# GCN_circulars

GRB_name: GRB201020B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28768
SUBJECT: GRB 201020B: continued Mondy optical observations
DATE:    20/10/24 09:51:25 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We continued observations of the GRB 201020B (Fermi GBM team, GCN 28702; 
Malacaria et al., GCN 28710; Arimoto et al., GCN 28716; Ursi et al., GCN 
28714; Ridnaia et al., GCN 28723) with AZT-33IK telescope of Sayan 
observatory (Mondy)  on Oct. 22, 23. The optical afterglow (Lipunov et 
al., GCN 28718; Xu et al., GCN 28719; Belkin et al., GCN 28725; Breeveld 
& Lien, GCN 28743; Vinko et al., GCN 28750; Kumar et al., GCN 28753) 
with redshift of z= 0.804 (Kann  et al., GCN 28765) is  detected in our 
stacked images in R-filter.

Preliminary photometry of the optical transient in a combined image is 
following

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

2020-10-22 17:35:31   2.02195    R      60*60   20.40 0.05   23.0
2020-10-23 14:33:52   2.89719    R      32*120  20.99 0.26   21.1


The photometry is based on the nearby USNO-B1.0 stars
USNO-B1.0_id R2
1670-0037414 16.74
1670-0037586 16.16


GRB_name: GRB201020B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28769
SUBJECT: GRB 201020B: follow-up observations at Konkoly
DATE:    20/10/24 11:11:02 GMT
FROM:    Jozsef Vinko at Konkoly Observatory  <vinko@konkoly.hu>

J. Vinko (Konkoly/ELTE/U Szeged), A. Pal, L. Kriskovics, R. Szakats, A. Ordasi and K. Vida (Konkoly) 
report on behalf of the "Transient Astrophysical Objects" project:

Follow-up observations of the optical afterglow of GRB 201020B 
(Fermi team, GCN 28702; Lipunov et al. GCN 28704; 
Malacaria and Meegan, GCN 28710; Ursi et al. 28714; Arimoto et al., GCN 28716; 
Lipunov et al., GCN 28718; Xu et al., GCN 28719; Ridnaia et al., GCN 28723;  
Belkin et al., GCN 28725; Sbarufatti et al., GCN 28740; Breeveld et al., GCN 28743;
Vinko et al. GCN 28750; Kumar et al. GCN 28753; Kann et al. GCN 28765; Belkin et al.
GCN 28768) with the 0.8m RC80 telescope at Konkoly Observatory yielded the following magnitudes
for the transient: 

Date         UT-mid    t-T0(hr)   Exp(s)   Filter   AB mag     Err
2020-10-22   19:31:01  49.94      6 x 300  SDSS-r   20.592  0.172
2020-10-22   19:36:07  50.04      6 x 300  SDSS-i   20.566  0.264

tied to local PS1 stars. 

Our data are consistent with the magnitudes reported by Belkin et al. (GCN 28768).
At the redshift of z=0.8 (Kann et al. GCN 28765) these correspond to
M ~ -22.9 absolute mag. 


GRB_name: GRB201024A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28770
SUBJECT: GRB 201024A: Enhanced Swift-XRT position
DATE:    20/10/24 11:13:17 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 890 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 201024A, 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 = 125.95224, +3.35444 which is equivalent
to:

RA (J2000): 08h 23m 48.54s
Dec (J2000): +03d 21' 16.0"

with an uncertainty of 2.7 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: GRB201024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28771
SUBJECT: GRB 201024A: VIRT optical observations
DATE:    20/10/24 15:49:18 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

P. Gokuldass (UVI), R. Strausbaugh (UVI), N. Orange (OrangeWave Innovative
Science, LLC), D. Morris (UVI), A. Cucchiara (UVI/College of Marin) report:

We observed the field of GRB201024A (F. E. Marchall et al., GCN 28761) with
the
0.5m Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 10-24-2020 starting at 06:39:34.2 UT (T+3.3
hrs). We performed a series of exposures in R filter with a total exposure
of 1430 s. The weather conditions were partly cloudy during the hours of

observation with an average arimass of 1.5.


We find no new source within the enhanced XRT position error circle
(P. A. Evans et al., 28770) and report the following 3-sigma upper limit:

T_mid       ||Exposure     ||Filter      ||Limit
T+ 5 hrs    ||1430s          ||R            ||>18.9

The limit is estimated from comparison to nearby USNO B1 stars and is not
corrected for Galactic extinction. The VIRT is still in the commissioning
phase.



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: GRB201020B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28772
SUBJECT: GRB 201020B: 1.3m DFOT optical observations
DATE:    20/10/24 18:24:59 GMT
FROM:    Dimple Panchal at ARIES, India  <dimple@aries.res.in>

Dimple (ARIES), A. Ghosh (ARIES), Bhavya (ARIES) , R. Gupta (ARIES) , A. Kumar (ARIES), B. Kumar (ARIES), K. Misra (ARIES), and S. B. Pandey (ARIES) report: 

We carried out the follow-up observations of GRB 201020B ( Fermi team, GCN 28702; Lipunov et al. GCN 28704; Malacaria and Meegan, GCN 28710; Ursi et al. 28714; Arimoto et al., GCN 28716; Lipunov et al., GCN 28718; Xu et al., GCN 28719; Ridnaia et al., GCN 28723; Belkin et al., GCN 28725; Sbarufatti et al., GCN 28740; Breeveld et al., GCN 28743; Vinko et al. GCN 28750; Kumar et al. GCN 28753; Kann et al. GCN 28765; Belkin et al. GCN 28768; Vinko et al. GCN 28769 ) using 1.3m Devasthal Fast Optical Telescope (DFOT) at Devasthal observatory of Aryabhatta Research Institute of observational sciencES (ARIES), India. The observation was started on 2020-10-21 at 21:41:37 UT. We observed a series of images with the exposure time of 60 seconds in both R and I filters (Johnson-Cousins) covering Swift UVOT position RA, Dec = 05h 01m 52.03s, +77d 04' 05.9" ( Sbarufatti et al. GCN 28740). An uncataloged source is clearly visible in the stacked images in both the bands at the position consistent with V. Lipunov et. al. GCN 28718; D. Xu et. al. GCN 28719. 

Preliminary photometry of the optical transient in the combined images is following 
Date Start_UT T_start-T0 (hrs) Filter Exp time (s) Magnitude Mag_error 


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

2020-10-21 21:41:37 28.280 R 15*60 19.741 0.0262 

2020-10-21 22:00:04 28.588 I 15*60 19.298 0.0468 

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

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


GRB_name: GRB201020B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28773
SUBJECT: GRB 201020B: follow-up observations with Savelli Telescope
DATE:    20/10/24 19:34:16 GMT
FROM:    Luciano Nicastro at INAF-OAS  <luciano.nicastro@inaf.it>

L. Nicastro (INAF-OAS), A. Brosio (Osservatorio Astronomico Lilio), S.
Savaglio (UNICAL)

We observed the afterglow
(Lipunov et al., GCN 28718; Xu et al., GCN 28719; Belkin et al., GCN 28725;
Breeveld & Lien, GCN 28743; Vinko et al., GCN 28750; Kumar et al., GCN
28753; Kann et al., GCN 28765; Belkin et al., GCN 28768;  Dimple et al.,
GCN 28772)
of GRB 201020B
(Fermi GBM Team, GCN 28702; Fermi GBM detection: Malacaria & Meegan, GCN
28710; Fermi LAT detection: Arimoto et al., GCN 28716; AGILE detection:
Ursi et al., GCN 28714; Konus-Wind detection: Ridnaia et al., GCN 28723)
with the 0.5m telescope of the Osservatorio Astronomico Lilio, located in
Savelli (South Italy).


Date / UT-mid    JD    T-T0(hr)    Exp(s)    Filter     Mag (AB)
2020-10-21T18:47:48.85 | 2459144.28320 | 25.23  | 5 x 300 | Sloan-r | 19.60
+/- 0.12
2020-10-21T19:35:28.72 | 2459144.31630 | 26.03  | 5 x 300 | Sloan-g | 20.02
+/- 0.15


Magnitudes, calibrated wrt nearby PanSTARRS field stars, are not corrected
for galactic extinction.

Fog prevented us from performing further observations in the following
nights.


GRB_name: GRB201024A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28774
SUBJECT: GRB 201024A: Swift/UVOT Detection
DATE:    20/10/25 00:02:46 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) 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 201024A
495 s after the BAT trigger (Marshall et al., GCN Circ. 28761).  A source
consistent with the XRT position (Evans et al. GCN Circ. 28770) is
detected in the initial UVOT exposures.

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

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

white              495          645          148         17.94 +/- 0.05
v                  653          845           39         17.39 +/- 0.30
b                  750         1348           58         18.65 +/- 0.32
u                  726         1151           39         17.86 +/- 0.29
w1                 702         1471           78         17.46 +/- 0.30
m2                 677         2140          117        >18.4
w2                 801         2091          117        >17.7

The observations show a rapid decay as reported by MASTER (Lipunov et al,
GCN Circ. No. 28762).
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: GRB201024A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28775
SUBJECT: GRB 201024A: Swift-XRT refined Analysis
DATE:    20/10/25 01:18:16 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), J. D. Gropp (PSU), J.A. Kennea (PSU), A.
Tohuvavohu (U. Toronto) and F.E. Marshall report on behalf of the
Swift-XRT team:

We have analysed 6.0 ks of XRT data for GRB 201024A (Marshall et al.
GCN Circ. 28761), from 450 s to 48.0 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Evans et al. (GCN Circ. 28770).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.98 (+0.07, -0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.08 (+0.19, -0.18). The
best-fitting absorption column is  1.7 (+0.6, -0.5) x 10^21 cm^-2, in
excess of the Galactic value of 3.6 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 3.6 x 10^20 cm^-2
Excess significance: 4.1 sigma
Photon index:      2.08 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
0.98, the count rate at T+24 hours will be 5.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-13 (2.6 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/01001514.

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


GRB_name: GRB201020B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28776
SUBJECT: GRB 201020B: HCT and GIT continued optical follow-up observations
DATE:    20/10/25 09:04:20 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar(IITB), S. Kiran (IIA), J.Stanzin (IAO), V. Bhalerao(IITB), G. C.
Anupama(IIA), S. Barway(IIA) report on behalf of the HCT team:

We followed-up GRB 201020B reported by Fermi GBM Team (GCN #28702, also
see: V. Lipunov et. al., GCN #28718; D. Xu et. al., GCN #28719) with 2.0m
Himalayan Chandra Telescope (HCT) and 0.7m GROWTH-India Telescope (GIT). We
obtained a series of 300-sec exposures in the Rc, r filters. Afterglow was
clearly detected at a position consistent with V. Lipunov et. al., GCN
#28718; D. Xu et. al., GCN #28719. Here are the photometric results from
HCT & GIT observations:-

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

 JD (mid) | T_mid-T0(hrs) | Filter | Mag | Telescope |

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

 2459145.40625 | 52.22 | r | 21.01 +/- 0.04 | GIT |

 2459146.32699 | 74.80 | Rc | 21.28 +/- 0.04 | HCT |

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

Our results are consistent with the power-law decay of 1.67 reported in S.
Belkin et al. GCN #28768; H. Kumar et al. GCN #28753.


These observations were carried out under the ToO program HCT-2020-C3-P6.
We thank HCT and GIT staff for undertaking the observations.

The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB201024A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28777
SUBJECT: GRB201024A: rebrightening after initial steep decline
DATE:    20/10/25 15:33:11 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

Paul Kuin (UCL/MSSL) reports on behalf of the Swift UVOT Team:

We now have the light curve of GRB 201024A in the seven UVOT filters
from the start of our observations T0+495s until T0+100ks. After
a steep decline a rebrightening is seen starting around T0+1400s
which then peaks between 20 and 70 ks.


GRB_name: GRB201024A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28778
SUBJECT: GRB 201024A: Swift-BAT refined analysis
DATE:    20/10/25 23:46:04 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@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), F. E. Marshall (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), (i.e. the Swift-BAT team):

Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 201024A (trigger #1001514)
(F. E. Marshall et al., GCN Circ. 28761).  The BAT ground-calculated position is
RA, Dec = 125.959, 3.357 deg which is
   RA(J2000)  =  08h 23m 50.3s
   Dec(J2000) = +03d 21' 24.6"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 22%.

The BAT light curve showed a single peak structure with a duration of about 6 sec.
T90 (15-350 keV) is 5.00 +- 2.24 sec (estimated error including systematics).

The time-averaged spectrum from T+0.01 to T+6.01 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.10 +- 0.18.  The fluence in the 15-150 keV band is 8.1 +- 0.9 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+1.01 sec in the 15-150 keV band
is 3.7 +- 0.6 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1001514/BA/


GRB_name: GRB201024A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28779
SUBJECT: GRB 201024A: MITSuME Akeno optical upper limits
DATE:    20/10/26 09:38:09 GMT
FROM:    Katsuhiro L. Murata at Nagoya U  <murata@u.phys.nagoya-u.ac.jp>

M. Niwano, K. L. Murata, R. Hosokawa, R. Adachi, F. Ogawa, N. Nakamura, N.
Ito, 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 201024A (F. E. Marshall et al.,GCN Circular
#28761) with the optical three color (g', Rc, and Ic) CCD cameras attached
to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan.

We observed for two nights. The observation with a series of 60 sec
exposures started at 2020-10-24 16:04:04UT for the first night and
2020-10-25 15:56:17UT for the second night. We stacked the images with good
conditions each night. We did not detect the point source reported by other
telescopes (Lipunov et al. GCN Circular #28760, Fernandez-Garcia et al.
#28763, de Ugarte Postigo et al. #28764, Martin Jelinek et al. #28766). We
obtained the 5-sigma limits of the stacked images as follows.

T0+[hour] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
13.78 2020-10-24T18:27:11 11520 g'>20.2, Rc>20.4, Ic>19.7
38.48 2020-10-25T17:17:59 1980 g'>19.4, Rc>19.6, Ic>18.8
------------------------------------------------------------------------------------------------
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., accepted for publication in
PASJ, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire).


GRB_name: GRB201024A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28780
SUBJECT: GRB201024A: correction to GCN28777 - there was no rebrightening
DATE:    20/10/26 11:23:46 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

Paul Kuin (UCL/MSSLL) reports:

Due to an incorrect background subtraction in the later exposures of
GRB201024A, an incorrect 'rebrightening' was found in the Swift-UVOT
photometry. In actuality the source had faded away.

My sincere apologies if this has caused any problems.


GRB_name: GRB201020B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28781
SUBJECT: GRB 201020B: 1.3m DFOT continued optical follow-up observations
DATE:    20/10/26 12:23:26 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

Amit Kumar (ARIES), Rahul Gupta (ARIES), Dimple (ARIES), Ankur Ghosh
(ARIES), Kaushal Sharma (ARIES), Amar Aryan (ARIES), Brajesh Kumar
(ARIES), Kuntal Misra (ARIES), and Shashi B. Pandey (ARIES) report:

We followed-up Fermi GBM triggered GRB 201020B (Fermi team, GCN 28702;
Lipunov et al. GCN 28704; Malacaria and Meegan, GCN 28710; Ursi et al.
GCN 28714; Arimoto et al., GCN 28716; Lipunov et al., GCN 28718; Xu et
al., GCN 28719; Kann et al. GCN 28765) using the 1.3m Devasthal Fast
Optical Telescope (DFOT) at Devasthal observatory of Aryabhatta
Research Institute of observational sciencES (ARIES), India.
The observations were carried out on 2020-10-23 (from 19:14:51 to
19:26:16 UT) and 2020-10-24 (from 18:18:43 to 19:24:14 UT) in multiple
bands. We took a series of images with the exposure time of 120
seconds in multiple Bessel filters, covering Swift UVOT position
(Sbarufatti et al. GCN 28740).
The optical transient reported by V. Lipunov et. al. GCN 28718; D. Xu
et. al. GCN 28719 is clearly visible in the stacked images.

The R-band magnitudes of the GRB afterglow estimated from the
photometry of stacked images are as follows:

Date       Start_UT   T_start-T0 (hrs)  Filter  Exp time (s)
Magnitude   Mag_error
----------------------------------------------------------------------------------------------------------------------------

2020-10-23   19:14:51   73.683            R      15*120         21.34       0.05
2020-10-24   19:24:14   97.839            R      30*120         21.83
     0.05
----------------------------------------------------------------------------------------------------------------------------

The estimated magnitudes have not been corrected for the Galactic
extinction in the direction of the GRB. Photometric calibration is
performed using the following standard stars from the USNO-B1.0
catalog:

1670-0037558
1670-0037526
1670-0037460
1670-0037451
1670-0037450
1670-0037447
Our estimated magnitudes in the R-band, along with the measurements
reported by Belkin et al., GCN 28725; Vinko et al. GCN 28750; Belkin
et al. GCN 28768; Vinko et al. GCN 28769; Dimple et al. GCN 28772;
Nicastro et al. GCN 28773, and Kumar et al. GCN 28776, suggest that
the afterglow of GRB 201020B is fading with a power-law index of 1.66
+/- 0.12.
The magnitudes reported by Vinko et al. GCN 28750, Vinko et al. GCN
28769, and Nicastro et al. GCN 28773 are convetred to R-band
magnitudes using the tranformation equations provided by Lupton et al.
(2005).
This power-law index is well consistent with those reported by Kumar
et al. GCN 28753 and Belkin et al. GCN 28768.

This circular may be cited.


GRB_name: GRB201024A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28782
SUBJECT: GRB 201024A: 1.3m DFOT optical observations
DATE:    20/10/26 20:10:16 GMT
FROM:    Rahul Gupta at ARIES, India  <rahul@aries.res.in>

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

We observed the optical afterglow ( Lipunov et al., GCN 28760; Marshall et al., GCN 28761; Fernandez-Garcia et al., GCN 28763; de Ugarte Postigo et al., GCN 28764; Jelinek et al., GCN 28766; and Kuin et al., GCN 28774 ) of Swift triggered GRB 201024A (Marshall et al., GCN 28761) using the 1.3m Devasthal Fast Optical Telescope (DFOT) at Devasthal observatory of Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2020-10-24 at 21:03:09 UT . Multiple frames having an exposure time of 120 s were taken in R and I filters. We clearly detected the optical counterpart in the stacked images. 

The preliminary photometric estimate of the afterglow in the stacked images is the following : 


Date Start_UT T_start-T0 (hrs) Filter Exp time (s) Magnitude Mag_err 
------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------------------------------------ 

2020-10-24 21:03:09 18.24 I 30*120 20.12 0.07 

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


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

This circular may be cited. 


GRB_name: GRB201026A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28784
SUBJECT: GRB 201026A: Swift detection of a burst
DATE:    20/10/26 22:56:15 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. B. Cenko (GSFC), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), M. J. Moss (GWU),
D. M. Palmer (LANL) and T. Sbarrato (INAF-OAB) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 22:37:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201026A (trigger=1002103).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 196.664, +83.761 which is 
   RA(J2000) = 13h 06m 39s
   Dec(J2000) = +83d 45' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex peak
structure with a duration of about 30 sec.  The peak count rate
was ~1700counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 22:38:53.0 UT, 78.8 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 196.7408, 83.7849 which is equivalent to:
   RA(J2000)  = 13h 06m 57.79s
   Dec(J2000) = +83d 47' 05.6"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 91 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 7.01e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 87 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
0.18. 

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


GRB_name: GRB201026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28785
SUBJECT: GRB 201026A: NOT optical upper limits
DATE:    20/10/27 00:31:29 GMT
FROM:    Daniele B Malesani at DTU Space  <malesani@space.dtu.dk>

L. Izzo (DARK/NBI), D. B. Malesani (DTU Space), T. Kuutma (NOT), report 
on behalf od a larger collaboration:

We observed the optical afterglow of GRB 201026A (Cenko et al., GCN 
28784) using the Nordic Optical Telescope (NOT) equipped with the ALFOSC 
imaging camera. A set of 2x300 s and 5x200 s images was secured in the 
SDSS r and z bands, respectively. The mid time of the observation was 
Oct 26.968 (36.2 min after the GRB). Observations were conducted at high 
airmass under moderate seeing conditions (1.4").

No new object is detected consistent with the XRT position, down to a 
limiting magnitude r= 21.5, z = 21.4 AB (3 sigma), calibrated against 
nearby stars from the Pan-STARRS catalog.

We note the presence of a faint, possibly extended object visible in the 
archival Pan-STARRS images, at a position consistent (RA = 13:06:58.71, 
Dec = +83:46:58.5) with that of the X-ray afterglow. This object could 
be the host galaxy of GRB 201026A, but we caution that the currently 
available uncertainty radius of the XRT position is still relatively 
large (3.9"), hence the association not robust.


GRB_name: GRB201026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28786
SUBJECT: GRB 201026A: NanShan/NEXT-0.6m optical upper limit
DATE:    20/10/27 01:11:02 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 201026A (Cenko et al., GCN 28784) using the 
NEXT-0.6m optical telescope located at Nanshan, Xinjiang, China. 
Observations automatically started at 22:49:35 UT on 2020-10-26, i.e., 
12 min after the BAT trigger. We obtained 3x40 s, 4x60 s and 12x90 s 
frames in the Sloan r-filter.

No new optical source is detected in our stacked image at the XRT 
position, down to a limiting magnitude of r = 20.5, calibrated with the 
nearby Pan-STARRS field.


GRB_name: GRB201027A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28788
SUBJECT: GRB 201027A: Swift detection of a burst
DATE:    20/10/27 01:24:01 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

S. B. Cenko (GSFC), S. D. Barthelmy (GSFC),
M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sbarrato (INAF-OAB)
and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels
Swift Observatory Team:

At 01:07:44 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201027A (trigger=1002158).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 155.974, -5.515 which is 
   RA(J2000) = 10h 23m 54s
   Dec(J2000) = -05d 30' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 20 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 01:09:07.5 UT, 83.4 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 155.9700,
-5.5101 which is equivalent to:
   RA(J2000)  = 10h 23m 52.81s
   Dec(J2000) = -05d 30' 36.2"
with an uncertainty of 2.3 arcseconds (radius, 90% containment). This
location is 22 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.67 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2.6
(+2.14/-1.93) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 86 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
0.04. 

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


GRB_name: GRB201020A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28789
SUBJECT: GRB 201020A: 1.3m DFOT, optical upper limits
DATE:    20/10/27 05:34:21 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

 Amit Kumar (ARIES), Rahul Gupta (ARIES), Ankur Ghosh (ARIES), Dimple
(ARIES), Kaushal Sharma (ARIES), Amar Aryan (ARIES), Shashi B. Pandey
(ARIES), and Kuntal Misra (ARIES) report:

We observed the field of GRB 201020A (E. Ambrosi et al., GCN 28696)
with the 1.3m Devasthal Fast Optical Telescope (DFOT)
at Devasthal observatory of Aryabhatta Research Institute of
observational sciencES (ARIES), India.

Multiple frames of the GRB field were obtained in the Bessel R and
I-bands (15*120sec in each filter).
Preliminary photometry on stacked images were performed and calibrated
against nearby USNO-B1 stars.
We do not detect any OT candidate (see Adachi et al. GCN 28697;
Lipunov et al. GCN 28700; Fu et al. GCN 28701;
Belkin et al. 28703; Pankov et al. GCN 28708; Kumar et al. GCN 28711;
Paek et al. 28713; Kann et al. 28717; Gokuldass et al. 28737; Siegel
et al. 28742 and Kumar et al. GCN 28747) within the enhanced XRT
position (Osborne et al., GCN 28698).

The 3-sigma upper limits at the location of the afterglow are as follows:

DATE       Start UT   Filter  Exposure(sec)    Lim_mag (3-sigma)
2020-10-24 12:51:08    I        15*120            >22.1
2020-10-24 13:23:45    R        15*120            >22.5

The estimated magnitudes have not been corrected for the Galactic
extinction in the direction of the GRB. This massage may be cited.


GRB_name: GRB201026A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28790
SUBJECT: GRB 201026A: FRAM-ORM optical detection limit
DATE:    20/10/27 08:33:15 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 GRB201026A (Cenko  et al
GCNC  28784), obtaining  a series  of 20  s unfiltered  images
starting at 22:50:58.9 UT, i.e. 13.4 min post trigger.

We  do not  detect  any  new source  within  or  near the  XRT
errorbox  neither in  single  images  (3-sigma limit  R>~17.1,
(Vega), calibrated  by the  Atlas catalog)  nor in  a combined
15x20s frame  (mean exp time  21.15 min post  trigger, 3-sigma
limit R>~18.5) similarly to Lipunov  et al. (GCNC 28783), Izzo
et al. (GCNC 28785) and Zhu et al. (GCNC 28786)


GRB_name: GRB201026A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28791
SUBJECT: GRB 201026A: Enhanced Swift-XRT position
DATE:    20/10/27 09:21:54 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 466 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 201026A, 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 = 196.74662, +83.78196 which is equivalent
to:

RA (J2000): 13h 06m 59.19s
Dec (J2000): +83d 46' 55.0"

with an uncertainty of 1.9 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB201027A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28792
SUBJECT: GRB 201027A: Enhanced Swift-XRT position
DATE:    20/10/27 11:11:55 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 1722 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 201027A, 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 = 155.96975, -5.51002 which is equivalent
to:

RA (J2000): 10h 23m 52.74s
Dec (J2000): -05d 30' 36.1"

with an uncertainty of 1.8 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: GRB201026A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28793
SUBJECT: GRB 201026A: Swift/UVOT Upper Limits
DATE:    20/10/27 14:17:32 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 201026A 88 s after the BAT trigger 
(Cenko et al., GCN Circ. 28784).
No optical afterglow consistent with the XRT position (Goad et al., GCN Circ. 28791) 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            88          238          147         >20.6
white               88          904          210         >20.9
u_FC               300          550          246         >20.1
v                  630          823           39         >18.3
b                  563          749           32         >19.2
u                  300          724          265         >20.2
w1                 680          873           39         >18.5
w2                4139         4518          197         >19.3

The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of 
E(B-V) = 0.18 in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB201027A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28794
SUBJECT: GRB 201027A: 1.5m OSN optical upper limit
DATE:    20/10/27 16:06:00 GMT
FROM:    Youdong HU at IAA-CSIC  <huyoudong072@hotmail.com>

Y.-D. Hu, F. J. Aceituno, A. J. Castro-Tirado, E. Fernandez-Garcia (IAA-CSIC) on behalf of a larger collaboration, report:

Following the detection of GRB201027A by Swift (Cenko et al. GCNC 28788), optical images in the I-band were obtained at the 1.5m OSN telescope in Granada (Spain) starting at 04:29 (Oct 27), i.e. ~3.4 h post burst. No optical afterglow is detected in the co-added image within the enhanced Swift/XRT error box (Osborne et al. GCNC 28792) down to I=21.9, which is consistent with the non-detection reported by Swift/UVOT (GCNC 28788).

We thank the staff at OSN for their excellent support.


GRB_name: GRB201026A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28796
SUBJECT: GRB 201026A: Swift-XRT refined Analysis
DATE:    20/10/27 22:56:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 3.2 ks of XRT data for GRB 201026A (Cenko et al. GCN
Circ. 28784), from 85 s to 46.3 ks after the  BAT trigger. The data
comprise 361 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. 28791).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.90 (+1.12, -0.13).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.82 (+/-0.03). The
best-fitting absorption column is  4.84 (+0.22, -0.21) x 10^21 cm^-2,
in excess of the Galactic value of 1.1 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 4.4 x 10^-11 (6.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:      4.84 (+0.22, -0.21) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 29.0 sigma
Photon index:      1.82 (+/-0.03)

If the light curve continues to decay with a power-law decay index of
0.90, the count rate at T+24 hours will be 5.6 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.5 x
10^-13 (3.6 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/01002103.

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


GRB_name: GRB201026A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28797
SUBJECT: GRB 201026A: Fermi GBM detection
DATE:    20/10/28 00:03:33 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 22:37:33.06 UT on 26 October 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 201026A (trigger 625444658 / 201026943), which
was initially misclassified as a distant particle event by the GBM
flight software. GRB 201026A was also detected by the Swift/BAT and the
Swift/XRT (Cenko et al. 2020, GCN 28784). The GBM on-ground location
is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 58
degrees.

The GBM light curve shows a main pulse with a duration (T90) of about
35 s (50-300 keV). There is also later emission extending to
approximately T0+280 s. We cannot conclusively confirm it is
related to the main emission episode with GBM data alone;
however, similar late-time emission can be seen in the
Swift-XRT lightcurve (Evans et al. 2020, GCN 28796).

The time-averaged spectrum of the main pulse from T0-16 s to T0+23 s
is best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.83 +/- 0.10 and
the cutoff energy, parameterized as Epeak, is 68 +/- 3 keV.
A Band function fits the spectrum equally well with
Epeak = 63 +/- 5 keV, alpha = -0.73 +/- 0.14 and beta = -2.84 +/- 0.34.

The event fluence (10-1000 keV) in this time interval is
(3.96 +/- 0.14)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.47 s in the 10-1000 keV band
is 3.04 +/- 0.22 ph/s/cm^2.

For the later emission episode, the time-averaged spectrum
from T0+188 s to T0+237 s is best fit by
a simple power law function with index -1.84 +/- 0.04.
The event fluence (10-1000 keV) in this time interval is
(4.51 +/- 0.29)E-06 erg/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: GRB201027A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28798
SUBJECT: GRB 201027A: Swift-XRT refined Analysis
DATE:    20/10/28 01:24:03 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), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), D.N.
Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester)
and S.B. Cenko report on behalf of the Swift-XRT team:

We have analysed 4.2 ks of XRT data for GRB 201027A (Cenko et al. GCN
Circ. 28788), from 93 s to 52.6 ks after the  BAT trigger. The data are
entirely in Photon Counting (PC) mode. The enhanced XRT position for
this burst was given by Osborne et al. (GCN Circ. 28792).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.54 (+0.15, -0.21), followed by a break at T+1066 s to
an alpha of 1.36 (+0.38, -0.21).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.23, -0.21). The
best-fitting absorption column is  1.3 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 4.7 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.8 x 10^-11 (4.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 4.7 x 10^20 cm^-2
Excess significance: 2.2 sigma
Photon index:      1.81 (+0.23, -0.21)

If the light curve continues to decay with a power-law decay index of
1.36, the count rate at T+24 hours will be 1.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.9 x
10^-14 (4.7 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/01002158.

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


GRB_name: GRB201027A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28799
SUBJECT: GRB 201027A: Swift/UVOT Upper Limits
DATE:    20/10/28 14:19:28 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 201027A 87 s after the BAT trigger 
(Cenko et al., GCN Circ. 28788). No optical afterglow consistent with the XRT position (Cenko et al. 
GCN Circ. 28788) 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            87          236          147         >20.2
u_FC               299          548          246         >19.5
white               87         1721          411         >21.2
v                  629         1771          136         >18.3
b                  554         1696          117         >19.3
u                  299         1671          343         >20.1
w1                 678         1818          135         >19.1
m2                 653         1795           78         >20.4
w2                 604         1574          117         >20.2

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: GRB201026A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28800
SUBJECT: GRB 201026A: Swift-BAT refined analysis
DATE:    20/10/29 01:11:22 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

GRB 201026A: Swift-BAT refined analysis

S. D. Barthelmy (GSFC), S. B. Cenko (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-60 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 201026A (trigger #1002103)
(S. B. Cenko et al., GCN Circ. 28784).  The BAT ground-calculated position is
RA, Dec = 196.696, 83.807 deg which is
   RA(J2000)  =  13h 06m 47.0s
   Dec(J2000) = +83d 48' 24.3"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.

The BAT light curve showed a complex structure. There are two prominent peaks, at
~ T+0 sec and T+210 sec with a duration of about 50 sec and 60 sec respectively.
There is a small peak at T+140 to T+170 sec, and possibly a precursor at
T-60 to T-40 sec.
T90 (15-350 keV) is 135.38 +- 120.84 sec (estimated error including systematics).

The time-averaged spectrum from T-13 to T+146 sec and T+165 to T+230 sec is best fit by
a simple power-law model.  The power law index of the time-averaged spectrum is
1.94 +- 0.09.  The fluence in the 15-150 keV band is 5.6 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+1.05 sec in the 15-150 keV band
is 2.2 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1002103/BA/


GRB_name: GRB201027A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28801
SUBJECT: GRB 201027A: Swift-BAT refined analysis
DATE:    20/10/29 01:23:20 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
S. B. Cenko (GSFC), J. R. Cummings (CPI),
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 201027A (trigger #1002158)
(S. B. Cenko, et al., GCN Circ. 28788).  The BAT ground-calculated position is
RA, Dec = 155.954, -5.499 deg which is
   RA(J2000)  =  10h 23m 49.0s
   Dec(J2000) = -05d 29' 56.8"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 44%.

The BAT light curve showed a complex structure with a duration of about 20 sec.
T90 (15-350 keV) is 546.73 +- 420.95 sec (estimated error including systematics).

