# GCN_circulars

GRB_name: GRB200306C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27338
SUBJECT: GRB200306C:  First Hour Liverpool Telescope Observations
DATE:    20/03/07 09:56:23 GMT
FROM:    Iain Steele at Liverpool/JMU  <i.a.steele@ljmu.ac.uk>

I.A.Steele (LJMU) reports on behalf of a larger collaboration:

The automated system of the Liverpool 2.0m telescope, La Palma, followed up GRB200306C starting at 23:01:37 UT (i.e. approximately 11 minutes post trigger) in the râ€™, iâ€™,and zâ€™ band filters for a period of 1 hour.

We clearly detect the afterglow reported in GCN numbers 27326, 27328, 27329, 27334 with a râ€™ band magnitude of 17.3 in our first frame calibrated with respect to a nearby APASS source.  The afterglow continues to fade over the course of the hour.









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GRB_name: GRB200306C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27339
SUBJECT: GRB 200306C: KCT upper limit of the optical afterglow
DATE:    20/03/07 14:23:18 GMT
FROM:    Gu Lim at Seoul National U  <lim9gu@gmail.com>

Gu Lim (SNU), Myungshin Im (SNU), Changbom Park (KIAS), Gregory S. H. Paek
(SNU) on behalf of GECKO

We carried out a follow-up observation of the afterglow of GRB 200306C
(Gropp et al GCNC 27326) using the 14-inch KCT (KIAS Chamnun Telescope) at
DeepSkyChile, Chile. A series of 30x120 s exposures on SDSS i-band were
obtained, starting at 04:37:13.849 UT on 06 March 2020.

We do not detect any sources on the stacked image at the previously
reported position of afterglow detections (Lipunov et al. GCN #27324, GCN
#27325, Jelinek et al. GCN #27328, Castro-Tirado et al. GCN #27329,
Moskvitin et al., GCN 27333, Izzo et al., GCN 27334, Kann et al., 27335).
After the flux calibration using SDSS dr12 photometric catalog, 5-sigma
detection limit is obtained as i > 18.40 AB magnitude.

KIAS Chamnun Telescope (KCT) is a 0.36m telescope of the Korea Institute
for Advanced Study (KIAS), recently installed at the DeepSkyChile site in
Chile. "Chamnun" is a Korean word for "True Eye", meaning the eye that can
see the truth.
Gravitational-wave EM Counterpart Korean Observatory (GECKO) is a network
of 10+ 0.5m to 1m class telescopes over the world.


á§


GRB_name: GRB200306A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27340
SUBJECT: GRB 200306A: AstroSat CZTI detection
DATE:    20/03/07 16:08:56 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 (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data showed the detection of the long GRB 200306A, which was also detected by Global MASTER-Net (Lipunov V. et al., GCN #27319), Swift (Simpson K. et al., GCN #27320) and Potential LCO (Strausbaugh R. et al., GCN #27321).
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 2020-03-06 00:19:55.46 UT. The measured peak count rate associated with the burst is 323 +/- 20.4 cts/s above the background in the combined data of four quadrants, with a total of 5603 +/- 41.2 cts. The local mean background count rate was 525 +/- 0.9 cts/s. Using cumulative rates, we measure a T90 of 33.7 +/- 0.07 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: GRB200306C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27341
SUBJECT: GRB 200306C: VIRT optical upper limits
DATE:    20/03/07 17:53:18 GMT
FROM:    Priyadarshini Gokuldass at U. of the Virgin Islands  <priyadass.94@gmail.com>

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


We observed the field of GRB200306C (Gropp et al., GCN 27326) with the 0.5m
Virgin Island Robotic Telescope (VIRT) at the University of the Virgin
Islands' Etelman Observatory on 03-07-2020 starting at 01:52:04 UT (T+3.0
hrs). We performed a series of exposures in R filter. The weather
conditions were clear during the hours of observation and the zenith angle
at the start of observations was 68 degrees and rising. We observed the
Swift XRT position with a 20'x20' field of view.

We find no new source at the position of previous optical
detections (Lipunov et al., GCN 27325, Jelinek et al., GCN 27328,
Castro-Tirado et al., GCN 27329, Moskvitin et al., GCN 27333, Izzo et al.,
GCN 27334, Kann et al., 27335) and report upper limits as follows:

T_mid       ||Exposure     ||Filter      ||Limit
T+3.3 hrs      ||1025s          ||R           ||18.0
T+4.0 hrs      ||3360s          ||R           ||19.0

The limits are estimated from comparison to nearby USNO B1 stars and are
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: GRB200306C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27342
SUBJECT: GRB 200306C: Enhanced Swift-XRT position
DATE:    20/03/07 18:07:44 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 1935 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 200306C, 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 = 198.55588, +11.26953 which is equivalent
to:

RA (J2000): 13h 14m 13.41s
Dec (J2000): +11d 16' 10.3"

with an uncertainty of 2.2 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB200306A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27343
SUBJECT: GRB 200306A: RATIR Optical Observations 
DATE:    20/03/07 21:07:13 GMT
FROM:    Alan M Watson at UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz
(UCSC), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Harvey
Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki
Toy (UMD) report:

We observed the field of GRB 200306A (Gropp et al., GCN Circ. 27326)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from 2020/03 7.27 to
2020/03 7.54 UTC (7.61 to 14.01 hours after the BAT trigger), obtaining
a total of 4.31 hours exposure in the r and i bands.

For a source within the Swift-XRT error circle, in comparison with the
SDSS DR9 catalog, we obtain the following 3-sigma upper limits :

  r > 23.34
  i > 23.71

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro 
MÃ¡rtir.


GRB_name: GRB200307A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27344
SUBJECT: GRB 200307A: Fermi GBM Final Real-time Localization
DATE:    20/03/07 21:37:14 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 21:26:59 UT on 7 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200307A (trigger 605309224.181756 / 200307894).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 84.2, Dec = -46.2 (J2000 degrees, equivalent to J2000 05h 36m, -46d 12'), with a statistical uncertainty of 22.5 degrees.

The angle from the Fermi LAT boresight is 13.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200307894/quicklook/glg_skymap_all_bn200307894.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/bn200307894/quicklook/glg_healpix_all_bn200307894.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200307894/quicklook/glg_lc_medres34_bn200307894.gif


GRB_name: GRB200306C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27345
SUBJECT: GRB 200306C: Swift-XRT refined Analysis
DATE:    20/03/07 23:02:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 6.0 ks of XRT data for GRB 200306C (Gropp et al. GCN
Circ. 27326), from 101 s to 18.9 ks after the  BAT trigger. The data
comprise 36 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Osborne et
al. (GCN Circ. 27342).

The late-time light curve (from T0+5.5 ks) can be modelled with a
power-law decay with a decay index of alpha=2.2 (+0.4, -0.3).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.56 (+0.11, -0.10). The
best-fitting absorption column is  4.1 (+3.0, -2.2) x 10^20 cm^-2,
consistent with the Galactic value of 1.9 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.2 x 10^-11 (4.4 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.1 (+3.0, -2.2) x 10^20 cm^-2
Galactic foreground: 1.9 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.56 (+0.11, -0.10)

If the light curve continues to decay with a power-law decay index of
2.2, the count rate at T+24 hours will be 4.4 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-14 (1.9 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00960102.

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


GRB_name: GRB200306A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27346
SUBJECT: GRB 200306A: Swift-BAT refined analysis
DATE:    20/03/07 23:12:45 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-240 to T+962 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200306A (trigger #959917)
(Simpson et al., GCN Circ. 27320).  The BAT ground-calculated position is
RA, Dec = 101.114, -62.010 deg which is
   RA(J2000)  =  06h 44m 27.3s
   Dec(J2000) = -62d 00' 34.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.

The mask-weighted light curve shows a few overlapping pulses
that starts at ~T-4 s and ends at ~T+50 s. The main peak
occurs at ~T+20 s. T90 (15-350 keV) is 32.87 +- 1.13 sec
(estimated error including systematics).

The time-averaged spectrum from T-3.67 to T+49.95 sec is best fit by a
power law
with an exponential cutoff.  This fit gives a photon index 1.06 +- 0.15,
and Epeak of 81.6 +- 6.9 keV (chi squared 32.91 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 1.0 +- 0.02 x 10^-5
erg/cm2
and the 1-sec peak flux measured from T+20.11 sec in the 15-150 keV band is
7.0 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.70 +- 0.03 (chi squared 98.65 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/959917/BA/


GRB_name: GRB200306C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27348
SUBJECT: GRB 200306C: Calar Alto 2.2m upper limit
DATE:    20/03/08 07:43:45 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), M. Blazek, C. C. Thoene, J. F. Agui Fernandez (all 
HETH/IAA-CSIC), R. Pedro Hedrosa, and E. Gallego (both CAHA) report:

We observed the field of the afterglow of GRB 200306C (Lipunov et al., 
GCNs #27324, #27325; Gropp et al., GCN #27326; Jelinek et al., GCN 
#27328; Hu et al., GCN #27329; Moskvitin, GCN #27333; Izzo &
Perley, GCN #27334; Kann et al., GCN #27335; Steele et al., GCN #27338) 
with the 2.2m telescope of Calar Alto equipped with CAFOS. We obtained 4 
x 720 s images in the Rc band under adverse conditions (moonlight, 
passing clouds, bright star still there).

Our stacked image centred at mean epoch 1.25519 d after the GRB shows no 
detection to a 3-sigma upper limit of Rc > 23.0 mag (AB). The magnitude 
limit was obtained versus SDSS stars in the field.


GRB_name: GRB200307A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27349
SUBJECT: Fermi  trigger No 605309224: Global MASTER-Net observations report 
DATE:    20/03/08 20:30:22 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-IAC robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 200307A ( Fermi GBM team, GCN 27344) errorbox  80771 sec after trigger time at 2020-03-08 19:53:10 UT, with upper limit up to  17.1 mag. Observations started at twilight.  The observations began at zenith distance = 75 deg. The sun  altitude  is -10.9 deg. 

The galactic latitude b = -32 deg., longitude l = 252 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1307366

We obtain a following upper limits.  

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

   75417 | 2020-03-08 18:23:26 |             MASTER- | (03h 15m 36.05s , -54d 03m 58.0s) |   C |    60 | 18.1 |        
   75787 | 2020-03-08 18:29:36 |             MASTER- | (03h 15m 40.56s , -54d 02m 21.4s) |   C |    60 | 17.9 |        
   76064 | 2020-03-08 18:34:13 |             MASTER- | (03h 25m 48.21s , -56d 02m 36.0s) |   C |    60 | 17.6 |        
   76064 | 2020-03-08 18:34:13 |             MASTER- | (03h 12m 53.59s , -56d 04m 03.5s) |   C |    60 | 18.2 |        
   76434 | 2020-03-08 18:40:23 |             MASTER- | (03h 25m 44.24s , -56d 03m 18.2s) |   C |    60 | 17.5 |        
   76434 | 2020-03-08 18:40:23 |             MASTER- | (03h 12m 49.40s , -56d 04m 42.9s) |   C |    60 | 18.2 |        
   77854 | 2020-03-08 19:04:03 |             MASTER- | (03h 37m 13.03s , -58d 02m 10.1s) |   C |    60 | 18.2 |        
   77854 | 2020-03-08 19:04:03 |             MASTER- | (03h 23m 36.28s , -58d 03m 36.8s) |   C |    60 | 18.2 |        
   78224 | 2020-03-08 19:10:13 |             MASTER- | (03h 37m 09.63s , -58d 02m 56.6s) |   C |    60 | 18.2 |        
   78224 | 2020-03-08 19:10:13 |             MASTER- | (03h 23m 32.70s , -58d 04m 21.9s) |   C |    60 | 18.2 |        
   78501 | 2020-03-08 19:14:50 |             MASTER- | (03h 42m 48.57s , -54d 01m 20.0s) |   C |    60 | 17.7 |        
   78501 | 2020-03-08 19:14:50 |             MASTER- | (03h 30m 32.77s , -54d 02m 43.6s) |   C |    60 | 17.9 |        
   78778 | 2020-03-08 19:19:27 |             MASTER- | (03h 31m 12.53s , -62d 03m 05.4s) |   C |    60 | 18.4 |        
   78871 | 2020-03-08 19:20:59 |             MASTER- | (03h 42m 51.44s , -54d 01m 21.9s) |   C |    60 | 17.7 |        
   78871 | 2020-03-08 19:20:59 |             MASTER- | (03h 30m 35.65s , -54d 02m 45.5s) |   C |    60 | 17.8 |        
   79148 | 2020-03-08 19:25:37 |             MASTER- | (03h 31m 05.18s , -62d 02m 05.3s) |   C |    60 | 18.4 |        
   79426 | 2020-03-08 19:30:15 |             MASTER- | (03h 32m 37.36s , -52d 03m 41.9s) |   C |    60 | 16.0 |        
   79426 | 2020-03-08 19:30:15 |             MASTER- | (03h 20m 54.29s , -52d 05m 03.6s) |   C |    60 | 16.0 |        
   79796 | 2020-03-08 19:36:25 |             MASTER- | (03h 32m 42.52s , -52d 02m 01.5s) |   C |    60 | 14.8 |        
   79796 | 2020-03-08 19:36:25 |             MASTER- | (03h 20m 59.66s , -52d 03m 21.9s) |   C |    60 | 13.8 |        
   80537 | 2020-03-08 19:48:45 |             MASTER- | (03h 54m 22.18s , -56d 01m 04.6s) |   C |    60 | 12.5 |        
   80801 | 2020-03-08 19:53:10 |          MASTER-IAC | (04h 01m 18.77s , -42d 02m 56.1s) |   C |    60 | 16.0 |        
   80801 | 2020-03-08 19:53:10 |          MASTER-IAC | (03h 50m 29.24s , -41d 59m 08.7s) |   C |    60 | 15.6 |        
   81035 | 2020-03-08 19:57:04 |          MASTER-IAC | (03h 54m 02.04s , -40d 05m 26.5s) |   C |    60 | 16.4 |        
   81035 | 2020-03-08 19:57:04 |          MASTER-IAC | (03h 43m 31.17s , -40d 01m 35.4s) |   C |    60 | 15.9 |        
   81152 | 2020-03-08 19:59:01 |          MASTER-IAC | (03h 50m 33.11s , -42d 01m 10.6s) |   C |    60 | 16.1 |        
   81152 | 2020-03-08 19:59:01 |          MASTER-IAC | (04h 01m 23.43s , -42d 04m 60.0s) |   C |    60 | 16.4 |        
   81391 | 2020-03-08 20:03:00 |          MASTER-IAC | (03h 43m 33.08s , -40d 01m 24.5s) |   C |    60 | 16.2 |        
   81391 | 2020-03-08 20:03:00 |          MASTER-IAC | (03h 54m 04.42s , -40d 05m 16.0s) |   C |    60 | 16.7 |        
   81512 | 2020-03-08 20:05:01 |          MASTER-IAC | (03h 37m 17.78s , -38d 00m 07.6s) |   C |    60 | 16.5 |        
   81512 | 2020-03-08 20:05:01 |          MASTER-IAC | (03h 47m 31.50s , -38d 04m 01.6s) |   C |    60 | 16.7 |        
   81634 | 2020-03-08 20:07:02 |          MASTER-IAC | (04h 22m 50.91s , -42d 03m 38.7s) |   C |    60 | 16.8 |        
   81634 | 2020-03-08 20:07:02 |          MASTER-IAC | (04h 12m 00.42s , -41d 59m 49.2s) |   C |    60 | 16.4 |        
   81755 | 2020-03-08 20:09:03 |          MASTER-IAC | (04h 14m 55.21s , -40d 02m 57.5s) |   C |    60 | 16.9 |        
   81755 | 2020-03-08 20:09:03 |          MASTER-IAC | (04h 04m 24.10s , -39d 59m 05.6s) |   C |    60 | 16.5 |        
   81757 | 2020-03-08 20:09:06 |             MASTER- | (03h 46m 12.22s , -64d 02m 32.7s) |   C |    60 | 13.6 |        
   81874 | 2020-03-08 20:11:03 |          MASTER-IAC | (03h 37m 17.77s , -38d 01m 02.0s) |   C |    60 | 16.5 |        
   81874 | 2020-03-08 20:11:03 |          MASTER-IAC | (03h 47m 31.88s , -38d 04m 54.6s) |   C |    60 | 16.7 |        
   81995 | 2020-03-08 20:13:04 |          MASTER-IAC | (04h 22m 51.35s , -42d 04m 42.6s) |   C |    60 | 16.8 |        
   81995 | 2020-03-08 20:13:04 |          MASTER-IAC | (04h 12m 00.31s , -42d 00m 53.2s) |   C |    60 | 16.4 |        
   82112 | 2020-03-08 20:15:01 |          MASTER-IAC | (04h 15m 02.11s , -40d 04m 40.1s) |   C |    60 | 17.0 |        
   82112 | 2020-03-08 20:15:01 |          MASTER-IAC | (04h 04m 30.27s , -40d 00m 48.2s) |   C |    60 | 16.5 |        
   82231 | 2020-03-08 20:16:59 |          MASTER-IAC | (03h 41m 31.47s , -36d 04m 35.2s) |   C |    60 | 17.1 |        
   82348 | 2020-03-08 20:18:56 |          MASTER-IAC | (03h 51m 20.42s , -36d 01m 20.8s) |   C |    60 | 16.7 |        
   82348 | 2020-03-08 20:18:56 |          MASTER-IAC | (04h 01m 19.25s , -36d 05m 16.8s) |   C |    60 | 17.0 |        
   82584 | 2020-03-08 20:22:53 |          MASTER-IAC | (03h 41m 28.39s , -36d 05m 11.9s) |   C |    60 | 17.0 |        
   82702 | 2020-03-08 20:24:51 |          MASTER-IAC | (04h 01m 15.40s , -36d 03m 33.4s) |   C |    60 | 16.9 |        
   82702 | 2020-03-08 20:24:51 |          MASTER-IAC | (03h 51m 16.27s , -35d 59m 37.4s) |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200308A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27350
SUBJECT: GRB 200308A: Fermi GBM Final Real-time Localization
DATE:    20/03/08 22:45:34 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 22:35:15 UT on 8 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200308A (trigger 605399720.791064 / 200308941).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 327.4, Dec = -27.8 (J2000 degrees, equivalent to J2000 21h 49m, -27d 48'), with a statistical uncertainty of 11.9 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/bn200308941/quicklook/glg_skymap_all_bn200308941.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/bn200308941/quicklook/glg_healpix_all_bn200308941.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200308941/quicklook/glg_lc_medres34_bn200308941.gif


GRB_name: GRB200306A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27351
SUBJECT: GRB 200306A: Swift/UVOT Upper Limits
DATE:    20/03/08 22:55:27 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

GRB 200306A: Swift/UVOT Upper Limits

J. D. Gropp (PSU) and K. K. Simpson (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200306A
85 s after the BAT trigger (Simpson et al., GCN Circ. 27320).
No optical afterglow consistent with the optical position
(Strausbaugh et al., GCN Circ. 27321)
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            85          235          147         >21.0
white               85         6191          459         >20.7
v                 5049        11928         1011         >20.1
b                 4434        16845         1278         >20.5
u                  297         5864          351         >20.1
w1                5459         5659          197         >19.7
m2                5254         5454          197         >19.1
w2                4844        11087         1082         >20.3

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200306C
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27352
SUBJECT: GRB 200306C: Swift/UVOT Detection
DATE:    20/03/09 06:03:35 GMT
FROM:    Sam LaPorte at PSU  <sjl5346@psu.edu>

 GRB 200306C: Swift/UVOT Detection

J. D. Gropp (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200306C
118 s after the BAT trigger (Gropp et al., GCN Circ. 27326).

A fading source consistent with the positions reported by
FRAM-ORM (Jelinek et al., GCN Circ. 27238),
BOOTES-1 (Hu et al., GCN Circ. 27329),
SAO RAS (Moskvitin et al., GCN Circ. 27333)
Liverpool Telescope (Izzo et al., GCN Circ 27334)
and OSN (Kann et al., GCN Circ. 27335)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  13:14:13.46 = 198.55607 (deg.)
    Dec (J2000) = +11:16:11.7  =  11.26992 (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

u_fc           141             390               245
16.90+-0.05
u                899           1049               147
18.39+-0.16


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: GRB200306C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27353
SUBJECT: GRB 200306C: Swift-BAT refined analysis
DATE:    20/03/09 06:03:42 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), 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+1065 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200306C (trigger #960102)
(Gropp et al., GCN Circ. 27326).  The BAT ground-calculated position is
RA, Dec = 198.577, 11.263 deg which is
   RA(J2000)  =  13h 14m 18.6s
   Dec(J2000) = +11d 15' 47.7"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 42%.

The mask-weighted light curve shows several overlapping pulses
that start at ~T-12 s and end at ~T+50 s. T90 (15-350 keV)
is 53.5 +- 12.8 sec (estimated error including systematics).

The time-averaged spectrum from T-12.33 to T+50.70 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
0.83 +- 0.12.  The fluence in the 15-150 keV band is 2.8 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+3.45 sec in the 15-150 keV band
is 1.3 +- 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/960102/BA/


GRB_name: GRB200306C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27354
SUBJECT: GRB 200306C: ALMA 3mm upper limit
DATE:    20/03/09 14:01:36 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (University of Bath), S. Bhandari (CSIRO), K. D. Alexander
(Northwestern), E. Berger (Harvard), W. Fong (Northwestern), R. Margutti
(Northwestern), C. G. Mundell (University of Bath), and P. Schady
(University of Bath) report on behalf of a larger collaboration:

"We observed GRB 200306C (Gropp et al., GCN 27326) with the Atacama Large
Millimeter/Submillimeter Array (ALMA) at 97.5 GHz over two epochs:

(i) on 2020 March 08 beginning at 05:08:54 UT (at a mean time of 0.99 d
after the burst),  and
(ii) on 2020 March 09 beginning at 05:46:00 UT (at a mean time of 2.01 d
after the burst).

No mm-band emission is detected at the optical position (Gropp et al., GCN
27326; Moskvitin, GCN 27333) in either epoch. Preliminary 3-sigma upper
limits are ~ 100 uJy and ~ 120 uJy from the individual observations and ~
80 uJy from stacking the two epochs.

We thank the JAO staff, AoD, P2G, and the entire ALMA team for their help
with scheduling and executing these observations."


GRB_name: GRB200310A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27355
SUBJECT: GRB 200310A: MAXI/GSC detection
DATE:    20/03/10 11:52:04 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro.hitoshi@nihon-u.ac.jp>

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

The MAXI/GSC nova alert system triggered on a bright uncatalogued X-ray transient source 
at 09:23:08 UT on March 10, 2020. Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (227.499 deg, 48.325 deg) = (15 09 59, +48 19 31) (J2000)
with a 90% C.L. statistical error of 0.44 deg and an additional systematic uncertainty of 
0.1 deg (90% containment radius).
Without assuming the source constancy, we obtain a rectangular 
error box (90%C.L.) with the following corners: 
(225.938, 49.050) deg = (15 03 45, +49 02 59) (J2000) 
(225.620, 48.200) deg = (15 02 28, +48 12 00) (J2000) 
(229.907, 47.407) deg = (15 19 37, +47 24 25) (J2000) 
(230.291, 48.244) deg = (15 21 09, +48 14 38) (J2000)
There is an additional systematic uncertainty of 0.2 deg (90% containment radius).

The X-ray flux averaged over the scan was 71 +- 17 mCrab (4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at 07:50 UT,
and in the next transit at 10:56 UT with an upper limit of 20 mCrab for each.


GRB_name: GRB200307A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27356
SUBJECT: GRB 200307A: Updated localization from Fermi/GBM and Swift/BAT-GUANO
DATE:    20/03/10 20:06:13 GMT
FROM:    Adam Goldstein at Fermi-GBM, USRA  <adam.michael.goldstein@gmail.com>

Adam Goldstein (USRA), Aaron Tohuvavohu (U Toronto), Jimmy DeLaunay (Penn
State), and Jamie Kennea (Penn State) report on behalf of Fermi/GBM and
Swift/BAT:



The Fermi/GBM Flight-Position notice, distributed at T0+7 seconds, from the
Fermi/GBM detected GRB 200307A (GCN. 27344) triggered the  Swift Mission
Operations Center operated Gamma-ray Urgent Archiver for Novel
Opportunities (GUANO; Tohuvavohu et al. 2020, in prep). Upon trigger by the
Fermi 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 GRB 200307A. All the requested event mode data was delivered to
the ground.



In a ground analysis of the event data, we detect GRB 200307A, determine
the signal in BAT is of astrophysical origin, and can confidently rule out
an origin from inside the contemporaneous BAT field-of-view. At T0, the
Earth's position and size relative to Swift were:



Earth RA: 30.0439

Earth Dec: 5.2549

Earth Radius: 67.139 deg



The Earth, with respect to Swift, occulted over 60% of the Fermi/GBM
localization region and can be ruled out for the GRB localization.



Fermi GBM provides an updated map by removing the Earth-occulted regions
and can be found at the following links:



Skymap image:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200307894/quicklook/glg_skymap_all_bn200307894.png



HEALPix:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200307894/quicklook/glg_healpix_all_bn200307894.fit



The 50% confidence region has decreased from 885 square degrees to 290
square degrees and the 90% confidence region has decreased from 2784 square
degrees to 978 square degrees.


GRB_name: GRB200311A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27363
SUBJECT: GRB 200311A: Fermi GBM Final Real-time Localization
DATE:    20/03/11 15:24:19 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 15:16:12 UT on 11 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200311A (trigger 605632577.928052 / 200311636).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 204.0, Dec = -49.7 (J2000 degrees, equivalent to J2000 13h 35m, -49d 42'), with a statistical uncertainty of 1.0 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/bn200311636/quicklook/glg_skymap_all_bn200311636.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/bn200311636/quicklook/glg_healpix_all_bn200311636.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200311636/quicklook/glg_lc_medres34_bn200311636.gif


GRB_name: GRB200311A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27365
SUBJECT: GRB 200311A: AGILE/MCAL and scientific ratemeters observations
DATE:    20/03/11 18:54:28 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), F. Longo (Univ. Trieste and INFN Trieste), M. Pilia
(INAF/OA-Cagliari), 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),
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 burst GRB 200311A reported by
Fermi/GBM (GCN #27363), that also triggered the automatic AGILE
Mini-CALorimeter (MCAL) GRB alert Notice (ID 511024575), published at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.

The event is visible in the scientific ratemeters (RMs) of the
Anti-Coincidence (AC, 50-200 keV) and MCAL (0.4-100 MeV) detectors. The
burst light curve shows a multi-peaked profile, lasting ~25 s and releasing
~33000 counts in the MCAL RMs. The ratemeters light curves can be found at
http://www.agilescienceapp.it/notices/GRB_066883_511024575.756958_RM.png.

The event also triggered an MCAL data acquisition at T0 = 2020-03-11
15:16:15.75 +/- 0.01 s (UTC), lasting ~10 s and releasing a total number of
~7550 counts in the detector, above a background rate of ~700 Hz. The MCAL
light curve can be found at:
http://www.agilescienceapp.it/notices/GRB_066883_511024575.756958.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.


GRB_name: GRB200307A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27367
SUBJECT: IPN triangulation of GRB 200307A (short)
DATE:    20/03/11 21:19:58 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

A. Ridnaia, D. Svinkin, and K. Hurley, on behalf of the IPN,

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

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

and

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

The short-duration GRB 200307A (The Fermi GBM team,
GCN Circ. 27344; Goldstein et al., GCN Circ. 27356) was detected
by Fermi (GBM trigger 605309224), INTEGRAL (SPI-ACS), and
Swift (BAT), at about 77219 s UT (21:26:59).
The burst was outside the coded field of view of the BAT.

We have triangulated this GRB to a GBM-INTEGRAL annulus centered at
RA(2000)=81.577 deg (05h 26m 18s)  Dec(2000)=-38.418 deg (-38d 25' 05"),
whose radius is 32.263 +/- 3.868 deg (3 sigma).

The IPN localization is consistent with, but reduces the area of, the
joint Fermi-GBM/Swift-BAT one (GCN Circ. 27356).

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200307_T77219/IPN/


GRB_name: GRB200311A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27370
SUBJECT: Fermi  trigger No 605632577: Global MASTER-Net observations report 
DATE:    20/03/12 04:15:19 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200311A ( Fermi GBM team, GCN 27363) errorbox  30385 sec after trigger time at 2020-03-11 23:42:38 UT, with upper limit up to  17.9 mag. Observations started at twilight.  The observations began at zenith distance = 76 deg. The sun  altitude  is -10.6 deg. 

MASTER-IAC robotic telescope  located in Spain (IAC Teide Observatory) started inspect of the Fermi GRB 200311A errorbox  39226 sec after trigger time at 2020-03-12 02:09:59 UT, with upper limit up to  16.7 mag. The observations began at zenith distance = 79 deg. The sun  altitude  is -61.8 deg. 

The galactic latitude b = 12 deg., longitude l = 311 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1311002

We obtain a following upper limits.  

