 | 2020-06-19 21:18:05 |          MASTER-IAC | (12h 46m 07.71s , -39d 49m 58.5s) |   C |    60 | 17.2 |        
   34311 | 2020-06-19 21:20:04 |          MASTER-IAC | (13h 20m 37.46s , -41d 53m 18.1s) |   C |    60 | 17.5 |        
   34311 | 2020-06-19 21:20:04 |          MASTER-IAC | (13h 09m 46.98s , -41d 48m 58.6s) |   C |    60 | 17.4 |        
   34434 | 2020-06-19 21:22:07 |          MASTER-IAC | (12h 37m 43.41s , -41d 54m 19.0s) |   C |    60 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200619C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27996
SUBJECT: GRB 200619C: Fermi GBM Final Real-time Localization
DATE:    20/06/19 23:01:20 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 06:03:22 UT on 19 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200619C (trigger 614239407 / 200619252). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 225.15, Dec = -10.39 (J2000 degrees, equivalent to J2000 15h 01m, -10d 23'), with a statistical uncertainty of 3.3 degrees. The angle from the Fermi LAT boresight is 24.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200619252/quicklook/glg_skymap_all_bn200619252.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200619252/quicklook/glg_healpix_all_bn200619252.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200619252/quicklook/glg_lc_medres34_bn200619252.gif


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27998
SUBJECT: GRB 200613A: Further Liverpool Telescope observations
DATE:    20/06/20 07:19:20 GMT
FROM:    Luca Izzo at DARK/NBI  <luca.izzo@gmail.com>

L. Izzo (DARK/NBI) reports:

We observed the field of GRB 200613A (Bissaldi and Lesage, GCN #27930; Ohno et al., GCN #27931) with the IO:O camera mounted on the 2-m Liverpool Telescope located in La Palma, Spain. Observations started on June 19th at 22:00:00 UT (6.687 days after the GRB trigger) and we obtained a series of 10x60s images in the r filter.

The afterglow (Kann et al., GCN #27935; Pozanenko et al., GCN #27937; Izzo et al., GCN #27939; Zhu et al., GCN #27943; Marshall, GCN #27944; Liu et al., GCN #27949; Belkin et al., GCN #27958; Fu et al., GCN #27971; Belkin et al., GCN #27978; Moskvitin et al., GCN #27982; Belkin et al., GCN #27983) is clearly visible in the combined image. We measure a preliminary AB magnitude r = 21.20 +- 0.30 mag (t_mid = 6.770 d) calibrated against Pan-STARRS catalogue stars.


GRB_name: GRB200613A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27999
SUBJECT: GRB 200613A: R-band observations from HCT
DATE:    20/06/20 11:29:46 GMT
FROM:    Brajesh Kumar at Indian Inst. of Astrophysics  <brajesh.kumar@iiap.res.in>

Anirban Dutta, Brajesh Kumar, Avinash Singh, G. C. Anupama, D. K. Sahu 
and B. S. Kiran (IIA, Bengaluru)

We observed the field of GRB 200613A (Fermi GBM team, GCN #27926; 
Bissaldi et al., GCN #27930; Ohno et al., GCN #27931; Evans, GCN #27932) 
with the Himalayan Faint Object Spectrograph and Camera (HFOSC) mounted 
on the 2-m Himalayan Chandra Telescope located at IAO, Hanle, India. 
Observations started on 2020-06-19 at 15:20:43 UT and we obtained 3 
frames, each of 300 sec in the Bessell R-band filter under moderate sky 
conditions.

The afterglow (Kann et al., GCN #27935; Pozanenko et al., GCN #27937; 
Zhu et al., GCN #27943; Marshall, GCN #27944; Liu et al., GCN #27949; 
Belkin et al., GCN #27958; GCN #27978; GCN #27983; Fu et al., GCN 
#27971; Moskvitin et al., GCN #27982; Izzo, GCN #27998) is clearly 
visible in the stacked image. We measure a preliminary magnitude of R = 
20.59 +/- 0.26 mag calibrated against the USNO-A2.0 catalogue stars. The 
host contamination has not been removed in the analysis.

We thank the observing staff at IAO and CREST for helping with the 
observations.


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28000
SUBJECT: GRB 200613A: CrAO optical observations
DATE:    20/06/20 11:51:17 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI),  V. Rumyantsev (CrAO),  A. Volnova 
(IKI), E. Mazaeva (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the  GRB 200613A (Fermi GBM team, GCN 27926; Bissaldi et 
al., GCN 27930; Ohno et al., GCN 27931; Yamaoka Ohno et al., GCN 27964)  
with ZTSH 2.6m telescope of CrAO observatory starting on 2020-06-19 (UT) 
18:58:23.  The optical afterglow (e.g., Kann et al., GCN 27935; 
Pozanenko et al., GCN 27937; Izzo et al., GCN 27939; Zhu et al., GCN 
27943; Marshall, GCN 27944; Liu et al., GCN 27949; Belkin et al., GCN 
27958) is detected in a stacked image. Preliminary photometry of the 
afterglow is following

Date       UT start  t-T0    Filter Exp.   OT    Err. UL
                     (mid, days)     (s)
2020-06-19 18:58:23  6.58142 R      29*120 21.06 0.09 23.6

The photometry is based on nearby SDSS star
SDSS-DR12_id      R(Lupton)
J101207.75+454443.4 17.877

A light curve of the afterglow of  GRB 200613A can be found in 
http://grb.rssi.ru/GRB200613A/GRB200613A_lc_v2.png


GRB_name: GRB200613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28003
SUBJECT: GRB 200613A: Continued CrAO optical observations
DATE:    20/06/21 10:36:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI),  V. Rumyantsev (CrAO),  A. Volnova 
(IKI), E. Mazaeva (IKI) report on behalf of larger GRB follow-up 
collaboration:

We observed the  GRB 200613A (Fermi GBM team, GCN 27926; Bissaldi et 
al., GCN 27930; Ohno et al., GCN 27931; Yamaoka Ohno et al., GCN 27964)  
with ZTSH 2.6m telescope of CrAO observatory starting on 2020-06-20 (UT) 
19:19:12.  The optical afterglow (e.g., Kann et al., GCN 27935; 
Pozanenko et al., GCN 27937; Izzo et al., GCN 27939; Zhu et al., GCN 
27943; Marshall, GCN 27944; Liu et al., GCN 27949; Belkin et al., GCN 
27958) is detected in a stacked image. Preliminary photometry of the 
afterglow is following

Date       UT start  t-T0    Filter Exp.   OT    Err. UL
                     (mid, days)     (s)
2020-06-20 19:19:12  6.58142 R      6*120 21.13 0.10 22.7

The photometry is based on nearby SDSS star
SDSS-DR12_id      R(Lupton)
J101207.75+454443.4 17.877

A light curve of the afterglow of  GRB 200613A can be found in 
http://grb.rssi.ru/GRB200613A/GRB200613A_lc_v2.png


GRB_name: GRB200622A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28008
SUBJECT: GRB 200622A: Fermi GBM Final Real-time Localization
DATE:    20/06/22 02:21:31 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 02:11:48 UT on 22 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200622A (trigger 614484713.116416 / 200622092).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 107.5, Dec = 38.3 (J2000 degrees, equivalent to J2000 07h 10m, 38d 17'), with a statistical uncertainty of 1.4 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/2020/bn200622092/quicklook/glg_skymap_all_bn200622092.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200622092/quicklook/glg_healpix_all_bn200622092.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200622092/quicklook/glg_lc_medres34_bn200622092.gif


GRB_name: GRB200623A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28011
SUBJECT: GRB 200623A: Fermi GBM Final Real-time Localization
DATE:    20/06/23 03:28:09 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 03:18:00 UT on 23 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200623A (trigger 614575085.637496 / 200623138).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 224.3, Dec = 60.4 (J2000 degrees, equivalent to J2000 14h 57m, 60d 23'), with a statistical uncertainty of 11.2 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/2020/bn200623138/quicklook/glg_skymap_all_bn200623138.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200623138/quicklook/glg_healpix_all_bn200623138.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200623138/quicklook/glg_lc_medres34_bn200623138.gif


GRB_name: GRB200623A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28012
SUBJECT: Fermi GRB 200623A: Global MASTER-Net observations report 
DATE:    20/06/23 05:30:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 200623A ( Fermi GBM team, GCN 28011) errorbox  924 sec after notice time and 957 sec after trigger time at 2020-06-23 03:33:58 UT, with upper limit up to  18.8 mag. The observations began at zenith distance = 63 deg. The sun  altitude  is -27.3 deg. 

The galactic latitude b = 45 deg., longitude l = 98 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1387999

We obtain a following upper limits.  

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

     988 | 2020-06-23 03:33:58 |          MASTER-IAC | (15h 03m 20.96s , +60d 01m 51.3s) |   C |    60 | 18.8 |        
     988 | 2020-06-23 03:33:58 |          MASTER-IAC | (14h 46m 59.24s , +60d 06m 59.1s) |   C |    60 | 18.3 |        
    1108 | 2020-06-23 03:35:59 |          MASTER-IAC | (14h 53m 55.06s , +62d 00m 52.3s) |   C |    60 | 18.5 |        
    1108 | 2020-06-23 03:35:59 |          MASTER-IAC | (14h 36m 29.92s , +62d 06m 01.8s) |   C |    60 | 18.2 |        
    1226 | 2020-06-23 03:37:56 |          MASTER-IAC | (15h 12m 34.01s , +58d 01m 45.3s) |   C |    60 | 18.6 |        
    1226 | 2020-06-23 03:37:56 |          MASTER-IAC | (14h 57m 07.88s , +58d 06m 52.4s) |   C |    60 | 18.3 |        
    1346 | 2020-06-23 03:39:56 |          MASTER-IAC | (15h 03m 20.54s , +60d 00m 47.4s) |   C |    60 | 18.7 |        
    1346 | 2020-06-23 03:39:56 |          MASTER-IAC | (14h 46m 59.37s , +60d 05m 55.7s) |   C |    60 | 18.5 |        
    1466 | 2020-06-23 03:41:56 |          MASTER-IAC | (14h 53m 54.70s , +61d 59m 46.6s) |   C |    60 | 18.5 |        
    1466 | 2020-06-23 03:41:56 |          MASTER-IAC | (14h 36m 30.27s , +62d 04m 56.3s) |   C |    60 | 18.2 |        
    1587 | 2020-06-23 03:43:57 |          MASTER-IAC | (15h 12m 38.65s , +57d 59m 56.1s) |   C |    60 | 18.6 |        
    1587 | 2020-06-23 03:43:58 |          MASTER-IAC | (14h 57m 13.35s , +58d 05m 03.5s) |   C |    60 | 18.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200623A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28013
SUBJECT: GRB 200623A: Swift/BAT-GUANO detection and arcminute localization of a short GRB
DATE:    20/06/23 13:18:09 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (PSU), Aaron Tohuvavohu (U Toronto), Jamie Kennea
(PSU), and Peter Veres (UAH) report:

Swift/BAT did not trigger on GRB 2006023A (T0: 2020-06-23 03:18:00
UTC, Fermi/GBM Team GCN 28011).

The Fermi/GBM notice, distributed at T0+24 seconds triggered the Swift
Mission Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, arXiv: 2005.01751). Upon
trigger by these notices, 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.

In a ground analysis of the data, we detect the burst in the full
detector-summed rates (no localization information) with an SNR of
~12.
The detected duration is ~0.2 seconds.

With a maximum likelihood analysis (DeLaunay et al. 2020, in prep.) on
the event-mode data we detect a location for the burst with a square
root of the test statistic, sqrt(TS), of 9.8. The sqrt(TS) behaves
similarly to SNR.
Using the normal BAT imaging technique, we find an SNR of 6.4 at the
same location.

The BAT ground-calculated position is
RA, Dec = 242.0952, +53.4678 deg which is
   RA(J2000)  = 16h 8m 22.8s
   Dec(J2000) = +53d 28â€™ 4â€
with an uncertainty of 4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 67.19%.

This position is consistent with the Fermi GBM localization (GCN
28011), falling on the 58% containment contour.

XRT and UVOT follow-up has been triggered. 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/

[GCN OPS NOTE: Per author's request, the sexagesimal Dec
was changed from +51d 28' 4"  to  +53 28' 4".]


GRB_name: GRB200623A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28015
SUBJECT: GRB 200623A: Swift ToO observations
DATE:    20/06/23 13:56:58 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Swift/BAT GRB 200623A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021005

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Swift/BAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

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

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


GRB_name: GRB200623A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28016
SUBJECT: GRB 200623A: Correction to GCN 28013
DATE:    20/06/23 14:23:56 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

The sexagesimal coordinates reported for the Swift/BAT-GUANO
localization of GRB 200623A have a typo.
The decimal coordinates in the original circular are correct.

The correct coordinates are RA, Dec: 242.0952, +53.4678:
   RA(J2000)  = 16h 8m 22.8s
   Dec(J2000) =  +53d 28' 4"

I apologize for any inconvenience caused.


GRB_name: GRB200623B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28017
SUBJECT: GRB 200623B: Fermi GBM Final Real-time Localization
DATE:    20/06/23 18:13:12 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 18:02:48 UT on 23 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200623B (trigger 614628173.95347 / 200623752).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 344.9, Dec = -47.0 (J2000 degrees, equivalent to J2000 22h 59m, -47d 00'), with a statistical uncertainty of 5.2 degrees.

The angle from the Fermi LAT boresight is 65.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200623752/quicklook/glg_skymap_all_bn200623752.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200623752/quicklook/glg_healpix_all_bn200623752.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200623752/quicklook/glg_lc_medres34_bn200623752.gif


GRB_name: GRB200623B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28018
SUBJECT: Fermi GRB 200623B: Global MASTER-Net observations report 
DATE:    20/06/23 18:30:18 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200623B ( Fermi GBM team, GCN 28017) errorbox  552 sec after notice time and 590 sec after trigger time at 2020-06-23 18:12:39 UT, with upper limit up to  18.9 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -30.9 deg. 

The galactic latitude b = -43 deg., longitude l = 328 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1388895

We obtain a following upper limits.  

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

     620 | 2020-06-23 18:12:39 |         MASTER-SAAO | (21h 51m 50.01s , -64d 03m 54.4s) |   C |    60 | 18.6 |        
     713 | 2020-06-23 18:14:12 |         MASTER-SAAO | (22h 08m 29.53s , -66d 03m 58.4s) |   C |    60 | 18.9 |        
     713 | 2020-06-23 18:14:12 |         MASTER-SAAO | (22h 25m 14.90s , -66d 03m 19.6s) |   C |    60 | 18.6 |        
     793 | 2020-06-23 18:15:32 |         MASTER-SAAO | (22h 37m 18.63s , -68d 05m 13.2s) |   C |    60 | 18.9 |        
     793 | 2020-06-23 18:15:32 |         MASTER-SAAO | (22h 55m 31.23s , -68d 04m 31.7s) |   C |    60 | 18.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200623A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28019
SUBJECT: GRB 200623A: Fermi GBM observation
DATE:    20/06/23 21:46:47 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

"At 03:18:00.64 UT on 23 June 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200623A (trigger 614575085 / 200623138)
which was also detected by the Swift/BAT-GUANO (DeLaunay et al., GCN 28013).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 36
degrees.

The GBM light curve consists of a single pulse
with a duration (T90) of about 0.6 s (50-300 keV).
The time-averaged spectrum from T0-64 ms to T0 is
best fit by a simple power law function with index -1.09 +/- 0.09.


The event fluence (10-1000 keV) in this time interval is
(5.2 +/- 0.6)E-7 erg/cm^2. The 64-ms peak photon flux measured
starting from T0-64 ms in the 10-1000 keV band
is 4.7 +/- 1.0 ph/s/cm^2.

A power law function with an exponential
high-energy cutoff fits the spectrum equally well
with Epeak= 353 +/- 131 keV, alpha = -0.07 +/- 0.53.


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: GRB200623A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28020
SUBJECT: GRB 200623A: AbAO afterglow candidate within XRT #2
DATE:    20/06/23 23:00:03 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), R. Ya. Inasaridze (AbAO), V.R. 
Ayvazian (AbAO),  G. V.  Kapanadze (AbAO),   E. Mazaeva (IKI), A. 
Volnova  (IKI),  I. Molotov (KIAM) report on behalf of  GRB IKI FuN:

We observed the field of Swift/BAT-GUANO position (DeLaunay et al., GCNs 
28013, 28016) of  GRB 200623A (Fermi GBM team,  GCN 28011; Veres et al., 
GCN 28019) with AS-32 (0.7m) telescope of Abastumani Observatory 
starting on 2020-06-23 (UT) 18:46:58.  We  detected only one object 
within the XRT #2 source localization 
(https://www.swift.ac.uk/ToO_GRBs/00021005/). The source is not 
presented in SDSS DR12. We suggest the object could be afterglow of  GRB 
200623A. However at this time we cannot confirm variability of the 
object.   Preliminary photometry of the object is following.

Date       UT start  t-T0    Filter Exp.  OT    Err. UL
                     (mid, days)     (s)
2020-06-23 18:46:58  0.66456 R      56*60 21.88 0.17 22.6

No new objects were found in the localization of the XRT # 3 source.

The photometry is based on nearby USNO-B1.0 stars
UUSNO-B1.0_id R2

1434-0283797 15.99
1434-0253851 17.48


GRB_name: GRB200623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28021
SUBJECT: GRB 200623A: TNG optical observations
DATE:    20/06/23 23:09:31 GMT
FROM:    Paolo D'Avanzo at INAF - OAB  <paolo.davanzo@inaf.it>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-SSDC), G. Andreuzzi, D. Carosati (INAF-TNG) on behalf of the CIBO collaboration report:

We observed the field of GRB 200623A (Fermi/GBM Team, GCN Circ. 28011; DeLaunay et al., GCN Circ. 28013; Veres and Meegan, 
GCN Circular. 28019) with the Italian 3.6m TNG telescope equipped with DOLORES in imaging mode. A series of images were 
obtained with the r-sdss filter on 2020-06-23 from 21:23:29 UT to 21:44:01 UT (i.e. about 18.3 hours after the burst) covering the entire 
Swift/BAT-GUANO error circle reported by DeLaunay et al. (GCN Circ. 28013,). Further observations are in progress. 

No obvious afterglow candidate is detected inside the BAT-GUANO error circle. 

Inside the 5" radius error circle of the Swift/XRT source #3 (see Evans, GCN Circ. 28015 and https://www.swift.ac.uk/ToO_GRBs/00021005) 
we detect a faint source at the following coordinates: 

RA(J2000), Dec (J2000) = 16:07:59.11, +53:28:39.0  (+/- 0.5"Â).

From preliminary photometry, we estimate for this object a magnitude r ~ 24.2 (AB, calibrated against the SDSS catalogue). This source is 
apparently not visible in the SDSS and Pan-STARRS archival images of this field. Given the faintness of the source, no conclusion can be 
derived about its variability and about its association to GRB 200623A. 

We note that the 5" radius error circle of the Swift/XRT source #3 is consistent with the catalogued galaxy SDSS J160758.62+532842.2 whose 
photometric redshift is 0.33 +/- 0.05. 

The position of the the Swift/XRT source #2 is outside the field of view of our images, therefore we cannot provide information on the optical 
afterglow candidate reported by Belkin et al. (GCN Circ. 28020). 


GRB_name: GRB200623A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28022
SUBJECT: GRB 200623A: OAJ deep multi-color imaging, XRT #2 is pre-detected
DATE:    20/06/24 01:07:31 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), M. Blazek, C. C. Thoene, J. F. Agui Fernandez (all 
HETH/IAA-CSIC), V. Tilve, A. Moreno Signes, and H. Vasquez Ramio (all 
CEFCA) report:

We observed the error circle of the short GRB 200623A (Fermi GBM 
detection and analysis: Fermi GBM Team, GCN #28011, Veres & Meegan, GCN 
#28019; Swift BAT/GUANO localization: DeLaunay et al., GCN #28013) with 
the T80 0.8m telescope at the Observatorio de Javalambre (Teruel, 
Spain). Observations consisted of 3 x 500 s in g', 3 x 500 s in r',  8 x 
180 s in i', and 8 x 180 s in z', at midtimes 0.816779, 0.798439, 
0.779694, and 0.755722 days after the GRB, respectively.

At the position of XRT source #1, the known quasar from the Veron-Cetty 
& Veron 2006 catalog is clearly detected.

At the position of XRT source #2, we clearly detect the source proposed 
by Belkin et al. (GCN #28020) as a candidate afterglow. Measured against 
three nearby SDSS comparison stars, we find (AB mags):

g' = 23.70 +/- 0.30 mag;
r' = 22.55 +/- 0.15 mag;
i' = 21.54 +/- 0.15 mag;
z' = 20.74 +/- 0.10 mag,

indicating this is a very red source. We assume that the observations of 
Belkin et al. were performed without a filter, this would explain the 
brighter magnitude they find (their use of comparison stars from the 
USNO catalog may also play a role).

These very red colors are untypical for a GRB afterglow. Furthermore, 
comparison with images form PanSTARRS clearly reveals a pre-detection of 
the source at a similar magnitude and color, see:

https://www.iaa.csic.es/~deugarte/GRBs/200623A/200623A_color2.jpg

for a comparison. We therefore believe it is unlikely that this source 
is associated with GRB 200623A (additionally, the XRT detection is of 
low significance for now).

At the position of XRT source #3, we detected multiple sources in the 
vicinity also seen in PanSTARRS imaging. The faint source detected by 
the TNG (D'Avanzo et al., GCN #28021), may be vaguely detected in our r' 
and z' images, but it is unclear how much this could be due to the PSF 
of a nearby bright star. We present a second comparison image here:

https://www.iaa.csic.es/~deugarte/GRBs/200623A/200623A_color.jpg

No other obviously bright afterglow candidate is detected in the BAT 
error circle, however, a second epoch of comparable depth would be 
needed for a more detailed analysis.


GRB_name: GRB200623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28023
SUBJECT: GRB 200623A: Swift-XRT observations
DATE:    20/06/24 16:22:54 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), T.
Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), M.G. Bernardini
(INAF-OAB), D.N. Burrows (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-detected burst GRB 200623A (James DeLaunay et al. GCN Circ.
28013), collecting 5.0 ks of Photon Counting (PC) mode data between
T0+37.8 ks and T0+50.1 ks. 

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

Source 1:
  RA (J2000):  242.2874  =  16:09:8.97
  Dec (J2000): +53.5321  =  +53:31:55.6
  Error: 4.4 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (3.5 [+1.2, -1.0])e-3 ct s^-1   
  Distance: 406 arcsec from Swift/BAT position.
  Flux: (1.09 [+0.39, -0.32])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 2:
  RA (J2000):  242.1106  =  16:08:26.55
  Dec (J2000): +53.3466  =  +53:20:47.9
  Error: 5.1 arcsec (radius, 90% conf.)
  Count-rate: (1.19 [+0.79, -0.56])e-3 ct s^-1  
  Distance: 462 arcsec from Swift/BAT position.

Source 3:
  RA (J2000):  241.9966  =  16:07:59.18
  Dec (J2000): +53.4786  =  +53:28:42.8
  Error: 5.0 arcsec (radius, 90% conf.)
  Count-rate: (3.10 [+1.11, -0.91])e-3 ct s^-1  
  Distance: 272 arcsec from Swift/BAT position.
  Flux: (1.96 [+0.70, -0.58])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 1 is consistent with a known quasar, [VV2006] J160908.9+533153.
Source 2 is poorly detected and is likely to be a background 
fluctuation.
Source 3 is not a known X-ray source, its position is consistent with a
background galaxy, SDSS J160758.62+532842.2 (D'Avanzo et al., GCN
#28021).

Follow up observation of source 3 are planned to be carried out at the
end of this week.

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/00021005.

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


GRB_name: GRB200623B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28024
SUBJECT: IPN triangulation of GRB 200623B (short)
DATE:    20/06/24 16:50:10 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

K. Hurley, on behalf of the IPN,

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

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

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

The short-duration GRB 200623B
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 28017)
has been detected by Fermi (GBM trigger 614628173),
Konus-Wind, INTEGRAL (SPI-ACS), and Swift (BAT), so far,
at about 64968 s UT (18:02:48).
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:
   343.079 (22h 52m 19s)  -53.378 (-53d 22' 41")
  Corners:
   330.417 (22h 01m 40s)  -61.535 (-61d 32' 06")
   328.804 (21h 55m 13s)  -63.180 (-63d 10' 48")
   349.757 (23h 19m 02s)  -41.929 (-41d 55' 45")
   348.242 (23h 12m 58s)  -43.351 (-43d 21' 04")
  ----------------------------------------------
The error box area is 17.6 sq. deg, and its maximum
dimension is 24.5 deg (the minimum one is 46 arcmin).
The Sun distance was about 115 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM final position (GCN Circ. 28017).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200623_T64972/IPN/

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


GRB_name: GRB200623A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28025
SUBJECT: GRB 200623A: Swift/UVOT Upper Limits
DATE:    20/06/24 19:15:37 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) and B. Sbarufatti (PSU) report on behalf of the Swift/UVOT team:

The Swift/UVOT began target-of-opportunity observations of the field of GRB 200623A 37910 s after 
the Guano and GBM trigger (Fermi GBM team, GCN Circ. 28011; Debaunay et al., GCN Circ. 28013).

No significant new sources were found at the positions of the XRT candidate sources 1 and 3 
(Tohuvavohu et al., GCN Circ. 28023). XRT source 2 was outside the field of view for all exposures.

Preliminary 3-sigma upper limit 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            37910        45836         4299         >22.4

The magnitude in the table is not corrected for the Galactic extinction due to the reddening of 
E(B-V) = 0.012 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB200623A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28026
SUBJECT: GRB 200623A: MMT observations at XRT Source #3
DATE:    20/06/24 21:47:34 GMT
FROM:    Jillian Rastinejad at Northwestern Univ.  <jillianrastinejad2024@u.northwestern.edu>

J. Rastinejad, Y. Dong, W. Fong, K. Paterson, and A. Rouco Escorial (Northwestern) report:

"We observed the location of the short-duration GRB 200623A at the position of XRT source #3 (Tohuvavohu et al. GCN 28023) within the GRB localization (Fermi GBM Team GCN 28011, DeLaunay et al. GCN 28013) with the MMTCam mounted on the MMT 6.5-meter telescope on Mount Hopkins, Arizona. We acquired 18 x 120-sec observations in the r-band at a mid-time of 2020 June 24.18 UT (25.03 hrs post-burst). The observations have a mean airmass of 1.11, seeing of 1.36", and were taken in thin clouds.

In the vicinity of the XRT Source #3 position, we detect several sources that are also apparent in SDSS and Pan-STARRs imaging. We find the brightest nearby galaxy, SDSS J160758.62+532842.2 (Dâ€™Avanzo et al. GCN 28021) to be consistent with the catalogued magnitude in SDSS (Alam et al. 2015). At the position of the XRT source, the 3-sigma limiting magnitude within the error circle is r > 23.1 AB magnitude, calibrated to SDSS and not corrected for Galactic Extinction. We note that our imaging was not deep enough to detect the faint source found by Dâ€™Avanzo et al. (GCN 28021).

Further observations are planned. We thank the MMT staff for their assistance with planning and executing these observations."

[GCN OPS NOTE(24jun20): Per author's request, "GRB 200624A: " was added to the SUBJECT field of the circular.]


GRB_name: GRB200625A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28028
SUBJECT: GRB 200625A: Fermi GBM Final Real-time Localization
DATE:    20/06/25 12:56:11 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 12:45:49 UT on 25 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200625A (trigger 614781954.14304 / 200625532).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 169.9, Dec = -22.0 (J2000 degrees, equivalent to J2000 11h 19m, -22d 00'), with a statistical uncertainty of 8.8 degrees.

The angle from the Fermi LAT boresight is 104.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200625532/quicklook/glg_skymap_all_bn200625532.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200625532/quicklook/glg_healpix_all_bn200625532.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200625532/quicklook/glg_lc_medres34_bn200625532.gif


GRB_name: GRB200625A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28029
SUBJECT: Fermi GRB 200625A: Global MASTER-Net observations report 
DATE:    20/06/25 17:30:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200625A ( Fermi GBM team, GCN 28028) errorbox  14507 sec after notice time and 14536 sec after trigger time at 2020-06-25 16:48:05 UT, with upper limit up to  19.6 mag. Observations started at twilight.  The observations began at zenith distance = 35 deg. The sun  altitude  is -13.4 deg. 

The galactic latitude b = 14 deg., longitude l = 260 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1389977

We obtain a following upper limits.  