The time-averaged spectrum from T-3.86 to T+960 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.50 +- 0.00.  The fluence in the 15-150 keV band is 0.0 +- 0.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.29 sec in the 15-150 keV band
is 1.4 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1002158/BA/


GRB_name: GRB201027A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28802
SUBJECT: GRB 201027A: MITSuME Akeno optical upper limits
DATE:    20/10/29 01:29:33 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

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

We observed the field of GRB 201027A (V. Lipunov et al., GCN #28787,
S. B. Cenko et al., GCN #28788, Y.-D. Hu et al., GCN #28794 ) 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 with a series of 60 sec exposures started at 2020-10-27
18:43:12 UT(17.2 hour after trigger). Since the first 18 images were
taken under high airmass conditions, we stacked the images with good
conditions. We did not find any new point sources within the enhanced
Swift/XRT circle (J.P. Osborne et al., GCN #28792) in all three bands.
We obtained the 5-sigma limits of the stacked images as follows.
T0+[hour] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
17.6 19:19:32 3180 g'>19.5,Rc>20.0,Ic>19.1
------------------------------------------------------------------------------------------------
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.,
https://doi.org/10.1093/pasj/psaa091,
https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire).


GRB_name: GRB201029A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28803
SUBJECT: GRB 201029A: Swift detection of a burst
DATE:    20/10/29 20:29:51 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Dichiara (NASA/GSFC/UMCP), J. A. Kennea (PSU),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
F. E. Marshall (NASA/GSFC), M. J. Moss (GWU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
A. Tohuvavohu (U Toronto) and E. Troja (NASA/GSFC/UMCP) report on
behalf of the Neil Gehrels Swift Observatory Team:

At 20:19:50 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201029A (trigger=1003002).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 229.601, +44.464 which is 
   RA(J2000) = 15h 18m 24s
   Dec(J2000) = +44d 27' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single complex peak
structure with a duration of about 40 sec.  The peak count rate
was ~1800 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 20:21:52.3 UT, 122.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 229.58280, 44.45975 which
is equivalent to:
   RA(J2000)  = 15h 18m 19.87s
   Dec(J2000) = +44d 27' 35.1"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 49 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 7.42e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 131 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 S. Dichiara (dichiara AT umd.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB201029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28805
SUBJECT: GRB 201029A: FRAM-ORM optical limit
DATE:    20/10/29 21:17:54 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek, 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   Swift  alert   of  GRB201029A
(trigger=1003002; Dichiara  et al.,  GCNC 28803),  obtaining a
series of 20s unfiltered images starting at 20:21:23.0UT, i.e.
93s post trigger.

We do not  detect any new source in the  XRT error box neither
in single  images (3-sigma  limit R>~15.7)  nor in  a combined
20x20s frame (mean  exp time 276s post  trigger, 3-sigma limit
R>~18.15) similarly to Lipunov et al. (GCNC 28804).


GRB_name: GRB201029A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28806
SUBJECT: GRB 201029A: Enhanced Swift-XRT position
DATE:    20/10/29 22:07:05 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 764 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 201029A, 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 = 229.58157, +44.45927 which is equivalent
to:

RA (J2000): 15h 18m 19.58s
Dec (J2000): +44d 27' 33.4"

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: GRB201029A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28807
SUBJECT: GRB 201029A: BOOTES-1 optical upper limit
DATE:    20/10/30 07:09:24 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 201029A (Dichiara et al., GCNC 28803), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), southern Spain, automatically responded to this burst at 8 degrees above the horizon. Series images were taken started 20:21:26UT (~96 s after trigger). In the co-added of following images, no source is detected within the enhanced XRT position (Beardmore et al., GCNC 28806) which down to 17.7 mag (clear filter), which consistent with the non-detections reported by UVOT (Dichiara et al., GCNC 2828803) and FRAM-ORM (Jelinek et al., GCNC 28805).

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


GRB_name: GRB201029A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28808
SUBJECT: GRB 201029A: Swift-XRT refined Analysis
DATE:    20/10/30 10:11:05 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), B. Sbarufatti
(PSU), D.N. Burrows (PSU), J. D. Gropp (PSU), K.L. Page (U. Leicester),
A.P. Beardmore (U. Leicester) and S. Dichiara (NASA/GSFC/UMCP) reporton
behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 201029A (Dichiara et al.
GCN Circ. 28803), from 128 s to 34.7 ks after the  BAT trigger. The
data comprise 764 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN Circ. 28806).

The light curve is dominated by flares. The first flare covers
~T0+200-650 s. The second flare started at T0+1100s and was still
ongoing when the GRB entered Earth eclipse at T0+1850 s. The third
flare began at T0+11.5 ks, was still ongoing at T0+23 ks and finished
at some point before T0+30.5 ks, although large observing gaps in this
window prevent acccurate measurements of the flare and it is possible
that there are multiple flares at this time rather than a single
long-lived flare. This behaviour, of multiple flares dominating the XRT
light curve for tens of kiloseconds, is reminiscent of GRBs 050904,
121027A and 130925A (see
https://www.swift.ac.uk/xrt_curves/allcurves.php for a mugshot gallery
of all XRT GRB afterglows).

This flaring activity makes it difficult to model the underlying
behaviour. Excluding all of the above times, the light curve can be
modelled with a power-law decay with a decay index of alpha=0.79
(+0.05, -0.06). These formal errors are likely underestimates, since
they depend on how accurate the estimates of flare times are, which are
themselves subject to proper modelling of the underlying emission.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index  of 1.65 (+/-0.05). The
best-fitting absorption column is  4.9 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 2.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.97 (+/-0.12) and a
best-fitting absorption column of 2.9 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.7 x 10^-11 (5.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.9 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 2.1 x 10^20 cm^-2
Excess significance: 9.6 sigma
Photon index:      1.97 (+/-0.12)

If the light curve continues to decay with a power-law decay index of
0.79, the count rate at T+24 hours will be 0.024 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.2 x
10^-13 (1.3 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team
automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01003002.

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


GRB_name: GRB201029A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28809
SUBJECT: GRB 201029A: Fermi GBM detection
DATE:    20/10/30 14:40:58 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 20:19:51.61 UT on 29 October 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 201029A (trigger 625695596 / 201029847)
which was also detected by the Swift/BAT (Dichiara et al., GCN 28803).
The GBM on-ground location is consistent with the Swift position.

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

The GBM light curve consists of a broad peak
with a duration (T90) of about 78 s (50-300 keV).
The time-averaged spectrum from T0-8.2 s to T0+34.8 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.03 +/- 0.10 and
the cutoff energy, parameterized as Epeak, is 647 +/- 230 keV.

The event fluence (10-1000 keV) in this time interval is
(1.59 +/- 0.14)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+1.4 s in the 10-1000 keV band
is 1.4 +/- 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: GRB201029A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28810
SUBJECT: GRB 201029A: Swift/UVOT Upper Limits
DATE:    20/10/30 17:25:08 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) and S. Dichiara (NASA/GSFC/UMCP)

report on behalf of the Swift/UVOT team:



The Swift/UVOT began settled observations of the field of GRB 201029A

131 s after the BAT trigger (Dichiara et al., GCN Circ. 28803).

No optical afterglow consistent with the XRT position

(Beardmore et al. GCN Circ. 28806)

is detected in the initial UVOT exposures.

Preliminary 3-sigma upper limits using the UVOT photometric system

(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first

finding chart (FC) exposure and subsequent exposures are:



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



white_FC           131          281          147         >20.6

u_FC               289          539          246         >19.9

white              131         1708          412         >21.4

v                  619         1759          127         >19.2

b                  545         1858          136         >19.9

u                  289         1833          362         >20.0

w1                 842         1808           97         >19.5



The magnitudes in the table are not corrected for the Galactic extinction

due to the reddening of E(B-V) = 0.02 in the direction of the burst

(Schlegel et al. 1998).


GRB_name: GRB201029A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28811
SUBJECT: Swift GRB 201029A: Global MASTER-Net observations report 
DATE:    20/10/30 20:21:58 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),

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 201029A ( S. Dichiara et al., GCN 28803) errorbox 103 sec after trigger time at 2020-10-29 20:23:35 UT, with upper limit up to  17.3 mag. The observations began at zenith distance = 77 deg. The sun  altitude  is -27.6 deg. 

The galactic latitude b = 56 deg., longitude l = 73 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1471870

We obtain a following upper limits.  

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

     113 |          MASTER-IAC |   C |    20 | 15.9 |        
     148 |          MASTER-IAC |   C |    90 | 16.6 |  Coadd 
     338 |          MASTER-IAC |   C |   470 | 17.3 |  Coadd 
     146 |          MASTER-IAC |   C |    30 | 16.0 |        
     197 |          MASTER-IAC |   C |    40 | 16.0 |        
     253 |          MASTER-IAC |   C |    50 | 16.3 |        
     343 |          MASTER-IAC |   C |   230 | 17.0 |  Coadd 
     322 |          MASTER-IAC |   C |    60 | 16.4 |        
     672 |          MASTER-IAC |   C |   120 | 16.5 |        
     817 |          MASTER-IAC |   C |   150 | 16.6 |        
     997 |          MASTER-IAC |   C |   510 | 16.6 |  Coadd 
     993 |          MASTER-IAC |   C |   180 | 16.4 |        
    1193 |          MASTER-IAC |   C |   180 | 16.4 |        
    1392 |          MASTER-IAC |   C |   180 | 16.1 |        
    1572 |          MASTER-IAC |   C |   540 | 16.6 |  Coadd 
    1591 |          MASTER-IAC |   C |   180 | 16.0 |        
    1791 |          MASTER-IAC |   C |   180 | 15.9 |        
    1991 |          MASTER-IAC |   C |   180 | 15.7 |        
    2601 |          MASTER-IAC |   C |   180 | 15.3 |        
   83049 |          MASTER-IAC |   C |    60 | 16.8 |        
   84836 |          MASTER-IAC |   C |    60 | 16.5 |        
   85552 |          MASTER-IAC |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201029A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28813
SUBJECT: GRB 201029A: Swift-BAT refined analysis
DATE:    20/10/30 20:48:43 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), S. Dichiara (NASA/GSFC/UMCP),
H. A. Krimm (NSF), 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-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 201029A (trigger #1003002)
(S. Dichiara et al., GCN Circ. 28803).  The BAT ground-calculated position is
RA, Dec = 229.607, 44.473 deg which is
   RA(J2000)  =  15h 18m 25.7s
   Dec(J2000) = +44d 28' 21.7"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The BAT light curve showed a complex structure with a duration of about 150 sec.
T90 (15-350 keV) is 120.55 +- 9.54 sec (estimated error including systematics).

The time-averaged spectrum from T-2.19 to T+133.11 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.09 +- 0.11.  The fluence in the 15-150 keV band is 2.2 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+7.06 sec in the 15-150 keV band
is 0.6 +- 0.1 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/1003002/BA/


GRB_name: GRB201031A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28814
SUBJECT: GRB 201031A: Swift detection of a burst
DATE:    20/10/31 14:33:07 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

S. Laha (GSFC/UMBC/CRESST), N. P. M. Kuin (UCL-MSSL),
K. L. Page (U Leicester) and B. Sbarufatti (PSU) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 14:19:55 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201031A (trigger=1003313).  Swift did not slew immediately 
to the burst due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 254.277, -9.140 which is 
   RA(J2000) = 16h 57m 06s
   Dec(J2000) = -09d 08' 23"
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 80 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 09:11 UT on 2021 January 19. There will thus be no XRT
or UVOT data for this trigger before this time. 

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


GRB_name: GRB201031B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28815
SUBJECT: GRB 201031B: Fermi GBM Final Real-time Localization
DATE:    20/10/31 18:01:39 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 17:51:24 UT on 31 Oct 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201031B (trigger 625859489.53606 / 201031744).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 44.2, Dec = 54.9 (J2000 degrees, equivalent to J2000 02h 56m, 54d 53'), with a statistical uncertainty of 4.0 degrees.

The angle from the Fermi LAT boresight is 16.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201031744/quicklook/glg_skymap_all_bn201031744.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/bn201031744/quicklook/glg_healpix_all_bn201031744.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201031744/quicklook/glg_lc_medres34_bn201031744.gif


GRB_name: GRB201031B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28816
SUBJECT: GRB 201031B: BALROG localization (Fermi Trigger 625859489 / GRB 201031744)
DATE:    20/10/31 18:25:47 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
625859489 at 17:51:24 on 31 Oct. 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) = 47.9+/-6.1 deg
Decl.(2000.0) = 42.0+/-6.2 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201031744/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201031744/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201031744/json

                        


GRB_name: GRB201031B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28817
SUBJECT: Fermi GRB 201031B: Global MASTER-Net observations report 
DATE:    20/10/31 21:30:36 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),

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 201031B ( Fermi GBM team, GCN 28815) errorbox  9553 sec after notice time and 9640 sec after trigger time at 2020-10-31 20:32:04 UT, with upper limit up to  16.8 mag. The observations began at zenith distance = 53 deg. The sun  altitude  is -29.8 deg. 

The galactic latitude b = -3 deg., longitude l = 141 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1473043

We obtain a following upper limits.  

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

    9670 | 2020-10-31 20:32:04 |          MASTER-IAC | (02h 28m 29.48s , +51d 55m 57.7s) |   C |    60 | 16.8 |        
    9750 | 2020-10-31 20:33:24 |          MASTER-IAC | (02h 41m 30.02s , +51d 57m 11.9s) |   C |    60 | 16.7 |        
   10166 | 2020-10-31 20:40:20 |          MASTER-IAC | (02h 54m 30.92s , +51d 55m 46.5s) |   C |    60 | 16.7 |        
   10257 | 2020-10-31 20:41:51 |          MASTER-IAC | (03h 05m 47.75s , +51d 56m 15.9s) |   C |    60 | 16.7 |        
   10509 | 2020-10-31 20:46:03 |          MASTER-IAC | (02h 41m 34.50s , +51d 56m 15.3s) |   C |    60 | 16.7 |        
   10777 | 2020-10-31 20:50:31 |          MASTER-IAC | (03h 05m 43.26s , +51d 56m 35.1s) |   C |    60 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201031A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28818
SUBJECT: Swift Trigger 1003313 (a.k.a. GRB 201031A) is not an astrophysical event
DATE:    20/10/31 23:36:27 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
S. Laha (GSFC/UMBC/CRESST), A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

Further analysis of Swift trigger 1003313 (previously reported
as GRB 201031A; Laha et al., CGN Circ. 28814) using
the data set from T-60 to T+243 sec shows that
the BAT image significance has now decreased to 2.6 sigma
(15-350 keV). Also, the mask-weighted light curve does not
show anything significant.

We thus conclude that this event is due to noise,
and is not an astrophysical event.


GRB_name: GRB201031A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28819
SUBJECT: Swift GRB 201031A: Global MASTER-Net observations report 
DATE:    20/11/01 00:18:23 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),

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) was pointed to the Swift GRB 201031A ( S. Laha et al., GCN 28814) errorbox  34924 sec after notice time and 35035 sec after trigger time at 2020-11-01 00:03:50 UT, with upper limit up to  16.6 mag. Observations started at twilight.  The observations began at zenith distance = 76 deg. The sun  altitude  is -13.9 deg. 

The galactic latitude b = 20 deg., longitude l = 11 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1472957

We obtain a following upper limits.  

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

   35125 |         MASTER-OAFA |   C |   180 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201103A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28820
SUBJECT: GRB 201103A: Fermi GBM Final Real-time Localization
DATE:    20/11/03 06:20:38 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:13:09 UT on 3 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201103A (trigger 626076794.808782 / 201103259).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 248.9, Dec = 71.0 (J2000 degrees, equivalent to J2000 16h 35m, 71d 00'), with a statistical uncertainty of 15.9 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/bn201103259/quicklook/glg_skymap_all_bn201103259.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/bn201103259/quicklook/glg_healpix_all_bn201103259.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201103259/quicklook/glg_lc_medres34_bn201103259.gif


GRB_name: GRB201103A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28821
SUBJECT: Fermi GRB 201103A: Global MASTER-Net observations report 
DATE:    20/11/03 06:30:15 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),

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 201103A ( Fermi GBM team, GCN 28820) errorbox  284 sec after notice time and 343 sec after trigger time at 2020-11-03 06:18:53 UT, with upper limit up to  16.7 mag. Observations started at twilight.  The observations began at zenith distance = 73 deg. The sun  altitude  is -13.0 deg. 

The galactic latitude b = 36 deg., longitude l = 103 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1474580

We obtain a following upper limits.  

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

     374 | 2020-11-03 06:18:53 |          MASTER-IAC | (16h 09m 29.35s , +70d 02m 37.3s) |   C |    60 | 16.6 |        
     453 | 2020-11-03 06:20:13 |          MASTER-IAC | (15h 22m 24.94s , +70d 04m 21.2s) |   C |    60 | 16.7 |        
     533 | 2020-11-03 06:21:32 |          MASTER-IAC | (16h 12m 13.39s , +66d 00m 40.5s) |   C |    60 | 16.5 |        
     612 | 2020-11-03 06:22:52 |          MASTER-IAC | (15h 27m 31.40s , +68d 03m 55.2s) |   C |    60 | 16.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201015A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28822
SUBJECT: GRB 201015A: Late X-ray Detections with Chandra
DATE:    20/11/03 16:45:05 GMT
FROM:    Ben Gompertz at U of Warwick  <b.gompertz@warwick.ac.uk>

B. Gompertz (1); A. Levan (2); N. Tanvir (3); A. Fruchter (4); A. 
Cucchiara (5); J. Greiner (6); J. Hjorth (7); T. Kangas (4); G. Lamb 
(3); J. Lyman (1); S. Oates (8); P. O'Brien (3); J. Osborne (3); K. Page 
(3); D. Perley (9); E. Pian (10); D. Steeghs (1); K. Wiersema (1); G. 
Wynn (3)

((1) University of Warwick, (2) Radboud University, (3) University of 
Leicester, (4) Space Telescope Science Institute, (5) University of the 
Virgin Islands, (6) MPE Garching, (7) University of Copenhagen, (8) 
University of Birmingham, (9) Liverpool John Moores University, (10) 
INAF-OAS)
report:

We observed the position of GRB 201015A (D'Elia et al., GCN 28632) with 
the Chandra X-ray Observatory with epochs 8.4 and 13.6 days after 
trigger. The X-ray afterglow is clearly detected with a flux around 100x 
brighter than expected based on the extrapolation of the early XRT data 
taken between 0.03 and 0.8 days after burst. The source is seen to fade 
between the two Chandra epochs with a power-law index of approximately 
-0.8. A Swift ToO has been approved.


GRB_name: GRB201104A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28823
SUBJECT: GRB 201104A: Fermi GBM Final Real-time Localization
DATE:    20/11/04 00:11:18 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 00:00:56 UT on 4 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201104A (trigger 626140861.749996 / 201104001).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 60.4, Dec = -72.7 (J2000 degrees, equivalent to J2000 04h 01m, -72d 42'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 65.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104001/quicklook/glg_skymap_all_bn201104001.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/bn201104001/quicklook/glg_healpix_all_bn201104001.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104001/quicklook/glg_lc_medres34_bn201104001.gif


GRB_name: GRB201104A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28824
SUBJECT: Fermi GRB 201104A: Global MASTER-Net observations report 
DATE:    20/11/04 00:15:27 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),

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 201104A ( Fermi GBM team, GCN 28823) errorbox 80 sec after trigger time at 2020-11-04 00:02:17 UT, with upper limit up to  17.8 mag. Observations started at twilight.  The observations began at zenith distance = 59 deg. The sun  altitude  is -13.0 deg. 

The galactic latitude b = -38 deg., longitude l = 287 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1475503

We obtain a following upper limits.  

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

      90 | 2020-11-04 00:02:17 |         MASTER-OAFA | (03h 58m 14.15s , -74d 30m 15.1s) |   C |    20 | 17.4 |        
     130 | 2020-11-04 00:02:56 |         MASTER-OAFA | (03h 58m 07.55s , -74d 31m 15.8s) |   C |    20 | 17.3 |        
     174 | 2020-11-04 00:03:35 |         MASTER-OAFA | (03h 58m 15.37s , -74d 30m 56.0s) |   C |    30 | 17.4 |        
     228 | 2020-11-04 00:04:25 |         MASTER-OAFA | (03h 58m 11.98s , -74d 29m 19.8s) |   C |    40 | 17.6 |        
     293 | 2020-11-04 00:05:24 |         MASTER-OAFA | (03h 58m 12.40s , -74d 30m 55.2s) |   C |    50 | 17.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201104B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28825
SUBJECT: GRB 201104B: Swift detection of a burst
DATE:    20/11/04 18:10:07 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

B. Sbarufatti (PSU), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester)
and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels
Swift Observatory Team:

At 17:33:46 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201104B (trigger=1004168).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 5.217, 7.820 which is 
   RA(J2000) = 00h 20m 52s
   Dec(J2000) = 07d 49' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty). Due to GCN downtime, no BAT light curves are
available at this moment. 

The XRT began observing the field at 17:35:28.2 UT, 102 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec = 5.21528, 7.84257 which is equivalent to:
   RA(J2000)  = 00h 20m 51.7s
   Dec(J2000) = +07d 50' 33.3"
with an uncertainty of 5 arcseconds (radius, 90% containment). This
location is 81.5 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. 

Due to GCN downtime, no UVOT data are available at this time. 

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


GRB_name: GRB201104B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28826
SUBJECT: GRB 201104B: MASTER optical observation
DATE:    20/11/04 19:56:02 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E.Gorbovskoy, N.Tiurina, P.Balanutsa,A.Kuznetsov,K.Zhirkov, F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, A.Chasovnikov,A.Pozdnyakov,
V.Topolev, D.Cheryasov(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley (South African Astronomical Observatory),
O.A. Gres, N.M. Budnev (Irkutsk State University, API),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov, Yu. Sergienko (Blagoveschensk Educational State University)

MASTER-SAAO started GRB 201104B (Sbarufatti  et al. GCN 28825, Ttrig=2020-11-04 17:33:46) observation by
MASTER-II (2x4sq.deg.) in 2020-11-04  19:14:43UT (unfiltered, manual pointing) 
and by
MASTER very wide field cameras (Lipunov et al. 2010, Advances in Astronomy,vol.2010, 30L),
started at 48deg. altitude in clouds (the sun altitude was -25deg)

There is no OT at Swift-XRT position with mlim=16.1 
Observation and reduction will continue.


GRB_name: GRB201104B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28827
SUBJECT: GRB 201104B: Swift/UVOT Detection
DATE:    20/11/04 20:16:09 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC), S. R. Oates (U.Warwick) and B. Sbarufatti (PSU)

report on behalf of the Swift/UVOT team:



The Swift/UVOT began settled observations of the field of GRB 201104B

56 s after the BAT trigger (Sbarufatti et al., GCN Circ. 28825).

A source consistent with the XRT position

(Sbarufatti et al. GCN Circ. 28825)

is detected in the initial UVOT exposures.



The preliminary UVOT position is:

    RA  (J2000) =  00:20:51.65 =   5.21520 (deg.)

    Dec (J2000) = +07:50:29.4  =   7.84150 (deg.)

with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).



Preliminary detections using the UVOT photometric system

(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:



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



white               56          206          147         18.63 +/- 0.06

u                  268          459          188         19.45 +/- 0.23



The magnitudes in the table are not corrected for the Galactic extinction

due to the reddening of E(B-V) = 0.045 in the direction of the burst

(Schlegel et al. 1998).


GRB_name: GRB201104A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28828
SUBJECT: GRB 201104A: Fermi-LAT detection
DATE:    20/11/04 20:30:07 GMT
FROM:    Masanori Ohno at Hiroshima University  <ohno@astro.hiroshima-u.ac.jp>

M. Ohno (Hiroshima U./Eotvos U.), N. Omodei (Stanford University), F. Longo
(University & INFN Trieste) and M. Axelsson (KTH & Stockholm Univ.)
report on behalf of the Fermi-LAT Collaboration:

On November 4, 2020, Fermi-LAT detected high-energy emission from
GRB 201104A, which was also detected by Fermi-GBM (trigger
626140861/201104001) (Fermi-GBM team; GCN Circ. 28823).

The best LAT on-ground location is found to be

RA, Dec = 81.4, -71.1 (degrees, J2000)

with an error radius of 0.24 deg (90% containment, statistical error only).
This was 6.7 deg from the LAT boresight at the time of the GBM trigger:
T0 =  00:00:56 UT.

The source quickly went out from the LAT FoV but the data from the
Fermi-LAT show a significant increase
in the event rate after the GBM trigger that is spatially and temporally
correlated with the
GBM emission with high significance.
The photon flux above 100 MeV in the time interval 0-100 s after the
GBM trigger is (2.6+/-0.4)e-4 ph/cm2/s.

The estimated photon index above 100 MeV is -2.5 +/-  0.2.

The highest-energy photon is a 3.7 GeV event which is observed  16 seconds
after the GBM trigger.

A Swift ToO has been requested 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.

[GCN OPS NOTE(06Nov20): Due to the uncertainty of the arrival time with respect
to the downtime window (15 hours) of the GCN Circulars processing system, 
the error in the date-time in the header of this Circular can be off anywhere from 0-15 hours.]


GRB_name: GRB201104A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28829
SUBJECT: GRB 201104A: AGILE/MCAL detection
DATE:    20/11/04 20:46:45 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE Mini-CALorimeter (MCAL) detected GRB 201104A at T0 = 2020-11-04
00:00:56.77 +/- 0.01 s (UTC), reported by Fermi/GBM (GCN #28823) and
INTEGRAL/SPI-ACS (trigger ID 8789,0).

The event lasted about 8 s and released a total number of ~7200 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 640 Hz.

The light curve shows sveral episodes and can be found at
http://www.agilescienceapp.it/notices/GRB_070287_531532856.770000.png .

The time-integrated spectrum of the burst can be fitted in the energy range
0.4-20 MeV with a single power-law with ph.ind. = -2.26 -0.15/+0.18,
resulting in a reduced chi-squared of 1.06 (75 d.o.f.) and a fluence of
3.57e-06 ergs/cm^2 (90% confidence level), in the same energy range.

The burst is clearly visible in the AGILE scientific ratemeters of the MCAL
detector. The event released a total number of 25100 counts, above a
background rate of 1255 Hz. The AGILE ratemeter light curves can be found
at http://www.agilescienceapp.it/notices/GRB_201104A_AGILE_RM.png .

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

[GCN OPS NOTE(06Nov20): Due to the uncertainty of the arrival time with respect 
to the downtime window (15 hours) of the GCN Circulars processing system, 
the error in the date-time in the header of this Circular can be off anywhere from 0-15 hours.]


GRB_name: GRB201104A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28830
SUBJECT: GRB 201104A: Fermi GBM observation
DATE:    20/11/04 20:51:58 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

E. Bissaldi (Politecnico and INFN Bari) and C. Malacaria (NASA-MSFC/USRA)
report on behalf of the Fermi GBM Team:

"At 00:00:56.75 UT on 4 November 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 201104A (trigger 626140861 / 201104001,
which was also detected by the Fermi-LAT (Ohno et al. 2020, GCN 28828) 
and AGILE (Ursi et al. 2020, GCN 28829).
The GBM on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger time is 57 degrees.

The GBM light curve shows a bright emission episode
with a duration (T90) of about 8.4 s (50-300 keV).
The time-averaged spectrum from T0 to T0+9 s is
best fit by a Band function with Epeak = 1140 +/- 130 keV,
alpha = -0.76 +/- 0.04, and beta = -2.24 +/- 0.17.

The event fluence (10-1000 keV) in this time interval is
(1.55 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0 in the 10-1000 keV band
is 12.1 +/- 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: GRB201103B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28831
SUBJECT: GRB 201103B: AGILE detection
DATE:    20/11/04 21:05:06 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected a burst at T0 = 2020-11-03 18:06:45.36 +/-
0.01 s (UTC), reported by INTEGRAL/SPI-ACS (trigger ID 8788,0).

The burst is clearly visible in the AGILE scientific ratemeters of the
SuperAGILE (SA; 20-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and
AntiCoincidence (AC; 50-200 keV) detectors. The event lasted ~7 s and
released a total number of 1850 counts in the SA detector (above a
background rate of 90 Hz), 25200 counts in the MCAL detector (above a
background rate of 1260 Hz), and 73000 counts in the AC detector (above a
background rate of 3650 Hz). The AGILE ratemeter light curves can be found
at http://www.agilescienceapp.it/notices/GRB_201103B_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition.

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.

[GCN OPS NOTE(06Nov20): Due to the uncertainty of the arrival time with respect 
to the downtime window (15 hours) of the GCN Circulars processing system, 
the error in the date-time in the header of this Circular can be off anywhere from 0-15 hours.]


GRB_name: GRB201104A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28832
SUBJECT: GRB 201104A: Tiled Swift observations
DATE:    20/11/04 21:22:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 201104A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00094

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

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

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

[GCN OPS NOTE(06Nov20): Due to the uncertainty of the arrival time with respect 
to the downtime window (15 hours) of the GCN Circulars processing system, 
the error in the date-time in the header of this Circular can be off anywhere from 0-15 hours.]


GRB_name: GRB201104C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28833
SUBJECT: GRB 201104C: Fermi GBM Final Real-time Localization
DATE:    20/11/04 21:35:03 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 19:23:25 UT on 4 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201104C (trigger 626210610.205754 / 201104808).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 240.3, Dec = -36.7 (J2000 degrees, equivalent to J2000 16h 01m, -36d 42'), with a statistical uncertainty of 7.7 degrees.

The angle from the Fermi LAT boresight is 90.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104808/quicklook/glg_skymap_all_bn201104808.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/bn201104808/quicklook/glg_healpix_all_bn201104808.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201104808/quicklook/glg_lc_medres34_bn201104808.gif

[GCN OPS NOTE(06Nov20): Due to the uncertainty of the arrival time with respect 
to the downtime window (15 hours) of the GCN Circulars processing system, 
the error in the date-time in the header of this Circular can be off anywhere from 0-15 hours.]


GRB_name: GRB201104A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28834
SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001)
DATE:    20/11/04 22:35:07 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
626140861 at 00:00:56 on 04 Nov. 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) = 67.9+/-10.4 deg
Decl.(2000.0) = -73.2+/-1.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201104001/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201104001/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201104001/json

                        


GRB_name: GRB201104A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28835
SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001)
DATE:    20/11/04 22:35:09 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
626140861 at 00:00:56 on 04 Nov. 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) = 67.9+/-10.4 deg
Decl.(2000.0) = -73.2+/-1.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201104001/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201104001/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201104001/json

                        


GRB_name: GRB201104A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28836
SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001)
DATE:    20/11/04 22:37:25 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
626140861 at 00:00:56 on 04 Nov. 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) = 67.9+/-10.4 deg
Decl.(2000.0) = -73.2+/-1.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201104001/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201104001/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201104001/json

                        


GRB_name: GRB201104A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28837
SUBJECT: GRB 201104A: BALROG localization (Fermi Trigger 626140861 / GRB 201104001)
DATE:    20/11/05 01:40:31 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
626140861 at 00:00:56 on 04 Nov. 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) = 67.9+/-10.4 deg
Decl.(2000.0) = -73.2+/-1.6 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201104001/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201104001/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201104001/json


[GCN OPS NOTE(04Nov20): This circular (28837) is a retransmission
of the circular being submitted 3 times and having delayed deliveries
due to GCN being down.  The original time of submission for this circular
was 22:35 UT 20/11/04.]


GRB_name: GRB201104B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28839
SUBJECT: GRB 201104B: Swift-BAT refined analysis
DATE:    20/11/05 02:50:15 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),
D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (PSU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-240 to T+302 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 201104B (trigger #1004168)
(Sbarufatti et al., GCN Circ. 28825).  The BAT ground-calculated position is
RA, Dec = 5.215, 7.834 deg which is
   RA(J2000)  =  00h 20m 51.5s
   Dec(J2000) = +07d 50' 03.6"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 53%.

The mask-weighted light curve shows several overlapping pulses that
start at ~T-9 s and end at ~T+1 s. The main peak occurs at ~T-8 s.
T90 (15-350 keV) is 8.66 +- 0.16 sec (estimated error including
systematics).

The time-averaged spectrum from T-8.86 to T+0.88 sec is best fit
by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.47 +- 0.07.  The fluence in the 15-150 keV band
is 1.8 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from
T-8.52 sec in the 15-150 keV band is 4.1 +- 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/1004168/BA/


GRB_name: GRB201104B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28840
SUBJECT: GRB 201104B: VLT/X-shooter redshift
DATE:    20/11/05 03:03:00 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

J.-B. Vielfaure (GEPI, Paris Observatory), D. B. Malesani (DTU Space), 
D. A. Kann (HETH/IAA-CSIC), B. Sbarufatti (PSU), N. R. Tanvir (Univ. 
Leicester), and D. H. Hartmann (Clemson University) report on behalf of 
the Stargate Consortium:

We observed the optical afterglow (Marshall et al., GCN 28827) of GRB 
201104B (Sbarufatti et al., GCN 28825) using the ESO VLT UT3 (Melipal) 
equipped with the X-shooter spectrograph. Our spectra cover the 
wavelength range 3000-21000 AA, and consist of 2 exposures of 1200 s 
each. The observation mid-time was 2020 Nov 5.0831 UT (8.431 hr after 
the GRB).