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

   30416 | 2020-03-11 23:42:38 |         MASTER-OAFA | (13h 33m 58.49s , -49d 55m 05.7s) |   C |    60 | 14.5 |        
   30781 | 2020-03-11 23:48:43 |         MASTER-OAFA | (13h 33m 50.99s , -49d 54m 03.4s) |   C |    60 | 15.4 |        
   30874 | 2020-03-11 23:50:17 |         MASTER-OAFA | (13h 46m 37.64s , -49d 54m 28.4s) |   C |    60 | 15.7 |        
   30965 | 2020-03-11 23:51:48 |         MASTER-OAFA | (13h 25m 57.05s , -47d 55m 01.5s) |   C |    60 | 16.0 |        
   31058 | 2020-03-11 23:53:20 |         MASTER-OAFA | (13h 37m 43.69s , -47d 55m 58.6s) |   C |    60 | 15.6 |        
   31240 | 2020-03-11 23:56:23 |         MASTER-OAFA | (13h 31m 03.43s , -51d 54m 32.2s) |   C |    60 | 16.7 |        
   31423 | 2020-03-11 23:59:25 |         MASTER-OAFA | (13h 21m 40.70s , -49d 53m 46.7s) |   C |    60 | 17.0 |        
   31515 | 2020-03-12 00:00:58 |         MASTER-OAFA | (13h 46m 16.75s , -49d 54m 16.0s) |   C |    60 | 16.3 |        
   31614 | 2020-03-12 00:02:36 |         MASTER-OAFA | (13h 37m 59.02s , -47d 54m 07.6s) |   C |    60 | 17.0 |        
   31705 | 2020-03-12 00:04:08 |         MASTER-OAFA | (13h 31m 01.12s , -51d 54m 57.3s) |   C |    60 | 17.4 |        
   31796 | 2020-03-12 00:05:39 |         MASTER-OAFA | (13h 21m 45.26s , -49d 54m 46.0s) |   C |    60 | 17.6 |        
   31887 | 2020-03-12 00:07:10 |         MASTER-OAFA | (13h 44m 02.54s , -51d 55m 02.3s) |   C |    60 | 17.5 |        
   31979 | 2020-03-12 00:08:41 |         MASTER-OAFA | (13h 49m 49.11s , -47d 54m 17.3s) |   C |    60 | 17.5 |        
   32252 | 2020-03-12 00:13:15 |         MASTER-OAFA | (13h 44m 02.79s , -51d 53m 12.0s) |   C |    60 | 17.8 |        
   32440 | 2020-03-12 00:16:22 |         MASTER-OAFA | (13h 49m 55.52s , -47d 53m 33.4s) |   C |    60 | 17.9 |        
   39256 | 2020-03-12 02:09:59 |          MASTER-IAC | (13h 21m 25.21s , -49d 54m 32.2s) |   C |    60 | 16.7 |        
   39861 | 2020-03-12 02:20:04 |          MASTER-IAC | (13h 21m 22.67s , -49d 54m 43.2s) |   C |    60 | 16.7 |        
   41037 | 2020-03-12 02:39:39 |             MASTER- | (13h 45m 21.20s , -49d 52m 09.1s) |   C |    60 | 17.1 |        
   41037 | 2020-03-12 02:39:39 |             MASTER- | (13h 34m 14.56s , -49d 53m 01.5s) |   C |    60 | 17.3 |        
   41130 | 2020-03-12 02:41:12 |             MASTER- | (13h 36m 48.75s , -47d 53m 11.9s) |   C |    60 | 15.7 |        
   41130 | 2020-03-12 02:41:12 |             MASTER- | (13h 26m 08.50s , -47d 54m 05.6s) |   C |    60 | 15.6 |        
   41222 | 2020-03-12 02:42:44 |             MASTER- | (13h 29m 49.21s , -51d 53m 59.9s) |   C |    60 | 18.3 |        
   41315 | 2020-03-12 02:44:17 |             MASTER- | (13h 44m 16.14s , -51d 54m 56.8s) |   C |    60 | 16.7 |        
   41407 | 2020-03-12 02:45:49 |             MASTER- | (13h 45m 22.86s , -49d 52m 17.4s) |   C |    60 | 16.1 |        
   41407 | 2020-03-12 02:45:49 |             MASTER- | (13h 34m 17.05s , -49d 53m 07.7s) |   C |    60 | 16.4 |        
   41499 | 2020-03-12 02:47:22 |             MASTER- | (13h 26m 05.07s , -47d 54m 54.6s) |   C |    60 | 13.5 |        
   41500 | 2020-03-12 02:47:22 |             MASTER- | (13h 36m 45.10s , -47d 54m 02.3s) |   C |    60 | 13.8 |        
   41592 | 2020-03-12 02:48:54 |             MASTER- | (13h 29m 54.43s , -51d 52m 21.2s) |   C |    60 | 17.4 |        
   41685 | 2020-03-12 02:50:27 |             MASTER- | (13h 44m 09.15s , -51d 54m 02.6s) |   C |    60 | 18.0 |        
   41777 | 2020-03-12 02:52:00 |             MASTER- | (13h 49m 56.03s , -47d 53m 15.9s) |   C |    60 | 16.7 |        
   42147 | 2020-03-12 02:58:10 |             MASTER- | (13h 49m 57.70s , -47d 53m 23.4s) |   C |    60 | 15.5 |        
   43079 | 2020-03-12 03:13:41 |             MASTER- | (13h 20m 33.19s , -49d 52m 24.0s) |   C |    60 | 16.5 |        
   43634 | 2020-03-12 03:22:56 |             MASTER- | (13h 20m 30.39s , -49d 52m 30.0s) |   C |    60 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200311A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27371
SUBJECT: GRB 200311A: AstroSat CZTI detection
DATE:    20/03/12 08:29:18 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 (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a GRB 200311A, which was also detected by Fermi GBM (GCN #27363), AGILE/MCAL (Ursi A. et al., GCN #27365) and Global MASTER-Net (Lipunov V. et al., GCN #27370).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 2020-03-11 15:16:13.516 UT. The measured peak count rate associated with the burst is 958 +/- 38.4 cts/s above the background in the combined data of four quadrants, with a total of 10660 +/- 42.9 cts. The local mean background count rate was 532 +/- 1.0 cts/s. Using cumulative rates, we measure a T90 of 30.5 +/- 0.03 s. In preliminary analysis, we find that 1186 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB200313A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27374
SUBJECT: GRB 200313A: Fermi GBM Final Real-time Localization
DATE:    20/03/13 01:51:55 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 01:41:36 UT on 13 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200313A (trigger 605756501.620896 / 200313071).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 75.8, Dec = 20.9 (J2000 degrees, equivalent to J2000 05h 03m, 20d 53'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 103.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200313071/quicklook/glg_skymap_all_bn200313071.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/bn200313071/quicklook/glg_healpix_all_bn200313071.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200313071/quicklook/glg_lc_medres34_bn200313071.gif


GRB_name: GRB200313A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27376
SUBJECT: Fermi  trigger No 605756501: Global MASTER-Net observations report 
DATE:    20/03/13 02:45:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-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 200313A ( Fermi GBM team, GCN 27374) errorbox  41 sec after notice time and 71 sec after trigger time at 2020-03-13 01:42:47 UT, with upper limit up to  17.4 mag. The observations began at zenith distance = 72 deg. The sun  altitude  is -35.1 deg. 

The galactic latitude b = -12 deg., longitude l = 182 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1312412

We obtain a following upper limits.  

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

      76 | 2020-03-13 01:42:47 |         MASTER-OAFA | (05h 02m 00.29s , +20d 57m 42.4s) |   C |    10 | 16.6 |        
     122 | 2020-03-13 01:43:29 |         MASTER-OAFA | (05h 01m 56.21s , +20d 59m 11.6s) |   C |    20 | 16.9 |        
     180 | 2020-03-13 01:44:21 |         MASTER-OAFA | (05h 01m 56.09s , +20d 57m 41.3s) |   C |    30 | 17.1 |        
     248 | 2020-03-13 01:45:24 |         MASTER-OAFA | (05h 01m 59.88s , +20d 59m 19.5s) |   C |    40 | 17.2 |        
     329 | 2020-03-13 01:46:35 |         MASTER-OAFA | (05h 01m 53.08s , +20d 58m 30.4s) |   C |    60 | 17.4 |        
     425 | 2020-03-13 01:48:06 |         MASTER-OAFA | (05h 01m 52.20s , +20d 59m 32.3s) |   C |    70 | 17.3 |        
     536 | 2020-03-13 01:49:48 |         MASTER-OAFA | (05h 01m 58.90s , +20d 58m 34.4s) |   C |    90 | 17.3 |        
     673 | 2020-03-13 01:51:49 |         MASTER-OAFA | (05h 01m 52.49s , +20d 57m 35.6s) |   C |   120 | 17.2 |        
     839 | 2020-03-13 01:54:20 |         MASTER-OAFA | (05h 01m 57.99s , +20d 58m 03.5s) |   C |   150 | 17.3 |        
    1035 | 2020-03-13 01:57:21 |         MASTER-OAFA | (05h 01m 55.87s , +20d 59m 18.9s) |   C |   180 | 17.2 |        
    1246 | 2020-03-13 02:00:53 |         MASTER-OAFA | (05h 01m 55.94s , +20d 57m 46.0s) |   C |   180 | 17.0 |        
    1458 | 2020-03-13 02:04:24 |         MASTER-OAFA | (05h 01m 58.08s , +20d 59m 23.5s) |   C |   180 | 16.7 |        
    1669 | 2020-03-13 02:07:55 |         MASTER-OAFA | (05h 01m 52.94s , +20d 58m 38.0s) |   C |   180 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200313A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27377
SUBJECT: GRB 200313A: BALROG localization (Fermi Trigger 605756501 / GRB 200313071)
DATE:    20/03/13 02:46:49 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
605756501 at 01:41:36 on 13 March 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) = 76.4+/-0.4 deg
Decl.(2000.0) = 21.7+/-0.3 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200313071/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200313071/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200313071/json

                        


GRB_name: GRB200313B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27379
SUBJECT: GRB 200313B: Fermi GBM Final Real-time Localization
DATE:    20/03/13 11:07:35 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 10:57:12 UT on 13 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200313B (trigger 605789837.130132 / 200313456).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 202.2, Dec = 40.5 (J2000 degrees, equivalent to J2000 13h 28m, 40d 30'), with a statistical uncertainty of 5.3 degrees.

The angle from the Fermi LAT boresight is 96.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200313456/quicklook/glg_skymap_all_bn200313456.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/bn200313456/quicklook/glg_healpix_all_bn200313456.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200313456/quicklook/glg_lc_medres34_bn200313456.gif


GRB_name: GRB200313B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27380
SUBJECT: Fermi  trigger No 605789837: Global MASTER-Net observations report 
DATE:    20/03/13 11:30:09 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),

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 200313B ( Fermi GBM team, GCN 27379) errorbox  277 sec after notice time and 306 sec after trigger time at 2020-03-13 11:02:18 UT, with upper limit up to  17.6 mag. Observations started at twilight.  The observations began at zenith distance = 66 deg. The sun  altitude  is -15.2 deg. 

The galactic latitude b = 75 deg., longitude l = 94 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1312669

We obtain a following upper limits.  

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

     336 | 2020-03-13 11:02:18 |         MASTER-Amur | (13h 59m 44.22s , +44d 04m 32.5s) |   C |    60 | 17.3 |        
     496 | 2020-03-13 11:04:57 |         MASTER-Amur | (13h 43m 27.40s , +46d 05m 54.5s) |   C |    60 | 17.4 |        
     740 | 2020-03-13 11:09:01 |         MASTER-Amur | (13h 29m 24.68s , +40d 04m 05.8s) |   C |    60 | 17.6 |        
     819 | 2020-03-13 11:10:21 |         MASTER-Amur | (13h 59m 47.11s , +44d 05m 39.2s) |   C |    60 | 17.6 |        
     979 | 2020-03-13 11:13:00 |         MASTER-Amur | (13h 43m 28.93s , +46d 05m 37.6s) |   C |    60 | 17.6 |        
    1297 | 2020-03-13 11:18:19 |         MASTER-Amur | (13h 29m 24.72s , +40d 05m 11.5s) |   C |    60 | 17.6 |        
    1376 | 2020-03-13 11:19:38 |         MASTER-Amur | (13h 39m 50.24s , +40d 03m 59.7s) |   C |    60 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200311A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27381
SUBJECT: IPN triangulation of GRB 200311A
DATE:    20/03/13 12:49:49 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

IPN triangulation of GRB 200311A

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

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

The long-duration GRB 200311A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27363;
AGILE-MCAL detection: Ursi et al., GCN Circ. 27365;
AstroSat-CZTI detection: Gupta et al., GCN Circ. 27371)
was detected by Fermi (GBM trigger  605632577), Konus-Wind,
INTEGRAL (SPI-ACS), AGILE-MCAL, and AstroSat-CZTI
at about 54973 s UT (15:16:13).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   209.245 (13h 56m 59s) -50.054 (-50d 03' 15")
  Corners:
   206.898 (13h 47m 35s) -52.496 (-52d 29' 46")
   211.898 (14h 07m 35s) -47.578 (-47d 34' 42")
   211.296 (14h 05m 11s) -47.578 (-47d 34' 39")
   206.215 (13h 44m 52s) -52.473 (-52d 28' 23")
  ---------------------------------------------
The error box area is 2.0 sq. deg, and its maximum
dimension is 6.1 deg (the minimum one is 21 arcmin).
The Sun distance was 117 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the 
Fermi-GBM final position (GCN Circ. 27363).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200311_T54974/IPN

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


GRB_name: GRB200313A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27383
SUBJECT: GRB 200313A: Fermi GBM detection
DATE:    20/03/13 19:20:45 GMT
FROM:    Stephen Lesage at Fermi-GBM Team  <sjl0014@uah.edu>

S. Lesage (UAH) and C. Meegan (UAH)

report on behalf of the Fermi GBM Team:


"At 01:41:36.62 UT on 13 March 2020, the Fermi Gamma-Ray Burst Monitor (GBM)

triggered and located GRB 200313A (trigger 605756501 / 200313071).


The location for this GRB was reported in the Fermi GBM Final Real-time

Localization GCN (GCN 27374).


The GBM light curve shows a single broad peak

with a duration (T90) of about 13.6 s (50-300 keV).

The time-averaged spectrum from T0 s to T0+22.5 s is

best fit by a Band function with Epeak = 279 +/- 10 keV,

alpha = -0.64 +/- 0.02, and beta = -1.84 +/- 0.02.


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

(7.37 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured

starting from T0+2.4 s in the 10-1000 keV band

is 57.0 +/- 0.7 ph/s/cm^2.


The spectral analysis results presented above are preliminary;

final results will be published in the GBM GRB Catalog:

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


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: GRB200313A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27385
SUBJECT: IPN triangulation of GRB 200313A
DATE:    20/03/15 16:56:10 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,

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

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

and

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

The long-duration GRB  200313A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27374;
Lesage and C. Meegan, GCN Circ. 27383;
BALROG localization: Biltzinger et al., GCN Circ. 27377)
has been detected by Fermi (GBM trigger 605756501), Konus-Wind,
INTEGRAL (SPI-ACS), and Mars-Odyssey (HEND), so far,
at about 6097 s UT (01:41:37).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    73.028 (04h 52m 06s) +24.623 (+24d 37' 24")
  Corners:
    73.480 (04h 53m 55s) +29.123 (+29d 07' 21")
    73.078 (04h 52m 19s) +35.837 (+35d 50' 13")
    72.077 (04h 48m 18s) +29.401 (+29d 24' 04")
    72.972 (04h 51m 53s) +19.772 (+19d 46' 18")
    74.907 (04h 59m 38s) +13.551 (+13d 33' 02")
    74.212 (04h 56m 51s) +20.241 (+20d 14' 26")
  ---------------------------------------------
The error box area is 18.9 sq. deg, and its maximum
dimension is 22 deg (the minimum one is 1.2 deg).
The Sun distance was 81 deg.

This box may be improved.

The localization is consistent with, but reduces
the area of, the final Fermi-GBM (GCN Circ. 27374) and
BALROG (GCN Circ. 27377) localizations.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200313_T06098/IPN/

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


GRB_name: GRB200313B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27386
SUBJECT: IPN triangulation of GRB 200313B (short)
DATE:    20/03/15 17:21:19 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, and

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

The short-duration GRB 200313B
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27379)
has been detected by Fermi (GBM trigger 605789837) and Konus-Wind, so 
far, at about 39432 s UT (10:57:12).

We have triangulated it to a Konus-GBM annulus centered at
RA(2000)=154.610 deg (10h 18m 26s) Dec(2000)=+8.761 deg (+8d 45' 41"),
whose radius is 60.602 +/- 2.419 deg (3 sigma).

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM one.

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200313_T39435/IPN/


GRB_name: GRB200317A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27392
SUBJECT: GRB 200317A: Fermi GBM Final Real-time Localization
DATE:    20/03/17 00:50:50 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 00:40:30 UT on 17 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200317A (trigger 606098435.488212 / 200317028).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 65.5, Dec = -46.3 (J2000 degrees, equivalent to J2000 04h 21m, -46d 17'), with a statistical uncertainty of 2.7 degrees.

The angle from the Fermi LAT boresight is 50.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200317028/quicklook/glg_skymap_all_bn200317028.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/bn200317028/quicklook/glg_healpix_all_bn200317028.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200317028/quicklook/glg_lc_medres34_bn200317028.gif


GRB_name: GRB200317A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27393
SUBJECT: Fermi  trigger No 606098435: Global MASTER-Net observations report 
DATE:    20/03/17 01:15:29 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-OAFA robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200317A ( Fermi GBM team, GCN 27392) errorbox  37 sec after notice time and 65 sec after trigger time at 2020-03-17 00:41:36 UT, with upper limit up to  20.0 mag. The observations began at zenith distance = 43 deg. The sun  altitude  is -24.3 deg. 

The galactic latitude b = -44 deg., longitude l = 252 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1315429

We obtain a following upper limits.  

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

      71 | 2020-03-17 00:41:36 |         MASTER-OAFA | (04h 16m 01.16s , -44d 46m 37.0s) |   C |    10 | 17.6 |        
     117 | 2020-03-17 00:42:17 |         MASTER-OAFA | (04h 16m 01.01s , -44d 45m 40.8s) |   C |    20 | 18.2 |        
     173 | 2020-03-17 00:43:08 |         MASTER-OAFA | (04h 16m 08.20s , -44d 46m 44.3s) |   C |    30 | 18.6 |        
     240 | 2020-03-17 00:44:10 |         MASTER-OAFA | (04h 16m 01.03s , -44d 47m 48.0s) |   C |    40 | 18.9 |        
     316 | 2020-03-17 00:45:21 |         MASTER-OAFA | (04h 16m 07.14s , -44d 47m 23.2s) |   C |    50 | 19.0 |        
     408 | 2020-03-17 00:46:43 |         MASTER-OAFA | (04h 16m 04.79s , -44d 45m 58.7s) |   C |    70 | 19.3 |        
     648 | 2020-03-17 00:50:18 |         MASTER-OAFA | (04h 21m 40.40s , -46d 21m 27.0s) |   C |   120 | 19.6 |        
     810 | 2020-03-17 00:52:50 |         MASTER-OAFA | (04h 21m 36.72s , -46d 19m 45.7s) |   C |   140 | 19.6 |        
    1001 | 2020-03-17 00:55:41 |         MASTER-OAFA | (04h 21m 36.73s , -46d 21m 43.2s) |   C |   180 | 19.9 |        
    1212 | 2020-03-17 00:59:12 |         MASTER-OAFA | (04h 21m 39.24s , -46d 20m 05.2s) |   C |   180 | 20.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200311A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27398
SUBJECT: Konus-Wind observation of GRB 200311A
DATE:    20/03/17 11:51:37 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 200311A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27363;
AGILE-MCAL detection: Ursi et al., GCN Circ. 27365;
AstroSat-CZTI detection: Gupta et al., GCN Circ. 27371;
IPN triangulation: Svinkin et al., GCN Circ. 27381)
triggered Konus-Wind at T0=54974.737 s UT (15:16:14.737).

The burst light curve shows a multipeaked structure
which starts at ~T0-0.8 s and has a total duration of ~65.2 s.
The emission is seen up to ~8 MeV.

As observed by Konus-Wind, the burst
had a fluence of 8.84(-0.76,+0.89)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.792 s,
of 1.56(-0.28,+0.28)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+64.512 s)
is best fit in the 20 keV - 8 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.93(-0.07,+0.08)
and Ep = 854(-112,+142) keV (chi2 = 113/81 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.1
(chi2 = 112/80 dof).

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+7.168 s)
is best fit in the 20 keV - 8 MeV range
by a power law with exponential cutoff model
with  alpha = -0.57(-0.08,+0.09)
and Ep = 957(-98,+114) keV (chi2 = 88/80 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 86/79 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200311_T54974/

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


GRB_name: GRB200313A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27399
SUBJECT: Konus-Wind observation of GRB 200313A
DATE:    20/03/17 13:49:15 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 200313A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27374;
Lesage and C. Meegan, GCN Circ. 27383;
BALROG localization: Biltzinger et al., GCN Circ. 27377;
IPN triangulation: Hurley et al., GCN Circ. 27385)
triggered Konus-Wind at T0=6098.088 s UT (01:41:38.088).

The burst light curve shows a multipeaked structure
which starts at ~T0-0.4 s and has a total duration of ~43 s.
The emission is seen up to ~6 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.46(-0.14,+0.15)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+2.528 s,
of 3.42(-0.52,+0.53)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+45.824 s)
is best fit in the 20 keV - 6 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.88(-0.10,+0.12),
the high energy photon index beta = -2.07(-0.17,+0.12),
the peak energy Ep = 442(-66,+77) keV
(chi2 = 70/75 dof).

The spectrum near the maximum count rate
(measured from T0+2.048 to T0+3.072 s)
is best fit in the 20 keV - 6 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.69(-0.13,+0.17),
the high energy photon index beta = -2.24(-0.21,+0.16),
the peak energy Ep = 424(-69,+70) keV
(chi2 = 61/58 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200313_T06098/

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


GRB_name: GRB200313B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27407
SUBJECT: Konus-Wind observation of GRB 200313B
DATE:    20/03/18 13:30:13 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

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

The short-duration GRB 200313B
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27379;
IPN triangulation: Svinkin et al., GCN Circ. 27386)
triggered Konus-Wind at T0=39435.021 s UT (10:57:15.021).

The burst light curve shows a single pulse
which starts at ~T0-0.5 s and has a total duration of ~1.4 s.
The emission is seen up to ~1 MeV.

As observed by Konus-Wind, the burst
had a fluence of 6.83(-2.07,+3.49)x10^-7 erg/cm2,
and a 16-ms peak flux, measured from T0-0.016 s,
of 1.90(-1.18,+1.53)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+0.256 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.71(-0.91,+1.65)
and Ep = 145(-55,+252) keV (chi2 = 31/26 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.8
(chi2 = 31/25 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200313_T39435/

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


GRB_name: GRB200318A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27412
SUBJECT: GRB 200318A: Fermi GBM Final Real-time Localization
DATE:    20/03/18 22:45:44 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:35:27 UT on 18 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200318A (trigger 606263732.221512 / 200318941).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 123.4, Dec = 59.1 (J2000 degrees, equivalent to J2000 08h 13m, 59d 06'), 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/bn200318941/quicklook/glg_skymap_all_bn200318941.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/bn200318941/quicklook/glg_healpix_all_bn200318941.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200318941/quicklook/glg_lc_medres34_bn200318941.gif


GRB_name: GRB200318A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27413
SUBJECT: Fermi  trigger No 606263732: Global MASTER-Net observations report 
DATE:    20/03/18 23:00:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200318A ( Fermi GBM team, GCN 27412) errorbox  55 sec after notice time and 82 sec after trigger time at 2020-03-18 22:36:50 UT, with upper limit up to  20.0 mag. The observations began at zenith distance = 42 deg. The sun  altitude  is -45.4 deg. 

The galactic latitude b = 34 deg., longitude l = 158 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1316766

We obtain a following upper limits.  

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

      93 | 2020-03-18 22:36:50 |      MASTER-Tavrida | (08h 19m 21.28s , +56d 57m 36.1s) |   C |    20 | 17.9 |        
     147 | 2020-03-18 22:37:39 |      MASTER-Tavrida | (08h 24m 37.29s , +56d 33m 38.1s) |   C |    30 | 18.3 |        
     182 | 2020-03-18 22:37:39 |      MASTER-Tavrida | (08h 24m 37.30s , +56d 33m 38.2s) |   C |   100 | 19.0 |  Coadd 
     198 | 2020-03-18 22:38:29 |      MASTER-Tavrida | (08h 24m 30.80s , +56d 32m 51.9s) |   C |    30 | 18.3 |        
     253 | 2020-03-18 22:39:20 |      MASTER-Tavrida | (08h 24m 30.94s , +56d 33m 52.4s) |   C |    40 | 18.5 |        
     324 | 2020-03-18 22:40:21 |      MASTER-Tavrida | (08h 24m 36.88s , +56d 32m 52.9s) |   C |    60 | 18.8 |        
     404 | 2020-03-18 22:40:21 |      MASTER-Tavrida | (08h 24m 36.88s , +56d 32m 52.9s) |   C |   220 | 19.6 |  Coadd 
     410 | 2020-03-18 22:41:41 |      MASTER-Tavrida | (08h 24m 31.25s , +56d 31m 52.8s) |   C |    70 | 19.0 |        
     510 | 2020-03-18 22:43:12 |      MASTER-Tavrida | (08h 24m 37.47s , +56d 32m 22.9s) |   C |    90 | 19.0 |        
     630 | 2020-03-18 22:45:02 |      MASTER-Tavrida | (08h 20m 46.62s , +59d 11m 30.9s) |   C |   110 | 19.2 |        
     785 | 2020-03-18 22:45:02 |      MASTER-Tavrida | (08h 20m 46.62s , +59d 11m 30.9s) |   C |   420 | 20.0 |  Coadd 
     776 | 2020-03-18 22:47:13 |      MASTER-Tavrida | (08h 20m 49.34s , +59d 13m 12.9s) |   C |   140 | 19.3 |        
     952 | 2020-03-18 22:49:54 |      MASTER-Tavrida | (08h 20m 43.99s , +59d 12m 16.3s) |   C |   170 | 19.5 |        
    1148 | 2020-03-18 22:53:05 |      MASTER-Tavrida | (08h 20m 44.65s , +59d 13m 13.8s) |   C |   180 | 19.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200319A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27415
SUBJECT: GRB 200319A: Fermi GBM Final Real-time Localization
DATE:    20/03/19 07:54:56 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 07:44:40 UT on 19 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200319A (trigger 606296685.320018 / 200319323).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 63.8, Dec = -20.9 (J2000 degrees, equivalent to J2000 04h 15m, -20d 53'), with a statistical uncertainty of 4.5 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/bn200319323/quicklook/glg_skymap_all_bn200319323.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/bn200319323/quicklook/glg_healpix_all_bn200319323.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200319323/quicklook/glg_lc_medres34_bn200319323.gif


GRB_name: GRB200319A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27416
SUBJECT: GRB 200319A: BALROG localization (Fermi Trigger 606296685 / GRB 200319323)
DATE:    20/03/19 08:05:17 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
606296685 at 07:44:40 on 19 March 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) = 63.2+/-5.0 deg
Decl.(2000.0) = -21.8+/-4.2 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200319323/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200319323/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200319323/json

                        


GRB_name: GRB200320A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27417
SUBJECT: GRB 200320A: Fermi GBM Final Localization
DATE:    20/03/20 15:45:19 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 09:56:46 UT on 20 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200320A (trigger 606391011 / 200320414). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 184.3, Dec = -38.7 (J2000 degrees, equivalent to J2000 12h 17m, -38d 42'), with a statistical uncertainty of 3.4 degrees. The angle from the Fermi LAT boresight is 79.0 degrees.

The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200320414/quicklook/glg_skymap_all_bn200320414.png

The HEALPix FITS file, including the estimated localization systematic, can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200320414/quicklook/glg_healpix_all_bn200320414.fit

The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200320414/quicklook/glg_lc_medres34_bn200320414.gif


GRB_name: GRB200320B
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27418
SUBJECT: GRB 200320B: MAXI/GSC detection
DATE:    20/03/21 14:13:23 GMT
FROM:    Hitoshi Negoro at Nihon U  <negoro.hitoshi@nihon-u.ac.jp>

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

The MAXI/GSC nova alert system triggered on a bright uncatalogued X-ray transient source 
at 13:12:27 UT on 2020 March 20. Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (125.923 deg, -75.733 deg) = (08 23 41, -75 43 58) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.68 deg and 0.65 deg, respectively. 
The roll angle of the long axis from the north direction is 59.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 65 +- 22 mCrab
(4.0-10.0keV, 1 sigma error).
Without the assumption on the source constancy, we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (129.795, -77.155) deg = (08 39 10, -77 09 18) (J2000)
(R.A., Dec) = (132.879, -76.048) deg = (08 51 30, -76 02 52) (J2000)
(R.A., Dec) = (123.641, -74.339) deg = (08 14 33, -74 20 20) (J2000)
(R.A., Dec) = (120.277, -75.319) deg = (08 01 06, -75 19 08) (J2000)

In the previous transit at 10:05 UT, a weak (30 +- 16 mCrab at 4-10 keV) enhancement 
was also recognized. There was no significant excess flux in the next transit 
at 14:45 UT with an upper limit of 20 mCrab.

Finally, we note that due to the poor statistics, we can not confirm that this event is a GRB.
Therefore, we also name the source MAXI J0823-757.


GRB_name: GRB200323A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27422
SUBJECT: GRB 200323A: Fermi GBM Final Real-time Localization
DATE:    20/03/23 18:56:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 18:46:32 UT on 23 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200323A (trigger 606681997.955906 / 200323782).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 156.5, Dec = -55.5 (J2000 degrees, equivalent to J2000 10h 26m, -55d 30'), with a statistical uncertainty of 1.4 degrees.

The angle from the Fermi LAT boresight is 18.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200323782/quicklook/glg_skymap_all_bn200323782.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/bn200323782/quicklook/glg_healpix_all_bn200323782.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200323782/quicklook/glg_lc_medres34_bn200323782.gif


GRB_name: GRB200323A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27423
SUBJECT: GRB 200323A: Fermi GBM detection
DATE:    20/03/23 22:23:15 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 18:46:32.96 UT on 23 March 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200323A (trigger 606681997 / 200323782).

The location for this GRB was reported in the Fermi GBM Final Real-time
Localization GCN (GCN 27422).

The angle from the Fermi LAT boresight at the GBM trigger time is 18
degrees.

The GBM light curve consists of of a single pulse
with a duration (T90) of about 2.1 s (50-300 keV).
The time-averaged spectrum from T0 to T0+3.6 s is
best fit by a Band function with Epeak = 63.0 +/- 3.7 keV,
alpha = -0.73 +/- 0.10, and beta = -2.50 +/- 0.09.