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

   14567 | 2020-06-25 16:48:05 |         MASTER-SAAO | (09h 42m 15.87s , -27d 53m 20.4s) |   C |    60 | 19.3 |        
   14567 | 2020-06-25 16:48:05 |         MASTER-SAAO | (09h 34m 31.43s , -27d 54m 33.0s) |   C |    60 | 19.0 |        
   14647 | 2020-06-25 16:49:25 |         MASTER-SAAO | (09h 32m 01.48s , -25d 54m 32.3s) |   C |    60 | 19.4 |        
   14647 | 2020-06-25 16:49:25 |         MASTER-SAAO | (09h 24m 25.35s , -25d 55m 45.4s) |   C |    60 | 19.1 |        
   14727 | 2020-06-25 16:50:45 |         MASTER-SAAO | (09h 49m 43.62s , -25d 55m 02.8s) |   C |    60 | 19.4 |        
   14727 | 2020-06-25 16:50:45 |         MASTER-SAAO | (09h 42m 07.31s , -25d 56m 14.8s) |   C |    60 | 19.1 |        
   14806 | 2020-06-25 16:52:05 |         MASTER-SAAO | (09h 40m 14.87s , -23d 54m 49.1s) |   C |    60 | 19.4 |        
   14806 | 2020-06-25 16:52:05 |         MASTER-SAAO | (09h 32m 46.08s , -23d 56m 01.3s) |   C |    60 | 19.2 |        
   14886 | 2020-06-25 16:53:25 |         MASTER-SAAO | (09h 42m 17.87s , -27d 53m 21.8s) |   C |    60 | 19.5 |        
   14886 | 2020-06-25 16:53:25 |         MASTER-SAAO | (09h 34m 33.52s , -27d 54m 32.8s) |   C |    60 | 19.2 |        
   14966 | 2020-06-25 16:54:45 |         MASTER-SAAO | (09h 31m 58.93s , -25d 55m 27.3s) |   C |    60 | 19.5 |        
   14966 | 2020-06-25 16:54:45 |         MASTER-SAAO | (09h 24m 22.77s , -25d 56m 39.4s) |   C |    60 | 19.3 |        
   15046 | 2020-06-25 16:56:04 |         MASTER-SAAO | (09h 42m 12.57s , -25d 54m 28.9s) |   C |    60 | 19.3 |        
   15126 | 2020-06-25 16:57:24 |         MASTER-SAAO | (09h 40m 09.34s , -23d 54m 15.1s) |   C |    60 | 19.6 |        
   15126 | 2020-06-25 16:57:24 |         MASTER-SAAO | (09h 32m 40.58s , -23d 55m 26.8s) |   C |    60 | 19.4 |        
   15206 | 2020-06-25 16:58:44 |         MASTER-SAAO | (09h 35m 13.23s , -29d 53m 37.1s) |   C |    60 | 19.5 |        
   15206 | 2020-06-25 16:58:44 |         MASTER-SAAO | (09h 27m 19.84s , -29d 54m 47.7s) |   C |    60 | 19.3 |        
   15285 | 2020-06-25 17:00:04 |         MASTER-SAAO | (09h 24m 15.09s , -27d 54m 53.3s) |   C |    60 | 19.5 |        
   15285 | 2020-06-25 17:00:04 |         MASTER-SAAO | (09h 16m 30.81s , -27d 56m 04.7s) |   C |    60 | 19.3 |        
   15577 | 2020-06-25 17:04:56 |         MASTER-SAAO | (09h 35m 20.29s , -29d 55m 08.6s) |   C |    60 | 19.5 |        
   15577 | 2020-06-25 17:04:56 |         MASTER-SAAO | (09h 27m 27.09s , -29d 56m 16.9s) |   C |    60 | 19.4 |        
   15657 | 2020-06-25 17:06:16 |         MASTER-SAAO | (09h 24m 12.21s , -27d 54m 16.1s) |   C |    60 | 19.6 |        
   15657 | 2020-06-25 17:06:16 |         MASTER-SAAO | (09h 16m 28.28s , -27d 55m 25.3s) |   C |    60 | 19.3 |        
   15737 | 2020-06-25 17:07:35 |         MASTER-SAAO | (09h 53m 43.70s , -29d 54m 39.3s) |   C |    60 | 19.6 |        
   15737 | 2020-06-25 17:07:35 |         MASTER-SAAO | (09h 45m 50.32s , -29d 55m 46.5s) |   C |    60 | 19.5 |        
   15817 | 2020-06-25 17:08:55 |         MASTER-SAAO | (10h 00m 26.93s , -27d 53m 20.6s) |   C |    60 | 19.6 |        
   15817 | 2020-06-25 17:08:55 |         MASTER-SAAO | (09h 52m 42.64s , -27d 54m 28.0s) |   C |    60 | 19.4 |        
   15896 | 2020-06-25 17:10:15 |         MASTER-SAAO | (09h 57m 37.66s , -23d 53m 52.2s) |   C |    60 | 19.5 |        
   15896 | 2020-06-25 17:10:15 |         MASTER-SAAO | (09h 50m 08.91s , -23d 55m 00.8s) |   C |    60 | 19.4 |        
   15977 | 2020-06-25 17:11:35 |         MASTER-SAAO | (09h 31m 34.82s , -21d 53m 30.1s) |   C |    60 | 19.6 |        
   15977 | 2020-06-25 17:11:35 |         MASTER-SAAO | (09h 24m 13.01s , -21d 54m 40.5s) |   C |    60 | 19.4 |        
   16057 | 2020-06-25 17:12:55 |         MASTER-SAAO | (09h 45m 52.65s , -29d 55m 20.0s) |   C |    60 | 19.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200626A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28030
SUBJECT: GRB 200626A: Fermi GBM Final Real-time Localization
DATE:    20/06/26 02:41:47 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 02:31:31 UT on 26 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200626A (trigger 614831496.751792 / 200626105).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 87.3, Dec = 16.1 (J2000 degrees, equivalent to J2000 05h 49m, 16d 06'), with a statistical uncertainty of 15.2 degrees.

The angle from the Fermi LAT boresight is 53.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200626105/quicklook/glg_skymap_all_bn200626105.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200626105/quicklook/glg_healpix_all_bn200626105.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200626105/quicklook/glg_lc_medres34_bn200626105.gif


GRB_name: GRB200625A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28031
SUBJECT: GRB 200625A: Swift ToO observations
DATE:    20/06/26 03:02:16 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 200625A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021006

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: GRB200626A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28032
SUBJECT: Fermi GRB 200626A: Global MASTER-Net observations report 
DATE:    20/06/26 06:15:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 200626A ( Fermi GBM team, GCN 28030) errorbox  4639 sec after notice time and 4666 sec after trigger time at 2020-06-26 03:49:18 UT, with upper limit up to  17.8 mag. The observations began at zenith distance = 77 deg. The sun  altitude  is -25.2 deg. 

The galactic latitude b = -11 deg., longitude l = 175 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1390351

We obtain a following upper limits.  

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

    4697 | 2020-06-26 03:49:18 |          MASTER-IAC | (03h 16m 07.72s , +33d 51m 22.9s) |   C |    60 | 14.2 |        
    4817 | 2020-06-26 03:51:18 |          MASTER-IAC | (03h 20m 54.72s , +35d 50m 25.6s) |   C |    60 | 16.4 |        
    5412 | 2020-06-26 04:01:14 |          MASTER-IAC | (03h 16m 07.88s , +33d 52m 13.9s) |   C |    60 | 17.1 |        
    5536 | 2020-06-26 04:03:18 |          MASTER-IAC | (03h 20m 53.05s , +35d 51m 39.3s) |   C |    60 | 17.4 |        
    6485 | 2020-06-26 04:19:06 |          MASTER-IAC | (03h 20m 56.43s , +21d 56m 24.2s) |   C |    60 | 17.7 |        
    6607 | 2020-06-26 04:21:08 |          MASTER-IAC | (03h 18m 15.59s , +19d 57m 22.7s) |   C |    60 | 17.6 |        
    7210 | 2020-06-26 04:31:11 |          MASTER-IAC | (03h 21m 00.87s , +21d 55m 47.1s) |   C |    60 | 17.8 |        
    7329 | 2020-06-26 04:33:10 |          MASTER-IAC | (03h 18m 17.27s , +19d 57m 03.8s) |   C |    60 | 17.8 |        
    7448 | 2020-06-26 04:35:09 |          MASTER-IAC | (03h 49m 12.31s , +27d 55m 51.9s) |   C |    60 | 17.3 |        
    7565 | 2020-06-26 04:37:06 |          MASTER-IAC | (03h 58m 44.02s , +31d 57m 26.1s) |   C |    60 | 17.4 |        
    7682 | 2020-06-26 04:39:03 |          MASTER-IAC | (03h 53m 38.68s , +29d 56m 50.8s) |   C |    60 | 17.5 |        
    7802 | 2020-06-26 04:41:03 |          MASTER-IAC | (03h 49m 09.29s , +27d 57m 46.4s) |   C |    60 | 17.4 |        
    7925 | 2020-06-26 04:43:06 |          MASTER-IAC | (03h 58m 44.12s , +31d 56m 52.9s) |   C |    60 | 17.4 |        
    8042 | 2020-06-26 04:45:03 |          MASTER-IAC | (03h 53m 38.41s , +29d 55m 48.6s) |   C |    60 | 17.5 |        
    8160 | 2020-06-26 04:47:01 |          MASTER-IAC | (04h 04m 13.34s , +33d 56m 10.2s) |   C |    60 | 17.4 |        
    8160 | 2020-06-26 04:47:01 |          MASTER-IAC | (04h 13m 58.68s , +33d 52m 01.7s) |   C |    60 | 13.3 |        
    8759 | 2020-06-26 04:57:00 |          MASTER-IAC | (04h 04m 11.95s , +33d 58m 00.3s) |   C |    60 | 17.2 |        
    8759 | 2020-06-26 04:57:00 |          MASTER-IAC | (04h 13m 58.27s , +33d 53m 52.7s) |   C |    60 | 16.2 |        
    8882 | 2020-06-26 04:59:03 |          MASTER-IAC | (03h 58m 56.00s , +23d 57m 11.2s) |   C |    60 | 17.1 |        
    9002 | 2020-06-26 05:01:03 |          MASTER-IAC | (03h 55m 24.64s , +21d 58m 07.1s) |   C |    60 | 16.9 |        
    9121 | 2020-06-26 05:03:02 |          MASTER-IAC | (03h 45m 11.47s , +25d 56m 48.8s) |   C |    60 | 16.9 |        
    9121 | 2020-06-26 05:03:02 |          MASTER-IAC | (03h 54m 11.50s , +25d 52m 40.0s) |   C |    60 | 14.9 |        
    9239 | 2020-06-26 05:05:01 |          MASTER-IAC | (03h 58m 56.30s , +23d 56m 09.2s) |   C |    60 | 16.9 |        
    9365 | 2020-06-26 05:07:07 |          MASTER-IAC | (03h 55m 30.81s , +21d 56m 10.3s) |   C |    60 | 16.4 |        
    9483 | 2020-06-26 05:09:04 |          MASTER-IAC | (03h 45m 08.45s , +25d 57m 31.9s) |   C |    60 | 16.4 |        
    9483 | 2020-06-26 05:09:04 |          MASTER-IAC | (03h 54m 08.22s , +25d 53m 24.9s) |   C |    60 | 15.9 |        
    9602 | 2020-06-26 05:11:04 |          MASTER-IAC | (03h 23m 58.69s , +23d 55m 30.6s) |   C |    60 | 16.9 |        
    9602 | 2020-06-26 05:11:04 |          MASTER-IAC | (03h 32m 49.37s , +23d 51m 25.4s) |   C |    60 | 16.3 |        
    9720 | 2020-06-26 05:13:02 |          MASTER-IAC | (03h 24m 26.97s , +17d 52m 57.1s) |   C |    60 | 16.2 |        
    9960 | 2020-06-26 05:17:01 |          MASTER-IAC | (03h 23m 54.61s , +23d 57m 26.7s) |   C |    60 | 16.4 |        
    9960 | 2020-06-26 05:17:01 |          MASTER-IAC | (03h 32m 45.38s , +23d 53m 21.7s) |   C |    60 | 15.8 |        
   10079 | 2020-06-26 05:19:00 |          MASTER-IAC | (03h 24m 27.02s , +17d 52m 14.0s) |   C |    60 | 15.8 |        
   10551 | 2020-06-26 05:26:53 |          MASTER-IAC | (03h 38m 49.79s , +15d 53m 34.7s) |   C |    60 | 14.3 |        
   10667 | 2020-06-26 05:28:48 |          MASTER-IAC | (03h 36m 53.39s , +13d 52m 32.5s) |   C |    60 | 14.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28033
SUBJECT: GRB 200623A : SMA observations at Swift/XRT Source #3  
DATE:    20/06/26 07:19:35 GMT
FROM:    Yuji Urata at Nat. Central U.  <urata@astro.ncu.edu.tw>

Kuiyun Huang (CYCU), Yuji Urata (NCU), Glen Petitpas (CfA) 
report

We used SMA to observe the location of the Swift/XRT source #3 
(Evans, GCN Circ. 28015) as one of the afterglow candidates of
GRB200623A (Fermi/GBM Team, GCN Circ. 28011; DeLaunay et al., GCN
Circ. 28013, 28016).  The 230 GHz observation was started at ~1 days
after the burst.  No clear submm source at the Swift/XRT sources #3
position was found brighter than ~1 mJy.

We thank the staff of SMA.


GRB_name: GRB200623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28034
SUBJECT: GRB 200623A: LBT optical observations
DATE:    20/06/26 09:30:40 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi (INAF-OAS) and P. D'Avanzo (INAF-OA Brera) report on behalf of 
the CIBO collaboration:

We observed the field of GRB200623A (DeLaunay et al., GCN 28013) 
simultaneously in the r' and z' bands with the LBC imager mounted on LBT 
(Mt Graham, AZ, USA). Observations started at 05:58 UT on 2020-06-25, 
50.7 hr after the GRB trigger and finished at 06:24 UT and allowed us to 
obtain 20min of exposure in each band. Observations were performed under 
good seeing conditions (seeing ~0.9") and reached a depth of r~26 mag.

The images covered all the three sources found by XRT (Sbarufatti et 
al., GCN 28023). No new point source is detected within their error circles.

Image subtraction against TNG r-band images obtained on 2020-06-23 
(D'Avanzo et al., GCN 28021) using HOTPANTS (v5.1.11) does not reveal 
any flux variation in the candidate found within the error circle of the 
XRT source #3. The near-by galaxy at z~0.33 noticed by D'Avanzo et al. 
(GCN 28021) is too close to saturation in LBC images, preventing us to 
make any statement about possible flux variations within the galaxy.

We also note that a faint, extended source is present within the XRT 
error circle of source #3, visible in both the r' and z' images, and not 
mentioned in previous reports about this event. This is also a candidate 
host galaxy of XRT source #3 though with a higher chance association 
probability compared to the brighter galaxy. Further Swift/XRT 
observations will help establishing variability and possibly reducing 
the X-ray position uncertainty.

We acknowledge the excellent support from the LBTO and LBT-INAF staff, 
particularly B. Rothberg, F. Cusano, S. Paiano and D. Paris, in 
obtaining these observations.


GRB_name: GRB200625A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28035
SUBJECT: GRB 200625A: Fermi-LAT detection is likely a flare from PKS 1127-14
DATE:    20/06/26 14:53:07 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

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

On June 25th, 2020, Fermi-LAT detected high-energy emission potentially related to the afterglow of GRB 200625A, detected by Fermi-GBM (trigger 614781954/200625532 Fermi GBM Team GCN 28028).

The best LAT on-ground location is found to be

RA, Dec 172.8, -14.7 (degrees, J2000)

with an error radius of 0.2 deg (90% containment, statistical error only). This was 97 deg from the LAT boresight at the time of the GBM trigger:

T0 =  12:45:49.14 UT.

The position is 8 degrees from the GBM location, and came into the LAT FoV ~3500 s after the trigger. The data from Fermi-LAT show a significant increase in the event rate in the time interval 3500-7000 s after the GBM trigger. The photon flux above 100 MeV in this time interval is 5.9e-07 +/- 2.9 e-07 ph/cm2/s, and the estimated photon index above 100 MeV is -1.8 +/-  0.3.

However, we note that the best localization is close (16 arcmin) from the known high-energy source PKS 1127-14 (4FGL J1129.8-1447). Analysis reveals that the significance of the excess increases in the following observation window, and reaches a maximum in the time interval T0+15ks to T0+18ks (photon flux 1.7e-06 +/- 5.7e-7 ph/cm2/s; spectral index -2.1 +/- 0.24).

The increased significance at later times points to PKS 1127-14 (an FSRQ at z=1.18) as the source of the emission, rather than GRB 200625A. However, we do not find any similar excess in the time windows before the trigger (T0-8ks to T0-5ks) or at later times (>T0+30ks), indicating a short and bright flare.

The initial detection of a transient event near the position of GRB 200625A led to a LAT offline position notice being issued. As a result, a Swift ToO observation has been made for this event (likely an FSRQ flare).

The Fermi-LAT point of contact for this burst is Magnus Axelsson (magaxe@kth.se<mailto:magaxe@kth.se>).

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: GRB200623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28036
SUBJECT: GRB 200623A: Further MMTCam Observations of XRT Source #3
DATE:    20/06/27 23:23:16 GMT
FROM:    Wen-fai Fong at Northwestern U  <wfong@northwestern.edu>

W. Fong (Northwestern) reports:

"We re-visited the location of XRT source #3 of the short GRB 200623A (Fermi-GBM Collab. et al., GCN 28011; DeLaunay et al., GCN 28013; Tohuvavohu et al., GCN 28023) with the MMT/MMTCam at a mid-time of 2020 June 26.176 UT (3.04 days post-burst and 2.0 days after our initial observations: Rastinejad et al., GCN 28026). We acquired 21x120-sec of r-band imaging in 0.88" seeing, and the 3-sigma depth of our image is 24.4 AB mag.

Upon inspection of the XRT source #3 position (90% confidence), we detect the faint optical source first reported in TNG observations (D'Avanzo et al.; GCN 28021) with r = 24.3 +/- 0.3 mag, at the same flux level as previous detections. In addition to a few catalogued sources, we report on an additional source toward the Eastern edge of the XRT position and in the wings of the bright star, with RA = 16:07:59.64, Dec = +53:28:43.6 (J2000) and r~22.2 AB mag. This source was marginally detected in our previous set of imaging although partially blended with the bright star, and it is not possible to discern at present whether this source is point-like or extended in nature. Finally, we do not detect the extended LBT source at the center of the XRT position (Rossi and D'Avanzo et al., GCN 28034), likely due to lack of sensitivity.

We perform image subtraction relative to our previous epoch, and do not detect any significant residuals. Thus, we find no evidence for significant variability in or around the XRT source #3 position, enabling a limit of r > 23.0 AB mag at 25.03 hrs post-burst on optical afterglow emission associated with this XRT candidate (c.f., Rastinejad et al., GCN 28026).

We thank Nelson Caldwell and Michael Calkins at the MMT for the rapid scheduling and execution of these observations."


GRB_name: GRB200623B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28037
SUBJECT: Konus-Wind detection of short/hard GRB 200623B
DATE:    20/06/28 18:08:03 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

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

The short-duration, hard-spectrum GRB200623B
(IPN triangulation: Ridnaia et al., GCN 28024)
triggered Konus-Wind at T0=64972.561 s UT (18:02:52.561).

The light curve of the burst shows two pulses
in the interval from ~T0-0.2 s to ~T0+0.3  s.
The emission is seen up to ~1 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.02(-0.23,+0.57)x10^-6 erg/cm2,
and a 64-ms peak energy flux, measured from T0-0.086 s,
of 6.65(-1.47,+3.74)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Fitting the time-integrated 3-channel spectrum of the burst
(measured from T0-0.118 s to T0+0.304 s)
in the 20 keV - 1.5 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -0.37(-0.41,+0.59),
and Ep = 753(-217,+582) keV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200623_T64972/

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


GRB_name: GRB200522A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28038
SUBJECT: GRB 200522A: Gemini North spectroscopy of the putative host galaxy
DATE:    20/06/29 14:52:45 GMT
FROM:    Simone Dichiara at UMCP/NASA/GSFC  <dichiara@umd.edu>

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

We obtained a spectrum of the putative host galaxy (Fong et al., GCN Circ.
27779; Strausbaugh et al., GCN Circ. 27792) of the short GRB 200522A (Evans
et al., GCN Circ. 27778) with the Gemini Multi-Object Spectrograph mounted
on the Gemini North telescope.  Observations began at 13:22 UT on June 27,
2020 (36 days after the Swift trigger) and cover the wavelength range from
5000-9900 A.

The spectra shows several well detected emission lines which we interpret
as [OII] 3727, H-beta, and [OIII] 5007 at a common redshift of z=0.554.

We thank the Gemini North staff for efficiently executing these
observations in these difficult times.


GRB_name: GRB200629A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28039
SUBJECT: GRB 200629A: BALROG localization (Fermi Trigger 615127794 / GRB 200629535)
DATE:    20/06/29 16:41:06 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
615127794 at 12:49:49 on 29 June 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 339.4+/-3.0 deg
Decl.(2000.0) = -64.8+/-1.0 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200629535/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200629535/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200629535/json

                        


GRB_name: GRB200629A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28040
SUBJECT: GRB 200629A: Fermi GBM Final Real-time Localization
DATE:    20/06/29 17:45:09 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

At 12:49:49.29 UT on 29 Jun 2020, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200629A (trigger 615127794 / 200629535). The
on-ground calculated location, using the Fermi GBM trigger data, is RA =
338.46, Dec = -65.59 (J2000 degrees, equivalent to J2000 22h 34m, -65d
35'), with a statistical uncertainty of 1.8 degrees. On-ground localization
was delayed by a network outage.

The angle from the Fermi LAT boresight is 71.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200629535/quicklook/glg_skymap_all_bn200629535.png

The HEALPix FITS file, including the estimated localization systematic, can
be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200629535/quicklook/glg_healpix_all_bn200629535.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200629535/quicklook/glg_lc_medres34_bn200629535.gif


GRB_name: GRB200629A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28041
SUBJECT: Fermi GRB 200629A: Global MASTER-Net observations report 
DATE:    20/06/29 18:15:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200629A ( Fermi GBM team, GCN 28040) errorbox  13771 sec after notice time and 13907 sec after trigger time at 2020-06-29 16:41:36 UT, with upper limit up to  18.0 mag. Observations started at twilight.  The observations began at zenith distance = 80 deg. The sun  altitude  is -11.9 deg. 

The galactic latitude b = -46 deg., longitude l = 322 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1392622

We obtain a following upper limits.  

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

   13998 | 2020-06-29 16:41:36 |         MASTER-SAAO | (22h 29m 03.34s , -64d 53m 38.3s) |   C |   180 | 17.5 |        
   13998 | 2020-06-29 16:41:36 |         MASTER-SAAO | (22h 45m 05.94s , -64d 52m 58.7s) |   C |   180 | 17.4 |        
   14197 | 2020-06-29 16:44:56 |         MASTER-SAAO | (22h 29m 02.68s , -64d 52m 33.6s) |   C |   180 | 17.9 |        
   14197 | 2020-06-29 16:44:56 |         MASTER-SAAO | (22h 45m 04.79s , -64d 51m 54.2s) |   C |   180 | 17.6 |        
   14396 | 2020-06-29 16:48:15 |         MASTER-SAAO | (22h 29m 08.28s , -64d 53m 30.0s) |   C |   180 | 18.0 |        
   14396 | 2020-06-29 16:48:15 |         MASTER-SAAO | (22h 45m 11.10s , -64d 52m 51.9s) |   C |   180 | 17.7 |        
   14596 | 2020-06-29 16:51:35 |         MASTER-SAAO | (22h 29m 00.76s , -64d 54m 27.9s) |   C |   180 | 17.8 |        
   14596 | 2020-06-29 16:51:35 |         MASTER-SAAO | (22h 45m 04.15s , -64d 53m 49.3s) |   C |   180 | 17.4 |        
   15055 | 2020-06-29 17:00:13 |         MASTER-SAAO | (22h 12m 29.44s , -68d 03m 48.9s) |   C |    60 | 17.7 |        
   15788 | 2020-06-29 17:12:26 |         MASTER-SAAO | (22h 12m 34.13s , -68d 04m 47.0s) |   C |    60 | 17.8 |        
   16206 | 2020-06-29 17:18:25 |         MASTER-SAAO | (22h 25m 05.83s , -65d 40m 42.3s) |   C |   180 | 17.7 |        
   16206 | 2020-06-29 17:18:25 |         MASTER-SAAO | (22h 41m 39.01s , -65d 40m 04.3s) |   C |   180 | 17.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200630A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28043
SUBJECT: GRB 200630A: Swift detection of a burst
DATE:    20/06/30 02:09:43 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), M. J. Moss (GWU) and D. M. Palmer (LANL)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 01:49:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200630A (trigger=980210).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 91.380, -60.789 which is 
   RA(J2000) = 06h 05m 31s
   Dec(J2000) = -60d 47' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 10 sec.  The peak count rate
was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:50:52.3 UT, 77.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 91.3308, -60.7524 which
is equivalent to:
   RA(J2000)  = 06h 05m 19.38s
   Dec(J2000) = -60d 45' 08.6"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 157 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 4.33
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 82 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 0.04. 

This burst is consistent with Fermi/GBM trigger number 615174580. 

Burst Advocate for this burst is K. L. Page (klp5 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: GRB200630A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28044
SUBJECT: GRB 200630A: Enhanced Swift-XRT position
DATE:    20/06/30 15:39:12 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 1889 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 200630A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 91.33040, -60.75279 which is equivalent
to:

RA (J2000): 06h 05m 19.30s
Dec (J2000): -60d 45' 10.1"

with an uncertainty of 2.0 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: GRB200629A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28045
SUBJECT: GRB 200629A: AstroSat CZTI detection
DATE:    20/06/30 17:34:42 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: 

Analysis of AstroSat CZTI data showed the detection of a long GRB 200629A, which was also detected by BALROG (Biltzinger B. et al., GCN #28039), Fermi GBM (GCN #28040) and Global MASTER-Net (Lipunov V. et al., GCN # 28041). 

The source was clearly detected in the 40-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-06-29 12:49:53.599 UT. The measured peak count rate associated with the burst is 337 +/- 28 cts/s above the background in the combined data of four quadrants, with a total of 3117 +/- 32 cts. The local mean background count rate was 486 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 27.14 +/- 0.12 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 2020-06-29 12:49:52.574 UT. The measured peak count rate is 310 +/- 33 cts/s above the background in the combined Veto data of four quadrants, with a total of 2105 +/- 42 cts. The local mean background count rate was 1414 +/- 1 cts/s. We measure a T90 of 21.01 +/- 0.20 s from the cumulative Veto light curve. 

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


GRB_name: GRB200630A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28046
SUBJECT: GRB 200630A: Fermi GBM detection
DATE:    20/06/30 21:14:09 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

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

"At 01:49:35.08 UT on 30 June 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200630A (trigger 615174580 / 200630076)
which was also detected by the Swift/BAT (Page et al. 2020, GCN 28043)
and the Swift/XRT (Beardmore et al. 2020, GCN 28044).
The Fermi GBM Final Position is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 42
degrees.

The GBM light curve shows one main peak
with a duration (T90) of about 7 s (50-300 keV).
The time-averaged spectrum from T0-1.5 s to T0+3.56 s is
best fit by a single power law function with index of -1.51 +/- 0.05.

The event fluence (10-1000 keV) in this time interval is
(1.41 +/- 0.12)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.19 s in the 10-1000 keV band
is 2.9 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB200623A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28047
SUBJECT: GRB 200623A: Swift XRT further observations 
DATE:    20/06/30 22:08:27 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

B. Sbarufatti (PSU), P.A. Evans (U. Leicester) and K. K. Simpson (PSU) report on behalf of the Swift XRT team.

Swift performed a second observation of the field of GRB 200623A, with a 4.5 ks exposure.

The only uncatalogued source in the field, Source 3 (Tohuvavohu et al., GCN 28023), is still detected and shows no evidence of fading, so we conclude that it is not the GRB afterglow.

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


GRB_name: GRB200630B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28048
SUBJECT: GRB 200630B: Fermi GBM Final Localization
DATE:    20/07/01 01:03:56 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

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

At 23:31:21.89 UT on 30 June 2002, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200630B (trigger 615252686 / 200630980).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 79.3, Dec = +31.0 (J2000 degrees, equivalent to J2000 79h 16m, 30d 59m'),
with a statistical uncertainty of 3.9 degrees.