In a 60 s image taken with the acquisition camera on Nov 5.0596 UT, we 
detect the optical afterglow, for which we measure a magnitude r = 21.01 
+/- 0.02 mag (AB magnitude, calibrated against nearby stars from the 
Pan-STARRS catalog; Chambers et al. 2016, arXiv:1612.05560).

We clearly detect continuum over the entire wavelength range. A trough 
is visible around 3590 AA, which we identify as due to H I. From 
detection of multiple absorption features, which we interpret as due to 
SiII, CI, CII, SiIV, CIV, FeII, AlII, AlIII, MgII, we infer a redshift z 
= 1.954. In particular, fine structure lines from Fe II* are visible, 
which confirm the association of the absorption system with the GRB. 
Emission lines are also detected, which we interpret as due to [O II], 
Hbeta, [O III], ad Halpha at the same redshift.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular Florian Rodler, Ivan Aranda, and Matias Jones.

[GCN OPS NOTE(06nov2020): Per author's request, has two changes:
1) from "which we interpret as due to [O II], [O III], ad Halpha"
to "which we interpret as due to [O II], Hbeta, [O III], ad Halpha"
2) adding Ivan Aranda, and Matias Jones to the acknowledgement list.]


GRB_name: GRB201105A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28842
SUBJECT: GRB 201105A: BALROG localization (Fermi Trigger 626247072 / GRB 201105230)
DATE:    20/11/05 21:35:41 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
626247072 at 05:31:07 on 05 Nov. 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) = 247.4+/-0.4 deg
Decl.(2000.0) = 12.6+/-0.5 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201105230/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201105230/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201105230/json

                        


GRB_name: GRB201105B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28843
SUBJECT: GRB 201105B: Fermi GBM observation
DATE:    20/11/05 23:54:22 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

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

"At 05:09:32.233 UT on 5 November 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 201105B (trigger 626245777 / 201105215).
The on-ground calculated location, using the GBM trigger data,
is RA = 244.5, DEC = 16.0 (J2000 degrees, equivalent
to 16h 18m, -16d 02'), with an uncertainty of 1.0 degrees
(radius, 1-sigma containment, statistical only; there is additionally a 
systematic error which we have characterized as a mixture of two Gaussians,
one with a radius of 1.8 degrees (52% contribution) and one with a radius 
of 4.1 degrees (47% contribution) [A. Goldstein et al. 2020, ApJ, 895, 1] ).

The angle from the Fermi LAT boresight at the GBM trigger time is 92 degrees.

The GBM light curve shows a FRED emission episode
with a duration (T90) of about 17 s (50-300 keV).
The time-averaged spectrum from T0 to T0+23 s is
best fit by a Band function with Epeak = 512 +/- 21 keV,
alpha = -0.95 +/- 0.01, and beta = -2.35 +/- 0.09.

The event fluence (10-1000 keV) in this time interval is
(5.13 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.7 s in the 10-1000 keV band
is 28.5 +/- 0.5 ph/s/cm^2.


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

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


GRB_name: GRB201103B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28844
SUBJECT: IPN triangulation of GRB 201103B (consistent with ZTF20acozryr/AT2020yxz)
DATE:    20/11/06 00:20:30 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

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. 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,

A. Ursi, N. Parmiggiani, F. Verrecchia, A. Bulgarelli,
A. Trois, M. Marisaldi, C. Pittori, M. Tavani, Y. Evangelista,
I. Donnarumma, M. Cardillo, G. Piano, G. Minervini, A. Argan,
F. Lucarelli, A. Zoli, V. Fioretti, F. Fuschino, M. Pilia,
F. Longo, A. Giuliani on behalf of the AGILE team,

and

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

The long-duration, bright GRB 201103B
(AGILE detection: Ursi et al., GCN Circ. 28831)
has been detected by AGILE, Konus-Wind, INTEGRAL (SPI-ACS),
Mars-Odyssey (HEND), and Swift (BAT),
so far, at about 65207 s UT (18:06:47).
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:
    42.089 (02h 48m 21s) +12.441 (+12d 26' 29")
  Corners:
    41.830 (02h 47m 19s) +14.128 (+14d 07' 41")
    42.595 (02h 50m 23s) +11.069 (+11d 04' 07")
    42.244 (02h 48m 59s) +10.759 (+10d 45' 32")
    41.511 (02h 46m 03s) +13.781 (+13d 46' 52")
  ---------------------------------------------
The error box area is 1.24 sq. deg, and its maximum
dimension is 3.4 deg (the minimum one is 23.8 arcmin).
The Sun distance was 175 deg.

This box may be improved.

The distance between the optical transient ZTF20acozryr/AT2020yxz (Coughlin 
et al., GCN Circ. 28841) and the IPN box center is 19 arcmin, thus 
confirming the association of the burst and the OT.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB201103_T65207/IPN

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


GRB_name: GRB201105A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28845
SUBJECT: GRB 201105A: Swift detected burst and BAT refined analysis
DATE:    20/11/06 01:13:41 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

At 2020-11-05 05:31:10 UT, the Swift Burst Alert Telescope (BAT)
triggered and located GRB 201105A (trigger=1004239).
The burst occurred during GCN downtime, and the initial
circular (Simpson et al.) may have been lost.
We thus include information from that circular here as well.

The GRB location is Sun-constrained until 2020-12-27,
so no XRT or UVOT data are available.

Using the data set from T-239 to T+963 sec from the recent
telemetry downlink, the BAT ground-calculated position is
RA, Dec = 245.610, 12.734 deg which is
   RA(J2000)  =  16h 22m 26.4s
   Dec(J2000) = +12d 44' 03.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%

The BAT mask-weighted light curve shows a FRED-like pulse that starts
at ~T-3 s and peaks at ~T+1 s. The main structure ends at ~T+40 s,
with a tail emission that lasts till ~T+100 s. T90 (15-350 keV)
is 33.82 +- 4.03 sec (estimated error including systematics).

The time-averaged BAT spectrum from T-2.85 to T+72.11 sec is best
fit by a simple power-law model.  The power law index of the
time-averaged spectrum is 1.08 +- 0.03.  The fluence in the
15-150 keV band is 1.2 +- 0.02 x 10^-5 erg/cm2. The 1-sec peak
photon flux measured from T+0.76 sec in the 15-150 keV band is
13.9 +- 0.5 ph/cm2/sec.  All the quoted errors are at
the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1004239/BA/

Burst Advocate for this burst is K. K. Simpson (kira.simpson1984 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: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28846
SUBJECT: GRB 201103B (ZTF20acozryr/AT2020yxz): Nanshan/NEXT-0.6m optical observations
DATE:    20/11/06 02:36:07 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the optical transient, ZTF20acozryr/AT2020yxz, an likely 
orphan GRB optical afterglow when discovered by ZTF (Coughlin et al., 
GCN 28841) and later confirmed by the IPN localisation as the optical 
afterglow of GRB 201103B (Svinkin et al., GCN 28844), using the 
NEXT-0.6m optical telescope located at Nanshan, Xinjiang, China. 
Observations started at 17:33:06 UT on 2020-11-05 and a series of 120s 
exposures were obtained in the Sloan r-filter.

Considering the IPN trigger time, 18:06:47 UT on 2020-11-03, as the 
onset of the burst, preliminary photometry results are as follows:

T_mid_obs (UT) T_mid_grb(day)  Mag   MagErr
2020-11-05T17:43:35    1.984      20.5    0.3
2020-11-05T18:31:28    2.017      20.8    0.2

calibrated with nearby PS1 stars.

Compared with the ZTF photometry, such a decay is consistent with that 
of a conventional GRB optical afterglow.


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28847
SUBJECT: GRB 201103B (ZTF20acozryr/AT2020yxz): VLT/X-shooter redshift
DATE:    20/11/06 04:58:38 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu (NAOC), J.-B. Vielfaure (APC, Paris University), D. A. Kann 
(HETH/IAA-CSIC), D. B. Malesani (DTU Space), D. A. Perley (LJMU), A. J. 
Levan (Radboud U. Nijmegen), S. Klose, B. Stecklum (both TLS Tautenburg),
K. Wiersema (Univ. Warwick), and A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI) 
report on behalf of the Stargate Consortium:

We observed the transient ZTF20acozryr/AT2020yxz (Coughlin et al., GCN 
28841), which has been proposed to be the optical afterglow of GRB 
201103B (Svinkin et al., GCN 28844) using the ESO VLT UT3 (Melipal) 
equipped with the X-shooter spectrograph. Our spectra cover the 
wavelength range 3000-21000 AA, and consist of 4 exposures of 1200 s 
each. The observation mid-time was 2020 Nov 6.116 UT (56.66 hr/2.361 
days after the GRB).

In a 60 s image taken with the acquisition camera on Nov 6.0771 UT, we 
detect the optical afterglow, for which we measure a preliminary 
magnitude r ~ 20.7 mag (AB magnitude, calibrated against a nearby galaxy 
from the Pan-STARRS catalog; Chambers et al. 2016, arXiv:1612.05560).

We clearly detect continuum over the entire wavelength range. From 
detection of multiple absorption features, which we interpret as due to 
CII, MgII, and multiple FeII lines, we infer a redshift z = 1.105. We 
suggest this to be the redshift of the transient, which we hereby 
confirm spectroscopically to be the afterglow of GRB 201103B.

We acknowledge excellent support from the ESO observing staff in Paranal,
in particular Ivan Aranda and Matias Jones.

[GCN OPS NOTE(04nov2020): Per author's request, Ivan Aranda and Matias Jones
were added to the last sentence.]
[GCN OPS NOTE(07nov20): Per author's request, Stecklum was added
to the author's list.]


GRB_name: GRB201104C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28848
SUBJECT: GRB 201104C: Swift ToO observations
DATE:    20/11/06 07:51:21 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 ZTF GRB 201104C. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021039

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 ZTF 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: GRB201104C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28849
SUBJECT: Correcton to GCN 28848: Swift observes ZTF20acozryr
DATE:    20/11/06 07:58:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans reports on behalf of the Swift-XRT team:

GCN CIrcular 28848 incorrectly referred to GRB 201104C. This was due to a software error, not recognising 'ZTF20acozryrâ€™ as a GRB name.

Swift is actually carrying out observations of the source ZTF20acozryr (Coughlin et al., GCN Circ. 28841) which has been possibly associated with GRB 201103B (Svinkin et al., GCN Circl. 28844), and has a redshift of 1.105 (Xu et al., GCN Circl. 28847).

The results of the automated search for an X-ray counterpart consistent with the ZTF position, and analysis of any source(s) found, will appear at the URL previous circulated, i.e.

https://www.swift.ac.uk/ToO_GRBs/00021039

Although the nature of this object has not been confirmed, the zeropoint for any source light curves will be set to the IPN trigger time, in the first instance.

We apologise for the confusion.


GRB_name: GRB201104B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28850
SUBJECT: GRB 201104B: Swift-XRT refined Analysis
DATE:    20/11/06 09:09:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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
B. Sbarufatti report on behalf of the Swift-XRT team:

We have analysed 4.9 ks of XRT data for GRB 201104B (Sbarufatti et al.
GCN Circ. 28825), from 105 s to 131.7 ks after the  BAT trigger. The
data comprise 347 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. Using 546 s of PC mode data and 3 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 =
5.21441, +7.84185 which is equivalent to:

RA (J2000): 00h 20m 51.46s
Dec(J2000): +07d 50' 30.7"

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.11 (+0.11, -0.12), followed by a break at T+338 s to
an alpha of 1.21 (+0.05, -0.04).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.80 (+/-0.07). The
best-fitting absorption column is  1.12 (+0.30, -0.28) x 10^22 cm^-2,
at a redshift of 1.954, in addition to the Galactic value of 5.7 x
10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.7 x 10^-11 (4.5 x 10^-11) erg cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Galactic foreground: 5.7 x 10^20 cm^-2
Intrinsic column:    1.12 (+0.30, -0.28) x 10^22 cm^-2 at z=1.954
Photon index:      1.80 (+/-0.07)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01004168.

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


GRB_name: GRB201104B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28851
SUBJECT: GRB 201104B: Swift/UVOT Detection
DATE:    20/11/06 09:41:59 GMT
FROM:    Samantha Oates at MSSL  <samantha.oates@alumni.ucl.ac.uk>

S. R. Oates (U.Birmingham) and B. Sbarufatti (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 201104B
56 s after the BAT trigger (Sbarufatti et al., GCN Circ. 28825).
A source consistent with the XRT position (Sbarufatti et al. GCN Circ. 28825)
and UVOT position (Marshall et al. GCN Circ. 28827) is detected in the initial UVOT exposures.

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

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag
white  (FC)         56          206          147         17.98 +/- 0.05
white            20890        21385          484        >21.1
b                 3718         3777           57        >19.0
u (FC)             268          459          188         18.72 +/- 0.16

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.048 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB201104B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28852
SUBJECT: GRB 201104B: TSHAO optical observation
DATE:    20/11/06 11:11:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), N. Pankov (HSE), I. Reva (FAPHI), A. Pozanenko (IKI) 
report on behalf of GRB-IKI-FuN:

We observed the field of GRB 201104B (Sbarufatti et al., GCN  28825) 
with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory 
starting on Nov. 05 (UT) 12:51:33.

The optical afterglow (Marshall et al., GCN 28827; Vielfaure  et al., 
GCN 28840; Oates  et al., GCN 28851) at redshift z = 1.954 (Vielfaure 
et al., GCN 28840) is detected in stacked image in R-filter. Preliminary 
photometry of the afterglow is following.

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

2020-11-05 12:51:33 0.82641  R      43*90 21.20 0.1 22.2

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

USNO-B1.0_id R2
0979-0003163 17.51
0979-0003223 17.47

We note the presence of a galaxy 3.6" South-East from the afterglow. The 
galaxy is clearly visible in Pan-STARRS and SDSS and detected in 
USNO-B1.0, PS1 and SDSS DR12 (J002051.50+075026.5).


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28854
SUBJECT: GRB 201103B (ZTF20acozryr/AT2020yxz): Xinglong-2.16m optical observations
DATE:    20/11/06 16:03:42 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of ZTF20acozryr/AT2020yxz (Coughlin et al. GCN 
28841), likely the optical afterglow of GRB 201103B (Svinkin et al., GCN 
28844), using the 2.16m telescope equipped with the BFOSC camera at 
Xinglong, Hebei, China. Observations started at 14:12:36 UT on 
2020-11-06, and 8x180s R-band frames were obtained.

The source is clearly detected in our stacked image, with R = 20.36 +/- 
0.05 mag at Tmid-T0 = 2.8373 days post-burst, calibrated with nearby 
Pan-STARRS1.

We acknowledge excellent support from the Xinglong-2.16m observing 
staff, in particular Jie Zheng.


GRB_name: GRB201105B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28855
SUBJECT: Correction to GCN 28843: GBM report of GRB 201105B should have been GRB 201105A
DATE:    20/11/06 16:07:49 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

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


"The preliminary temporal and spectral analysis reported
in GCN 28843 refer to trigger 626247072 / 201105230,
detected by Fermi-GBM at 05:31:07.76 UT on 5 November 2020.
This event was also detected by the Swift/BAT
(Markwardt et al. 2020, GCN 28845).
The GBM on-ground location, also reported in GCN 28843,
is consistent with the Swift position.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201105230/quicklook/glg_skymap_all_bn201105230.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/bn201105230/quicklook/glg_healpix_all_bn201105230.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201105230/quicklook/glg_lc_medres34_bn201105230.gif

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: GRB201104B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28856
SUBJECT: GRB 201104B: Kitab optical observations
DATE:    20/11/06 17:01:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Zhornichenko (KIAM),  A. Pozanenko (IKI), V. 
Agletdinov (KIAM), Sh. Ehgamberdiev (UBAI) report on behalf of IKI-GRB-FuN:

We observed the field of GRB 201104B (Sbarufatti et al., GCN  28825) 
with Kitab-ISON RC-36  telescope in Clear filter.  Observation started 
on Nov. 4  (UT) 18:44:28, i.e. 77 minutes after trigger.
The optical afterglow (Marshall et al., GCN 28827; Vielfaure  et al., 
GCN 28840; Oates  et al., GCN 28851) at redshift z = 1.954 (Vielfaure et 
al., GCN 28840) is marginally (S/N = 1.8) detected in stacked image. 
Preliminary photometry of the afterglow is following.

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

2020-11-04  18:44:28 0.0741   72*60  CR      20.4  1.8   20.0

The photometry is based on nearby USNO-B1.0 stars, R magnitude.
USNO-B1.0_id R2
0979-0003163 17.51
0979-0003223 17.47


GRB_name: GRB201015A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28857
SUBJECT: GRB 201015A: Swift-XRT late time observations
DATE:    20/11/06 17:24:55 GMT
FROM:    Valerio D'Elia at ASDC  <valerio.delia@ssdc.asi.it>

V. Dâ€™Elia (SSDC) reports on behalf of the Swift team:

Following the Chandra late time detection (Gompertz et al., GCN Circ. 28822) of GRB 201015A (Dâ€™Elia et al., GCN Circ. 28632), Swift performed a ToO observation of its X-ray afterglow. 13 ks of data were acquired between 3 and 6 November, i.e., 18-21 days after the trigger. Consistent with the prediction reported by Gompertz et al., XRT detected the afterglow at a level of (7+/-3)E-4 cts/s.

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

[GCN OPS NOTE(06nov2020): Per author's request, the tail end containing the signiture block was removed.]


GRB_name: GRB201103B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28858
SUBJECT: Swift XRT and UVOT detection of ZTF20acozryr/AT2020yxz/GRB201103B 
DATE:    20/11/06 17:44:52 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

P. A. Evans (U Leicester), N. P. M. Kuin (UCL-MSSL) and B. Sbarufatti (PSU) report on behalf of the Swift team:

Swift-XRT has performed follow-up observations of the ZTF-detected afterglow candidate ZTF20acozryr/AT2020yxz, (Coughlin et al., GCN 28841) proposed to be associated with the AGILE and IPN-detected GRB 201103B (Ursi et al., GCN Circ. 28831, Svinkin et al., GCN Circ. 28844), collecting 1.2 ks of Photon Counting (PC) mode data between T0+199.5 ks and T0+206.0 ks. 

An uncatalogued X-ray source is detected, at RA, Dec=42.1842, +12.1382 which is equivalent to:

RA (J2000): 02:48:44.21
Dec(J2000): +12:08:17.6

with an uncertainty of 5.3 arcsec (radius, 90% confidence).  This position is 3.8 arcsec from the ZTF position, consistent with that source. We cannot determine at the present time whether the source is fading.

The mean count-rate of the source is (1.5 +/- 0.5) x 10^-3 ct/sec, and we cannot yet confirm any variability.

This location has been previously observed by Swift in 2014 November, and these observations are in the 2SXPS catalogue (Evans et al., 2020): 
https://www.swift.ac.uk/2SXPS/doSimpleSearch.php?searchpos=42.18421+12.1382&searchrad=750&getWhat=1&subset=1&dssubset=0&coordType=0&retType=0&searchWhat=1

The stacked image (field 10000005379) created from the 2014 observation contained about 2043 s of exposure at this position, and contained only 2 events at the ZTF location, giving a 3-sigma upper limit of 5.4 x 10^-3 ct/sec. Thus the XRT source reported above is a transient event, and we identify it as the X-ray afterglow to GRB 201103B.

It has been pointed out to us that we incorrectly stated in GCN 28849 that the nature of the object had not been confirmed, whereas Xu et al (GCN Circ. 28847) has in fact confirmed the associated with the GRB via their spectroscopy. We apologize for the confusion.

The automated analysis of this object is available at https://www.swift.ac.uk/xrt_products/00021039 

A source is also detected in UVOT data with magnitude  B=20.25+-0.26 at ~T+205 ks. A weak signal is also detected in the V band at less than 3 sigma significance (V > 19.6) with some evidence of fading.

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


GRB_name: GRB201104A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28859
SUBJECT: GRB 201104A: Swift-XRT observations
DATE:    20/11/06 17:46:49 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), J. D.
Gropp (PSU), J.A. Kennea (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/LAT-detected burst GRB 201104A (Ohno et al. GCN Circ. 28828) in a
series of observations tiled on the sky. The total exposure time is 4.7
ks, distributed over 3 tiles; the maximum exposure at a single sky
location was 2.4 ks. The data were collected between T0+67.6 ks and
T0+80.9 ks, and are entirely in Photon Counting (PC) mode. 

One uncatalogued X-ray source has been detected, it is not above the
RASS limit or shows definitive signs of fading. Furthermore, it is
coincident with a known optical source and the XRT data are possibly
affected by stray light. Therefore we believe that XRT has not detected
any viable candidate afterglow.
Details of the sources are given below:

Source 3:
  RA (J2000):  80.9041  =  05:23:36.99
  Dec (J2000): -71.0096  =  -71:00:34.6
  Error: 4.1 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (5.3 [+2.7, -2.0])e-3 ct s^-1   
  Distance: 664 arcsec from Fermi/LAT position.
  Flux: (1.53 [+0.77, -0.59])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


A catalogued source was also detected inside the LAT error circle, and
two more sources were detected outside of it.

The 3 sigma upper limit at the LAT GRB position is 7.6Ã—10-3 ct s-1.

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_GRB00094.

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


GRB_name: GRB201104B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28860
SUBJECT: GRB 201104B: 1.3m DFOT optical observations
DATE:    20/11/06 19:56:54 GMT
FROM:    Rahul Gupta at ARIES, India  <rahul@aries.res.in>

Rahul Gupta (ARIES), Dimple (ARIES), Amit Kumar (ARIES), Ankur Ghosh (ARIES), Amar Aryan (ARIES), Shubham Kishore (ARIES) , Shashi B. Pandey (ARIES), Kuntal Misra (ARIES), and Alok C. Gupta (ARIES ) report: 

We observed the optical afterglow ( Marshall et al., GCN 28827 ; Vielfaure et al., GCN 28840; Oates et al., GCN 28851; and Belkin et al., GCN 28852, GCN 28856) of Swift triggered GRB 201104B (Sbarufatti et al., GCN 28825) using the 1.3m Devasthal Fast Optical Telescope (DFOT) at Devasthal observatory of Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2020-11-05 at 17:44:45 UT . Multiple frames having an exposure time of 60 s were taken in the R filter. We clearly detected the optical counterpart in the stacked images. 

The preliminary photometric estimate of the afterglow in the stacked images is the following : 


Date Start_UT T_start-T0 (hrs) Filter Exp time (s) Magnitude Mag_err 
------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------------------ ------------------ 

2020-11-05 17:44:45 24.18 R 30*60 22.40 0.23 

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


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

This circular may be cited. 


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28861
SUBJECT: GRB201103B: GMG observation
DATE:    20/11/07 12:16:59 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, C.-J. Wang, and J.-M. Bai (YNAO) report:

 


We observed the field of GRB201103B/ZTF20acozryr/AT2020yxz with the 2.4-meter optical telescope

at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 16:41:52, 6th,

Nov. 2020. We clearly detected the source, and the preliminary magnitude is measured to be R~20.6.


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28862
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): Assy optical observations
DATE:    20/11/07 13:47:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the ZTF20acozryr/AT2020yxz (Coughlin et al., GCN  28841) 
with AZT-20 telescope of Assy-Turgen observatory starting on  Nov. 06 
(UT) 19:10:28  in  r'-filter.  We detect the optical transient (Coughlin 
et al., GCN  28841; Coughlin et al., GCN  28841; Xu  et al., GCN 28846; 
Xu  et al., GCN 28854; Mao et al., GCN  28861; ) which can be afterglow 
of GRB 201103B (Svinkin et al., GCN 28844; Evans  et al., GCN 28858).

Preliminary photometry of the afterglow is following

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

2020-11-06 19:10:28  3.06508  r'(AB)  60*60   20.84 0.06   23.1

The photometry is based on the nearby stars of PanSTARRS-PS1.

RA DEC r
02:48:57.72094 +12:12:04.2202 16.6938
02:48:41.68064 +12:09:59.6523 17.0772


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28863
SUBJECT: GRB 201103B: GMG observation (2nd epoch)
DATE:    20/11/07 16:02:50 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, C.-J. Wang, and J.-M. Bai (YNAO) report:




We observed the field of GRB201103B/ZTF20acozryr/AT2020yxz with

the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan

Observatories once again. The observation began at UT 14:27:51, 7th,

Nov. 2020. We clearly detected the source, and the preliminary magnitude

is measured to be R~20.9. It seems that the source is fading very slightly.

We suggest to perform both photometric monitors to obtain the variability

behavior and spectral observations to obtain the possible spectral evolution

in the following nights.


GRB_name: GRB201105A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28864
SUBJECT: Konus-Wind detection of GRB 201105A
DATE:    20/11/07 16:14:54 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 long-duration GRB 201105A
(Fermi-GBM detection: Biltzinger et al., GCN Circ. 28842,
Bissaldi & Lesage, GCN Circ. 28843;
Swift-BAT trigger #1004239: Markwardt et al., GCN Circ. 28845)
triggered Konus-Wind at T0=19865.464 s UT (05:31:05.464).

The burst light curve shows a single FRED-like pulse
which starts at ~T0-2.4 s and has a total duration of ~29.6 s.
The emission is seen up to ~4 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB201105_T19865/

As observed by Konus-Wind, the burst
had a fluence of 7.88(-0.85,+0.79)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+2.624 s,
of 1.59(-0.30,+0.30)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+26.368 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.55(-0.12,+0.13),
the high energy photon index beta = -2.11(-0.17,+0.11),
the peak energy Ep = 286(-31,+42) keV
(chi2 = 92/71 dof).

The spectrum near the maximum count rate
(measured from T0+2.304 to T0+4.096 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.43(-0.18,+0.20),
the high energy photon index beta = -2.05(-0.18,+0.12),
the peak energy Ep = 305(-48,+66) keV
(chi2 = 51/60 dof).

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


GRB_name: GRB201108A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28866
SUBJECT: GRB 201108A: Fermi GBM Final Real-time Localization
DATE:    20/11/08 15:38:43 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 15:28:23 UT on 8 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201108A (trigger 626542108.26729 / 201108645).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 289.0, Dec = 35.9 (J2000 degrees, equivalent to J2000 19h 15m, 35d 53'), with a statistical uncertainty of 9.7 degrees.

The angle from the Fermi LAT boresight is 66.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201108645/quicklook/glg_skymap_all_bn201108645.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/bn201108645/quicklook/glg_healpix_all_bn201108645.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201108645/quicklook/glg_lc_medres34_bn201108645.gif


GRB_name: GRB201108A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28867
SUBJECT: Fermi GRB 201108A: Global MASTER-Net observations report 
DATE:    20/11/08 15:45:12 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),

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 201108A ( Fermi GBM team, GCN 28866) errorbox  359 sec after notice time and 389 sec after trigger time at 2020-11-08 15:34:52 UT, with upper limit up to  16.7 mag. Observations started at twilight.  The observations began at zenith distance = 17 deg. The sun  altitude  is -13.0 deg. 

The galactic latitude b = 11 deg., longitude l = 68 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1477785

We obtain a following upper limits.  

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

     420 | 2020-11-08 15:34:52 |      MASTER-Tavrida | (19h 53m 10.99s , +33d 59m 17.0s) |   C |    60 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201109A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28868
SUBJECT: GRB 201109A: Fermi GBM Final Real-time Localization
DATE:    20/11/09 02:41:28 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 02:31:05 UT on 9 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201109A (trigger 626581870.79309 / 201109105).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 136.1, Dec = -5.1 (J2000 degrees, equivalent to J2000 09h 04m, -5d 05'), with a statistical uncertainty of 3.3 degrees.

The angle from the Fermi LAT boresight is 66.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201109105/quicklook/glg_skymap_all_bn201109105.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/bn201109105/quicklook/glg_healpix_all_bn201109105.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201109105/quicklook/glg_lc_medres34_bn201109105.gif


GRB_name: GRB201109A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28869
SUBJECT: Fermi GRB 201109A: Global MASTER-Net observations report 
DATE:    20/11/09 03:00:09 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),

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 201109A ( Fermi GBM team, GCN 28868) errorbox  533 sec after notice time and 585 sec after trigger time at 2020-11-09 02:40:50 UT, with upper limit up to  18.2 mag. The observations began at zenith distance = 69 deg. The sun  altitude  is -61.5 deg. 

The galactic latitude b = 27 deg., longitude l = 235 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1478104

We obtain a following upper limits.  

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

     645 | 2020-11-09 02:40:50 |          MASTER-IAC | (09h 03m 30.97s , -05d 02m 21.6s) |   C |   120 | 17.3 |        
     805 | 2020-11-09 02:40:50 |          MASTER-IAC | (09h 03m 30.96s , -05d 02m 21.6s) |   C |   440 | 18.2 |  Coadd 
     795 | 2020-11-09 02:43:10 |          MASTER-IAC | (09h 03m 28.96s , -05d 01m 05.9s) |   C |   140 | 17.6 |        
     974 | 2020-11-09 02:45:50 |          MASTER-IAC | (09h 03m 29.14s , -05d 02m 40.8s) |   C |   180 | 17.9 |        
    1174 | 2020-11-09 02:49:09 |          MASTER-IAC | (09h 03m 33.03s , -05d 00m 53.6s) |   C |   180 | 17.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201104B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28870
SUBJECT: GRB 201104B: MITSuME Akeno optical observation
DATE:    20/11/09 09:47:55 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

R. Hosokawa, R. Adachi, K. L. Murata, M. Niwano, F. Ogawa, N.
Nakamura, N. Ito, 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 201104B (B. Sbarufatti et al., GCN
#28825) 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 with a series of 60 sec exposures started at
2020-11-05 08:14:33 UT. The first 29 images were heavily affected by
twilight at Akeno Observatory. We marginally detected the point source
at the position consistent with the afterglow detected previously
(Marshall et al., GCN #28827, Vielfaure et al., GCN #28840, Oates et
al., GCN #28851, Belkin et al., GCN #28852, Belkin et al., GCN #28856,
and Gupta et al., GCN #28860).

We measured the magnitudes as follows.
T0+[hour] MID-UT T-EXP[sec] measured magnitudes
------------------------------------------------------------------------------------------------
15.2 2020-11-05 12:59:59 21360 g'=21.5+/-0.3, Rc=20.7+/-0.2, Ic=20.3+/-0.3
------------------------------------------------------------------------------------------------
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.,
https://doi.org/10.1093/pasj/psaa091,
https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire).


GRB_name: GRB201104B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28871
SUBJECT: GRB 201104B: continued TSHAO optical observation
DATE:    20/11/09 12:57:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Kusakin (FAP), N. Pankov (HSE), I. Reva (FAP), A. 
Pozanenko (IKI) report on behalf of GRB-IKI-FuN:

We continued observations of the  GRB 201104B (Sbarufatti et al., GCN 
28825) with Zeiss-1000 1-m telescope of Tien Shan Astronomical 
Observatory starting on Nov. 06 (UT) 15:04:58.

The optical afterglow (Marshall et al., GCN 28827; Vielfaure  et al., 
GCN 28840; Oates  et al., GCN 28851; Belkin et al., GCNs 28852, 28856; 
Gupta et al., GCN 28860; Hosokawa et al., GCN 28870) at redshift z = 
1.954 (Vielfaure et al., GCN 28840) is detected in stacked image in 
R-filter. Preliminary photometry of the afterglow is following.

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

2020-11-06 15:04:58 1.92271  R      50*90 22.20 0.21 22.4

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

USNO-B1.0_id R2
0979-0003163 17.51
0979-0003223 17.47


GRB_name: GRB201103B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28872
SUBJECT: Konus-Wind observation of GRB 201103B
DATE:    20/11/09 15:28:16 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 long-duration GRB 201103B
(AGILE detection: Ursi et al., GCN Circ. 28831;
ZTF afterglow discovery: Coughlin et al., GCN Circ. 28841;
IPN triangulation: Svinkin et al., GCN Circ. 28844)
triggered Konus-Wind at T0=65207.923 s UT (18:06:47.923).

The burst light curve shows a multi-peaked structure
which starts at ~T0-14 s, peaks at ~T0+1.5, and ends at ~T0+20 s,
followed by a weaker emission seen up to ~T0+91 s.
The total burst duration is ~105 s.
The emission is seen up to ~5 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB201103_T65207/

As observed by Konus-Wind, the burst
had a fluence of 5.26(-0.77,+0.82)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.536 s,
of 1.49(-0.24,+0.25)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+16.640 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.72(-0.16,+0.19),
the high energy photon index beta = -2.54(-1.13,+0.33),
the peak energy Ep = 403(-60,+74) keV
(chi2 = 102/97 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 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 = -0.71(-0.12,+0.13)
and Ep = 466(-47,+58) keV (chi2 = 104/98 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 102/97 dof).

Assuming the redshift z=1.105 (Xu et al., GCN Circ. 28847)
and a standard cosmology model 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 is ~1.8x10^53 erg,
the peak luminosity L_iso is ~1.1x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,z,i is ~850 keV.