The event fluence (10-1000 keV) in this time interval is
(3.23 +/- 0.10)E-6 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.32 s in the 10-1000 keV band
is 25.60 +/- 0.44 ph/s/cm^2. The 64 ms peak photon flux measured
starting from T0+0.58 s in the same band
is 34.0 +/- 1.9 ph/s/cm^2.

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

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


GRB_name: GRB200323A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27424
SUBJECT: Fermi  trigger No 606681997: Global MASTER-Net observations report 
DATE:    20/03/24 01:45:15 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-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 200323A ( Fermi GBM team, GCN 27422) errorbox  17767 sec after trigger time at 2020-03-23 23:42:40 UT, with upper limit up to  18.1 mag. Observations started at twilight.  The observations began at zenith distance = 41 deg. The sun  altitude  is -13.9 deg. 

The galactic latitude b =  2 deg., longitude l = 284 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1320359

We obtain a following upper limits.  

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

      88 | 2020-03-23 18:47:55 |             MASTER- | (10h 21m 10.74s , -56d 03m 31.5s) |   C |    10 | 15.6 |        
      88 | 2020-03-23 18:47:55 |             MASTER- | (10h 07m 59.36s , -56d 04m 27.9s) |   C |    10 | 17.5 |        
     138 | 2020-03-23 18:48:40 |             MASTER- | (10h 21m 05.77s , -56d 04m 32.4s) |   C |    20 | 15.8 |        
     138 | 2020-03-23 18:48:40 |             MASTER- | (10h 07m 54.08s , -56d 05m 29.4s) |   C |    20 | 18.1 |        
     195 | 2020-03-23 18:49:32 |             MASTER- | (10h 21m 11.74s , -56d 04m 28.7s) |   C |    30 | 15.9 |        
     195 | 2020-03-23 18:49:32 |             MASTER- | (10h 08m 00.09s , -56d 05m 26.0s) |   C |    30 | 18.4 |        
     263 | 2020-03-23 18:50:35 |             MASTER- | (10h 21m 08.53s , -56d 02m 54.1s) |   C |    40 | 16.0 |        
     263 | 2020-03-23 18:50:35 |             MASTER- | (10h 07m 57.47s , -56d 03m 51.5s) |   C |    40 | 18.5 |        
     345 | 2020-03-23 18:51:48 |             MASTER- | (10h 21m 09.08s , -56d 04m 08.7s) |   C |    60 | 16.9 |        
     345 | 2020-03-23 18:51:48 |             MASTER- | (10h 07m 57.63s , -56d 05m 05.7s) |   C |    60 | 18.8 |        
     447 | 2020-03-23 18:53:20 |             MASTER- | (10h 21m 12.69s , -56d 02m 42.4s) |   C |    80 | 16.1 |        
     447 | 2020-03-23 18:53:20 |             MASTER- | (10h 08m 01.88s , -56d 03m 40.2s) |   C |    80 | 18.7 |        
     569 | 2020-03-23 18:55:12 |             MASTER- | (10h 21m 05.66s , -56d 03m 40.5s) |   C |   100 | 16.2 |        
     569 | 2020-03-23 18:55:12 |             MASTER- | (10h 07m 54.64s , -56d 04m 38.6s) |   C |   100 | 19.0 |        
     717 | 2020-03-23 18:57:25 |             MASTER- | (10h 30m 56.36s , -55d 21m 05.8s) |   C |   130 | 15.9 |        
     717 | 2020-03-23 18:57:25 |             MASTER- | (10h 17m 59.63s , -55d 22m 02.5s) |   C |   130 | 18.6 |        
     895 | 2020-03-23 19:00:07 |             MASTER- | (10h 31m 04.88s , -55d 22m 08.0s) |   C |   160 | 16.0 |        
     895 | 2020-03-23 19:00:07 |             MASTER- | (10h 18m 07.87s , -55d 23m 04.4s) |   C |   160 | 18.7 |        
    1097 | 2020-03-23 19:03:20 |             MASTER- | (10h 30m 58.45s , -55d 23m 11.3s) |   C |   180 | 16.1 |        
    1097 | 2020-03-23 19:03:20 |             MASTER- | (10h 18m 01.05s , -55d 24m 07.9s) |   C |   180 | 18.7 |        
    1310 | 2020-03-23 19:06:52 |             MASTER- | (10h 18m 08.64s , -55d 23m 56.9s) |   C |   180 | 18.9 |        
    1310 | 2020-03-23 19:06:52 |             MASTER- | (10h 31m 06.16s , -55d 23m 00.2s) |   C |   180 | 16.2 |        
    1522 | 2020-03-23 19:10:24 |             MASTER- | (10h 31m 02.53s , -55d 21m 37.4s) |   C |   180 | 16.2 |        
    1522 | 2020-03-23 19:10:24 |             MASTER- | (10h 18m 05.32s , -55d 22m 34.8s) |   C |   180 | 18.9 |        
    1734 | 2020-03-23 19:13:57 |             MASTER- | (10h 31m 03.28s , -55d 23m 16.0s) |   C |   180 | 16.1 |        
    1734 | 2020-03-23 19:13:57 |             MASTER- | (10h 18m 05.54s , -55d 24m 13.3s) |   C |   180 | 18.7 |        
    1887 | 2020-03-23 19:17:29 |             MASTER- | (10h 34m 46.22s , -55d 49m 20.9s) |   C |    60 | 15.6 |        
    1887 | 2020-03-23 19:17:29 |             MASTER- | (10h 21m 39.90s , -55d 50m 17.2s) |   C |    60 | 18.4 |        
    1979 | 2020-03-23 19:19:01 |             MASTER- | (10h 06m 11.14s , -55d 50m 40.0s) |   C |    60 | 16.0 |        
    3257 | 2020-03-23 19:40:19 |             MASTER- | (10h 34m 43.30s , -55d 51m 03.1s) |   C |    60 | 17.9 |        
    3257 | 2020-03-23 19:40:19 |             MASTER- | (10h 21m 36.46s , -55d 52m 02.7s) |   C |    60 | 18.0 |        
    3349 | 2020-03-23 19:41:52 |             MASTER- | (10h 06m 20.69s , -55d 51m 49.5s) |   C |    60 | 17.6 |        
    3442 | 2020-03-23 19:43:24 |             MASTER- | (10h 09m 37.09s , -57d 50m 00.4s) |   C |    60 | 17.2 |        
    3534 | 2020-03-23 19:44:57 |             MASTER- | (10h 31m 04.94s , -53d 51m 01.0s) |   C |    60 | 16.9 |        
    3534 | 2020-03-23 19:44:57 |             MASTER- | (10h 18m 35.95s , -53d 52m 03.0s) |   C |    60 | 17.0 |        
    3627 | 2020-03-23 19:46:29 |             MASTER- | (10h 39m 43.60s , -57d 49m 24.7s) |   C |    60 | 16.7 |        
    3627 | 2020-03-23 19:46:29 |             MASTER- | (10h 25m 54.01s , -57d 50m 23.7s) |   C |    60 | 16.7 |        
    3812 | 2020-03-23 19:49:35 |             MASTER- | (10h 09m 34.78s , -57d 49m 53.7s) |   C |    60 | 15.2 |        
    3905 | 2020-03-23 19:51:07 |             MASTER- | (10h 31m 07.95s , -53d 50m 31.0s) |   C |    60 | 15.9 |        
    3905 | 2020-03-23 19:51:07 |             MASTER- | (10h 18m 38.75s , -53d 51m 33.5s) |   C |    60 | 15.5 |        
    3997 | 2020-03-23 19:52:39 |             MASTER- | (10h 39m 38.15s , -57d 51m 10.5s) |   C |    60 | 15.4 |        
    3997 | 2020-03-23 19:52:39 |             MASTER- | (10h 25m 47.50s , -57d 52m 09.9s) |   C |    60 | 15.9 |        
   17797 | 2020-03-23 23:42:40 |         MASTER-OAFA | (10h 21m 36.06s , -55d 52m 31.9s) |   C |    60 | 17.3 |        
   18071 | 2020-03-23 23:47:13 |         MASTER-OAFA | (10h 18m 28.11s , -53d 52m 44.4s) |   C |    60 | 17.3 |        
   18162 | 2020-03-23 23:48:44 |         MASTER-OAFA | (10h 21m 32.24s , -55d 51m 42.7s) |   C |    60 | 17.7 |        
   18253 | 2020-03-23 23:50:16 |         MASTER-OAFA | (10h 35m 54.16s , -55d 52m 36.9s) |   C |    60 | 17.4 |        
   18435 | 2020-03-23 23:53:18 |         MASTER-OAFA | (10h 07m 22.16s , -55d 53m 34.4s) |   C |    60 | 18.1 |        
   18617 | 2020-03-23 23:56:20 |         MASTER-OAFA | (10h 10m 42.80s , -57d 53m 30.0s) |   C |    60 | 17.9 |        
   18708 | 2020-03-23 23:57:50 |         MASTER-OAFA | (10h 18m 34.61s , -53d 52m 09.8s) |   C |    60 | 17.4 |        
   18799 | 2020-03-23 23:59:22 |         MASTER-OAFA | (10h 32m 03.67s , -53d 52m 44.0s) |   C |    60 | 17.4 |        
   18890 | 2020-03-24 00:00:53 |         MASTER-OAFA | (10h 35m 47.66s , -55d 51m 42.2s) |   C |    60 | 17.5 |        
   18982 | 2020-03-24 00:02:24 |         MASTER-OAFA | (10h 07m 20.98s , -55d 52m 58.9s) |   C |    60 | 18.1 |        
   19073 | 2020-03-24 00:03:55 |         MASTER-OAFA | (10h 10m 39.03s , -57d 53m 55.4s) |   C |    60 | 17.9 |        
   19164 | 2020-03-24 00:05:27 |         MASTER-OAFA | (10h 32m 08.58s , -53d 53m 19.4s) |   C |    60 | 17.3 |        
   19255 | 2020-03-24 00:06:58 |         MASTER-OAFA | (10h 25m 46.65s , -57d 53m 33.6s) |   C |    60 | 17.5 |        
   19620 | 2020-03-24 00:13:03 |         MASTER-OAFA | (10h 25m 46.27s , -57d 51m 52.2s) |   C |    60 | 17.5 |        
   19711 | 2020-03-24 00:14:34 |         MASTER-OAFA | (10h 40m 49.75s , -57d 53m 17.5s) |   C |    60 | 17.4 |        
   20349 | 2020-03-24 00:25:12 |         MASTER-OAFA | (10h 40m 49.33s , -57d 51m 40.6s) |   C |    60 | 17.4 |        
   20440 | 2020-03-24 00:26:43 |         MASTER-OAFA | (10h 04m 54.88s , -53d 53m 42.3s) |   C |    60 | 17.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200317A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27425
SUBJECT: GRB 200317A: AstroSat CZTI detection
DATE:    20/03/24 12:16:53 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 (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data showed the detection of a GRB 200317A, which was also detected by Fermi GBM (GCN #27392) and Global MASTER-Net (Lipunov V. et al., GCN #27393).
The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 2020-03-17 00:40:30.0 UT. The measured peak count rate associated with the burst is 507 +/- 32.0 cts/s above the background in the combined data of four quadrants, with a total of 1355 +/- 8.6 cts. The local mean background count rate was 528 +/- 1.0 cts/s. Using cumulative rates, we measure a T90 of 6.1 +/- 0.025 s.
CZTI GRB detections are reported regularly on the payload site atâ€‹ 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: GRB200318A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27426
SUBJECT: GRB 200318A : AstroSat CZTI detection
DATE:    20/03/24 12:17:59 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data showed the detection of a long GRB 200318A, which was also detected by Fermi GBM (GCN #27412).â€‹ 
The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak of emission peaking atâ€‹ 2020-03-18â€‹ 22:35:27â€‹ UT. The measured peak count rate associated with the burst isâ€‹ 197 +/- 21.6â€‹ cts/s above the background in the combined data of four quadrants, with a total ofâ€‹ 990 +/- 48.8â€‹ cts. The local mean background count rate was 566 +/- 3.1 cts/s. Using cumulative rates, we measure a T90 of 10.1 +/- 0.33 s.
It was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.
CZTI GRB detections are reported regularly on the payload site atâ€‹ 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: GRB200324A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27428
SUBJECT: GRB 200324A: Swift detection of a burst
DATE:    20/03/24 16:57:02 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Dichiara (NASA/GSFC/UMCP), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), V. D'Elia (SSDC), 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),
K. L. Page (U Leicester), D. M. Palmer (LANL), T. Sbarrato (INAF-OAB),
B. Sbarufatti (PSU) and T. N. Ukwatta (LANL) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 16:39:07 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200324A (trigger=963260).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 222.685, +35.968 which is 
   RA(J2000) = 14h 50m 44s
   Dec(J2000) = +35d 58' 06"
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 60 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 16:42:11.8 UT, 183.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 222.67198,
35.94100 which is equivalent to:
   RA(J2000)  = 14h 50m 41.28s
   Dec(J2000) = +35d 56' 27.6"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 104 arcseconds from the BAT onboard position, within the
BAT error circle. This position may be improved as more data are
received; the latest position is available at
https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.07 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.9
(+2.21/-1.93) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.27e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 194 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
0.01. 

This source lies within the current (Sector 23) field-of-view of TESS camera 2. 

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: GRB200324A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27429
SUBJECT: GRB 200324A:MITSuME Akeno optical upper limits
DATE:    20/03/24 17:45:42 GMT
FROM:    Ryohei Hosokawa at Tokyo Institute of Technology  <hosokawa@hp.phys.titech.ac.jp>

R. Hosokawa,R. Adachi, K. L. Murata, M. Oeda, K. Shiraishi, K. Iida,
M. Niwano, F. Ogawa, S. Toma, N. Nakamura, Y. Yatsu, and N.
Kawai(TokyoTech) report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 200324A (S. Dichiara et
al., GCN Circular #27428) with the optical three color (g', Rc, and
Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno
Observatory, Yamanashi, Japan.
The observation started on 16:42:46 UT. We did not find any new point
sources within the Swift XRT circle (S. Dichiara et al., GCN Circular
#27428) in all three bands.
We obtained the 5-sigma limits as follows.
T0+[sec] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
219 16:46:39 420 g'>18.9,Rc>18.6,Ic>17.6
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used UCAC4 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. ,in prep;
https://github.com/MNiwano/Eclair)


GRB_name: GRB200324A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27430
SUBJECT: GRB 200324A: Enhanced Swift-XRT position
DATE:    20/03/24 19:14:23 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 1203 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 200324A, 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 = 222.67373, +35.94173 which is equivalent
to:

RA (J2000): 14h 50m 41.70s
Dec (J2000): +35d 56' 30.2"

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: GRB200324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27431
SUBJECT: GRB 200324A: Tautenburg observations 
DATE:    20/03/24 22:50:57 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

B. Stecklum, S. Klose, A. Nicuesa Guelbenzu, S. Melnikov, and F. Ludwig (all 
Tautenburg) report:

We observed the field of GRB 200324A (Dichiara et al., GCN 27428) with the 
Tautenburg 1.34m Schmidt telescope equipped with the TAUKAM 6k x 6k CCD camera 
and the wide V-band filter (VB). The transmission curve of this filter closely 
follows the Gaia GBP filter. Observations started at 20:08:15 UT and consisted 
of 5x5 min exposures.

Inside the enhanced XRT error circle (Beardmore et al., GCN 27430) we do not 
find any optical transient. Based on Gaia DR2 stars in the field, we provide an 
upper limit of VB > 22.0 mag (Vega system; 3.5 hr after the burst). We note 
that only ~5 arcsec north of the center of the XRT error circle lies the faint 
SDSS-DR8 source J145041.56+355635.6, possibly the GRB host galaxy.


GRB_name: GRB200324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27432
SUBJECT: GRB 200324A: NOT optical upper limit
DATE:    20/03/24 23:47:48 GMT
FROM:    Daniele B Malesani at DTU Space  <malesani@space.dtu.dk>

Johan P. U. Fynbo (DAWN/NBI), Daniele B. Malesani (DTU Space), Abel de 
Burgos Sierra (NOT), Thomas Augusteijn (NOT), report on behalf of a 
larger collaboration:

On 2020 March 24.97 UT (6 hr 39 min after the trigger) we observed the 
field of GRB 200324A (Dichiara et al., GCN 27428; Beardmore et al., GCN 
27430) with the Nordic Optical Telescope equipped with ALFOSC in the 
SDSS r filter, for a total integration time of 300 s. We find no 
evidence for afterglow emission above a 3-sigma limit of about 23 mag. 
Our result is consistent with the non-detection by Stecklum et al. (GCN 
27431).


GRB_name: GRB200324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27433
SUBJECT: GRB 200324A: Konkoly Obs. optical upper limit
DATE:    20/03/25 03:08:41 GMT
FROM:    Jozsef Vinko at Konkoly Observatory  <vinko@konkoly.hu>

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

We observed the field of GRB 200324A (Dichiara et al. GCN 27428; Beardmore et al., GCN
27430; Stecklum et al. GCN 27431; Fynbo et al. GCN 27432) with the 0.8m RC80 robotic telescope
at Piszkesteto Mountain Station of Konkoly Observatory through SDSS r' filter on 2020 March 24.88 UT   
(MJD 58932.885, 4h 36m after the trigger). The total exposure time was 1800 s. The frames were tied
to PS1-photometry of local stellar sources. No optical counterpart for the GRB has been detected 
above the 3-sigma upper limit of 21.7 AB-mag, which is consistent with other reports of non-detection. 


GRB_name: GRB200325A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27434
SUBJECT: GRB 200325A: Fermi GBM Final Real-time Localization
DATE:    20/03/25 03:28:53 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 03:18:31 UT on 25 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200325A (trigger 606799116.742442 / 200325138).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 22.1, Dec = -29.1 (J2000 degrees, equivalent to J2000 01h 28m, -29d 06'), with a statistical uncertainty of 4.2 degrees.

The angle from the Fermi LAT boresight is 102.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200325138/quicklook/glg_skymap_all_bn200325138.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/bn200325138/quicklook/glg_healpix_all_bn200325138.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200325138/quicklook/glg_lc_medres34_bn200325138.gif


GRB_name: GRB200324A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27435
SUBJECT: GRB 200324A: Swift-XRT refined Analysis
DATE:    20/03/25 05:02:10 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), A.
Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.
Melandri (INAF-OAB) and S. Dichiara report on behalf of the Swift-XRT
team:

We have analysed 6.2 ks of XRT data for GRB 200324A (Dichiara et al.
GCN Circ. 27428), from 190 s to 35.9 ks after the  BAT trigger. The
data comprise 163 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. 27430).

The light curve can be modelled with an initial power-law decay with an
index of alpha=3.61 (+0.29, -0.25), followed by a break at T+434 s to
an alpha of 1.03 (+/-0.07).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.48 (+0.13, -0.11). The
best-fitting absorption column is  1.49 (+0.28, -0.26) x 10^21 cm^-2,
in excess of the Galactic value of 1.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.92 (+0.18, -0.17)
and a best-fitting absorption column of 2.7 (+/-0.7) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (5.3 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+/-0.7) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^20 cm^-2
Excess significance: 6.3 sigma
Photon index:      1.92 (+0.18, -0.17)

If the light curve continues to decay with a power-law decay index of
1.03, the count rate at T+24 hours will be 8.1 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-13 (4.4 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00963260.

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


GRB_name: GRB200324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27436
SUBJECT: GRB 200324A: LCO Optical Upper Limit
DATE:    20/03/25 07:21:16 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

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

We observed Swift GRB 200324A (Dichiara et al., GCN 27428) with the LCO 1-m Sinistro instrument at the McDonald Observatory, USA site, on March 25, from 6:06 to 6:46 UT (corresponding to 13.28 to 13.95 hours from the GRB trigger time) with the Bessel I and R filters.

We performed a series of 5x240s exposures in I and R. We do not detect any sources in the individual frames (nor in stacked images) in the Swift enhanced error region (Beardmore et al., GCN 27430), consistent with other optical non-detections.  Using the USNO-B.1 catalog as reference, we obtain the following 3-sigma upper limits:

R > 24.21

I > 22.56

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


GRB_name: GRB200325A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27437
SUBJECT: GRB 200325A: AGILE/MCAL observations
DATE:    20/03/25 11:17:45 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the short burst GRB 200325A reported by
Fermi/GBM (GCN #27434), that also triggered the automatic AGILE
Mini-CALorimeter (MCAL) GRB alert Notice (ID 512191111), published at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.

The event was detected by MCAL at T0 = 2020-03-25 03:18:31.71 +/- 0.01 s
(UTC), lasting ~1.2 s and releasing a total number of ~1000 counts in the
detector, above a background rate of ~580 Hz. The MCAL light curve can be
found at:
http://www.agilescienceapp.it/notices/GRB_067078_512191111.714274.png. The
time-integrated spectrum of the burst in 1.2 s can be fitted in the energy
range 0.4-10 MeV with a single power-law with ph.ind. = 1.72 -0.17/+0.20,
resulting in a reduced chi-squared of 1.03 (36 d.o.f.). The burst fluence
in the same energy range and time interval is 3.62e-06 erg/cm^2 (90%
confidence level).

The event localization according to Fermi/GBM, RA = 22.1, Dec = -29.1
(J2000; GCN #27434), is within the AGILE Gamma-Ray Imaging Detector (GRID)
Field-of-View, but no detection is obtained in the integrations (T0;T0+5s)
and (T0;T0+10s).

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.


GRB_name: GRB200325A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27438
SUBJECT: GRB 200325A: AstroSat CZTI detection
DATE:    20/03/25 11:39:26 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 200325A, which was also detected by Fermi GBM (GCN #27434) and AGILE/MCAL (Ursi A. e al., GCN #27437). 

The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak of emission peaking at 2020-03-25 03:18:31 UT. The measured peak count rate associated with the burst is 185 +/- 24.5 cts/s above the background in the combined data of four quadrants, with a total of 492 +/- 21.4 cts. The local mean background count rate was 602 +/- 2.2 cts/s. Using cumulative rates, we measure a T90 of 4.9 +/- 0.12 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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


GRB_name: GRB200324A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27439
SUBJECT: GRB 200324A: Swift/UVOT Upper Limits
DATE:    20/03/25 12:48:41 GMT
FROM:    Alice Breeveld at MSSL-UCL  <a.breeveld@ucl.ac.uk>

A. A. Breeveld (UCL-MSSL) 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 200324A 215 s after the BAT trigger 
(Dichiara et al., GCN Circ. 27428).
No optical afterglow consistent with the XRT position (Beardmore et al. GCN Circ. 27430)
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           215          365          147         >21.0
u_FC               374          624          246         >20.6
white              215         1376          373         >21.7
v                  704         1427           78         >18.9
b                  630         1527           97         >19.8
u                  374         1327          304         >20.2
w1                 754         1477           78         >19.1
w2                1381         1401           19         >19.1

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


GRB_name: GRB200324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27440
SUBJECT: GRB 200324A:: TSHAO optical upper limit
DATE:    20/03/25 14:19:13 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), I. Reva (FAPHI), A. Pozanenko (IKI), M. Krugov (FAPHI), 
   E. Mazaeva (IKI), A. Volnova (IKI) report on behalf of IKI-GRB-FuN:

We observed the field of GRB 200324A: (Dichiara et al.  GCN 27428) with 
Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting 
on Mar. 24 (UT) 17:35:57.   We found no one object within enhanced 
Swift-XRT position (Beardmore et al., GCN 27430).  Preliminary 
photometry of the field is following.

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

2020-03-24 17:35:57 0.0638  R      4200  n/d   n/d  21.3

The photometry is based on nearby SDSS-DR12 stars.

RA DEC               R(Lupton transformation)
222.719432 35.941281 17.353
222.755165 35.913578 16.314
222.698647 35.902796 16.214
222.827959 35.919356 15.822


GRB_name: GRB200325B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27441
SUBJECT: GRB 200325B: Fermi GBM Final Real-time Localization
DATE:    20/03/25 15:03:33 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 14:53:16 UT on 25 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200325B (trigger 606840801.036936 / 200325620).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 166.9, Dec = 26.2 (J2000 degrees, equivalent to J2000 11h 07m, 26d 11'), with a statistical uncertainty of 3.3 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/bn200325620/quicklook/glg_skymap_all_bn200325620.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/bn200325620/quicklook/glg_healpix_all_bn200325620.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200325620/quicklook/glg_lc_medres34_bn200325620.gif


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27442
SUBJECT: Fermi  trigger No 606840801: Global MASTER-Net observations report 
DATE:    20/03/25 19:45:36 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),

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200325B ( Fermi GBM team, GCN 27441) errorbox  101 sec after notice time and 129 sec after trigger time at 2020-03-25 14:55:25 UT, with upper limit up to  18.5 mag. The observations began at zenith distance = 25 deg. The sun  altitude  is -29.4 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200325B errorbox  101 sec after notice time and 5198 sec after trigger time at 2020-03-25 16:19:54 UT, with upper limit up to  18.1 mag. Observations started at twilight.  The observations began at zenith distance = 48 deg. The sun  altitude  is -10.0 deg. 

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200325B errorbox  101 sec after notice time and 7545 sec after trigger time at 2020-03-25 16:59:01 UT, with upper limit up to  17.2 mag. Observations started at twilight.  The observations began at zenith distance = 46 deg. The sun  altitude  is -11.1 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200325B errorbox  101 sec after notice time and 11810 sec after trigger time at 2020-03-25 18:10:06 UT, with upper limit up to  16.1 mag. The observations began at zenith distance = 75 deg. The sun  altitude  is -19.1 deg. 

The galactic latitude b = 70 deg., longitude l = 205 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1321597

We obtain a following upper limits.  

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

     145 | 2020-03-25 14:55:25 |        MASTER-Tunka | (11h 16m 38.82s , +30d 17m 40.1s) |  P| |    30 | 17.1 |        
     194 | 2020-03-25 14:56:15 |        MASTER-Tunka | (11h 16m 35.54s , +30d 19m 13.0s) |  P| |    30 | 17.2 |        
     249 | 2020-03-25 14:57:04 |        MASTER-Tunka | (11h 16m 35.52s , +30d 17m 42.4s) |  P| |    40 | 17.1 |        
     313 | 2020-03-25 14:58:04 |        MASTER-Tunka | (11h 16m 39.10s , +30d 19m 15.7s) |  P| |    50 | 17.5 |        
     393 | 2020-03-25 14:59:13 |        MASTER-Tunka | (11h 16m 33.29s , +30d 18m 25.1s) |  P| |    70 | 17.9 |        
     643 | 2020-03-25 15:02:59 |        MASTER-Tunka | (11h 08m 06.42s , +26d 38m 13.4s) |  P| |   120 | 18.2 |        
     792 | 2020-03-25 15:05:18 |        MASTER-Tunka | (11h 08m 12.76s , +26d 37m 16.6s) |  P| |   140 | 18.5 |        
    5228 | 2020-03-25 16:19:54 |   MASTER-Kislovodsk | (11h 18m 11.30s , +30d 09m 55.5s) |   C |    60 | 17.1 |        
    5228 | 2020-03-25 16:19:54 |   MASTER-Kislovodsk | (11h 27m 41.11s , +29d 42m 01.1s) |   C |    60 | 17.5 |        
    5309 | 2020-03-25 16:21:15 |   MASTER-Kislovodsk | (11h 05m 15.52s , +28d 09m 12.6s) |   C |    60 | 17.4 |        
    5309 | 2020-03-25 16:21:15 |   MASTER-Kislovodsk | (11h 14m 34.63s , +27d 41m 21.4s) |   C |    60 | 17.6 |        
    5390 | 2020-03-25 16:22:35 |   MASTER-Kislovodsk | (11h 13m 45.48s , +32d 07m 57.3s) |   C |    60 | 17.5 |        
    5390 | 2020-03-25 16:22:35 |   MASTER-Kislovodsk | (11h 23m 26.74s , +31d 40m 04.0s) |   C |    60 | 17.7 |        
    5470 | 2020-03-25 16:23:56 |   MASTER-Kislovodsk | (10h 59m 49.50s , +30d 08m 33.1s) |   C |    60 | 17.8 |        
    5470 | 2020-03-25 16:23:56 |   MASTER-Kislovodsk | (11h 09m 19.34s , +29d 40m 43.5s) |   C |    60 | 17.9 |        
    5551 | 2020-03-25 16:25:16 |   MASTER-Kislovodsk | (11h 18m 16.68s , +30d 09m 33.0s) |   C |    60 | 17.6 |        
    5551 | 2020-03-25 16:25:16 |   MASTER-Kislovodsk | (11h 27m 44.96s , +29d 41m 36.3s) |   C |    60 | 17.9 |        
    5631 | 2020-03-25 16:26:36 |   MASTER-Kislovodsk | (11h 05m 14.16s , +28d 08m 24.5s) |   C |    60 | 17.7 |        
    5631 | 2020-03-25 16:26:36 |   MASTER-Kislovodsk | (11h 14m 32.00s , +27d 40m 31.1s) |   C |    60 | 17.8 |        
    5711 | 2020-03-25 16:27:57 |   MASTER-Kislovodsk | (11h 13m 50.96s , +32d 09m 38.0s) |   C |    60 | 17.5 |        
    5711 | 2020-03-25 16:27:57 |   MASTER-Kislovodsk | (11h 23m 31.48s , +31d 41m 42.2s) |   C |    60 | 18.0 |        
    5792 | 2020-03-25 16:29:18 |   MASTER-Kislovodsk | (10h 59m 44.77s , +30d 09m 23.4s) |   C |    60 | 17.8 |        
    5792 | 2020-03-25 16:29:18 |   MASTER-Kislovodsk | (11h 09m 14.00s , +29d 41m 32.0s) |   C |    60 | 18.1 |        
    5872 | 2020-03-25 16:30:38 |   MASTER-Kislovodsk | (11h 23m 18.78s , +28d 09m 51.7s) |   C |    60 | 17.7 |        
    5872 | 2020-03-25 16:30:38 |   MASTER-Kislovodsk | (11h 32m 35.10s , +27d 41m 53.3s) |   C |    60 | 17.9 |        
    7576 | 2020-03-25 16:59:01 |      MASTER-Tavrida | (10h 59m 11.46s , +26d 01m 29.0s) |   C |    60 | 17.2 |        
   11841 | 2020-03-25 18:10:06 |         MASTER-SAAO | (11h 01m 49.44s , +26d 06m 26.4s) |   C |    60 | 12.1 |        
   12139 | 2020-03-25 18:15:04 |         MASTER-SAAO | (11h 01m 58.23s , +26d 06m 59.4s) |   C |    60 | 13.1 |        
   12705 | 2020-03-25 18:24:30 |         MASTER-SAAO | (11h 11m 47.63s , +26d 05m 56.0s) |   C |    60 | 14.4 |        
   12705 | 2020-03-25 18:24:30 |         MASTER-SAAO | (11h 19m 56.86s , +26d 06m 42.1s) |   C |    60 | 14.0 |        
   13076 | 2020-03-25 18:30:41 |         MASTER-SAAO | (11h 11m 35.71s , +26d 07m 07.0s) |   C |    60 | 15.6 |        
   13076 | 2020-03-25 18:30:41 |         MASTER-SAAO | (11h 19m 45.03s , +26d 07m 51.9s) |   C |    60 | 16.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200324A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27443
SUBJECT: GRB 200324A, Swift-BAT refined analysis
DATE:    20/03/25 21:13:14 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), 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), 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 200324A (trigger #963260)
(Dichiara et al., GCN Circ. 27428).  The BAT ground-calculated position is
RA, Dec = 222.682, 35.931 deg which is
   RA(J2000)  =  14h 50m 43.7s
   Dec(J2000) = +35d 55' 51.0"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a weak pulse that starts
at ~T-40 s, peaks at ~T0, and lasts until >~T+80 s. The burst was
temporarily out of the BAT FOV from T+100.39 s to T+119.39 s.
There might be additional burst emission during this period.
Due to this data gap, the standard data analysis pipeline
is unable to estimate an accurate T90.