The angle from the Fermi LAT boresight is 66 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200630980/quicklook/glg_skymap_all_bn200630980.png

The HEALPix FITS file, including the estimated localization systematic, can
be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200630980/quicklook/glg_healpix_all_bn200630980.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200630980/quicklook/glg_lc_medres34_bn200630980.gif


GRB_name: GRB200630A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28049
SUBJECT: GRB 200630A: Swift-XRT refined Analysis
DATE:    20/07/01 02:09:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 2.9 ks of XRT data for GRB 200630A (Page et al. GCN
Circ. 28043), from 86 s to 7.0 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Beardmore et al. (GCN Circ. 28044).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.66 (+0.27, -0.20).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.7 (+/-0.5). The
best-fitting absorption column is  3.7 (+3.4, -2.3) x 10^21 cm^-2, in
excess of the Galactic value of 4.3 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.6 x 10^-11 (6.1 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.7 (+3.4, -2.3) x 10^21 cm^-2
Galactic foreground: 4.3 x 10^20 cm^-2
Excess significance: 2.3 sigma
Photon index:      1.7 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
0.66, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.2 x
10^-14 (1.1 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00980210.

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


GRB_name: GRB200630A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28050
SUBJECT: GRB 200630A: Swift/UVOT Upper Limits 
DATE:    20/07/01 02:15:16 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

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

The Swift/UVOT began settled observations of the field of GRB 200630A
83 s after the BAT trigger (Page et al., GCN Circ. 28043).
No optical afterglow consistent with the XRT position
(Page et al. GCN Circ. 28043)
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            83          233          147         >19.7
u_FC               295          545          246         >19.8
white               83         1189          353         >20.4
v                  624         1239           78         >18.9
b                  550         1164           58         >19.6
u                  295         5310          433         >20.1
w1                 674         5154          253         >20.1
m2                 822         4949          232         >20.5
w2                 600         1214           78         >20.0

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200630A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28051
SUBJECT: GRB 200630A: Swift-BAT refined analysis
DATE:    20/07/01 04:06:52 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), K. L. Page (U Leicester),
T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-61 to T+242 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200630A (trigger #980210)
(Page et al., GCN Circ. 28043).  The BAT ground-calculated position is
RA, Dec = 91.389, -60.779 deg which is
   RA(J2000)  =  06h 05m 33.3s
   Dec(J2000) = -60d 46' 44.8"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 70%.

The mask-weighted light curve shows a single-pulse structure that starts
and peaks at ~T0, and ends at~T+17 s. T90 (15-350 keV) is 14.83 +- 3.63 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.51 to T+16.64 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.64 +- 0.24.  The fluence in the 15-150 keV band is 4.7 +- 0.7 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+0.06 sec in the 15-150 keV band
is 1.4 +- 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/980210/BA/


GRB_name: GRB200701A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28052
SUBJECT: GRB 200701A: Swift detection of a burst
DATE:    20/07/01 12:58:38 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

M. G. Bernardini (INAF-OAB), S. D. Barthelmy (GSFC),
P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU), J. A. Kennea (PSU),
A. Y. Lien (GSFC/UMBC), A. Melandri (INAF-OAB),
K. L. Page (U Leicester), T. Sbarrato (INAF-OAB), B. Sbarufatti (PSU)
and M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 12:46:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200701A (trigger=980421).  Swift did not slew immediately
due to a Sun observing constraint. 
The BAT on-board calculated location is 
RA, Dec 123.555, -14.494 which is 
   RA(J2000) = 08h 14m 13s
   Dec(J2000) = -14d 29' 37"
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 ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 06:11 UT on 2020 September 07. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB200701A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28053
SUBJECT: Fermi-GBM Sub-Threshold Detection of GRB 200701A
DATE:    20/07/01 22:59:04 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

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

Swift-BAT detected GRB 200701A at 12:46:59 UT (Bernardini et al. 2020, GCN 28052). 
There was no Fermi-GBM onboard trigger around the event.
An automated, blind search for short gamma-ray bursts below the onboard triggering 
threshold in Fermi-GBM also identified no counterparts.

The GBM targeted search [1], the most sensitive, coherent search for GRB-like 
signals, was run from +/-30 s around BAT trigger time.
A transient source was identified whose most significant timescale according to 
the search is 8.192 s, with a log likelihood ratio of 39.

The location is consistent with that from Swift-BAT.
The spectrum is consistent with a "normal" GRB template 
(Band function with Epeak = 230 keV, alpha = -1.0, beta = -2.3).

[1] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB200701A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28054
SUBJECT: GRB 200701A: Swift-BAT refined analysis
DATE:    20/07/02 02:12:24 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), J. R. Cummings (CPI),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-60 to T+243 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200701A (trigger #980421)
(Bernardini et al., GCN Circ. 28052).  The BAT ground-calculated position is
RA, Dec = 123.563, -14.553 deg which is
   RA(J2000)  =  08h 14m 15.2s
   Dec(J2000) = -14d 33' 09.8"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.

The mask-weighted light curve shows a single-pulse structure that
starts at ~T-7 s and peaks at ~T0. The main pulse ends at ~T+20 s,
followed by a weak tail that lasts till ~T+40 s. T90 (15-350 keV)
is 38.9 +- 8.6 sec (estimated error including systematics).

The time-averaged spectrum from T-6.81 to T+42.17 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.91 +- 0.16.  The fluence in the 15-150 keV band
is 9.3 +- 1.0 x 10^-7 erg/cm2. The 1-sec peak photon flux measured
from T-1.72 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/980421/BA/


GRB_name: GRB200702A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28056
SUBJECT: GRB 200702A: Fermi GBM Final Real-time Localization
DATE:    20/07/02 21:34:52 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 21:24:18 UT on 2 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200702A (trigger 615417863.9672 / 200702892).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 300.4, Dec = -57.7 (J2000 degrees, equivalent to J2000 20h 01m, -57d 42'), with a statistical uncertainty of 21.4 degrees.

The angle from the Fermi LAT boresight is 51.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200702892/quicklook/glg_skymap_all_bn200702892.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200702892/quicklook/glg_healpix_all_bn200702892.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200702892/quicklook/glg_lc_medres34_bn200702892.gif


GRB_name: GRB200702A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28057
SUBJECT: Fermi GRB 200702A: Global MASTER-Net observations report 
DATE:    20/07/02 23:30:16 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200702A ( Fermi GBM team, GCN 28056) errorbox  2633 sec after notice time and 2660 sec after trigger time at 2020-07-02 22:08:39 UT, with upper limit up to  17.4 mag. The observations began at zenith distance = 56 deg. The sun  altitude  is -78.2 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200702A errorbox  4891 sec after notice time and 4918 sec after trigger time at 2020-07-02 22:46:17 UT, with upper limit up to  16.1 mag. Observations started at twilight.  The observations began at zenith distance = 57 deg. The sun  altitude  is -13.1 deg. 

The galactic latitude b = -20 deg., longitude l = 324 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1394636

We obtain a following upper limits.  

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

    2750 | 2020-07-02 22:08:39 |         MASTER-SAAO | (23h 24m 08.23s , -67d 49m 09.3s) |   C |   180 | 17.4 |        
    5009 | 2020-07-02 22:46:17 |         MASTER-OAFA | (08h 24m 50.56s , -83d 12m 13.3s) |   C |   180 | 15.9 |        
    5431 | 2020-07-02 22:53:19 |         MASTER-OAFA | (09h 32m 08.12s , -83d 10m 44.3s) |   C |   180 | 16.1 |        
    5642 | 2020-07-02 22:56:50 |         MASTER-OAFA | (10h 55m 46.36s , -83d 10m 36.9s) |   C |   180 | 15.1 |        
    5853 | 2020-07-02 23:00:21 |         MASTER-OAFA | (12h 02m 42.06s , -83d 10m 11.7s) |   C |   180 | 15.4 |        
    6064 | 2020-07-02 23:03:52 |         MASTER-OAFA | (09h 40m 30.39s , -83d 09m 58.7s) |   C |   180 | 15.4 |        
    6487 | 2020-07-02 23:10:56 |         MASTER-OAFA | (10h 47m 30.09s , -83d 08m 45.3s) |   C |   180 | 15.8 |        
    6698 | 2020-07-02 23:14:27 |         MASTER-OAFA | (08h 24m 48.11s , -83d 12m 12.8s) |   C |   180 | 15.9 |        
    6910 | 2020-07-02 23:17:58 |         MASTER-OAFA | (09h 32m 01.22s , -83d 09m 46.7s) |   C |   180 | 16.1 |        
    7121 | 2020-07-02 23:21:29 |         MASTER-OAFA | (10h 55m 51.35s , -83d 09m 36.8s) |   C |   180 | 15.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200703A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28058
SUBJECT: GRB 200703A: Fermi GBM Final Real-time Localization
DATE:    20/07/03 08:20:50 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 08:11:39 UT on 3 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200703A (trigger 615456704.610832 / 200703341).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 249.2, Dec = -3.6 (J2000 degrees, equivalent to J2000 16h 36m, -3d 36'), with a statistical uncertainty of 5.5 degrees.

The angle from the Fermi LAT boresight is 40.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200703341/quicklook/glg_skymap_all_bn200703341.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200703341/quicklook/glg_healpix_all_bn200703341.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200703341/quicklook/glg_lc_medres34_bn200703341.gif


GRB_name: GRB200703B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28059
SUBJECT: GRB 200703B: Fermi GBM Final Real-time Localization
DATE:    20/07/03 23:27:02 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 23:16:41 UT on 3 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200703B (trigger 615511006.839074 / 200703970).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 148.5, Dec = 6.3 (J2000 degrees, equivalent to J2000 09h 54m, 6d 17'), with a statistical uncertainty of 2.4 degrees.

The angle from the Fermi LAT boresight is 63.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200703970/quicklook/glg_skymap_all_bn200703970.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200703970/quicklook/glg_healpix_all_bn200703970.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200703970/quicklook/glg_lc_medres34_bn200703970.gif


GRB_name: GRB200703B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28060
SUBJECT: GRB 200703B: AstroSat CZTI detection
DATE:    20/07/04 10:25:02 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 200703B, which was also detected by Fermi GBM (GCN #28059).

The source was clearly detected in the 40-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-07-03 23:17:06.531 UT. The measured peak count rate associated with the burst is 226 +/- 23 cts/s above the background in the combined data of four quadrants, with a total of 3165 +/- 66 cts. The local mean background count rate was 585 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 31.58 +/- 0.35 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 2020-07-03 23:17:09.576 UT. The measured peak count rate is 733 +/- 42 cts/s above the background in the combined Veto data of four quadrants, with a total of 8880 +/- 119 cts. The local mean background count rate was 1808 +/- 2 cts/s.  We measure a T90 of 31.945 +/- 0.209 s from the cumulative Veto light curve.

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


GRB_name: GRB200703B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28061
SUBJECT: GRB 200703B: Insight-HXMT/HE detection
DATE:    20/07/04 16:11:22 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, Y. G. Zheng, C. Cai, S. Xiao, Q. B. Yi, W. C. Xue,
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-07-03T23:16:52.80 (T0), Insight-HXMT/HE detected 
GRB 200703B (trigger ID: HEB200703970) in a routine search of the data, 
which was also triggered by Fermi/GBM (GCN #28059) and AstroSat/CZTI (GCN #28060).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 0.161 s measured from T0-11.360 s. 
The 1-ms peak rate, measured from T0+17.803 s, is 1950 cnts/sec. 
The total counts from this burst is 23638 counts.
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200703970_lc.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200705A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28062
SUBJECT: GRB 200705A: Fermi GBM Final Real-time Localization
DATE:    20/07/05 16:19:59 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 16:09:53 UT on 5 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200705A (trigger 615658198.251492 / 200705674).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 60.5, Dec = -48.3 (J2000 degrees, equivalent to J2000 04h 01m, -48d 17'), with a statistical uncertainty of 23.7 degrees.

The angle from the Fermi LAT boresight is 106.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200705674/quicklook/glg_skymap_all_bn200705674.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200705674/quicklook/glg_healpix_all_bn200705674.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200705674/quicklook/glg_lc_medres34_bn200705674.gif


GRB_name: GRB200705A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28064
SUBJECT: Fermi GRB 200705A: Global MASTER-Net observations report 
DATE:    20/07/06 02:30:46 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200705A ( Fermi GBM team, GCN 28062) errorbox  33087 sec after notice time and 33114 sec after trigger time at 2020-07-06 01:21:47 UT, with upper limit up to  18.4 mag. The observations began at zenith distance = 67 deg. The sun  altitude  is -53.9 deg. 

The galactic latitude b = -71 deg., longitude l = 241 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1396328

We obtain a following upper limits.  

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

   33144 | 2020-07-06 01:21:47 |         MASTER-SAAO | (03h 48m 30.12s , -52d 03m 51.2s) |   C |    60 | 17.9 |        
   33144 | 2020-07-06 01:21:47 |         MASTER-SAAO | (03h 59m 34.11s , -52d 02m 39.2s) |   C |    60 | 17.7 |        
   35195 | 2020-07-06 01:55:58 |         MASTER-SAAO | (03h 48m 32.31s , -52d 03m 46.0s) |   C |    60 | 18.1 |        
   35195 | 2020-07-06 01:55:58 |         MASTER-SAAO | (03h 59m 36.25s , -52d 02m 29.2s) |   C |    60 | 18.0 |        
   35762 | 2020-07-06 02:05:24 |         MASTER-SAAO | (03h 48m 30.20s , -52d 02m 33.4s) |   C |    60 | 18.4 |        
   35762 | 2020-07-06 02:05:24 |         MASTER-SAAO | (03h 59m 33.43s , -52d 01m 15.9s) |   C |    60 | 18.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200706A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28065
SUBJECT: GRB 200706A: Fermi GBM Final Real-time Localization
DATE:    20/07/06 05:42:33 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:32:09 UT on 6 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200706A (trigger 615706334.325502 / 200706231).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 89.3, Dec = 54.6 (J2000 degrees, equivalent to J2000 05h 57m, 54d 36'), with a statistical uncertainty of 48.5 degrees.

The angle from the Fermi LAT boresight is 71.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200706231/quicklook/glg_skymap_all_bn200706231.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200706231/quicklook/glg_healpix_all_bn200706231.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200706231/quicklook/glg_lc_medres34_bn200706231.gif


GRB_name: GRB200704A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28066
SUBJECT: GRB 200704A: Insight-HXMT/HE detection
DATE:    20/07/06 06:03:09 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, Y. G. Zheng, C. Cai, S. Xiao, Q. B. Yi, W. C. Xue,
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-07-04T09:27:38.35 (T0), Insight-HXMT/HE detected 
GRB 200704A (trigger ID: HEB200704394) in a routine search of the data, 
which also triggered Konus-Wind.

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 39.119 s measured from T0-0.070 s. 
The 1-ms peak rate, measured from T0-0.076 s, is 2352 cnts/sec. 
The total counts from this burst is 22227 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200704394_lc.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200707A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28068
SUBJECT: GRB 200707A: Fermi GBM Final Localization
DATE:    20/07/07 03:21:08 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

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

At 01:44:02.54 UT on 07 July 2020, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200707A (trigger 615779047 / 200707072).

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 80.8, Dec = -14.9 (J2000 degrees, equivalent to J2000 05h 23m, -14d 53'),
with a statistical uncertainty of 3.1 degrees.

The angle from the Fermi LAT boresight is 13 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200707072/quicklook/glg_skymap_all_bn200707072.png

The HEALPix FITS file, including the estimated localization systematic, can
be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200707072/quicklook/glg_healpix_all_bn200707072.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200707072/quicklook/glg_lc_medres34_bn200707072.gif


GRB_name: GRB200707A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28069
SUBJECT: GRB 200707A: Insight-HXMT/HE detection
DATE:    20/07/08 12:35:34 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, S. Xiao, Y. F. Du, Y. G. Zheng, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-07-07T01:44:02.54 (T0), Insight-HXMT/HE detected 
GRB 200707A (trigger ID: HEB200707072) in a routine search of the data, 
which also triggered Fermi/GBM (GCN #28068).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 14.81 s measured from T0-0.72 s. 
The 1-ms peak rate, measured from T0-0.91 s, is 563 cnts/sec. 
The total counts from this burst is 3374 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200707072_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 
 
Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200709A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28070
SUBJECT: GRB 200709A: Fermi GBM Final Real-time Localization
DATE:    20/07/09 03:41:40 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 03:31:16 UT on 9 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200709A (trigger 615958281.763912 / 200709147).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 119.9, Dec = -53.0 (J2000 degrees, equivalent to J2000 07h 59m, -53d 00'), with a statistical uncertainty of 7.3 degrees.

The angle from the Fermi LAT boresight is 115.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200709147/quicklook/glg_skymap_all_bn200709147.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200709147/quicklook/glg_healpix_all_bn200709147.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200709147/quicklook/glg_lc_medres34_bn200709147.gif


GRB_name: GRB200709B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28071
SUBJECT: GRB 200709B: Tiled Swift observations
DATE:    20/07/09 06:00:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
HAWC GRB 200709B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00091

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

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

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


GRB_name: GRB200709B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28072
SUBJECT: GRB 200709B: Swift-XRT observations
DATE:    20/07/09 13:50:53 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@inaf.it>

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

Swift-XRT has performed follow-up observations of the HAWC-detected
burst GRB 200709B in a series of observations tiled on the sky. The
total exposure time is 4.9 ks, distributed over 7 tiles; the maximum
exposure at a single sky location was 1.4 ks. The data were collected
between T0+5.1 ks and T0+16.9 ks, and are entirely in Photon Counting
(PC) mode. 

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

Source 1:
  RA (J2000):  252.0755  =  16:48:18.12
  Dec (J2000): +15.0921  =  +15:05:31.6
  Error: 5.8 arcsec (radius, 90% conf.)
  Count-rate: 0.0165 [+0.0067, -0.0053] ct s^-1   
  Distance: 1121 arcsec from HAWC position.

Source 3:
  RA (J2000):  252.3306  =  16:49:19.35
  Dec (J2000): +15.4197  =  +15:25:11.0
  Error: 6.2 arcsec (radius, 90% conf.)
  Count-rate: (7.3 [+4.4, -3.2])e-3 ct s^-1   
  Distance: 791 arcsec from HAWC position.

A catalogued source was also detected.

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00091.

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


GRB_name: GRB200710A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28073
SUBJECT: GRB 200710A: Fermi GBM Final Real-time Localization
DATE:    20/07/10 01:02:28 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 SHORT GRB

At 00:52:07 UT on 10 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200710A (trigger 616035132.072806 / 200710036).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 77.9, Dec = 4.0 (J2000 degrees, equivalent to J2000 05h 11m, 4d 00'), with a statistical uncertainty of 16.6 degrees.

The angle from the Fermi LAT boresight is 62.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200710036/quicklook/glg_skymap_all_bn200710036.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200710036/quicklook/glg_healpix_all_bn200710036.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200710036/quicklook/glg_lc_medres34_bn200710036.gif


GRB_name: GRB200711A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28077
SUBJECT: GRB 200711A: Fermi GBM Final Real-time Localization
DATE:    20/07/11 11:14:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 11:04:32 UT on 11 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200711A (trigger 616158277.930672 / 200711461).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 287.1, Dec = 1.3 (J2000 degrees, equivalent to J2000 19h 08m, 1d 18'), with a statistical uncertainty of 1.6 degrees.

The angle from the Fermi LAT boresight is 79.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200711461/quicklook/glg_skymap_all_bn200711461.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200711461/quicklook/glg_healpix_all_bn200711461.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200711461/quicklook/glg_lc_medres34_bn200711461.gif


GRB_name: GRB200711A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28078
SUBJECT: GRB 200711A: Swift detection of a burst
DATE:    20/07/11 11:29:06 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), E. Ambrosi (INAF-IASFPA),
S. D. Barthelmy (GSFC), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), 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 11:04:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200711A (trigger=981957).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 285.977, -0.136, which is 
   RA(J2000)  =  19h 03m 54s
   Dec(J2000) = -00d 08' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed multiple peaks
with a duration of about 30 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 11:07:22.8 UT, 166.3 seconds after
the BAT trigger. Due to a poor slew, the promptly downlinked data only
cover 30% of the BAT error circle. No source was detected in 779 s within 
the small part of the BAT error region covered. We are waiting for the
full dataset covering the full field of view to detect and localise 
the XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White
filter starting 169 seconds after the BAT trigger. This is a very crowded
region with large extinction. No credible afterglow candidate has been
found in the initial data products. 

Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.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: GRB200711A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28079
SUBJECT: Swift GRB 200711A: Global MASTER-Net observations report 
DATE:    20/07/11 18:41:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB 200711A ( F. E. Marshall et al., GCN 28078) errorbox  26829 sec after notice time and 26854 sec after trigger time at 2020-07-11 18:32:11 UT, with upper limit up to  15.9 mag. Observations started at twilight.  The observations began at zenith distance = 59 deg. The sun  altitude  is -10.2 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 200711A errorbox  26939 sec after notice time and 26964 sec after trigger time at 2020-07-11 18:34:00 UT, with upper limit up to  16.7 mag. Observations started at twilight.  The observations began at zenith distance = 54 deg. The sun  altitude  is -15.0 deg. 

The galactic latitude b = -3 deg., longitude l = 35 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1399126

We obtain a following upper limits.  

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

   26945 |      MASTER-Tavrida |   C |   180 | 15.9 |        
   26994 |   MASTER-Kislovodsk |   C |    60 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200711A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28080
SUBJECT: GRB 200711A: Fermi GBM detection
DATE:    20/07/11 18:47:25 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

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

"At 11:04:32.93 UT on 11 July 2020, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 200711A(trigger 616158277 / 200711461),
which was also detected by the Swift/BAT (Marshall et al. 2020, GCN 28078).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 77
degrees.

The GBM light curve consists of a single bright pulse followed by some
extended emission with a duration (T90) of about 29 s (50-300 keV).
The time-averaged spectrum from T0 s to T0+24.58 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.04 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 287 +/- 18 keV.
A Band function fits equally well, with Epeak = 215 +/- 23 keV,
alpha = -0.95 +/- 0.05 and beta = -2.04 +/- 0.10.

The event fluence (10-1000 keV) in this time interval is
(1.510 +/- 0.042)E-05 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+3.64 s in the 10-1000 keV band
is 16.3 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB200711A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28081
SUBJECT: GRB 200711A: Swift-XRT refined Analysis
DATE:    20/07/12 06:34:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.9 ks of XRT data for GRB 200711A (Marshall et al.
GCN Circ. 28078), from 150 s to 40.4 ks after the  BAT trigger. The
data comprise 29 s in Windowed Timing (WT) mode (the first 10 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. Using 1145 s of PC mode data and 2 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 285.97020, -0.14708
which is equivalent to:

RA (J2000): 19h 03m 52.85s
Dec(J2000): -00d 08' 49.5"

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.51 (+0.13, -0.14), followed by a break at T+3349 s to
an alpha of 1.41 (+/-0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.01 (+0.22, -0.21). The
best-fitting absorption column is  1.65 (+0.30, -0.27) x 10^22 cm^-2,
in excess of the Galactic value of 5.7 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 5.6 x 10^-11 (1.2 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.65 (+0.30, -0.27) x 10^22 cm^-2
Galactic foreground: 5.7 x 10^21 cm^-2
Excess significance: 6.5 sigma
Photon index:      2.01 (+0.22, -0.21)

If the light curve continues to decay with a power-law decay index of
1.41, the count rate at T+24 hours will be 9.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.4 x
10^-13 (1.1 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/00981957.

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


GRB_name: GRB200711A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28082
SUBJECT: GRB 200711A: KAIT Optical Upper Limit
DATE:    20/07/12 07:57:23 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

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

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to GRB 200711A (GBM detection:
GCN 28077; Swfit detection: Marshall et al., GCN 28078)
starting at ~0.90 hours after the Swfit trigger, and again
on the second night around 0.81 days after burst. Observations
were performed in the clear (roughly R) filters, and the exposure
time was 20 s per image. We do not detect any optical afterglow
candidate within the enhanced XRT position error circle (Osborne
et al., GCN 28081), neither in the first night image with upper
limit of ~17.5 mag calibrated to the Pan-STARRS1 catalog, nor in
the second night co-added image with upper limit of ~20.0 mag.


GRB_name: GRB200711A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28083
SUBJECT: GRB 200711A: Fermi-LAT marginal detection
DATE:    20/07/12 18:47:27 GMT
FROM:    Milena Crnogorcevic at GSFC,UMD, Fermi  <milena.crnogorcevic@nasa.gov>

M. Crnogorcevic (Univ. of Maryland & NASA/GSFC), M. Kovacevic (INFN Perugia),
M. Ohno (Hiroshima Univ.), F. Longo (University & INFN Trieste),
report on behalf of the Fermi-LAT Collaboration:

On July, 11th, 2020, Fermi-LAT detected high-energy emission from GRB 200711A,
which was also detected by Fermi-GBM (trigger 616158277/200711461;
Poolakkil et al. GCN 28080) and Swift-BAT (Marshall et al. GCN 28078).

The best LAT on-ground location is found to be RA, Dec = 285.8, 0.2 (degrees, J2000) 
with an error radius of 0.4 deg (90% containment, statistical error only).
The 95% containment error is consistent with the Swift-XRT position 
(Osborne et al. GCN 28081).

This GRB was outside LAT FoV at the trigger time of the GBM and came
into the LAT FoV around 200 s after the trigger. The data from the 
Fermi-LAT in the time interval 200-600 s after the GBM trigger at the
Swift-XRT position show a marginal increase of the detection
significance of the high energy (GeV) photons for this burst.

The photon flux above 100 MeV in the time interval 200 - 600 s after
the GBM trigger is 3.3e-6 +/- 1.9e-6 ph/cm2/s.

The highest-energy photon is a 5.7 GeV event which is observed 542 seconds
after the GBM trigger.

The Fermi-LAT point of contact for this burst is
Milena Crnogorcevic (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: GRB200711A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28084
SUBJECT: GRB 200711A: Swift-BAT refined analysis
DATE:    20/07/12 19:14:05 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
T. N. Ukwatta (LANL) (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 200711A
(trigger #981957) (Marshall et al., GCN Circ. 28078).
The BAT ground-calculated position is
RA, Dec = 285.975, -0.134 deg which is
   RA(J2000)  =  19h 03m 53.9s
   Dec(J2000) = -00d 08' 04.1"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 8%.

The mask-weighted light curve shows a multi-peaked structure that
starts at ~T-5 s and ends at ~T+30 s. The three major peaks occur
at ~T0, ~T+5 s, and ~T+20 s, respectively. T90 (15-350 keV)
is 29.39 +- 3.07 sec (estimated error including systematics).

The time-averaged spectrum from T-4.72 to T+29.73 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.42 +- 0.10.  The fluence in the 15-150 keV band
is 5.3 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+0.20 sec in the 15-150 keV band is 7.7 +- 1.0 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/981957/BA/


GRB_name: GRB200711A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28085
SUBJECT: GRB 200711A: Swift/UVOT Upper Limits
DATE:    20/07/13 02:22:08 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 200711A: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200711A
170 s after the BAT trigger (Marshall et al., GCN Circ. 28078).
No optical afterglow consistent with the BAT position
(Marshall et al. GCN Circ 28078)
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           170          319          147         >20.2
white              170          999          310         >20.6
v                  404         4651          255         >18.7
b                  503          868           58         >19.1
u                  477         5088           80         >19.0
w1                 453         5061          255         >19.3
m2                 428          448           19         >18.0
w2                 379         4446          255         >19.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.96 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200711A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28086
SUBJECT: GRB 200711A: AbAO optical upper limit
DATE:    20/07/13 09:39:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), N. Pankov (HSE), K. Kamyshnikov (HSE), R. Ya. 
Inasaridze (AbAO),  V.R. Ayvazian (AbAO),  G. V.  Kapanadze (AbAO),  S. 
Belkin (IKI), E. Mazaeva (IKI), A. Volnova  (IKI),  I. Molotov (KIAM) 
report on behalf of  GRB IKI FuN:

We observed the field of GRB 200711A (Fermi GBM Team, GCN 28077; 
Marshall et al., GCN 28078; Crnogorcevic et al., GCN 28083) with AS-32 
(0.7m) telescope of Abastumani Observatory starting on 2020-07-11 (UT) 
23:05:40.  We do not detect any object  within the enhanced XRT position 
error circle (Osborne et al., GCN 28081).  Preliminary photometry of the 
field is following.

Date       UT start  t-T0    Filter Exp.  OT    Err. UL
                     (mid, days)     (s)
2020-07-11 23:05:40  0.50074 R      49*60 n/d   n/d 21.3

The photometry is based on nearby USNO-B1.0 stars


GRB_name: GRB200711A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28087
SUBJECT: GRB 200711A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/07/13 12:00:51 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

Y. Asaoka (Waseda U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
S. Torii (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 200711A (Swift detection: Marshall et al., GCN Circ. 28078;
Fermi GBM detection: Poolakkil et al., GCN Circ. 28080;
Fermi-LAT detection: Crnogorcevic et al., GCN Circ. 28083;
https://gcn.gsfc.nasa.gov/other/200711A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM)
at 11:04:34.187 UTC on 11 July 2020
(http://cgbm.calet.jp/cgbm_trigger/flight/1278500601/).
The burst signal was seen only by the SGM detector.