With these values, GRB 201103B is consistent with the 'Amati'
and 'Yonetoku' relations built for 316 KW GRBs with known z
classified as Type II (Tsvetkova et al., ApJ 2020 submitted).
The 68% and 90% prediction bands for Type II are show with
dark and light shaded regions, respectively, see
http://www.ioffe.ru/LEA/GRBs/GRB201103_T65207/GRB201103B.pdf

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


GRB_name: GRB201104A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28873
SUBJECT: GRB 201104A: AstroSat CZTI detection
DATE:    20/11/09 20:42:02 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:

The AstroSat CZT Imager recorded a transient event in all four of its CsI anticoincidence (Veto) detectors in the 100-500 keV energy range, coincident with the long GRB 201104A reported by Fermi GBM (GCN #28823), Global MASTER-Net (Lipunov V. et al., GCN #28824), Fermi LAT (Ohno M. et al., GCN #28828), AGILE/MCAL (Ursi A. et al., GCN #28829), Fermi GBM (Bissaldi E. et al., GCN #28830), Tiled Swift (Evans P. et al., GCN #28832), BALROG (Kunzweiler F. et al., GCN #28834) and Swift-XRT (D'Elia V. et al., GCN #28859). There was a weak detection in the main CZT detectors in the 40-200 keV energy range.

The light curve showed multiple peaks of emission with the strongest peak at 2020-11-04 00:00:55.000 UT. The measured peak count rate is 1757 +/- 68 cts/s above the background in the combined Veto data of four quadrants, with a total of 6949 +/- 80 cts. The local mean background count rate was 2774 +/- 5 cts/s.  We measure a T90 of 8.18 +/- 0.13 s from the cumulative Veto light curve.

In the main CZT detectors, the light curve showed multiple peaks of emission with the strongest peak at 2020-11-04 00:00:56.000 UT. The measured peak count rate associated with the burst is 330 +/- 33 cts/s above the background in the combined data of four quadrants, with a total of 1170 +/- 23 cts. The local mean background count rate was  792 +/- 2 cts/s. Using cumulative rates, we measure a T90 of 7.36 +/- 0.11 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: GRB201109A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28874
SUBJECT: GRB 201109A: Fermi GBM detection
DATE:    20/11/09 20:47:49 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

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

"At 02:31:05.79  UT on 9 November 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 201109A (trigger 626581870 / 201109105).
The Fermi GBM Final Real-time Localization was reported in GCN 28868.

The angle from the Fermi LAT boresight at the GBM trigger time is 66 degrees.

The GBM light curve consists of a bright peak
with a duration (T90) of about 0.45 s (50-300 keV).
The time-averaged spectrum from T0-0.128 s to T0+0.384 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.61 +/- 0.11 and
the cutoff energy, parameterized as Epeak, is 318 +/- 41 keV.

The event fluence (10-1000 keV) in this time interval is
(9.55 +/- 0.72)E-07 erg/cm^2. The 64-msec peak photon flux measured
starting from T0+64 ms in the 10-1000 keV band
is 18.4 +/- 1.2 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 304 +/- 56 keV, alpha = -0.59 +/- 0.14 and beta = -2.93 +/- 1.42 .


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: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28875
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): Mondy, Kitab, TSHAO optical observations
DATE:    20/11/09 23:22:50 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI),  E. Klunko (ISTP), A. Zhornichenko (KIAM), A. Kusakin 
(FAI), I. Reva(FAI),  A. Pozanenko (IKI), N. Pankov (HSE) report on 
behalf of GRB IKI FuN:

We observed the ZTF20acozryr/AT2020yxz (Coughlin et al., GCN  28841) 
with AZT-33IK telescope of Mondy observatory, RC-36 telescope of Kitab 
observatory, and Zeiss-1000 of Tian Shan observatory.  We detect the 
optical transient (Coughlin et al., GCN  28841; Xu  et al., GCN 28846; 
Zhu et al., GCN 28854; Mao et al., GCN  28861; Belkin et al., GCN 28862; 
  Mao et al., GCN 28863) associated with afterglow of GRB 201103B (Ursi 
et al., GCN 28831; Svinkin et al., GCN 28844; Evans  et al., GCN 28858).

Preliminary photometry of the afterglow is following
Date       UT start  t-T0     Filter Exp.    OT    Err.   UL. Telescope
                      (mid, days)      (s)

2020-11-05 21:57:40 2.16938   CR     26*60   n/d   n/d   19.0 RC-36
2020-11-06 15:42:41 2.92217    R     32*120  20.23 0.26  20.5 AZT-33IK
2020-11-06 16:56:13 2.97237    R     32*120  20.49 0.12  21.7 Z-1000
2020-11-08 14:13:52 4.85911    R     32*120  21.50 0.10  23.0 AZT-33IK

The photometry is based on the nearby stars of PanSTARRS-PS1

RA DEC r
02:48:57.72094 +12:12:04.2202 16.6938
02:48:41.68064 +12:09:59.6523 17.0772


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28876
SUBJECT: ZTF20acozryr (GRB 201103B): GROWTH-India Telescope optical observations
DATE:    20/11/10 15:25:55 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

K. Sharma (IITB), H. Kumar (IITB), P. Dorjay (IAO), J. Stanzin (IAO), U.
Stanzin (IAO), V. Bhalerao (IITB), G. C. Anupama (IIA), S. Barway (IIA),
report on behalf of the GROWTH-India collaboration:

We followed-up the optical afterglow ZTF20acozryr (Michael Coughlin et.
al., GCN #28841) of GRB 201103B, detected by the AGILE (GCN #28831) and IPN
(D. Svinkin et. al. GCN #28844), with 0.7 m GROWTH-India telescope. We
obtained 300-sec exposures in the SDSS r' filter over multiple nights.

Here are the photometric results from GIT observations:-

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

JD (mid) | Filter | Exposure | mag | e_mag |

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

2459160.322200 | r' | 300 x 20 | 21.08 | 0.08 |

2459163.145455 | r' | 300 x 30 | 21.91 | 0.06 |

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

Combining our photometric results with r/r' band measurements of Michael
Coughlin et. al., GCN #28841; D. Xu et. al., GCN #28846; D. Xu et. al., GCN
#28847; S. Belkin et. al., GCN #28862; we conclude that the source is
fading with a power-law index of 1.16 +/- 0.07. The magnitudes are
calibrated against PanSTARRs PS1 data release, (Flewelling et al., 2018)
and are not corrected for galactic extinction.

The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB201109A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28877
SUBJECT: IPN triangulation of GRB 201109A (short)
DATE:    20/11/10 23:38:09 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

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

K. Hurley, on behalf of the IPN,

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

and

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

The short-duration GRB 201109A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 28868;
Malacaria et al., GCN Circ. 28874)
was detected by Fermi (GBM trigger 626581870),
INTEGRAL (SPI-ACS), and Konus-Wind
at about 9066 s UT (02:31:06).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   138.382 (09h 13m 32s)  -9.192 ( -9d 11' 31")
  Corners:
   140.147 (09h 20m 35s)  -6.874 ( -6d 52' 27")
   139.193 (09h 16m 46s)  -6.204 ( -6d 12' 13")
   136.612 (09h 06m 27s) -11.514 (-11d 30' 52")
   137.577 (09h 10m 19s) -12.196 (-12d 11' 46")
  ---------------------------------------------
The error box area is 6.75 sq. deg, and its maximum
dimension is 6.2 deg (the minimum one is 1.15 deg).
The Sun distance was 83 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the 
Fermi-GBM final position (GCN Circ. 28868).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB201109_T09065/IPN

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


GRB_name: GRB201111A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28878
SUBJECT: GRB 201111A: Fermi GBM Final Real-time Localization
DATE:    20/11/11 07:56:08 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 07:45:45 UT on 11 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201111A (trigger 626773550.984268 / 201111323).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 80.6, Dec = -16.6 (J2000 degrees, equivalent to J2000 05h 22m, -16d 36'), with a statistical uncertainty of 12.1 degrees.

The angle from the Fermi LAT boresight is 64.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201111323/quicklook/glg_skymap_all_bn201111323.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/bn201111323/quicklook/glg_healpix_all_bn201111323.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201111323/quicklook/glg_lc_medres34_bn201111323.gif


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28880
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): Flattening of the optical light curve
DATE:    20/11/11 11:54:49 GMT
FROM:    Gregory SungHak Paek at SNU  <shpaek@astro.snu.ac.kr>

Gregory S.H. Paek (SNU), Myungshin Im (SNU), Joonho Kim (SNU), Gu Lim
(SNU), Mankeun Jeong (SNU), Chung-Uk Lee (KASI), Seung-Lee Kim (KASI),
Hyun-Il Sung (KASI),  Taewoo Kim (DOAO), and Wonseok Kang (DOAO) and GECKO
team

 We observed the ZTF20acozryr/AT2020yxz (Coughlin et al., GCN 28841) in
BVRI with various optical telescopes of the GW EM-Counterpart Korean
Observatory (GECKO). The facilities used for the observations are the 1.6-m
class telescopes of Korea Microlensing Telescope Network (KMTNet) located
in Siding Spring Observatory (SSO) and South African Astronomical
Observatory (SAAO), the 1-m telescope in Deokheung Optical Astronomy
Observatory (DOAO), the 1-m telescope the Mt. Lemmon Optical Astronomy
Observatory (LOAO), and the 0.36-m KIAS Chamnun Telescope (KCT) and RASA36
telescope in Chile. We calibrated flux with PS1 and APASS catalog, and the
magnitudes are in AB system. The magnitudes are not corrected for galactic
extinction. Preliminary R-band magnitudes are given for the most recent a
few epoch observations.

Obs.&Tel.           DATE-OBS(UT)    Filter   Mag    Error  t-t0(days since
burst)
----------- ----------------------- ------ ------- -------
----------------------
DOAO        2020-11-08T19:51:31     R      21.6    0.1     5.07
KCT         2020-11-10T04:27:38     R      21.8    0.3     6.43
KMTNet-SAAO 2020-11-10T21:37:55     R      21.8    0.1     7.1

t0 = 2020-11-03T18:06:45.36 (Ursi et al., GCN 28831)

About a week after GRB occurs, the brightness seems to remain nearly
constant, suggesting a possible onset of a supernova component accompanied
with GRB.

We thank all the operators at GECKO facilities for performing the
observation.

Gravitational-wave EM Counterpart Korean Observatory (GECKO) is a network
of 10+ 0.5m to 1m class telescopes over the world.


GRB_name: GRB201109A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28881
SUBJECT: Konus-Wind observation of GRB 201109A
DATE:    20/11/11 18:00:02 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 short-duration GRB 201109A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 28868;
Malacaria et al., GCN Circ. 28874;
IPN triangulation: Svinkin et al., GCN Circ. 28877)
triggered Konus-Wind at T0=9065.305 s UT (02:31:05.305).

The burst light curve shows a single pulse
which starts at ~T0-0.2 s and has a total duration of ~0.4 s.
The emission is seen up to ~2 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB201109_T09065/

As observed by Konus-Wind, the burst
had a fluence of 9.79(-1.84,+2.96)x10^-7 erg/cm2,
and a 16-ms peak flux, measured from T0+0.018 s,
of 6.13(-2.75,+3.42)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.192 s)
is best fit in the 20 keV - 5 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.96(-0.51,+0.65)
and Ep = 244(-73,+249) keV (chi2 = 13/16 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.9
(chi2 = 13/15 dof).

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


GRB_name: GRB201111A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28882
SUBJECT: Fermi GRB 201111A: Global MASTER-Net observations report 
DATE:    20/11/11 21:45:11 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),

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 201111A ( Fermi GBM team, GCN 28878) errorbox  49227 sec after notice time and 49238 sec after trigger time at 2020-11-11 21:26:24 UT, with upper limit up to  18.8 mag. The observations began at zenith distance = 56 deg. The sun  altitude  is -63.7 deg. 

The galactic latitude b = -26 deg., longitude l = 219 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1480057

We obtain a following upper limits.  

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

   49269 | 2020-11-11 21:26:24 |      MASTER-Tavrida | (05h 14m 19.42s , -03d 53m 02.4s) |   C |    60 | 18.7 |        
   49430 | 2020-11-11 21:29:05 |      MASTER-Tavrida | (05h 30m 19.56s , -03d 53m 04.9s) |   C |    60 | 18.3 |        
   49510 | 2020-11-11 21:30:26 |      MASTER-Tavrida | (05h 15m 12.59s , -05d 53m 15.5s) |   C |    60 | 18.6 |        
   49591 | 2020-11-11 21:31:46 |      MASTER-Tavrida | (05h 14m 13.92s , -03d 52m 15.0s) |   C |    60 | 18.8 |        
   49671 | 2020-11-11 21:33:07 |      MASTER-Tavrida | (05h 22m 22.24s , -03d 52m 57.2s) |   C |    60 | 18.4 |        
   49913 | 2020-11-11 21:37:08 |      MASTER-Tavrida | (05h 30m 19.40s , -03d 51m 53.2s) |   C |    60 | 18.4 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28883
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): Mondy continued optical observations
DATE:    20/11/12 11:36:35 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We continued observations of the ZTF20acozryr/AT2020yxz (Coughlin et 
al., GCN  28841) with AZT-33IK telescope of Mondy observatory.  We 
detect the optical transient (Coughlin et al., GCN  28841; Xu  et al., 
GCN 28846; Zhu et al., GCN 28854; Mao et al., GCN  28861; Belkin et al., 
GCNs 28862, 28875;  Mao et al., GCN 28863; Kumar et al., GCN 28876; 
SungHak  et al., GCN 28880) at redshift  z = 1.105 (Xu et al., GCN 
28847) associated with afterglow of GRB 201103B (Ursi et al., GCN 28831; 
Svinkin et al., GCN 28844; Evans  et al., GCN 28858).

Preliminary photometry of the afterglow is following
Date       UT start  t-T0     Filter Exp.    OT    Err.   UL. Telescope
                      (mid, days)      (s)


2020-11-09 14:53:25 5.88657    R     30*120  21.67 0.19  22.5 AZT-33IK
2020-11-11 13:59:54 7.84871    R     29*120  21.60 0.25  21.8 AZT-33IK


The photometry is based on the same stars used in GCNs 28862, 28875.


GRB_name: GRB201114A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28885
SUBJECT: GRB 201114A: AstroSat CZTI detection
DATE:    20/11/14 06:10:05 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma, A. Vibhute 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 detection of a long GRB 201114A.

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 2020-11-14 00:39:25.539 UT. The measured peak count rate associated with the burst is 463 +/- 28 cts/s above the background in the combined data of four quadrants, with a total of 6961 +/- 43 cts. The local mean background count rate was  753 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 32.67 +/- 0.02 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: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28886
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): CrAO/ZTSh optical observations
DATE:    20/11/14 12:26:46 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We continued observations of the ZTF20acozryr/AT2020yxz (Coughlin et 
al., GCN  28841)  with ZTSh 2.6m telescope of CrAO observatory starting 
on Nov., 13 (UT) 22:58:04.  We detect the optical transient (Coughlin et 
al., GCN  28841; Xu  et al., GCN 28846; Zhu et al., GCN 28854; Mao et 
al., GCN  28861; Belkin et al., GCNs 28862, 28875, 28883;  Mao et al., 
GCN 28863; Kumar et al., GCN 28876; SungHak  et al., GCN 28880) at 
redshift  z = 1.105 (Xu et al., GCN 28847) associated with afterglow of 
GRB 201103B (Ursi et al., GCN 28831; Svinkin et al., GCN 28844; Evans et 
al., GCN 28858).

Preliminary photometry of the afterglow is following
Date       UT start  t-T0     Filter Exp.    OT    Err.   UL. Telescope
                      (mid, days)      (s)


2020-11-13 22:58:04 10.21897    R     24*120 21.67 0.16  22.1 ZTSh

The photometry is based on the same stars used in GCNs 28862, 28875, 28883.


GRB_name: GRB201116A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28897
SUBJECT: GRB 201116A: Fermi GBM Final Real-time Localization
DATE:    20/11/16 01:00:12 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 LONG GRB

At 00:49:47 UT on 16 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201116A (trigger 627180592.69203 / 201116035).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 149.5, Dec = -4.2 (J2000 degrees, equivalent to J2000 09h 58m, -4d 12'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 14.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201116035/quicklook/glg_skymap_all_bn201116035.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/bn201116035/quicklook/glg_healpix_all_bn201116035.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201116035/quicklook/glg_lc_medres34_bn201116035.gif


GRB_name: GRB201116A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28898
SUBJECT: GRB 201116A: BALROG localization (Fermi Trigger 627180592 / GRB 201116035)
DATE:    20/11/16 01:14:14 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
627180592 at 00:49:47 on 16 Nov. 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) = 148.42+/-0.33 deg
Decl.(2000.0) = 2.46+/-0.57 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201116035/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201116035/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201116035/json    


GRB_name: GRB201116A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28906
SUBJECT: GRB 201116A: Tiled Swift observations
DATE:    20/11/16 13:43:44 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 201116A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00095

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

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

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


GRB_name: GRB201116A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28907
SUBJECT: GRB 201116A: Fermi-LAT detection
DATE:    20/11/16 14:09:02 GMT
FROM:    Frederic Piron at CNRS/IN2P3/LUPM  <piron@in2p3.fr>

M. Axelsson (KTH & Stockholm Univ.), M. Ohno (Hiroshima Univ. & Eotvos 
Univ.),
E. Bissaldi (Politecnico & INFN Bari), F. Longo (University and INFN, 
Trieste) and
F. Piron (CNRS/IN2P3/LUPM) report on behalf of the Fermi-LAT Collaboration:

On November 16, 2020 Fermi-LAT detected high-energy emission from
GRB 201116A, which was also detected by Fermi-GBM (trigger 627180592,
GCN 28897).

The best LAT on-ground location is found to be

RA, Dec 149.33, 0.32 (degrees, J2000)

with an error radius of 0.24 deg (90% containment, statistical error only).
This was 14 deg from the LAT boresight at the time of the GBM trigger:

T0 = 00:49:47 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 (4 degrees from the GBM location) with high significance.
The photon flux above 100 MeV in the time interval 0-1000s after the
GBM trigger is (2.25+/-0.07)e-06 ph/cm2/s.

The estimated photon index above 100 MeV is -1.9 +/- 0.3.

The highest-energy photon is a 2.4 GeV event which is observed 82 
seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is
Frederic Piron (piron@in2p3.fr).

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


GRB_name: GRB201116A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28915
SUBJECT: GRB 201116A: OSN Afterglow Candidate
DATE:    20/11/17 04:36:25 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

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

We observed the location of the Swift XRT source #3 found in tiled Swift 
observations (Evans, GCN #28906), potentially the (X-ray) afterglow of 
Fermi GBM/LAT GRB 201116A (Fermi GBM Team, GCN #28897; Kunzweiler et 
al., GCN #28898; Axelsson et al., GCN #28907) with the 1.5m telescope of 
the Observatorio Sierra Nevada, in Granada, Spain. We obtained 15 x 180 
s images in Rc, beginning 2020-11-17 03:24:46.56 UT, 1.1076 days after 
the GRB.

We detect a faint source in the Rc-band stack at (J2000)

RA   =  09:57:17.94
Dec. = +00:16:34.1

with Rc = 23.18 +/ 0.18 mag (AB), as measured against multiple SDSS 
comparison stars.

This source is not visible in SDSS or PanSTARRS imaging, suggesting it 
is the GRB afterglow. We cannot determine evidence for fading, however.

We wish to congratulate the SpaceX Crew-1 astronauts for their 
successful arrival at the ISS.


GRB_name: GRB201116A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28916
SUBJECT: GRB 201116A: Swift-XRT afterglow detection
DATE:    20/11/17 08:48:42 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), 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
Fermi/LAT-detected burst GRB 201116A (Axelsson et al. GCN Circ. 28907)
in a series of observations tiled on the sky. The total exposure time
is 4.8 ks, distributed over 3 tiles; the maximum exposure at a single
sky location was 3.1 ks. The data were collected between T0+46.5 ks and
T0+62.3 ks, and are entirely in Photon Counting (PC) mode. 

Four uncatalogued X-ray sources are detected, of which one ("Source 3")
is above the RASS 3-sigma upper limit at this position, and shows
signes of fading, and is therefore likely the GRB afterglow. Using 2405
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 = 149.32493, +0.27586 which is equivalent
to:

RA (J2000): 09h 57m 17.98s
Dec(J2000): +00d 16' 33.1"

with an uncertainty of 2.5 arcsec (radius, 90% confidence). This
position is 2.4 arcmin from the Fermi/LAT position.  As already
reported by de Ugarte Postigo et al (GCN Circ. 28915), there is an
optical afterglow counterpart consistent with this X-ray object. The
light curve is consistent with a constant source of mean count rate
5.2e-02 ct/sec, however fading also cannot be ruled out. A power-law
fit gives an index of 1.6 (+1.4, -2.0), thus the large uncertainties
hinder a confident statement about fading.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.6, -0.5). The
best-fitting absorption column is  2.7 (+2.5, -1.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.8 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.2 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+2.5, -1.9) x 10^21 cm^-2
Galactic foreground: 2.8 x 10^20 cm^-2
Excess significance: 2.1 sigma
Photon index:      1.9 (+0.6, -0.5)

The results of the XRT-team automatic analysis of the afterglow are at:
https://www.swift.ac.uk/xrt_products/00021040.

The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00095.

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


GRB_name: GRB201116A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28917
SUBJECT: GRB 201116A: NOT optical observations
DATE:    20/11/17 11:25:52 GMT
FROM:    Daniele B Malesani at DTU Space  <malesani@space.dtu.dk>

Z.P. Zhu (NAOC, HUST), D. B. Malesani (DTU Space), D. Xu (NAOC), A. de 
Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), L. Izzo (DARK/NBI), P. Galindo 
(NOT), report on behalf of a larger collaboration:

On 2020 Nov 17, we observed the afterglow (de Ugarte Postigo et al., GCN 
28915; Tohuvavohu  et al., GCN 28916) of GRB 201116A, detected by 
Fermi/GBM and Fermi/LAT (Axelsson et al., GCN 28907), using the Nordic 
Optical Telescope (NOT) equipped with the ALFOSC camera. We obtained one 
and three 300-s images in the r and z bands, respectively.

An optical source is detected in both filters, respectively, being 
consistent with the reported OSN position as well as with the Swift/XRT 
position. Preliminary photometry results are as follows:

     T_start          T_mid   Exptime  Filter   Mag   MagErr
      (UT)            (day)   (s)
2020-11-17T04:33:15  1.157   1x300    sdss-r   23.18 0.20
2020-11-17T04:38:51  1.165   3x300    sdss-z   22.50 0.27

calibrated against nearby PS1 stars. Our observations confirm the 
presence of the source, which is a clear afterglow candidate, though the 
photometric error and short time difference do not allow to establish 
variability compared to the OSN measurement (de Ugarte Postigo et al., 
GCN 28915).


GRB_name: GRB201116A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28920
SUBJECT: Konus-Wind detection of GRB 201116A
DATE:    20/11/18 13:18:10 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 long-duration GRB 201116A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 28897,
Kunzweiler et al., GCN Circ. 28898;
Fermi-LAT detection: Axelsson et al., GCN Circ. 28907)
triggered Konus-Wind at T0=2988.982 s UT (00:49:48.982).

The burst light curve shows a multipeaked structure
which starts at ~T0-1.3 s and has a total duration of ~9.5 s.
The emission is seen up to ~4 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB201116_T02988/

As observed by Konus-Wind, the burst
had a fluence of 2.46(-0.34,+0.33)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.792 s,
of 9.01(-2.15,+2.14)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+7.680 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.53(-0.23,+0.25),
the high energy photon index beta = -2.56(-0.69,+0.23),
the peak energy Ep = 220(-28,+40) keV
(chi2 = 90/97 dof).

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


GRB_name: GRB201116A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28923
SUBJECT: GRB 201116A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/11/19 09:01:00 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

N. Cannady (GSFC/UMBC),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The bright GRB 201116A (Fermi GBM Final Real-time Localization: The Fermi
GBM team, GCN Circ. 28897; BALROG localization: Kunzweiler et al.,
GCN Circ. 28898; Fermi-LAT detection: Axelsson and Ohno, GCN Circ. 28907;
Konus-Wind detection: Ridnaia et al., GCN Circ. 28920;
https://gcn.gsfc.nasa.gov/other/201116A.gcn3) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 00:49:45.039 UTC on 16 November 2020
(http://cgbm.calet.jp/cgbm_trigger/flight/1289522797/).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked pulse which starts at T+2.6
sec, peaks at T+7.9 sec, and ends at T+12.4 sec. The T90 and T50 durations
measured by the SGM data are 6.5 +- 0.6 sec and 3.0 +- 0.4 sec (40-1000
keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1289522797/

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


GRB_name: GRB201103B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28925
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): correction to the GCN #28883 CrAO/ZTSh optical observations
DATE:    20/11/19 23:02:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

Below is a correction of the photometry reported in GCN 28883 after 
CrAO/ZTSh optical observations on Nov., 13 (UT) 22:58:04.

Preliminary photometry of the afterglow is following
Date       UT start  t-T0     Filter Exp.    OT    Err.   UL.
                      (mid, days)      (s)

2020-11-13 22:58:04 10.21897    R    24*120  22.45 0.14   23.6

The photometry is based on the same stars used in GCNs 28862, 28875, 28883.

We apologize for a possible confusion after erroneously reported 
photometry in GCN 28883.


GRB_name: GRB201103B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28926
SUBJECT: ZTF20acozryr/AT2020yxz (GRB 201103B): SAO RAS optical observations
DATE:    20/11/20 09:52:20 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

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

We observed the field of the ZTF20acozryr/AT2020yxz (Coughlin et al.,
GCN  28841) associated with the GRB 201103B (Ursi et al., GCN 28831;
Svinkin et al., GCNs 28844, 28872; Evans et al., GCN 28858)
with Zeiss-1000 telescope of SAO RAS equipped with CCD photometer
on November 14, 20:58:48 -- 23:02:42 UT, t_mid - T0 = 11.1625 days.
We obtained 8 x 300 sec. images in Rc band.

The OT (Coughlin et al., GCN  28841; Xu  et al., GCNs 28846, 28847;
Zhu et al., GCN 28854; Evans et al., GCN 28858; Mao et al.,
GCNs 28861, 28863; Belkin et al., GCNs 28862, 28875, 28883, 28886;
Sharma et al., GCN 28876; Paek et al., GCN 28880; Volnova et al.,
GCN 28925) is clearly detected in the stacked image with the
brightness of R = 22.8 +/- 0.2. This preliminary photometry is
based on R2 magnitudes of nearby USNO-B1 stars.


GRB_name: GRB201120A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28932
SUBJECT: GRB 201120A: Fermi GBM Final Localization
DATE:    20/11/20 22:16:18 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 09:38:50 UT on 20 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201120A (trigger 627557935 / 201120402).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 277.7, Dec = 19.5 (J2000 degrees, equivalent to J2000 18h 31m, +19d 30'), with a statistical uncertainty of 15.6 degrees.

The angle from the Fermi LAT boresight is 97.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201120402/quicklook/glg_skymap_all_bn201120402.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/bn201120402/quicklook/glg_healpix_all_bn201120402.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201120402/quicklook/glg_lc_medres34_bn201120402.gif


GRB_name: GRB201120B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28933
SUBJECT: GRB 201120B: Fermi GBM Final Localization
DATE:    20/11/20 22:21:08 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 10:35:49.07 UT on 20 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201120A (trigger 627561354 / 201120442).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 78.2, Dec = -57.7 (J2000 degrees, equivalent to J2000 5h 13m, -57d 42'), with a statistical uncertainty of 15.2 degrees.

The angle from the Fermi LAT boresight is 26.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201120442/quicklook/glg_skymap_all_bn201120442.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/bn201120442/quicklook/glg_healpix_all_bn201120442.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201120442/quicklook/glg_lc_medres34_bn201120442.gif


GRB_name: GRB201120B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28934
SUBJECT: Fermi GRB 201120B: Global MASTER-Net observations report 
DATE:    20/11/20 23:45:09 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),

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 201120B ( Fermi GBM team, GCN 28933) errorbox  2525 sec after notice time and 36327 sec after trigger time at 2020-11-20 20:41:16 UT, with upper limit up to  21.0 mag. The observations began at zenith distance = 24 deg. The sun  altitude  is -32.5 deg. 

The galactic latitude b = -36 deg., longitude l = 266 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1486357

We obtain a following upper limits.  

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

   36417 | 2020-11-20 20:41:16 |         MASTER-SAAO | (03h 29m 13.76s , -50d 03m 39.9s) |   C |   180 | 20.6 |        
   36417 | 2020-11-20 20:41:16 |         MASTER-SAAO | (03h 27m 55.01s , -50d 04m 02.4s) |   C |   180 | 21.0 |        
   37016 | 2020-11-20 20:51:15 |         MASTER-SAAO | (03h 29m 17.44s , -50d 03m 25.9s) |   C |   180 | 20.6 |        
   37016 | 2020-11-20 20:51:15 |         MASTER-SAAO | (03h 27m 58.46s , -50d 03m 48.2s) |   C |   180 | 20.9 |        
   40569 | 2020-11-20 21:50:28 |         MASTER-SAAO | (03h 44m 24.56s , -48d 02m 26.7s) |   C |   180 | 20.3 |        
   40569 | 2020-11-20 21:50:28 |         MASTER-SAAO | (03h 43m 08.88s , -48d 02m 57.6s) |   C |   180 | 20.5 |        
   40769 | 2020-11-20 21:53:48 |         MASTER-SAAO | (04h 21m 31.88s , -46d 01m 43.8s) |   C |   180 | 20.3 |        
   40769 | 2020-11-20 21:53:48 |         MASTER-SAAO | (04h 20m 18.73s , -46d 02m 16.7s) |   C |   180 | 20.5 |        
   41169 | 2020-11-20 22:00:28 |         MASTER-SAAO | (03h 44m 25.03s , -48d 03m 15.9s) |   C |   180 | 19.6 |        
   41169 | 2020-11-20 22:00:28 |         MASTER-SAAO | (03h 43m 09.41s , -48d 03m 48.5s) |   C |   180 | 19.8 |        
   41370 | 2020-11-20 22:03:48 |         MASTER-SAAO | (04h 21m 32.38s , -46d 02m 51.0s) |   C |   180 | 17.0 |        
   41370 | 2020-11-20 22:03:48 |         MASTER-SAAO | (04h 20m 19.31s , -46d 03m 24.6s) |   C |   180 | 17.2 |        
   41770 | 2020-11-20 22:10:28 |         MASTER-SAAO | (03h 58m 32.69s , -46d 02m 20.4s) |   C |   180 | 16.9 |        
   41770 | 2020-11-20 22:10:28 |         MASTER-SAAO | (03h 57m 19.68s , -46d 02m 54.0s) |   C |   180 | 17.1 |        
   42449 | 2020-11-20 22:21:47 |         MASTER-SAAO | (03h 58m 35.28s , -46d 03m 51.4s) |   C |   180 | 17.5 |        
   42449 | 2020-11-20 22:21:47 |         MASTER-SAAO | (03h 57m 22.36s , -46d 04m 24.3s) |   C |   180 | 17.6 |        
   42648 | 2020-11-20 22:25:07 |         MASTER-SAAO | (04h 12m 01.44s , -44d 01m 57.1s) |   C |   180 | 17.8 |        
   42648 | 2020-11-20 22:25:07 |         MASTER-SAAO | (04h 10m 50.90s , -44d 02m 30.9s) |   C |   180 | 18.0 |        
   42848 | 2020-11-20 22:28:27 |         MASTER-SAAO | (04h 19m 11.18s , -50d 02m 56.4s) |   C |   180 | 17.2 |        
   42848 | 2020-11-20 22:28:27 |         MASTER-SAAO | (04h 17m 52.33s , -50d 03m 28.6s) |   C |   180 | 17.4 |        
   43048 | 2020-11-20 22:31:46 |         MASTER-SAAO | (03h 50m 37.41s , -54d 02m 54.3s) |   C |   180 | 17.7 |        
   43048 | 2020-11-20 22:31:46 |         MASTER-SAAO | (03h 49m 11.48s , -54d 03m 25.0s) |   C |   180 | 17.8 |        
   43248 | 2020-11-20 22:35:06 |         MASTER-SAAO | (04h 11m 58.86s , -44d 02m 46.0s) |   C |   180 | 18.5 |        
   43248 | 2020-11-20 22:35:06 |         MASTER-SAAO | (04h 10m 48.31s , -44d 03m 19.0s) |   C |   180 | 18.8 |        
   43388 | 2020-11-20 22:38:26 |         MASTER-SAAO | (04h 05m 35.65s , -54d 58m 07.2s) |   C |    60 | 17.5 |        
   43388 | 2020-11-20 22:38:26 |         MASTER-SAAO | (04h 04m 07.77s , -54d 58m 38.0s) |   C |    60 | 17.6 |        
   43468 | 2020-11-20 22:39:46 |         MASTER-SAAO | (04h 04m 13.81s , -54d 59m 41.8s) |   V |    60 | 17.4 |        
   44367 | 2020-11-20 22:54:46 |         MASTER-SAAO | (04h 03m 52.20s , -54d 58m 30.4s) |   C |    60 | 17.4 |        
   44367 | 2020-11-20 22:54:46 |         MASTER-SAAO | (04h 02m 24.79s , -54d 59m 01.0s) |   C |    60 | 17.4 |        
   44447 | 2020-11-20 22:56:06 |         MASTER-SAAO | (04h 03m 45.90s , -54d 59m 30.1s) |   B |    60 | 17.1 |        
   44447 | 2020-11-20 22:56:06 |         MASTER-SAAO | (04h 02m 18.03s , -54d 59m 57.1s) |   V |    60 | 17.3 |        
   45785 | 2020-11-20 23:17:24 |         MASTER-SAAO | (04h 30m 40.58s , -48d 03m 30.6s) |   C |   180 | 15.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201121A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28935
SUBJECT: GRB 201121A: Fermi GBM Final Real-time Localization
DATE:    20/11/21 01:40:04 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 01:29:49 UT on 21 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201121A (trigger 627614994.006474 / 201121062).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 210.8, Dec = -27.9 (J2000 degrees, equivalent to J2000 14h 03m, -27d 53'), with a statistical uncertainty of 2.6 degrees.