The time-averaged spectrum from T-38.1 to T+100.4 sec (before
the burst went out of the BAT FOV) is best fit by a simple power-law model.

The power law index of the time-averaged spectrum is 1.72 +- 0.15.
The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-6 erg/cm2. The 1-sec
peak photon flux measured from T+0.07 sec in the 15-150 keV band
is 0.7 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/963260/BA/


GRB_name: GRB200325A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27444
SUBJECT: GRB 200325A: Swift/BAT detection and probable arcminute localization of a short GRB from GUANO
DATE:    20/03/26 00:52:23 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not trigger on GRB 200325A.

The Fermi/GBM Flight-Position notice, distributed at T0+8 seconds,
from the Fermi/GBM detected GRB 200325A (GCN. 27434), as well as the
INTEGRAL SPI-ACS notice (Trig #8558) distributed at T0+44 seconds,
both triggered the Swift Mission Operations Center operated Gamma-ray
Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al.
2020, in prep). GRB 200325A was also detected by AGILE/MCAL (GCN.
27437) and AstroSat CZTI (GCN. 27438).

The 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.

Upon trigger by these notices, GUANO sent a command to the Swift Burst
Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from
[-50,+150] seconds around the time of GRB 200228A.

All the requested event mode data was delivered to the ground.

In a ground analysis of the data, using the normal BAT imaging
technique, we detect GRB 200228A with a SNR of 7.5.

With a more sophisticated maximum likelihood analysis (DeLaunay et
al.,  2020 in prep.) on the event-mode data we detect GRB 200325A more
confidently, with a square root of the test statistic, sqrt(TS), of
21.7. The sqrt(TS) behaves similarly to SNR.
The detected duration is ~1.1s.

The BAT ground-calculated position is
RA, Dec = 31.7203, -31.816 deg which is
   RA(J2000)  = 2h 6m 52.8s
   Dec(J2000) =  -31d 48â€™ 57.60â€
with an uncertainty of 4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 8.2%.

This arcminute location is consistent with the localization region
distributed by the Fermi/GBM team (GCN. 27434), lying on the 75%
containment contour.
Due to the very low partial coding, we stress that this localization,
while significant, has some additional unquantified uncertainties
associated with it.

No XRT or UVOT follow-up will take place due to the sourceâ€™s proximity
to the sun (1.5 hours).
We encourage follow-up from instruments capable of observing near the sun.

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


GRB_name: GRB200324A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27445
SUBJECT: GRB 200324A: AROMA-N Optical Observation
DATE:    20/03/26 06:44:11 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Nakamura, T. Sakamoto (AGU)

We observed the field of GRB 200324A detected by Swift
(Dichiara et al., GCN Circ. 27428) with the 14-inch AGU Robotic
Optical Monitor for Astrophysical object - Narrow (AROMA-N)
located at the Sagamihara campus of Aoyama Gakuin University.

22 images of 60 sec, 120 sec, 180 sec and 300 sec exposures
were taken in the R filter starting from March 24 16:42:55 (UT)
about 228 seconds after the trigger and stopped on March 24 19:06:11 (UT).
We do not detect the optical afterglow both in the individual
images and the stacked image.  The estimated five sigma upper limit
of the combined image (total exposure of 3240 sec) is ~17.6 mag
using the USNO-B1 catalog.


GRB_name: GRB200325B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27446
SUBJECT: GRB 200325B: MASTERt OT detection
DATE:    20/03/26 12:13:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov,  E. Gorbovskoy, V.Kornilov, N.Tyurina, 
P.Balanutsa,A.Kuznetsov,F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo 
Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix
Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State
University)


MASTER OT J111012.51+274912.8 discovery - new OT inside Fermi GRB 200325B 
(trigger 606840801)

MASTER Global Robotic Net inspected GRB 200325B:
Fermi trigger 606840801, Ttr=2020-03-05 14:53:16 UT, GCN #27441,
MASTER report GCN #27442, MASTER map and OT position.
During inspection
MASTER-Kislovodsk auto-detection system ( Lipunov et al., "MASTER Global 
Robotic Net", Advances in Astronomy, 2010, 30L )
discovered new OT source at (RA, Dec) = 11h 10m 12.51s +27d 49m 12.8s on 
2020-03-25 16:21:15 UT.
The OT unfiltered magnitude is 16.1m (mlim=17.8).
The OT is seen in 2 inspect images
(MASTER has 2 tubes at each observatory and works with large error-fields 
like Fermi in open mode, that gives 8 square degrees, i.e. 2x4sq.deg.).
There is no minor planet at this place and no any sources in VIZIER 
database (22mag limit in POSS history).

We have reference images on 2010-03-13.87244 UT with unfiltered mlim= 
20.2m, on 2020-02-21 21:54:40UT with mlim=20.3.
Spectral observations are required.
The discovery and reference images are available at: 
http://master.sai.msu.ru/static/OT/111012.51274912.8.png


GRB_name: GRB200326A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27447
SUBJECT: GRB 200326A: Fermi GBM Final Real-time Localization
DATE:    20/03/26 12:35:06 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 12:24:47 UT on 26 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200326A (trigger 606918292.90322 / 200326517).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 245.3, Dec = -21.1 (J2000 degrees, equivalent to J2000 16h 21m, -21d 06'), with a statistical uncertainty of 6.9 degrees.

The angle from the Fermi LAT boresight is 89.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200326517/quicklook/glg_skymap_all_bn200326517.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/bn200326517/quicklook/glg_healpix_all_bn200326517.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200326517/quicklook/glg_lc_medres34_bn200326517.gif


GRB_name: GRB200325A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27448
SUBJECT: Fermi  trigger No 606799116: Global MASTER-Net observations report 
DATE:    20/03/26 14:30:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200325A ( Fermi GBM team, GCN 27434) errorbox  15 sec after notice time and 44 sec after trigger time at 2020-03-25 03:19:16 UT, with upper limit up to  19.7 mag. The observations began at zenith distance = 70 deg. The sun  altitude  is -19.1 deg. 

MASTER-OAFA robotic telescope  located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 200325A errorbox  29 sec after notice time and 59 sec after trigger time at 2020-03-25 03:19:30 UT, with upper limit up to  19.0 mag. The observations began at zenith distance = 61 deg. The sun  altitude  is -55.1 deg. 

The galactic latitude b = -34 deg., longitude l = 290 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1321238

We obtain a following upper limits.  

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

      50 | 2020-03-25 03:19:16 |         MASTER-SAAO | (04h 23m 50.57s , -77d 32m 51.4s) |   C |    10 | 18.4 |        
      50 | 2020-03-25 03:19:16 |         MASTER-SAAO | (04h 56m 48.78s , -77d 30m 55.2s) |   C |    10 | 18.1 |        
      64 | 2020-03-25 03:19:30 |         MASTER-OAFA | (04h 39m 22.28s , -77d 37m 35.3s) |   C |    10 | 17.5 |        
      92 | 2020-03-25 03:19:58 |         MASTER-SAAO | (04h 23m 43.90s , -77d 33m 23.3s) |   C |    10 | 18.4 |        
      92 | 2020-03-25 03:19:58 |         MASTER-SAAO | (04h 56m 43.18s , -77d 31m 27.9s) |   C |    10 | 18.0 |        
     110 | 2020-03-25 03:20:11 |         MASTER-OAFA | (04h 39m 28.23s , -77d 37m 12.8s) |   C |    20 | 18.2 |        
     140 | 2020-03-25 03:20:42 |         MASTER-SAAO | (04h 23m 46.13s , -77d 32m 21.9s) |   C |    20 | 19.0 |        
     140 | 2020-03-25 03:20:42 |         MASTER-SAAO | (04h 56m 42.53s , -77d 30m 27.1s) |   C |    20 | 18.6 |        
     167 | 2020-03-25 03:21:03 |         MASTER-OAFA | (04h 39m 24.81s , -77d 35m 51.5s) |   C |    30 | 18.4 |        
     198 | 2020-03-25 03:21:34 |         MASTER-SAAO | (04h 23m 50.30s , -77d 33m 18.8s) |   C |    30 | 19.2 |        
     198 | 2020-03-25 03:21:34 |         MASTER-SAAO | (04h 56m 49.01s , -77d 31m 24.6s) |   C |    30 | 18.8 |        
     233 | 2020-03-25 03:22:04 |         MASTER-OAFA | (04h 39m 24.99s , -77d 37m 22.5s) |   C |    40 | 18.7 |        
     265 | 2020-03-25 03:22:36 |         MASTER-SAAO | (04h 23m 42.47s , -77d 34m 17.0s) |   C |    40 | 19.5 |        
     265 | 2020-03-25 03:22:36 |         MASTER-SAAO | (04h 56m 43.61s , -77d 32m 23.0s) |   C |    40 | 19.1 |        
     309 | 2020-03-25 03:23:16 |         MASTER-OAFA | (04h 39m 27.94s , -77d 35m 38.9s) |   C |    50 | 18.9 |        
     347 | 2020-03-25 03:23:49 |         MASTER-SAAO | (04h 23m 48.15s , -77d 34m 03.8s) |   C |    60 | 19.7 |        
     347 | 2020-03-25 03:23:49 |         MASTER-SAAO | (04h 56m 48.57s , -77d 32m 10.8s) |   C |    60 | 19.3 |        
     401 | 2020-03-25 03:24:37 |         MASTER-OAFA | (04h 39m 21.75s , -77d 36m 39.4s) |   C |    70 | 19.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200325A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27449
SUBJECT: IPN triangulation of 200325A (short)
DATE:    20/03/26 17:15:15 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,

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

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

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

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

The short-duration GRB 200325A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 27434;
AGILE-MCAL detection: Ursi, et al., GCN Circ. 27437;
AstroSat-CZTI detection: Gupta et al., GCN Circ. 27438;
Swift-BAT detection: DeLaunay et al., GCN Circ. 27444)
was detected by Fermi (GBM trigger 606799116), Konus-Wind,
INTEGRAL (SPI-ACS), AGILE (MCAL), AstroSat (CZTI),
Mars-Odyssey (HEND), and Swift (BAT)
at about 11912 s UT (03:18:32).
The burst was found in ground analysis of Swift (BAT) data
with very low partial coding.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    31.754 (02h 07m 01s) -31.920 (-31d 55' 14")
  Corners:
    31.301 (02h 05m 12s) -30.580 (-30d 34' 50")
    32.340 (02h 09m 22s) -32.899 (-32d 53' 58")
    32.205 (02h 08m 49s) -33.240 (-33d 14' 25")
    31.173 (02h 04m 41s) -30.931 (-30d 55' 53")
  ---------------------------------------------
The error box area is 2023 sq. arcmin, and its maximum
dimension is 2.77 deg (the minimum one is 13.6 arcmin).
The Sun distance was 41 deg.

This box may be improved.

The Swift-BAT position (GCN 27444) is consistent with the IPN localization.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200325_T11908/IPN

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


GRB_name: GRB200325B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27450
SUBJECT: GRB 200325B: Swift ToO observations
DATE:    20/03/26 18:35:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

Swift has initiated a ToO observation of the Fermi/GBM GRB 200325B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00020978

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

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

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


GRB_name: GRB200326A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27451
SUBJECT: Fermi  trigger No 606918292: Global MASTER-Net observations report 
DATE:    20/03/26 20:15:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tunka robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200326A ( Fermi GBM team, GCN 27447) errorbox  19451 sec after trigger time at 2020-03-26 17:48:58 UT, with upper limit up to  18.1 mag. The observations began at zenith distance = 78 deg. The sun  altitude  is -35.9 deg. 

The galactic latitude b = 19 deg., longitude l = 355 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1322435

We obtain a following upper limits.  

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

   19481 | 2020-03-26 17:48:58 |        MASTER-Tunka | (15h 59m 56.19s , -16d 05m 17.0s) |   C |    60 | 17.9 |        
   19561 | 2020-03-26 17:50:18 |        MASTER-Tunka | (16h 07m 25.70s , -14d 05m 29.1s) |   C |    60 | 18.1 |        
   19641 | 2020-03-26 17:51:39 |        MASTER-Tunka | (15h 53m 23.54s , -18d 06m 48.7s) |   C |    60 | 17.9 |        
   19802 | 2020-03-26 17:54:19 |        MASTER-Tunka | (16h 23m 54.03s , -14d 08m 22.8s) |   C |    60 | 17.9 |        
   20045 | 2020-03-26 17:58:22 |        MASTER-Tunka | (16h 16m 31.52s , -16d 06m 14.7s) |   C |    60 | 17.8 |        
   20576 | 2020-03-26 18:07:14 |        MASTER-Tunka | (15h 47m 54.66s , -20d 06m 06.1s) |   C |    60 | 17.9 |        
   20659 | 2020-03-26 18:08:36 |        MASTER-Tunka | (16h 40m 25.97s , -14d 08m 58.2s) |   C |    60 | 17.8 |        
   20751 | 2020-03-26 18:10:08 |        MASTER-Tunka | (16h 10m 06.15s , -18d 06m 28.3s) |   C |    60 | 17.7 |        
   21340 | 2020-03-26 18:19:57 |        MASTER-Tunka | (16h 33m 14.00s , -16d 07m 15.3s) |   C |    60 | 18.0 |        
   21420 | 2020-03-26 18:21:17 |        MASTER-Tunka | (16h 04m 54.51s , -20d 06m 27.2s) |   C |    60 | 17.6 |        
   21699 | 2020-03-26 18:25:57 |        MASTER-Tunka | (16h 26m 56.12s , -18d 06m 54.3s) |   C |    60 | 17.9 |        
   21941 | 2020-03-26 18:29:59 |        MASTER-Tunka | (16h 49m 52.24s , -16d 08m 41.8s) |   C |    60 | 17.6 |        
   23027 | 2020-03-26 18:48:04 |        MASTER-Tunka | (16h 21m 49.78s , -20d 04m 52.6s) |   C |    60 | 17.8 |        
   23107 | 2020-03-26 18:49:25 |        MASTER-Tunka | (16h 00m 33.07s , -22d 05m 51.5s) |   C |    60 | 17.7 |        
   23188 | 2020-03-26 18:50:45 |        MASTER-Tunka | (16h 43m 48.61s , -18d 06m 22.5s) |   C |    60 | 17.8 |        
   23350 | 2020-03-26 18:53:28 |        MASTER-Tunka | (16h 17m 54.79s , -22d 05m 43.1s) |   C |    60 | 17.6 |        
   23512 | 2020-03-26 18:56:09 |        MASTER-Tunka | (16h 38m 57.11s , -20d 06m 43.4s) |   C |    60 | 17.8 |        
   23694 | 2020-03-26 18:59:12 |        MASTER-Tunka | (15h 57m 22.35s , -24d 03m 40.9s) |   C |    60 | 17.5 |        
   26790 | 2020-03-26 19:50:47 |        MASTER-Tunka | (16h 15m 06.20s , -24d 03m 35.1s) |   C |    60 | 17.6 |        
   26871 | 2020-03-26 19:52:08 |        MASTER-Tunka | (16h 35m 16.41s , -22d 05m 17.1s) |   C |    60 | 17.9 |        
   26954 | 2020-03-26 19:53:31 |        MASTER-Tunka | (16h 13m 13.61s , -26d 04m 18.4s) |   C |    60 | 17.6 |        
   27036 | 2020-03-26 19:54:54 |        MASTER-Tunka | (16h 32m 28.92s , -24d 04m 25.3s) |   C |    60 | 18.1 |        
   27137 | 2020-03-26 19:56:35 |        MASTER-Tunka | (15h 55m 29.65s , -26d 03m 53.5s) |   C |    60 | 17.5 |        
   27221 | 2020-03-26 19:57:58 |        MASTER-Tunka | (16h 49m 57.97s , -24d 05m 16.4s) |   C |    60 | 17.7 |        
   27303 | 2020-03-26 19:59:21 |        MASTER-Tunka | (16h 52m 30.54s , -22d 05m 48.1s) |   C |    60 | 17.5 |        
   27391 | 2020-03-26 20:00:48 |        MASTER-Tunka | (16h 55m 58.04s , -20d 05m 23.1s) |   C |    60 | 17.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27452
SUBJECT: GRB 200325B: Mondy and CrAO observations, Master MASTER OT J111012.51+274912.8 confirmation
DATE:    20/03/26 23:30:56 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of Fermi-GBM GRB 200325B (Fermi GBM team, GCN 
27441) with AZT-33VM 1.5-m telescope of Sayan observatory (Mondy) 
starting on  2020-03-26 (UT) 15:08:10 and and ZTSh 2.6m telescope of 
CrAO starting on 2020-03-26 (UT) 20:11:20. We clearly detected the OT 
discovered by MASTER (Lipunov et al., GCN 27446). Coordinates of the OT 
are (J2000) 11:10:12.54 +27:49:11.7 with uncertainty of 0.5 arcses. The 
R magnitude of the OT is 19.8 +/- 0.15 at 2020-03-26 (UT) 15:08:10. 
Observations and data reduction is ongoing.


GRB_name: GRB200325A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27453
SUBJECT: GRB 200325A: Fermi GBM observation
DATE:    20/03/27 01:55:20 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres (UAH), C. M. Hui (NASA/MSFC), C. Meegan (UAH) and J. Wood
(NASA/MSFC) report on behalf of the Fermi GBM Team:

"At 03:18:31.74 UT on 25 March 2020, the Fermi Gamma-Ray Burst Monitor
(GBM) triggered
and located GRB 200325A (trigger 606799116 / 200325138)
which was also detected by the Swift/BAT (GCN 27444). The Fermi GBM Final
Real-time Localization (GCN 27434) is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 107
degrees.


The GBM light curve consists of a single peak with a duration (T90) of
about 1 s (50-300 keV). The time-averaged spectrum from T0-0.1 s to T0+1.2
s is
best fit by a power law function with an exponential high-energy cutoff.
The power law index is -0.64 +/- 0.11 and the cutoff energy, parameterized
as Epeak, is 913 +/- 192 keV.

The event fluence (10-1000 keV) in this time interval is  (2.49 +/-
0.12)E-6 erg/cm^2. The 64 ms peak photon flux measured starting from T0 +
256 ms in the 10-1000 keV band is 9.6 +/- 1.5 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: GRB200326B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27454
SUBJECT: GRB 200326B: AstroSat LAXPC detection
DATE:    20/03/27 12:41:54 GMT
FROM:    Tilak Katoch at TIFR  <tilak@tifr.res.in>

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

Analysis of AstroSat LAXPC data showed the detection of a long
GRB 200326B. The light curve showed a double peak profile
triggered at T0 = 21h 13m 52s UT on 26 Mar 2020, with T90=10 sec
for the first peak followed by a second smaller peak of similar
duration about 10 s later. The measured peak count rate above the
background associated with the burst is 158 +/- 24 cts/s in
LAXPC10 and 171 +/- 20 cts/s in LAXPC20 at T0+3 sec. The total
counts in the first peak are 542 +/- 71 cts in LAXPC10 and
773 +/- 54 in LAXPC20.

Both LAXPC instruments (LAXPC10 and LAXPC20) have registered this
burst profile in the light curve. For LAXPC20 the nominal energy
range is 3-100 keV, but due to lower gain in LAXPC10 the energy
range is about 30-400 keV.

The background subtracted light curve with 1 sec time-bin is
available at the web-site:
https://www.tifr.res.in/~astrosat_laxpc/grb200326blc.jpg

LAXPC was built by TIFR in collaboration with the Indian Space
Research Organisation. The Indian Space Research Organisation
funded, managed and facilitated the project.


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27455
SUBJECT: GRB 200325B: Mondy, CrAO, AbAO afterglow confirmation and refined photometry of MASTER OT J111012.51+274912.8
DATE:    20/03/27 13:14:36 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI),  A. Pozanenko (IKI), E. Klunko (ISTP), A. Sosnovskij 
(CrAO), R. Ya. Inasaridze (AbAO), V. Rumyantsev (CrAO), M. Eselevich 
(ISTP), E. Mazaeva (IKI), A. Volnova (IKI) report on behalf of IKI-GRB-FuN:

We observed the  MASTER OT J111012.51+274912.8  (Lipunov et al., GCN 
27446) as a candidate in afterglow of the Fermi GRB 200325B (Fermi GBM 
team, GCN 27441) with AZT-33VM 1.5-m telescope of Sayan observatory 
(Mondy) starting on  2020-03-26 (UT) 15:08:10,  ZTSh 2.6m telescope of 
CrAO starting on 2020-03-26 (UT) 20:11:20 (Pozanenko et al., GCN 27452), 
and AS-32 0.7m telescope of Abastumani observatory starting on 
2020-03-26 (UT) 20:27:39. Below we present refined photometry of the OT.
Preliminary photometry of the object is following.

Date UT start       t-T0  Filter Exp. OT Err UL(3sigma)   telescope
                         (mid, days) (s)
2020-03-26 15:08:10 1.0263   R 23*120  19.89 0.05  22.6 AZT-33VM
2020-03-26 20:11:20 1.2306   R 14*120  20.07 0.08  22.3 ZTSh
2020-03-26 20:27:39 1.2444   R 35*60    n/d  n/d   20.0 AS-32

the photometry is based on nearby SDSS-DR12 stars
RA DEC               R(Lupton transformations)
167.569191 27.848262 16.015
167.513655 27.832992 16.930
167.510507 27.850424 15.261

We note that coordinates of the OT (Lipunov et al., GCN 27446; Pozanenko 
et al., GCN 27452) coincide with only one XRT source 
(https://www.swift.ac.uk/ToO_GRBs/00020978/ ) found in the error 
localization of GBM/Fermi. Taking into account the XRT source and fading 
OT we suggest the MASTER OT J111012.51+274912.8  is an afterglow GRB 
200325B.


GRB_name: GRB200325B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27456
SUBJECT: GRB 200325B: LCO Optical Detection
DATE:    20/03/27 15:26:37 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

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

We observed Fermi GRB 200325A (Fermi GBM Team, GCN 27441) with the LCO 1-m Sinistro instrument at the Siding Spring Observatory, Australia site, on March 27, from 12:08 to 12:48 UT (corresponding to 45.25 to 45.92 hours from the GRB trigger time) with the Bessel R and I filters.

We performed a series of 5x240s exposures in R and I.  We detect a source consistent with other optical detections (Lipunov et al., GCN 27446, Pozanenko et al., GCN 27452) in stacked images.  Using the USNO-B.1 catalog as reference, we obtain the following magnitudes:

R = 21.36 +/- 0.11

I = 20.52 +/- 0.13

These magnitudes are not corrected for Galactic Extinction.

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


GRB_name: GRB200325B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27457
SUBJECT: GRB 200325B: Swift-XRT and UVOT observations
DATE:    20/03/27 17:35:01 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <pda.davanzo@gmail.com>

P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), A. Melandri (INAF-OAB), 
T. Sbarrato (INAF-OAB), S. R. Oates (U. of Birmingham), M. H. Siegel (PSU), 
F. E. Marshall (NASA/GSFC), S. Dichiara (NASA/GSFC/UMCP) and P.A. Evans 
(U.Leicester) report on behalf of the Swift-XRT and UVOT teams:


Swift-XRT has performed follow-up observations of the Fermi-detected
burst GRB 200325B (Fermi GBM team, GCN Cir. 27441), collecting 1.1
ks of Photon Counting (PC) mode data between T0+102.4 ks and T0+124.8 ks 
in a single pointing covering the region of the candidate GRB optical 
counterpart initially reported by Lipunov et al. (GCN Circ. 27446).

An uncatalogued X-ray source has been detected: 

Source 1:
 RA (J2000):  167.55381  =  11:10:12.91
 Dec (J2000):  +27.8196  =  +27:49:10.5
 Error: 4.9 arcsec (radius, 90% conf. [Enhanced position])
 Count-rate: 0.020 [+/-0.005] ct s^-1   
 Flux: (7.2 [+/-1.8])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

The source is below the RASS limit and, due to the limited amount of
data available so far, shows no signs of fading.

The position of this source is consistent with the one reported for the 
GRB optical afterglow (Lipunov et al., GCN Circ. 27446; Pozanenko et al., 
GCN Circ. 27452; Belkin et al., GCN Circ. 27455; Strausbaugh & Cucchiara, 
GCN Circ. 27456). We therefore conclude that this is the X-ray afterglow of 
GRB 200325B.

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/00020978 <https://www.swift.ac.uk/ToO_GRBs/00020978>.



The Swift/UVOT began settled observations of the field of GRB 200325B
102ks after the Fermi/GBM trigger. An optical source consistent with the 
GRB optical afterglow (Lipunov et al., GCN Circ. 27446; Pozanenko et al., 
GCN Circ. 27452; Belkin et al., GCN Circ. 27455; Strausbaugh & Cucchiara, 
GCN Circ. 27456) is detected in the initial UVOT white exposure. 
A preliminary magnitude in white using the UVOT photometric system 
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is:

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

white             102.39       124.75         1044        21.27 Â± 0.24

This magnitude is 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: GRB200327A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27458
SUBJECT: GRB 200327A: Fermi GBM Final Real-time Localization
DATE:    20/03/27 21:07:11 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 20:56:48 UT on 27 Mar 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200327A (trigger 607035413.165342 / 200327873).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 233.4, Dec = 2.4 (J2000 degrees, equivalent to J2000 15h 33m, 2d 23'), with a statistical uncertainty of 17.5 degrees.

The angle from the Fermi LAT boresight is 109.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200327873/quicklook/glg_skymap_all_bn200327873.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/bn200327873/quicklook/glg_healpix_all_bn200327873.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200327873/quicklook/glg_lc_medres34_bn200327873.gif


GRB_name: GRB200327A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27459
SUBJECT: Fermi  trigger No 607035413: Global MASTER-Net observations report 
DATE:    20/03/27 22:31:34 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200327A ( Fermi GBM team, GCN 27458) errorbox  2773 sec after notice time and 2803 sec after trigger time at 2020-03-27 21:43:31 UT, with upper limit up to  19.8 mag. The observations began at zenith distance = 62 deg. The sun  altitude  is -57.6 deg. 

The galactic latitude b = 43 deg., longitude l =  8 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1323666

We obtain a following upper limits.  

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

    2833 | 2020-03-27 21:43:31 |         MASTER-SAAO | (15h 44m 24.56s , -11d 52m 31.7s) |   C |    60 | 19.6 |        
    2833 | 2020-03-27 21:43:31 |         MASTER-SAAO | (15h 51m 31.06s , -11d 51m 56.8s) |   C |    60 | 19.6 |        
    3204 | 2020-03-27 21:49:41 |         MASTER-SAAO | (15h 44m 16.74s , -11d 54m 34.4s) |   C |    60 | 19.6 |        
    3204 | 2020-03-27 21:49:41 |         MASTER-SAAO | (15h 51m 23.36s , -11d 53m 57.9s) |   C |    60 | 19.6 |        
    3667 | 2020-03-27 21:57:25 |         MASTER-SAAO | (15h 37m 49.74s , -09d 53m 23.0s) |   C |    60 | 19.7 |        
    3667 | 2020-03-27 21:57:25 |         MASTER-SAAO | (15h 44m 53.62s , -09d 52m 44.8s) |   C |    60 | 19.7 |        
    3759 | 2020-03-27 21:58:57 |         MASTER-SAAO | (15h 54m 06.40s , -09d 52m 26.4s) |   C |    60 | 19.6 |        
    3759 | 2020-03-27 21:58:57 |         MASTER-SAAO | (16h 01m 10.19s , -09d 51m 48.9s) |   C |    60 | 19.6 |        
    4036 | 2020-03-27 22:03:34 |         MASTER-SAAO | (15h 37m 54.80s , -09d 54m 01.9s) |   C |    60 | 19.7 |        
    4036 | 2020-03-27 22:03:34 |         MASTER-SAAO | (15h 44m 58.77s , -09d 53m 23.6s) |   C |    60 | 19.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200325B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27460
SUBJECT: GRB 200325B: Fermi GBM observation
DATE:    20/03/28 00:39:30 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 14:53:16.04  UT on 25 March 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200325B (trigger 606840801 / 200325620),
which was also detected by the Swift/XRT (GCN 27457).
The optical counterpart was detected by MASTER (GCN 27446), Mondy (GCN 27452), 
and LCO (GCN 27457).

The angle from the Fermi LAT boresight at the GBM trigger time is 102.5 degrees.