The burst light curve shows a weak pulse which starts at T-0.9 sec and
ends at T+4.0 sec. The T90 and T50 durations measured by the SGM data are
4.2 +- 1.3 sec and 2.1 +- 1.3 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1278500601/

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


GRB_name: GRB200713A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28088
SUBJECT: GRB 200713A: Swift detection of a burst
DATE:    20/07/13 12:05:03 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

A. Y. Lien (GSFC/UMBC), E. Ambrosi (INAF-IASFPA),
S. D. Barthelmy (GSFC), V. D'Elia (SSDC), J.D. Gropp (PSU),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
K. L. Page (U Leicester) and A. Tohuvavohu (U Toronto) report on
behalf of the Neil Gehrels Swift Observatory Team:

At 11:42:54 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200713A (trigger=982201).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 76.962, -32.825, which is 
   RA(J2000)  =  05h 07m 51s
   Dec(J2000) = -32d 49' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is the usual for image triggers, the light curve
does not show anything. 

The XRT began observing the field at 11:45:24.7 UT, 150.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
76.9492, -32.8144 which is equivalent to:
   RA(J2000)  = 05h 07m 47.81s
   Dec(J2000) = -32d 48' 51.7"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 54 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.99
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 1.27e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 159 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
0.02. 

Burst Advocate for this burst is A. Y. Lien (amy.y.lien 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: GRB200713A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28089
SUBJECT: GRB 200713A: Enhanced Swift-XRT position
DATE:    20/07/13 16:12:16 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 208 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200713A, 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 = 76.94990, -32.81475 which is equivalent
to:

RA (J2000): 05h 07m 47.98s
Dec (J2000): -32d 48' 53.1"

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: GRB200714A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28091
SUBJECT: GRB 200714A: Fermi GBM Final Real-time Localization
DATE:    20/07/14 06:06:18 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:56:02 UT on 14 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200714A (trigger 616398967.25892 / 200714247).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 10.4, Dec = 57.5 (J2000 degrees, equivalent to J2000 00h 41m, 57d 30'), with a statistical uncertainty of 6.7 degrees.

The angle from the Fermi LAT boresight is 70.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714247/quicklook/glg_skymap_all_bn200714247.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714247/quicklook/glg_healpix_all_bn200714247.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714247/quicklook/glg_lc_medres34_bn200714247.gif


GRB_name: GRB200713A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28092
SUBJECT: GRB 200713A: Swift-XRT refined Analysis
DATE:    20/07/14 06:59:31 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Tohuvavohu
(U. Toronto), B. Sbarufatti (PSU), D.N. Burrows (PSU), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester)
and A.Y. Lien report on behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 200713A (Lien et al. GCN
Circ. 28088), from 156 s to 62.7 ks after the  BAT trigger. The data
comprise 128 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN Circ. 28089).

The light curve can be modelled with an initial power-law decay with an
index of alpha=5.1 (+/-0.3), followed by a break at T+358 s to an alpha
of 0.41 (+0.04, -0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.71 (+0.26, -0.24). The
best-fitting absorption column is  3.2 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 2.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.13 (+0.18, -0.17)
and a best-fitting absorption column of 1.7 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.2 x 10^-11 (4.5 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 2.0 x 10^20 cm^-2
Excess significance: 5.0 sigma
Photon index:      2.13 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
0.41, 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 1.9 x
10^-12 (2.7 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/00982201.

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


GRB_name: GRB200714B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28093
SUBJECT: GRB 200714B: Fermi GBM Final Real-time Localization
DATE:    20/07/14 08:25:54 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 08:15:25 UT on 14 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200714B (trigger 616407330.91385 / 200714344).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 190.4, Dec = -54.0 (J2000 degrees, equivalent to J2000 12h 41m, -54d 00'), with a statistical uncertainty of 2.2 degrees.

The angle from the Fermi LAT boresight is 84.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714344/quicklook/glg_skymap_all_bn200714344.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714344/quicklook/glg_healpix_all_bn200714344.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714344/quicklook/glg_lc_medres34_bn200714344.gif


GRB_name: GRB200711A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28094
SUBJECT: GRB 200711A: Insight-HXMT/HE detection
DATE:    20/07/14 09:52:44 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, C. Cai, Y. F. Du, Y. G. Zheng, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-07-11T11:04:32.93 (T0), Insight-HXMT/HE detected 
GRB 200711A (trigger ID: HEB200711461) in a routine search of the data, 
which also triggered Fermi-GBM (Poolakkil et al. GCN 28080) 
and Swift-BAT (Marshall et al. GCN 28078).

The Insight-HXMT/HE light curve mainly consists of single 
pulse with a duration (T90) of 9.15 s measured from T0-0.64 s. 
The 1-ms peak rate, measured from T0+3.56 s, is 1098 cnts/sec. 
The total counts from this burst is 3109 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200711461_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 
 
Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200714C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28095
SUBJECT: GRB 200714C: Fermi GBM Final Real-time Localization
DATE:    20/07/14 10:39:00 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 10:28:45 UT on 14 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200714C (trigger 616415330.458832 / 200714437).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 210.3, Dec = -3.6 (J2000 degrees, equivalent to J2000 14h 01m, -3d 36'), with a statistical uncertainty of 4.2 degrees.

The angle from the Fermi LAT boresight is 32.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714437/quicklook/glg_skymap_all_bn200714437.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714437/quicklook/glg_healpix_all_bn200714437.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714437/quicklook/glg_lc_medres34_bn200714437.gif


GRB_name: GRB200713A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28096
SUBJECT: GRB 200713A: Swift-BAT refined analysis
DATE:    20/07/14 16:02:02 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
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-100 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 200713A
(trigger #982201) (Lien et al., GCN Circ. 28088).
The BAT ground-calculated position is
RA, Dec = 76.941, -32.846 deg which is
   RA(J2000)  =  05h 07m 45.8s
   Dec(J2000) = -32d 50' 47.1"
with an uncertainty of 2.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.

The mask-weighted light curve shows several weak overlapping pulses
that start at ~T+20 s and end at ~T+80 s. T90 (15-350 keV)
is 48.98 +- 9.52 sec (estimated error including systematics).

The time-averaged spectrum from T+18.45 to T+74.94 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 2.48 +- 0.32.  The fluence in the 15-150 keV band
is 9.0 +- 1.6 x 10^-7 erg/cm2. The 1-sec peak photon flux measured
from T+49.94 sec in the 15-150 keV band is 0.8 +- 0.3 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/982201/BA/


GRB_name: GRB200714D
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28097
SUBJECT: GRB 200714D: Fermi GBM Final Real-time Localization
DATE:    20/07/14 16:02:37 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 15:52:16 UT on 14 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200714D (trigger 616434741.793704 / 200714661).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 13.7, Dec = 31.1 (J2000 degrees, equivalent to J2000 00h 54m, 31d 06'), with a statistical uncertainty of 28.9 degrees.

The angle from the Fermi LAT boresight is 36.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714661/quicklook/glg_skymap_all_bn200714661.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714661/quicklook/glg_healpix_all_bn200714661.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714661/quicklook/glg_lc_medres34_bn200714661.gif


GRB_name: GRB200714E
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28098
SUBJECT: GRB 200714E: Fermi GBM Final Real-time Localization
DATE:    20/07/14 18:45:56 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 18:35:05 UT on 14 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200714E (trigger 616444510.078062 / 200714774).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 215.8, Dec = -49.7 (J2000 degrees, equivalent to J2000 14h 23m, -49d 42'), with a statistical uncertainty of 1.1 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/2020/bn200714774/quicklook/glg_skymap_all_bn200714774.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714774/quicklook/glg_healpix_all_bn200714774.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200714774/quicklook/glg_lc_medres34_bn200714774.gif


GRB_name: GRB200714E
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28099
SUBJECT: GRB 200714E: BALROG localization (Fermi Trigger 616444510 / GRB 200714774)
DATE:    20/07/14 19:18:04 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
616444510 at 18:35:05 on 14 July 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:

RA(2000.0) = 194.8+/-2.2 deg
Decl.(2000.0) = -52.4+/-1.8 deg

We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200714774/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200714774/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200714774/json


GRB_name: GRB200522A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28100
SUBJECT: GRB 200522A: Candidate Optical/nIR Counterpart from Gemini and HST Imaging
DATE:    20/07/14 19:19:42 GMT
FROM:    Brendan O'Connor at UMD  <oconnorb@umd.edu>

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

We report on further observations of the short GRB 200522A (Evans et al.,
GCN Circ. 27778) taken at 3.1 and 9.1 d post-burst in the r-band filter
with the Gemini Multi-Object Spectrograph (GMOS) mounted on the 8.1m Gemini
North telescope. Image subtraction with HOTPANTS (Becker 2015) identifies
a low significance residual close to the candidate host galaxy's center
(Fong et al., GCN Circ. 27779; Strausbaugh et al., GCN Circ. 27792),
and at the edge of the XRT enhanced position (Beardmore et al., GCN Circ.
27780). We independently reanalyzed the HST images (Fong et al., GCN Circ.
27827; Kilpatrick et al., GCN Circ. 27904), and performed image subtraction
between the two epochs at 3.5 and 16.3 d. Although the analysis is
complicated by the presence of a bright galaxy's nucleus, a residual signal
of brightness F125W ~ 25.6 AB mag is present at the location of the Gemini
optical candidate. We suggest this to be the candidate optical/nIR
counterpart of GRB 200522A. The observed magnitude is much brighter than
expected for a kilonova like AT2017gfo, and suggests that the afterglow
emission is the dominant component. The projected offset from the galaxy's
nucleus is ~0.23 arcseconds, corresponding to 1.5 kpc at redshift z = 0.554
(Dichiara et al., GCN Circ. 28038). This physical offset is low yet not
unprecedented, falling in the bottom 15% of the short GRB offset
distribution
(Fong & Berger, 2013).

We thank the Gemini North staff for efficiently executing
these observations.


GRB_name: GRB200714A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28101
SUBJECT: Fermi GRB 200714A: Global MASTER-Net observations report 
DATE:    20/07/14 19:45:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200714A ( Fermi GBM team, GCN 28091) errorbox  45106 sec after notice time and 45116 sec after trigger time at 2020-07-14 18:27:58 UT, with upper limit up to  18.7 mag. Observations started at twilight.  The observations began at zenith distance = 59 deg. The sun  altitude  is -10.0 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200714A errorbox  47705 sec after notice time and 47715 sec after trigger time at 2020-07-14 19:11:17 UT, with upper limit up to  19.0 mag. The observations began at zenith distance = 59 deg. The sun  altitude  is -19.3 deg. 

The galactic latitude b = -4 deg., longitude l = 120 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1400744

We obtain a following upper limits.  

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

   45147 | 2020-07-14 18:27:58 |      MASTER-Tavrida | (23h 40m 26.22s , +63d 46m 42.1s) |   C |    60 | 16.5 |        
   45227 | 2020-07-14 18:29:19 |      MASTER-Tavrida | (23h 57m 01.87s , +61d 46m 41.9s) |   C |    60 | 16.6 |        
   45308 | 2020-07-14 18:30:40 |      MASTER-Tavrida | (23h 48m 25.51s , +61d 46m 41.7s) |   C |    60 | 16.8 |        
   45388 | 2020-07-14 18:32:00 |      MASTER-Tavrida | (23h 32m 54.46s , +65d 46m 18.1s) |   C |    60 | 16.9 |        
   45469 | 2020-07-14 18:33:21 |      MASTER-Tavrida | (23h 40m 21.86s , +63d 47m 42.5s) |   C |    60 | 16.9 |        
   45549 | 2020-07-14 18:34:41 |      MASTER-Tavrida | (23h 58m 37.81s , +63d 46m 26.9s) |   C |    60 | 16.7 |        
   45630 | 2020-07-14 18:36:02 |      MASTER-Tavrida | (23h 56m 56.98s , +61d 46m 10.8s) |   C |    60 | 17.0 |        
   45711 | 2020-07-14 18:37:22 |      MASTER-Tavrida | (00h 14m 02.59s , +61d 46m 30.3s) |   C |    60 | 17.1 |        
   45791 | 2020-07-14 18:38:43 |      MASTER-Tavrida | (23h 48m 26.20s , +61d 47m 57.3s) |   C |    60 | 17.2 |        
   45872 | 2020-07-14 18:40:03 |      MASTER-Tavrida | (00h 05m 24.60s , +61d 46m 37.8s) |   C |    60 | 17.2 |        
   45952 | 2020-07-14 18:41:24 |      MASTER-Tavrida | (23h 33m 01.10s , +65d 47m 02.5s) |   C |    60 | 17.5 |        
   46033 | 2020-07-14 18:42:45 |      MASTER-Tavrida | (23h 52m 31.76s , +65d 46m 01.4s) |   C |    60 | 17.7 |        
   46113 | 2020-07-14 18:44:05 |      MASTER-Tavrida | (23h 58m 31.29s , +63d 47m 34.1s) |   C |    60 | 17.3 |        
   46194 | 2020-07-14 18:45:26 |      MASTER-Tavrida | (00h 14m 01.33s , +61d 47m 10.3s) |   C |    60 | 17.5 |        
   46274 | 2020-07-14 18:46:46 |      MASTER-Tavrida | (00h 05m 21.87s , +61d 46m 11.5s) |   C |    60 | 17.5 |        
   46355 | 2020-07-14 18:48:07 |      MASTER-Tavrida | (23h 57m 07.19s , +59d 48m 41.0s) |   C |    60 | 17.8 |        
   46435 | 2020-07-14 18:49:27 |      MASTER-Tavrida | (23h 56m 37.11s , +67d 46m 22.8s) |   C |    60 | 17.9 |        
   46596 | 2020-07-14 18:52:08 |      MASTER-Tavrida | (00h 35m 53.12s , +65d 44m 12.8s) |   C |    60 | 18.0 |        
   46677 | 2020-07-14 18:53:29 |      MASTER-Tavrida | (23h 52m 36.80s , +65d 45m 31.1s) |   C |    60 | 18.2 |        
   46757 | 2020-07-14 18:54:49 |      MASTER-Tavrida | (23h 57m 07.55s , +59d 48m 34.7s) |   C |    60 | 18.0 |        
   46838 | 2020-07-14 18:56:09 |      MASTER-Tavrida | (00h 13m 03.78s , +59d 47m 19.9s) |   C |    60 | 18.0 |        
   46918 | 2020-07-14 18:57:30 |      MASTER-Tavrida | (23h 56m 36.75s , +67d 46m 36.2s) |   C |    60 | 18.2 |        
   46999 | 2020-07-14 18:58:50 |      MASTER-Tavrida | (00h 17m 46.73s , +67d 45m 01.1s) |   C |    60 | 18.2 |        
   47160 | 2020-07-14 19:01:31 |      MASTER-Tavrida | (23h 47m 27.89s , +67d 46m 10.7s) |   C |    60 | 18.3 |        
   47241 | 2020-07-14 19:02:52 |      MASTER-Tavrida | (00h 35m 52.80s , +65d 44m 31.3s) |   C |    60 | 18.3 |        
   47321 | 2020-07-14 19:04:13 |      MASTER-Tavrida | (00h 55m 35.26s , +65d 44m 33.0s) |   C |    60 | 18.2 |        
   47401 | 2020-07-14 19:05:33 |      MASTER-Tavrida | (00h 13m 04.33s , +59d 48m 40.5s) |   C |    60 | 18.1 |        
   47482 | 2020-07-14 19:06:53 |      MASTER-Tavrida | (00h 17m 48.58s , +67d 44m 28.7s) |   C |    60 | 18.4 |        
   47562 | 2020-07-14 19:08:14 |      MASTER-Tavrida | (23h 56m 49.55s , +63d 46m 54.3s) |   C |    60 | 17.9 |        
   47644 | 2020-07-14 19:09:36 |      MASTER-Tavrida | (23h 47m 22.47s , +67d 47m 25.1s) |   C |    60 | 18.5 |        
   47724 | 2020-07-14 19:10:56 |      MASTER-Tavrida | (00h 55m 34.12s , +65d 45m 18.3s) |   C |    60 | 18.4 |        
   47745 | 2020-07-14 19:11:17 |   MASTER-Kislovodsk | (00h 45m 35.80s , +63d 34m 55.7s) |   C |    60 | 18.5 |        
   47745 | 2020-07-14 19:11:17 |   MASTER-Kislovodsk | (00h 27m 04.12s , +64d 03m 49.9s) |   C |    60 | 18.0 |        
   47805 | 2020-07-14 19:12:16 |      MASTER-Tavrida | (23h 56m 46.97s , +65d 45m 41.2s) |   C |    60 | 18.6 |        
   47885 | 2020-07-14 19:13:37 |      MASTER-Tavrida | (23h 56m 53.27s , +63d 47m 42.3s) |   C |    60 | 18.0 |        
   47907 | 2020-07-14 19:13:59 |   MASTER-Kislovodsk | (00h 42m 31.29s , +61d 33m 09.4s) |   C |    60 | 18.1 |        
   47907 | 2020-07-14 19:13:59 |   MASTER-Kislovodsk | (00h 25m 15.40s , +62d 02m 01.6s) |   C |    60 | 17.9 |        
   47965 | 2020-07-14 19:14:57 |      MASTER-Tavrida | (00h 15m 04.13s , +63d 46m 16.9s) |   C |    60 | 17.9 |        
   47988 | 2020-07-14 19:15:20 |   MASTER-Kislovodsk | (00h 53m 33.16s , +67d 32m 37.8s) |   C |    60 | 18.8 |        
   47988 | 2020-07-14 19:15:20 |   MASTER-Kislovodsk | (00h 31m 56.86s , +68d 01m 49.7s) |   C |    60 | 18.7 |        
   48046 | 2020-07-14 19:16:17 |      MASTER-Tavrida | (00h 28m 57.73s , +59d 47m 53.5s) |   C |    60 | 18.3 |        
   48068 | 2020-07-14 19:16:40 |   MASTER-Kislovodsk | (00h 45m 38.12s , +63d 33m 01.8s) |   C |    60 | 18.6 |        
   48068 | 2020-07-14 19:16:40 |   MASTER-Kislovodsk | (00h 27m 09.53s , +64d 02m 00.9s) |   C |    60 | 18.3 |        
   48126 | 2020-07-14 19:17:38 |      MASTER-Tavrida | (23h 56m 40.48s , +65d 47m 44.0s) |   C |    60 | 18.7 |        
   48206 | 2020-07-14 19:18:58 |      MASTER-Tavrida | (00h 16m 22.05s , +65d 46m 21.5s) |   C |    60 | 18.6 |        
   48230 | 2020-07-14 19:19:21 |   MASTER-Kislovodsk | (00h 42m 32.62s , +61d 34m 16.5s) |   C |    60 | 18.8 |        
   48230 | 2020-07-14 19:19:21 |   MASTER-Kislovodsk | (00h 25m 16.99s , +62d 03m 09.1s) |   C |    60 | 18.4 |        
   48287 | 2020-07-14 19:20:19 |      MASTER-Tavrida | (00h 15m 01.31s , +63d 45m 52.3s) |   C |    60 | 18.0 |        
   48310 | 2020-07-14 19:20:42 |   MASTER-Kislovodsk | (00h 53m 27.01s , +67d 34m 26.7s) |   C |    60 | 18.8 |        
   48310 | 2020-07-14 19:20:42 |   MASTER-Kislovodsk | (00h 31m 49.89s , +68d 03m 39.4s) |   C |    60 | 18.6 |        
   48367 | 2020-07-14 19:21:39 |      MASTER-Tavrida | (00h 29m 02.81s , +59d 46m 53.4s) |   C |    60 | 18.4 |        
   48448 | 2020-07-14 19:23:00 |      MASTER-Tavrida | (00h 44m 57.63s , +59d 48m 47.6s) |   C |    60 | 18.3 |        
   48551 | 2020-07-14 19:24:43 |   MASTER-Kislovodsk | (23h 25m 58.19s , +61d 36m 20.2s) |   C |    60 | 18.8 |        
   48551 | 2020-07-14 19:24:43 |   MASTER-Kislovodsk | (23h 08m 37.45s , +62d 05m 19.5s) |   C |    60 | 18.7 |        
   48793 | 2020-07-14 19:28:44 |   MASTER-Kislovodsk | (23h 52m 44.46s , +63d 36m 59.4s) |   C |    60 | 18.7 |        
   48793 | 2020-07-14 19:28:44 |   MASTER-Kislovodsk | (23h 34m 10.74s , +64d 06m 06.5s) |   C |    60 | 18.6 |        
   49034 | 2020-07-14 19:32:46 |   MASTER-Kislovodsk | (23h 25m 59.05s , +61d 37m 28.3s) |   C |    60 | 18.8 |        
   49034 | 2020-07-14 19:32:46 |   MASTER-Kislovodsk | (23h 08m 36.68s , +62d 06m 26.2s) |   C |    60 | 18.7 |        
   49275 | 2020-07-14 19:36:47 |   MASTER-Kislovodsk | (23h 52m 43.40s , +63d 37m 13.6s) |   C |    60 | 18.7 |        
   49275 | 2020-07-14 19:36:47 |   MASTER-Kislovodsk | (23h 34m 08.64s , +64d 06m 18.7s) |   C |    60 | 18.6 |        
   49355 | 2020-07-14 19:38:07 |   MASTER-Kislovodsk | (23h 46m 09.87s , +65d 36m 00.7s) |   C |    60 | 19.0 |        
   49355 | 2020-07-14 19:38:07 |   MASTER-Kislovodsk | (23h 26m 09.29s , +66d 05m 15.2s) |   C |    60 | 18.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200714D
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28102
SUBJECT: Fermi GRB 200714D: Global MASTER-Net observations report 
DATE:    20/07/14 19:45:17 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200714D ( Fermi GBM team, GCN 28097) errorbox  9313 sec after notice time and 9342 sec after trigger time at 2020-07-14 18:27:58 UT, with upper limit up to  18.7 mag. Observations started at twilight.  The observations began at zenith distance = 59 deg. The sun  altitude  is -10.0 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200714D errorbox  11912 sec after notice time and 11940 sec after trigger time at 2020-07-14 19:11:17 UT, with upper limit up to  19.3 mag. The observations began at zenith distance = 59 deg. The sun  altitude  is -19.3 deg. 

The galactic latitude b = -8 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=1401105

We obtain a following upper limits.  