The angle from the Fermi LAT boresight is 77.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201121062/quicklook/glg_skymap_all_bn201121062.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/bn201121062/quicklook/glg_healpix_all_bn201121062.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201121062/quicklook/glg_lc_medres34_bn201121062.gif


GRB_name: GRB201121A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28936
SUBJECT: GRB 201121A: BALROG localization (Fermi Trigger 627614994 / GRB 201121062)
DATE:    20/11/21 01:49:50 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
627614994 at 01:29:49 on 21 Nov. 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) = 212.11+/-1.14 deg
Decl.(2000.0) = -25.44+/-1.07 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201121062/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201121062/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201121062/json    


GRB_name: GRB201121B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28937
SUBJECT: GRB 201121B: Fermi GBM Final Real-time Localization
DATE:    20/11/21 03:18:02 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 03:07:45 UT on 21 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201121B (trigger 627620870.546802 / 201121130).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 234.9, Dec = -38.9 (J2000 degrees, equivalent to J2000 15h 39m, -38d 53'), with a statistical uncertainty of 6.0 degrees.

The angle from the Fermi LAT boresight is 101.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201121130/quicklook/glg_skymap_all_bn201121130.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/bn201121130/quicklook/glg_healpix_all_bn201121130.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201121130/quicklook/glg_lc_medres34_bn201121130.gif


GRB_name: GRB201121A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28938
SUBJECT: Fermi GRB 201121A: Global MASTER-Net observations report 
DATE:    20/11/21 04:30:09 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),

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 201121A ( Fermi GBM team, GCN 28935) errorbox  663 sec after notice time and 719 sec after trigger time at 2020-11-21 01:41:48 UT, with upper limit up to  16.9 mag. The observations began at zenith distance = 84 deg. The sun  altitude  is -19.8 deg. 

The galactic latitude b = 32 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=1486547

We obtain a following upper limits.  

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

     790 | 2020-11-21 01:41:48 |         MASTER-SAAO | (13h 47m 06.60s , -27d 51m 18.4s) |   C |   140 | 16.9 |        
     964 | 2020-11-21 01:44:28 |         MASTER-SAAO | (13h 47m 11.79s , -27d 51m 18.3s) |   C |   170 | 16.9 |        
    1159 | 2020-11-21 01:47:37 |         MASTER-SAAO | (13h 47m 06.55s , -27d 49m 47.6s) |   C |   180 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201015A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28939
SUBJECT: GRB 201015A radio afterglow with e-MERLIN
DATE:    20/11/21 09:28:54 GMT
FROM:    Stefano Giarratana at University of Bologna  <s.giarratana@ira.inaf.it>

S. Giarratana (Univ. of Bologna, INAF/IRA), M. Giroletti (INAF/IRA),
B. Marcote (JIV-ERIC), G. Ghirlanda (INAF/OABrera),
M. RibÃ³ (Univ. of Barcelona), J.M. Paredes (Univ. of Barcelona)

On UT 2020 November 5 and 8 we observed the radio counterpart of the
GRB 201015A (Dâ€™Elia V. et al., GCN Circ. 28632) with e-MERLIN at 5 GHz.
We detect a point-like source at a position consistent with the VLA
GRB 201015A afterglow coordinates (RA(J2000) = 23:37:16.41,
Dec(J2000)= +53:24:56.4, Fong W. et al., GCN Circ. 28688).

Preliminary analysis indicates a significance of the detection of 4.5
and 3.3 sigma confidence for November 5 and 8 observations respectively.
We note that the noise level in the November 8 observation is 20% higher
than on November 5.

Additional radio observations are in progress.

We would like to thank the e-MERLIN personnel for approving, executing,
and processing these observations.


GRB_name: GRB201015A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28945
SUBJECT: GRB 201015A L-band observations with e-MERLIN
DATE:    20/11/23 10:44:45 GMT
FROM:    Lauren Rhodes at Oxford  <lauren.rhodes@physics.ox.ac.uk>

L. Rhodes, R. Fender (Oxford), J. Bray and D.R.A. Williams (JBCA) report:


e-MERLIN observed the position of GRB 201015A (D'Elia et al., GCN Circ. 28632) at 1.5GHz at 19 and 23 days post burst. Both epochs show a point source with coordinates consistent with those from the VLA detection (Fong et al., GCN Circ. 28688). The flux densities of the detections are 214+/-25uJy and 256+/-27uJy for epochs 1 and 2, respectively. We tentatively attribute the observed emission to the GRBs host galaxy as there is very little variation in the flux density between our two epochs. There is also no significant variation between our detections and that from Fong et al., when using an optically thin spectrum to scale between the two observing bands.


We are in the process of obtaining further radio observations.


We thank the e-MERLIN staff for the time allocation and their assistance with the observations.


GRB_name: GRB201122A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28948
SUBJECT: GRB 201122A: Insight-HXMT/HE detection
DATE:    20/11/24 02:41:51 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, C. Zheng, C. Cai, J. C. Liu, Q. Luo,  
S. Xiao, W. C. Xue, Q. B. Yi, Y. Huang, C. K. Li, 
G. Li, X. B. Li, J. Y. Liao, X. Y. Song, 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 2020-11-22T08:32:01.000 (T0), Insight-HXMT/HE detected 
GRB 201122A (trigger ID: HEB201122355) in a routine search of the data, 
which also triggered INTEGRAL.

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 11.68 s measured from T0+0.69 s. 
The 1-ms peak rate, measured from T0+0.65 s, is 863 cnts/sec. 
The total counts from this burst is 2964 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB201122355_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: GRB200826A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28949
SUBJECT: GRB 200826A: TNG and LBT constraints on a supernova bump
DATE:    20/11/24 10:54:35 GMT
FROM:    Andrea Rossi at INAF  <andrea.rossi@inaf.it>

A. Rossi (INAF-OAS), P. D'Avanzo (INAF-OAB), V. D'Elia (ASI-SSDC), A. 
Melandri (INAF-OAB) and E.Palazzi (INAF-OAS) on behalf of the CIBO 
collaboration, and B. Rothberg (LBTO/GMU), O. Kuhn, C. Veillet (LBTO) 
report:

We searched for a supernova bump associated to ZTF20abwysqy/AT2020scz 
(Ahumada et al. GCN 28295), the afterglow of GRB 200826A (Fermi, GCN 
28284; Ridnaia et al., GCN 28294), which energetics are consistent with 
being a long/soft event (Svinkin et al., GCN 28301).

We obtained two series of r-sdss images with the Italian 3.6m TNG 
telescope equipped with DOLORES. The first set consists in a series of 
13 x 240 s obtained on 2020-09-27 at a midtime 02:01 UT (~32 days after 
the burst). A second set of 26x200 s of exposure time each have been 
obtained on 2020-11-09.
Another two series of r-sdss images have been obtained with the MODS 
double imager and spectrographs mounted on LBT. Both series consists of 
13x180 sec r-band images with the MODS double imager and spectrographs 
mounted on LBT and otained on 2020-09-28 and 2020-11-13.

Image subtraction between the two TNG observing epochs and between the 
two LBT/MODS observing epochs using HOTPANTS (v5.1.11) does not reveal 
the source found by Ahumada et al. (GCN 28727) and constrain the 
presence of a SN bump beyond the conservative 5 sigma limit of r>25 in 
both TNG and LBT first epochs. Assuming that the supernova responsible 
for the bump detected by Ahumada et al. is similar to SN1998bw, at the 
redshift of GRB 200826A z=0.748 (Rothberg et al., GCN 28319) its 
brightness would be r~24.8, that includes the foreground Galactic 
extinction on the line of sight of GRB 200826A (A_V=0.184; Schlafly & 
Finkbeiner 2011). Our non detection then might indicate that the 
supernova detected by Ahumada et al. was at least 10% faster and/or 
fainter than SN1998bw.

At the position of the afterglow we clearly detect the host galaxy of 
GRB 200826A, for which we report r=23.33+-0.09 in all observations, 
calibrated against SDSS field stars.

We acknowledge the excellent support from the TNG staff, in particular 
W. Boschin, and the LBTO and LBT-INAF staff, particularly A. Cardwell, 
F. Cusano, S. Paiano and D. Paris, in obtaining these observations.


GRB_name: GRB201121A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28954
SUBJECT: GRB 201121A: Insight-HXMT/HE detection
DATE:    20/11/26 15:32:16 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, C. Zheng, C. Cai, J. C. Liu, Q. Luo,  
S. Xiao, W. C. Xue, Q. B. Yi, Y. Huang, C. K. Li, 
G. Li, X. B. Li, J. Y. Liao, X. Y. Song, 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 2020-11-21T01:29:49.01 (T0), Insight-HXMT/HE detected 
GRB 201121A (trigger ID: HEB201121062) in a routine search of the data, 
which also triggered Fermi/GBM (Fermi GBM team, GCN #28935).

The Insight-HXMT/HE light curve mainly consists of a single 
pulse with a duration (T90) of 5.47 s measured from T0-0.84 s. 
The 1-ms peak rate, measured from T0+0.30 s, is 487 cnts/sec. 
The total counts from this burst is 2001 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB201121062_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 (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: GRB201128A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28958
SUBJECT: GRB 201128A: Swift detection of a burst
DATE:    20/11/28 06:44:21 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Y. Lien (GSFC/UMBC), E. Ambrosi (INAF-IASFPA),
A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and
M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Neil Gehrels
Swift Observatory Team:

At 06:27:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201128A (trigger=1009679).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 223.136, +26.678 which is 
   RA(J2000) = 14h 52m 33s
   Dec(J2000) = +26d 40' 41"
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 ~600 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 06:30:04.8 UT, 126.6 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 223.1083, 26.6844 which
is equivalent to:
   RA(J2000)  = 14h 52m 26.00s
   Dec(J2000) = +26d 41' 03.8"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 92 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.53
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 130 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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 0.03. 

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: GRB201128A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28959
SUBJECT: GRB 201128A: DDOTI Observations 
DATE:    20/11/28 15:11:50 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Simone Dichiara
(GSFC/UMD), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), OcÃ©lotl Lopez
(UNAM), Diego Gonzalez (UNAM), Margarita Pereyra (UNAM), Srihari Ravi (ASU), and
Eleonora Troja (GSFC/UMD) report:

We observed the field of GRB 201128A (Lien et al., GCN Circ. 28958) with with
the DDOTI/OAN wide-field imager at the Observatorio AstronÃ³mico Nacional on
Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) on the night of
2020-11-28 UTC.

We observed from 2020-11-30 12:45 to 13:07 (from 6.3 to 6.7 hours after the
trigger) obtaining a total of 960 seconds exposure in the w filter. We calibrate
our images against the APASS catalog. Our 5-sigma limiting magnitude is w =
20.4.

Comparing our observations to the USNO-B1 and PanSTARRS PS1 DR2 catalogs, we
detect no uncatalogued sources in the Swift/XRT error region (Lien et al., GCN
Circ. 28958 to our 5-sigma limit.

We thank the staff of the Observatorio Astronomico Nacional in San Pedro Martir.


GRB_name: GRB201128A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28960
SUBJECT: GRB 201128A: Enhanced Swift-XRT position
DATE:    20/11/28 15:58:08 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 1017 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 201128A, 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 = 223.10767, +26.68502 which is equivalent
to:

RA (J2000): 14h 52m 25.84s
Dec (J2000): +26d 41' 06.1"

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: GRB201128A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28962
SUBJECT: GRB 201128A: Swift-XRT refined Analysis
DATE:    20/11/28 22:44:04 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 9.4 ks of XRT data for GRB 201128A (Lien et al. GCN
Circ. 28958), from 133 s to 46.1 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Evans et al. (GCN Circ. 28960).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.58 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.09 (+0.23, -0.21). The
best-fitting absorption column is  1.6 (+0.7, -0.6) x 10^21 cm^-2, in
excess of the Galactic value of 3.5 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 3.3 x 10^-11 (4.0 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 3.5 x 10^20 cm^-2
Excess significance: 3.4 sigma
Photon index:      2.09 (+0.23, -0.21)

If the light curve continues to decay with a power-law decay index of
0.58, the count rate at T+24 hours will be 0.014 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.6 x
10^-13 (5.5 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01009679.

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


GRB_name: GRB201128A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28963
SUBJECT: GRB 201128A: Swift-BAT refined analysis
DATE:    20/11/29 03:42:15 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@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), 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 201128A (trigger #1009679)
(Lien et al., GCN Circ. 28958).  The BAT ground-calculated position is
RA, Dec = 223.091, 26.716 deg which is
   RA(J2000)  =  14h 52m 21.9s
   Dec(J2000) = +26d 42' 58.6"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.

The BAT light curve showed a complex structure with a duration of about 30 sec.
T90 (15-350 keV) is 5.41 +- 3.22 sec (estimated error including systematics).

The time-averaged spectrum from T-0.44 to T+8.74 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.37 +- 0.37.  The fluence in the 15-150 keV band is 2.0 +- 0.4 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+4.21 sec in the 15-150 keV band
is 0.4 +- 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/1009679/BA/


GRB_name: GRB201130A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28965
SUBJECT: GRB 201130A: Fermi GBM Final Real-time Localization
DATE:    20/11/30 05:41:09 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 05:30:49 UT on 30 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201130A (trigger 628407054.55185 / 201130230).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 165.9, Dec = 29.6 (J2000 degrees, equivalent to J2000 11h 03m, 29d 36'), with a statistical uncertainty of 21.2 degrees.

The angle from the Fermi LAT boresight is 108.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201130230/quicklook/glg_skymap_all_bn201130230.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/bn201130230/quicklook/glg_healpix_all_bn201130230.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201130230/quicklook/glg_lc_medres34_bn201130230.gif


GRB_name: GRB201130A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28966
SUBJECT: Fermi GRB 201130A: Global MASTER-Net observations report 
DATE:    20/11/30 05:45:16 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),

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 201130A ( Fermi GBM team, GCN 28965) errorbox  197 sec after notice time and 205 sec after trigger time at 2020-11-30 05:34:15 UT, with upper limit up to  17.5 mag. The observations began at zenith distance = 15 deg. The sun  altitude  is -26.4 deg. 

The galactic latitude b = 67 deg., longitude l = 201 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1492996

We obtain a following upper limits.  

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

     236 | 2020-11-30 05:34:15 |          MASTER-IAC | (10h 16m 57.83s , +32d 07m 21.5s) |   C |    60 | 17.4 |        
     315 | 2020-11-30 05:35:34 |          MASTER-IAC | (10h 31m 08.69s , +34d 06m 38.7s) |   C |    60 | 17.5 |        
     395 | 2020-11-30 05:36:54 |          MASTER-IAC | (10h 35m 48.60s , +32d 06m 44.9s) |   C |    60 | 17.4 |        
     475 | 2020-11-30 05:38:14 |          MASTER-IAC | (10h 26m 55.79s , +36d 07m 37.0s) |   C |    60 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201130A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28967
SUBJECT: GRB 201130A: DDOTI Observations 
DATE:    20/11/30 16:25:05 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Margarita Pereyra (UNAM), Nat Butler (ASU), Rosa L.
Becerra (UNAM), Simone Dichiara (GSFC/UMD), Alexander Kutyrev (GSFC/UMD),
William H. Lee (UNAM), OcÃ©lotl Lopez (UNAM), Diego Gonzalez (UNAM), Srihari Ravi
(ASU), and Eleonora Troja (GSFC/UMD) report:

We observed the field of the Fermi/GBM likely short GRB 201130A (Fermi GBM Team,
GCN Circ. 28965) with the DDOTI/OAN wide-field imager at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx)
from 2020-11-30 07:56 UTC to 13:09 UTC (from 2.4 to 7.7 hours after the trigger)

We observed a region covering 20.4 degrees in RA and 20.4 degrees in declination
(about 416 square degrees) centered on 10:28:57.60 +31:59:24.0 (J2000). We
obtained between 1020 and 1620 seconds exposure in the w filter. We calibrated
our images against the APASS catalog. Our 10-sigma limiting magnitudes vary from
w = 17.8 to 19.3.

Compared to the USNO-B1, DSS DR2 and Pan-STARRS DR1 catalogs, we detect no
uncataloged sources to our 10-sigma limit.

We thank the staff of the Observatorio Astronomico Nacional in San Pedro Martir.


GRB_name: GRB201128A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28970
SUBJECT: GRB 201128A: Swift/UVOT Upper Limits
DATE:    20/11/30 23:24:56 GMT
FROM:    Alexander Belles at PSU/Swift  <aub1461@psu.edu>

GRB 201128A: Swift/UVOT Upper Limits

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

The Swift/UVOT began settled observations of the field of GRB 201128A
130 s after the BAT trigger (Lien et al., GCN Circ. 28958).
No optical afterglow consistent with the XRT position
(Lien et al. GCN Circ. 28958)
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) exposures and subsequent exposures are:

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

white_FC           130          280          147         >20.0
u_FC               289          538          246         >19.3
white              130          761          186         >20.0
v                  619          639           19         >17.4
b                  544          737           39         >18.6
u                  289          538          246         >19.3
w1                 668          688           19         >18.3

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: GRB201128B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28971
SUBJECT: GRB 201128B: Swift/BAT-GUANO detection and arcminute localization
DATE:    20/11/30 23:46:57 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

James DeLaunay (PSU), Aaron Tohuvavohu (U Toronto), Jamie Kennea (PSU) report:

Swift/BAT did not trigger on GRB 201128B (T0: 2020-11-28 17:54:11 UTC,
Fermi/GBM TRIGGER 628278856).

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

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

The burst is detected in BAT with a duration of ~15 seconds. This was
a weak and slow burst that occurred during a rapid part of a Swift
slew. The position of the burst was found with a novel and
uncalibrated slew image mosaicing procedure, and so the positional
uncertainty is not yet well characterized.


The BAT position is
RA, Dec = 339.354, -49.246 deg which is
   RA(J2000)  = 22h 37m 24.96s
   Dec(J2000) =  -49d 14â€™ 45.6â€
with an estimated uncertainty of at least 5 arcmin.

This position is consistent with the Fermi GBM localization
(https://gcn.gsfc.nasa.gov/other/628278856.fermi).

XRT and UVOT follow-up has been requested. Results of follow-up
observations will be reported in future circulars.

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

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


GRB_name: GRB201201A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28972
SUBJECT: GRB 201201A: Fermi GBM Final Real-time Localization
DATE:    20/12/01 03:03:37 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 02:52:14 UT on 1 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201201A (trigger 628483939.910616 / 201201120).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 307.5, Dec = 20.8 (J2000 degrees, equivalent to J2000 20h 30m, 20d 48'), with a statistical uncertainty of 8.8 degrees.

The angle from the Fermi LAT boresight is 122.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201201120/quicklook/glg_skymap_all_bn201201120.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/bn201201120/quicklook/glg_healpix_all_bn201201120.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201201120/quicklook/glg_lc_medres34_bn201201120.gif


GRB_name: GRB201128B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28974
SUBJECT: GRB 201128B: Swift ToO observations
DATE:    20/12/01 14:14:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Swift/BAT GRB 201128B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021044

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: GRB201201A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28975
SUBJECT: Fermi GRB 201201A: Global MASTER-Net observations report 
DATE:    20/12/01 15:30:16 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),

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 201201A ( Fermi GBM team, GCN 28972) errorbox  44316 sec after notice time and 44327 sec after trigger time at 2020-12-01 15:11:02 UT, with upper limit up to  17.1 mag. Observations started at twilight.  The observations began at zenith distance = 30 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = -11 deg., longitude l = 64 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1493496

We obtain a following upper limits.  

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

   44358 | 2020-12-01 15:11:02 |      MASTER-Tavrida | (20h 35m 25.58s , +21d 59m 09.7s) |   C |    60 | 17.1 |        
   44644 | 2020-12-01 15:15:49 |      MASTER-Tavrida | (20h 35m 59.02s , +20d 00m 37.3s) |   C |    60 | 15.7 |        
   44725 | 2020-12-01 15:17:09 |      MASTER-Tavrida | (20h 35m 18.93s , +21d 59m 49.8s) |   C |    60 | 16.0 |        
   44805 | 2020-12-01 15:18:30 |      MASTER-Tavrida | (20h 43m 56.87s , +22d 00m 54.7s) |   C |    60 | 16.1 |        
   44900 | 2020-12-01 15:20:05 |      MASTER-Tavrida | (20h 22m 03.16s , +21d 55m 31.5s) |   C |    60 | 15.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201201A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28976
SUBJECT: GRB 201201A: DDOTI Observations 
DATE:    20/12/01 17:55:19 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Rosa L. Becerra (UNAM), Simone Dichiara
(GSFC/UMD), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), OcÃ©lotl Lopez
(UNAM), Diego Gonzalez (UNAM), Margarita Pereyra (UNAM), Srihari Ravi (ASU), and
Eleonora Troja (GSFC/UMD) report:

We observed the field of the Fermi/GBM likely long GRB 201201A (Fermi GBM Team,
GCN Circ. 28972) with the DDOTI wide-field imager at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx)
from 2020-12-01 02:56 UTC to 03:39 UTC (from 4.4 to 47.2 minutes after the
trigger).

We observed a region covering 20.4 degrees in RA and 20.4 degrees in declination
(about 416 square degrees) centered on 19:23:21.60 +16:54:36.0 (J2000). We
obtained between 120 and 360 seconds of exposure in the w filter. We calibrated
our images against the APASS catalog. Our 10-sigma limiting magnitudes vary from
w = 16.4 to 18.2.

Compared to the USNO-B1, Pan-STARRS DR1, and APASS DR10 catalogs, we detect no
uncataloged sources to our 10-sigma limit.

We thank the staff of the Observatorio Astronomico Nacional in San Pedro Martir.


GRB_name: GRB201128B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28980
SUBJECT: GRB 201128B: Swift-XRT observations
DATE:    20/12/02 15:12:57 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@inaf.it>

M. Perri (ASDC), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Tohuvavohu
(U. Toronto), B. Sbarufatti (PSU), D.N. Burrows (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester) 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 201128B (James DeLaunay et al. GCN Circ.
28971), collecting 5.0 ks of Photon Counting (PC) mode data between
T0+246.0 ks and T0+303.8 ks. 

Ten 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):  339.4164  =  22:37:39.94
  Dec (J2000): -49.2698  =  -49:16:11.1
  Error: 5.1 arcsec (radius, 90% conf.)
  Count-rate: (3.32 [+1.13, -0.93])e-3 ct s^-1  
  Distance: 169 arcsec from Swift/BAT position.
  Flux: (1.67 [+0.57, -0.47])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 2:
  RA (J2000):  339.0250  =  22:36:5.99
  Dec (J2000): -49.1319  =  -49:07:54.7
  Error: 5.2 arcsec (radius, 90% conf.)
  Count-rate: (4.7 [+2.8, -2.0])e-3 ct s^-1   
  Distance: 876 arcsec from Swift/BAT position.

Source 4:
  RA (J2000):  339.5648  =  22:38:15.55
  Dec (J2000): -49.2141  =  -49:12:50.9
  Error: 7.7 arcsec (radius, 90% conf.)
  Count-rate: (2.35 [+1.05, -0.81])e-3 ct s^-1  
  Distance: 508 arcsec from Swift/BAT position.
  Flux: (7.8 [+3.5, -2.7])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 5:
  RA (J2000):  339.4267  =  22:37:42.42
  Dec (J2000): -49.1173  =  -49:07:02.2
  Error: 5.3 arcsec (radius, 90% conf.)
  Count-rate: (1.36 [+0.77, -0.57])e-3 ct s^-1  
  Distance: 494 arcsec from Swift/BAT position.
  Flux: (9.5 [+5.4, -4.0])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 6:
  RA (J2000):  339.2905  =  22:37:9.71
  Dec (J2000): -49.3858  =  -49:23:08.7
  Error: 5.1 arcsec (radius, 90% conf.)
  Count-rate: (6.6 [+2.0, -1.6])e-3 ct s^-1   
  Distance: 524 arcsec from Swift/BAT position.
  Flux: (1.69 [+0.50, -0.42])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 7:
  RA (J2000):  339.2768  =  22:37:6.43
  Dec (J2000): -49.1392  =  -49:08:21.0
  Error: 4.9 arcsec (radius, 90% conf.)
  Count-rate: (4.7 +/- 1.3)e-3 ct s^-1  
  Distance: 425 arcsec from Swift/BAT position.
  Flux: (2.03 +/- 0.55)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 8:
  RA (J2000):  339.2888  =  22:37:9.31
  Dec (J2000): -49.1961  =  -49:11:45.9
  Error: 7.2 arcsec (radius, 90% conf.)
  Count-rate: (2.17 [+0.97, -0.77])e-3 ct s^-1  
  Distance: 236 arcsec from Swift/BAT position.
  Flux: (1.84 [+0.83, -0.65])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 9:
  RA (J2000):  339.2747  =  22:37:5.92
  Dec (J2000): -49.1221  =  -49:07:19.5
  Error: 9.8 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (3.04 [+1.19, -0.95])e-3 ct s^-1  
  Distance: 483 arcsec from Swift/BAT position.
  Flux: (7.4 [+2.9, -2.3])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 10:
  RA (J2000):  339.5188  =  22:38:4.51
  Dec (J2000): -49.1801  =  -49:10:48.4
  Error: 6.9 arcsec (radius, 90% conf.)
  Count-rate: (1.89 [+0.94, -0.72])e-3 ct s^-1  
  Distance: 454 arcsec from Swift/BAT position.
  Flux: (3.0 [+1.5, -1.1])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 11:
  RA (J2000):  339.5043  =  22:38:1.04
  Dec (J2000): -49.3084  =  -49:18:30.2
  Error: 5.2 arcsec (radius, 90% conf.)
  Count-rate: (2.14 [+1.07, -0.81])e-3 ct s^-1  
  Distance: 418 arcsec from Swift/BAT position.
  Flux: (1.04 [+0.52, -0.39])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

A catalogued source was also detected.

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/00021044.

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


GRB_name: GRB201130A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28981
SUBJECT: GRB201130A: Zwicky Transient Facility Follow-Up of a Fermi Short GRB (Trigger 628407054)
DATE:    20/12/02 15:41:48 GMT
FROM:    Shreya Anand at GROWTH Caltech  <sanand@caltech.edu>

Simeon Reusch (DESY), Igor Andreoni (Caltech), Harsh Kumar (IITB), Tomas Ahumada (UMD), Varun Bhalerao (IITB), Shreya Anand (Caltech), Eric Bellm (UW), Michael Coughlin (UMN), Mansi Kasliwal (Caltech), Erik Kool (OKC), Ana Sagues Carracedo (OKC), Leo Singer (NASA/GSFC), and Robert Stein (DESY) on behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations:

We observed the localization region of the short GRB201130A (trigger 628407054) detected by the Gamma-Ray Burst Monitor (GBM) on the Fermi satellite with the Palomar 48 inch telescope equipped with the 47 square degree Zwicky Transient Facility (ZTF) camera. We obtained a series of g-band images covering about 400 square degrees beginning at 12:28 UT on 2020 Nov 30 (about 7 hours after the burst trigger time) for two consecutive nights. This corresponds to ~75% of the probability enclosed in the region of the GRB localization map that was unocculted by the Earth for the Fermi GBM (GCN 28965). Exposures reached a g-band median depth of 20.5 mag and 20.3 mag in the first and second night. The images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC (Masci et al. 2019).

We queried the ZTF alert stream using Kowalski (Duev et al. 2019) and AMPEL (Nordin et al. 2019). We required at least 2 detections separated by at least 15 minutes to select against moving objects. Furthermore, we cross-matched our candidates with the Minor Planet Center to flag known asteroids, reject stellar sources (Tachibana and Miller 2018), and apply machine learning algorithms (Duev et al. 2019, Mahabal et al. 2019). We require no spatially coincident ZTF alert to be issued before the detection time of the GBM trigger. 

We found no candidates consistent with a potential GRB counterpart within the localization region.

ZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia.
ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341.
GROWTH acknowledges generous support of the NSF under PIRE Grant No 1545949.
Alert distribution service provided by DIRAC@UW (Patterson et al. 2019).
Alert database searches are done by AMPEL (Nordin et al. 2019) and Kowalski (Duev et al. 2019).


GRB_name: GRB201203A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28985
SUBJECT: GRB 201203A: Swift detection of a burst
DATE:    20/12/03 07:10:00 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

S. Dichiara (NASA/GSFC/UMCP), C. Gronwall (PSU),
S. Laha (GSFC/UMBC/CRESST), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 06:52:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201203A (trigger=1010946).  
Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 38.080, -26.538 which is 
   RA(J2000) = 02h 32m 19s
   Dec(J2000) = -26d 32' 14"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of about 20 sec.  The peak count rate
was ~600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 06:54:27.2 UT, 120.0 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of  68 seconds with the White filter
starting 123 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 25% of
the BAT 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
BAT 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 S. Dichiara (dichiara AT umd.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB201203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28986
SUBJECT: GRB 201203A: FRAM-Auger optical limit
DATE:    20/12/03 08:09:11 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

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

report:

The 30 cm robotic telescope FRAM-Auger in Malargue
(Argentina) reacted robotically to the Swift/BAT alert
of GRB201203A (Dichiara et al., GCNC 28985), starting
with a series of 20 s unfiltered images at 06:54:04 UT,
i.e. 97 s post trigger.

We do not detect any new or strongly variable source at
or around the reported gamma-ray errorbox in single
frames or a combined 20 x 20 s image taken between 1.5
min and 12.5 min after the initial trigger. The
combined exposure has a limiting magnitude r'(AB) ~
17, as calibrated against the Atlas Catalogue.


GRB_name: GRB201203A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28987
SUBJECT: GRB 201203A: DDOTI Observations 
DATE:    20/12/03 08:54:12 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Simone Dichiara
(GSFC/UMD), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), OcÃ©lotl Lopez
(UNAM), Diego Gonzalez (UNAM), Margarita Pereyra (UNAM), Srihari Ravi (ASU), and
Eleonora Troja (GSFC/UMD) report:

We observed the field of the Swift/BAT GRB 201203A (Dichiara et al., GCN Circ.
28985) with the DDOTI wide-field imager at the Observatorio AstronÃ³mico Nacional
on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) from 2020-12-03
06:57 UTC to 08:31 UTC (from 5.5 to 99 minutes after the trigger).

We observed a region covering aproximately 7 degrees in RA and 10 degrees in
declination (about 70 square degrees), including the entire BAT uncertainty
region centered on 02:32:19.18 -26:32:15.0 (J2000). We obtained 4290 seconds of
exposure in the w filter at high airmass and with almost full Moon. We
calibrated our images against the APASS DR10 catalog. Our 5-sigma limiting
magnitudes is 19.9.

Compared to the USNO-B1, Pan-STARRS DR1, and APASS DR10 catalogs, we detect no
uncataloged sources to our 5-sigma limit in the BAT 90% uncertainty region. No
XRT detection is available at this moment.

We thank the staff of the Observatorio Astronomico Nacional in San Pedro Martir.


GRB_name: GRB201203A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28988
SUBJECT: GRB 201203A: KAIT Optical Upper Limit
DATE:    20/12/03 10:02:27 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

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

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 201203A (Dichiara et al.,
GCN 28985) starting at 06:54:43 UT, 136 s after the burst.
Observations were performed with an automatic sequence in the
clear (roughly R), V, and I filters, and the exposure time was 20 s
per image. We do not detect any optical afterglow candidate within
the BAT position error circle (Dichiara et al., GCN 28985),
neither in single image, nor in the co-add images.
The typical limiting magnitude of our single clear image is about
18.0 mag calibrated to the USNOB1.0 catalog.
Our observation is consistent with the non-detection reported by
other groups (Jelinek et al, GCN 28986; Watson et al., GCN 28987). ï»¿


GRB_name: GRB201203A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28990
SUBJECT: GRB 201203A: Swift-XRT afterglow detection
DATE:    20/12/03 15:11:51 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

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

Swift-XRT has observed GRB 201203A (Dichiara et al. GCN Circ. 28985),
collecting 2.8 ks of Photon Counting (PC) mode data between T0+4.7 ks
and T0+17.6 ks. 