The GBM light curve shows a broad peak with several spikes overimposed,
with a duration (T90) of about 36.6 s (50-300 keV).
The time-averaged spectrum from T0-8.1 s to T0+36.9 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.33 +/- 0.04  and
the cutoff energy, parameterized as Epeak, is 150.1 +/- 12.8 keV.

The event fluence (10-1000 keV) in this time interval is
(1.12 +/- 0.04)e-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+10.7 s in the 10-1000 keV band
is 9.1 +/- 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: GRB200327A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27461
SUBJECT: GRB 200327A: AGILE/MCAL observations
DATE:    20/03/28 10:13:16 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

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

The AGILE satellite detected the short burst GRB 200327A reported by
Fermi/GBM (GCN #27458), that also triggered the automatic AGILE
Mini-CALorimeter (MCAL) GRB alert Notice (ID 512427408), published at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.

The event was detected by MCAL at T0 = 2020-03-27 20:56:48.25 +/- 0.01 s
(UTC), lasting ~0.13 s and releasing a total number of ~150 counts in the
detector, above a background rate of ~530 Hz. The MCAL light curve can be
found at:
http://www.agilescienceapp.it/notices/GRB_067116_512427408.252268.png. The
time-integrated spectrum of the burst in 0.13 s can be fitted in the energy
range 0.4-10 MeV with a single power-law with ph.ind. = 2.56 -0.43/+0.54,
resulting in a reduced chi-squared of 1.19 (8 d.o.f.). The burst fluence in
the same energy range and time interval is 6.34e-07 erg/cm^2 (90%
confidence level).

At the T0, the event localization according to Fermi/GBM, RA = 233.4, Dec =
2.4 (J2000) was outside the AGILE Gamma-Ray Imaging Detector (GRID)
Field-of-View.

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.


GRB_name: GRB200326B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27462
SUBJECT: GRB 200326B: AstroSat CZTI detection
DATE:    20/03/28 12:29:36 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 200326B, which was also detected by AstroSat LAXPC (Antia H. et al., GCN #27454). 

The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak of emission peaking at 2020-03-26 21:13:52 UT. The measured peak count rate associated with the burst is 146 +/- 23.5 cts/s above the background in the combined data of four quadrants, with a total of 354 +/- 10.6 cts. The local mean background count rate was 546 +/- 1.3 cts/s. Using cumulative rates, we measure a T90 of 8.1 +/- 0.6 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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


GRB_name: GRB200327A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27463
SUBJECT: IPN triangulation of 200327A (short)
DATE:    20/03/28 17:40:04 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. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

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

and

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

The short-duration GRB 200327A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 27458;
AGILE-MCAL detection: Ursi, et al., GCN Circ. 27461)
was detected by Fermi (GBM trigger 607035413), Konus-Wind,
INTEGRAL (SPI-ACS), AGILE (MCAL), and Swift (BAT)
at about 75408 s UT (20:56:48).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   236.574 (15h 46m 18s)  -4.217 ( -4d 13' 02")
  Corners:
   236.885 (15h 47m 32s)  -2.457 ( -2d 27' 24")
   236.477 (15h 45m 54s)  -5.963 ( -5d 57' 48")
   236.244 (15h 44m 59s)  -5.977 ( -5d 58' 36")
   236.654 (15h 46m 37s)  -2.472 ( -2d 28' 18")
  ---------------------------------------------
The error box area is 2897 sq. arcmin, and its maximum
dimension is 3.6 deg (the minimum one is 13.7 arcmin).
The Sun distance was 130 deg.

This box may be improved.

The IPN localization is consistent with, but reduces the area of, the 
Fermi-GBM final position (GCN Circ. 27458).

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200327_T75409/IPN

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


GRB_name: GRB200325B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27464
SUBJECT: GRB 200325B: Tautenburg observations
DATE:    20/03/28 20:01:16 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose, B. Stecklum, A. Nicuesa Guelbenzu, S. Melnikov, and F. Ludwig
(all Tautenburg) report:

We observed the field of GRB 200325B (Ferni GBM team, GCN 27441) with the 
Tautenburg 1.34m Schmidt telescope equipped with the TAUKAM 6k x 6k CCD 
camera and the wide V-band filter (VB). The transmission curve of this 
filter closely follows the Gaia GBP filter. Observations were performed 
during several epochs starting 1.2 days after the burst.

The optical transient discovered by the MASTER Global Robotic Net (Lipunov 
et al., GCN 27446) is clearly detected (see also Pozanenko et al., GCN 
27452; Belkin et al., GCN 27455; Strausbaugh et al., GCN 27456; D'Avanzo 
et al., GCN 27457). Aperture photometry was performed using several Gaia 
DR2 stars in the field. Between dt = 1.2 and 2.4 days the optical 
transient was fading by 1.3 mag. During our last observation (2.4 days 
post burst) it had reached VB = 20.7 +/- 0.2 mag.


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27465
SUBJECT: GRB 200325B: Mondy continued observations
DATE:    20/03/28 21:26:56 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the  MASTER OT J111012.51+274912.8  (Lipunov et al., GCN 
27446)  afterglow of the Fermi GRB 200325B (Fermi GBM team, GCN 27441) 
with AZT-33IK 1.5-m telescope of Sayan observatory (Mondy) starting on 
2020-03-27 (UT) 14:07:34.
Preliminary photometry of the OT is following.

Date UT start       t-T0  Filter Exp. OT Err UL(3sigma)
                         (mid, days) (s)
2020-03-27 14:07:34 1.9877   R 28*120  21.15  0.06  23.1


the photometry is based on nearby SDSS-DR12 stars
RA DEC               R(Lupton transformations)
167.569191 27.848262 16.015
167.513655 27.832992 16.930
167.510507 27.850424 15.261

The photometry presented above corroborates the photometry presented by 
LCO (Strausbaugh et al. GCN 27456) at about the same time.


GRB_name: GRB200327A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27466
SUBJECT: GRB 200327A: Fermi GBM detection
DATE:    20/03/29 01:40:48 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 20:56:48.17 UT on 27 March 2020, the Fermi Gamma-Ray Burst Monitor
(GBM) triggered
and located GRB 200327A (trigger 607035413 / 200327873) which was also
detected by AGILE-MCAL (Ursi et al., GCN 27461) and localized by IPN (Svinkin
et al., GCN 27463). The GBM on-ground location is consistent with the IPN
position.

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

The GBM light curve consists of two pulses with a duration (T90) of about
0.64 s (50-300 keV). The time-averaged spectrum from T0-64 ms to T0+192 ms
is best fit by a power law function with an exponential high-energy
cutoff.  The power law index is -0.60 +/- 0.09 and the cutoff energy,
parameterized as Epeak, is 1100 +/- 180 keV.

The event fluence (10-1000 keV) in this time interval is (1.53 +/- 0.06)E-6
erg/cm^2. The 64 ms peak photon flux measured starting from T0+64 ms in the
10-1000 keV band is 19.2 +/- 1.4 ph/s/cm^2.

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

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


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27467
SUBJECT: GRB 200325B: Mondy continued observations
DATE:    20/03/29 12:18:52 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the  MASTER OT J111012.51+274912.8  (Lipunov et al., GCN
27446)  afterglow of the Fermi GRB 200325B (Fermi GBM team, GCN 27441)
with AZT-33IK 1.5-m telescope of Sayan observatory (Mondy) starting on
2020-03-28 (UT) 14:50:17.
Preliminary photometry of the OT is following.

Date UT start       t-T0  Filter Exp. OT Err UL(3sigma)
                          (mid, days) (s)
2020-03-28 14:50:17 3.01182  R 20*120  21.82  0.13  23.4


the photometry is based on nearby SDSS-DR12 stars
RA DEC               R(Lupton transformations)
167.569191 27.848262 16.015
167.513655 27.832992 16.930
167.510507 27.850424 15.261


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27468
SUBJECT: GRB 200325B: Mondy continued observations
DATE:    20/03/30 16:43:10 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the  MASTER OT J111012.51+274912.8  (Lipunov et al., GCN
27446)  afterglow of the Fermi GRB 200325B (Fermi GBM team, GCN 27441)
with AZT-33IK 1.5-m telescope of Sayan observatory (Mondy) starting on
2020-03-29 (UT) 13:47:58.
Preliminary photometry of the OT is following.

Date UT start       t-T0  Filter Exp. OT Err UL(3sigma)
                          (mid, days) (s)
2020-03-29 13:47:58 3.96785  R 19*120  22.30  0.25  22.4

the photometry is based on nearby SDSS-DR12 stars
RA DEC               R(Lupton transformations)
167.569191 27.848262 16.015
167.513655 27.832992 16.930
167.510507 27.850424 15.261


GRB_name: GRB200401A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27469
SUBJECT: GRB 200401A: Fermi GBM Final Real-time Localization
DATE:    20/04/01 07:10:47 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 07:00:28 UT on 1 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200401A (trigger 607417233.807052 / 200401292).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 141.1, Dec = 17.4 (J2000 degrees, equivalent to J2000 09h 24m, 17d 23'), with a statistical uncertainty of 13.7 degrees.

The angle from the Fermi LAT boresight is 29.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200401292/quicklook/glg_skymap_all_bn200401292.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/bn200401292/quicklook/glg_healpix_all_bn200401292.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200401292/quicklook/glg_lc_medres34_bn200401292.gif


GRB_name: GRB200401A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27470
SUBJECT: Fermi GRB 200401A: Global MASTER-Net observations report 
DATE:    20/04/01 12:30:16 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 200401A ( Fermi GBM team, GCN 27469) errorbox  15214 sec after notice time and 15242 sec after trigger time at 2020-04-01 11:14:30 UT, with upper limit up to  17.5 mag. Observations started at twilight.  The observations began at zenith distance = 34 deg. The sun  altitude  is -12.0 deg. 

The galactic latitude b = 37 deg., longitude l = 216 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1327489

We obtain a following upper limits.  

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

   15272 | 2020-04-01 11:14:30 |         MASTER-Amur | (09h 27m 57.60s , +18d 03m 51.2s) |   C |    60 | 17.2 |        
   15352 | 2020-04-01 11:15:50 |         MASTER-Amur | (09h 21m 55.66s , +16d 03m 03.0s) |   C |    60 | 17.2 |        
   15431 | 2020-04-01 11:17:09 |         MASTER-Amur | (09h 38m 32.22s , +16d 03m 05.9s) |   C |    60 | 17.1 |        
   15510 | 2020-04-01 11:18:29 |         MASTER-Amur | (09h 34m 43.85s , +20d 03m 44.3s) |   C |    60 | 17.2 |        
   15590 | 2020-04-01 11:19:48 |         MASTER-Amur | (09h 27m 53.86s , +18d 04m 43.8s) |   C |    60 | 17.2 |        
   15669 | 2020-04-01 11:21:08 |         MASTER-Amur | (09h 36m 23.78s , +18d 03m 45.9s) |   C |    60 | 17.2 |        
   15750 | 2020-04-01 11:22:28 |         MASTER-Amur | (09h 21m 51.89s , +16d 02m 42.0s) |   C |    60 | 17.2 |        
   15829 | 2020-04-01 11:23:47 |         MASTER-Amur | (09h 30m 15.73s , +16d 02m 54.4s) |   C |    60 | 17.2 |        
   15909 | 2020-04-01 11:25:07 |         MASTER-Amur | (09h 38m 32.58s , +16d 04m 21.2s) |   C |    60 | 17.0 |        
   15988 | 2020-04-01 11:26:27 |         MASTER-Amur | (09h 46m 51.33s , +16d 03m 13.6s) |   C |    60 | 17.1 |        
   16073 | 2020-04-01 11:27:51 |         MASTER-Amur | (09h 34m 51.09s , +20d 04m 22.2s) |   C |    60 | 17.2 |        
   16157 | 2020-04-01 11:29:16 |         MASTER-Amur | (09h 43m 14.92s , +20d 03m 41.7s) |   C |    60 | 17.1 |        
   16247 | 2020-04-01 11:30:46 |         MASTER-Amur | (09h 36m 16.97s , +18d 04m 42.1s) |   C |    60 | 17.0 |        
   16329 | 2020-04-01 11:32:07 |         MASTER-Amur | (09h 30m 16.05s , +16d 03m 41.8s) |   C |    60 | 17.3 |        
   16408 | 2020-04-01 11:33:27 |         MASTER-Amur | (09h 46m 49.85s , +16d 02m 47.4s) |   C |    60 | 17.1 |        
   16488 | 2020-04-01 11:34:46 |         MASTER-Amur | (09h 43m 22.30s , +20d 03m 01.8s) |   C |    60 | 17.1 |        
   16568 | 2020-04-01 11:36:06 |         MASTER-Amur | (09h 33m 10.02s , +14d 03m 12.4s) |   C |    60 | 17.0 |        
   16648 | 2020-04-01 11:37:26 |         MASTER-Amur | (09h 44m 43.16s , +18d 03m 42.5s) |   C |    60 | 17.1 |        
   16727 | 2020-04-01 11:38:46 |         MASTER-Amur | (09h 16m 44.38s , +14d 03m 37.6s) |   C |    60 | 17.1 |        
   16807 | 2020-04-01 11:40:05 |         MASTER-Amur | (09h 25m 21.07s , +22d 02m 48.1s) |   C |    60 | 17.2 |        
   16886 | 2020-04-01 11:41:25 |         MASTER-Amur | (09h 33m 10.23s , +14d 04m 26.8s) |   C |    60 | 17.3 |        
   16966 | 2020-04-01 11:42:44 |         MASTER-Amur | (09h 41m 25.07s , +14d 02m 50.0s) |   C |    60 | 17.3 |        
   17046 | 2020-04-01 11:44:04 |         MASTER-Amur | (09h 44m 49.15s , +18d 04m 25.7s) |   C |    60 | 17.2 |        
   17126 | 2020-04-01 11:45:24 |         MASTER-Amur | (09h 53m 07.25s , +18d 03m 44.0s) |   C |    60 | 17.2 |        
   17205 | 2020-04-01 11:46:44 |         MASTER-Amur | (09h 16m 37.55s , +14d 04m 36.2s) |   C |    60 | 17.1 |        
   17285 | 2020-04-01 11:48:03 |         MASTER-Amur | (09h 24m 58.46s , +14d 03m 38.1s) |   C |    60 | 17.3 |        
   17364 | 2020-04-01 11:49:23 |         MASTER-Amur | (09h 25m 15.33s , +22d 02m 27.2s) |   C |    60 | 17.2 |        
   17444 | 2020-04-01 11:50:42 |         MASTER-Amur | (09h 33m 59.19s , +22d 02m 42.0s) |   C |    60 | 17.4 |        
   17523 | 2020-04-01 11:52:02 |         MASTER-Amur | (09h 41m 25.38s , +14d 04m 44.0s) |   C |    60 | 17.3 |        
   17612 | 2020-04-01 11:53:30 |         MASTER-Amur | (09h 53m 10.41s , +18d 02m 47.9s) |   C |    60 | 17.2 |        
   17692 | 2020-04-01 11:54:50 |         MASTER-Amur | (09h 24m 59.64s , +14d 04m 30.5s) |   C |    60 | 17.4 |        
   17771 | 2020-04-01 11:56:09 |         MASTER-Amur | (09h 33m 54.25s , +22d 03m 29.0s) |   C |    60 | 17.5 |        
   17851 | 2020-04-01 11:57:29 |         MASTER-Amur | (09h 28m 38.48s , +12d 03m 39.5s) |   C |    60 | 17.0 |        
   17930 | 2020-04-01 11:58:48 |         MASTER-Amur | (09h 42m 38.34s , +22d 02m 46.8s) |   C |    60 | 17.3 |        
   18009 | 2020-04-01 12:00:08 |         MASTER-Amur | (09h 51m 49.87s , +20d 02m 50.8s) |   C |    60 | 17.2 |        
   18096 | 2020-04-01 12:01:34 |         MASTER-Amur | (09h 49m 37.22s , +14d 03m 45.2s) |   C |    60 | 17.2 |        
   18175 | 2020-04-01 12:02:54 |         MASTER-Amur | (09h 28m 32.57s , +12d 04m 39.1s) |   C |    60 | 17.2 |        
   18255 | 2020-04-01 12:04:13 |         MASTER-Amur | (09h 36m 47.63s , +12d 03m 40.5s) |   C |    60 | 17.1 |        
   18334 | 2020-04-01 12:05:32 |         MASTER-Amur | (09h 42m 31.26s , +22d 02m 30.6s) |   C |    60 | 17.2 |        
   18413 | 2020-04-01 12:06:52 |         MASTER-Amur | (09h 51m 15.35s , +22d 02m 59.2s) |   C |    60 | 17.5 |        
   18493 | 2020-04-01 12:08:11 |         MASTER-Amur | (09h 51m 51.16s , +20d 04m 13.2s) |   C |    60 | 17.2 |        
   18572 | 2020-04-01 12:09:31 |         MASTER-Amur | (10h 00m 21.49s , +20d 03m 01.2s) |   C |    60 | 17.3 |        
   18652 | 2020-04-01 12:10:50 |         MASTER-Amur | (09h 49m 42.15s , +14d 04m 43.5s) |   C |    60 | 17.3 |        
   18732 | 2020-04-01 12:12:10 |         MASTER-Amur | (09h 57m 52.00s , +14d 03m 45.9s) |   C |    60 | 17.5 |        
   18811 | 2020-04-01 12:13:29 |         MASTER-Amur | (09h 36m 42.00s , +12d 04m 39.9s) |   C |    60 | 17.1 |        
   18891 | 2020-04-01 12:14:49 |         MASTER-Amur | (09h 51m 16.93s , +22d 03m 31.6s) |   C |    60 | 17.4 |        
   18999 | 2020-04-01 12:16:38 |         MASTER-Amur | (10h 00m 18.41s , +20d 02m 37.0s) |   C |    60 | 17.1 |        
   19079 | 2020-04-01 12:17:57 |         MASTER-Amur | (09h 57m 57.86s , +14d 03m 08.8s) |   C |    60 | 17.3 |        
   19160 | 2020-04-01 12:19:18 |         MASTER-Amur | (09h 55m 13.22s , +16d 02m 50.8s) |   C |    60 | 17.1 |        
   19240 | 2020-04-01 12:20:38 |         MASTER-Amur | (09h 44m 54.12s , +12d 03m 39.8s) |   C |    60 | 16.8 |        
   19329 | 2020-04-01 12:22:08 |         MASTER-Amur | (09h 11m 44.18s , +11d 57m 32.4s) |   C |    60 | 16.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200325B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27471
SUBJECT: GRB 200325B: further Swift-XRT observations
DATE:    20/04/01 14:42:38 GMT
FROM:    Paolo D'Avanzo at INAF - OAB  <paolo.davanzo@inaf.it>

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

Swift-XRT has performed further follow-up observations of the
GBM-detected burst GRB 200325B (Fermi GBM team, GCN Cir. 27441),
collecting overall 4.6 ks of Photon Counting (PC) mode data between
T0+102.4 ks and T0+505.5 ks. 

The uncatalogued X-ray source (Source 1) reported in D'Avanzo et al.
(GCN Circ. 27457) has faded with alpha >1.2, confirming that this is
the GRB afterglow. 

The results of the XRT-team automatic analysis of the afterglow are at
https://www.swift.ac.uk/ToO_GRBs/00020978/Source1.php.
The results of the full analysis of the XRT observations are available
at https://www.swift.ac.uk/ToO_GRBs/00020978.

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


GRB_name: GRB200402A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27472
SUBJECT: GRB 200402A: Fermi GBM Final Real-time Localization
DATE:    20/04/02 09:49:59 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 09:39:37 UT on 2 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200402A (trigger 607513182.90837 / 200402403).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 50.5, Dec = 42.3 (J2000 degrees, equivalent to J2000 03h 22m, 42d 17'), with a statistical uncertainty of 5.1 degrees.

The angle from the Fermi LAT boresight is 88.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200402403/quicklook/glg_skymap_all_bn200402403.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/bn200402403/quicklook/glg_healpix_all_bn200402403.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200402403/quicklook/glg_lc_medres34_bn200402403.gif


GRB_name: GRB200325B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27473
SUBJECT: GRB 200325B: Optical upper limit
DATE:    20/04/02 10:08:41 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

TITLE:   GCN CIRCULAR
NUMBER:  27472
SUBJECT: GRB 200325B: Optical upper limit
DATE:    20/04/02 9:44:53 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com,amit@aries.res.in>

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

We observed the optical afterglow field of the Fermi GRB 200325B
(Fermi GBM team, GCN 27441, Lipunov et al., GCN 27446)
with 1.3m Devsthal Fast Optical Telescope (DFOT) at Aryabhatta
Research Institute of Observational Sciences (ARIES), Nainital
(India),
from 2020-03-30 UT 19:37:08 to 2020-03-30 UT 20:59:28. We observed 16
frames each of 300 seconds in Bessell I filter.
No new optical source was detected within the Swift XRT enhanced error
circle in any individual as well as stacked frame.


The 3-sigma upper limit is as follows:

T_start-T0 (days)   Start Date (UTC)             End Date (UTC)
      Filter        3-sigma upper limit (mag)
---------------------------------------------------------------------------------------------------------------
5.21                2020-03-30 19:37:08          2020-03-30 20:59:28
        I               >23.2

Photometry is done based on the standard star PB 2256 and USNO-B1.0
catalog. The quoted magnitude is not corrected for Galactic
extinction.


GRB_name: GRB200402A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27474
SUBJECT: GRB 200402A: BALROG localization (Fermi Trigger 607513182 / GRB 200402403)
DATE:    20/04/02 10:20:48 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
607513182 at 09:39:37 on 02 April 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) = 44.0+/-2.4 deg
Decl.(2000.0) = 43.7+/-2.3 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200402403/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200402403/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200402403/json

                        


GRB_name: GRB200402A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27475
SUBJECT: Fermi GRB 200402A: Global MASTER-Net observations report 
DATE:    20/04/02 11:30:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 200402A ( Fermi GBM team, GCN 27472) errorbox  5729 sec after notice time and 5754 sec after trigger time at 2020-04-02 11:15:32 UT, with upper limit up to  17.0 mag. Observations started at twilight.  The observations began at zenith distance = 55 deg. The sun  altitude  is -11.9 deg. 

The galactic latitude b = -12 deg., longitude l = 151 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1328194

We obtain a following upper limits.  

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

    5785 | 2020-04-02 11:15:32 |         MASTER-Amur | (02h 52m 11.07s , +43d 55m 08.3s) |   C |    60 | 15.8 |        
    5864 | 2020-04-02 11:16:52 |         MASTER-Amur | (02h 46m 41.32s , +41d 54m 04.5s) |   C |    60 | 15.8 |        
    5944 | 2020-04-02 11:18:11 |         MASTER-Amur | (02h 58m 14.77s , +45d 54m 24.0s) |   C |    60 | 16.1 |        
    6105 | 2020-04-02 11:20:53 |         MASTER-Amur | (02h 52m 05.11s , +43d 55m 55.5s) |   C |    60 | 16.7 |        
    6185 | 2020-04-02 11:22:12 |         MASTER-Amur | (03h 03m 17.29s , +43d 54m 57.2s) |   C |    60 | 17.0 |        
    6264 | 2020-04-02 11:23:32 |         MASTER-Amur | (02h 46m 34.49s , +41d 53m 50.0s) |   C |    60 | 16.6 |        
    6344 | 2020-04-02 11:24:51 |         MASTER-Amur | (02h 57m 26.77s , +41d 54m 01.6s) |   C |    60 | 16.9 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200402B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27476
SUBJECT: GRB 200402B: BALROG localization (Fermi Trigger 607537834 / GRB 200402688)
DATE:    20/04/02 16:53:08 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
607537834 at 16:30:29 on 02 April 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) = 193.9+/-2.2 deg
Decl.(2000.0) = -10.1+/-2.7 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200402688/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200402688/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200402688/json

                        


GRB_name: GRB200402B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27478
SUBJECT: GRB 200402B: Fermi GBM Final Localization
DATE:    20/04/02 17:36:11 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

At 16:30:29.65 UT on 2 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200402B (trigger 607537834 / 200402688). This
trigger was initially classified as a particle event by the flight
software, but is in fact a GRB.

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 190.1, Dec = -6.6 (J2000 degrees, equivalent to J2000 12h 40m, -06d 36'),
with a statistical uncertainty of 6.5 degrees.

The angle from the Fermi LAT boresight is 88 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200402688/quicklook/glg_skymap_all_bn200402688.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/bn200402688/quicklook/glg_healpix_all_bn200402688.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200402688/quicklook/glg_lc_medres34_bn200402688.gif


GRB_name: GRB200402C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27479
SUBJECT: GRB 200402C: Fermi GBM Final Localization
DATE:    20/04/02 21:07:24 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

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

At 19:46:23.08 UT on 2 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200402C (trigger 607549588 / 200402824). This
trigger was initially classified as a particle event by the flight
software, but is in fact a GRB.

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 226.4, Dec = -8.1 (J2000 degrees, equivalent to J2000 15h 06m, -08d 06'),
with a statistical uncertainty of 9.0 degrees.

The angle from the Fermi LAT boresight is 83 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200402824/quicklook/glg_skymap_all_bn200402824.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/bn200402824/quicklook/glg_healpix_all_bn200402824.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200402824/quicklook/glg_lc_medres34_bn200402824.gif


GRB_name: GRB200402C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27480
SUBJECT: Fermi GRB 200402C: Global MASTER-Net observations report 
DATE:    20/04/02 21:15:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200402C ( Fermi GBM team, GCN 27479) errorbox  795 sec after notice time and 824 sec after trigger time at 2020-04-02 20:00:07 UT, with upper limit up to  18.8 mag. The observations began at zenith distance = 71 deg. The sun  altitude  is -38.9 deg. 

MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200402C errorbox  3198 sec after notice time and 3226 sec after trigger time at 2020-04-02 20:40:09 UT, with upper limit up to  17.5 mag. The observations began at zenith distance = 64 deg. The sun  altitude  is -38.5 deg. 

The galactic latitude b = 41 deg., longitude l = 351 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1328483

We obtain a following upper limits.  

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

     914 | 2020-04-02 20:00:07 |   MASTER-Kislovodsk | (15h 39m 46.92s , -02d 19m 10.2s) |   C |   180 | 18.5 |        
    1342 | 2020-04-02 20:07:15 |   MASTER-Kislovodsk | (15h 41m 28.75s , -04d 17m 34.1s) |   C |   180 | 18.5 |        
    1543 | 2020-04-02 20:10:36 |   MASTER-Kislovodsk | (15h 39m 42.18s , -02d 18m 24.0s) |   C |   180 | 18.8 |        
    1744 | 2020-04-02 20:13:56 |   MASTER-Kislovodsk | (15h 44m 19.40s , -06d 18m 32.7s) |   C |   180 | 18.7 |        
    1884 | 2020-04-02 20:17:17 |   MASTER-Kislovodsk | (14h 59m 55.59s , -08d 17m 44.2s) |   C |    60 | 18.4 |        
    1965 | 2020-04-02 20:18:37 |   MASTER-Kislovodsk | (15h 04m 49.88s , -10d 17m 55.1s) |   C |    60 | 18.2 |        
    2045 | 2020-04-02 20:19:58 |   MASTER-Kislovodsk | (14h 56m 01.60s , -06d 17m 06.3s) |   C |    60 | 18.6 |        
    2126 | 2020-04-02 20:21:18 |   MASTER-Kislovodsk | (15h 12m 12.24s , -06d 17m 29.7s) |   C |    60 | 18.1 |        
    2466 | 2020-04-02 20:25:59 |   MASTER-Kislovodsk | (15h 41m 29.86s , -04d 18m 49.1s) |   C |   180 | 18.8 |        
    2868 | 2020-04-02 20:32:40 |   MASTER-Kislovodsk | (15h 44m 17.84s , -06d 18m 41.3s) |   C |   180 | 18.6 |        
    3209 | 2020-04-02 20:39:22 |   MASTER-Kislovodsk | (14h 59m 51.89s , -08d 16m 45.8s) |   C |    60 | 18.4 |        
    3257 | 2020-04-02 20:40:09 |      MASTER-Tavrida | (14h 57m 13.88s , -03d 29m 26.4s) |   C |    60 | 15.2 |        
    3290 | 2020-04-02 20:40:42 |   MASTER-Kislovodsk | (15h 07m 57.40s , -08d 15m 55.7s) |   C |    60 | 18.3 |        
    3370 | 2020-04-02 20:42:03 |   MASTER-Kislovodsk | (15h 04m 56.13s , -10d 16m 49.8s) |   C |    60 | 18.3 |        
    3451 | 2020-04-02 20:43:24 |   MASTER-Kislovodsk | (15h 12m 55.89s , -10d 18m 00.2s) |   C |    60 | 18.3 |        
    3531 | 2020-04-02 20:44:44 |   MASTER-Kislovodsk | (14h 56m 09.67s , -06d 17m 04.1s) |   C |    60 | 18.6 |        
    3612 | 2020-04-02 20:46:04 |   MASTER-Kislovodsk | (15h 04m 09.25s , -06d 15m 45.8s) |   C |    60 | 18.4 |        
    3692 | 2020-04-02 20:47:25 |   MASTER-Kislovodsk | (15h 12m 10.84s , -06d 17m 24.2s) |   C |    60 | 18.4 |        
    3773 | 2020-04-02 20:48:45 |   MASTER-Kislovodsk | (15h 20m 16.38s , -06d 16m 07.6s) |   C |    60 | 18.5 |        
    3819 | 2020-04-02 20:49:32 |      MASTER-Tavrida | (15h 05m 20.26s , -03d 28m 42.8s) |   C |    60 | 15.7 |        
    4141 | 2020-04-02 20:54:53 |      MASTER-Tavrida | (14h 55m 36.26s , -01d 28m 41.2s) |   C |    60 | 17.4 |        
    4221 | 2020-04-02 20:56:14 |      MASTER-Tavrida | (14h 42m 24.22s , -11d 28m 11.8s) |   C |    60 | 16.3 |        
    4302 | 2020-04-02 20:57:34 |      MASTER-Tavrida | (14h 41m 17.34s , -03d 29m 15.5s) |   C |    60 | 17.4 |        
    4455 | 2020-04-02 21:00:08 |   MASTER-Kislovodsk | (15h 07m 59.11s , -08d 17m 23.8s) |   C |    60 | 18.3 |        
    4535 | 2020-04-02 21:01:28 |   MASTER-Kislovodsk | (15h 13m 04.45s , -10d 17m 09.9s) |   C |    60 | 18.3 |        
    4543 | 2020-04-02 21:01:36 |      MASTER-Tavrida | (14h 55m 41.60s , -01d 28m 02.6s) |   C |    60 | 17.5 |        
    4616 | 2020-04-02 21:02:48 |   MASTER-Kislovodsk | (15h 04m 10.48s , -06d 15m 39.0s) |   C |    60 | 18.4 |        
    4624 | 2020-04-02 21:02:56 |      MASTER-Tavrida | (15h 03m 36.08s , -01d 28m 52.9s) |   C |    60 | 17.5 |        
    4696 | 2020-04-02 21:04:09 |   MASTER-Kislovodsk | (15h 20m 14.75s , -06d 17m 33.2s) |   C |    60 | 18.2 |        
    4704 | 2020-04-02 21:04:17 |      MASTER-Tavrida | (14h 42m 19.74s , -11d 27m 19.2s) |   C |    60 | 17.0 |        
    4776 | 2020-04-02 21:05:29 |   MASTER-Kislovodsk | (14h 45m 21.39s , -14d 15m 54.5s) |   C |    60 | 18.2 |        
    4785 | 2020-04-02 21:05:37 |      MASTER-Tavrida | (14h 50m 35.10s , -11d 28m 24.6s) |   C |    60 | 16.2 |        
    4856 | 2020-04-02 21:06:49 |   MASTER-Kislovodsk | (15h 25m 32.44s , -04d 16m 40.2s) |   C |    60 | 18.3 |        
    4865 | 2020-04-02 21:06:58 |      MASTER-Tavrida | (14h 41m 12.31s , -03d 29m 30.5s) |   C |    60 | 17.4 |        
    4937 | 2020-04-02 21:08:10 |   MASTER-Kislovodsk | (15h 28m 20.50s , -06d 17m 26.3s) |   C |    60 | 18.2 |        
    4946 | 2020-04-02 21:08:19 |      MASTER-Tavrida | (14h 49m 17.89s , -03d 29m 21.3s) |   C |    60 | 17.4 |        
    5018 | 2020-04-02 21:09:30 |   MASTER-Kislovodsk | (14h 32m 27.83s , -10d 16m 08.1s) |   C |    60 | 18.2 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200325B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27481
SUBJECT: GRB 200325B: Mondy continued observations
DATE:    20/04/03 08:42:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We continued observations of the  MASTER OT J111012.51+274912.8 
(Lipunov et al., GCN 27446)  which is now is confirmed afterglow 
(Pozanenko et al., GCN 27452; Strausbaugh et al.,  GCN 27456; Klose et 
al.,  GCN 27464; D'Ai  et al.,  GCN 27471) of the Fermi GRB 200325B 
(Fermi GBM team, GCN 27441) with AZT-33IK 1.5-m telescope of Sayan 
observatory (Mondy).
Preliminary photometry of the OT is following.