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

    9372 | 2020-07-14 18:27:58 |      MASTER-Tavrida | (23h 40m 26.22s , +63d 46m 42.1s) |   C |    60 | 16.5 |        
    9453 | 2020-07-14 18:29:19 |      MASTER-Tavrida | (23h 57m 01.87s , +61d 46m 41.9s) |   C |    60 | 16.6 |        
    9533 | 2020-07-14 18:30:40 |      MASTER-Tavrida | (23h 48m 25.51s , +61d 46m 41.7s) |   C |    60 | 16.8 |        
    9614 | 2020-07-14 18:32:00 |      MASTER-Tavrida | (23h 32m 54.46s , +65d 46m 18.1s) |   C |    60 | 16.9 |        
    9694 | 2020-07-14 18:33:21 |      MASTER-Tavrida | (23h 40m 21.86s , +63d 47m 42.5s) |   C |    60 | 16.9 |        
    9775 | 2020-07-14 18:34:41 |      MASTER-Tavrida | (23h 58m 37.81s , +63d 46m 26.9s) |   C |    60 | 16.7 |        
    9856 | 2020-07-14 18:36:02 |      MASTER-Tavrida | (23h 56m 56.98s , +61d 46m 10.8s) |   C |    60 | 17.0 |        
    9936 | 2020-07-14 18:37:22 |      MASTER-Tavrida | (00h 14m 02.59s , +61d 46m 30.3s) |   C |    60 | 17.1 |        
   10017 | 2020-07-14 18:38:43 |      MASTER-Tavrida | (23h 48m 26.20s , +61d 47m 57.3s) |   C |    60 | 17.2 |        
   10097 | 2020-07-14 18:40:03 |      MASTER-Tavrida | (00h 05m 24.60s , +61d 46m 37.8s) |   C |    60 | 17.2 |        
   10178 | 2020-07-14 18:41:24 |      MASTER-Tavrida | (23h 33m 01.10s , +65d 47m 02.5s) |   C |    60 | 17.5 |        
   10258 | 2020-07-14 18:42:45 |      MASTER-Tavrida | (23h 52m 31.76s , +65d 46m 01.4s) |   C |    60 | 17.7 |        
   10339 | 2020-07-14 18:44:05 |      MASTER-Tavrida | (23h 58m 31.29s , +63d 47m 34.1s) |   C |    60 | 17.3 |        
   10419 | 2020-07-14 18:45:26 |      MASTER-Tavrida | (00h 14m 01.33s , +61d 47m 10.3s) |   C |    60 | 17.5 |        
   10500 | 2020-07-14 18:46:46 |      MASTER-Tavrida | (00h 05m 21.87s , +61d 46m 11.5s) |   C |    60 | 17.5 |        
   10580 | 2020-07-14 18:48:07 |      MASTER-Tavrida | (23h 57m 07.19s , +59d 48m 41.0s) |   C |    60 | 17.8 |        
   10661 | 2020-07-14 18:49:27 |      MASTER-Tavrida | (23h 56m 37.11s , +67d 46m 22.8s) |   C |    60 | 17.9 |        
   10741 | 2020-07-14 18:50:48 |      MASTER-Tavrida | (23h 26m 06.10s , +67d 47m 33.4s) |   C |    60 | 18.1 |        
   10822 | 2020-07-14 18:52:08 |      MASTER-Tavrida | (00h 35m 53.12s , +65d 44m 12.8s) |   C |    60 | 18.0 |        
   10902 | 2020-07-14 18:53:29 |      MASTER-Tavrida | (23h 52m 36.80s , +65d 45m 31.1s) |   C |    60 | 18.2 |        
   10983 | 2020-07-14 18:54:49 |      MASTER-Tavrida | (23h 57m 07.55s , +59d 48m 34.7s) |   C |    60 | 18.0 |        
   11063 | 2020-07-14 18:56:09 |      MASTER-Tavrida | (00h 13m 03.78s , +59d 47m 19.9s) |   C |    60 | 18.0 |        
   11144 | 2020-07-14 18:57:30 |      MASTER-Tavrida | (23h 56m 36.75s , +67d 46m 36.2s) |   C |    60 | 18.2 |        
   11224 | 2020-07-14 18:58:50 |      MASTER-Tavrida | (00h 17m 46.73s , +67d 45m 01.1s) |   C |    60 | 18.2 |        
   11305 | 2020-07-14 19:00:11 |      MASTER-Tavrida | (23h 26m 05.74s , +67d 47m 49.9s) |   C |    60 | 18.5 |        
   11385 | 2020-07-14 19:01:31 |      MASTER-Tavrida | (23h 47m 27.89s , +67d 46m 10.7s) |   C |    60 | 18.3 |        
   11466 | 2020-07-14 19:02:52 |      MASTER-Tavrida | (00h 35m 52.80s , +65d 44m 31.3s) |   C |    60 | 18.3 |        
   11546 | 2020-07-14 19:04:13 |      MASTER-Tavrida | (00h 55m 35.26s , +65d 44m 33.0s) |   C |    60 | 18.2 |        
   11627 | 2020-07-14 19:05:33 |      MASTER-Tavrida | (00h 13m 04.33s , +59d 48m 40.5s) |   C |    60 | 18.1 |        
   11707 | 2020-07-14 19:06:53 |      MASTER-Tavrida | (00h 17m 48.58s , +67d 44m 28.7s) |   C |    60 | 18.4 |        
   11788 | 2020-07-14 19:08:14 |      MASTER-Tavrida | (23h 56m 49.55s , +63d 46m 54.3s) |   C |    60 | 17.9 |        
   11869 | 2020-07-14 19:09:36 |      MASTER-Tavrida | (23h 47m 22.47s , +67d 47m 25.1s) |   C |    60 | 18.5 |        
   11950 | 2020-07-14 19:10:56 |      MASTER-Tavrida | (00h 55m 34.12s , +65d 45m 18.3s) |   C |    60 | 18.4 |        
   11971 | 2020-07-14 19:11:17 |   MASTER-Kislovodsk | (00h 45m 35.80s , +63d 34m 55.7s) |   C |    60 | 18.5 |        
   11971 | 2020-07-14 19:11:17 |   MASTER-Kislovodsk | (00h 27m 04.12s , +64d 03m 49.9s) |   C |    60 | 18.0 |        
   12030 | 2020-07-14 19:12:16 |      MASTER-Tavrida | (23h 56m 46.97s , +65d 45m 41.2s) |   C |    60 | 18.6 |        
   12051 | 2020-07-14 19:12:38 |   MASTER-Kislovodsk | (00h 12m 00.02s , +69d 34m 32.0s) |   C |    60 | 19.2 |        
   12051 | 2020-07-14 19:12:38 |   MASTER-Kislovodsk | (23h 48m 16.56s , +70d 03m 59.3s) |   C |    60 | 18.7 |        
   12110 | 2020-07-14 19:13:37 |      MASTER-Tavrida | (23h 56m 53.27s , +63d 47m 42.3s) |   C |    60 | 18.0 |        
   12132 | 2020-07-14 19:13:59 |   MASTER-Kislovodsk | (00h 42m 31.29s , +61d 33m 09.4s) |   C |    60 | 18.1 |        
   12133 | 2020-07-14 19:13:59 |   MASTER-Kislovodsk | (00h 25m 15.40s , +62d 02m 01.6s) |   C |    60 | 17.9 |        
   12191 | 2020-07-14 19:14:57 |      MASTER-Tavrida | (00h 15m 04.13s , +63d 46m 16.9s) |   C |    60 | 17.9 |        
   12213 | 2020-07-14 19:15:20 |   MASTER-Kislovodsk | (00h 53m 33.16s , +67d 32m 37.8s) |   C |    60 | 18.8 |        
   12213 | 2020-07-14 19:15:20 |   MASTER-Kislovodsk | (00h 31m 56.86s , +68d 01m 49.7s) |   C |    60 | 18.7 |        
   12271 | 2020-07-14 19:16:17 |      MASTER-Tavrida | (00h 28m 57.73s , +59d 47m 53.5s) |   C |    60 | 18.3 |        
   12294 | 2020-07-14 19:16:40 |   MASTER-Kislovodsk | (00h 45m 38.12s , +63d 33m 01.8s) |   C |    60 | 18.6 |        
   12294 | 2020-07-14 19:16:40 |   MASTER-Kislovodsk | (00h 27m 09.53s , +64d 02m 00.9s) |   C |    60 | 18.3 |        
   12351 | 2020-07-14 19:17:38 |      MASTER-Tavrida | (23h 56m 40.48s , +65d 47m 44.0s) |   C |    60 | 18.7 |        
   12374 | 2020-07-14 19:18:01 |   MASTER-Kislovodsk | (00h 11m 59.20s , +69d 35m 34.0s) |   C |    60 | 19.3 |        
   12374 | 2020-07-14 19:18:01 |   MASTER-Kislovodsk | (23h 48m 16.49s , +70d 05m 05.4s) |   C |    60 | 18.7 |        
   12432 | 2020-07-14 19:18:58 |      MASTER-Tavrida | (00h 16m 22.05s , +65d 46m 21.5s) |   C |    60 | 18.6 |        
   12455 | 2020-07-14 19:19:21 |   MASTER-Kislovodsk | (00h 42m 32.62s , +61d 34m 16.5s) |   C |    60 | 18.8 |        
   12455 | 2020-07-14 19:19:21 |   MASTER-Kislovodsk | (00h 25m 16.99s , +62d 03m 09.1s) |   C |    60 | 18.4 |        
   12512 | 2020-07-14 19:20:19 |      MASTER-Tavrida | (00h 15m 01.31s , +63d 45m 52.3s) |   C |    60 | 18.0 |        
   12535 | 2020-07-14 19:20:42 |   MASTER-Kislovodsk | (00h 53m 27.01s , +67d 34m 26.7s) |   C |    60 | 18.8 |        
   12535 | 2020-07-14 19:20:42 |   MASTER-Kislovodsk | (00h 31m 49.89s , +68d 03m 39.4s) |   C |    60 | 18.6 |        
   12593 | 2020-07-14 19:21:39 |      MASTER-Tavrida | (00h 29m 02.81s , +59d 46m 53.4s) |   C |    60 | 18.4 |        
   12616 | 2020-07-14 19:22:02 |   MASTER-Kislovodsk | (00h 58m 40.96s , +69d 33m 07.4s) |   C |    60 | 18.9 |        
   12616 | 2020-07-14 19:22:02 |   MASTER-Kislovodsk | (00h 35m 02.58s , +70d 02m 29.9s) |   C |    60 | 18.8 |        
   12673 | 2020-07-14 19:23:00 |      MASTER-Tavrida | (00h 44m 57.63s , +59d 48m 47.6s) |   C |    60 | 18.3 |        
   12777 | 2020-07-14 19:24:43 |   MASTER-Kislovodsk | (23h 25m 58.19s , +61d 36m 20.2s) |   C |    60 | 18.8 |        
   12777 | 2020-07-14 19:24:43 |   MASTER-Kislovodsk | (23h 08m 37.45s , +62d 05m 19.5s) |   C |    60 | 18.7 |        
   12857 | 2020-07-14 19:26:03 |   MASTER-Kislovodsk | (23h 35m 26.42s , +69d 37m 08.0s) |   C |    60 | 19.1 |        
   13018 | 2020-07-14 19:28:44 |   MASTER-Kislovodsk | (23h 52m 44.46s , +63d 36m 59.4s) |   C |    60 | 18.7 |        
   13018 | 2020-07-14 19:28:44 |   MASTER-Kislovodsk | (23h 34m 10.74s , +64d 06m 06.5s) |   C |    60 | 18.6 |        
   13098 | 2020-07-14 19:30:05 |   MASTER-Kislovodsk | (00h 58m 36.39s , +69d 33m 26.6s) |   C |    60 | 18.9 |        
   13098 | 2020-07-14 19:30:05 |   MASTER-Kislovodsk | (00h 34m 56.85s , +70d 02m 50.8s) |   C |    60 | 18.6 |        
   13259 | 2020-07-14 19:32:46 |   MASTER-Kislovodsk | (23h 25m 59.05s , +61d 37m 28.3s) |   C |    60 | 18.8 |        
   13259 | 2020-07-14 19:32:46 |   MASTER-Kislovodsk | (23h 08m 36.68s , +62d 06m 26.2s) |   C |    60 | 18.7 |        
   13340 | 2020-07-14 19:34:06 |   MASTER-Kislovodsk | (23h 35m 23.46s , +69d 35m 32.9s) |   C |    60 | 18.9 |        
   13501 | 2020-07-14 19:36:47 |   MASTER-Kislovodsk | (23h 52m 43.40s , +63d 37m 13.6s) |   C |    60 | 18.7 |        
   13501 | 2020-07-14 19:36:47 |   MASTER-Kislovodsk | (23h 34m 08.64s , +64d 06m 18.7s) |   C |    60 | 18.6 |        
   13581 | 2020-07-14 19:38:07 |   MASTER-Kislovodsk | (23h 46m 09.87s , +65d 36m 00.7s) |   C |    60 | 19.0 |        
   13581 | 2020-07-14 19:38:07 |   MASTER-Kislovodsk | (23h 26m 09.29s , +66d 05m 15.2s) |   C |    60 | 18.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200714E
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28103
SUBJECT: GRB 200714E: Swift/BAT-GUANO detection and arcminute localization
DATE:    20/07/15 04:01:20 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

Aaron Tohuvavohu (U Toronto), James DeLaunay (PSU), Jamie Kennea (PSU) report:

Swift/BAT did not trigger on GRB 200714E (T0: 2020-07-14 18:35:05 UTC,
Fermi/GBM Team GCN 28098) due to a slew.

The Fermi/GBM notice, distributed at T0+6 seconds triggered the Swift
Mission Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, arXiv: 2005.01751).

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.

Using the normal BAT imaging technique, we find the location of the
GRB with an SNR of 11.5.

The BAT ground-calculated position is
RA, Dec = 196.8656, -51.6403 deg which is
   RA(J2000)  = 13h 7m 27.7s
   Dec(J2000) =  -51d 38' 25"
with an uncertainty of 5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 28.9%.

This position is consistent with the Fermi GBM localization (GCN
28098) and the BALROG localization (GCN 28099).

XRT and UVOT follow-up has been triggered. 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: GRB200714E
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28104
SUBJECT: GRB 200714E: Swift ToO observations
DATE:    20/07/15 04:26:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Swift/BAT GRB 200714E. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021017

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. These are
not necessarily related to the Swift/BAT event. Any X-ray source
considered to be a probable afterglow candidate will be reported via a 
GCN Circular after manual consideration.

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

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


GRB_name: GRB200714E
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28105
SUBJECT: GRB 200714E: AGILE detection
DATE:    20/07/15 09:03:33 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the GRB 200714E reported by Fermi-GBM (GCN
#28098, trigger 616444510.078062 / 200714774), occurring at T0 = 2020-07-14
18:35:05 s (UTC).

The event is clearly visible in the scientific ratemeters (RMs) of the
SuperAGILE detector (18-60 keV). The light curve shows a double-peaked FRED
profile, lasting ~13 s and releasing ~1200 counts. The SuperAGILE RMs light
curve can be found at
http://www.agilescienceapp.it/notices/GRB200714E_SuperAGILE_RMs.png .

Additional analysis of AGILE data is in progress.


GRB_name: GRB200714E
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28106
SUBJECT: Fermi GRB 200714E: Global MASTER-Net observations report 
DATE:    20/07/15 10:15:45 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 200714E ( Fermi GBM team, GCN 28098) errorbox  8778 sec after notice time and 8805 sec after trigger time at 2020-07-14 21:01:50 UT, with upper limit up to  16.5 mag. Observations started at twilight.  The observations began at zenith distance = 76 deg. The sun  altitude  is -12.5 deg. 

The galactic latitude b = 17 deg., longitude l = 321 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1401343

We obtain a following upper limits.  

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

    8836 | 2020-07-14 21:01:50 |          MASTER-IAC | (14h 49m 10.37s , -47d 53m 55.1s) |   C |    60 | 16.3 |        
    8836 | 2020-07-14 21:01:50 |          MASTER-IAC | (14h 37m 06.81s , -47d 49m 28.7s) |   C |    60 | 15.8 |        
    9188 | 2020-07-14 21:07:43 |          MASTER-IAC | (14h 49m 16.41s , -47d 55m 48.3s) |   C |    60 | 16.5 |        
    9188 | 2020-07-14 21:07:43 |          MASTER-IAC | (14h 37m 12.64s , -47d 51m 21.3s) |   C |    60 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200714E
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28107
SUBJECT: GRB 200714E: Swift-XRT observations
DATE:    20/07/15 13:24:55 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the Fermi-GBM and
Swift/BAT (GUANO)-detected burst GRB 200714E (GCN Circs. 28098 and
28103), collecting 2.2 ks of Photon Counting (PC) mode data between
T0+37.3 ks and T0+44.5 ks. 

One uncatalogued X-ray source has been detected, it is below the RASS
limit and shows no definitive signs of fading. Therefore, at the
present time we cannot confirm this as the afterglow. Details of this
source are given below:

Source 1:
  RA (J2000):  196.8225  =  13:07:17.41
  Dec (J2000): -51.6390  =  -51:38:20.4
  Error: 3.1 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.0138 +/- 0.0033 ct s^-1   
  Distance: 96 arcsec from Swift/BAT position.
  Flux: (6.2 +/- 1.5)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021017.

Further observations are planned.

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


GRB_name: GRB200714E
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28108
SUBJECT: GRB 200714E: Fermi GBM observation
DATE:    20/07/15 20:30:31 GMT
FROM:    Cori Fletcher at USRA  <cfletcher@usra.edu>

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

"At 18:35:05.08 UT on 14 July 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200714E (trigger 616444510 / 200714774), which was also
detected by the Swift/BAT-GUANO (Tohuvavohu et al. 2020, GCN 28103). The Fermi GBM
Final Real-time Localization (GCN 28098) is consistent with the Swift position.

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

The GBM light curve shows a single bright peak
with a duration (T90) of about 20 s (50-300 keV).
The time-averaged spectrum from T0+0.8 s to T0+21.3 s is
best fit by a Band function with Epeak = 189 +/- 28 keV,
alpha = -0.92 +/- 0.09, and beta = -2.3 +/- 0.3.

The event fluence (10-1000 keV) in this time interval is
(9.4 +/- 0.5)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.4 s in the 10-1000 keV band
is 11.1 +/- 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: GRB200716A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28109
SUBJECT: GRB 200716A: Fermi GBM Final Real-time Localization
DATE:    20/07/16 01:36:55 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 01:26:37 UT on 16 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200716A (trigger 616555602.759372 / 200716060).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 134.8, Dec = -15.0 (J2000 degrees, equivalent to J2000 08h 59m, -15d 00'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 76.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716060/quicklook/glg_skymap_all_bn200716060.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716060/quicklook/glg_healpix_all_bn200716060.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716060/quicklook/glg_lc_medres34_bn200716060.gif


GRB_name: GRB200715A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28110
SUBJECT: GRB 200715A : A long GRB detected by INTEGRAL
DATE:    20/07/16 01:45:01 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro.mereghetti@inaf.it>

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

a gamma ray burst lasting about 160 s has been detected by IBAS in the
IBIS/ISGRI data at 23:51:40  UT of July 15, 2020.

The refined coordinates (J2000) are:
R.A.= 248.5372   deg
DEC.=  -51.8392  deg
with an uncertainty of  1.5   arcmin (90% c.l.).

Due to telemetry saturation, we can provide only lower limits to its peak
flux and fluence.
The   peak flux is greater than 1.2  ph/cm2/s (20-200 keV, 1-s integration
time) and the fluence in the same energy range is greater than  1.8e-6
 erg/cm2.

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


GRB_name: GRB200715A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28111
SUBJECT: GRB 200715A: Swift ToO observations
DATE:    20/07/16 01:48:23 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 INTEGRAL GRB 200715A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021018

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 INTEGRAL 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: GRB200716A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28112
SUBJECT: GRB 200716A: BALROG localization (Fermi Trigger 616555602 / GRB 200716060)
DATE:    20/07/16 05:50:07 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
616555602 at 01:26:37 on 16 July 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 137.4+/-0.6 deg
Decl.(2000.0) = -16.2+/-0.8 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200716060/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200716060/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200716060/json

                        


GRB_name: GRB200716B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28113
SUBJECT: GRB 200716B: Fermi GBM Final Real-time Localization
DATE:    20/07/16 07:44:52 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 07:34:28 UT on 16 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200716B (trigger 616577673.479748 / 200716316).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 344.4, Dec = -15.9 (J2000 degrees, equivalent to J2000 22h 57m, -15d 54'), with a statistical uncertainty of 4.2 degrees.

The angle from the Fermi LAT boresight is 67.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716316/quicklook/glg_skymap_all_bn200716316.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716316/quicklook/glg_healpix_all_bn200716316.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716316/quicklook/glg_lc_medres34_bn200716316.gif


GRB_name: GRB200716B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28114
SUBJECT: GRB 200716B: BALROG localization (Fermi Trigger 616577673 / GRB 200716316)
DATE:    20/07/16 08:04:03 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
616577673 at 07:34:28 on 16 July 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 343.0+/-3.9 deg
Decl.(2000.0) = -22.2+/-2.5 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200716316/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200716316/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200716316/json

                        


GRB_name: GRB200715A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28115
SUBJECT: GRB 200715A: Swift-XRT afterglow detection
DATE:    20/07/16 08:44:31 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the INTEGRAL-detected
burst GRB 200715A (Mereghetti et al. GCN Circ. 28110), collecting 3.3
ks of Photon Counting (PC) mode data between T0+7.5 ks and T0+26.2 ks. 


An uncatalogued X-ray source is detected consistent with being within
266 arcsec of the INTEGRAL position and is above the RASS limit, and is
therefore likely the GRB afterglow.  The position of this source is RA,
Dec=248.5377, -51.8356 which is equivalent to:

RA (J2000): 16:34:9.04
Dec(J2000): -51:50:08.0

with an uncertainty of 3.7 arcsec (radius, 90% confidence).  This
position is 13 arcsec from the INTEGRAL position (Mereghetti et al. GCN
Circ. 28110). 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.06 (+0.32, -0.27).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.5). The
best-fitting absorption column is  1.06 (+0.60, -0.29) x 10^22 cm^-2,
consistent with the Galactic value of 7.6 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 4.8 x 10^-11 (9.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.06 (+0.60, -0.29) x 10^22 cm^-2
Galactic foreground: 7.6 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.1 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 6.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 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/00021018.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021018.

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


GRB_name: GRB200716A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28116
SUBJECT: GRB 200716A: AGILE detection
DATE:    20/07/16 12:56:58 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the long GRB 200716A reported by Fermi-GBM
(GCN #28109, trigger 616555602.759372 / 200716060), occurring at T0 =
2020-07-16 01:26:37 s (UTC).

The event is clearly visible in the scientific ratemeters (RMs) of the
SuperAGILE (SA, 18-60 keV), MiniCALorimeter (MCAL, 0.4-100 MeV), and
Anti-Coincidence (50-200 keV) detectors. Their light curves show a
multi-peaked profile, lasting about ~60 s and releasing ~4200 counts in the
SA detector (above a background rate of 60 Hz), ~75200 counts in the MCAL
detector (above a background rate of 1200 Hz), and ~225000 counts in the AC
detector (above a background rate of 3700 Hz). The AGILE RMs light curves
can be found at
http://www.agilescienceapp.it/notices/GRB200716A_AGILE_RMs.png .

The intense episode occurring at about T0 + 30 s triggered a MCAL high time
resolution data acquisition. The time-integrated spectrum of this episode
in ~7 s can be fitted in the energy range 0.4-10 MeV with a single
power-law with ph.ind. = 1.51 -0.05/+0.05, resulting in a reduced
chi-squared of 1.6 (48 d.o.f.). The episode fluence in the same energy
range and time interval is 3.5e-05 ergs/cm^2 (90% confidence level).

Additional analysis of AGILE data is in progress.


GRB_name: GRB200716A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28117
SUBJECT: GRB 200716A: AstroSat CZTI detection
DATE:    20/07/16 16:53:57 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 200716A, which was also detected by Fermi GBM (GCN #28109), BALROG (Biltzinge B. et al., GCN #28112) and AGILE (Ursi A. et al., GCN #28116).

The source was clearly detected in the 40-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-07-16 01:27:08.646 UT. The measured peak count rate associated with the burst is 641 +/- 30 cts/s above the background in the combined data of four quadrants, with a total of 5950 +/- 52 cts. The local mean background count rate was 480 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 44.029 +/- 0.032 s. In preliminary analysis, we find that 637 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-07-16 01:27:07.277 UT. The measured peak count rate is 641 +/- 30 cts/s above the background in the combined Veto data of four quadrants, with a total of 6218 +/- 72 cts. The local mean background count rate was 1442 +/- 1.4 cts/s.  We measure a T90 of 43.651 +/- 0.024 s from the cumulative Veto light curve.

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


GRB_name: GRB200716B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28118
SUBJECT: GRB 200716B: AstroSat CZTI detection
DATE:    20/07/16 17:49:32 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 200716B, which was also detected by Fermi GBM (GCN #28113) and BALROG (Biltzinge B. et al., GCN #28114).

The source was clearly detected in the 40-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-07-16 07:34:29.531 UT. The measured peak count rate associated with the burst is 356 +/- 27 cts/s above the background in the combined data of four quadrants, with a total of 3023 +/- 68 cts. The local mean background count rate was 572 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 29.35 +/- 0.08 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 2020-07-16 07:34:28.000 UT. The measured peak count rate is 1190 +/- 53 cts/s above the background in the combined Veto data of four quadrants, with a total of 8920 +/- 167 cts. The local mean background count rate was 1623 +/- 3 cts/s.  We measure a T90 of 28.17 +/- 0.31 s from the cumulative Veto light curve.

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


GRB_name: GRB200716B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28119
SUBJECT: Fermi GRB 200716B: Global MASTER-Net observations report 
DATE:    20/07/16 20:45:09 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200716B ( Fermi GBM team, GCN 28113) errorbox  45224 sec after notice time and 45252 sec after trigger time at 2020-07-16 20:08:40 UT, with upper limit up to  19.8 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -53.7 deg. 

The galactic latitude b = -70 deg., longitude l = 44 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1402322

We obtain a following upper limits.  

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

   45282 | 2020-07-16 20:08:40 |         MASTER-SAAO | (22h 38m 50.10s , -18d 03m 55.3s) |   C |    60 | 19.2 |        
   45282 | 2020-07-16 20:08:40 |         MASTER-SAAO | (22h 46m 01.07s , -18d 03m 22.7s) |   C |    60 | 17.1 |        
   45362 | 2020-07-16 20:10:00 |         MASTER-SAAO | (22h 38m 13.09s , -20d 03m 06.5s) |   C |    60 | 19.2 |        
   45362 | 2020-07-16 20:10:00 |         MASTER-SAAO | (22h 45m 29.21s , -20d 02m 33.4s) |   C |    60 | 18.0 |        
   45442 | 2020-07-16 20:11:20 |         MASTER-SAAO | (22h 39m 22.40s , -22d 04m 22.9s) |   C |    60 | 19.6 |        
   45442 | 2020-07-16 20:11:20 |         MASTER-SAAO | (22h 46m 44.51s , -22d 03m 48.5s) |   C |    60 | 18.4 |        
   45521 | 2020-07-16 20:12:39 |         MASTER-SAAO | (22h 42m 03.41s , -24d 05m 39.3s) |   C |    60 | 19.8 |        
   45521 | 2020-07-16 20:12:39 |         MASTER-SAAO | (22h 49m 32.15s , -24d 05m 03.9s) |   C |    60 | 19.1 |        
   45601 | 2020-07-16 20:13:59 |         MASTER-SAAO | (22h 46m 43.65s , -26d 05m 52.0s) |   C |    60 | 19.8 |        
   45601 | 2020-07-16 20:13:59 |         MASTER-SAAO | (22h 54m 19.84s , -26d 05m 15.2s) |   C |    60 | 19.0 |        
   46905 | 2020-07-16 20:35:43 |         MASTER-SAAO | (22h 38m 50.90s , -18d 04m 05.7s) |   C |    60 | 19.6 |        
   46905 | 2020-07-16 20:35:43 |         MASTER-SAAO | (22h 46m 01.63s , -18d 03m 33.8s) |   C |    60 | 18.9 |        
   46985 | 2020-07-16 20:37:03 |         MASTER-SAAO | (22h 38m 08.68s , -20d 05m 22.3s) |   C |    60 | 19.7 |        
   46985 | 2020-07-16 20:37:03 |         MASTER-SAAO | (22h 45m 24.81s , -20d 04m 49.1s) |   C |    60 | 19.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200716A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28120
SUBJECT: GRB 200716A: Fermi GBM detection
DATE:    20/07/16 20:57:27 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

C. Malacaria (NASA-MSFC/USRA), E. Bissaldi (Politecnico and INFN Bari),

R. Dunwoody (UCD), J. Mangan (UCD) and C. Meegan (UAH)

report on behalf of the Fermi GBM Team:



"At 01:26:37.76 UT on 16 July 2020, the Fermi Gamma-Ray Burst Monitor (GBM)

triggered and located GRB 200716A (trigger 616555602 / 200716060) ,

which also triggered AGILE (Ursi A. et al., GCN #28116)

and AstroSat (Gupta et al., GCN #28117).



The Fermi GBM Final Real-time Localization is reported in GCN #28109.

The angle from the Fermi LAT boresight at the GBM trigger time is 76 degrees.



The GBM light curve shows multiple peaks with

a duration (T90) of about 45 s (50-300 keV).

The time-averaged spectrum from T0-9.5 s to T0+59.1 s is

best fit by a Comptonized model with Epeak = 456 +/- 17 keV

and alpha = -0.97 +/- 0.01 .



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

(5.986 +/- 0.041)E-05 erg/cm^2. The 1-sec peak photon flux measured

starting from T0+31 s in the 10-1000 keV band

is 24.0 +/- 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: GRB200716A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28121
SUBJECT: IPN triangulation of GRB 200716A
DATE:    20/07/16 21:32:56 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

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

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

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

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

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

and

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

The intense long-duration GRB 200716A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 28109,
Malacaria et al., GCN Circ. 28120;
BALROG localization: Biltzinger et al., GCN Circ. 28112;
AGILE detection: Ursi et al., GCN Circ. 28116;
AstroSat CZTI detection: Gupta et al., GCN Circ. 28117)
was detected by Fermi (GBM trigger 616555602), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), AGILE,
AstoSat (CZTI), and Swift (BAT) at about 5195 s UT (01:26:35).
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:
  139.332 (09h 17m 20s) -16.730 (-16d 43' 46")
 Corners:
  138.969 (09h 15m 53s) -16.190 (-16d 11' 23")
  139.223 (09h 16m 54s) -17.334 (-17d 20' 01")
  139.702 (09h 18m 48s) -17.266 (-17d 15' 58")
  139.445 (09h 17m 47s) -16.124 (-16d 07' 25")
 ---------------------------------------------
The error box area is 1939 sq. arcmin, and its maximum
dimension is 1.3 deg (the minimum one is 28 arcmin).
The Sun distance was 44 deg.

This box may be improved.

The localization is consistent with, but reduces
the area of, the final Fermi-GBM (GCN Circ. 28109) and
BALROG (GCN Circ. 28112) localizations.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200716_T05194/IPN/

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


GRB_name: GRB200716C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28123
SUBJECT: GRB 200716C: Fermi GBM Final Real-time Localization
DATE:    20/07/16 23:08:03 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:57:41 UT on 16 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200716C (trigger 616633066.180458 / 200716957).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 192.1, Dec = 35.3 (J2000 degrees, equivalent to J2000 12h 48m, 35d 17'), with a statistical uncertainty of 2.3 degrees.

The angle from the Fermi LAT boresight is 36.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716957/quicklook/glg_skymap_all_bn200716957.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716957/quicklook/glg_healpix_all_bn200716957.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200716957/quicklook/glg_lc_medres34_bn200716957.gif


GRB_name: GRB200716C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28124
SUBJECT: GRB 200716C: Swift detection of a burst with an optical counterpart
DATE:    20/07/16 23:10:50 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J.D. Gropp (PSU), N. J. Klingler (PSU),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and B. Sbarufatti (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 22:57:41 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200716C (trigger=982707).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 196.013, +29.630 which is 
   RA(J2000) = 13h 04m 03s
   Dec(J2000) = +29d 37' 47"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~30000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 22:59:04.2 UT, 82.9 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 196.0100, 29.6465 which is equivalent to:
   RA(J2000)  = 13h 04m 2.40s
   Dec(J2000) = +29d 38' 47.4"
with an uncertainty of 6.6 arcseconds (radius, 90% containment). This
location is 60 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 0.1 s image was 1.10e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 93 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 13:04:02.43 = 196.01011
DEC(J2000) = +29:38:40.6 = 29.64460
with a 90%-confidence error radius of about 0.75 arc sec. This position is 6.85
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.34 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta 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: GRB200716C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28125
SUBJECT: Swift GRB200716C: Global MASTER-Net OT detection
DATE:    20/07/16 23:41:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, D.Kuvshinov, N.Tyurina, 
P.Balanutsa,
A.Kuznetsov, D. Vlasenko, F. Balakin, I. Gorbunov
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

K. Ivanov, O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk
Irkutsk State University

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory

V. Yurkov, A. Gabovich, Yu. Sergienko
Blagoveschensk Educational State University, Blagoveschensk


D. Buckley, S. Potter, A. Kniazev, M. Kotze
South African Astronomical Observatory

R. Podesta, Carlos Lopez and F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)

Hugo Levato
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

MASTER-IAC robotic telescope (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L) located in Spain (IAC Teide Observatory) was pointed to 
the  GRB200716C (Ukwatta et al, GCN 28124)  55 sec after notice time and 
79 sec after trigger time at 2020-07-16 22:59:00 UT.
On our 5-th (50s exposure)  set , obtained 243 sec after tigger time
at 2020-07-16 23:01:45 UT, we  found an optical transient within Swift 
error-box (ra=196.012 dec=29.6292 r=0.05) brighter.


  T-Tmid      Date      Time       Expt.        Ra                Dec          Mag
---------|---------------------|-------|-----------------|-----------------|-----
      268   2020-07-16 23:01:45      50   (13h 04m 02.41s , +29d 38m 39.4s)   16.3

The 5-sigma upper limit has been about  16.6mag
The message may be cited.


GRB_name: GRB200716C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28126
SUBJECT: GRB200716C: BOOTES-1 optical afterglow detection
DATE:    20/07/17 03:29:41 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

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

Following the Swift trigger of GRB 200716C (Ukwatta et al., GCNC 28124), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst. Series images were taken started 22:58:53UT (72 s after trigger). In the first 10s image, the afterglow reported by UVOT (Ukwatta et al., GCNC 28124) and MASTER (Lipunov et al., GCNC 28125) is detected with magnitude of 16.8 (clear filter). Further observation are on going.