One uncatalogued X-ray source is detected within the BAT error circle.
Using 857 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 = 38.05521, -26.51820 which is
equivalent to:

RA (J2000): 02h 32m 13.25s
Dec(J2000): -26d 31' 05.5"

with an uncertainty of 3.3 arcsec (radius, 90% confidence). This
position is 107 arcsec from the BAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.4 (+1.3, -1.1).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.7, -0.4). The
best-fitting absorption column is  consistent with the Galactic value
of 1.8 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.3 x 10^-11 (1.6 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.8 (+/-7.3) x 10^20 cm^-2
Galactic foreground: 1.8 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.9 (+0.7, -0.4)

If the light curve continues to decay with a power-law decay index of
1.4, the count rate at T+24 hours will be 3.4 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-14 (5.5 x 10^-15) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01010946.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/01010946.

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


GRB_name: GRB201203A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28991
SUBJECT: Swift GRB 201203A: Global MASTER-Net observations report 
DATE:    20/12/03 18:38:16 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),

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 201203A ( S. Dichiara et al., GCN 28985) errorbox  41763 sec after notice time and 41845 sec after trigger time at 2020-12-03 18:29:52 UT, with upper limit up to  17.6 mag. The observations began at zenith distance = 72 deg. The sun  altitude  is -46.7 deg. 

The galactic latitude b = -67 deg., longitude l = 217 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1494824

We obtain a following upper limits.  

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

   41936 |      MASTER-Tavrida |   C |   180 | 17.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201203A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28992
SUBJECT: GRB 201203A: MITSuME Okayama optical upper limits
DATE:    20/12/04 08:01:15 GMT
FROM:    Masafumi Niwano at Tokyo Institute of Tech  <niwano@hp.phys.titech.ac.jp>

M. Niwano, R. Hosokawa, K. L. Murata, R. Adachi, F. Ogawa, N. Nakamura,
N. Ito, 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 201203A (S. Dichiara et al.,GCN Circular 
#28985) with the optical three color (g', Rc, and Ic) CCD cameras 
attached to the MITSuME 50 cm telescope of Okayama Astrophysical 
Observatory, Okayama, Japan.
The observation started at 12:02:06 UT. We did not find any new point 
sources within the Swift-XRT circle ( V. D'Elia et al., GCN Circular 
#28990) in all three bands.
We obtained the 5-sigma limits as follows.
T0+[hour]  MID-UT  T-EXP[sec]  5-sigma limits
------------------------------------------------------------------------------------------------ 

6.9  13:45:28.19  9000  g'>17.9, Rc>18.6, Ic>17.7
------------------------------------------------------------------------------------------------ 

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., 10.1093/pasj/psaa091, arXiv:2008.11486; 
https://github.com/MNiwano/Eclaire).


GRB_name: GRB201203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28993
SUBJECT: GRB 201203A: GROWTH-India Telescope optical upper limit.
DATE:    20/12/04 15:32:31 GMT
FROM:    Harsh Kumar at Indian Inst of Tech,Bombay  <harshkosli13@gmail.com>

H. Kumar (IITB), P. Dorje (IAO), J. Stanzin (IAO), S. Joharle (Fergusson
College), K. Sharma (IITB), V. Bhalerao (IITB), G. C. Anupama (IIA), S.
Barway (IIA), report on behalf of the GROWTH-India collaboration:


We observed GRB 201203A reported by S. Dichiara et. al., (GCN 28985) with
0.7m GROWTH-India Telescope, starting at 2020-12-03T15:21:51.55 UT. We
obtained 25 images of 300 sec each in the r' filter. We did not detect any
new source within an uncertainty region of 3.3 arcseconds (radius, 90%
containment) around Swift-XRT position i.e., RA(J2000) = 02h 32m 13.25s,
Dec(J2000) = -26d 31' 05.5" (V. D'Elia et. al., GCN 28990).


We obtained the following upper limits:

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

 JD_Mid | T_mid-T0 (hrs) | Exposure(sec) | Filter | lim_Mag |

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

2459187.19431 | ~8.49 | 300*25 | r' | > 21.7 |

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

Magnitudes are in the AB system and are calibrated against PanSTARRs PS1
data release, (Flewelling et al., 2018).


The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).


GRB_name: GRB201203A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28995
SUBJECT: GRB 201203A: Swift-BAT refined analysis
DATE:    20/12/04 23:07:12 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), S. Dichiara (NASA/GSFC/UMCP),
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-239 to T+130 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 201203A (trigger #1010946)
(Dichiara et al., GCN Circ. 28985).  The BAT ground-calculated position is
RA, Dec = 38.055, -26.505 deg which is
   RA(J2000)  =  02h 32m 13.1s
   Dec(J2000) = -26d 30' 19.2"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 91%.

The BAT light curve showed a complex structure with a duration of about ~20 sec.
T90 (15-350 keV) is 12.18 +- 2.10 sec (estimated error including systematics).

The time-averaged spectrum from T-2.73 to T+12.84 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.78 +- 0.26.  The fluence in the 15-150 keV band is 2.9 +- 0.5 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+11.49 sec in the 15-150 keV band
is 0.5 +- 0.1 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/1010946/BA/


GRB_name: GRB201207A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28996
SUBJECT: GRB 201207A: Fermi GBM Final Real-time Localization
DATE:    20/12/07 23:37:17 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 23:26:55 UT on 7 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201207A (trigger 629076420.72719 / 201207977).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 124.1, Dec = -50.5 (J2000 degrees, equivalent to J2000 08h 16m, -50d 30'), with a statistical uncertainty of 2.4 degrees.

The angle from the Fermi LAT boresight is 120.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201207977/quicklook/glg_skymap_all_bn201207977.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/bn201207977/quicklook/glg_healpix_all_bn201207977.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201207977/quicklook/glg_lc_medres34_bn201207977.gif


GRB_name: GRB201207A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28997
SUBJECT: Fermi GRB 201207A: Global MASTER-Net observations report 
DATE:    20/12/08 00:45:17 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),

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 201207A ( Fermi GBM team, GCN 28996) errorbox  3980 sec after notice time and 4062 sec after trigger time at 2020-12-08 00:34:37 UT, with upper limit up to  16.0 mag. Observations started at twilight.  The observations began at zenith distance = 76 deg. The sun  altitude  is -12.7 deg. 

The galactic latitude b = -8 deg., longitude l = 266 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1497702

We obtain a following upper limits.  

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

    4092 | 2020-12-08 00:34:37 |         MASTER-OAFA | (08h 10m 40.49s , -49d 15m 18.0s) |   C |    60 | 16.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201208A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28998
SUBJECT: GRB 201208A: Fermi GBM Final Real-time Localization
DATE:    20/12/08 06:13:46 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 06:03:23 UT on 8 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201208A (trigger 629100208.248204 / 201208252).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 156.7, Dec = -29.3 (J2000 degrees, equivalent to J2000 10h 26m, -29d 18'), with a statistical uncertainty of 1.9 degrees.

The angle from the Fermi LAT boresight is 11.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201208252/quicklook/glg_skymap_all_bn201208252.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/bn201208252/quicklook/glg_healpix_all_bn201208252.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201208252/quicklook/glg_lc_medres34_bn201208252.gif


GRB_name: GRB201208A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  28999
SUBJECT: Fermi GRB 201208A: Global MASTER-Net observations report 
DATE:    20/12/08 08:15:45 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),

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 201208A ( Fermi GBM team, GCN 28998) errorbox  129 sec after notice time and 199 sec after trigger time at 2020-12-08 06:06:42 UT, with upper limit up to  18.3 mag. The observations began at zenith distance = 47 deg. The sun  altitude  is -31.2 deg. 

The galactic latitude b = 24 deg., longitude l = 269 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1497931

We obtain a following upper limits.  

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

     229 | 2020-12-08 06:06:42 |         MASTER-OAFA | (10h 22m 26.04s , -30d 34m 40.3s) |   C |    60 | 18.3 |        
     308 | 2020-12-08 06:08:01 |         MASTER-OAFA | (10h 35m 33.22s , -32d 34m 16.4s) |   C |    60 | 18.3 |        
     388 | 2020-12-08 06:09:21 |         MASTER-OAFA | (10h 16m 42.48s , -32d 36m 29.2s) |   C |    60 | 18.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201207A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29000
SUBJECT: GRB 201207A: AstroSat CZTI detection
DATE:    20/12/08 08:42:24 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, P. Sawant, V. Sharma, A. Vibhute 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 detection of a bright long GRB 201207A, which was also detected by Fermi GBM Final Real-time (GCN #28996) and Global MASTER-Net (Lipunov V. et al., GCN #28997).

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 2020-12-07 23:27:02.669 UT. The measured peak count rate associated with the burst is 283 +/- 24 cts/s above the background in the combined data of four quadrants, with a total of 2494 +/- 34 cts. The local mean background count rate was  509 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 18.3 +/- 0.4 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-12-07 23:27:01.628 UT. The measured peak count rate is 820 +/- 40 cts/s above the background in the combined Veto data of four quadrants, with a total of 5754 +/- 46 cts. The local mean background count rate was 1467 +/- 1  cts/s. We measure a T90 of 19.6 +/- 0.3 s from the cumulative Veto light curve.

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


GRB_name: GRB201208A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29001
SUBJECT: GRB 201208A: AstroSat CZTI detection
DATE:    20/12/08 17:26:54 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

D. Nadella (NITK), A. Marathe (NITK), G. Waratkar (IITB), V. Shenoy (IITB), V. Bhalerao (IITB), A. Vibhute (IUCAA), S. Gupta (IUCAA), D. Bhattacharya (IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al, 2020, arXiv:2011.07067) showed detection of a long GRB 201208A, which was also detected by Fermi GBM Final Real-time (GCN #28998).

The source was clearly detected in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2020-12-08 06:03:32.500 UT. The measured peak count rate associated with the burst is 383 (+53, -58) cts/s above the background in the combined data of four quadrants, with a total of 2992 (+511, -554) cts. The local mean background count rate was 757 (+3, -5) cts/s. Using cumulative rates, we measure a T90 of 39.75 (+5, -14) s. A weak signal was also seen in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. 

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


GRB_name: GRB201208A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29002
SUBJECT: GRB 201208A: Swift ToO observations
DATE:    20/12/09 01:35:18 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 201208A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021405

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: GRB201208A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29003
SUBJECT: GRB 201208A: Fermi-LAT detection
DATE:    20/12/09 03:07:46 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

F. Dirirsa (LAPP), N. Omodei (Stanford University),  F. Longo (University and INFN Trieste), D. Kocevski (NASA/MSFC), M. Ohno (Hiroshima Univ. & Eotvos Univ.) and M. Axelsson (KTH and Stockholm Univ.) report on behalf of the Fermi-LAT Collaboration:

On December 08, 2020, Fermi-LAT detected high-energy emission from GRB 201208A, which was also detected by Fermi-GBM (trigger 201208252, GCN 28998) and AstroSat CZTI (GCN 29001).

The best LAT on-ground location is found to be

RA, Dec 158.3, -28.8 (degrees, J2000)

with an error radius of 0.16 deg (90% containment, statistical error only).
This was 11 deg from the LAT boresight at the time of the GBM trigger:

T0 = 06:03:23 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 0-3000 s after the GBM trigger is (9.7+/-5.8)e-07 ph/cm2/s.

The estimated photon index above 100 MeV is -1.6 +/- 0.3.

The highest-energy photon is a 6.2 GeV event which is observed 1320 seconds after the GBM trigger.

A Swift ToO has been approved for this burst.

The Fermi-LAT point of contact for this burst is Feraol Fana Dirirsa (ffdirirsa@gmail.com).

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


GRB_name: GRB201209A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29005
SUBJECT: GRB 201209A: Swift detection of a burst
DATE:    20/12/09 05:56:54 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC),
M. J. Moss (GWU), D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (PSU), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 05:44:52 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201209A (trigger=1011980).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 23.106, -1.763 which is 
   RA(J2000) = 01h 32m 25s
   Dec(J2000) = -01d 45' 47"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 30 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~7 sec after the trigger. 

The XRT began observing the field at 05:46:44.1 UT, 111.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 23.09079, -1.75347 which
is equivalent to:
   RA(J2000)  = 01h 32m 21.79s
   Dec(J2000) = -01d 45' 12.5"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 64 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 3.60
x 10^20 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 6.48e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 121 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 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
0.04. 

Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)


GRB_name: GRB201209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29006
SUBJECT: GRB 201209A: FRAM-Auger optical limit
DATE:    20/12/09 06:50:15 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

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

report:

The 30cm robotic telescope FRAM-Auger in Malargue (Argentina) reacted
robotically to the Swift/BAT alert of GRB201209A (Gropp et al., GCNC
29005), starting with a series of 20 s R-band images at 05:45:40 UT, i.e.
48 s post trigger.

We do not detect any new or strongly variable source at or around the
reported X-ray error box in single frames nor in a combined 20 x 20 s image
spanning the
period from 0.8 min to 11.9 min after the initial trigger. The combined
exposure has a 3-sigma limiting magnitude R(Vega) ~ 17.4.


GRB_name: GRB201209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29007
SUBJECT: GRB 201209A: KAIT Optical Upper Limit
DATE:    20/12/09 07:05:46 GMT
FROM:    Weikang Zheng at UC Berkeley  <weikang@berkeley.edu>

The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 201209A (Gropp et al.,
GCN 29005) starting at 05:48:09 UT, 197 s after the burst under
cloudy condition. Observations were performed with an automatic
sequence in the clear (roughly R), V, and I filters, and the
exposure time was 20 s per image. We do not detect any optical
afterglow candidate within the XRT position error circle (Gropp
et al., GCN 29005), neither in single image, nor in the co-add images.
The typical limiting magnitude of our single clear image is about
15.0 mag calibrated to the USNOB1.0 catalog.


GRB_name: GRB201209A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29009
SUBJECT: GRB 201209A: Enhanced Swift-XRT position
DATE:    20/12/09 09:32:44 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 1536 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 201209A, 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 = 23.09069, -1.75468 which is equivalent
to:

RA (J2000): 01h 32m 21.77s
Dec (J2000): -01d 45' 16.8"

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: GRB201207A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29010
SUBJECT: GRB 201207A: AGILE detection
DATE:    20/12/09 10:05:43 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the long GRB 201207A at T0 = 2020-12-07
23:26:59 (UTC), reported by Fermi/GBM (GCN #28996) and AstroSat CZTI (GCN
#29000).

The burst is clearly visible in the AGILE scientific ratemeters of the
SuperAGILE (SA; 20-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and
AntiCoincidence (AC; 50-200 keV) detectors. The event lasted ~6 s and
released a total number of 640 counts in the SA detector (above a
background rate of 90 Hz), 8045 counts in the MCAL detector (above a
background rate of 1270 Hz), and 22670 counts in the AC detector (above a
background rate of 3630 Hz). The AGILE ratemeter light curves can be found
at http://www.agilescienceapp.it/notices/GRB_201207A_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition.

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: GRB201209A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29011
SUBJECT: GRB 201209A: AstroSat CZTI detection
DATE:    20/12/09 12:05:42 GMT
FROM:    Gaurav Waratkar at IIT Bombay  <gauravwaratkar24@gmail.com>

D. Nadella (NITK), G. Waratkar (IITB), A. Vibhute (IUCAA), S. Gupta
(IUCAA), P. Sawant (IUCAA), V. Bhalerao (IITB), D. Bhattacharya
(IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on
behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al,
2020, arxiv:2011.07067) showed detection of a long GRB 201209A, which
was also detected by Swift-BAT (GCN #29005).

The source was clearly detected in the 20-200 keV energy range. The
light curve showed multiple peaks of emission with the strongest peak
at 2020-12-09 05:44:56.500 UT. The measured peak count rate associated
with the burst is 456 (+51, -54) cts/s above the background in the
combined data of four quadrants, with a total of 3215 (+719, -885)
cts. The local mean background count rate was 557 (+4, -3) cts/s.
Using cumulative rates, we measure a T90 of 23 (+14, -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 2020-12-09
05:44:56.336 UT. The measured peak count rate is 697 (+81, -89) cts/s
above the background in the combined Veto data of four quadrants, with
a total of 4866 (+1506, -1667) cts. The local mean background count
rate was 1856 (+6, -7) cts/s. We measure a T90 of 25 (+26, -15) 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: GRB201209A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29013
SUBJECT: GRB 201209A: Xinglong-2.16m likely optical afterglow detection
DATE:    20/12/09 15:24:53 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

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

We observed the field of GRB 201209A (Gropp et al., GCN 29005) using the 
2.16-m optical telescope located at Xinglong, Hebei, China, equipped 
with the BFOSC camera. Observations started at 13:05:43 UT on 
2020-12-09, and 2x360 s, 3x600 s R-band frames were obtained.

An uncatalogued source is detected in our stacked image at coordinates

R.A. (J2000) = 1:32:21.76
Dec. (J2000) = -1:45:17.13

with an uncertainty of ~0.5 arcsec, being fully consistent with the 
Enhanced XRT position (Goad et al., GCN 29009). Calibrated with nearby 
PS1 stars, the source has m(R) = 22.05 +/- 0.16 mag at a median time of 
0.321 days post-burst, whereas PS1 is deeper but no object is present at 
the position. We thus conclude that the source is likely the optical 
afterglow of the burst.

We acknowledge excellent support from the Xinglong-2.16m observing 
staff, in particular Aiying Zhou and Jie Zheng.


GRB_name: GRB201209A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29014
SUBJECT: GRB 201209A: Swift-XRT refined Analysis
DATE:    20/12/09 15:38:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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), P. D'Avanzo
(INAF-OAB) and J.D. Gropp report on behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 201209A (Gropp et al. GCN
Circ. 29005), from 117 s to 29.1 ks after the  BAT trigger. The data
comprise 43 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. 29009).A spectrum formed from the PC mode
data can be fitted with an absorbed power-law with a photon spectral
index of 1.98 (+/-0.08). The best-fitting absorption column is 1.54
(+0.26, -0.25) x 10^21 cm^-2, in excess of the Galactic value of 3.6 x
10^20 cm^-2 (Willingale et al. 2013). The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.5 x 10^-11 (4.3 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.54 (+0.26, -0.25) x 10^21 cm^-2
Galactic foreground: 3.6 x 10^20 cm^-2
Excess significance: 7.9 sigma
Photon index:      1.98 (+/-0.08)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01011980.

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


GRB_name: GRB201208A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29015
SUBJECT: GRB 201208A: LCO observations 
DATE:    20/12/09 15:55:55 GMT
FROM:    Luca Izzo at DARK/NBI  <luca.izzo@gmail.com>

L. Izzo (DARK/NBI) and D. B. Malesani (DTU Space) report:

We observed the field of GRB 201208A (Fermi-GBM team, GCN #28998, Nadella et al., GCN #29001, Dirirsa et al., GCN #29003) with the Sinistro instrument mounted on the 1-m telescope of the LCO network located at the McDonald Observatory (Texas). Observations started on December 9 at 12:09:55 UT (1.25 days after the GRB trigger). We obtained a series of 5x120s images in r filter.

Within the XRT best candidate afterglow position at RA (J2000) = 10:33:17.64, Dec. (J2000) = -28:43:11.6, and with an error of 3.1" (see Evans, GCN #29002) we do not detect any optical afterglow candidate.  In our stacked image we measure an upper limit value of r > 23 (AB mag), calibrated against nearby Pan-STARRS catalog stars. 

This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No 730890.


GRB_name: GRB201208A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29017
SUBJECT: GRB 201208A: Fermi GBM observation
DATE:    20/12/09 18:43:38 GMT
FROM:    Rachel Dunwoody at UCD  <rachel.dunwoody@ucdconnect.ie>

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

At 06:03:23.25 UT on 08 December 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 201208A (trigger 629100208 / 201208252)
which was also detected by the Fermi/LAT (F. Dirirsa et al. 2020, GCN 29003)
The Fermi GBM Final Real-time Localization (GCN 28998) is consistent with
the Fermi/LAT position.
This source was also detected by AstroSat (D. Nadella et al. 2020,
GCN29001).

The angle from the Fermi LAT boresight at the GBM trigger time is 11
degrees.

The GBM light curve consists of one main pulse
with a duration (T90) of about 45 s (50-300 keV).
The time-averaged spectrum from T0-14 s to T0+34 s is
best fit by a power law with an exponential high-energy cutoff.
The power law index is -0.87 +/- 0.07 and the cutoff energy,
parameterized as Epeak, is 254 +/- 24.

The event fluence (10-1000 keV) in this time interval is
 (1.07 +/- 0.22)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+12 s in the 10-1000 keV band
is 5.1 +/- 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: GRB201208A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29018
SUBJECT: GRB 201208A: Swift-XRT afterglow detection
DATE:    20/12/09 19:48:17 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), J. D. Gropp (PSU), J.A.
Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester),
A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB) 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 201208A (Dirirsa et al. GCN Circ. 29003),
collecting 5.0 ks of Photon Counting (PC) mode data between T0+70.4 ks
and T0+111.4 ks. 

Four uncatalogued X-ray sources are detected, of which one ("Source 2")
is above the 2SXPS 3-sigma upper limit at this position, and is
therefore likely the GRB afterglow. Using 2046 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 = 158.32352, -28.71989 which is equivalent to:

RA (J2000): 10h 33m 17.64s
Dec(J2000): -28d 43' 11.6"

with an uncertainty of 3.1 arcsec (radius, 90% confidence). This
position is 112 arcsec from the Fermi/LAT position.  The results of the
XRT-team automatic analysis of the likely afterglow are at
https://www.swift.ac.uk/ToO_GRBs/00021405/Source2.php.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021405.

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


GRB_name: GRB201207A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29020
SUBJECT: IPN triangulation of GRB 201207A
DATE:    20/12/09 22:58:11 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,

A. Ursi, F. Verrecchia, M. Tavani, N. Parmiggiani, C. Pittori,
A. Bulgarelli, on behalf of the AGILE team,

and

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

The long-duration GRB 201207A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 28996;
AstroSat-CZTI detection: Gupta et al., GCN Circ. 29000;
AGILE detection: Ursi et al., GCN Circ. 29010)
was detected by Fermi (GBM trigger 629076420), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), AstroSat (CZTI),
and AGILE (MCAL) at about 84414 s UT (23:26:54).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  120.193 (08h 00m 46s) -49.327 (-49d 19' 36")
 Corners:
  119.115 (07h 56m 27s) -48.611 (-48d 36' 40")
  119.340 (07h 57m 22s) -50.448 (-50d 26' 55")
  121.306 (08h 05m 13s) -50.030 (-50d 01' 48")
  121.014 (08h 04m 03s) -48.193 (-48d 11' 36")
 ---------------------------------------------
The error box area is 2.4 sq. deg, and its maximum
dimension is 2.5 deg (the minimum one is 1.3 deg).
The Sun distance was 97 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB201207_T84417/IPN/

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


GRB_name: GRB201209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29021
SUBJECT: GRB 201209A: Swift-BAT refined analysis
DATE:    20/12/09 23:01:54 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (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 201209A (trigger #1011980)
(Gropp, et al., GCN Circ. 29005).  The BAT ground-calculated position is
RA, Dec = 23.096, -1.762 deg which is 
  RA(J2000)  =  01h 32m 23.0s 
  Dec(J2000) = -01d 45' 43.8" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11%.

The mask-weighted light curve shows some early emission starting at ~T-20 sec,
and two bright, symmetrical peaks centered at T+0 and T+7 sec.  The burst has
faded to background by T+30 sec.  T90 (15-350 keV) is 48.0 +- 16.0 sec 
(estimated error including systematics).

The time-averaged spectrum from T-31.66 to T+32.34 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.56 +- 0.06.  The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+7.84 sec in the 15-150 keV band
is 12.2 +- 1.1 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/1011980/BA/


GRB_name: GRB201209A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29026
SUBJECT: GRB 201209A: Swift/UVOT Upper Limits
DATE:    20/12/11 13:01:06 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 201209A: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 201209A
121 s after the BAT trigger (Gropp et al., GCN Circ. 29005).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 29009)
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           121          271          147         >20.1
u_FC               334          584          246         >20.3
white              121         1706          412         >20.9
v                  663         1583          117         >19.2
b                  590         1682          117         >19.5
u                  334         1657          343         >20.7
w1                 712         1632           97         >19.8
m2                 688         1260           39         >19.2
w2                1018         1211           39         >19.4

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: GRB201015A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29028
SUBJECT: GRB 201015A: 5-GHz radio afterglow detection with the EVN
DATE:    20/12/11 17:07:03 GMT
FROM:    Benito Marcote at JIVE  <marcote@jive.eu>

B. Marcote (JIVE), M. RibÃ³ (Univ. of Barcelona), J. M. Paredes (Univ. of Barcelona), M. Giroletti (INAF/IRA), S. Giarratana (Univ. of Bologna, INAF/IRA), G. Ghirlanda (INAF/OABrera)

We observed the radio counterpart of GRB 201015A (D'Elia et al., GCN 28632) with the European VLBI Network (EVN) on 9 November 2020 and 1 December 2020 at a central frequency of 5.0 GHz.

Preliminary analysis reports the detection of a compact radio source at a >8-sigma confidence level in both epochs at a consistent position of:

RA (J2000) = 23h37m16.4223s
Dec (J2000) = +53d24'56.439"

With an uncertainty of ~1 mas on each coordinate. The synthesized beams are 1.1 x 2.1 mas (PA = 7.1 deg) and 3.1 x 3.6 mas (PA = -29 deg) for the first and second epoch, respectively. We note that this position is consistent with the one previously reported by the VLA (Fong et al. GCN 28688) and eMERLIN (Giarratana et al. GCN 28939).

Further analysis is in progress.



We thank the directors and staff of all the EVN telescopes for making this target of opportunity observation possible.
The European VLBI Network is a joint facility of independent European, African, Asian, and North American radio astronomy institutes. Scientific results from data presented in this publication are derived from the following EVN project code: RM016. e-VLBI research infrastructure in Europe is supported by the European Unionâ€™s Seventh Framework Programme (FP7/2007-2013) under grant agreement number RI-261525 NEXPReS. e-MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC.


GRB_name: GRB200826A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29029
SUBJECT: GRB 200826A: GMOS-N detected source magnitude (Correction)
DATE:    20/12/11 23:06:21 GMT
FROM:    Tomas Ahumada at U. of Maryland  <tahumada@astro.umd.edu>

Tomas Ahumada (UMD), Harsh Kumar (IITB), Christoffer Fremling (Caltech),
Leo Singer (NASA GSFC) report on behalf of the ZTF and GROWTH
collaborations:

Reanalysing the data used in Ahumada et al. GCN 28727, we provide a revised
magnitude of the source detected in the Gemini Multi-Object Spectrograph
(GMOS-N) i-band image of ZTF20abwysqy/AT2020scz (Ahumada et al. GCN 28295).

We imaged the region of GRB 200826A (GCN 28284) with GMOS-N, mounted on the
Gemini-North 8-meter telescope on Mauna Kea, on three nights: 2020-09-23
(2459115.9675 mjd), 2020-10-10 (2459133.8039 mjd) and 2020-11-08
(2459167.9342 mjd). Each epoch consisted of 14 r- and i- band 200s
exposures. We reduced and co-added the images from each epoch using
DRAGONS, a Python-based data reduction platform provided by the Gemini
Observatory. We subtracted the coadded images using HOTPANTS and PyZOGY
independently. We now present the revised magnitudes using a zero-point
calculated using 23 stars in the field from the SDSS catalog. We apologize
for any possible confusion caused by the erroneously reported photometry in
GCN 28727.

In the 2020-09-23 images, a source is detected at the position of the
afterglow with i = 25.49 +- 0.15 mag, but not in r-band up to r > 25.6 AB
mag. In the 2020-10-10 images, we do not detect a transient in either
filter up to a 5-sigma limit of i > 25.4 mag and r > 25.5 mag.

At the host galaxy's redshift of z = 0.7481 (GCN 28319) and assuming Planck
2015 cosmological parameters, the absolute magnitude of the GMOS-N
detection is M_i = -17.9 AB mag.

We thank the Gemini Observatory Director for awarding this observing time
and the Gemini staff for help with planning and executing the observations.

-- 
Tomas Ahumada (he/him)
Ph.D. Student
Department of Astronomy
University of Maryland, College Park
NASA <tomas.f.ahumdamena@nasa.gov> Goddard Space Flight Center, Code 661
B.Sc. Astronomy, Pontificia Universidad CatÃ³lica de Chile


GRB_name: GRB201203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29030
SUBJECT: GRB 201203A: 1.3m DFOT, optical upper limits
DATE:    20/12/12 13:02:59 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

Amit Kumar (ARIES), Rahul Gupta (ARIES), Raya Dastidar (ARIES), Dimple
(ARIES), Ankur Ghosh (ARIES), Sapna Mishra (ARIES), Amar Aryan (ARIES),
Shashi B. Pandey (ARIES), and Kuntal Misra (ARIES) report:

We observed the field of Swift discovered GRB 201203A (Dichiara et al., GCN
28985, D'Elia et al., GCN 28990) with the 1.3m Devasthal Fast Optical
Telescope (DFOT) at Devasthal observatory of Aryabhatta Research Institute
of Observational Sciences (ARIES), India. We observed a series of images
~7.774 hours after the burst in both R and I (300sx6 in each) filters
(Johnson-Cousins) covering Swift UVOT position (Sakamoto et al., GCN
28995). Preliminary photometry on the stacked images was performed and
calibrated against USNO-B1 catalog stars. We do not detect any OT candidate
(Jelinek et al., GCN 28986, Watson et al., GCN 28987, Zheng et al., 28988,
Niwano et al., GCN 28992, Kumar et al. 28993) within the enhanced XRT
position. The upper limits in the stacked images are the following:

DATE       UT (start)  Filter Exposure(sec) Frames    Upper limit (mag)
2020-12-03 14:38:54    R      300           6        21.4
2020-12-03 15:11:18    I        300           6        21.2

This circular may be cited.


GRB_name: GRB201203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29032
SUBJECT: GRB 201203A: Zeiss-1000 (Koshka observatory) optical upper limit
DATE:    20/12/12 22:21:35 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

N. Pankov (HSE),  A. Zhornichenko (KIAM),   A. Pozanenko (IKI),  A. 
Novichonok (Petrozavodsk State University, KIAM), S. Belkin (IKI), 
report  on behalf of IKI GRB FuN:

We observed the field of  GRB 201203A (Dichiara  et al., GCN 28985) with 
Zeiss-1000 telescope of Koshka observatory starting on Dec. 03 (UT) 
20:50:46. We do not detect any optical source within XRT position 
(D'Elia  et al., GCN 28990) in agreement with previous observations 
(Jelinek et al., GCN 28986, Watson et al., GCN 28987, Zheng et al., 
28988, Niwano et al., GCN 28992, Kumar et al. GCN 28993; Kumar et al. 
GCN29030)

Preliminary photometry of the field is following

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

2020-12-03 20:50:46   0.58216    R      120*25   n/d  n/d   20.5


The photometry is based on the nearby USNO-B1.0 stars
USNO-B1.0_id R2
USNO_B10_0634-0041449
USNO_B10_0634-0041608
USNO_B10_0634-0041460
USNO_B10_0635-0033957


GRB_name: GRB201015A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29033
SUBJECT: GRB 201015A: optical observations and supernova identification
DATE:    20/12/12 23:11:17 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), S. Belkin (IKI, HSE), A. Volnova (IKI), A. Moskvitin 
(SAO RAS), O. Burhonov (UBAI), V. Kim (FAI),  M. Krugov (FAI),  V. 
Rumyantsev (CrAO), E. Klunko (ISTP), R. Ya. Inasaridze (AbAO), I. Reva 
(FAI), P. Minaev (IKI), N. Pankov (HSE), Sh. Ehgamberdiev (UBAI) report 
on behalf of GRB IKI FuN:

We observed the GRB 201015A  (D'Elia et al., GCN 28632) with ZTSh 2.6m 
telescope of CrAO observatory, AZT-33IK of Mondy observatory, AZT-20 of 
Assy observatory, AS-32 of Abastumani observatory, Zeiss-1000 of SAO 
RAS, AZT-22 of Maidanak observatory, and Zeiss-1000(E) of TSHAO.

The optical transient of GRB 201015A (Lipunov et al., GCN 28633; Kennea 
et al., GCN 28635; Malesani et al., GCN 28637; Ackley et al., GCN 28639; 
Hu et al., GCN 28645; Zhu et al., GCN 28653; Belkin  et al., 28656; 
Marshall et al., GCN 28662; Jelinek et al., GCN 28664; Belkin et al., 
GCN 28673; Grossan et al., GCN 28674; Rastinejad et al., GCN 28676; Zhu 
et al., GCN 28677; Kumar et al., GCN 28680; Kumar et al., GCN 28681; 
Moskvitin et al., GCN 28721) at redshift z=0.426 (de Ugarte Postigo et 
al., GCN 28649; Izzo et al., GCN 28661) is not spatially resolved in 
most of our images besides a few imaging in Maidanak observatory between 
Oct. 26 - Nov. 6 when observations were carried out under good weather 
conditions (FWHM = 0.8 - 0.9 arcsec). The finding chart of stacked image 
obtained in Maidanak observatory on Oct. 26, Nov. 4 and Nov. 6  is 
presented in the left panel of the Figure 1.

http://grb.rssi.ru/GRB201015A/GRB201015A_SN_imaging.png

(In all of the stacked images in the Figure 1 we subtracted nearby stars 
which positions are designated by white and green circles. The white 
circles denote the stars presented in PS DR1 catalogue, and the green 
circle denote the star is not presented in PS DR1. Stacked images of 
Zeiss-1000 of SAO RAS observations on 32 days (central panel) and 47 
days (right panel) are also presented in the Figure 1.)