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

2020-03-30  15:07:22 5.03063  R 30*120  22.40  0.20  22.7
2020-03-31  17:09:44 6.11561  R 30*120  22.45  0.17  22.8
2020-04-01  16:40:59 7.10254  R 40*120  n/d    n/d   22.6

the photometry is based on nearby SDSS-DR12 stars
RA         DEC       R(Lupton transformations)
167.569191 27.848262 16.015
167.513655 27.832992 16.930
167.510507 27.850424 15.261

A light curve of the GRB 200325B afterglow based on our observations 
(Belkin et al., GCNs 27455, 27465, 27467, 27468) can be found at 
http://grb.rssi.ru/GRB200325B/GRB200325B_lc.png


GRB_name: GRB200403A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27482
SUBJECT: GRB 200403A: Fermi GBM Final Real-time Localization
DATE:    20/04/03 21:40:37 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 21:30:16 UT on 3 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200403A (trigger 607642221.34614 / 200403896).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 81.3, Dec = 73.3 (J2000 degrees, equivalent to J2000 05h 25m, 73d 17'), with a statistical uncertainty of 1.1 degrees.

The angle from the Fermi LAT boresight is 161.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200403896/quicklook/glg_skymap_all_bn200403896.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/bn200403896/quicklook/glg_healpix_all_bn200403896.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200403896/quicklook/glg_lc_medres34_bn200403896.gif


GRB_name: GRB200403B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27484
SUBJECT: GRB 200403B: Fermi GBM Final Real-time Localization
DATE:    20/04/03 22:14:27 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 22:04:03 UT on 3 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200403B (trigger 607644248.41943 / 200403919).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 239.9, Dec = 73.2 (J2000 degrees, equivalent to J2000 15h 59m, 73d 12'), with a statistical uncertainty of 4.2 degrees.

The angle from the Fermi LAT boresight is 36.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200403919/quicklook/glg_skymap_all_bn200403919.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/bn200403919/quicklook/glg_healpix_all_bn200403919.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200403919/quicklook/glg_lc_medres34_bn200403919.gif


GRB_name: GRB200403C
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27489
SUBJECT: GRB 200403C: Fermi GBM Final Real-time Localization
DATE:    20/04/03 23:32:22 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 23:21:57 UT on 3 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200403C (trigger 607648922.370564 / 200403974).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 48.8, Dec = 19.1 (J2000 degrees, equivalent to J2000 03h 15m, 19d 06'), with a statistical uncertainty of 5.0 degrees.

The angle from the Fermi LAT boresight is 107.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200403974/quicklook/glg_skymap_all_bn200403974.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/bn200403974/quicklook/glg_healpix_all_bn200403974.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200403974/quicklook/glg_lc_medres34_bn200403974.gif


GRB_name: GRB200403A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27490
SUBJECT: Fermi GRB 200403A: Global MASTER-Net observations report 
DATE:    20/04/04 08:00:09 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),

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200403A ( Fermi GBM team, GCN 27482) errorbox  36 sec after notice time and 64 sec after trigger time at 2020-04-03 21:31:20 UT, with upper limit up to  18.5 mag. The observations began at zenith distance = 51 deg. The sun  altitude  is -40.2 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200403A errorbox  5527 sec after notice time and 5555 sec after trigger time at 2020-04-03 23:02:52 UT, with upper limit up to  18.9 mag. The observations began at zenith distance = 62 deg. The sun  altitude  is -35.4 deg. 

The galactic latitude b = 21 deg., longitude l = 142 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1329090

We obtain a following upper limits.  

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

      69 | 2020-04-03 21:31:20 |      MASTER-Tavrida | (06h 03m 30.97s , +73d 27m 42.3s) |   C |    10 | 16.8 |        
     105 | 2020-04-03 21:31:51 |      MASTER-Tavrida | (06h 02m 42.66s , +73d 28m 28.0s) |   C |    20 | 17.4 |        
    1393 | 2020-04-03 21:52:59 |      MASTER-Tavrida | (05h 09m 17.87s , +71d 17m 20.8s) |   C |    60 | 17.6 |        
    1474 | 2020-04-03 21:54:19 |      MASTER-Tavrida | (05h 46m 40.66s , +73d 18m 35.6s) |   C |    60 | 16.8 |        
    2917 | 2020-04-03 22:18:23 |      MASTER-Tavrida | (05h 09m 20.99s , +71d 18m 05.3s) |   C |    60 | 17.7 |        
    2997 | 2020-04-03 22:19:43 |      MASTER-Tavrida | (05h 35m 03.03s , +71d 17m 48.8s) |   C |    60 | 17.8 |        
    3078 | 2020-04-03 22:21:04 |      MASTER-Tavrida | (05h 46m 51.99s , +73d 18m 07.5s) |   C |    60 | 18.0 |        
    3158 | 2020-04-03 22:22:24 |      MASTER-Tavrida | (06h 15m 43.28s , +73d 20m 59.6s) |   C |    60 | 18.0 |        
    4576 | 2020-04-03 22:46:02 |      MASTER-Tavrida | (05h 35m 07.25s , +71d 19m 49.2s) |   C |    60 | 17.9 |        
    4657 | 2020-04-03 22:47:23 |      MASTER-Tavrida | (06h 15m 55.03s , +73d 20m 01.5s) |   C |    60 | 18.1 |        
    4737 | 2020-04-03 22:48:43 |      MASTER-Tavrida | (05h 29m 21.00s , +75d 17m 32.7s) |   C |    60 | 18.2 |        
    4818 | 2020-04-03 22:50:04 |      MASTER-Tavrida | (06h 01m 00.14s , +71d 18m 50.9s) |   C |    60 | 18.0 |        
    4898 | 2020-04-03 22:51:24 |      MASTER-Tavrida | (05h 26m 01.86s , +69d 18m 22.2s) |   C |    60 | 17.8 |        
    5059 | 2020-04-03 22:54:05 |      MASTER-Tavrida | (05h 29m 14.89s , +75d 17m 27.9s) |   C |    60 | 18.2 |        
    5220 | 2020-04-03 22:56:46 |      MASTER-Tavrida | (06h 01m 00.67s , +71d 19m 57.3s) |   C |    60 | 17.0 |        
    5586 | 2020-04-03 23:02:52 |   MASTER-Kislovodsk | (04h 56m 58.20s , +72d 18m 49.4s) |   C |    60 | 18.1 |        
    6590 | 2020-04-03 23:19:36 |      MASTER-Tavrida | (06h 26m 53.55s , +71d 21m 22.8s) |   C |    60 | 18.0 |        
    6671 | 2020-04-03 23:20:57 |      MASTER-Tavrida | (05h 26m 09.73s , +69d 18m 26.5s) |   C |    60 | 17.8 |        
    6751 | 2020-04-03 23:22:17 |      MASTER-Tavrida | (05h 49m 24.89s , +69d 18m 06.2s) |   C |    60 | 17.9 |        
    7073 | 2020-04-03 23:27:39 |      MASTER-Tavrida | (06h 26m 58.66s , +71d 20m 57.9s) |   C |    60 | 18.2 |        
    7153 | 2020-04-03 23:28:59 |      MASTER-Tavrida | (05h 49m 25.62s , +69d 19m 00.9s) |   C |    60 | 17.6 |        
    8324 | 2020-04-03 23:48:30 |   MASTER-Kislovodsk | (04h 57m 13.02s , +72d 16m 06.6s) |   C |    60 | 18.2 |        
    8404 | 2020-04-03 23:49:50 |   MASTER-Kislovodsk | (05h 22m 51.79s , +72d 15m 25.0s) |   C |    60 | 18.3 |        
    8485 | 2020-04-03 23:51:11 |   MASTER-Kislovodsk | (05h 32m 54.85s , +74d 17m 11.2s) |   C |    60 | 18.6 |        
    8646 | 2020-04-03 23:53:51 |   MASTER-Kislovodsk | (05h 15m 12.48s , +70d 17m 16.5s) |   C |    60 | 18.1 |        
    8726 | 2020-04-03 23:55:12 |   MASTER-Kislovodsk | (05h 23m 00.88s , +72d 16m 18.3s) |   C |    60 | 18.3 |        
    8806 | 2020-04-03 23:56:32 |   MASTER-Kislovodsk | (05h 32m 55.40s , +74d 15m 21.6s) |   C |    60 | 18.6 |        
    8887 | 2020-04-03 23:57:53 |   MASTER-Kislovodsk | (06h 01m 51.41s , +74d 15m 53.8s) |   C |    60 | 18.7 |        
    9208 | 2020-04-04 00:03:14 |   MASTER-Kislovodsk | (05h 38m 34.54s , +70d 16m 27.1s) |   C |    60 | 18.2 |        
    9288 | 2020-04-04 00:04:34 |   MASTER-Kislovodsk | (06h 01m 49.69s , +74d 17m 41.1s) |   C |    60 | 18.8 |        
    9449 | 2020-04-04 00:07:15 |   MASTER-Kislovodsk | (05h 48m 50.54s , +72d 15m 52.3s) |   C |    60 | 18.5 |        
    9529 | 2020-04-04 00:08:35 |   MASTER-Kislovodsk | (05h 38m 38.45s , +70d 17m 08.3s) |   C |    60 | 18.2 |        
    9770 | 2020-04-04 00:12:36 |   MASTER-Kislovodsk | (05h 48m 52.83s , +72d 16m 24.0s) |   C |    60 | 18.6 |        
    9851 | 2020-04-04 00:13:56 |   MASTER-Kislovodsk | (06h 14m 31.83s , +72d 15m 46.9s) |   C |    60 | 18.9 |        
   10203 | 2020-04-04 00:19:49 |      MASTER-Tavrida | (05h 18m 04.58s , +73d 18m 13.7s) |   C |    60 | 18.2 |        
   10252 | 2020-04-04 00:20:38 |   MASTER-Kislovodsk | (06h 14m 34.61s , +72d 16m 39.5s) |   C |    60 | 18.9 |        
   10654 | 2020-04-04 00:27:20 |   MASTER-Kislovodsk | (06h 01m 57.31s , +70d 16m 29.3s) |   C |    60 | 18.7 |        
   11055 | 2020-04-04 00:34:01 |   MASTER-Kislovodsk | (06h 02m 05.17s , +70d 18m 17.8s) |   C |    60 | 18.8 |        
   11136 | 2020-04-04 00:35:22 |   MASTER-Kislovodsk | (06h 25m 21.54s , +70d 17m 10.1s) |   C |    60 | 18.8 |        
   11457 | 2020-04-04 00:40:43 |   MASTER-Kislovodsk | (06h 25m 17.95s , +70d 16m 36.9s) |   C |    60 | 18.9 |        
   11925 | 2020-04-04 00:48:30 |      MASTER-Tavrida | (05h 21m 22.25s , +74d 11m 54.5s) |   C |    60 | 18.5 |        
   16683 | 2020-04-04 02:07:49 |      MASTER-Tavrida | (05h 05m 39.87s , +70d 10m 30.5s) |   C |    60 | 18.0 |        
   16923 | 2020-04-04 02:11:49 |      MASTER-Tavrida | (06h 15m 46.19s , +70d 14m 23.5s) |   C |    60 | 18.1 |        
   17047 | 2020-04-04 02:13:53 |      MASTER-Tavrida | (05h 05m 33.52s , +70d 11m 27.4s) |   C |    60 | 17.5 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200403B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27491
SUBJECT: Fermi GRB 200403B: Global MASTER-Net observations report 
DATE:    20/04/04 08:00:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Tavrida robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 200403B ( Fermi GBM team, GCN 27484) errorbox  6502 sec after notice time and 6530 sec after trigger time at 2020-04-03 23:52:54 UT, with upper limit up to  19.7 mag. The observations began at zenith distance = 33 deg. The sun  altitude  is -32.7 deg. 

MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200403B errorbox  9291 sec after notice time and 9319 sec after trigger time at 2020-04-04 00:39:23 UT, with upper limit up to  19.6 mag. The observations began at zenith distance = 27 deg. The sun  altitude  is -22.8 deg. 

The galactic latitude b = 34 deg., longitude l = 107 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1329159

We obtain a following upper limits.  

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

    6561 | 2020-04-03 23:52:54 |      MASTER-Tavrida | (17h 19m 29.12s , +72d 29m 19.2s) |   C |    60 | 19.0 |        
    6642 | 2020-04-03 23:54:15 |      MASTER-Tavrida | (16h 27m 37.28s , +72d 30m 45.6s) |   C |    60 | 19.0 |        
    8258 | 2020-04-04 00:21:11 |      MASTER-Tavrida | (17h 19m 26.57s , +72d 27m 30.6s) |   C |    60 | 19.2 |        
    8338 | 2020-04-04 00:22:31 |      MASTER-Tavrida | (17h 45m 28.63s , +72d 27m 18.3s) |   C |    60 | 19.0 |        
    8419 | 2020-04-04 00:23:52 |      MASTER-Tavrida | (16h 27m 34.56s , +72d 30m 31.0s) |   C |    60 | 18.8 |        
    9350 | 2020-04-04 00:39:23 |   MASTER-Kislovodsk | (16h 57m 40.90s , +69d 44m 20.8s) |   C |    60 | 19.6 |        
    9510 | 2020-04-04 00:42:03 |   MASTER-Kislovodsk | (17h 54m 44.01s , +71d 44m 38.4s) |   C |    60 | 19.1 |        
    9671 | 2020-04-04 00:44:44 |   MASTER-Kislovodsk | (16h 57m 38.95s , +69d 45m 06.5s) |   C |    60 | 19.5 |        
    9804 | 2020-04-04 00:46:56 |      MASTER-Tavrida | (16h 53m 18.54s , +72d 30m 00.4s) |   C |    60 | 18.6 |        
    9832 | 2020-04-04 00:47:25 |   MASTER-Kislovodsk | (17h 54m 52.89s , +71d 44m 37.3s) |   C |    60 | 19.1 |        
    9978 | 2020-04-04 00:49:51 |      MASTER-Tavrida | (17h 42m 09.04s , +71d 31m 53.0s) |   C |    60 | 19.1 |        
   10073 | 2020-04-04 00:51:26 |   MASTER-Kislovodsk | (15h 43m 47.62s , +72d 31m 22.9s) |   C |    60 | 17.3 |        
   10139 | 2020-04-04 00:52:32 |      MASTER-Tavrida | (16h 50m 13.13s , +71d 34m 54.6s) |   C |    60 | 19.4 |        
   10219 | 2020-04-04 00:53:52 |      MASTER-Tavrida | (15h 26m 54.60s , +75d 37m 30.7s) |   C |    60 | 19.3 |        
   10299 | 2020-04-04 00:55:12 |      MASTER-Tavrida | (16h 33m 27.54s , +75d 36m 07.9s) |   C |    60 | 19.3 |        
   10315 | 2020-04-04 00:55:27 |   MASTER-Kislovodsk | (17h 02m 46.31s , +71d 46m 04.3s) |   C |    60 | 16.7 |        
   11782 | 2020-04-04 01:19:55 |      MASTER-Tavrida | (16h 08m 31.96s , +78d 30m 31.9s) |   C |    60 | 19.5 |        
   11863 | 2020-04-04 01:21:16 |      MASTER-Tavrida | (15h 30m 54.56s , +76d 30m 34.7s) |   C |    60 | 19.4 |        
   11944 | 2020-04-04 01:22:37 |      MASTER-Tavrida | (16h 04m 16.55s , +76d 30m 04.3s) |   C |    60 | 19.5 |        
   12024 | 2020-04-04 01:23:57 |      MASTER-Tavrida | (16h 37m 28.83s , +76d 30m 32.4s) |   C |    60 | 19.5 |        
   12105 | 2020-04-04 01:25:18 |      MASTER-Tavrida | (17h 10m 38.63s , +76d 28m 08.5s) |   C |    60 | 19.3 |        
   12186 | 2020-04-04 01:26:39 |      MASTER-Tavrida | (16h 08m 35.80s , +78d 31m 20.0s) |   C |    60 | 19.7 |        
   12266 | 2020-04-04 01:27:59 |      MASTER-Tavrida | (16h 04m 12.66s , +76d 30m 44.5s) |   C |    60 | 19.5 |        
   13592 | 2020-04-04 01:50:05 |      MASTER-Tavrida | (17h 10m 34.15s , +76d 29m 37.1s) |   C |    60 | 19.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200403A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27492
SUBJECT: GRB 200403A: AstroSat CZTI detection
DATE:    20/04/04 14:12:59 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 200403A, which was also detected by Fermi GBM Final Real-time (GCN #27482) and Global MASTER-Net (Lipunov V. et al., GCN #27490) . 

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 2020-04-03 21:30:16 UT. The measured peak count rate associated with the burst is 220 +/- 18.3 cts/s above the background in the combined data of four quadrants, with a total of 2564 +/- 50.1 cts. The local mean background count rate was 578 +/- 1.2 cts/s. Using cumulative rates, we measure a T90 of 25.5 +/- 1.08 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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


GRB_name: GRB200404A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27493
SUBJECT: GRB 200404A: BALROG localization (Fermi Trigger 607712227 / GRB 200404706)
DATE:    20/04/04 17:32:47 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
607712227 at 16:57:02 on 04 April 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) = 59.1+/-2.7 deg
Decl.(2000.0) = 6.7+/-1.9 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200404706/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200404706/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200404706/json

                        


GRB_name: GRB200403C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27494
SUBJECT: Fermi GRB 200403C: Global MASTER-Net observations report 
DATE:    20/04/04 18:15:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Kislovodsk robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 200403C ( Fermi GBM team, GCN 27489) errorbox  62342 sec after notice time and 62370 sec after trigger time at 2020-04-04 16:41:27 UT, with upper limit up to  17.3 mag. Observations started at twilight.  The observations began at zenith distance = 68 deg. The sun  altitude  is -11.6 deg. 

The galactic latitude b = -32 deg., longitude l = 163 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1329210

We obtain a following upper limits.  

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

   62401 | 2020-04-04 16:41:27 |   MASTER-Kislovodsk | (03h 11m 42.15s , +19d 58m 00.3s) |   C |    60 | 16.7 |        
   62401 | 2020-04-04 16:41:27 |   MASTER-Kislovodsk | (03h 03m 13.52s , +20d 24m 11.0s) |   C |    60 | 16.7 |        
   62642 | 2020-04-04 16:45:29 |   MASTER-Kislovodsk | (03h 28m 50.74s , +19d 56m 42.9s) |   C |    60 | 17.0 |        
   62642 | 2020-04-04 16:45:29 |   MASTER-Kislovodsk | (03h 20m 20.50s , +20d 22m 48.3s) |   C |    60 | 17.0 |        
   62722 | 2020-04-04 16:46:49 |   MASTER-Kislovodsk | (03h 11m 45.22s , +19d 57m 25.2s) |   C |    60 | 17.0 |        
   62722 | 2020-04-04 16:46:49 |   MASTER-Kislovodsk | (03h 03m 16.81s , +20d 23m 27.9s) |   C |    60 | 17.0 |        
   62978 | 2020-04-04 16:51:05 |   MASTER-Kislovodsk | (03h 28m 45.82s , +19d 57m 12.6s) |   C |    60 | 17.1 |        
   62978 | 2020-04-04 16:51:05 |   MASTER-Kislovodsk | (03h 20m 15.83s , +20d 23m 15.2s) |   C |    60 | 17.3 |        
   63058 | 2020-04-04 16:52:25 |   MASTER-Kislovodsk | (03h 14m 17.49s , +21d 57m 37.1s) |   C |    60 | 16.9 |        
   63058 | 2020-04-04 16:52:25 |   MASTER-Kislovodsk | (03h 05m 41.29s , +22d 23m 38.2s) |   C |    60 | 17.0 |        
   63139 | 2020-04-04 16:53:46 |   MASTER-Kislovodsk | (03h 26m 22.18s , +17d 56m 59.2s) |   C |    60 | 16.9 |        
   63139 | 2020-04-04 16:53:46 |   MASTER-Kislovodsk | (03h 17m 59.46s , +18d 22m 59.6s) |   C |    60 | 17.0 |        
   63219 | 2020-04-04 16:55:06 |   MASTER-Kislovodsk | (03h 31m 31.08s , +21d 56m 01.3s) |   C |    60 | 17.3 |        
   63219 | 2020-04-04 16:55:06 |   MASTER-Kislovodsk | (03h 22m 53.40s , +22d 22m 04.8s) |   C |    60 | 17.2 |        
   63300 | 2020-04-04 16:56:27 |   MASTER-Kislovodsk | (03h 17m 15.19s , +23d 55m 48.4s) |   C |    60 | 16.6 |        
   63300 | 2020-04-04 16:56:27 |   MASTER-Kislovodsk | (03h 08m 30.41s , +24d 21m 49.5s) |   C |    60 | 16.6 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200404A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27495
SUBJECT: GRB 200404A: Fermi GBM Final Localization
DATE:    20/04/04 19:14:14 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

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

At 16:57:02.83 UT on 4 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200404A (trigger 607712227 / 200404706). This
trigger was initially classified as a solar flare by the flight software,
but is in fact a GRB.

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 61.93, Dec = 3.27, with a statistical uncertainty of 5.02 degrees.

The angle from the Fermi LAT boresight is 90 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200404706/quicklook/glg_skymap_all_bn200404706.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/bn200404706/quicklook/glg_healpix_all_bn200404706.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200404706/quicklook/glg_lc_medres34_bn200404706.gif


GRB_name: GRB200405A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27496
SUBJECT: GRB 200405A: Fermi GBM Final Real-time Localization
DATE:    20/04/05 09:37:43 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 09:27:21 UT on 5 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200405A (trigger 607771646.555024 / 200405394).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 59.8, Dec = -28.6 (J2000 degrees, equivalent to J2000 03h 59m, -28d 36'), with a statistical uncertainty of 5.5 degrees.

The angle from the Fermi LAT boresight is 83.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200405394/quicklook/glg_skymap_all_bn200405394.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/bn200405394/quicklook/glg_healpix_all_bn200405394.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200405394/quicklook/glg_lc_medres34_bn200405394.gif


GRB_name: GRB200405B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27497
SUBJECT: GRB 200405B: Swift/BAT-GUANO detection and *possible* arcminute localization of a short GRB
DATE:    20/04/05 22:52:50 GMT
FROM:    Aaron Tohuvavohu at U Toronto  <aaron.tohu@gmail.com>

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

Swift/BAT did not trigger on GRB 200405B (T0: 2020-04-05 03:53:38 UTC).

The INTEGRAL/SPI-ACS Notice #8579, distributed at T0+35 seconds
triggered the Swift Mission Operations Center operated Gamma-ray
Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al.
2020, in prep).

Upon trigger by these notices, GUANO sent a command to the Swift Burst
Alert Telescope (BAT) to save 90 seconds of BAT event-mode data from
[-45,+45] seconds around the time of the burst.
All the requested event mode data was delivered to the ground.

In a ground analysis of the data, we detect the burst in the full
detector-summed rates (no localization information) with an SNR of ~9.
The detected duration is ~0.5 seconds.

With a maximum likelihood analysis (DeLaunay et al. 2020, in prep.) on
the event-mode data we detect a location for the burst with a square
root of the test statistic, sqrt(TS), of 12.4. The sqrt(TS) behaves
similarly to SNR.
Using the normal BAT imaging technique, we find an SNR of ~4 at the
same location.

The BAT ground-calculated position is
RA, Dec = 62.7894, -51.5326 deg which is
   RA(J2000)  = 4h 11m 9.5s
   Dec(J2000) =  -51d 31â€™ 57.4â€
with an uncertainty of 4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11.6%.

Due to the low partial coding, and the lack of any localization
information from SPI-ACS for a consistency check, we stress that while
this localization is significant, we cannot be certain of whether or
not the burst actually originated from outside the BAT coded field-of-view.

XRT and UVOT follow-up has been triggered and observations of this
region have already begun. 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: GRB200405A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27498
SUBJECT: Fermi GRB 200405A: Global MASTER-Net observations report 
DATE:    20/04/06 00:15:23 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-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 200405A ( Fermi GBM team, GCN 27496) errorbox  49435 sec after notice time and 49462 sec after trigger time at 2020-04-05 23:11:44 UT, with upper limit up to  16.8 mag. Observations started at twilight.  The observations began at zenith distance = 47 deg. The sun  altitude  is -10.7 deg. 

The galactic latitude b = -48 deg., longitude l = 226 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1330172

We obtain a following upper limits.  

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

   49493 | 2020-04-05 23:11:44 |         MASTER-OAFA | (03h 54m 51.61s , -30d 03m 29.4s) |   C |    60 | 16.4 |        
   49584 | 2020-04-05 23:13:15 |         MASTER-OAFA | (03h 46m 11.39s , -26d 03m 32.4s) |   C |    60 | 16.4 |        
   49675 | 2020-04-05 23:14:46 |         MASTER-OAFA | (04h 08m 21.33s , -28d 02m 21.9s) |   C |    60 | 16.6 |        
   49766 | 2020-04-05 23:16:17 |         MASTER-OAFA | (03h 50m 13.31s , -28d 01m 54.2s) |   C |    60 | 16.8 |        
   49857 | 2020-04-05 23:17:48 |         MASTER-OAFA | (03h 59m 22.88s , -28d 02m 38.1s) |   C |    60 | 16.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200405B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27499
SUBJECT: GRB 200405B: Swift ToO observations
DATE:    20/04/06 06:50:50 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 200405B. 
Automated analysis of the XRT data will be presented online at
https://www.swift.ac.uk/ToO_GRBs/00020979

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: GRB200405B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27500
SUBJECT: GRB 200405B: Swift-XRT observations
DATE:    20/04/06 15:18:06 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

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

Swift-XRT has performed follow-up observations of the INTEGRAL/SPI-ACS
and Swift-BAT GUANO detected possible short burst GRB 200405B (James
DeLaunay et al. GCN Circ. 27497), collecting 5.0 ks of Photon Counting
(PC) mode data between T0+66.6 ks and T0+80.0 ks. 

Four 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. We note that Source 2 lies within the 4 arcmin BAT error
region reported in GCN Circ. 27497. Details of these sources are given
below:

Source 1:
  RA (J2000):  62.6009  =  04:10:24.21
  Dec (J2000): -51.4435  =  -51:26:36.5
  Error: 5.5 arcsec (radius, 90% conf.)
  Count-rate: (1.87 [+0.90, -0.69])e-3 ct s^-1  
  Distance: 530 arcsec from BAT position.
  Flux: (1.15 [+0.55, -0.43])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 2:
  RA (J2000):  62.8248  =  04:11:17.95
  Dec (J2000): -51.5687  =  -51:34:07.5
  Error: 6.5 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: (3.31 [+1.13, -0.93])e-3 ct s^-1  
  Distance: 152 arcsec from BAT position.
  Flux: (4.1 [+1.4, -1.1])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 3:
  RA (J2000):  62.5137  =  04:10:3.28
  Dec (J2000): -51.4509  =  -51:27:03.3
  Error: 4.6 arcsec (radius, 90% conf.)
  Count-rate: (1.96 [+0.97, -0.73])e-3 ct s^-1  
  Distance: 684 arcsec from BAT position.