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


GRB_name: GRB200522A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28127
SUBJECT: GRB 200522A: HST NIR counterpart confirmation
DATE:    20/07/17 04:04:46 GMT
FROM:    Wen-fai Fong at Northwestern U  <wfong@northwestern.edu>

W. Fong (Northwestern), C. D. Kilpatrick (UCSC), J. Rastinejad (Northwestern), T. Laskar (U. Bath), and E. Berger (Harvard) report on behalf of a larger collaboration:

â€œWe report on new HST/WFC3 IR observations (PI: Berger; Program 15964) of the short GRB 200522A (Evans et al., GCN 27778) in the F125W and F160W filters at approximately 55 days post-burst. A total of 5223-s was obtained in both filters and the resulting images are deep enough to provide adequate templates for all previous epochs (F125W at 3.6 and 16.4 days, and F160W at 3.6 days; Fong et al., GCN 27826; Kilpatrick et al., GCN 27904). An independent analysis of the first two epochs of data resulted in a candidate afterglow (Oâ€™Connor et al., GCN 28100).

To constrain the presence of any transient sources, we first performed image subtraction between the observations in each filter taken at 3.6 days and the new 55-day templates using the HOTPANTS software (Becker 2015). In the difference images, we detect a high-significance residual within the XRT position (Beardmore et al., GCN 27780) and close to the host galaxy center in both filters. Given the contamination from residuals as a result of the core of the host galaxy, accurate photometry of the source will require further analysis.

We also perform image subtraction between the F125W observations at 16.4 days and 55 days. The source is no longer detected to a 3-sigma limit of m_F125W>27.3 AB mag. The fading behavior, coupled with the detection at 3.6 days in both filters, confirms the source as the counterpart to GRB 200522A. Based on our preliminary analysis, we cannot distinguish between whether the emission is resulting from the afterglow alone, or a combination of afterglow and kilonova emission.

We thank the HST staff for scheduling and implementing these observations.â€


GRB_name: GRB200716C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28128
SUBJECT: GRB 200716C: Enhanced Swift-XRT position
DATE:    20/07/17 05:32:43 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Using 1666 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 200716C, 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 = 196.01029, +29.64407 which is equivalent
to:

RA (J2000): 13h 04m 2.47s
Dec (J2000): +29d 38' 38.6"

with an uncertainty of 1.5 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: GRB200716C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28129
SUBJECT: GRB 200716C: Swift-XRT refined Analysis
DATE:    20/07/17 06:44:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.3 ks of XRT data for GRB 200716C (Ukwatta et al. GCN
Circ. 28124), from 86 s to 23.1 ks after the  BAT trigger. The data
comprise 578 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Goad et al. (GCN Circ. 28128). We cannot determine at the
present time whether the source is fading.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.56 (+/-0.03). The
best-fitting absorption column is  5.8 (+1.0, -0.9) x 10^20 cm^-2, in
excess of the Galactic value of 1.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.45 (+0.13, -0.05)
and a best-fitting absorption column consistent with the Galactic
value. The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.4 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.1 (+2.3, -0.0) x 10^20 cm^-2
Galactic foreground: 1.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.45 (+0.13, -0.05)

If the light curve continues to decay with a power-law decay index of
1.46, the count rate at T+24 hours will be 8.5 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.7 x
10^-13 (3.8 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/00982707.

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


GRB_name: GRB200716C
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28130
SUBJECT: GRB 200716C: Fermi-LAT detection 
DATE:    20/07/17 06:53:04 GMT
FROM:    Nicola Omodei at Stanford U.  <nicola.omodei@slac.stanford.edu>

M. Ohno (Hiroshima Univ/Eotvos Univ.), M. Arimoto (Kanazawa Univ.), N. Di Lalla, N. Omodei (Stanford University), F. Longo (University and INFN, Trieste),  
report on behalf of the Fermi-LAT Collaboration:

On July, 16th, 2020, Fermi-LAT detected high-energy emission from GRB 200716C, which was also detected by Fermi-GBM (trigger 616633066.180458/200716957; Fermi GBM Team GCN 28123) and Swift (Ukwatta et al. GCN 28124).

The best LAT on-ground location is found to be RA, Dec = 195.7, 29.9 (degrees, J2000) with an error radius of 0.3 deg (90% containment, statistical error only).
The best LAT position is consistent with the Swift position. This was 6 deg from the LAT boresight at the time of the GBM trigger: T0 =  22:57:41 UT.

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

The photon flux above 100 MeV in the time interval 0-1000 s after the GBM trigger is 5.3e-6 +/- 2.0e-6 ph/cm2/s.
The estimated photon index above 100 MeV is -1.9+/-0.2.

The highest-energy photon is a 8.2 GeV event which is observed 152 seconds after the GBM trigger.

The Fermi-LAT point of contact for this burst is
Nicola Omodei (nicola.omodei@stanford.edu).

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


GRB_name: GRB200716C
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28131
SUBJECT: GRB 200716C: Swift-XRT refined analysis correction
DATE:    20/07/17 07:01:57 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

GCN 28129 (Gropp et al.) incorrectly included a sentence that stated it
was not possible to tell if the X-ray afterglow of GRB 200716C was fading.
In fact, the first snapshot of data shows a complicated structure, which
can be modelled by changes in slope and overlapping flares. The late-time
light curve (from T0+4.3 ks) can be modelled with a power-law decay with a
decay index of alpha=1.56 (+/-0.11).

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


GRB_name: GRB200716C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28132
SUBJECT: GRB 200716C: possible host galaxy from the SDSS
DATE:    20/07/17 09:34:53 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. Dâ€™Avanzo (INAF-OAB), on behalf of the CIBO collaboration report:

Inspection of the SDSS reveals the presence of an extended object, classified as a galaxy, at a position consistent (within ~ 1â€) 
with the one reported for the optical afterglow of GRB 200716C (Ukwatta et al., GCN Circ. 28124; Lipunov et al., GCN Circ. 28125;
 Hu et al., GCN Circ. 28126). 

According to the SDSS DR16 this galaxy has AB magnitudes: 
u = 21.48 +/- 0.21, 
g = 20.46 +/- 0.05, 
r = 19.29 +/- 0.03,
i = 18.88 +/- 0.03, 
z = 18.54 +/- 0.09

and a photoz = 0.348 +/- 0.053. 

Further details can be found at the following link: 
http://skyserver.sdss.org/dr16/en/tools/explore/Summary.aspx?id=1237665442053095703

This object can be the host galaxy of GRB 200716C.


GRB_name: GRB200716C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28133
SUBJECT: GRB 200716C: AGILE/MCAL detection
DATE:    20/07/17 10:49:24 GMT
FROM:    Francesco Verrecchia at SSDC,INAF-OAR  <francesco.verrecchia@ssdc.asi.it>

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

The AGILE Mini-CALorimeter (MCAL) detected the GRB 200716C at T0 =
2020-07-16 22:57:41.38 +/- 0.01 s (UTC), reported by Swift-BAT (GCN #28122,
#28124), Fermi-GBM (GCN #28123), BOOTES-1 (GCN #28126), Swift-XRT (GCN
#28128, #28129, #28131), and Fermi-LAT (GCN #28130).

The event consists of two main episodes, lasting ~0.64 s and ~0.26 s,
respectively, which released a total number of 623 counts and 416 counts
in the detector (in the 0.4-100 MeV energy range), above an average
background rate of 650 Hz.

The time-integrated spectrum of the first episode can be fitted in the
energy range 0.4-20 MeV with single power-law with ph.ind. = 2.40
-0.29/+0.32, resulting in a reduced chi-squared of 1.15 (21 d.o.f.) and a
fluence of 4.6e-06 ergs/cm^2 (90% confidence level). The time-integrated
spectrum of the second episode can be fitted in the energy range 0.4-20
MeV with single power-law with ph.ind. = 2.51 -0.37/+0.43, resulting in a
reduced chi-squared of 1.08 (21 d.o.f.) and a fluence of 5.7e-06 ergs/cm^2
(90% confidence level).

The MCAL light curve can be found at
http://www.agilescienceapp.it/notices/GRB_068714_522025061.386471.png .

The event is also clearly visible in the scientific ratemeters (RMs) of
the MCAL (0.4-100 MeV) and Anti-Coincidence (50-200 keV) detectors. Their
light curves can be found at
http://www.agilescienceapp.it/notices/GRB200716C_AGILE_RMs.png .

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


GRB_name: GRB200716A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28134
SUBJECT: Fermi GRB 200716A: Global MASTER-Net observations report 
DATE:    20/07/17 11:30:20 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200716A ( Fermi GBM team, GCN 28109) errorbox  55482 sec after notice time and 55509 sec after trigger time at 2020-07-16 16:51:47 UT, with upper limit up to  19.0 mag. Observations started at twilight.  The observations began at zenith distance = 63 deg. The sun  altitude  is -12.5 deg. 

The galactic latitude b =  9 deg., longitude l = 252 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1402195

We obtain a following upper limits.  

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

   55539 | 2020-07-16 16:51:47 |         MASTER-SAAO | (09h 17m 38.83s , -17d 56m 49.4s) |   C |    60 | 18.4 |        
   55539 | 2020-07-16 16:51:47 |         MASTER-SAAO | (09h 10m 28.60s , -17d 57m 40.1s) |   C |    60 | 18.1 |        
   56058 | 2020-07-16 17:00:25 |         MASTER-SAAO | (09h 17m 34.76s , -17d 54m 58.7s) |   C |    60 | 19.0 |        
   56058 | 2020-07-16 17:00:25 |         MASTER-SAAO | (09h 10m 24.70s , -17d 55m 50.1s) |   C |    60 | 18.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200716C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28135
SUBJECT: GRB 200716C: Fermi GBM detection
DATE:    20/07/17 16:02:54 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

"At 22:57:41.18 UT on 16 July 2020, the Fermi Gamma-Ray Burst Monitor
(GBM) triggered
and located GRB 200716C (trigger 616633066 / 200716957) which was also
detected by the Swift (Ukwatta et al.,  GCN 28124), Fermi-LAT (Ohno et al.,
GCN 28130). The GBM on-ground location is consistent with both the Swift
and Fermi-LAT positions.

The angle from the Fermi LAT boresight at the GBM trigger time is 37
degrees.

The GBM light curve shows two overlapping pulses with a duration (T90) of
about 5.3 s (50-300 keV). The time-averaged spectrum from T0-0.26 s to
T0+4.9 s is best fit by a power law function with an exponential high-energy
cutoff.  The power law index is -1.07 +/- 0.03 and the cutoff energy,
parameterized as Epeak, is 716 +/- 97 keV.

The event fluence (10-1000 keV) in this time interval is (9.57 +/- 0.25)E-6
erg/cm^2. The 1-sec peak photon flux measured starting from T0 + 64 ms in
the 10-1000 keV band is 19.3 +/- 0.3 ph/s/cm^2.

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

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


GRB_name: GRB200716C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28136
SUBJECT: GRB 200716C: Swift-BAT refined analysis
DATE:    20/07/17 20:26:57 GMT
FROM:    Tilan Ukwatta at LANL  <tilan.ukwatta@gmail.com>

S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF),S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(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 200716C (trigger #982707)
(Ukwatta, et al., GCN Circ. 28124). The BAT ground-calculated
position is RA, Dec = 196.011, 29.636 deg which is
   RA(J2000)  =  13h 04m 02.5s
   Dec(J2000) = +29d 38' 08.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat,
90% containment). The partial coding was 57%.

The mask-weighted light curve shows two prominent peaks,
first at ~T+0.1 s and the second at ~T+2.1. Significant
activity is still visible until ~T+90 s. T90 (15-350 keV) is
86 +- 17 sec (estimated error including systematics).

The time-averaged spectrum from T-0.42 to T+112.63 sec is best
fit by a simple power-law model.  The power law index of the
time-averaged spectrum is1.65 +- 0.09.  The fluence in the
15-150 keV band is 3.6 +- 0.2 x 10^-06 erg/cm2. The 1-sec peak
photon flux measured from T-0.18 sec in the 15-150 keV band
is 10.7 +- 0.5 ph/cm2/sec.  All the quoted errors are at the
90% confidencelevel.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/982707/BA/


GRB_name: GRB200716B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28137
SUBJECT: GRB 200716B: Insight-HXMT/HE detection
DATE:    20/07/18 10:41:55 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, C. Cai, Y. F. Du, Y. G. Zheng, Q. Luo, Q. B. Yi, 
Y. Huang, C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-07-16T07:34:29.50 (T0), Insight-HXMT/HE detected 
GRB 200716B (trigger ID: HEB200716315) in a routine search of the data, 
which also triggered Fermi-GBM (Fermi GBM team, GCN 28113) 
and AstroSat-CZTI (Gupta et al. GCN 28118).

The Insight-HXMT/HE light curve mainly consists of single 
pulse with a duration (T90) of 3.41 s measured from T0-0.64 s. 
The 1-ms peak rate, measured from T0-0.21 s, is 1026 cnts/sec. 
The total counts from this burst is 2519 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200716315_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 
 
Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200716C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28138
SUBJECT: GRB 200716C: Optical observations from HCT
DATE:    20/07/18 12:03:42 GMT
FROM:    Brajesh Kumar at Indian Inst. of Astrophysics  <brajesh.kumar@iiap.res.in>

Brajesh Kumar (ARIES, Nainital), Anirban Dutta, Avinash Singh, G. C. 
Anupama, D. K. Sahu and Pramod Kumar (IIA, Bengaluru)

We observed the field of GRB 200716C (Fermi GBM, GCN #28123; Ukwatta et 
al., GCN #28124) with the Himalaya Faint Object Spectrograph and Camera 
(HFOSC) mounted on the 2-m Himalayan Chandra Telescope (IAO, Hanle, 
India). Multiple frames (each 300 sec) of the GRB field in Bessell R and 
I bands were obtained under moderate sky conditions. Preliminary PSF 
photometry on the stacked images was performed and calibrated against 
USNO-B1 catalogue. The estimated magnitudes are listed below:

   DATE     | UT (mean) | Exposure | Filter |  Mag
2020-07-17   17:06:34     300x3        R     17.55 +/- 0.18
2020-07-17   17:23:33     300X3        I     17.19 +/- 0.15

Here, we caution that there is an extended object near the GRB location 
(possibly the host galaxy, D'Avanzo et al. GCN #28132). However, the 
extended source is fainter (~19.23 and ~18.67 mag in R and I bands, 
respectively, USNO-B1). Therefore, the estimated magnitudes likely 
belong to the OT candidate (Lipunov et al., GCN #28125; Hu et al., GCN 
#28126), affected by the host contamination.

We thank the staff at IAO and CREST for helping with the observations.


GRB_name: GRB200716C
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28139
SUBJECT: GRB 200716C: CALET Gamma-Ray Burst Monitor detection
DATE:    20/07/18 12:06:31 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

S. Torii (Waseda U),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), 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 bright GRB 200716C (Swift detection: Ukwatta et al., GCN Circ. 28124,
Barthelmy et al., GCN Circ. 28136; Fermi-LAT detection: Ohno et al.,
GCN Circ. 28130; Fermi GBM detection: Veres and Meegan, GCN Circ. 28135;
https://gcn.gsfc.nasa.gov/other/200716C.gcn3) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 22:57:41.346 UTC on 16 July 2020.
The burst signal was seen by all CGBM detectors.
Because of a problem in one of the ground alert processing script,
the GCN notice was not distributed automatically for this event.

The burst light curve shows two narrow pulses followed by a weak tail. The
emission starts at T-0.1 sec and ends at T+6.8 sec. The T90 and T50
durations measured by the SGM data are 5.3 +- 1.1 sec and 1.9 +- 0.1 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1278975378/

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


GRB_name: GRB200718A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28140
SUBJECT: GRB 200718A: Fermi GBM Final Real-time Localization
DATE:    20/07/18 15:01:15 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 14:50:52 UT on 18 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200718A (trigger 616776657.413512 / 200718619).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 295.1, Dec = -3.9 (J2000 degrees, equivalent to J2000 19h 40m, -3d 53'), with a statistical uncertainty of 16.3 degrees.

The angle from the Fermi LAT boresight is 76.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200718619/quicklook/glg_skymap_all_bn200718619.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200718619/quicklook/glg_healpix_all_bn200718619.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200718619/quicklook/glg_lc_medres34_bn200718619.gif


GRB_name: GRB200718A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28143
SUBJECT: Fermi GRB 200718A: Global MASTER-Net observations report 
DATE:    20/07/18 22:45:15 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

V. Yurkov, A. Gabovich, Yu. Sergienko 
(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 200718A ( Fermi GBM team, GCN 28140) errorbox  24097 sec after notice time and 24129 sec after trigger time at 2020-07-18 21:33:02 UT, with upper limit up to  20.4 mag. The observations began at zenith distance = 32 deg. The sun  altitude  is -70.4 deg. 

The galactic latitude b = 10 deg., longitude l = 26 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1403477

We obtain a following upper limits.  

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

   24220 | 2020-07-18 21:33:02 |         MASTER-SAAO | (18h 46m 18.81s , +00d 03m 58.2s) |   C |   180 | 19.1 |        
   24220 | 2020-07-18 21:33:02 |         MASTER-SAAO | (18h 39m 29.75s , +00d 03m 03.8s) |   C |   180 | 19.3 |        
   24419 | 2020-07-18 21:36:21 |         MASTER-SAAO | (18h 46m 12.45s , +00d 03m 32.9s) |   C |   180 | 20.1 |        
   24419 | 2020-07-18 21:36:21 |         MASTER-SAAO | (18h 39m 23.34s , +00d 02m 37.4s) |   C |   180 | 19.5 |        
   24619 | 2020-07-18 21:39:41 |         MASTER-SAAO | (18h 46m 13.45s , +00d 04m 39.1s) |   B |   180 | 20.4 |        
   24619 | 2020-07-18 21:39:41 |         MASTER-SAAO | (18h 39m 24.06s , +00d 03m 42.6s) |   V |   180 | 18.4 |        
   24819 | 2020-07-18 21:43:01 |         MASTER-SAAO | (18h 46m 18.45s , +00d 03m 41.8s) |   B |   180 | 20.3 |        
   24819 | 2020-07-18 21:43:01 |         MASTER-SAAO | (18h 39m 29.05s , +00d 02m 44.8s) |   V |   180 | 18.4 |        
   25018 | 2020-07-18 21:46:20 |         MASTER-SAAO | (18h 46m 11.15s , +00d 02m 44.3s) |   B |   180 | 20.4 |        
   25018 | 2020-07-18 21:46:20 |         MASTER-SAAO | (18h 39m 21.74s , +00d 01m 47.1s) |   V |   180 | 18.4 |        
   25218 | 2020-07-18 21:49:40 |         MASTER-SAAO | (18h 46m 17.22s , +00d 03m 07.3s) |   R |   180 | 18.5 |        
   25218 | 2020-07-18 21:49:40 |         MASTER-SAAO | (18h 39m 27.79s , +00d 02m 19.8s) |   I |   180 | 18.0 |        
   25418 | 2020-07-18 21:53:00 |         MASTER-SAAO | (18h 46m 13.86s , +00d 04m 19.2s) |   R |   180 | 18.4 |        
   25418 | 2020-07-18 21:53:00 |         MASTER-SAAO | (18h 39m 24.44s , +00d 03m 31.6s) |   I |   180 | 17.8 |        
   25618 | 2020-07-18 21:56:20 |         MASTER-SAAO | (18h 46m 13.32s , +00d 02m 44.8s) |   R |   180 | 18.4 |        
   25618 | 2020-07-18 21:56:20 |         MASTER-SAAO | (18h 39m 23.91s , +00d 01m 57.0s) |   I |   180 | 17.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200716C
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28145
SUBJECT: GRB 200716C: Insight-HXMT/HE detection
DATE:    20/07/19 10:56:08 GMT
FROM:    Wangchen Xue at IHEP  <xuewc@ihep.ac.cn>

W. C. Xue, S. Xiao, Q. B. Yi, Y. G. Zheng, C. Cai, Q. Luo, 
C. K. Li, G. Li, X. B. Li, J. Y. Liao, S. L. Xiong, 
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team:

At 2020-07-16T22:57:41.18 (T0), Insight-HXMT/HE detected 
GRB 200716C (trigger ID: HEB200716956) in a routine search of the data, 
which also triggered Fermi/GBM (Fermi GBM team, GCN #28123), 
Swift/BAT (Ukwatta et al., GCN #28124), Fermi-LAT (Ohno et al., GCN #28130) 
and CALET GBM (Torii et al., GCN #28139).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 2.16 s measured from T0+0.19 s. 
The 1-ms peak rate, measured from T0+0.31 s, is 27488 cnts/sec. 
The total counts from this burst is 6590 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200716956_lc.jpg

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (deposited energy). 
Only gamma-rays with energy greater than about 200 keV can penetrate 
the spacecraft and leave signals in the CsI detectors installed inside 
of the telescope. 

Insight-HXMT is the first Chinese space X-ray telescope, which was 
funded jointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information about it could be found at: 
http://www.hxmt.org.


GRB_name: GRB200716C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28146
SUBJECT: GRB 200716C: VIRT optical detection.
DATE:    20/07/19 22:10:18 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

P. Gokuldass (UVI), D. Morris (UVI), N. Orange (OrangeWave Innovative
Science, LLC), A. Cucchiara (UVI/College of Marin), R. Strausbaugh (UVI)
report:

We observed the field of GRB200716C (Ukwatta et al, GCN 28124) with the
0.5m Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 07-17-2020 starting at 01:48:10 UT (T+2.8
hrs). We performed a series of exposures in R filter with a total exposure
of 1210 s. The weather conditions were clear during the hours of
observation with an average airmass of 2.2.

We detect a source consistent with the UVOT position (Ukwatta et al, GCN
28124) and optical transient identified by others (Lipunov et al. 28125, Hu
et al. 28126, Kumar et al. 28138) with magnitude:

  R= 17.1 +/- 0.2

The magnitude is estimated from comparison to nearby USNO B1 stars and is
not corrected for Galactic extinction. Further analysis is in progress to
confirm the decaying nature of the source. The VIRT is still in the
commissioning phase.

This work is supported by NASA-MUREP-MIRO grant NNX15AP95A, NSF EiR AST
Award 1901296, and NSF HBCU-UP AST Award 1831682. This message can be cited.


GRB_name: GRB200716C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28147
SUBJECT: Konus-Wind observation of GRB 200716C
DATE:    20/07/19 23:32:33 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

The GRB 200716C (Swift-BAT detection: Ukwatta et al., GCN 28124;
Fermi-LAT detection: Ohno et al., GCN 28130;
AGILE-MCAL detection: Ursi et al., GCN 28133;
Fermi-GBM detection: Veres & Meegan, GCN 28135;
CALET-GBM detection: Torii et al., GCN 28139;
Insight-HXMT/HE detection: Xue et al., GCN 28145)
triggered Konus-Wind (KW) at T0=82658.337 s UT (22:57:38.337).

The burst light curve shows two bright, short, hard-spectrum pulses
in the interval from ~T0-0.5 s to ~T0+2.5 s.
Both pulses are ~0.5 s wide and they are peaked
at ~T0-0.128 s and ~T0+2.096 s, respectively.
A much weaker post-burst emission is visible
in the KW 20-80 keV band up to ~T0+75 s.
The emission in the main pulses is seen up to ~7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200716_T82658/

As observed by Konus-Wind, the burst had
a fluence of (1.2 +/- 0.2)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0+0.128 s,
of (3.7 +/- 0.6)x10^-5 erg/cm^2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (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 = -1.07(-0.12,+0.14)
and Ep = 652(-154,+241) keV (chi2 = 91/97 dof).
Fitting by a GRB (Band) model yields similar alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 =91/96 dof).

The spectrum near the peak count rate (measured from T0
to T0+0.256 s) is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.51 (-0.19,+0.31),
the high energy photon index beta = -2.23 (-0.58,+0.29),
the peak energy Ep = 616 (-200,+226) keV,
(chi2 = 48/42 dof).

Assuming the photo z=0.348 of a possible host galaxy (D'Avanzo, GCN 28132)
and a standard cosmology with H_0 = 67.3 km/s/Mpc,
Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso ~ 3.9x10^51 erg,
the peak luminosity L_iso ~ 1.6x10^52 erg/s,
and the rest-frame peak energy of the time-integrated (peak)
spectrum Ep,z ~ 880 keV (~830 keV).

With these values, GRB 200716C is a clear outlier in the 'Amati' relation
built for 138 KW GRBs with known z (Tsvetkova et al., ApJ 850 161, 2017).
Meanwile, in both Eiso-Ep,z and Liso-Ep,z planes, the GRB 200716C position
is consistent with short-hard (Type I) GRB population,
see http://www.ioffe.ru/LEA/GRBs/GRB200716_T82658/GRB200716C.pdf

All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.


GRB_name: GRB200716C
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28148
SUBJECT: Konus-Wind observation of GRB 200716C: correction to GCN 28147
DATE:    20/07/20 12:49:52 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The GRB 200716C (Swift-BAT detection: Ukwatta et al., GCN 28124;
Fermi-LAT detection: Ohno et al., GCN 28130;
AGILE-MCAL detection: Ursi et al., GCN 28133;
Fermi-GBM detection: Veres & Meegan, GCN 28135;
CALET-GBM detection: Torii et al., GCN 28139;
Insight-HXMT/HE detection: Xue et al., GCN 28145)
triggered Konus-Wind (KW) at T0=82658.337 s UT (22:57:38.337).

The burst light curve shows two bright, short, hard-spectrum pulses
in the interval from ~T0-0.5 s to ~T0+2.5 s.
Both pulses are ~0.5 s wide and they are peaked
at ~T0+0.128 s and ~T0+2.096 s, respectively.
A much weaker extended post-burst emission is visible
in the KW 20-80 keV band up to ~T0+75 s.
The emission in the main pulses is seen up to ~7 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200716_T82658/

As observed by Konus-Wind, the burst had
a fluence of (1.2 +/- 0.2)x10^-5 erg/cm^2 and
a 64-ms peak energy flux, measured from T0+0.128 s,
of (3.7 +/- 0.6)x10^-5 erg/cm^2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (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 = -1.07(-0.12,+0.14)
and Ep = 652(-154,+241) keV (chi2 = 91/97 dof).
Fitting by a GRB (Band) model yields similar alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 =91/96 dof).

The spectrum near the peak count rate (measured from T0
to T0+0.256 s) is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.51 (-0.19,+0.31),
the high energy photon index beta = -2.23 (-0.58,+0.29),
the peak energy Ep = 616 (-200,+226) keV,
(chi2 = 48/42 dof).

Assuming the photo z=0.348 of a possible host galaxy (D'Avanzo, GCN 28132)
and a standard cosmology with H_0 = 67.3 km/s/Mpc,
Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso ~ 3.9x10^51 erg,
the peak luminosity L_iso ~ 1.6x10^52 erg/s,
and the rest-frame peak energy of the time-integrated (peak)
spectrum Ep,z ~ 880 keV (~830 keV).

With these values, GRB 200716C is a clear outlier in the 'Amati' relation
built for 138 long KW GRBs with known z (Tsvetkova et al., ApJ 850 161, 2017).
Meanwile, in both Eiso-Ep,z and Liso-Ep,z planes, the GRB 200716C position
is consistent with short-hard (Type I) GRB population,
see http://www.ioffe.ru/LEA/GRBs/GRB200716_T82658/GRB200716C.pdf

All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.


GRB_name: GRB200716C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28149
SUBJECT: GRB 200716C: FRAM-ORM afterglow detection
DATE:    20/07/21 09:04:42 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

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

report:

The 25cm robotic telescope FRAM-ORM at La Palma (Spain)
reacted robotically to the alert of GRB200716C (Ukwatta
et al GCNC 28124), obtaining a series of 20s unfiltered
images starting at 22:58:17.9 UT, i.e. 36.5s post trigger.

We clearly detect the source reported by other telescopes
(Ukwatta et al GCN 28124, Lipunov et al GCN 28125, Hu et al
GCN 28126) as it rises slowly. The brightness of the object
reaches maximum several minutes after the trigger with R =
16.1 and then it decays until the end of our dataset 2.4 h
after the trigger.