Using the stacked image of Maidanak observations (left panel of the 
Figure 1, an upper limit of the image is R=24.6)  we obtained photometry 
of the nearby stars. The photometry of the stars is used for flux 
subtraction to obtain R-magnitudes of unresolved optical transient in 
all of observations, and a light curve of the optical transient is 
presented in Figure 2

http://grb.rssi.ru/GRB201015A/GRB201015A_SN_LC.png

The light curve is preliminary and represent the joint photometry of the 
optical transient and a possible host galaxy.

The source raised on in the left panel of the Figure 1 (red circle) 
coincides with an afterglow coordinates of GRB 201015A reported by NOT 
observation (Malesani et al., GCN 28637). We suggest the object clearly 
visible on Oct.26 - Nov.6 at the place of the afterglow is a supernova 
associated with GRB 201015A. The light curve in the Figure 2 suggests 
the supernova maximum between 12 and 20 days after GRB trigger.  The 
supernova identification rules out the GRB 201015A as a questionable 
short burst with extended emission (Markwardt  et al., GCN 28658)   and 
corroborates the  GRB 201015A as a long duration burst (Minaev et al., 
GCN 28668). The afterglow in the first two days after the trigger can be 
approximated by a power law with the index of -0.91 Â± 0.03.

We apologize for late report due to  delay of Maidanak data which is 
critical for supernova identification.


GRB_name: GRB201213A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29034
SUBJECT: GRB 201213A: Fermi GBM Final Real-time Localization
DATE:    20/12/13 18:04:23 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 17:54:05 UT on 13 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201213A (trigger 629574850.751498 / 201213746).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 239.8, Dec = -28.5 (J2000 degrees, equivalent to J2000 15h 59m, -28d 30'), with a statistical uncertainty of 8.2 degrees.

The angle from the Fermi LAT boresight is 56.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201213746/quicklook/glg_skymap_all_bn201213746.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/bn201213746/quicklook/glg_healpix_all_bn201213746.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201213746/quicklook/glg_lc_medres34_bn201213746.gif


GRB_name: GRB201214A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29036
SUBJECT: GRB 201214A: Swift ToO observations
DATE:    20/12/14 07:46:18 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 201214A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021406

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: GRB201214A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29037
SUBJECT: GRB 201214A: A long GRB detected by INTEGRAL
DATE:    20/12/14 08:10:16 GMT
FROM:    Sandro Mereghetti at IASF-Milano/INAF  <sandro.mereghetti@inaf.it>

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

a gamma ray burst lasting about 150 s has been detected by IBAS in the
IBIS/ISGRI
data at 6:18:20  UT of 14 December 2020.

The refined coordinates (J2000) are:

R.A.  =  170.9361  deg
DEC.  =  +33.8725  deg

with an uncertainty of  2.5   arcmin (90% c.l.).

A preliminary analysis gives a peak flux of about 0.1  ph/cm2/s (20-200
keV, 1-s integration time) and a fluence in the same energy range of about
5e-7  erg/cm2.

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


GRB_name: GRB201214B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29039
SUBJECT: GRB 201214B: Fermi GBM Final Real-time Localization
DATE:    20/12/14 16:15:39 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 SHORT GRB

At 16:07:46 UT on 14 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201214B (trigger 629654871.61686 / 201214672).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 206.2, Dec = 12.2 (J2000 degrees, equivalent to J2000 13h 44m, 12d 11'), with a statistical uncertainty of 11.1 degrees.

The angle from the Fermi LAT boresight is 20.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201214672/quicklook/glg_skymap_all_bn201214672.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/bn201214672/quicklook/glg_healpix_all_bn201214672.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201214672/quicklook/glg_lc_medres34_bn201214672.gif


GRB_name: GRB201214A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29040
SUBJECT: GRB 201214A: Mates' birthday GRB optical limit from FRAM-ORM
DATE:    20/12/14 16:48:18 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 INTEGRAL alert of GRB201214A (Mereghetti et al., GCNC 29037),
obtaining a series of 20s unfiltered images starting at 06:19:23.3 UT, i.e.
32.8s post trigger.

We do not detect any new or strongly variable source within a 20 arcmin FOV
around the reported gamma-ray errorbox - neither in single images
(detection limit R>~18.0) nor in a combined 40x20s frame (mean exp time
541s post trigger, with a limit R>~19.5).


GRB_name: GRB201214B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29043
SUBJECT: GRB 201214B: Swift ToO observations
DATE:    20/12/14 23:42:21 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 201214B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021407

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: GRB201214B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29044
SUBJECT: Fermi GRB 201214B: Global MASTER-Net observations report 
DATE:    20/12/15 00:15:31 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),

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 201214B ( Fermi GBM team, GCN 29039) errorbox  27106 sec after notice time and 27134 sec after trigger time at 2020-12-14 23:40:01 UT, with upper limit up to  19.1 mag. The observations began at zenith distance = 78 deg. The sun  altitude  is -57.5 deg. 

The galactic latitude b = 70 deg., longitude l = 346 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1502538

We obtain a following upper limits.  

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

   27165 | 2020-12-14 23:40:01 |      MASTER-Tavrida | (13h 38m 31.09s , +18d 15m 51.4s) |   C |    60 | 18.6 |        
   27483 | 2020-12-14 23:45:19 |      MASTER-Tavrida | (13h 38m 25.91s , +18d 14m 10.0s) |   C |    60 | 18.5 |        
   27867 | 2020-12-14 23:51:43 |      MASTER-Tavrida | (13h 12m 59.27s , +16d 17m 10.4s) |   C |    60 | 18.4 |        
   28027 | 2020-12-14 23:54:23 |      MASTER-Tavrida | (13h 21m 32.36s , +18d 15m 02.8s) |   C |    60 | 18.4 |        
   28106 | 2020-12-14 23:55:42 |      MASTER-Tavrida | (13h 31m 21.52s , +20d 14m 55.6s) |   C |    60 | 18.9 |        
   28186 | 2020-12-14 23:57:02 |      MASTER-Tavrida | (13h 13m 02.71s , +16d 17m 02.2s) |   C |    60 | 18.4 |        
   28421 | 2020-12-15 00:00:57 |      MASTER-Tavrida | (13h 21m 31.21s , +18d 17m 09.9s) |   C |    60 | 18.4 |        
   28500 | 2020-12-15 00:02:16 |      MASTER-Tavrida | (13h 31m 22.57s , +20d 16m 00.3s) |   C |    60 | 18.9 |        
   28580 | 2020-12-15 00:03:36 |      MASTER-Tavrida | (13h 05m 33.46s , +14d 15m 34.2s) |   C |    60 | 18.5 |        
   28659 | 2020-12-15 00:04:55 |      MASTER-Tavrida | (13h 14m 18.52s , +20d 15m 55.0s) |   C |    60 | 18.6 |        
   28739 | 2020-12-15 00:06:15 |      MASTER-Tavrida | (13h 04m 42.98s , +18d 17m 31.2s) |   C |    60 | 18.9 |        
   28818 | 2020-12-15 00:07:34 |      MASTER-Tavrida | (13h 42m 17.57s , +22d 15m 25.0s) |   C |    60 | 19.0 |        
   28897 | 2020-12-15 00:08:53 |      MASTER-Tavrida | (13h 25m 03.32s , +22d 17m 01.8s) |   C |    60 | 19.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201214B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29045
SUBJECT: GRB 201214B: Swift BAT location of short burst
DATE:    20/12/15 02:40:30 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. K. Simpson (PSU), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 16:07:46 UT on 2020-12-14, simultaneously with the Fermi GBM 
detection of GRB 201214B (GCN 29039), BAT triggered (Trigger=1012872) 
on a rate increase at the 0.064 s timescale and produced an image. 
This image shows a 6 sigma peak, which was not significant enough 
to trigger an automated ground notification and repoint. 
The on-board calculated location 
ra, dec = 188.032, +9.045 was refined by ground analysis 
to 187.9710, +9.1031 which is
 RA(J2000) = 12h 31m 53s
 Dec(J2000) = 09d 06' 11â€
with an uncertainty of 2 arcminutes (radius, 90% containment, including 
systematic uncertainty).  The currently-available BAT light curve shows
a ~0.1 second long peak, with a possible smaller peak 0.3 seconds earlier. 
The peak value on a 64 ms timescale is ~3000 counts/s (15-350 keV)
at the trigger time. 

Swift has begun XRT and UVOT observations of this source starting at T0+~28ks
using the on-board BAT location (GCN 29043). 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021407

The BAT location is consistent with both the Fermi-GBM position and 
the IPN annulus (Svinkin, priv. comm.).  The temporal and positional 
coincidence with the Fermi GBM burst convinces us that the BAT
location is correct. 

Burst Advocate for this burst is K. K. Simpson (kira.simpson1984 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: GRB201215A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29046
SUBJECT: GRB 201215A: Fermi GBM Final Real-time Localization
DATE:    20/12/15 06:33:47 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:23:28 UT on 15 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201215A (trigger 629706213.838334 / 201215266).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 211.8, Dec = 42.4 (J2000 degrees, equivalent to J2000 14h 07m, 42d 23'), with a statistical uncertainty of 15.7 degrees.

The angle from the Fermi LAT boresight is 118.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201215266/quicklook/glg_skymap_all_bn201215266.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/bn201215266/quicklook/glg_healpix_all_bn201215266.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201215266/quicklook/glg_lc_medres34_bn201215266.gif


GRB_name: GRB201215A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29047
SUBJECT: GRB 201215A: BALROG localization (Fermi Trigger 629706213 / GRB 201215266)
DATE:    20/12/15 06:48:33 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

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

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
629706213 at 06:23:28 on 15 Dec. 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) = 192.9+/-3.8 deg
Decl.(2000.0) = 18.1+/-3.8 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201215266/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201215266/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201215266/json

                        


GRB_name: GRB201214A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29048
SUBJECT: GRB 201214A: Swift-XRT observations
DATE:    20/12/15 07:17:06 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), T. Sbarrato (INAF-OAB), P.
D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), B. Sbarufatti (PSU)
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 201214A (Mereghetti et al. GCN Circ. 29037), collecting 4.1
ks of Photon Counting (PC) mode data between T0+5.2 ks and T0+23.6 ks. 

One uncatalogued X-ray source has been detected consistent with being
within 246 arcsec of the INTEGRAL position, 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 2:
  RA (J2000):  170.92446  =  11:23:41.87
  Dec (J2000): +33.86930  =  +33:52:09.5
  Error: 2.2 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.0182 +/- 0.0024 ct s^-1   
  Distance: 36 arcsec from INTEGRAL position.
  Flux: (4.48 +/- 0.60)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

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

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021406.

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


GRB_name: GRB201209A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29050
SUBJECT: GRB 201209A: Insight-HXMT/HE detection
DATE:    20/12/15 14:40:28 GMT
FROM:    Y Q Zhang at IHEP  <yqzhang@ihep.ac.cn>

Y. Q. Zhang, C. Cai, J. C. Liu, Q. Luo, S. Xiao, 
W. C. Xue, Q. B. Yi, C. Zhengï¼ŒY. Huang, C. K. Li, 
G. Li, X. B. Li, J. Y. Liao, X. Y. Song, 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 2020-12-09T05:44:52.53 (T0), Insight-HXMT/HE detected 
GRB 201209A (trigger ID: HEB201209239) in a routine search of the data, 
which also triggered Swift/BAT (Gropp J. et al., GCN #29005) and 
AstroSat/CZTI ( Nadella D. et al., GCN #29011)..

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 9.99 s measured from T0-1.09 s. 
The 1-ms peak rate, measured from T0+7.16 s, is 778 cnts/sec. 
The total counts from this burst is 2926 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB201209239_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: GRB201215A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29051
SUBJECT: Fermi GRB 201215A: Global MASTER-Net observations report 
DATE:    20/12/15 15:30:49 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),

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 201215A ( Fermi GBM team, GCN 29046) errorbox  31642 sec after notice time and 31660 sec after trigger time at 2020-12-15 15:11:09 UT, with upper limit up to  17.8 mag. Observations started at twilight.  The observations began at zenith distance = 77 deg. The sun  altitude  is -11.4 deg. 

The galactic latitude b = 68 deg., longitude l = 81 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1502976

We obtain a following upper limits.  

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

   31690 | 2020-12-15 15:11:09 |      MASTER-Tavrida | (14h 27m 07.35s , +49d 45m 44.0s) |   C |    60 | 16.8 |        
   32055 | 2020-12-15 15:17:13 |      MASTER-Tavrida | (14h 27m 02.08s , +49d 46m 19.8s) |   C |    60 | 17.3 |        
   32134 | 2020-12-15 15:18:32 |      MASTER-Tavrida | (14h 39m 26.74s , +49d 47m 24.8s) |   C |    60 | 17.5 |        
   32453 | 2020-12-15 15:23:51 |      MASTER-Tavrida | (14h 39m 30.99s , +49d 45m 32.6s) |   C |    60 | 17.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201214B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29052
SUBJECT: GRB 201214B: Swift-XRT observations
DATE:    20/12/15 15:48:15 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

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

Swift-XRT has performed follow-up observations of the
Swift/BAT-detected burst GRB 201214B, collecting 5.8 ks of Photon
Counting (PC) mode data between T0+27.2 ks and T0+51.1 ks. 

Eight 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):  187.8292  =  12:31:19.02
  Dec (J2000): +9.0458  =  +09:02:44.8
  Error: 4.9 arcsec (radius, 90% conf.)
  Count-rate: (2.47 [+1.03, -0.83])e-3 ct s^-1  
  Distance: 720 arcsec from Swift/BAT position.
  Flux: (4.9 [+2.1, -1.6])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 2:
  RA (J2000):  187.9923  =  12:31:58.15
  Dec (J2000): +9.0742  =  +09:04:26.9
  Error: 4.6 arcsec (radius, 90% conf.)
  Count-rate: (2.50 [+0.94, -0.77])e-3 ct s^-1  
  Distance: 175 arcsec from Swift/BAT position.
  Flux: (8.2 [+3.1, -2.5])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 3:
  RA (J2000):  187.8467  =  12:31:23.21
  Dec (J2000): +9.1051  =  +09:06:18.5
  Error: 4.6 arcsec (radius, 90% conf.)
  Count-rate: (1.57 [+0.86, -0.65])e-3 ct s^-1  
  Distance: 693 arcsec from Swift/BAT position.

Source 4:
  RA (J2000):  188.1338  =  12:32:32.10
  Dec (J2000): +9.1148  =  +09:06:53.1
  Error: 6.0 arcsec (radius, 90% conf.)
  Count-rate: (1.89 [+0.85, -0.67])e-3 ct s^-1  
  Distance: 440 arcsec from Swift/BAT position.
  Flux: (5.9 [+2.6, -2.1])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 5:
  RA (J2000):  188.1013  =  12:32:24.32
  Dec (J2000): +9.1072  =  +09:06:26.1
  Error: 6.1 arcsec (radius, 90% conf.)
  Count-rate: (1.49 [+0.76, -0.59])e-3 ct s^-1  
  Distance: 333 arcsec from Swift/BAT position.
  Flux: (5.4 [+2.7, -2.1])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 6:
  RA (J2000):  188.0148  =  12:32:3.54
  Dec (J2000): +8.9310  =  +08:55:51.5
  Error: 5.2 arcsec (radius, 90% conf.)
  Count-rate: (2.02 [+0.86, -0.69])e-3 ct s^-1  
  Distance: 415 arcsec from Swift/BAT position.

Source 7:
  RA (J2000):  187.9055  =  12:31:37.31
  Dec (J2000): +8.9889  =  +08:59:19.9
  Error: 5.0 arcsec (radius, 90% conf.)
  Count-rate: (1.93 [+0.94, -0.73])e-3 ct s^-1  
  Distance: 493 arcsec from Swift/BAT position.
  Flux: (3.7 [+1.8, -1.4])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 9:
  RA (J2000):  187.9206  =  12:31:40.95
  Dec (J2000): +9.0086  =  +09:00:31.1
  Error: 5.3 arcsec (radius, 90% conf.)
  Count-rate: (8.0 [+6.0, -4.2])e-4 ct s^-1   
  Distance: 417 arcsec from Swift/BAT position.

A catalogued source was also detected.

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/00021407.

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


GRB_name: GRB201214B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29054
SUBJECT: GRB 201214B: Lowell Discovery Telescope optical observations
DATE:    20/12/16 11:42:27 GMT
FROM:    Simone Dichiara at UMCP/NASA/GSFC  <dichiara@umd.edu>

S.Dichiara (UMD, NASA-GSFC), E. Troja (UMD, NASA-GSFC), P. Gatkine
(Caltech), J.M. Durbak (UMD), S.B. Cenko (NASA-GSFC), B. O'Connor
(GWU, UMD), A. Kutyrev (UMD, NASA-GSFC), S. Veilleux (UMD) report:

We observed the field of the short GRB 201214B (Simpson et al.,
GCN 29045; Fermi GBM team, GCN 29039) using the Large Monolithic Imager
(LMI) on the 4.3m Lowell Discovery Telescope (LDT) at Happy Jack, AZ.
Observations started on December 15, at 11:21 UT (about 19.2 hours after
the Swift trigger) using the SDSS r, i and z filters. Observations were
taken at an airmass of about 1.3 and seeing of about 2.5". Our average
sensitivity is i<23.5 AB mag.

We do not detect any uncatalogued optical source at the position of the
Swift/XRT sources reported by Tohuvavohu et al. (GCN 29052).

By cross-correlating the refined BAT localization with the GLADE v2.3
galaxy catalog (Dalya et al. 2018), as described in Dichiara et al.
(2020), we note the presence of a nearby lenticular galaxy
(HyperLEDA-1359588 at ~280 Mpc) within the BAT error circle.

Further observations are planned.

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


GRB_name: GRB201214B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29056
SUBJECT: GRB 201214B: MITSuME Akeno optical upper limits
DATE:    20/12/16 13:52:03 GMT
FROM:    Noriatsu Nakamura at Tokyo Inst. of Tech.  <nnakamura@hp.phys.titech.ac.jp>

N. Nakamura,  R. Hosokawa, K. L. Murata, R. Adachi, M. Niwano, F.
Ogawa, N. Ito, 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 201214B (The Fermi GBM team,  GCN #29039,
P. Evans et al., GCN #29043, V. Lipunov et al., GCN #29044, D. Palmer
et al., GCN #29045, B. Sbarufatti et al., GCN #29052 ) 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 with a series of 60 sec exposures started at 2020-12-15
18:51:41 UT(28.8 hour after trigger). We did not find any new point
sources within the enhanced Swift BAT circle (D. Palmer et al., GCN
#29045) in all three bands.
We obtained the 5-sigma limits of the stacked images as follows
T0+[hour] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
28.8 18:51:41 10380 g'>20.9,Rc>21.0,Ic>20.3
------------------------------------------------------------------------------------------------
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.,
https://doi.org/10.1093/pasj/psaa091,
https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire).


GRB_name: GRB201216A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29057
SUBJECT: GRB 201216A: Fermi GBM Final Real-time Localization
DATE:    20/12/16 19:10:45 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 19:00:31 UT on 16 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201216A (trigger 629838036.239118 / 201216792).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 190.6, Dec = 40.3 (J2000 degrees, equivalent to J2000 12h 42m, 40d 17'), with a statistical uncertainty of 7.5 degrees.

The angle from the Fermi LAT boresight is 39.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201216792/quicklook/glg_skymap_all_bn201216792.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/bn201216792/quicklook/glg_healpix_all_bn201216792.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201216792/quicklook/glg_lc_medres34_bn201216792.gif


GRB_name: GRB201216B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29058
SUBJECT: GRB 201216B: AGILE detection of a burst
DATE:    20/12/16 21:37:32 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected a burst at T0 = 2020-12-16 14:46:35.66 +/-
0.01 s (UTC).

The burst is clearly visible in the AGILE scientific ratemeters of the
SuperAGILE (SA; 20-60 keV), MiniCALorimeter (MCAL; 0.4-100 MeV), and
AntiCoincidence (AC; 50-200 keV) detectors. The event lasted about ~10 s
and it released a total number of 1600 counts in the SA detector (above a
background rate of 100 Hz), 1500 counts in the MCAL detector (above a
background rate of 1220 Hz), and 37500 counts in the AC detector (above a
background rate of 3500 Hz). The AGILE ratemeter light curves can be found
at http://www.agilescienceapp.it/notices/GRB_201216B_AGILE_RM.png .

The event also triggered a partial high time resolution MCAL data
acquisition, where it released ~2500 counts (in the 0.4-100 MeV energy
range), above a background rate of 570 Hz. The MCAL light curve can be
found at
http://www.agilescienceapp.it/notices/GRB_070900_535214795.665353.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: GRB201216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29059
SUBJECT: GRB 201216A: Swift/BAT-GUANO detection and arcminute localization
DATE:    20/12/16 22:05:10 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 201216A (T0: 2020-12-16 19:00:31 UTC,
Fermi/GBM TRIGGER 629838036, GCN 29057).

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

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

Using the normal BAT imaging technique, we find the location of the
GRB with an SNR of 8.9.
The BAT position is
RA, Dec = 201.4872, +36.3116 deg which is
   RA(J2000)  = 13h 25m 56.93s
   Dec(J2000) =  +36d 18' 41.76"
with an estimated uncertainty of 3 arcmin.

This position is consistent with the Fermi GBM localization (GCN 29057).

XRT and UVOT follow-up has been requested. Results of follow-up
observations will be reported in future circulars.

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

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


GRB_name: GRB201216A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29060
SUBJECT: Fermi GRB 201216A: Global MASTER-Net observations report 
DATE:    20/12/16 22:45:26 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),

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 201216A ( Fermi GBM team, GCN 29057) errorbox  9093 sec after notice time and 9123 sec after trigger time at 2020-12-16 21:32:34 UT, with upper limit up to  18.8 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -69.3 deg. 

The galactic latitude b = 77 deg., longitude l = 129 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1504672

We obtain a following upper limits.  

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

     363 | 2020-12-16 19:06:04 |             MASTER- | (13h 07m 43.55s , +46d 36m 09.3s) |   C |    60 | 17.5 |        
     363 | 2020-12-16 19:06:04 |             MASTER- | (12h 56m 31.09s , +45d 15m 10.4s) |   C |    60 | 17.5 |        
     614 | 2020-12-16 19:10:15 |             MASTER- | (13h 17m 46.46s , +40d 35m 28.8s) |   C |    60 | 17.5 |        
     614 | 2020-12-16 19:10:15 |             MASTER- | (13h 07m 38.14s , +39d 14m 22.3s) |   C |    60 | 17.0 |        
     775 | 2020-12-16 19:12:56 |             MASTER- | (12h 35m 54.29s , +40d 38m 28.4s) |   C |    60 | 17.9 |        
     775 | 2020-12-16 19:12:56 |             MASTER- | (12h 25m 42.42s , +39d 17m 23.9s) |   C |    60 | 18.1 |        
     860 | 2020-12-16 19:14:21 |             MASTER- | (13h 07m 48.15s , +46d 38m 21.3s) |   C |    60 | 17.5 |        
     860 | 2020-12-16 19:14:21 |             MASTER- | (12h 56m 33.49s , +45d 17m 18.4s) |   C |    60 | 17.5 |        
    1201 | 2020-12-16 19:20:02 |             MASTER- | (13h 17m 40.00s , +40d 36m 02.3s) |   C |    60 | 17.5 |        
    1201 | 2020-12-16 19:20:02 |             MASTER- | (13h 07m 32.84s , +39d 14m 53.9s) |   C |    60 | 17.7 |        
    1365 | 2020-12-16 19:22:46 |             MASTER- | (12h 35m 53.87s , +40d 40m 42.6s) |   C |    60 | 17.7 |        
    1365 | 2020-12-16 19:22:46 |             MASTER- | (12h 25m 42.35s , +39d 19m 32.2s) |   C |    60 | 18.1 |        
    1529 | 2020-12-16 19:25:30 |             MASTER- | (12h 56m 52.61s , +40d 39m 36.4s) |   C |    60 | 17.6 |        
    1529 | 2020-12-16 19:25:30 |             MASTER- | (12h 46m 41.02s , +39d 18m 11.5s) |   C |    60 | 17.9 |        
    1613 | 2020-12-16 19:26:54 |             MASTER- | (12h 37m 40.78s , +42d 40m 05.5s) |   C |    60 | 17.7 |        
    1613 | 2020-12-16 19:26:54 |             MASTER- | (12h 27m 08.40s , +41d 18m 42.9s) |   C |    60 | 18.2 |        
    1702 | 2020-12-16 19:28:23 |             MASTER- | (12h 59m 14.32s , +42d 39m 51.6s) |   C |    60 | 17.7 |        
    1702 | 2020-12-16 19:28:23 |             MASTER- | (12h 48m 43.16s , +41d 18m 30.3s) |   C |    60 | 17.6 |        
    1779 | 2020-12-16 19:29:39 |             MASTER- | (12h 55m 28.20s , +38d 39m 04.6s) |   C |    60 | 17.5 |        
    1779 | 2020-12-16 19:29:39 |             MASTER- | (12h 45m 33.95s , +37d 17m 42.3s) |   C |    60 | 18.0 |        
    1870 | 2020-12-16 19:31:11 |             MASTER- | (12h 56m 47.12s , +40d 38m 06.5s) |   C |    60 | 17.6 |        
    1871 | 2020-12-16 19:31:11 |             MASTER- | (12h 46m 35.22s , +39d 16m 45.1s) |   C |    60 | 18.0 |        
    1955 | 2020-12-16 19:32:36 |             MASTER- | (12h 37m 47.00s , +42d 39m 43.4s) |   C |    60 | 17.6 |        
    1955 | 2020-12-16 19:32:36 |             MASTER- | (12h 27m 14.01s , +41d 18m 21.4s) |   C |    60 | 17.9 |        
    2056 | 2020-12-16 19:34:17 |             MASTER- | (12h 59m 18.21s , +42d 40m 03.2s) |   C |    60 | 17.8 |        
    2056 | 2020-12-16 19:34:17 |             MASTER- | (12h 48m 46.39s , +41d 18m 42.0s) |   C |    60 | 17.5 |        
    2133 | 2020-12-16 19:35:34 |             MASTER- | (12h 55m 26.16s , +38d 38m 24.3s) |   C |    60 | 17.5 |        
    2133 | 2020-12-16 19:35:34 |             MASTER- | (12h 45m 31.47s , +37d 17m 03.0s) |   C |    60 | 18.1 |        
    9153 | 2020-12-16 21:32:34 |      MASTER-Tavrida | (12h 45m 40.62s , +40d 18m 38.4s) |   C |    60 | 17.7 |        
    9153 | 2020-12-16 21:32:34 |      MASTER-Tavrida | (12h 53m 28.77s , +40d 16m 14.0s) |   C |    60 | 17.0 |        
    9233 | 2020-12-16 21:33:54 |      MASTER-Tavrida | (12h 24m 52.90s , +40d 17m 40.3s) |   C |    60 | 18.0 |        
    9233 | 2020-12-16 21:33:54 |      MASTER-Tavrida | (12h 32m 41.13s , +40d 15m 19.0s) |   C |    60 | 17.5 |        
    9783 | 2020-12-16 21:43:04 |      MASTER-Tavrida | (12h 45m 48.84s , +40d 17m 40.0s) |   C |    60 | 17.6 |        
    9783 | 2020-12-16 21:43:04 |      MASTER-Tavrida | (12h 53m 37.95s , +40d 15m 15.4s) |   C |    60 | 16.8 |        
    9862 | 2020-12-16 21:44:23 |      MASTER-Tavrida | (12h 26m 14.09s , +42d 16m 45.6s) |   C |    60 | 18.1 |        
    9862 | 2020-12-16 21:44:23 |      MASTER-Tavrida | (12h 34m 18.02s , +42d 14m 26.0s) |   C |    60 | 17.3 |        
   10178 | 2020-12-16 21:49:39 |      MASTER-Tavrida | (12h 31m 52.23s , +38d 16m 14.2s) |   C |    60 | 17.2 |        
   10178 | 2020-12-16 21:49:39 |      MASTER-Tavrida | (12h 24m 16.46s , +38d 18m 38.4s) |   C |    60 | 18.3 |        
   10257 | 2020-12-16 21:50:58 |      MASTER-Tavrida | (12h 44m 44.32s , +38d 17m 29.0s) |   C |    60 | 18.1 |        
   10257 | 2020-12-16 21:50:58 |      MASTER-Tavrida | (12h 52m 19.55s , +38d 15m 01.7s) |   C |    60 | 17.2 |        
   10542 | 2020-12-16 21:55:43 |      MASTER-Tavrida | (12h 31m 51.85s , +38d 16m 13.5s) |   C |    60 | 17.1 |        
   10542 | 2020-12-16 21:55:43 |      MASTER-Tavrida | (12h 24m 16.24s , +38d 18m 37.4s) |   C |    60 | 18.1 |        
   10823 | 2020-12-16 22:00:24 |      MASTER-Tavrida | (12h 55m 48.97s , +42d 14m 10.9s) |   C |    60 | 17.6 |        
   10823 | 2020-12-16 22:00:24 |      MASTER-Tavrida | (12h 47m 51.94s , +42d 16m 04.5s) |   C |    60 | 18.0 |        
   10904 | 2020-12-16 22:01:45 |      MASTER-Tavrida | (12h 28m 51.45s , +44d 16m 33.9s) |   C |    60 | 18.2 |        
   10904 | 2020-12-16 22:01:45 |      MASTER-Tavrida | (12h 37m 04.73s , +44d 14m 43.5s) |   C |    60 | 17.9 |        
   10983 | 2020-12-16 22:03:04 |      MASTER-Tavrida | (12h 32m 06.09s , +36d 15m 53.7s) |   C |    60 | 16.3 |        
   10983 | 2020-12-16 22:03:04 |      MASTER-Tavrida | (12h 24m 48.08s , +36d 17m 48.3s) |   C |    60 | 17.9 |        
   11491 | 2020-12-16 22:11:32 |      MASTER-Tavrida | (12h 28m 47.70s , +44d 17m 34.5s) |   C |    60 | 18.5 |        
   11491 | 2020-12-16 22:11:32 |      MASTER-Tavrida | (12h 37m 05.31s , +44d 15m 26.3s) |   C |    60 | 17.9 |        
   11571 | 2020-12-16 22:12:51 |      MASTER-Tavrida | (12h 24m 42.22s , +36d 16m 17.9s) |   C |    60 | 18.4 |        
   11571 | 2020-12-16 22:12:51 |      MASTER-Tavrida | (12h 32m 03.55s , +36d 14m 07.0s) |   C |    60 | 16.5 |        
   11650 | 2020-12-16 22:14:11 |      MASTER-Tavrida | (12h 59m 23.80s , +44d 14m 39.0s) |   C |    60 | 17.7 |        
   11650 | 2020-12-16 22:14:11 |      MASTER-Tavrida | (12h 51m 06.64s , +44d 16m 49.7s) |   C |    60 | 18.6 |        
   11958 | 2020-12-16 22:19:19 |      MASTER-Tavrida | (12h 12m 38.80s , +42d 16m 47.5s) |   C |    60 | 18.0 |        
   11958 | 2020-12-16 22:19:19 |      MASTER-Tavrida | (12h 04m 35.75s , +42d 19m 00.2s) |   C |    60 | 18.7 |        
   12037 | 2020-12-16 22:20:38 |      MASTER-Tavrida | (12h 44m 37.32s , +36d 17m 14.9s) |   C |    60 | 18.3 |        
   12037 | 2020-12-16 22:20:38 |      MASTER-Tavrida | (12h 51m 58.70s , +36d 14m 59.1s) |   C |    60 | 16.9 |        
   12247 | 2020-12-16 22:24:08 |      MASTER-Tavrida | (12h 11m 35.33s , +40d 16m 43.8s) |   C |    60 | 17.8 |        
   12247 | 2020-12-16 22:24:08 |      MASTER-Tavrida | (12h 03m 46.80s , +40d 18m 57.4s) |   C |    60 | 18.6 |        
   12327 | 2020-12-16 22:25:27 |      MASTER-Tavrida | (12h 41m 00.54s , +46d 15m 34.6s) |   C |    60 | 18.3 |        
   12327 | 2020-12-16 22:25:27 |      MASTER-Tavrida | (12h 32m 23.51s , +46d 17m 48.7s) |   C |    60 | 18.8 |        
   12558 | 2020-12-16 22:29:19 |      MASTER-Tavrida | (13h 14m 24.24s , +40d 15m 57.8s) |   C |    60 | 17.6 |        
   12558 | 2020-12-16 22:29:19 |      MASTER-Tavrida | (13h 06m 37.08s , +40d 18m 17.0s) |   C |    60 | 18.0 |        
   12637 | 2020-12-16 22:30:38 |      MASTER-Tavrida | (12h 12m 42.90s , +42d 15m 48.4s) |   C |    60 | 18.1 |        
   12637 | 2020-12-16 22:30:38 |      MASTER-Tavrida | (12h 04m 40.36s , +42d 17m 57.5s) |   C |    60 | 18.5 |        
   12717 | 2020-12-16 22:31:57 |      MASTER-Tavrida | (12h 11m 34.27s , +40d 14m 44.4s) |   C |    60 | 17.8 |        
   12717 | 2020-12-16 22:31:57 |      MASTER-Tavrida | (12h 03m 46.53s , +40d 16m 54.4s) |   C |    60 | 18.6 |        
   12796 | 2020-12-16 22:33:17 |      MASTER-Tavrida | (12h 40m 58.33s , +46d 14m 45.0s) |   C |    60 | 18.2 |        
   12796 | 2020-12-16 22:33:17 |      MASTER-Tavrida | (12h 32m 22.10s , +46d 16m 55.3s) |   C |    60 | 18.5 |        
   12875 | 2020-12-16 22:34:36 |      MASTER-Tavrida | (12h 14m 41.97s , +44d 16m 31.5s) |   C |    60 | 18.0 |        
   12954 | 2020-12-16 22:35:55 |      MASTER-Tavrida | (13h 14m 26.63s , +40d 14m 07.0s) |   C |    60 | 17.5 |        
   12954 | 2020-12-16 22:35:55 |      MASTER-Tavrida | (13h 06m 39.70s , +40d 16m 25.9s) |   C |    60 | 18.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201216C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29061
SUBJECT: GRB 201216C: Swift detection of a burst
DATE:    20/12/16 23:15:47 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
A. Y. Lien (GSFC/UMBC), M. J. Moss (GWU), 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 23:07:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 201216C (trigger=1013243).  Swift did not slew immediately 
to the burst due to an observing constraint. 
The BAT on-board calculated location is 
RA, Dec 16.358, +16.537 which is 
   RA(J2000) = 01h 05m 26s
   Dec(J2000) = +16d 32' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 50 sec.  The peak count rate
was ~13000 counts/sec (15-350 keV), at ~20 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+46.8
minutes. There will be no XRT or UVOT data until this time. 