Source 4:
  RA (J2000):  62.6146  =  04:10:27.49
  Dec (J2000): -51.5329  =  -51:31:58.3
  Error: 4.3 arcsec (radius, 90% conf.)
  Count-rate: (3.74 [+1.18, -0.99])e-3 ct s^-1  
  Distance: 391 arcsec from BAT position.
  Flux: (1.20 [+0.38, -0.32])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)


The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
https://www.swift.ac.uk/ToO_GRBs/00020979.

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


GRB_name: GRB200405B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27501
SUBJECT: GRB 200405B: LCO Optical Upper Limits
DATE:    20/04/06 19:41:26 GMT
FROM:    Robert Strausbaugh at U. of the Virgin Islands  <robert.strausbaugh@uvi.edu>

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

We observed Swift/BAT-GUANO GRB 200405B (DeLaunay et al., GCN 27497) with the LCO 1-m Sinistro instrument at the Siding Spring Observatory, Australia site, on April 6, from 08:49 to 09:29 UT (corresponding to 28.9 to 29.6 hours from the GRB trigger time) with the Bessel I and R filters.

We performed a series of 5x240s exposures in I and R. We do not detect any fading sources in the individual frames (or in stacked images).  We also do not detect any optical counterparts to the 4 potential Swift XRT candidates (Sbarufatti et al., GCN 27500).  Using the USNO-B.1 catalog as reference, we obtain the following 3-sigma upper limits:

R > 21.75

I > 20.86

These magnitudes are not corrected for galactic extinction.

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


GRB_name: GRB200407A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27502
SUBJECT: GRB 200407A: Fermi GBM Final Real-time Localization
DATE:    20/04/07 06:32:19 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 06:22:01 UT on 7 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200407A (trigger 607933326.481534 / 200407265).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 276.6, Dec = 5.2 (J2000 degrees, equivalent to J2000 18h 26m, 5d 12'), with a statistical uncertainty of 9.2 degrees.

The angle from the Fermi LAT boresight is 79.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200407265/quicklook/glg_skymap_all_bn200407265.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/bn200407265/quicklook/glg_healpix_all_bn200407265.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200407265/quicklook/glg_lc_medres34_bn200407265.gif


GRB_name: GRB200407B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27503
SUBJECT: GRB 200407B: Fermi GBM Final Real-time Localization
DATE:    20/04/07 09:28:46 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 09:18:33 UT on 7 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200407B (trigger 607943918.47521 / 200407388).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 182.0, Dec = 35.4 (J2000 degrees, equivalent to J2000 12h 07m, 35d 23'), with a statistical uncertainty of 4.7 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/bn200407388/quicklook/glg_skymap_all_bn200407388.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/bn200407388/quicklook/glg_healpix_all_bn200407388.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200407388/quicklook/glg_lc_medres34_bn200407388.gif


GRB_name: GRB200405B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27505
SUBJECT: IPN triangulation of GRB 200405B (short)
DATE:    20/04/07 16:47:34 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,

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

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

The short-duration GRB 200405B (DeLaunay et al., GCN Circ. 27497)
was detected by Swift (BAT), INTEGRAL (SPI-ACS), and Konus-Wind,
at about 14018 s UT (03:53:38).
The burst was found in ground analysis of Swift (BAT) data
with low partial coding.

We have triangulated it to INTEGRAL-Konus annulus centered at
RA(2000)=354.104 deg (23h 36m 25s) Dec(2000)=-6.682 deg (-6d 40' 55"),
whose radius is 71.411 +/- 18.656 deg (3 sigma) and
to a BAT-INTEGRAL annulus centered at
RA(2000)=59.460 deg (03h 57m 50s) Dec(2000)=-50.201 deg (-50d 12' 02"),
whose radius is 8.804(-8.804,+15.572) deg (3 sigma).
These annuli intersect to form a very large region
with an area of ~1600 sq. deg.

The Swift-BAT position reported in DeLaunay et al.
is consistent with the IPN localization.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200405_T14018/IPN

The Swift (BAT) event data used for the IPN localization
came from the GUANO system (https://www.swift.psu.edu/guano/).


GRB_name: GRB200407A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27506
SUBJECT: IPN triangulation of GRB 200407A (short)
DATE:    20/04/07 17:57:46 GMT
FROM:    Anna Ridnaia at Ioffe Institute  <ridnaia@mail.ioffe.ru>

A. Ridnaia, D. Svinkin, and K. Hurley, on behalf of the IPN,

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

and

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

The short-duration GRB 200407A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27502)
has been detected by Fermi (GBM trigger 607933326) and
INTEGRAL (SPI-ACS), so far, at about 22921 s UT (06:22:01).

We have triangulated it to a GBM-INTEGRAL annulus centered at
RA(2000)=217.298 deg (14h 29m 12s)  Dec(2000)=+55.704 deg (+55d 42' 15"),
whose radius is 66.821 +/- 4.108 deg (3 sigma).

The IPN localization is consistent with, but reduces the area of, the
Fermi-GBM one.

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200407_T22921/IPN/


GRB_name: GRB200407B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27507
SUBJECT: Fermi GRB 200407B: Global MASTER-Net observations report 
DATE:    20/04/07 21:30:10 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 200407B ( Fermi GBM team, GCN 27503) errorbox  7492 sec after notice time and 7519 sec after trigger time at 2020-04-07 11:23:52 UT, with upper limit up to  16.3 mag. Observations started at twilight.  The observations began at zenith distance = 37 deg. The sun  altitude  is -11.7 deg. 

MASTER-Tunka robotic telescope  located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 200407B errorbox  17824 sec after notice time and 17851 sec after trigger time at 2020-04-07 14:16:05 UT, with upper limit up to  16.3 mag. The observations began at zenith distance = 25 deg. The sun  altitude  is -21.1 deg. 

The galactic latitude b = 78 deg., longitude l = 168 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1331904

We obtain a following upper limits.  

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

    7549 | 2020-04-07 11:23:52 |         MASTER-Amur | (12h 07m 14.05s , +36d 05m 39.6s) |   C |    60 | 13.1 |        
    7629 | 2020-04-07 11:25:12 |         MASTER-Amur | (12h 06m 19.90s , +38d 05m 44.5s) |   C |    60 | 13.8 |        
    7708 | 2020-04-07 11:26:31 |         MASTER-Amur | (11h 47m 25.63s , +36d 05m 58.9s) |   C |    60 | 13.6 |        
    7788 | 2020-04-07 11:27:51 |         MASTER-Amur | (11h 45m 57.49s , +38d 04m 11.2s) |   C |    60 | 13.3 |        
    7869 | 2020-04-07 11:29:12 |         MASTER-Amur | (12h 07m 09.40s , +36d 05m 38.2s) |   C |    60 | 15.0 |        
    7948 | 2020-04-07 11:30:31 |         MASTER-Amur | (12h 17m 08.22s , +36d 05m 08.7s) |   C |    60 | 13.4 |        
    8107 | 2020-04-07 11:33:10 |         MASTER-Amur | (12h 16m 29.87s , +38d 05m 30.4s) |   C |    60 | 13.6 |        
    8194 | 2020-04-07 11:34:37 |         MASTER-Amur | (11h 47m 26.05s , +36d 07m 58.4s) |   C |    60 | 13.0 |        
    8273 | 2020-04-07 11:35:56 |         MASTER-Amur | (11h 57m 19.88s , +36d 06m 41.2s) |   C |    60 | 12.9 |        
    8353 | 2020-04-07 11:37:16 |         MASTER-Amur | (11h 46m 02.55s , +38d 04m 59.2s) |   C |    60 | 14.6 |        
    8433 | 2020-04-07 11:38:36 |         MASTER-Amur | (11h 56m 04.71s , +38d 04m 25.1s) |   C |    60 | 15.4 |        
    8512 | 2020-04-07 11:39:55 |         MASTER-Amur | (12h 17m 03.64s , +36d 05m 54.6s) |   C |    60 | 14.1 |        
    8672 | 2020-04-07 11:42:35 |         MASTER-Amur | (11h 57m 16.86s , +36d 05m 16.8s) |   C |    60 | 14.9 |        
    8751 | 2020-04-07 11:43:54 |         MASTER-Amur | (11h 56m 11.71s , +38d 05m 33.6s) |   C |    60 | 14.8 |        
    9123 | 2020-04-07 11:50:06 |         MASTER-Amur | (12h 06m 14.57s , +40d 05m 36.8s) |   C |    60 | 14.7 |        
    9202 | 2020-04-07 11:51:25 |         MASTER-Amur | (12h 26m 55.64s , +36d 06m 28.4s) |   C |    60 | 14.3 |        
    9282 | 2020-04-07 11:52:45 |         MASTER-Amur | (12h 26m 39.43s , +38d 06m 51.3s) |   C |    60 | 13.8 |        
    9361 | 2020-04-07 11:54:04 |         MASTER-Amur | (11h 45m 24.89s , +40d 03m 05.9s) |   C |    60 | 14.1 |        
    9441 | 2020-04-07 11:55:24 |         MASTER-Amur | (12h 06m 14.59s , +40d 04m 55.9s) |   C |    60 | 14.1 |        
    9520 | 2020-04-07 11:56:43 |         MASTER-Amur | (12h 16m 40.51s , +40d 04m 18.2s) |   C |    60 | 14.7 |        
    9602 | 2020-04-07 11:58:05 |         MASTER-Amur | (12h 27m 03.07s , +36d 06m 17.5s) |   C |    60 | 15.7 |        
    9681 | 2020-04-07 11:59:24 |         MASTER-Amur | (12h 36m 50.78s , +36d 03m 54.2s) |   C |    60 | 14.5 |        
    9844 | 2020-04-07 12:02:07 |         MASTER-Amur | (12h 36m 48.63s , +38d 04m 32.0s) |   C |    60 | 15.5 |        
    9923 | 2020-04-07 12:03:26 |         MASTER-Amur | (11h 45m 19.29s , +40d 04m 10.0s) |   C |    60 | 15.0 |        
   10003 | 2020-04-07 12:04:46 |         MASTER-Amur | (11h 55m 52.29s , +40d 04m 36.0s) |   C |    60 | 14.4 |        
   10162 | 2020-04-07 12:07:25 |         MASTER-Amur | (12h 36m 52.89s , +36d 06m 03.5s) |   C |    60 | 13.3 |        
   10310 | 2020-04-07 12:09:53 |         MASTER-Amur | (12h 07m 01.81s , +42d 05m 01.9s) |   C |    60 | 14.3 |        
   10389 | 2020-04-07 12:11:12 |         MASTER-Amur | (11h 55m 50.71s , +40d 04m 53.6s) |   C |    60 | 14.0 |        
   10469 | 2020-04-07 12:12:32 |         MASTER-Amur | (12h 27m 12.24s , +40d 04m 45.9s) |   C |    60 | 14.1 |        
   10628 | 2020-04-07 12:15:11 |         MASTER-Amur | (12h 07m 09.67s , +42d 07m 02.7s) |   C |    60 | 13.7 |        
   10787 | 2020-04-07 12:17:50 |         MASTER-Amur | (12h 27m 06.29s , +40d 08m 07.2s) |   C |    60 | 14.3 |        
   11025 | 2020-04-07 12:21:48 |         MASTER-Amur | (11h 40m 04.62s , +34d 04m 41.7s) |   C |    60 | 16.1 |        
   11344 | 2020-04-07 12:27:07 |         MASTER-Amur | (11h 40m 00.89s , +34d 04m 58.1s) |   C |    60 | 16.3 |        
   17882 | 2020-04-07 14:16:05 |        MASTER-Tunka | (12h 06m 00.94s , +35d 58m 51.6s) |   C |    60 | 15.0 |        
   17961 | 2020-04-07 14:17:24 |        MASTER-Tunka | (12h 05m 04.45s , +37d 58m 16.5s) |   C |    60 | 15.5 |        
   21594 | 2020-04-07 15:17:57 |        MASTER-Tunka | (11h 46m 00.82s , +36d 01m 12.7s) |   C |    60 | 15.8 |        
   21673 | 2020-04-07 15:19:16 |        MASTER-Tunka | (11h 56m 03.63s , +36d 00m 06.7s) |   C |    60 | 15.8 |        
   21752 | 2020-04-07 15:20:35 |        MASTER-Tunka | (12h 15m 46.01s , +35d 58m 50.6s) |   C |    60 | 16.0 |        
   21832 | 2020-04-07 15:21:55 |        MASTER-Tunka | (12h 15m 11.13s , +37d 58m 57.0s) |   C |    60 | 15.9 |        
   21991 | 2020-04-07 15:24:34 |        MASTER-Tunka | (11h 55m 59.05s , +35d 59m 29.1s) |   C |    60 | 15.2 |        
   22254 | 2020-04-07 15:28:57 |        MASTER-Tunka | (12h 25m 44.31s , +35d 59m 06.2s) |   C |    60 | 15.6 |        
   22492 | 2020-04-07 15:32:55 |        MASTER-Tunka | (11h 54m 40.89s , +38d 00m 25.3s) |   C |    60 | 16.0 |        
   22572 | 2020-04-07 15:34:15 |        MASTER-Tunka | (12h 04m 46.24s , +40d 01m 19.3s) |   C |    60 | 16.3 |        
   22651 | 2020-04-07 15:35:34 |        MASTER-Tunka | (12h 15m 21.43s , +40d 00m 11.3s) |   C |    60 | 16.3 |        
   22731 | 2020-04-07 15:36:53 |        MASTER-Tunka | (12h 25m 37.12s , +35d 59m 05.4s) |   C |    60 | 15.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200407A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27508
SUBJECT: Fermi GRB 200407A: Global MASTER-Net observations report 
DATE:    20/04/08 03:45:08 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-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 200407A ( Fermi GBM team, GCN 27502) errorbox  71781 sec after notice time and 71810 sec after trigger time at 2020-04-08 02:18:51 UT, with upper limit up to  17.3 mag. Observations started at twilight.  The observations began at zenith distance = 43 deg. The sun  altitude  is -10.0 deg. 

MASTER-SAAO robotic telescope  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200407A errorbox  73424 sec after notice time and 73453 sec after trigger time at 2020-04-08 02:46:14 UT, with upper limit up to  19.0 mag. The observations began at zenith distance = 42 deg. The sun  altitude  is -28.0 deg. 

The galactic latitude b =  7 deg., longitude l = 35 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1331640

We obtain a following upper limits.  

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

   71840 | 2020-04-08 02:18:51 |      MASTER-Tavrida | (18h 24m 07.18s , +02d 04m 24.6s) |   C |    60 | 17.3 |        
   71922 | 2020-04-08 02:20:13 |      MASTER-Tavrida | (18h 26m 04.20s , +04d 04m 46.0s) |   C |    60 | 17.1 |        
   72002 | 2020-04-08 02:21:33 |      MASTER-Tavrida | (18h 40m 01.92s , +02d 02m 23.3s) |   C |    60 | 17.3 |        
   72083 | 2020-04-08 02:22:54 |      MASTER-Tavrida | (18h 42m 09.65s , +04d 04m 08.4s) |   C |    60 | 16.6 |        
   73483 | 2020-04-08 02:46:14 |         MASTER-SAAO | (18h 32m 17.25s , +06d 02m 07.6s) |   C |    60 | 18.0 |        
   73485 | 2020-04-08 02:46:16 |         MASTER-SAAO | (18h 25m 13.14s , +06d 01m 29.1s) |   C |    60 | 18.4 |        
   73563 | 2020-04-08 02:47:34 |         MASTER-SAAO | (18h 42m 14.60s , +00d 01m 03.1s) |   C |    60 | 18.5 |        
   73565 | 2020-04-08 02:47:36 |         MASTER-SAAO | (18h 35m 12.38s , +00d 00m 22.6s) |   C |    60 | 18.8 |        
   73643 | 2020-04-08 02:48:54 |         MASTER-SAAO | (18h 26m 09.48s , +00d 00m 01.7s) |   C |    60 | 19.0 |        
   73644 | 2020-04-08 02:48:55 |         MASTER-SAAO | (18h 19m 07.13s , -00d 00m 41.0s) |   C |    60 | 18.9 |        
   73723 | 2020-04-08 02:50:14 |         MASTER-SAAO | (18h 26m 56.94s , -01d 59m 42.6s) |   C |    60 | 19.0 |        
   73724 | 2020-04-08 02:50:15 |         MASTER-SAAO | (18h 19m 54.16s , -02d 00m 26.0s) |   C |    60 | 19.0 |        
   73802 | 2020-04-08 02:51:33 |         MASTER-SAAO | (18h 32m 20.77s , +06d 01m 54.1s) |   C |    60 | 18.0 |        
   73804 | 2020-04-08 02:51:35 |         MASTER-SAAO | (18h 25m 16.17s , +06d 01m 08.2s) |   C |    60 | 18.4 |        
   73882 | 2020-04-08 02:52:53 |         MASTER-SAAO | (18h 42m 13.17s , +00d 00m 21.9s) |   C |    60 | 18.6 |        
   73883 | 2020-04-08 02:52:54 |         MASTER-SAAO | (18h 35m 10.60s , -00d 00m 23.7s) |   C |    60 | 18.8 |        
   73962 | 2020-04-08 02:54:13 |         MASTER-SAAO | (18h 26m 17.09s , +00d 01m 49.6s) |   C |    60 | 19.0 |        
   73963 | 2020-04-08 02:54:14 |         MASTER-SAAO | (18h 19m 14.43s , +00d 01m 02.6s) |   C |    60 | 18.9 |        
   74042 | 2020-04-08 02:55:33 |         MASTER-SAAO | (18h 26m 49.97s , -01d 59m 03.8s) |   C |    60 | 19.0 |        
   74043 | 2020-04-08 02:55:34 |         MASTER-SAAO | (18h 19m 46.93s , -01d 59m 51.0s) |   C |    60 | 19.0 |        
   74121 | 2020-04-08 02:56:52 |         MASTER-SAAO | (18h 42m 50.82s , -01d 58m 11.5s) |   C |    60 | 18.1 |        
   74123 | 2020-04-08 02:56:54 |         MASTER-SAAO | (18h 35m 47.78s , -01d 58m 58.9s) |   C |    60 | 18.4 |        
   74201 | 2020-04-08 02:58:12 |         MASTER-SAAO | (18h 37m 12.32s , +08d 00m 53.1s) |   C |    60 | 17.6 |        
   74203 | 2020-04-08 02:58:14 |         MASTER-SAAO | (18h 30m 05.81s , +08d 00m 03.3s) |   C |    60 | 18.1 |        
   74281 | 2020-04-08 02:59:32 |         MASTER-SAAO | (18h 48m 23.04s , +05d 59m 52.9s) |   C |    60 | 18.5 |        
   74282 | 2020-04-08 02:59:33 |         MASTER-SAAO | (18h 41m 18.29s , +05d 59m 03.7s) |   C |    60 | 18.1 |        
   74362 | 2020-04-08 03:00:53 |         MASTER-SAAO | (18h 05m 53.92s , +03d 59m 33.9s) |   C |    60 | 18.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200409A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27509
SUBJECT: GRB 200409A: Swift detection of a burst with an optical counterpart
DATE:    20/04/09 03:30:47 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J.D. Gropp (PSU), S. D. Barthelmy (GSFC), J. A. Kennea (PSU),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), M. J. Moss (GWU),
D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 03:19:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200409A (trigger=965484).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 60.553, -50.247, which is 
   RA(J2000)  =  04h 02m 13s
   Dec(J2000) = -50d 14' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a total duration of about 20 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 03:21:13.1 UT, 73.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 60.53820, -50.22509 which is equivalent
to:
   RA(J2000)  = 04h 02m 09.17s
   Dec(J2000) = -50d 13' 30.3"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 85 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.27 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 5
(+4.06/-3.42) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 77 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 04:02:08.75 =  60.53646
  DEC(J2000) = -50:13:28.4  = -50.22455
with a 90%-confidence error radius of about 0.77 arc sec. This position is 4.6
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.14 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.01. 

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: GRB200409A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27510
SUBJECT: GRB 200409A: Enhanced Swift-XRT position
DATE:    20/04/09 08:49:18 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 2685 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 200409A, 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 = 60.53633, -50.22498 which is equivalent
to:

RA (J2000): 04h 02m 8.72s
Dec (J2000): -50d 13' 29.9"

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: GRB200409A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27511
SUBJECT: GRB 200409A: Swift-XRT refined Analysis
DATE:    20/04/09 10:11:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.6 ks of XRT data for GRB 200409A (Gropp et al. GCN
Circ. 27509), from 59 s to 18.1 ks after the  BAT trigger. The data
comprise 7 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Evans et al. (GCN Circ.
27510).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=2.8 (+5.2, -0.8). At T+123 s  the decay
flattens to an alpha of -0.2 (+0.4, -0.7) before breaking again at
T+441 s to a final decay with index alpha=0.80 (+0.34, -0.07).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+0.17, -0.16). The
best-fitting absorption column is  3.2 (+3.7, -1.9) x 10^20 cm^-2,
consistent with the Galactic value of 1.3 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.3 x 10^-11 (3.6 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.2 (+3.7, -1.9) x 10^20 cm^-2
Galactic foreground: 1.3 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.94 (+0.17, -0.16)

If the light curve continues to decay with a power-law decay index of
0.80, the count rate at T+24 hours will be 9.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x
10^-13 (3.2 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/00965484.

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


GRB_name: GRB200409A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27512
SUBJECT: Swift GRB 200409A: Global MASTER-Net observations report 
DATE:    20/04/09 17:32:31 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),

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 200409A ( J.D. Gropp et al., GCN 27509) errorbox  49717 sec after notice time and 49742 sec after trigger time at 2020-04-09 17:09:01 UT, with upper limit up to  19.1 mag. Observations started at twilight.  The observations began at zenith distance = 44 deg. The sun  altitude  is -10.2 deg. 

The galactic latitude b = -47 deg., longitude l = 259 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1333122

We obtain a following upper limits.  

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

   49832 |         MASTER-SAAO |   C |   180 | 19.1 |        
   49834 |         MASTER-SAAO |   C |   180 | 19.0 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200409A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27514
SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 200409A
DATE:    20/04/09 18:58:23 GMT
FROM:    Eric Burns at GSFC  <erickayserburns@gmail.com>

E. Burns (GSFC), M. S. Briggs (UAH), C. M. Hui (MSFC), C. Malacaria (MSFC),
and P. Veres (UAH) reports on behalf of the Fermi-GBM Team

Swift-BAT detected GRB 200409A at 03:19:59 UT (GCN 27509). There was no
Fermi-GBM onboard trigger around the event.

An automated, blind search for short gamma-ray bursts below the onboard
triggering threshold in Fermi-GBM identified GRB 200904A with high
reliability [1], with a localization consistent with the Swift-BAT
location, and a discovery timescale of 0.703 s.

The GBM targeted search [2], the most sensitive, coherent search for
GRB-like signals, was run from +/-30 s around BAT trigger time. A transient
source was identified whose most significant timescale according to the
search is 1.024 s, with a log likelihood ratio of 62, with a consistent
location, and is consistent with a soft spectrum for a GRB.

Preliminary spectral analysis statistically prefers a power-law fit over
models that constrain Epeak. Using T0-0.320 to T0+0.320 as the source
interval gives an alpha of -1.84 +/- 0.06, a photon flux of 3.3 +/- 0.4
ph/s/cm^2, and a fluence of (2.0+/-0.2)E-7 erg/s/cm^2.

[1] https://gcn.gsfc.nasa.gov/notices_gbm_sub/608095205.fermi
[2] Goldstein et al. 2019 arXiv:1903.12597


GRB_name: GRB200405B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27516
SUBJECT: GRB 200405B: ATCA follow-up and ASKAP limits on pre-burst radio emission
DATE:    20/04/10 01:56:01 GMT
FROM:    Dougal Dobie at VAST  <ddobie94@gmail.com>

Dougal Dobie (USYD/CSIRO), Tara Murphy (USYD), James Leung (USYD/CSIRO),
Adam Stewart (USYD), Joshua Pritchard (USYD), David Kaplan (UWM)

GRB 200405B (GCN 27497) occurred in a field that has been observed 5 times
as part of the ASKAP Variables And Slow Transients (VAST; Murphy et al.
2013)
pilot survey between 2019-08-27 and 2020-01-25. We have searched for radio
emission from the BAT ground-calculated position and the 4 uncatalogued
X-ray sources detected by Swift (GCN 27500) and find no radio counterparts
to a detection limit of ~1.5 mJy at 888 MHz.

We also performed follow-up observations of all 5 positions with the ATCA
between 2020-04-09 05:00-10:30 UTC with 2x2 GHz bands centered on
5.5 and 9 GHz. No radio emission was detected coincident with any of the
sources, we list 3-sigma upper limits below

Source      5.5 GHz (uJy)    9 GHz (uJy)
BAT pos     81               54
Source 1    90               120
Source 2    84               96
Source 3    87               90
Source 4    90               114

We do detect a radio source at coordinates of 04:10:26.8, -51:31:55
(offset 7.2 arcsec from Source 4), coincident with WISEA
J041026.82-513155.2,
with a flux density of ~4 mJy at 5.5 GHz and ~7 mJy at 9 GHz. This source is
also detected in the VAST pilot survey with a flux density of ~10 mJy. We do
not consider this a candidate afterglow for the GRB.

Further observations with ATCA and as part of the VAST program are planned.

Thank you to CSIRO staff for supporting these observations during these
especially difficult times.


GRB_name: GRB200410A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27518
SUBJECT: GRB 200410A: Swift detection of a burst with a possible optical counterpart
DATE:    20/04/10 02:49:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

K. K. Simpson (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU)
and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels
Swift Observatory Team:

At 02:25:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200410A (trigger=965638).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 299.637, +51.763, which is 
   RA(J2000)  =  19h 58m 33s
   Dec(J2000) = +51d 45' 48"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a total duration of about 45 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 02:26:51.7 UT, 101.3 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 299.6456,
51.7813 which is equivalent to:
   RA(J2000)  = 19h 58m 34.94s
   Dec(J2000) = +51d 46' 52.5"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 68 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (2.15 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 2.3
(+2.17/-1.95) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 104 seconds after the BAT trigger. There is a possible candidate
afterglow in the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 19:58:35.32 = 299.64717
  DEC(J2000) = +51:46:53.0  = +51.78138
with a 90%-confidence error radius of about 0.6 arc sec. This position is 3.5
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.71 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.15. 

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: GRB200409A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27519
SUBJECT: GRB 200409A: Swift-BAT refined analysis
DATE:    20/04/10 03:56:27 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-240 to T+963 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200409A (trigger #965484)
(Gropp et al., GCN Circ. 27509).  The BAT ground-calculated position is
RA, Dec = 60.555, -50.243 deg which is
   RA(J2000)  =  04h 02m 13.3s
   Dec(J2000) = -50d 14' 36.4"
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.

The mask-weighted light curve shows several overlapping pulses that start
at ~T0 and ends at~T+19 s. The main peak occurs at ~T0. T90 (15-350 keV)
is 17.91 +- 5.20 sec (estimated error including systematics).

The time-averaged spectrum from T+0.01 to T+19.01 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
2.14 +- 0.44.  The fluence in the 15-150 keV band is 2.3 +- 0.6 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T+0.01 sec in the 15-150 keV band
is 1.2 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/965484/BA/


GRB_name: GRB200410A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27520
SUBJECT: GRB 200410A: Ondrejov D50 afterglow confirmation
DATE:    20/04/10 04:01:45 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

M. Jelinek, J. Strobl, R. Hudec, C. Polasek (ASU CAS Ondrejov)
report:

We observed the position of the GRB 200410A (Simpson et al., GCN 27518)
with the D50 telescope of the Astronomical Institute Ondrejov, near Prague,
Czech Republic, obtaining a series of 10s unfiltered images starting at
02:26:05.4UT, i.e. 55s post trigger.

The optical afterglow reported from UVOT (Simpson et al., GCN 27518) is
detected in the early single 20 s images.

We note the presence of two nearby stars which may confuse the observer
and/or complicate photometry. For this reason, we do not provide brightness
at this stage.


GRB_name: GRB200409A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27521
SUBJECT: GRB 200409A: No detection of radio emission 5 hours post-burst
DATE:    20/04/10 04:09:36 GMT
FROM:    Dougal Dobie at VAST  <ddobie94@gmail.com>

Dougal Dobie (USYD/CSIRO), Tara Murphy (USYD), David Kaplan (UWM)

While performing follow-up of GRB 200405B (GCN 27497, 27516) we received
notification of the detection of GRB 200409A and the associated optical
and X-ray candidate counterpart (GCN 27509). We added it to our schedule
and carried out observations of it from 2020-04-09 07:00-09:30 UTC,
approximately 5 hours post-burst.

We make no detection of radio emission at 5.5 or 9 GHz with 3-sigma upper
limits of 90 uJy and 81 uJy respectively.

Thank you to CSIRO staff for supporting these observations during these
especially difficult times.


GRB_name: GRB200410A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27522
SUBJECT: GRB 200410A: Enhanced Swift-XRT position
DATE:    20/04/10 07:18:55 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 1479 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200410A, 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 = 299.64593, +51.78078 which is equivalent
to:

RA (J2000): 19h 58m 35.02s
Dec (J2000): +51d 46' 50.8"

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: GRB200410A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27523
SUBJECT: GRB 200410A: Swift-XRT refined Analysis
DATE:    20/04/10 10:52:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 7.0 ks of XRT data for GRB 200410A (Simpson et al. GCN
Circ. 27518), from 86 s to 24.4 ks after the  BAT trigger. The data
comprise 15 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 27522).

The light curve can be modelled with an initial power-law decay with an
index of alpha=4.2 (+2.6, -0.8), followed by a break at T+148 s to an
alpha of 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 1.99 (+0.18, -0.17). The
best-fitting absorption column is  2.7 (+0.7, -0.5) x 10^21 cm^-2,
consistent with the Galactic value of 2.2 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.7 x 10^-11 (5.3 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.7 (+0.7, -0.5) x 10^21 cm^-2
Galactic foreground: 2.2 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.99 (+0.18, -0.17)

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 0.037 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x
10^-12 (1.9 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/00965638.