GRB_name: GRB200714E
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28150
SUBJECT: GRB 200714E: Swift-XRT afterglow detection
DATE:    20/07/21 15:18:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has conducted further observations of the field of the
Swift/BAT-GUANO-detected burst GRB 200714E (Tohuvavohu et al. GCN Circ.
28103). The observations now extend from T0+37.4 ks to T0+578.8 ks. The
source previously reported by D'Elia et al. (GCN Circ. 28107), "Source
1", is fading with 3-sigma significance, and is therefore likely the
GRB afterglow. Using 4152 s of PC mode data and 4 UVOT images, we find
an enhanced XRT position (using the XRT-UVOT alignment and matching
UVOT field sources to the USNO-B1 catalogue): RA, Dec = 196.82291,
-51.63937 which is equivalent to:

RA (J2000): 13h 07m 17.50s
Dec(J2000): -51d 38' 21.7"

with an uncertainty of 2.2 arcsec (radius, 90% confidence). This
position is 95 arcsec from the Swift/BAT position.  The source is
fading with alpha >0.5.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+0.6, -0.3). The
best-fitting absorption column is  consistent with the Galactic value
of 3.1 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 4.6 x 10^-11 (5.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.1 (+/-2.2) x 10^21 cm^-2
Galactic foreground: 3.1 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.6 (+0.6, -0.3)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00021017.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021017.

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


GRB_name: GRB200716C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28151
SUBJECT: GRB 200716C: CrAO, Terskol, Assy-Turgen optical observations
DATE:    20/07/21 15:34:11 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), S. Belkin (IKI),  V. Rumyantsev (CrAO), A. Gorshkov 
(INASAN), V. Kim (AFIF, Pulkovo Observatory),  N. Pankov (HSE), K. 
Kamyshnikov (HSE),   M. Krugov (AFIF), A. Volnova (IKI), E. Mazaeva 
(IKI) report on behalf of larger GRB follow-up collaboration:

We observed GRB 200716C (Fermi GBM team, GCN 28123; Ukwatta et al GCN 
28124;  Torii et al., GCN 28139;  Xue et al., GCN 28145; Frederiks et 
al., GCN 28147)  with ZTSH 2.6m telescope of CrAO observatory, 
Zeiss-2000 of Terskol observatory, and AZT-20 telescope of Assy-Turgen 
observatory.   The optical afterglow (Ukwatta et al., GCN 28124; Lipunov 
et al., GCN 28125; Hu et al., GCN 28126; Kumar et al., GCN 28138; 
Gokuldass et al., GCN 28146; Jelinek et al., GCN 28149) and possible 
host galaxy (Dâ€™Avanzo et al., GCN 28132)  is detected in a stacked 
image. Preliminary photometry of the (afterglow + possible host galaxy) 
is following

Date       UT start  t-T0    Filter Exp.   OT    Err. UL Telescope
                     (mid, days)     (s)
2020-07-17 19:17:52  0.84735 R      29*60  19.04 0.03 22.0 ZTSh
2020-07-17 19:50:49  0.87023 R      30*60  19.21 0.03 21.9 ZTSh
2020-07-18 18:33:32  1.83323 R      24*120 19.21 0.06 22.1 Zeiss-2000
2020-07-18 19:25:19  1.85253 R      17*60  19.21 0.06 22.1 ZTSh
2020-07-19 17:15:50  2.78066 r'     52*60  19.31 0.03 22.4 AZT-20

The photometry is based for R-calibration on the star
USNO-B1.0_id R
1196-0207871 16.18

and nearby SDSS stars for r' calibration
SDSS-DR12_id        r
J130423.13+294053.3 15.970
J130352.15+293733.9 16.592
J130416.16+293906.8 16.914

The above photometry besides of the first observation   is consistent 
with a brightness of possible host in USNO-B1.0 (R2=19.23) and in SDSS 
DR12 (r'= 19.301 +/- 0.026). We may conclude that we detected afterglow 
only in the first observation on  0.84735 days after trigger at R=19.04 
+/- 0.03.


GRB_name: GRB200716C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28152
SUBJECT: GRB 200716C: CAHA optical observation // Anomalous light curve behavior?
DATE:    20/07/21 21:36:27 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), M. Jelinek (ASU CAS Ondrejov), L. Izzo 
(DARK/NBI), A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), C. C. 
Thoene, M. Blazek, J. F. Agui Fernandez (all HETH/IAA-CSIC), B. Arroyo, 
G. Bergond, and S. Pedraz (all CAHA) report:

We observed the position of the afterglow (Ukwatta et al., GCN 28124; 
Lipunov et al., GCN 28125; Hu et al., GCN 28126; Kumar et al., GCN 
28138; Gokuldass et al., GCN 28146; Jelinek et al., GCN 28149; Pozanenko 
et al., GCN 28151) and potential host galaxy (D'Avanzo, GCN 28132) of 
the bright GRB 200716C (Swift detection: Ukwatta et al., GCN 28124; 
Fermi GBM/LAT detections: Veres & Meegan, GCN 28135/Ohno et al., GCN 
28130; AGILE detection: Ursi et al., GCN 28133; CALET detection: Torii 
et al., GCN 28139; Insight-HXMT/HE detection: Xue et al., GCN 28145) 
with the 2.2m telescope at Calar Alto, Almeria, Spain, equipped with 
CAFOS. We obtained a 180 s image in SDSS r', starting 2020-07-17 
20:37:13 UT, (mid-time 0.903495 days after the GRB trigger), at high 
airmass.

The host galaxy is clearly visible, but there is no clear detection of 
the afterglow. Calibrating against four nearby SDSS stars, we measure r' 
= 19.67 +/- 0.07 mag (AB mag). This value is fainter than those given by 
Pozanenko et al., GCN 28151, but we caution that an uneven background 
nearby may be influencing our magnitude measurement somewhat. Therefore, 
we are in agreement with Pozanenko et al. that the afterglow was not 
distinguishable from the host galaxy anymore at this point in time.

Combining the above-mentioned sources and the automatically reduced UVOT 
data (but excluding the point from Kumar et al.), we find the afterglow, 
starting with the second Swift orbit, decays according to a broken 
power-law with decay slopes alpha_1 = 0.80 +/- 0.04, alpha_2 = 5.5 +/- 
1.3, and break time 0.44 +/- 0.03 days. Hereby, we estimated host galaxy 
magnitudes in UVOT ubv based on the magnitudes given by D'Avanzo, GCN 
28132, and assumed a significantly fainter host in the UV filters. Even 
compared to this extreme fit, the data point given by Kumar et al. is 
nearly two magnitudes too bright, as the steep decay should have set on 
already here assuming it is achromatic. While we caution the second 
decay slope depends strongly on the assumed host magnitudes, even 
without a host there is clearly a break to a very steep decay seen in 
uvw2, b, white, and partially v.

This behavior is in strong contrast to the X-rays, which show an 
unbroken decay at alpha_X = 1.56 across this time span (Page & Evans, 
GCN 28131). Combined with indications from the Konus-Wind analysis that 
this may actually be a non-collapsar event (Frederiks et al., GCN 
28148), this points to this being an event of interest. Further 
follow-up is warranted.

[GCN OPS NOTE(21jul20):  Due to some non-printing characters in the
Subject-line of the submission, the MIME processor left a large chunk
of the header of the submission email to appear as more of the body
of the email. This has been removed from the archive copies.]


GRB_name: GRB200722A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28153
SUBJECT: GRB 200722A: BALROG localization (Fermi Trigger 617076900 / GRB 200722094)
DATE:    20/07/22 04:16:06 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
617076900 at 02:14:55 on 22 July 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 187.5+/-1.5 deg
Decl.(2000.0) = 4.7+/-1.3 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200722094/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200722094/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200722094/json

                        


GRB_name: GRB200716C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28154
SUBJECT: GRB 200716C: Kitab optical observations
DATE:    20/07/23 09:34:07 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), A. Zhornichenko (KIAM), A. 
Novichonok (Petrozavodsk State University, KIAM), Sh. Ehgamberdiev 
(UBAI) report on behalf of IKI-GRB-FuN:

We observed GRB 200716C  (Fermi GBM team, GCN 28123; Ukwatta et al GCN 
28124; Ohno et al., GCN 28130; Ursi et al., GCN 28133; Torii et al., GCN 
28139; Xue et al., GCN 28145; Frederiks et al., GCN 28147) with RC-36 
telescope of Kitab observatory starting July 17 (UT) 17:24:57.   The 
optical afterglow (Ukwatta et al., GCN 28124; Lipunov et al., GCN 28125; 
Hu et al., GCN 28126; Kumar et al., GCN 28138; Gokuldass et al., GCN 
28146; Jelinek et al., GCN 28149; Pozanenko et al., GCN 28151; Kann  et 
al., GCN 28152)  is detected in a stacked image. Despite we do not 
detect possible host galaxy (Dâ€™Avanzo et al., GCN 28132) the galaxy may 
contaminate photometry result.   Preliminary photometry of the afterglow 
   is following

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

2020-07-17 17:24:57  0.78952 R      59*60  18.2 0.3  18.6

The photometry is based  on nearby stars of USNO-B1.0

USNO-B1.0_id R2
1196-0207884 15.42
1197-0206830 14.99


GRB_name: GRB200723A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28155
SUBJECT: GRB 200723A: Fermi GBM Final Real-time Localization
DATE:    20/07/23 16:45:46 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 16:35:24 UT on 23 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200723A (trigger 617214929.786984 / 200723691).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 249.5, Dec = 58.1 (J2000 degrees, equivalent to J2000 16h 37m, 58d 06'), with a statistical uncertainty of 4.0 degrees.

The angle from the Fermi LAT boresight is 42.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200723691/quicklook/glg_skymap_all_bn200723691.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200723691/quicklook/glg_healpix_all_bn200723691.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200723691/quicklook/glg_lc_medres34_bn200723691.gif


GRB_name: GRB200723A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28156
SUBJECT: GRB 200723A: BALROG localization (Fermi Trigger 617214929 / GRB 200723691)
DATE:    20/07/23 17:05:27 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
617214929 at 16:35:24 on 23 July 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 233.5+/-8.3 deg
Decl.(2000.0) = 61.0+/-2.7 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200723691/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200723691/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200723691/json

                        


GRB_name: GRB200723A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28157
SUBJECT: Fermi GRB 200723A: Global MASTER-Net observations report 
DATE:    20/07/23 17:30:26 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200723A ( Fermi GBM team, GCN 28155) errorbox  61 sec after notice time and 87 sec after trigger time at 2020-07-23 16:36:52 UT, with upper limit up to  19.3 mag. The observations began at zenith distance = 12 deg. The sun  altitude  is -18.6 deg. 

The galactic latitude b = 33 deg., longitude l = 90 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1406982

We obtain a following upper limits.  

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

      98 | 2020-07-23 16:36:52 |        MASTER-Tunka | (18h 25m 28.78s , +57d 41m 39.0s) |  P| |    20 | 16.9 |        
     138 | 2020-07-23 16:37:33 |        MASTER-Tunka | (17h 10m 07.98s , +60d 43m 48.8s) |  P| |    20 | 17.3 |        
     182 | 2020-07-23 16:38:12 |        MASTER-Tunka | (17h 10m 03.28s , +60d 42m 46.7s) |  P| |    30 | 17.7 |        
     237 | 2020-07-23 16:39:01 |        MASTER-Tunka | (17h 10m 09.23s , +60d 42m 45.4s) |  P| |    40 | 17.8 |        
     301 | 2020-07-23 16:40:00 |        MASTER-Tunka | (17h 10m 05.43s , +60d 44m 21.0s) |  P| |    50 | 18.1 |        
     381 | 2020-07-23 16:41:10 |        MASTER-Tunka | (17h 10m 05.24s , +60d 42m 58.8s) |  P| |    70 | 18.4 |        
     465 | 2020-07-23 16:42:39 |        MASTER-Tunka | (16h 54m 47.92s , +59d 52m 11.4s) |   C |    60 | 19.3 |        
     581 | 2020-07-23 16:44:35 |        MASTER-Tunka | (16h 52m 45.47s , +61d 52m 08.0s) |   C |    60 | 18.9 |        
     690 | 2020-07-23 16:45:54 |        MASTER-Tunka | (16h 36m 47.21s , +57d 55m 40.5s) |  P| |   120 | 18.9 |        
     845 | 2020-07-23 16:48:14 |        MASTER-Tunka | (16h 36m 53.38s , +57d 55m 51.2s) |  P| |   150 | 19.0 |        
    1029 | 2020-07-23 16:51:03 |        MASTER-Tunka | (16h 36m 49.68s , +57d 57m 08.3s) |  P| |   180 | 19.0 |        
    1228 | 2020-07-23 16:54:22 |        MASTER-Tunka | (16h 36m 49.18s , +57d 55m 45.7s) |  P| |   180 | 19.0 |        
    1538 | 2020-07-23 17:00:33 |        MASTER-Tunka | (16h 54m 46.63s , +59d 52m 54.7s) |   C |    60 | 19.0 |        
    1619 | 2020-07-23 17:01:53 |        MASTER-Tunka | (17h 10m 54.87s , +59d 51m 40.0s) |   C |    60 | 19.0 |        
    1698 | 2020-07-23 17:03:13 |        MASTER-Tunka | (16h 52m 36.95s , +61d 50m 49.9s) |   C |    60 | 19.0 |        
    1778 | 2020-07-23 17:04:32 |        MASTER-Tunka | (17h 09m 48.78s , +61d 50m 45.5s) |   C |    60 | 19.1 |        
    2691 | 2020-07-23 17:19:45 |        MASTER-Tunka | (17h 10m 50.96s , +59d 50m 26.8s) |   C |    60 | 18.5 |        
    2771 | 2020-07-23 17:21:05 |        MASTER-Tunka | (17h 09m 50.15s , +61d 50m 39.3s) |   C |    60 | 19.1 |        
    2867 | 2020-07-23 17:22:42 |        MASTER-Tunka | (17h 00m 03.82s , +58d 20m 47.8s) |   C |    60 | 19.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200724A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28158
SUBJECT: GRB 200724A: Fermi GBM Final Real-time Localization
DATE:    20/07/24 05:16:35 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 05:06:18 UT on 24 Jul 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200724A (trigger 617259983.984672 / 200724213).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 121.7, Dec = -10.8 (J2000 degrees, equivalent to J2000 08h 06m, -10d 48'), with a statistical uncertainty of 6.1 degrees.

The angle from the Fermi LAT boresight is 71.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200724213/quicklook/glg_skymap_all_bn200724213.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200724213/quicklook/glg_healpix_all_bn200724213.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200724213/quicklook/glg_lc_medres34_bn200724213.gif


GRB_name: GRB200723A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28159
SUBJECT: GRB 200723A: GOTO candidate afterglow and host galaxy
DATE:    20/07/24 10:33:09 GMT
FROM:    Ben Gompertz at U of Warwick  <b.gompertz@warwick.ac.uk>

B. Gompertz (1); K. Wiersema (1); D. K. Galloway (2); R. Starling (3); 
J. Lyman (1); K. Ackley (2); Y.-L. Mong (2); D. Steeghs (1); V.Dhillon 
(4); P. O'Brien (3); G. Ramsay (5); D. Pollacco (1); E. Thrane (2); S. 
Poshyachinda (6); R. Kotak (7); L. Nuttall (8); E. Pall\'e (9); K. 
Ulaczyk (1); R. Cutter (1); A. Levan (1); T. Marsh (1); R. West (1); E. 
Stanway (1); T. Killestein (1); A. Casey (2); M. Brown (2); B. Muller 
(2); M. Dyer (4); J. Mullaney (4); E. Daw (4); S. Littlefair (4); J. 
Maund (4); L. Makrygianni (4); U. Burhanudin (4); R. Eyles (3); S. Tooke 
(3); S. Aukkaravittayapun (6); U. Sawangwit (6); S. Awiphan (6); D. 
Mkrtichian (6); P. Irawati (6); S. Mattila (7); T. Heikkil\"a (7); E. 
Rol (1)
((1) Warwick University, (2) Monash University, (3) University of 
Leicester, (4) University of Sheffield, (5) Armagh Observatory & 
Planetarium, (6) National Astronomical Research Institute of Thailand, 
(7) University of Turku, (8) University of Portsmouth, (9) Instituto de 
Astrofisica de Canarias)

report on behalf of the GOTO collaboration:

We carried out observations with the Gravitational-wave Optical 
Transient Observer (GOTO) in response to GRB 200723A (Fermi GBM; GCN 28155).

We made a series of 4x90 s exposures using our wide L-band filter 
(400-700 nm) covering the Fermi GBM error box (GCN 28155), with midtime 
22:42:55 UT on 23 July 2020.

Using a difference imaging analysis with recent survey observations of 
the same pointings as reference, we detect an uncatalogued source in a 
tiled observation taken at 21:25 UT (4.8 hours after trigger) with a 
magnitude of L = 18.5 Â± 0.05 mag based on PS1 catalogue calibrators 
located at (J2000):
RA 16:18:34.973
Dec +60:19:16.21

This source is coincident with a galaxy in the 2MASS redshift survey 
(Huchra et al, 2012) at a redshift of z = 0.0557. Given the large Fermi 
GBM uncertainty region, the probability that this source is an unrelated 
transient is large. We have registered it with the TNS with the ID 
AT2020qer. A previous GOTO observation taken on July 17 23:28:49 UT 
places a limiting magnitude of L > 19.2 (5 sigma) on this source 6 days 
prior to the Fermi GBM trigger.

GOTO is operated at the La Palma observing facilities of the University 
of Warwick on behalf of a consortium including the University of 
Warwick, Monash University, Armagh Observatory, the University of 
Leicester, the University of Sheffield, the National Astronomical 
Research Institute of Thailand (NARIT) and the Instituto de Astrofisica 
de Canarias (IAC) (https://goto-observatory.org 
<https://goto-observatory.org/>)


GRB_name: GRB200723A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28160
SUBJECT: GRB 200723A: Swift ToO observations
DATE:    20/07/24 13:47:15 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Fermi/GBM GRB 200723A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021019

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/GBM 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: GRB200723A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28161
SUBJECT: GRB 200723A: ATLAS observations of GOTO candidate AT2020qer 
DATE:    20/07/24 18:21:59 GMT
FROM:    Ken Smith at Queen's University Belfast  <k.w.smith@qub.ac.uk>

K. W. Smith, S. Srivastav, O. McBrien, S. J. Smartt, J. Gillanders,
P. Clark, M. Fulton, D. O'Neill, D. R. Young, M. McCollum (QUB),
A. Townsend (University of Manchester, QUB), T.-W. Chen (Stockholm),
J. Anderson (ESO), L. Denneau, A. Heinze, J. Tonry, H. Weiland (IfA,
University of Hawaii), B. Stalder (LSST), A. Rest (STScI), D. E. Wright
(University of Minnesota)

The transient AT2020qer reported by Gompertz et al (GCN 28159) as a
possible counterpart to GRB 200723A (Fermi GBM; GCN 28155), was detected
independently by ATLAS, the twin telescope system on Haleakala and Mauna
Loa as part of normal sky operations (Tonry et al. 2018, PASP, 130f4505,
Smith et al. 2020, PASP, 132f1014) on 2020-07-24.32 (MJD 59054.32).

Forced photometry at that position shows clear, rising activity before
the GRB event.

ATLAS forced photometry:
MJD          dt   m      dm    filter
59048.36523 -5.33 19.50  0.15  c
59048.36843 -5.32 20.13  0.24  c
59048.37442 -5.32 19.36  0.14  c
59048.40300 -5.29 19.47  0.15  c
59050.33364 -3.36 18.89  0.09  o
59050.33733 -3.35 19.10  0.11  o
59050.34287 -3.35 18.95  0.10  o
59050.35486 -3.34 19.01  0.10  o
59054.31747  0.63 18.18  0.06  o
59054.32069  0.63 18.20  0.05  o
59054.32670  0.64 18.34  0.06  o
59054.33871  0.65 18.27  0.06  o

where dt is the time difference between ATLAS MJD and the GRB trigger.

We therefore conclude that AT2020qer is unrelated to GRB 200723A and is
probably a young supernova candidate.


GRB_name: GRB200729A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28165
SUBJECT: GRB 200729A: Swift detection of a burst
DATE:    20/07/29 20:10:34 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P. A. Evans (U Leicester), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), M. J. Moss (GWU),
K. L. Page (U Leicester), M. H. Siegel (PSU) and
E. Troja (NASA/GSFC/UMCP) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 19:38:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200729A (trigger=984929).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 184.375, +45.582 which is 
   RA(J2000) = 12h 17m 30s
   Dec(J2000) = +45d 34' 56"
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 ~500 counts/sec (15-350 keV), at ~10 sec after the trigger. 

The XRT began observing the field at 19:40:25.5 UT, 140.4 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 184.37782, 45.59380 which
is equivalent to:
   RA(J2000)  = 12h 17m 30.68s
   Dec(J2000) = +45d 35' 37.7"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 43 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.07 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 6.5
(+3.87/-3.22) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
303 seconds after the BAT trigger. No credible afterglow candidate has been
found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the
XRT error circle. The typical 3-sigma upper limit has been about 19.2 mag. 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 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.01. 

The XRT position is within the extent of the nearby galaxy NGC 4242,
for which SIMBAD lists a redshift of 0.00176 (~7.4 Mpc). Follow up
observations are strongly encouraged. 

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


GRB_name: GRB200729A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28166
SUBJECT: Swift GRB 200729A: Global MASTER-Net observations report 
DATE:    20/07/29 20:52:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) was pointed to the Swift GRB 200729A ( P. A. Evans et al., GCN 28165) errorbox  3549 sec after notice time and 3617 sec after trigger time at 2020-07-29 20:38:22 UT, with upper limit up to  15.9 mag. Observations started at twilight.  The observations began at zenith distance = 48 deg. The sun  altitude  is -9.7 deg. 

The galactic latitude b = 71 deg., longitude l = 140 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1410562

We obtain a following upper limits.  

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

    3707 |          MASTER-IAC |  P- |   180 | 15.3 |        
    3946 |          MASTER-IAC |  P- |   180 | 15.9 |        


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


GRB_name: GRB200729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28167
SUBJECT: GRB200729A: BOOTES-1 optical upper limit
DATE:    20/07/29 22:00:41 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

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

Following the Swift trigger of GRB 200729A (Evans et al., GCNC 28165), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst. A given number of images were taken starting 19:39:29UT (84 s after trigger) during the twilight. In the co-adding of images taken later on, no source is detected which down to 19.6 mag (clear filter) at the XRT position, in the outskirts of the NGC 4242 galaxy. This is consistent with the non-detection reported by UVOT (Evans et al., GCNC 28165) and MASTER (Lipunov et al., GCNC 28166). Further observations are ongoing.

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


GRB_name: GRB200729A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28168
SUBJECT: GRB 200729A: Enhanced Swift-XRT position
DATE:    20/07/29 23:17:24 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 1504 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200729A, 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 = 184.37626, +45.59476 which is equivalent
to:

RA (J2000): 12h 17m 30.30s
Dec (J2000): +45d 35' 41.1"

with an uncertainty of 1.7 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: GRB200729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28169
SUBJECT: GRB 200729A: NOT optical upper limits
DATE:    20/07/29 23:50:29 GMT
FROM:    Daniele B Malesani at DTU Space  <malesani@space.dtu.dk>

Daniele B. Malesani (DTU Space), Antonio de Ugarte Postigo (HETH, 
IAA-CSIC; DARK/NBI), Luca Izzo (DARK/NBI), Jens Hjorth (DARK/NBI), D. 
Alexander Kann (HETH, IAA-CSIC), Christina C. Thoene (HETH, IAA-CSIC), 
Martin A. Guerrero (IAA-CSIC), report on behalf of a larger collaboration:

We observed the field of GRB 200729A (Evans et al., GCN 28165) with the 
Nordic Optical Telescope equipped with the ALFOSC imager. Observations 
were carried out in the r and z filters, and started on 2020 Jul 29.911 
UT (2.2 hr after the trigger), as soon as visibility allowed.

Within the XRT position of the candidate afterglow (Osborne et al., GCN 
28168), we detect no new sources compared to archival Pan-STARRS images. 
The 3-sigma limiting magnitudes are:

r > 22.5 AB
z > 22.0 AB

As noted by Evans et al. (GCN 28165), the location of the X-ray source 
lies on top of the nearby galaxy NGC 4242, whose distance is ~5.5 Mpc 
(from Simbad, which however presents values up to 10 Mpc). We note that, 
if the GRB is associated with NGC 4242, our limit would correspond to an 
absolute magnitude M_r > -6.2, which, in lack of significant extinction, 
provides a deep limit to the GRB optical luminosity. For example, the 
earliest detection of SN 2008D (3.5 hr after the outburst; Soderberg et 
al. 2008, Nat, 453, 469) had an absolute U-band magnitude M(U) = -12.3 
(even before correcting for the significant extinction).

At 5.5 Mpc, the gamma-ray fluence of 8*10^-7 erg cm^-2 (taken from 
https://gcn.gsfc.nasa.gov/notices_s/984929/BA/) would correspond to 
3*10^45 erg - fainter than the low-luminosity events GRB 980425, GRB 
170817A, and the X-ray output of SN 2008D.

While the visibility of this target from La Palma is now over, we 
encourage further observations from other locations.


GRB_name: GRB200729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28170
SUBJECT: GRB 200729A: TNG NIR upper limits
DATE:    20/07/30 00:13:08 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-SSDC), S. Campana, S. Covino (INAF-OAB), D. Malesani (DTU Space), 
A. Fiorenzano, A. Garcia de Gurtubai Escudero (INAF-TNG) on behalf of the CIBO collaboration report:

We observed the field of GRB 200729A (Evans et al., GCN Circ. 28165) with the Italian 3.6m TNG telescope equipped with 
NICS in imaging mode. A series of images were obtained with the J filter on 2020-06-29 from 22:28:28 UT to 22:55:43 UT 
(i.e. between about 2.8 and 3.3 hours after the burst). 

No obvious source is found within the enhanced XRT position (Osborne et al., GCN Circ. 28168) down to a 3-sigma limiting 
magnitude of J > 19.6 (Vega, calibrated against the 2MASS catalogue). 


GRB_name: GRB200729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28171
SUBJECT: GRB 200729A: Spitzer archival source detection
DATE:    20/07/30 00:50:11 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (U. of Bath), E. Berger (Harvard), C. Kilpatrick (UCSC), W. Fong,
R. Margutti, R. Chornock, A. Hajela, K. Alexander, D. Coppejans
(Northwestern) report:

"In an archival observation of NGC4242 by the Spitzer Space Telescope on
2012-08-06 (PI: van Zee), we find a point-like source coincident with the
enhanced X-ray position of GRB 200729A (Osborne et al, GCN 28168).
Photometry is complicated by the variable background; preliminary analysis
suggests the object has a flux density of ~ 11 uJy (21.3 AB mag), about 1
mag brighter than the NOT r/z limits (Malesani et al., GCN 28169).

Further analysis is in progress."


GRB_name: GRB200729A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28172
SUBJECT: GRB 200729A: Pan-STARRS pre-explosion source detection
DATE:    20/07/30 02:59:30 GMT
FROM:    Charles Kilpatrick at UC Santa Cruz  <cdkilpat@ucsc.edu>

C. D. Kilpatrick (UCSC), W. Fong, A. Hajela, R. Chornock, T. Laskar, R. Margutti, D. Coppejans, K. D. Alexander, (Northwestern), E. Berger (Harvard) report:

We examined the latest, enhanced XRT position of the long GRB 200729A detected by Swift (Evans et al., GCN 28165) in PAN-STARRS imaging. We downloaded the Pan-STARRS DR1 images and note the presence of a faint source detected within the XRT error circle (90% confidence Osborne et al., GCN 28168) at:

RA (J2000) = 12:17:30.32
Dec (J2000) = +45:35:41.4

The location of this source is consistent with the pre-burst counterpart detected in Spitzer/IRAC imaging (Laskar et al., GCN 28171).  Using a 1.5 arcsec aperture, we measure that the source has i=21.4+/-0.2 mag, y=21.0+/-0.2 mag, and z=21.0+/-0.1 mag. We note that our z-band photometry is 1 magnitude brighter than the limit reported by NOT (Malesani et al., GCN 28169). The source is not obviously detected in either Pan-STARRS g or r-band imaging. The source may be marginally extended, although it is too faint to definitively determine whether the source is intrinsically extended beyond the PSF of the Pan-STARRS DR1 imaging. 

Based on the column of neutral hydrogen inferred from the Swift/XRT X-ray spectrum (7.1e21 cm-2; https://www.swift.ac.uk/xrt_unenh_positions/00984929/), the total optical extinction to any counterpart is approximately A_V = 3.7 mag (Guver & Ozel, 2009, MNRAS, 400, 2050).  Assuming the Pan-STARRS source is in NGC 4242 with a TRGB distance of 5.3 Mpc (Sabbi et al. 2018, ApJS, 235, 23), any stellar counterpart would have M_i~-9.3 mag, which is extremely luminous for a star even with initial mass > 25 M_sun.  Thus the lack of an optical or near-infrared counterpart (Hu et al., GCN 28167; Lipunov et al., GCN 28166; Malesani et al., GCN 28169; Dâ€™Avanzo et al., GCN 28170) and large implied luminosity suggests that a supernova or non-terminal outburst from such a star in NGC 4242 is unlikely.