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


GRB_name: GRB201216C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29063
SUBJECT: GRB 201216C: Fermi GBM Final Real-time Localization
DATE:    20/12/16 23:17:45 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 23:07:25 UT on 16 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201216C (trigger 629852850.753568 / 201216963).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 17.9, Dec = 16.8 (J2000 degrees, equivalent to J2000 01h 11m, 16d 48'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 93.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201216963/quicklook/glg_skymap_all_bn201216963.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/bn201216963/quicklook/glg_healpix_all_bn201216963.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201216963/quicklook/glg_lc_medres34_bn201216963.gif


GRB_name: GRB201216C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29064
SUBJECT: GRB 201216C: Swift-XRT observations
DATE:    20/12/17 00:58:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

The XRT began observing the field of GRB 201216C at 23:56:58.5 UT,
2966.8 seconds after the BAT trigger. Using promptly downlinked data we
find a fading, uncatalogued X-ray source located at RA, Dec 16.37114,
16.51659 which is equivalent to:
   RA(J2000)  = 01h 05m 29.07s
   Dec(J2000) = +16d 30' 59.7"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 86 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (5.04 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 7.4
(+2.86/-2.53) x 10^21 cm^-2 (90% confidence). 


GRB_name: GRB201216A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29065
SUBJECT: GRB 201216A: Swift ToO observations
DATE:    20/12/17 01:00:14 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 201216A. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00021408

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: GRB201216C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29066
SUBJECT: GRB 201216C: VLT afterglow candidate discovery
DATE:    20/12/17 02:36:55 GMT
FROM:    Luca Izzo at DARK/NBI  <luca.izzo@gmail.com>

L. Izzo (DARK/NBI), D. B. Malesani (DTU Space) and D. A. Kann (HETH, IAA/CSIC) report:

We observed the field of GRB 201216C (Beardmore et al., GCN #29061, Fermi GBM team, GCN #29063) using the ESO VLT UT3 (Melipal) equipped with the X-shooter acquisition camera. Observations started at 01:18:47 UT on 2020-12-17 (2.19 hr after the BAT trigger) and consisted of 3x40 s, 3x30 s, 3x60 s exposures obtained in the Sloan g', r', z' bands, respectively.

We detect a new source at coordinates RA: 01:05:28.980, Dec: +16:31:00.0 (J2000), consistent with the Swift-XRT refined position (Campana et al., GCN #29064). No source is detected in archival Pan-STARRS images at this position, we therefore consider it to be the afterglow of GRB 201216C. From the stacked r'-band image we report a preliminary magnitude of 21.81+-0.05 mag (AB).
We acknowledge excellent support from the ESO observing staff in Paranal, in particular Zahed Wahhaj and Bin Yang.


GRB_name: GRB201216C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29067
SUBJECT: GRB 201216C: Enhanced Swift-XRT position
DATE:    20/12/17 05:30:00 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 656 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 201216C, 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 = 16.37032, +16.51612 which is equivalent
to:

RA (J2000): 01h 05m 28.88s
Dec (J2000): +16d 30' 58.0"

with an uncertainty of 1.6 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB201216A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29069
SUBJECT: GRB 201216A: Swift-XRT observations
DATE:    20/12/17 09:36:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the Fermi-GBM and
Swift/BAT-detected burst GRB 201216A (GBM team, GCN Circ. 29057;
Tohuvavohu et al. GCN Circ. 29059), collecting 4.9 ks of Photon
Counting (PC) mode data between T0+21.5 ks and T0+34.2 ks. 

No X-ray sources have been detected consistent with being within 197
arcsec of the Swift/BAT position. The 3-sigma upper limit in the field
ranges from ~0.002 to ~0.003 ct s^-1, corresponding to a 0.3-10 keV
observed flux of 7.3e-14 to 1.1e-13 erg cm^-2 s^-1 (assuming a typical
GRB spectrum).

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

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00021408.

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


GRB_name: GRB201216C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29070
SUBJECT: GRB 201216C: FRAM-ORM afterglow confirmation
DATE:    20/12/17 11:16:09 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 GRB201216C (Beardmore et al GCNC 29061, Fermi/GBM team GCNC
29063, Campana et al. GCNC 29064 and Osborne et al. GCNC 29067), obtaining
a series of 20s unfiltered images starting at 23:08:04.3 UT, i.e. 31.6s
post trigger.

We clearly detect the source reported by Izzo et al. (GCNC 29066) at the
VLT. The observations by FRAM cover the onset of the afterglow and its
peak. The joint fit of our final points from ~1ks post trigger and the VLT
point provide a power-law decay rate of ~1.07, all of these confirm the
afterglow nature of the transient and provide an extrapolation of the
brightness to r~24.6 for the next night.


GRB_name: GRB201216C
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29071
SUBJECT: GRB 201216C: Swift/UVOT Upper Limits
DATE:    20/12/17 11:19:46 GMT
FROM:    Samantha Oates at MSSL  <samantha.oates@alumni.ucl.ac.uk>

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

The Swift/UVOT began settled observations of the field of GRB 201216C
2970 s after the BAT trigger (Beardmore et al., GCN Circ. 29061).
No optical afterglow consistent with the enhanced XRT position
(Osborne et al. GCN Circ. 29067) or the VLT position
(Izzo et al., GCN Circ. 29066) 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          2970         3120          147         >20.0
white             2970         3739          344         >20.7
v                 3950         4150          197         >19.1
b                 3334         3534          197         >19.9
u                 3129         3329          197         >19.3
m2                4154         4331          174         >19.3
w2                3745         3945          197         >19.7

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


GRB_name: GRB201216A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29072
SUBJECT: GRB 201216A: Fermi GBM detection
DATE:    20/12/17 15:01:51 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

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

"At 19:00:31.24 UT on 16 December 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 201216A (trigger 629838036 / 201216792),
which was also detected by the Swift/BAT (Tohuvavohu et al. 2020, GCN 29059)
and initiated a Swift/XRT ToO (Evans 2020, GCN 29065).
The Fermi GBM Final Real-time Localization (GCN 29057) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 30 degrees.

The GBM light curve consists of a main peak followed by multiple subsequent peaks.
The duration (T90) is about 25.6 s (50-300 keV).
The time-averaged spectrum from T0-10 s to T0+13 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.51 +/- 0.22 and
the cutoff energy, parameterized as Epeak, is 263 +/- 55 keV.

The event fluence (10-1000 keV) in this time interval is
(2.343 +/- 0.330)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+64 ms in the 10-1000 keV band
is 1.6 +/- 0.2 ph/s/cm^2.

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

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


GRB_name: GRB201216C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29073
SUBJECT: GRB 201216C: Fermi GBM detection
DATE:    20/12/17 15:03:27 GMT
FROM:    Christian Malacaria at NASA-MSFC/USRA  <cmalacaria@usra.edu>

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

"At 23:07:25.75 UT on 16 December 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 201216C (trigger 629852850 / 201216963),
which was also detected by the Swift/BAT (Beardmore et al. 2020, GCN 29061).
The Fermi GBM Final Real-time Localization (GCN 29063) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 94 degrees.

GRB 201216C is particularly bright and hard.
The GBM light curve shows a broad, structured peak
with a duration (T90) of about 29.9 s (50-300 keV).
The time-averaged spectrum from T0-0.003 s to T0+49.665 s is
best fit by a Band function with Epeak = 326 +/- 7  keV,
alpha = -1.06 +/- 0.01, and beta = -2.25 +/- 0.03.

The event fluence (10-1000 keV) in this time interval is
(1.41 +/- 0.06)E-4 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+24.8 s in the 10-1000 keV band
is 54.9 +/- 0.6 ph/s/cm^2.

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

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


GRB_name: GRB201216C
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29074
SUBJECT: GRB 201216C: AstroSat CZTI detection
DATE:    20/12/17 15:10:28 GMT
FROM:    Gaurav Waratkar at IIT Bombay  <gauravwaratkar24@gmail.com>

D. Nadella (NITK), G. Waratkar (IITB), A. Vibhute (IUCAA), S. Gupta 
(IUCAA), P. Sawant (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (IUCAA), 
A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the 
AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al, 
2020, arxiv:2011.07067) showed detection of a bright long GRB 201216C, 
which was also detected by Swift BAT (GCN #29061) and Fermi GBM (GCN 
#29063).

The source was clearly detected in the 20-200 keV energy range. The 
light curve showed multiple peaks of emission with the strongest peak at 
2020-12-16 23:07:47.500 UT. The measured peak count rate associated with 
the burst is 1160 (+72, -40) cts/s above the background in the combined 
data of four quadrants, with a total of 18073 (+682, -728) cts. The 
local mean background count rate was 652 (+4, -4) cts/s. Using 
cumulative rates, we measure a T90 of 29 (+2, -2) s.

It was also clearly detected in the CsI anticoincidence (Veto) detector 
in the 100-500 keV energy range. The light curve showed multiple peaks 
of emission with the strongest peak at 2020-12-16 23:07:47.247 UT. The 
measured peak count rate is 1679 (+106, -78) cts/s above the background 
in the combined Veto data of four quadrants, with a total of 22904 
(+1443 -1654) cts. The local mean background count rate was 2400 (+7, 
-8) cts/s. We measure a T90 of 26 (+4, -2) s from the cumulative Veto 
light curve.

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


GRB_name: GRB201216C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29075
SUBJECT: GRB 201216C: MAGIC detection in very high energy gamma rays
DATE:    20/12/17 17:23:13 GMT
FROM:    Oscar Blanch at MAGIC Collaboration  <blanch@ifae.es>

O.Blanch (IFAE-BIST Barcelona), F. Longo (University and INFN Trieste), A. Berti (INFN Torino),
S. Fukami (ICRR University of Tokyo), Y. Suda (MPP Munich), S. Loporchio (University and INFN Bari), 
S. Micanovic (University of Rijeka), J. G. Green (INAF Rome), V. Pinter (IFAE-BIST), 
M. Takahashi (ICRR University of Tokyo), on behalf of the MAGIC collaboration report:

On December 16, 2020, the MAGIC telescopes observed GRB 201216C following the
trigger by Swift-BAT and Fermi-GBM (Beardmore et al., GCN 29061, Fermi/GBM team GCN 29063).
MAGIC started observations under good conditions about 57 seconds after the GRB onset.
The preliminary offline analyses show an excess above 5 sigma, compatible with the GRB position reported
by the Swift and Fermi teams. Refined off-line analyses of the data are ongoing.

We strongly encourage follow-up observations by other instruments at all wavelengths.

The MAGIC point of contact for this burst is O. Blanch (blanch@ifae.es). 
Burst Advocate for this burst is F. Longo (francesco.longo@ts.infn.it).

MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes
located at the Observatory Roque de los Muchachos on the Canary island
La Palma, Spain, and designed to perform gamma-ray astronomy in the energy
range from 50 GeV to greater than 50 TeV.


-- 
Avs -
Aviso - Legal Notice - (LOPD) - http://legal.ifae.es 
<http://legal.ifae.es/>


GRB_name: GRB201216C
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29076
SUBJECT: GRB 201216C: Fermi-LAT upper limit
DATE:    20/12/17 19:15:12 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico and INFN Bari), N. Omodei (Stanford University),
D. Kocevski (UAH), M. Axelsson (KTH & Stockholm Univ.),
F. Longo (University and INFN Trieste), and E. Moretti (IFAE-BIST Barcelona)
report on behalf of the Fermi-LAT Collaboration:


Fermi-LAT observed the position of GRB 201216C, which was detected
by Fermi-GBM (GCN Circ. 29073), Swift (GCN Circ. 29061, 29064),
and MAGIC (GCN Circ. 29075).
The GRB position was not in the LAT field of view at the time
of the GBM trigger (T0 = 2019-12-16, 23:07:25.75 UT), and was not visible
until ~T0+3500 s. The position remained visible until ~T0+5500 s.

No significant high-energy gamma-ray emission associated with this burst
was detected by the LAT in this time interval.

A LAT upper limit (95% confidence level, 100 MeV - 1 GeV), assuming a
photon index of -2.0, covering the same time interval is 7.3E-7 ph/s/cm2.
The corresponding upper limit for energy flux is 3E-10 erg/s/cm2.

The Fermi-LAT point of contact for this burst is
Elena Moretti (moretti@ifae.es).


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: GRB201216C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29077
SUBJECT: GRB 201216C: VLT X-shooter spectroscopy and potential high redshift of a VHE-emitting GRB
DATE:    20/12/17 22:12:41 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

J.-B. Vielfaure (APC, Paris University), L. Izzo (DARK/NBI), D. Xu 
(NAOC), S. D. Vergani (GEPI, Observatoire de Paris), D. B. Malesani (DTU 
Space), A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), V. D'Elia 
(ASI/SSDC, INAF/OAR), J. P. U. Fynbo (DAWN/NBI), D. A. Kann 
(HETH/IAA-CSIC), A. J. Levan (Radboud U. Nijmegen), G. Pugliese (API, 
Univ. Amsterdam), N. R. Tanvir (Univ. Leicester), D. Burgarella (AMU, 
CNRS, CNES, LAM), and A. Rossi (INAF-OAS) report on behalf of the 
Stargate Consortium:

We obtained spectroscopic observations of the optical counterpart (Izzo 
et al., GCN #29066, Jelinek et al., GCN #29070) of the MAGIC-detected 
(Blanch et al., GCN #29075) GRB 201216C (Beardmore et al., GCN #29061, 
Malacaria et al., GCN #29073, Nadella et al., GCN #29074) with the ESO 
Very Large Telescope UT 3 (Melipal) equipped with the X-shooter 
spectrograph, covering the wavelength range 3200-22000 AA. Observations 
started at 01:30 UT on 2020-12-17, 2.38 hr after the burst, and 
consisted of 4 exposures of 600 s each.

The afterglow is well-detected in the stacked spectrum, but the 
continuum is very red. As a consequence, the S/N drops dramatically from 
the red to the blue end. We identify a doublet which we tentatively 
match to Ca II H & K at z = 1.10. Unfortunately, no other lines are 
detected to confirm this value, though most of them would fall in a 
spectral region of poor S/N. We note that Ca II H&K absorption is 
uncommon in intervening absorbers, making it likely this is the actual 
redshift of the GRB, and that it does not lie at an even greater 
distance (in accordance with the VHE detection).

A redshift of z = 1.1 would place this object among the most distant 
known VHE sources. Using the Fermi GBM parameters (Malacaria et al., GCN 
#29073), we derive a an observer-frame 10-1000 keV isotropic energy 
release of E_iso = (4.71 +/- 0.16) * 10^53 erg.

Based on our grz photometry (Izzo et al., GCN 29066), we measure a 
spectral slope beta_opt = 4.1 +- 0.2 (Fnu propto nu^-beta), which is an 
unusually red value, suggesting significant extinction. This is 
confirmed by the optical-to-X-ray spectral index, beta_OX ~ 0.1 which 
indicates a very low optical/X-ray flux ratio, making this a bona fide 
dark GRB.

We acknowledge excellent support from the ESO observing staff in 
Paranal, in particular, Diego Parraguez, Bin Yang, and Zahed Wahhaj.


GRB_name: GRB201217A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29078
SUBJECT: GRB 201217A: Fermi GBM Final Localization
DATE:    20/12/17 22:35:27 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 02:35:03.51 UT on 17 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201217A (trigger 629865308 / 201217108).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 273.3, Dec = -65.1 (J2000 degrees, equivalent to J2000 18h 13m, -65d 05'), with a statistical uncertainty of 3.2 degrees.

The angle from the Fermi LAT boresight is 82.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201217108/quicklook/glg_skymap_all_bn201217108.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/bn201217108/quicklook/glg_healpix_all_bn201217108.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201217108/quicklook/glg_lc_medres34_bn201217108.gif


GRB_name: GRB201217A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29079
SUBJECT: Fermi GRB 201217A: Global MASTER-Net observations report 
DATE:    20/12/18 01:30:28 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),

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 201217A ( Fermi GBM team, GCN 29078) errorbox  30237 sec after notice time and 81228 sec after trigger time at 2020-12-18 01:08:52 UT, with upper limit up to  13.1 mag. The observations began at zenith distance = 73 deg. The sun  altitude  is -17.1 deg. 

The galactic latitude b = -21 deg., longitude l = 329 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1505292

We obtain a following upper limits.  

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

   81259 | 2020-12-18 01:08:52 |         MASTER-OAFA | (18h 11m 02.61s , -66d 41m 50.5s) |   C |    60 | 13.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201216C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29080
SUBJECT: GRB 201216C: Swift-BAT refined analysis
DATE:    20/12/18 02:04:50 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), 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-240 to T+962 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 201216C (trigger #1013243)
(Beardmore et al., GCN Circ. 29061).  The BAT ground-calculated position is
RA, Dec = 16.364, 16.538 deg which is
   RA(J2000)  =  01h 05m 27.4s
   Dec(J2000) = +16d 32' 16.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~ T-16 s and ends at ~T+64 s. The main peak occurs at ~T+20 s.
T90 (15-350 keV) is 48.0 +- 16.0 sec (estimated error including
systematics).

The time-averaged spectrum from T-15.89 to T+64.11 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.43 +- 0.03.  The fluence in the 15-150 keV band is 4.5 +- 0.1 x 10^-5
erg/cm2.
The 1-sec peak photon flux measured from T+23.61 sec in the 15-150 keV band
is 18.0 +- 1.1 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/1013243/BA/


GRB_name: GRB201218A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29081
SUBJECT: GRB 201218A: Fermi GBM Final Real-time Localization
DATE:    20/12/18 04:24:37 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:14:15 UT on 18 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201218A (trigger 629957660.899176 / 201218177).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 286.9, Dec = 24.2 (J2000 degrees, equivalent to J2000 19h 07m, 24d 11'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 95.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201218177/quicklook/glg_skymap_all_bn201218177.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/bn201218177/quicklook/glg_healpix_all_bn201218177.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201218177/quicklook/glg_lc_medres34_bn201218177.gif


GRB_name: GRB201218A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29083
SUBJECT: GRB 201218A: BALROG localization (Fermi Trigger 629957660 / GRB 201218177)
DATE:    20/12/18 04:43:49 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
629957660 at 04:14:15 on 18 Dec. 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) = 287.38+/-0.29 deg
Decl.(2000.0) = 26.80+/-0.30 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201218177/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201218177/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201218177/json    


GRB_name: GRB201216C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29084
SUBJECT: Konus-Wind detection of GRB 201216C
DATE:    20/12/18 14:50:32 GMT
FROM:    Dmitry Frederiks at Ioffe Institute  <fred@mail.ioffe.ru>

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

The long GRB 201216C (Swift detection:  Beardmore et al., GCN 29061;
Fermi GBM detection:  Malacaria et al., GCN 29071;
AstroSat CZTI detection:  Nadella et al., GCN 29074;
MAGIC detection:  Blanch et al., GCN 29075)
triggered Konus-Wind (KW) at T0=83248.844 s UT (23:07:28.844).

The burst light curve shows a multi-peaked structure with the total duration of ~40 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/GRB201216_T83248/

As observed by Konus-Wind, the burst had
a fluence of (1.86 Â± 0.10)x10^-4 erg/cm^2 and
a 64-ms peak energy flux, measured from T0+24.704,
of (1.82 Â± 0.12)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+24.832 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.09 (-0.05,+0.06),
the high energy photon index beta = -2.32 (-0.13,+0.10),
the peak energy Ep = 333 (-28,+29) keV,
chi2 = 102/97 dof.

The spectrum near the peak count rate (measured from T0+18.944
to T0+26.368 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 = -0.99 (-0.05,+0.06),
the high energy photon index beta = -2.24 (-0.14,+0.10),
the peak energy Ep = 326 (-41,+47) keV,
chi2 = 121/97 dof.

Assuming the redshift z=1.1 (Vielfaure et al., GCN 29077)
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 = (6.2 Â± 0.6)x10^53 erg,
the peak luminosity L_iso = (1.3 Â± 0.1)x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum Ep,z=(700 Â± 61) keV.
With these values, GRB 201216C is within 68% prediction bands
for both 'Amati' and 'Yonetoku' relations built for the sample
of long KW GRBs with known redshifts (part I: Tsvetkova et al., ApJ 850 161, 2017;
part II: Tsvetkova et al., ApJ, submitted),
see http://www.ioffe.ru/LEA/GRBs/GRB201216_T83248/GRB201216C.pdf


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


GRB_name: GRB201216C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29085
SUBJECT: GRB 201216C: Liverpool Telescope First Hour Observations
DATE:    20/12/18 14:51:28 GMT
FROM:    Manisha Shrestha at Liverpool John Moores U  <m.shrestha@ljmu.ac.uk>

M. Shrestha (Liverpool JMU), A. Melandri (INAF), R. Smith (LJMU) , I.A. Steele (LJMU), S. Kobayashi (LJMU), C. Mundell (Univ. Bath), A. Gomboc (Univ. Nova Gorica), C. Guidorzi (Univ. Ferrara)  report on behalf of a wider collaboration:



We observed the field of Swift GRB 201216C (GCN 29061) with the 2.0m Liverpool Telescope (LT), La Palma on 2020 Dec 16 starting at 23:10:29.13 UT using the IO:O optical camera in the r bands.  Data was calibrated with respect to nearby APASS secondary standard stars.



We confirm the optical counterpart reported by Swift UVOT and VLT (GCN 29066).



At T=177 seconds after the BAT trigger time, we measure r = 18.38. The r band light curve made along with VLT (GCN 29066) data point and inferred data from FRAM-ORM (GCN 29070) show a power law decay in flux vs time with alpha = 1. From the light curve, LT observations seem to be around the peak of afterglow.







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GRB_name: GRB201216C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29086
SUBJECT: GRB201216C: No significant detection in HAWC
DATE:    20/12/18 17:04:28 GMT
FROM:    Hugo Ayala at Pennsylvania State University  <hgayala@psu.edu>

On 2020/12/16 at 23:07:31 UTC, following the trigger by Swift-BAT
and Fermi-GBM (GCN 29061, GCN 29063), HAWC observed the
position of GRB 201216C.

The position of the GRB at the time of trigger (t0) fell just inside the
field of
view of HAWC, at 40 deg from zenith. We observed the position in the time
range
[t0-100s,t0+3600s]. At the end of the analysis, the position was at 25 deg
from zenith.
We scanned this range with time bins of 100s width. The time window advances
every 20s, producing 80% overlap between different time windows.

No emission was observed. The most conservative
 flux upper-limit at 95% C.L. measured during the time range is

dN/dE = 4.05e-10 (E/TeV)^-2.0 [TeV^-1 cm^-2 s^-1]

HAWC is a very-high-energy gamma-ray observatory operating in Central
Mexico at latitude 19 deg. north. Operating day and night with over
95% duty cycle, HAWC has an instantaneous field of view of 2 sr and
surveys 2/3 of the sky every day. It is sensitive to gamma rays from
300 GeV to 100 TeV.


GRB_name: GRB201218A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29087
SUBJECT: Fermi GRB 201218A: Global MASTER-Net observations report 
DATE:    20/12/18 19:15:25 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),

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 201218A ( Fermi GBM team, GCN 29081) errorbox  53279 sec after notice time and 53345 sec after trigger time at 2020-12-18 19:03:21 UT, with upper limit up to  16.5 mag. Observations started at twilight.  The observations began at zenith distance = 64 deg. The sun  altitude  is -11.5 deg. 

The galactic latitude b =  7 deg., longitude l = 57 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1505659

We obtain a following upper limits.  

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

   22028 | 2020-12-18 10:20:53 |             MASTER- | (19h 12m 49.70s , +21d 30m 56.1s) |   C |    60 | 15.4 |        
   23215 | 2020-12-18 10:40:41 |             MASTER- | (19h 12m 56.18s , +21d 28m 59.3s) |   C |    60 | 13.0 |        
   53435 | 2020-12-18 19:03:21 |          MASTER-IAC | (19h 01m 57.16s , +23d 55m 31.2s) |   C |   180 | 16.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201218B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29088
SUBJECT: GRB 201218B: Fermi GBM Final Real-time Localization
DATE:    20/12/18 19:19:33 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 19:09:13 UT on 18 Dec 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201218B (trigger 630011358.922416 / 201218798).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 82.2, Dec = 26.4 (J2000 degrees, equivalent to J2000 05h 28m, 26d 23'), with a statistical uncertainty of 5.7 degrees.

The angle from the Fermi LAT boresight is 60.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201218798/quicklook/glg_skymap_all_bn201218798.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/bn201218798/quicklook/glg_healpix_all_bn201218798.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201218798/quicklook/glg_lc_medres34_bn201218798.gif


GRB_name: GRB201218B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29089
SUBJECT: Fermi GRB 201218B: Global MASTER-Net observations report 
DATE:    20/12/18 19:30:30 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),

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 201218B ( Fermi GBM team, GCN 29088) errorbox  486 sec after notice time and 588 sec after trigger time at 2020-12-18 19:19:02 UT, with upper limit up to  17.8 mag. Observations started at twilight.  The observations began at zenith distance = 70 deg. The sun  altitude  is -14.8 deg. 

The galactic latitude b = -4 deg., longitude l = 181 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1506140

We obtain a following upper limits.  

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

     252 | 2020-12-18 19:13:00 |             MASTER- | (05h 45m 58.58s , +27d 19m 06.2s) |   C |    50 | 15.6 |        
     252 | 2020-12-18 19:13:00 |             MASTER- | (05h 44m 02.34s , +25d 55m 42.8s) |   C |    50 | 15.7 |        
     317 | 2020-12-18 19:14:01 |             MASTER- | (05h 45m 47.34s , +27d 18m 10.9s) |   C |    60 | 15.7 |        
     317 | 2020-12-18 19:14:01 |             MASTER- | (05h 44m 18.35s , +25d 55m 09.0s) |   C |    60 | 15.8 |        
     648 | 2020-12-18 19:19:02 |          MASTER-IAC | (05h 26m 31.86s , +26d 23m 46.8s) |   C |   120 | 17.4 |        
     798 | 2020-12-18 19:21:21 |          MASTER-IAC | (05h 26m 37.93s , +26d 24m 01.9s) |   C |   140 | 17.6 |        
     977 | 2020-12-18 19:24:00 |          MASTER-IAC | (05h 26m 35.23s , +26d 25m 12.9s) |   C |   180 | 17.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB201218A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29090
SUBJECT: IPN triangulation of GRB 201218A
DATE:    20/12/19 01:12:10 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@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,

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Ridnaia,
and T. Cline on behalf of the Konus-Wind 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 long-duration, very bright GRB 201218A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 29081;
BALROG localization: Biltzinger et al., GCN Circ. 29083)
has been detected by Fermi (GBM trigger 629957660),
Konus-Wind,  Mars-Odyssey (HEND), and Swift (BAT),
so far, at about 15256 s UT (04:14:16).
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:
   288.498 (19h 13m 59s) +28.356 (+28d 21' 23")
  Corners:
   288.470 (19h 13m 53s) +28.144 (+28d 08' 38")
   288.400 (19h 13m 36s) +28.556 (+28d 33' 23")
   288.526 (19h 14m 06s) +28.569 (+28d 34' 08")
   288.596 (19h 14m 23s) +28.156 (+28d 09' 22")
  ---------------------------------------------
The error box area is 168 sq. arcmin, and its maximum
dimension is 26 arcmin (the minimum one is 6.7 arcmin).
The Sun distance was 56 deg.

The IPN localization is consistent with, but reduces the area of, the 
Fermi RoboBA and BALROG localizations (GCN Circ. 29081 and 29083).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB201218_T15255/IPN/

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


GRB_name: GRB201214A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29091
SUBJECT: GRB 201214A: 1.3m DFOT, optical upper limits
DATE:    20/12/19 18:14:24 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

Amit Kumar (ARIES), Rahul Gupta (ARIES), Neelam Panwar (ARIES), Dimple
(ARIES), Ankur Ghosh (ARIES), Avinash Singh (ARIES), Amar Aryan (ARIES),
Shashi B. Pandey (ARIES), and Kuntal Misra (ARIES) report:

We observed the field of INTEGRAL-detected burst GRB 201214A (Mereghetti et
al. GCN Circ. 29037; Evans et al., GCN 29036) with the 1.3m Devasthal Fast
Optical Telescope (DFOT) located at Devasthal observatory of Aryabhatta
Research Institute of Observational Sciences (ARIES), India. We observed a
series of images ~16.6 hours after the burst in both R and I (300sx3 in
each) filters (Johnson-Cousins) covering Swift XRT position (Kennea et al.,
GCN 29048). Preliminary photometry on the stacked images was performed and
calibrated against the USNO-B1 catalog stars. We do not detect any OT
candidate within the XRT position (see also Jelinek & Strobl GCN 29040).
The upper limits in the stacked images are the following:

DATE       UT (start)  Filter Exposure(sec) Frames    Upper limit (mag)
2020-12-14 22:51:42    R      300           3        21.5
2020-12-14 23:27:40    I      300           3        21.0

This circular may be cited.


GRB_name: GRB201214A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29092
SUBJECT: GRB 201214A: Swift-XRT afterglow detection
DATE:    20/12/19 19:28:30 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), T. Sbarrato (INAF-OAB), P.
D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), B. Sbarufatti (PSU)
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
INTEGRAL-detected burst GRB 201214A (Mereghetti et al. GCN Circ.
29037). The observations now extend from T0+5.3 ks to T0+378.1 ks. The
source previously reported by Kennea et al. (GCN Circ. 29048), "Source
2", is fading with 3-sigma significance, and is therefore likely the
GRB afterglow. Using 2671 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 = 170.92446,
+33.86930 which is equivalent to:

RA (J2000): 11h 23m 41.87s
Dec(J2000): +33d 52' 09.5"

with an uncertainty of 2.2 arcsec (radius, 90% confidence). This
position is 36 arcsec from the INTEGRAL position.  The source is fading
with alpha >0.6.

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.7 (+0.9, -0.7). The
best-fitting absorption column is  1.9 (+2.2, -1.6) x 10^21 cm^-2, in
excess of the Galactic value of 2.4 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 2.6 x 10^-11 (2.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.9 (+2.2, -1.6) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 1.8 sigma
Photon index:      2.7 (+0.9, -0.7)

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/ToO_GRBs/00021406/Source2.php.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00021406.

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


GRB_name: GRB201214A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  29093
SUBJECT: GRB 201214A: TSHAO optical upper limit
DATE:    20/12/19 22:01:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), N. Pankov (HSE), I. Reva (FAPHI), V. Kim (FAPHI), A. 
Pozanenko (IKI) report on behalf of GRB IKI FuN:

We observed the field of GRB 201214A (Mereghetti et al., GCN  29037) 
with Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory 
starting on Dec. 14 (UT) 18:15:39. We did not find any source in the 
enhanced XRT position  of an afterglow  (Kennea et al., GCN  29092), see 
also (Jelinek et. al GCN 29040; Kumar  et. al GCN 29091). Preliminary 
photometry of the filed is following.

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

2020-12-14 18:15:39 0.50959  R      22*90 n/d   n/d  21.1

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