Alternatively, if the source is a background galaxy, and the i-z color represents a 4000 Angstrom break, this places the redshift of the galaxy at z~1.1, which would provide a natural explanation for the faint XRT flux (GCN 28165), and the lack of detected optical or NIR afterglow.


GRB_name: GRB200729A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28173
SUBJECT: GRB 200729A: IceCube neutrino search
DATE:    20/07/30 03:06:52 GMT
FROM:    Alex Pizzuto at ICECUBE/U of Wisconsin  <pizzuto@wisc.edu>

The IceCube Collaboration (http://icecube.wisc.edu/) reports:

IceCube has performed a search for track-like muon neutrino events arriving from the direction of GRB 200729A (https://gcn.gsfc.nasa.gov/gcn3/28165.gcn3) in a time window one hour in duration, beginning 10 minutes prior to the Swift BAT trigger (2020-07-29 19:28:05 UTC to 2020-07-29 20:28:05 UTC), during which IceCube was collecting good quality data.  Zero track-like events are found in spatial coincidence with GRB 200729A during this time period. We accordingly derive a time-integrated muon-neutrino flux upper limit for this source of E^2 dN/ dE = 5.5 x 10^-5 TeV cm^-2 at 90% CL, under the assumption of an E^-2 power law. 90% of events IceCube would detect from a source at this declination with an E^-2 spectrum are between approximately 1 TeV and 200 TeV.

The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica.  The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu<mailto:roc@icecube.wisc.edu>.


GRB_name: GRB200729A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28174
SUBJECT: Fermi-GBM Sub-Threshold candidate for GRB 200729A
DATE:    20/07/30 04:09:25 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

C. Malacaria (NASA-MSFC/USRA), E. Burns (NASA-GSFC), C. M. Hui (NASA-MSFC) 
and P. Veres (UAH) report on behalf of the Fermi-GBM team:

At 19:38:05 UT on 29 July 2020, the Swift Burst Alert Telescope (BAT)
triggered and located GRB 200729A (Evans et al. 2020, GCN 28165).

There was no Fermi-GBM onboard trigger around the event time of GRB 200729A. 
An automated, blind search for short gamma-ray 
bursts below the onboard triggering threshold in Fermi-GBM also 
identified no counterpart candidates.
The GBM targeted search [1], 
the most sensitive, coherent search for GRB-like signals, 
was run from +/-30 s around the GRB 200729A time.

The targeted search identified a transient source with an offset 
of about 7 s with respect to the Swift-BAT trigger time, 
consistent with the Swift-BAT light curve peak.
The candidate most significant timescale is 8.192 s centered at the offset time, 
with a log likelihood ratio of 62.
The Swift-XRT location is slightly out of the 3 sigma Fermi-GBM contours.
However, given the reasonable coincidence of trigger time, 
light curve peak-time and morphology,
this candidate is likely coincident with GRB 200729A.
The source spectrum at all significant time scales identified by the search 
is best fit by a power law function with an exponential
high-energy cutoff. 
The fit was performed between the Fermi-GBM trigger time T0 and T0+33 s.
The power law index is 0.70 +/- 0.53, 
and the cutoff energy, parameterized as Epeak, is 159 +/- 19 keV. 

The spectral analysis results presented above are preliminary.

[1] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB200729A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28175
SUBJECT: GRB 200729A: HST imaging
DATE:    20/07/30 04:27:51 GMT
FROM:    Gagandeep S. Anand at University of Hawaii  <gsanand@hawaii.edu>

G. S. Anand (Hawaii), R. B. Tully (Hawaii), L. Rizzi (Keck), I.
Karachentsev (Special Astrophysical Observatory, Russia), E. Shaya (UMD)

On 2020-07-15 12:14:59, we obtained Hubble Space Telescope imaging of NGC
4242 as part of the Every Known Nearby Galaxy survey (SNAP-15922, PI R.
Tully). Our data consists of imaging in F606W (760s) and F814W (760s)
bands, which cover the localized region from Swift of GRB 200729A.

Our observations show an extended red source within the 1.7" Swift
localization region, which may be a background galaxy.  DOLPHOT PSF
photometry shows several point sources within the 1.7" region as well, with
the two brightest point sources having (F606W, F814W) magnitudes of
(23.556, 23.509) and (26.182, 23.833). In our deep CMD, the observed
location of the TRGB suggests a distance of ~7.5 Mpc, further than previous
TRGB determinations of 5.3 Mpc (Sabbi et al. 2018, ApJS, 235, 23).

Link to color HST image, with background galaxy manually highlighted in red
circle:
https://gsanand.github.io/ngc4242.jpg


GRB_name: GRB200729A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28176
SUBJECT: GRB 200729A: Swift-XRT refined Analysis
DATE:    20/07/30 04:58:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.2 ks of XRT data for GRB 200729A (Evans et al. GCN
Circ. 28165), from 144 s to 25.2 ks after the  BAT trigger. The data
comprise 213 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. 28168).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.45 (+/-0.05).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.78 (+0.14, -0.13). The
best-fitting absorption column is  7.9 (+1.2, -1.1) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.35 (+0.22, -0.21)
and a best-fitting absorption column of 9.0 (+2.8, -2.4) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 6.8 x 10^-11 (8.8 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.0 (+2.8, -2.4) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^20 cm^-2
Excess significance: 6.2 sigma
Photon index:      1.35 (+0.22, -0.21)

If the light curve continues to decay with a power-law decay index of
1.45, the count rate at T+24 hours will be 1.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.6 x
10^-14 (9.9 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/00984929.

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


GRB_name: GRB200729A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28177
SUBJECT: GRB 200729A: Swift/UVOT Upper Limits
DATE:    20/07/30 12:41:58 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 200729A
145 s after the BAT trigger (Evans et al., GCN Circ. 28165).
No optical afterglow is detected above the flux of NGC 4242, consistent with the XRT position
(Osborne et al. GCN Circ. 28168), in the initial UVOT exposures. For all filters, we
have attempted to subtract off the light of NGC 4242 by measuring the flux
at a position offset from the XRT position, but of a similar brightness.

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           145          295          147         >20.0
u_FC               303          553          246         >18.9
white              145          1874         431         >20.0
v                  633          1749         136         >17.6
b                  559          1849         136         >18.7
u                  303          1824         362         >18.9
w1                 682          1799          97         >18.2
m2                 658          1428          39         >17.8
w2                1359          1725          58         >17.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28178
SUBJECT: GRB 200729A: further analysis of the NOT data
DATE:    20/07/30 15:36:00 GMT
FROM:    Daniele B Malesani at DTU Space  <malesani@space.dtu.dk>

Daniele B. Malesani (DTU Space), Antonio de Ugarte Postigo (HET, 
IAA-CSIC), Luca Izzo (DARK/NBI), Jens Hjorth (DARK/NBI), D. Alexander 
Kann (HET, IAA-CSIC), Christina C. Thoene (HET, IAA-CSIC), Martin A. 
Guerrero (IAA-CSIC), report on behalf of a larger collaboration:

With the availability of the full calibration set, we inspected again 
the data from our observation of GRB 200729A (Malesani et al., GCN 
28169) taken with the Nordic Optical Telescope (NOT). The seeing in our 
images is 1".

The object mentioned by Kilpatrick et al. (GCN 28172; see also Laskar et 
al., GCN 28171; Anand et al., GCN 28175) is marginally seen in our 
z-band image (a stack of 3x200 s exposures, with mean time 2.5 hr after 
the GRB trigger). Computing forced photometry against nearby stars from 
the Pan-STARRS catalog (and using a 1.5" radius aperture), we measure z 
= 22.1 +- 0.3 AB. We also note that the photometry value is sensitive to 
the chosen aperture size. This measurement is consistent with the 
preliminary upper limit we reported in GCN 28169.

No clear detection is present in the r-band image, though there is 
clearly a background of diffuse, patchy emission from NGC 4242 (as also 
visible in the HST image; Anand et al. GCN 28175).

We downloaded the Pan-STARRS images from 
https://ps1images.stsci.edu/cgi-bin/ps1cutouts . Using a 1.5" radius 
aperture, we measure for the object z = 22.5 +- 0.5 AB, which is 
consistent with our measurement. As a check, we also measure i = 22.45 
+- 0.18 AB. Both values are fainter than reported by Kilpatrick et al. 
(GCN 28172).

In summary, our NOT images provide confirmation for the optical source 
mentioned by Kilpatrick et al. (GCN 28172), but we do not find any 
indication for variability compared to the archival magnitudes from the 
Pan-STARRS survey. As other groups have noted (Kilpatrick et al., GCN 
28172; Anand et al., GCN 28175), this object could be a background 
galaxy unrelated to NGC 4242.


GRB_name: GRB200729A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28179
SUBJECT: GRB 200729A: Swift-BAT refined analysis
DATE:    20/07/30 18:22:38 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), P. A. Evans (U Leicester),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (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 200729A
(trigger #984929) (Evans et al., GCN Circ. 28165).
The BAT ground-calculated position is
RA, Dec = 184.360, 45.571 deg which is
   RA(J2000)  =  12h 17m 26.5s
   Dec(J2000) = +45d 34' 13.9"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.

The mask-weighted light curve shows a weak pulse that starts at ~T0,
peaks at ~T+6 s, and ends at ~T+130 s. T90 (15-350 keV)
is 122.0 +- 34.2 sec (estimated error including systematics).

The time-averaged spectrum from T+0.54 to T+136.54 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 0.96 +- 0.27.  The fluence in the 15-150 keV band
is 1.6 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+5.54 sec in the 15-150 keV band is 0.7 +- 0.3 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/984929/BA/


GRB_name: GRB200729A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28180
SUBJECT: GRB 200729A: Nanshan/NEXT optical upper limit
DATE:    20/07/30 23:10:38 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 200729A (Evans et al., GCN 28165) using the 
NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We obtained 
10x100s frames in the Sloan r-band, starting at 15:51:05 UT on 
2020-07-30, i.e., 20.22 hr after the burst.

No optical source is detected in our stacked image at the enhanced XRT 
position (Osborne et al., GCN 28168), down to a limiting magnitude of 
r~20.2, calibrated with the nearby PanSTARRS field.


GRB_name: GRB200729A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28181
SUBJECT: GRB 200729A: VLA Observations
DATE:    20/07/31 04:30:44 GMT
FROM:    Aprajita Hajela at Northwestern U  <AprajitaHajela2015@u.northwestern.edu>

A. Hajela, K. D. Alexander, R. Margutti (Northwestern), T. Laskar (U.
Bath), W. Fong (Northwestern), C. D. Kilpatrick (UCSC), and E. Berger
(Harvard) report on behalf of a larger collaboration:

We observed the Swift GRB 200729A (Evans et al., GCN 28165) at a mean
frequency of 6 GHz with the Karl G. Jansky Very Large Array (VLA) beginning
2020 July 31 00:06:33.0 UT (1.19 days after the burst). We do not detect
radio emission down to a 3-sigma limit of ~23 microJy.

We thank the VLA staff for rapidly approving our DDT and executing these
observations.


GRB_name: GRB200729A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28182
SUBJECT: GRB 200729A: RT-22 observations at 36.8 GHz
DATE:    20/07/31 15:44:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.E. Volvach (CrAO), A. Pozanenko (IKI), L.N. Volvach (CrAO)  report on 
behalf of IKI-GRB-FuN:

We observed the field of GRB 200729A (Evans et al., GCN 28165) with 
RT-22 telescope at 36.8 GHz starting on July 30 (UT) 14:12:00 i.e. 0.774 
days after trigger.
We do not detect radio emission in the enhanced XRT position (Osborne et 
al., GCN 28168). This is in agreement with non detection by VLA (Hajela 
et al. GCN 28181). Preliminary result of the observations is following.

Date       UT-start UT-stop  OT      Upper Limit (2 sigma)
                              mJy     mJy

2019-07-30  14:12   17:24    n/d     0.8


GRB_name: GRB200801A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28183
SUBJECT: GRB 200801A: Fermi GBM Final Real-time Localization
DATE:    20/08/01 08:37:39 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 08:27:14 UT on 1 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200801A (trigger 617963239.0814 / 200801352).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 321.1, Dec = 85.3 (J2000 degrees, equivalent to J2000 21h 24m, 85d 17'), with a statistical uncertainty of 11.3 degrees.

The angle from the Fermi LAT boresight is 73.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200801352/quicklook/glg_skymap_all_bn200801352.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200801352/quicklook/glg_healpix_all_bn200801352.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200801352/quicklook/glg_lc_medres34_bn200801352.gif


GRB_name: GRB200801B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28184
SUBJECT: GRB 200801B: Fermi GBM Final Real-time Localization
DATE:    20/08/01 15:46:11 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 15:35:46 UT on 1 Aug 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200801B (trigger 617988951.753576 / 200801650).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 70.5, Dec = -33.1 (J2000 degrees, equivalent to J2000 04h 42m, -33d 06'), with a statistical uncertainty of 1.3 degrees.

The angle from the Fermi LAT boresight is 38.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200801650/quicklook/glg_skymap_all_bn200801650.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200801650/quicklook/glg_healpix_all_bn200801650.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200801650/quicklook/glg_lc_medres34_bn200801650.gif


GRB_name: GRB200801B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28185
SUBJECT: GRB 200801B: BALROG localization (Fermi Trigger 617988951 / GRB 200801650)
DATE:    20/08/01 16:03:02 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

B. Biltzinger, F. Kunzweiler, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
617988951 at 15:35:46 on 01 Aug. 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).

The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 78.8+/-2.8 deg
Decl.(2000.0) = -28.7+/-1.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200801650/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200801650/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200801650/json

                        


GRB_name: GRB200801A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28188
SUBJECT: Fermi GRB 200801A: Global MASTER-Net observations report 
DATE:    20/08/01 23:30:13 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, E. Gorbovskoy, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, F.Balakin, 
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov,  D. Cheryasov
(Lomonosov Moscow State University, SAI, Physics Department),

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

H.Levato 
(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200801A ( Fermi GBM team, GCN 28183) errorbox  34900 sec after notice time and 34953 sec after trigger time at 2020-08-01 18:09:47 UT, with upper limit up to  18.1 mag. Observations started at twilight.  The observations began at zenith distance = 52 deg. The sun  altitude  is -10.5 deg. 

The galactic latitude b = 24 deg., longitude l = 128 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1411903

We obtain a following upper limits.  

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

   34983 | 2020-08-01 18:09:47 |      MASTER-Tavrida | (04h 52m 24.50s , +83d 37m 44.5s) |   C |    60 | 16.8 |        
   35073 | 2020-08-01 18:11:17 |      MASTER-Tavrida | (04h 50m 58.02s , +81d 47m 15.2s) |   C |    60 | 16.9 |        
   35154 | 2020-08-01 18:12:38 |      MASTER-Tavrida | (06h 27m 11.91s , +83d 49m 36.9s) |   C |    60 | 17.0 |        
   35244 | 2020-08-01 18:14:08 |      MASTER-Tavrida | (06h 00m 13.29s , +79d 40m 02.5s) |   C |    60 | 17.0 |        
   35338 | 2020-08-01 18:15:41 |      MASTER-Tavrida | (03h 54m 47.29s , +83d 47m 10.7s) |   C |    60 | 17.2 |        
   35432 | 2020-08-01 18:17:16 |      MASTER-Tavrida | (06h 08m 47.59s , +83d 39m 45.9s) |   C |    60 | 17.2 |        
   35525 | 2020-08-01 18:18:49 |      MASTER-Tavrida | (04h 50m 50.77s , +81d 46m 56.3s) |   C |    60 | 17.2 |        
   35619 | 2020-08-01 18:20:22 |      MASTER-Tavrida | (06h 32m 02.39s , +81d 39m 49.6s) |   C |    60 | 17.5 |        
   35710 | 2020-08-01 18:21:54 |      MASTER-Tavrida | (06h 27m 04.12s , +83d 51m 10.0s) |   C |    60 | 17.5 |        
   35791 | 2020-08-01 18:23:15 |      MASTER-Tavrida | (07h 43m 53.85s , +83d 51m 37.2s) |   C |    60 | 17.7 |        
   35879 | 2020-08-01 18:24:43 |      MASTER-Tavrida | (06h 00m 24.24s , +79d 40m 38.7s) |   C |    60 | 17.5 |        
   35970 | 2020-08-01 18:26:14 |      MASTER-Tavrida | (06h 10m 58.25s , +79d 50m 22.2s) |   C |    60 | 17.6 |        
   36061 | 2020-08-01 18:27:44 |      MASTER-Tavrida | (06h 08m 50.26s , +83d 40m 42.9s) |   C |    60 | 17.6 |        
   36152 | 2020-08-01 18:29:16 |      MASTER-Tavrida | (05h 48m 10.13s , +81d 49m 29.8s) |   C |    60 | 17.6 |        
   36233 | 2020-08-01 18:30:37 |      MASTER-Tavrida | (07h 43m 51.48s , +83d 51m 20.6s) |   C |    60 | 17.9 |        
   36324 | 2020-08-01 18:32:07 |      MASTER-Tavrida | (06h 46m 25.83s , +79d 40m 23.0s) |   C |    60 | 17.7 |        
   36416 | 2020-08-01 18:33:40 |      MASTER-Tavrida | (05h 51m 45.35s , +85d 47m 23.0s) |   C |    60 | 18.0 |        
   36509 | 2020-08-01 18:35:13 |      MASTER-Tavrida | (07h 29m 36.27s , +81d 42m 24.0s) |   C |    60 | 17.8 |        
   36607 | 2020-08-01 18:36:51 |      MASTER-Tavrida | (03h 53m 21.08s , +79d 46m 52.5s) |   C |    60 | 17.7 |        
   36697 | 2020-08-01 18:38:21 |      MASTER-Tavrida | (03h 40m 28.93s , +81d 35m 39.9s) |   C |    60 | 17.8 |        
   36783 | 2020-08-01 18:39:47 |      MASTER-Tavrida | (05h 51m 23.79s , +85d 49m 06.8s) |   C |    60 | 18.1 |        
   36864 | 2020-08-01 18:41:08 |      MASTER-Tavrida | (07h 46m 32.69s , +85d 50m 35.8s) |   C |    60 | 18.1 |        
   36955 | 2020-08-01 18:42:38 |      MASTER-Tavrida | (07h 29m 45.55s , +81d 43m 03.6s) |   C |    60 | 17.9 |        
   37046 | 2020-08-01 18:44:09 |      MASTER-Tavrida | (07h 43m 08.60s , +81d 52m 40.4s) |   C |    60 | 17.8 |        
   37131 | 2020-08-01 18:45:34 |      MASTER-Tavrida | (04h 28m 33.88s , +79d 38m 31.9s) |   C |    60 | 17.9 |        
   37222 | 2020-08-01 18:47:06 |      MASTER-Tavrida | (04h 39m 10.84s , +79d 47m 57.1s) |   C |    60 | 17.9 |        
   37311 | 2020-08-01 18:48:35 |      MASTER-Tavrida | (03h 40m 24.02s , +81d 35m 17.2s) |   C |    60 | 17.9 |        
   37401 | 2020-08-01 18:50:05 |      MASTER-Tavrida | (03h 53m 50.36s , +81d 45m 42.5s) |   C |    60 | 17.9 |        
   37482 | 2020-08-01 18:51:25 |      MASTER-Tavrida | (07h 46m 08.69s , +85d 51m 58.2s) |   C |    60 | 18.1 |        
   37562 | 2020-08-01 18:52:46 |      MASTER-Tavrida | (07h 43m 09.17s , +81d 52m 05.9s) |   C |    60 | 17.9 |        
   37648 | 2020-08-01 18:54:12 |      MASTER-Tavrida | (05h 14m 32.31s , +79d 39m 29.2s) |   C |    60 | 17.8 |        
   37741 | 2020-08-01 18:55:45 |      MASTER-Tavrida | (03h 53m 40.51s , +81d 46m 40.7s) |   C |    60 | 17.9 |        
   37839 | 2020-08-01 18:57:22 |      MASTER-Tavrida | (07h 32m 40.93s , +79d 42m 37.1s) |   C |    60 | 18.0 |        
   37934 | 2020-08-01 18:58:58 |      MASTER-Tavrida | (05h 48m 24.14s , +77d 48m 58.2s) |   C |    60 | 17.7 |        
   38029 | 2020-08-01 19:00:32 |      MASTER-Tavrida | (07h 34m 59.26s , +77d 41m 55.8s) |   C |    60 | 17.7 |        
   38125 | 2020-08-01 19:02:08 |      MASTER-Tavrida | (08h 40m 57.58s , +81d 54m 05.9s) |   C |    60 | 18.0 |        
   38214 | 2020-08-01 19:03:38 |      MASTER-Tavrida | (07h 32m 37.41s , +79d 43m 33.5s) |   C |    60 | 18.0 |        
   38306 | 2020-08-01 19:05:09 |      MASTER-Tavrida | (07h 43m 21.99s , +79d 52m 53.6s) |   C |    60 | 17.9 |        
   38386 | 2020-08-01 19:06:30 |      MASTER-Tavrida | (08h 29m 38.12s , +79d 53m 02.5s) |   C |    60 | 17.9 |        
   38474 | 2020-08-01 19:07:57 |      MASTER-Tavrida | (06h 18m 00.72s , +77d 41m 32.2s) |   C |    60 | 17.5 |        
   38565 | 2020-08-01 19:09:29 |      MASTER-Tavrida | (06h 26m 48.90s , +77d 50m 17.7s) |   C |    60 | 17.6 |        
   38661 | 2020-08-01 19:11:04 |      MASTER-Tavrida | (07h 35m 04.96s , +77d 43m 44.5s) |   C |    60 | 17.7 |        
   38753 | 2020-08-01 19:12:36 |      MASTER-Tavrida | (07h 43m 49.50s , +77d 53m 04.6s) |   C |    60 | 17.8 |        
   38833 | 2020-08-01 19:13:57 |      MASTER-Tavrida | (08h 40m 54.82s , +81d 55m 06.3s) |   C |    60 | 18.0 |        
   38914 | 2020-08-01 19:15:17 |      MASTER-Tavrida | (09h 38m 56.99s , +81d 55m 19.2s) |   C |    60 | 18.1 |        
   38995 | 2020-08-01 19:16:38 |      MASTER-Tavrida | (07h 43m 18.16s , +79d 51m 50.2s) |   C |    60 | 18.0 |        
   39075 | 2020-08-01 19:17:59 |      MASTER-Tavrida | (08h 29m 38.88s , +79d 53m 23.6s) |   C |    60 | 17.9 |        
   39156 | 2020-08-01 19:19:19 |      MASTER-Tavrida | (09h 15m 51.15s , +79d 55m 44.5s) |   C |    60 | 18.1 |        
   39244 | 2020-08-01 19:20:48 |      MASTER-Tavrida | (06h 56m 29.59s , +77d 40m 51.8s) |   C |    60 | 17.6 |        
   39335 | 2020-08-01 19:22:18 |      MASTER-Tavrida | (07h 43m 55.57s , +77d 53m 36.5s) |   C |    60 | 17.9 |        
   39416 | 2020-08-01 19:23:39 |      MASTER-Tavrida | (09h 38m 51.67s , +81d 55m 16.0s) |   C |    60 | 18.0 |        
   39496 | 2020-08-01 19:25:00 |      MASTER-Tavrida | (09h 15m 48.46s , +79d 56m 00.9s) |   C |    60 | 18.0 |        
   39577 | 2020-08-01 19:26:21 |      MASTER-Tavrida | (08h 22m 27.12s , +77d 52m 58.1s) |   C |    60 | 18.0 |        
   39663 | 2020-08-01 19:27:46 |      MASTER-Tavrida | (05h 01m 15.10s , +77d 39m 23.8s) |   C |    60 | 17.5 |        
   39755 | 2020-08-01 19:29:19 |      MASTER-Tavrida | (04h 59m 27.29s , +75d 49m 30.7s) |   C |    60 | 17.5 |        
   39846 | 2020-08-01 19:30:50 |      MASTER-Tavrida | (04h 18m 58.77s , +75d 38m 44.0s) |   C |    60 | 17.5 |        
   39931 | 2020-08-01 19:32:14 |      MASTER-Tavrida | (08h 22m 32.13s , +77d 53m 58.7s) |   C |    60 | 17.8 |        
   40013 | 2020-08-01 19:33:36 |      MASTER-Tavrida | (09h 01m 06.46s , +77d 53m 50.0s) |   C |    60 | 18.0 |        
   40093 | 2020-08-01 19:34:57 |      MASTER-Tavrida | (04h 31m 38.87s , +77d 47m 31.9s) |   C |    60 | 17.7 |        
   40187 | 2020-08-01 19:36:31 |      MASTER-Tavrida | (05h 39m 38.29s , +77d 40m 21.8s) |   C |    60 | 17.6 |        
   40280 | 2020-08-01 19:38:04 |      MASTER-Tavrida | (04h 59m 26.72s , +75d 48m 05.5s) |   C |    60 | 17.5 |        
   40374 | 2020-08-01 19:39:38 |      MASTER-Tavrida | (05h 58m 03.05s , +75d 41m 06.1s) |   C |    60 | 17.6 |        
   40455 | 2020-08-01 19:40:59 |      MASTER-Tavrida | (04h 18m 56.67s , +75d 37m 43.9s) |   C |    60 | 17.5 |        
   40536 | 2020-08-01 19:42:19 |      MASTER-Tavrida | (04h 51m 58.21s , +75d 39m 27.2s) |   C |    60 | 17.1 |        
   40620 | 2020-08-01 19:43:44 |      MASTER-Tavrida | (09h 01m 11.58s , +77d 54m 55.6s) |   C |    60 | 17.8 |        
   40705 | 2020-08-01 19:45:09 |      MASTER-Tavrida | (05h 39m 33.70s , +77d 38m 34.7s) |   C |    60 | 17.6 |        
   40797 | 2020-08-01 19:46:41 |      MASTER-Tavrida | (05h 32m 30.39s , +75d 49m 15.9s) |   C |    60 | 17.6 |        
   40888 | 2020-08-01 19:48:12 |      MASTER-Tavrida | (04h 52m 00.54s , +75d 39m 09.6s) |   C |    60 | 17.2 |        
   40969 | 2020-08-01 19:49:33 |      MASTER-Tavrida | (03h 44m 23.28s , +77d 37m 57.2s) |   C |    60 | 17.4 |        
   41050 | 2020-08-01 19:50:54 |      MASTER-Tavrida | (02h 56m 37.96s , +79d 41m 26.2s) |   C |    60 | 17.5 |        
   41130 | 2020-08-01 19:52:14 |      MASTER-Tavrida | (04h 45m 15.05s , +73d 37m 22.5s) |   C |    60 | 17.2 |        
   41212 | 2020-08-01 19:53:36 |      MASTER-Tavrida | (01h 46m 19.83s , +81d 46m 46.6s) |   C |    60 | 17.6 |        
   41379 | 2020-08-01 19:56:22 |      MASTER-Tavrida | (03h 44m 15.87s , +77d 37m 45.9s) |   C |    60 | 17.5 |        
   41459 | 2020-08-01 19:57:43 |      MASTER-Tavrida | (04h 22m 42.14s , +77d 37m 49.1s) |   C |    60 | 17.7 |        
   41540 | 2020-08-01 19:59:03 |      MASTER-Tavrida | (02h 56m 32.46s , +79d 42m 21.3s) |   C |    60 | 17.6 |        
   41620 | 2020-08-01 20:00:24 |      MASTER-Tavrida | (03h 42m 28.22s , +79d 36m 56.9s) |   C |    60 | 17.6 |        
   41701 | 2020-08-01 20:01:44 |      MASTER-Tavrida | (04h 45m 08.18s , +73d 37m 26.6s) |   C |    60 | 17.3 |        
   41842 | 2020-08-01 20:04:05 |      MASTER-Tavrida | (04h 53m 28.85s , +73d 48m 27.0s) |   C |    60 | 13.9 |        
   41926 | 2020-08-01 20:05:30 |      MASTER-Tavrida | (01h 46m 29.45s , +81d 47m 10.7s) |   C |    60 | 17.8 |        
   42007 | 2020-08-01 20:06:50 |      MASTER-Tavrida | (02h 43m 15.42s , +81d 42m 34.8s) |   C |    60 | 17.7 |        
   42091 | 2020-08-01 20:08:14 |      MASTER-Tavrida | (07h 11m 36.93s , +75d 52m 26.4s) |   C |    60 | 17.3 |        
   42178 | 2020-08-01 20:09:42 |      MASTER-Tavrida | (04h 22m 42.79s , +77d 38m 52.6s) |   C |    60 | 17.6 |        
   42259 | 2020-08-01 20:11:03 |      MASTER-Tavrida | (03h 42m 33.58s , +79d 38m 17.8s) |   C |    60 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