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


GRB_name: GRB200327A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27525
SUBJECT: Konus-Wind observation of GRB 200327A
DATE:    20/04/10 13:15:13 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 200327A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 27458;
Veres and Meegan, GCN Circ. 27466;
AGILE-MCAL detection: Ursi, et al., GCN Circ. 27461;
IPN triangulation: Svinkin et al., GCN Circ. 27463)
triggered Konus-Wind at T0=75409.744 s UT (20:56:49.744).

The burst light curve shows a double-peaked structure
which starts at ~T0-0.1 s and has a total duration of ~0.2 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/GRB200327_T75409/

As observed by Konus-Wind, the burst
had a fluence of 2.32(-0.67,+0.82)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0-0.016 s,
of 2.45(-1.16,+1.37)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.064 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 = -0.56(-0.36,+0.52)
and Ep = 1323(-545,+961) keV (chi2 = 11/14 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
(chi2 = 11/13 dof).

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


GRB_name: GRB200410A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27532
SUBJECT: GRB 200410A: Swift/UVOT Detection
DATE:    20/04/10 21:38:49 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and K. K. Simpson (PSU) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200410A
104 s after the BAT trigger (Simpson et al., GCN Circ. 27518).
A source consistent with the XRT position (Goad et al. GCN Circ. 27522)
is detected in the initial UVOT exposures.

The uvot position has been determined from the first white image to be
RA  = 19:58:35.3
Dec = +51:46:53.0
or 299.64717 =51.78138 Deg (J2000) with an error estimate of 0.5".
There are two nearby stars visible at 4 and 6 arcsec.


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              104          254          147         19.51 +/- 0.14
v                 5051         6869          396         21.23 +/- 0.90
b                  572         1519           98         19.61 +/- 0.32
u                  317          567          246         20.39 +/- 0.37
w1                 696         1294           57        >19.8
m2                 671         1220           57        >20.0
w2                 622         1270           57        >19.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200411A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27535
SUBJECT: GRB 200411A: Fermi GBM Final Real-time Localization
DATE:    20/04/11 04:39:27 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 04:29:02 UT on 11 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200411A (trigger 608272147.522124 / 200411187).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 69.6, Dec = -60.3 (J2000 degrees, equivalent to J2000 04h 38m, -60d 17'), with a statistical uncertainty of 24.1 degrees.

The angle from the Fermi LAT boresight is 128.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200411187/quicklook/glg_skymap_all_bn200411187.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/bn200411187/quicklook/glg_healpix_all_bn200411187.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200411187/quicklook/glg_lc_medres34_bn200411187.gif


GRB_name: GRB200411A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27536
SUBJECT: GRB 200411A: Swift detection of a short burst
DATE:    20/04/11 04:43:03 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. Tohuvavohu (U Toronto), S. D. Barthelmy (GSFC), J. A. Kennea (PSU),
N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and
T. N. Ukwatta (LANL) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 04:29:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200411A (trigger=965784).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 47.659, -52.314, which is 
   RA(J2000)  =  03h 10m 38s
   Dec(J2000) = -52d 18' 51"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 0.5 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:29:53.0 UT, 50.7 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find a fading, uncatalogued X-ray source located at RA, Dec
47.66239, -52.31805 which is equivalent to:
   RA(J2000)  = 03h 10m 38.97s
   Dec(J2000) = -52d 19' 05.0"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 16 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.55 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 5.4
(+5.14/-3.83) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of nominal 150.000 seconds with the White
filter starting 58 seconds after the BAT trigger. Further analysis is
required before any results can be obtained. 

Burst Advocate for this burst is A. Tohuvavohu (tohuvavohu AT astro.utoronto.ca). 
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: GRB200411A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27538
SUBJECT: GRB 200411A: Enhanced Swift-XRT position
DATE:    20/04/11 09:33:23 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 980 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 200411A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 47.66418, -52.31764 which is equivalent
to:

RA (J2000): 03h 10m 39.40s
Dec (J2000): -52d 19' 03.5"

with an uncertainty of 1.5 arcsec (radius, 90% confidence).

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

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


GRB_name: GRB200411A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27539
SUBJECT: GRB 200411A: Swift/UVOT Upper Limits
DATE:    20/04/11 09:55:39 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

N. P. M. Kuin (UCL-MSSL) and A. Tohuvavohu (U. Toronto)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200411A
58 s after the BAT trigger (Tohuvavohu et al., GCN Circ. 27536). No optical
afterglow consistent with the XRT position (Osborne et al., GCN Circ.
27538) 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            58          208          147         >20.8
u_FC               270          520          246         >20.4
white               58         1540          392         >21.2
v                  601         1417           97         >18.5
b                  525         1343           78         >20.3
u                  270         1490          343         >21.0
w1                 651         1466           97         >18.8
m2                 626          646           19         >18.1
w2                 576         1220           58         >19.2

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: GRB200411A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27540
SUBJECT: GRB 200411A: Swift-XRT refined Analysis
DATE:    20/04/11 10:43:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore
(U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) ,
M. Capalbi (INAF-IASFPA), J.A. Kennea (PSU), B. Sbarufatti (PSU) and A.
Tohuvavohu report on behalf of the Swift-XRT team:

We have analysed 6.6 ks of XRT data for GRB 200411A (Tohuvavohu et al.
GCN Circ. 27536), from 39 s to 13.0 ks after the  BAT trigger. The data
comprise 8 s in Windowed Timing (WT) mode (taken while Swift was
slewing), with the remainder in Photon Counting (PC) mode. The enhanced
XRT position for this burst was given by Osborne et al. (GCN Circ.
27538).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.16 (+0.11, -0.10).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.74 (+0.25, -0.24). The
best-fitting absorption column is  1.3 (+0.9, -0.7) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 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 3.9 x 10^-11 (4.7 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.3 (+0.9, -0.7) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: 2.6 sigma
Photon index:      1.74 (+0.25, -0.24)

If the light curve continues to decay with a power-law decay index of
1.16, the count rate at T+24 hours will be 4.9 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-14 (2.3 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00965784.

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


GRB_name: GRB200411A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27542
SUBJECT: Swift GRB 200411A: Global MASTER-Net observations report 
DATE:    20/04/11 17:56:28 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB 200411A ( A. Tohuvavohu et al., GCN 27536) errorbox  46681 sec after notice time and 46701 sec after trigger time at 2020-04-11 17:27:24 UT, with upper limit up to  18.9 mag. Observations started at twilight.  The observations began at zenith distance = 56 deg. The sun  altitude  is -14.6 deg. 

The galactic latitude b = -54 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=1334193

We obtain a following upper limits.  

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

   46792 |         MASTER-SAAO |   C |   180 | 18.9 |        
   46794 |         MASTER-SAAO |   C |   180 | 18.9 |        
   47360 |         MASTER-SAAO |   C |   180 | 17.8 |        
   47363 |         MASTER-SAAO |   C |   180 | 17.8 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200411A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27543
SUBJECT: GRB 200411A: Fermi GBM observation
DATE:    20/04/11 20:18:43 GMT
FROM:    Joshua Wood at MSFC/Fermi-GBM  <joshua.r.wood@nasa.gov>

E. Bissaldi (Politecnico and INFN Bari), C. Meegan (UAH), and J. Wood (NASA/MSFC)
report on behalf of the Fermi GBM Team:

"At 04:29:02.52 UT on 11 April 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200411A (trigger 608272147 / 200411187),
which was also detected by the Swift/BAT (Tohuvavohu et al. 2020, GCN 27536)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 116 degrees.

The GBM light curve shows a single pulse
with a duration (T90) of about 1.4 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.192 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.64 +/- 0.22 and
the cutoff energy, parameterized as Epeak, is 420 +/- 120 keV.

The event fluence (10-1000 keV) in this time interval is
(4.7 +/- 0.6)E-07 erg/cm^2. The 64-ms peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 11.9 +/- 1.5 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: GRB200411A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27545
SUBJECT: GRB 200411A: Swift-BAT refined analysis
DATE:    20/04/12 03:24:25 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

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

Using the data set from T-239 to T+880 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200411A (trigger #965784)
(Tohuvavohu et al., GCN Circ. 27536).  The BAT ground-calculated position is
RA, Dec = 47.686, -52.320 deg which is
   RA(J2000)  =  03h 10m 44.7s
   Dec(J2000) = -52d 19' 12.6"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a couple overlapping pulses
that starts at ~T-0.02 s and ends at ~T+0.25 s. The highest peak
occurs at ~ T+0.05 s. T90 (15-350 keV) is 0.22 +- 0.04 sec
(estimated error including systematics).

The time-averaged spectrum from T-0.02 to T+0.25 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
0.95 +- 0.19.  The fluence in the 15-150 keV band is 8.6 +- 1.1 x 10^-8
erg/cm2.
The 1-sec peak photon flux measured from T-0.38 sec in the 15-150 keV band
is 1.1 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Using the 4-ms binned light curve, the spectral lag of the short pulse
is 1 (+7, -4) ms for the 100-350 keV to 25-50 keV bands, and 8 (+6, -6) ms
for the 50-100 keV to 15-25 keV bands. These values are more consistent
with those of short GRBs.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/965784/BA/


GRB_name: GRB200412A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27546
SUBJECT: GRB 200412A: BALROG localization (Fermi Trigger 608367436 / GRB 200412290)
DATE:    20/04/12 07:23:34 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

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

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
608367436 at 06:57:11 on 12 April 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) = 134.2+/-0.8 deg
Decl.(2000.0) = -38.2+/-1.1 deg
We estimate an additional systematic error of 2 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200412290/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200412290/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200412290/json

                        


GRB_name: GRB200412B
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27547
SUBJECT: GRB 200412B: Fermi GBM Final Real-time Localization
DATE:    20/04/12 09:18:58 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 09:08:40 UT on 12 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200412B (trigger 608375325.70677 / 200412381).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 279.8, Dec = 64.1 (J2000 degrees, equivalent to J2000 18h 39m, 64d 05'), with a statistical uncertainty of 1.0 degrees.

The angle from the Fermi LAT boresight is 57.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200412381/quicklook/glg_skymap_all_bn200412381.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/bn200412381/quicklook/glg_healpix_all_bn200412381.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200412381/quicklook/glg_lc_medres34_bn200412381.gif


GRB_name: GRB200412B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27548
SUBJECT: GRB 200412B: BALROG localization (Fermi Trigger 608375325 / GRB 200412381)
DATE:    20/04/12 09:45:13 GMT
FROM:    Jochen Greiner at MPE,Garching  <jcg@mpe.mpg.de>

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

We note that the spectral fit from the automated pipeline appears off due to more high-energy emission than normal. We are re-running the pipeline manually to test this hypothesis. This position may be updated. 

The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
608375325 at 09:08:40 on 12 April 2020 were automatically fitted for spectrum
and sky location with the official 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) = 271.0+/-1.1 deg
Decl.(2000.0) = 64.4+/-0.3 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200412381/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200412381/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200412381/json

                        


GRB_name: GRB200412B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27549
SUBJECT: Fermi GRB 200412B: Global MASTER-Net observations report 
DATE:    20/04/12 12:00:09 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),

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-Amur robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 200412B ( Fermi GBM team, GCN 27547) errorbox  8581 sec after notice time and 8607 sec after trigger time at 2020-04-12 11:32:08 UT, with upper limit up to  18.1 mag. Observations started at twilight.  The observations began at zenith distance = 62 deg. The sun  altitude  is -11.6 deg. 

The galactic latitude b = 21 deg., longitude l = 93 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1334873

We obtain a following upper limits.  

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

    8638 | 2020-04-12 11:32:08 |         MASTER-Amur | (18h 42m 54.00s , +64d 01m 02.2s) |   C |    60 | 17.7 |        
    8717 | 2020-04-12 11:33:27 |         MASTER-Amur | (18h 36m 40.79s , +62d 00m 23.4s) |   C |    60 | 17.7 |        
    8876 | 2020-04-12 11:36:06 |         MASTER-Amur | (18h 51m 29.33s , +66d 00m 50.1s) |   C |    60 | 17.8 |        
    8955 | 2020-04-12 11:37:26 |         MASTER-Amur | (18h 42m 48.05s , +64d 01m 55.3s) |   C |    60 | 18.1 |        
    9036 | 2020-04-12 11:38:46 |         MASTER-Amur | (19h 01m 08.17s , +64d 00m 49.8s) |   C |    60 | 17.9 |        
    9115 | 2020-04-12 11:40:06 |         MASTER-Amur | (18h 36m 35.84s , +61d 59m 55.8s) |   C |    60 | 18.0 |        
    9195 | 2020-04-12 11:41:25 |         MASTER-Amur | (18h 53m 41.44s , +62d 00m 17.0s) |   C |    60 | 17.7 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200412A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27550
SUBJECT: GRB 200412A: Fermi GBM detection
DATE:    20/04/12 14:04:54 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

B. Mailyan (Institute for Basic Science, South Korea) and R. Hamburg (UAH)
report on behalf of the Fermi GBM Team:

"At 06:57:11.95 UT on 12 April 2020, the Fermi Gamma-Ray Burst Monitor
(GBM) triggered and located GRB 200412A (trigger 608367436 / 200412290).
This trigger was originally misclassified as a particle event by the flight
software.

The on-ground calculated location, using the Fermi GBM trigger data, is RA
= 140.01, Dec = -41.67 (J2000 degrees, equivalent to J2000 09h 20m, -41d
40â€™), with a statistical uncertainty of 1.4 degrees.

The angle from the Fermi LAT boresight is 108 degrees.

The GBM light curve shows multiple short peaks with a duration (T90) of
about 12.6 s (50-300 keV).

The time-averaged spectrum from T0 s to T0+14.0 s is best fit by a Band
function with Epeak = 255 +/- 8.5 keV, alpha = -0.64 +/- 0.03, and beta =
-2.66 +/- 0.14.

The event fluence (10-1000 keV) in this time interval is (3.1 +/- 0.04)E-05
erg/cm^2. The 1-sec peak photon flux measured starting from T0+3.2 s in the
10-1000 keV band is 34.3 +/- 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: GRB200412B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27551
SUBJECT: GRB 200412B: Tiled Swift observations
DATE:    20/04/12 14:37:38 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 200412B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00089

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(12apr20): The "C" on the GRN name in the Subject-line and in the first sentence
has been changed to the correct "B" designation.]


GRB_name: GRB200412B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27553
SUBJECT: Correction to GCN 27551 - Swift is observing GRB 200412*B* 
DATE:    20/04/12 15:26:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

Phil Evans & Kim Page (U. Leicester) report on behalf of the Swift team.

There was an error in GRB name given in GCN Circ 27551; Swift has in fact begun observations of GRB 200412B, rather than (as yet) non-existent GRB 200412C. We apologise for the confusion.


GRB_name: GRB200412B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27555
SUBJECT: GRB 200412B: MASTERt Optical Couterpart in Gagarin day! 
DATE:    20/04/12 15:28:52 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov (Lomonosov MSU) and  V. Yurkov, A. Gabovich, Yu. Sergienko( 
[BBlagoveschensk 
Educational State University)

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(Lomonosov Moscow State University, SAI, Physics Department),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix
Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State
University)


MASTER OT J111012.51+274912.8 discovery - new OT inside Fermi GRB 200325B
(trigger 606840801).

MASTER-Amur auto-detection system ( located near Russia Kosmodrom 
Vostochniy) discovered OT source at (RA, Dec) = 18h 33m 15.33s +62d 31m 
57.0s on 
2020-04-12.48156 UT in Fermi error box (GCN 27547, 27548) Lipunov et al., 
GCN  27549).

The OT unfiltered magnitude is 16.6m
(mlim18.0).

The OT is seen in 2 images. There is no minor planet at this place.

We have reference image on 2016-08-12.64123 UT with unfiltered mlim= 
19.3m.

Spectral observations are required.

The discovery and reference images are available at:

http://master.sai.msu.ru/static/OT/183315.33623157.0.png


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27556
SUBJECT: GRB 200412B: MASTER-Amur Optical Couterpart in Gagarin day! 
DATE:    20/04/12 15:47:07 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov (Lomonosov MSU) and  V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State University)
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(Lomonosov Moscow State University, SAI, Physics Department),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo 
Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix
Aguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State
University)


MASTER-Amur  ( located near  Russian Kosmodrom Vostochniy) comeback to 
MASTER OT J111012.51+274912.8  (Lipunov et al., GCN 27555) 
after 2 hours and we find optical transient with limit ~ 17.5 . So this 
is real afterglow:
at (RA, Dec) = 18h 33m 15.33s +62d 31m 57.0s on

The OT is seen in 2 images. There is no minor planet at this place.

We have reference image on 2016-08-12.64123 UT with unfiltered mlim= 19.3m.

Spectral observations are required.

The discovery and reference images are available at:

http://master.sai.msu.ru/static/OT/183315.33623157.0.png


GRB_name: GRB200412B
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27557
SUBJECT: GRB 200412B: Fermi-LAT detection
DATE:    20/04/12 15:53:48 GMT
FROM:    Francesco Longo at U of Trieste,INFN Trieste  <franzlongo1969@gmail.com>

F. Longo (University & INFN Trieste), D.Kocesvki (NASA/MSFC),
E.Bissaldi (Politecnico and INFN, Bari), M.Ohno (Hiroshima University)
and M.Palatiello (University of Udine & INFN, Trieste)
report on behalf of the Fermi-LAT Collaboration:

On April 12, 2020, Fermi-LAT detected high-energy emission from
GRB 200412B, which was also detected by Fermi-GBM
(trigger 608375325/200412381).

The best LAT on-ground location is found to be
RA, Dec = 277.48, 61.79 (degrees, J2000)
with an error radius of 0.5 deg (90% containment, statistical error only).
This was 59 deg from the LAT boresight at the time of the GBM trigger:
T0 = 09:08:40 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 (2.6 degrees from the GBM position) with high significance.
The photon flux above 100 MeV in the time interval 0-1000 s after the
GBM trigger is 6.0 +/- 1.6 e-5 ph/cm2/s.

The estimated photon index above 100 MeV is -2.9 +/- 0.4

The highest-energy photon is a 1.1 GeV event which is observed 134 seconds
after the GBM trigger.

A Swift ToO has been requested for this burst.

The Fermi-LAT point of contact for this burst is
Michele Palatiello (michele.palatiello@gmail.com)

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


GRB_name: GRB200412B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27558
SUBJECT: GRB 200412B: Fermi GBM detection
DATE:    20/04/12 17:23:16 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

B. Mailyan (Institute for Basic Science, South Korea) and R. Hamburg (UAH)
report on behalf of the Fermi GBM Team:

"At 09:08:40.71 UT on 12 April 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200412B (trigger 608375325 / 200412381),
which was also detected by the Fermi LAT (Longo et al. 2020, GCN 27557)
and observed to have a candidate optical afterglow by MASTER
(GCN 27555 & GCN 27556). The GBM on-ground location is consistent
with the LAT position.

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

The GBM light curve shows a multi-peaked structure
with a duration (T90) of about 6 s (50-300 keV).
The time-averaged spectrum from T0+3.1s to T0+21.5 s is
best fit by a Band function with Epeak = 257 +/- 4 keV,
alpha = -0.54 +/- 0.01, and beta = -2.24 +/- 0.02.

The event fluence (10-1000 keV) in this time interval is
(8.00 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+9.1 s in the 10-1000 keV band
is 127.5 +/- 0.7 ph/s/cm^2.

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

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: GRB200412A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27559
SUBJECT: Fermi GRB 200412A: Global MASTER-Net observations report 
DATE:    20/04/12 19:30:09 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),

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200412A ( B. Mailyan et al., GCN 27550) errorbox  36730 sec after notice time and 36757 sec after trigger time at 2020-04-12 17:09:48 UT, with upper limit up to  19.6 mag. Observations started at twilight.  The observations began at zenith distance = 18 deg. The sun  altitude  is -11.1 deg. 

The galactic latitude b =  1 deg., longitude l = 261 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1334799

We obtain a following upper limits.  

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

   36787 | 2020-04-12 17:09:48 |         MASTER-SAAO | (09h 13m 52.34s , -41d 51m 51.9s) |   C |    60 | 18.4 |        
   37119 | 2020-04-12 17:15:21 |         MASTER-SAAO | (09h 13m 54.79s , -41d 51m 51.5s) |   C |    60 | 18.8 |        
   38182 | 2020-04-12 17:33:03 |         MASTER-SAAO | (09h 10m 06.68s , -43d 53m 01.7s) |   C |    60 | 19.5 |        
   38513 | 2020-04-12 17:38:34 |         MASTER-SAAO | (09h 10m 03.48s , -43d 53m 49.3s) |   C |    60 | 19.5 |        
   38840 | 2020-04-12 17:44:01 |         MASTER-SAAO | (09h 06m 39.51s , -39d 52m 36.7s) |   C |    60 | 19.5 |        
   38843 | 2020-04-12 17:44:04 |         MASTER-SAAO | (08h 57m 23.15s , -39d 53m 40.6s) |   C |    60 | 19.6 |        
   38922 | 2020-04-12 17:45:24 |         MASTER-SAAO | (09h 02m 33.15s , -37d 54m 37.1s) |   C |    60 | 19.1 |        
   39169 | 2020-04-12 17:49:31 |         MASTER-SAAO | (09h 06m 35.97s , -39d 53m 37.7s) |   C |    60 | 19.5 |        
   39172 | 2020-04-12 17:49:34 |         MASTER-SAAO | (08h 57m 19.39s , -39d 54m 42.5s) |   C |    60 | 19.6 |        
   39252 | 2020-04-12 17:50:54 |         MASTER-SAAO | (09h 02m 39.08s , -37d 53m 08.5s) |   C |    60 | 19.1 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200412A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27560
SUBJECT: IPN triangulation of GRB 200412A
DATE:    20/04/12 21:20:47 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,

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 200412A
(BALROG localization: Kunzweiler et al., GCN Circ. 27546;
Fermi-GBM detection: Mailyan & Hamburg, GCN Circ. 27550)
was detected by Fermi (GBM trigger 608367436), Konus-Wind,
INTEGRAL (SPI-ACS), and Mars-Odyssey (HEND)
at about 25032 s UT (06:57:12).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
 ---------------------------------------------
  RA(2000), deg                 Dec(2000), deg
 ---------------------------------------------
 Center:
  137.164 (09h 08m 39s) -39.022 (-39d 01' 20")
 Corners:
  136.598 (09h 06m 24s) -38.953 (-38d 57' 12")
  136.795 (09h 07m 11s) -39.172 (-39d 10' 21")
  137.730 (09h 10m 55s) -39.086 (-39d 05' 11")
  137.530 (09h 10m 07s) -38.870 (-38d 52' 11")
 ---------------------------------------------
The error box area is 616 sq. arcmin, and its maximum
dimension is 53 arcmin (the minimum one is 14 arcmin).
The Sun distance was 115 deg.

This box may be improved.

The localization is consistent with, but reduces
the area of, the final Fermi-GBM (GCN Circ. 27546) and
BALROG (GCN Circ. 27550) localizations.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200412_T25034/IPN/

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


GRB_name: GRB200412B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27561
SUBJECT: GRB 200412B: Swift-XRT afterglow detection
DATE:    20/04/12 23:35:46 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), E. Ambrosi 
(INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (ASDC), A.
Tohuvavohu (U. Toronto), 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
Fermi/LAT-detected burst GRB 200412B (Longo et al. GCN Circ. 27557) in
a series of observations tiled on the sky. The total exposure time is
4.9 ks, distributed over 7 tiles; the maximum exposure at a single sky
location was 1.5 ks. The data were collected between T0+20.1 ks and
T0+31.7 ks, and are entirely in Photon Counting (PC) mode. 

Two uncatalogued X-ray sources are detected, of which one ("Source 2")
is above the RASS limit, and is therefore likely the GRB afterglow.
Using 671 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 = 278.31339, +62.53253 which is
equivalent to:

RA (J2000): 18h 33m 15.21s
Dec(J2000): +62d 31' 57.1"

with an uncertainty of 2.5 arcsec (radius, 90% confidence). This
position is 30.1 arcmin from the Fermi/LAT position. 

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.9 (+1.3, -1.2).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+0.6, -0.5). The
best-fitting absorption column is  1.6 (+1.8, -1.0) x 10^21 cm^-2,
consistent with the Galactic value of 5.1 x 10^20 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 3.1 x 10^-11 (3.8 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+1.8, -1.0) x 10^21 cm^-2
Galactic foreground: 5.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.8 (+0.6, -0.5)

If the light curve continues to decay with a power-law decay index of
1.9, the count rate at T+24 hours will be 0.015 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.7 x
10^-13 (5.8 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis of the likely afterglow
are at https://www.swift.ac.uk/xrt_products/TILED_GRB00089/Source2.php.
The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00089.

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


GRB_name: GRB200412B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27563
SUBJECT: GRB 200412B : AstroSat CZTI detection
DATE:    20/04/13 08:06:48 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 (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:

Analysis of AstroSat CZTI data showed the detection of a long GRB 200412B, which was also detected by Fermi GBM Final Real-time (GCN #27547), BALROG (Burgess J. et al., GCN #27548), Global MASTER-Net (Lipunov V. et al, GCN #27549), Tiled Swift (Evans P. et al., GCN #27551), Fermi-LAT (Longo F. et al., GCN #27557), Fermi GBM (Mailyan B. et al., GCN #27558) and Swift-XRT (Page K. et al., GCN #27561). 

The source was clearly detected in the 40-200 keV energy range. The light curve shows a single peak of emission peaking at 2020-04-12 09:08:49.5 UT. The measured peak count rate associated with the burst is 1160 +/- 40.72 cts/s above the background in the combined data of four quadrants, with a total of 3452 +/- 16.55 cts. The local mean background count rate was 519 +/- 0.87 cts/s. Using cumulative rates, we measure a T90 of 7.17 +/- 0.06 s.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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


GRB_name: GRB200412B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27564
SUBJECT: GRB 200412B: Optical afterglow detection with 1.3m DFOT
DATE:    20/04/13 09:14:18 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

TITLE:   GCN CIRCULAR
NUMBER:  27563
SUBJECT: GRB 200412B: Optical afterglow detection with 1.3m DFOT
DATE:    20/04/13 09:05:41 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com,
amit@aries.res.in>

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

We observed the optical afterglow of the Fermi GBM detected GRB 200412B
(GCN 27547, Lipunov et al., GCN 27555, GCN 27561)
with the 1.3m Devsthal Fast Optical Telescope (DFOT) at Aryabhatta Research
Institute of Observational Sciences (ARIES), Nainital
(India),
from 2020-04-12 UT 22:03:14 to 2020-04-12 UT 23:29:44 (corresponding to
12.90 to 14.46 hours from the GRB trigger time). We observed a series of
9x300s exposures in Bessel R filter and a series of 7x360s exposures in
Bessel I filter. We stacked the images and detected the optical afterglow
of GRB 200412B in both Bessel R and I filters which is consistent with
optical detections by Lipunov et al., GCN 27555, 27556.

The observed magnitudes are as follows:

T_start-T0 (hours)   Start Date (UTC)             End Date
(UTC)                  Filter            Magnitudes
---------------------------------------------------------------------------------------------------------------
12.90               2020-04-12 UT 22:03:14          2020-04-12 UT
22:46:11          R               18.90 +- 0.03
13.72               2020-04-12 UT 22:52:02          2020-04-12 UT
23:29:44          I               17.54 +- 0.02


Photometry is done based on the USNO-B1.0 catalog. The quoted magnitudes
are not corrected for Galactic extinction.


GRB_name: GRB200412B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27565
SUBJECT: GRB 200412B: Insight-HXMT/HE detection
DATE:    20/04/13 09:40:36 GMT
FROM:    YaoGuang Zheng at IHEP  <zhengyg@ihep.ac.cn>

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

At 2020-04-12T09:08:45.80 (T0), Insight-HXMT/HE detected 
GRB 200412B (trigger ID: HEB200412381) in a routine search of the data, 
which also triggered Fermi/GBM (GCN #27547).

The Insight-HXMT/HE light curve mainly consists of a single  
pulse with a duration (T90) of 5.50 s measured from T0+0.05 s. 
The 1-ms peak rate, measured from T0+4.28 s, is 14908 cnts/sec. 
The total counts from this burst is 25230 counts. 
URL_LC: http://twiki.ihep.ac.cn/pub/HXMT/GRBList/HEB200412381_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: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27566
SUBJECT: GRB 200412B: AbAO optical observations
DATE:    20/04/13 10:09:07 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of Fermi GRB 200412B (Fermi GBM team  GCN 27547; 
Longo et al., GCN 27557) with AS-32 (0.7m) telescope of Abastumani 
Observatory starting on 2020-04-12 (UT) 18:42:21.  We  detected  the 
afterglow of GRB 200412B  (Lipunov et al., GCNs 27555; Kumar et al., GCN 
27564).  Preliminary photometry of the afterglow is following.

Date       UT start  t-T0    Filter Exp.  OT    Err. UL
                     (mid, days)     (s)
2020-04-12 18:42:21  0.41783 R      56*60 18.31 0.02 21.3

The photometry is based on nearby USNO-B1.0 stars
UUSNO-B1.0_id R2
1525-0302108 17.21
1524-0300914 17.20
1525-0301929 17.85

[GCN OPS NOTE(13apr20): Removed the extra "GRB" in the SUBJECT-line.]


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27567
SUBJECT: GRB 200412B: Tautenburg observations 
DATE:    20/04/13 12:26:07 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

B. Stecklum, S. Klose, S. Melnikov, and A. Nicuesa Guelbenzu (all 
Tautenburg) report:

We observed the field of GRB 200412B (Fermi GBM team, GCN 27547; Mailyan 
et al., GCN 27558; see also Burgess et al., GCN 27548; Longo et al., GCN 
27557; Page et al., GCN 27561; Gupta et al., GCN 27563; Zheng et al., GCN 
27565) with the Tautenburg 1.34m Schmidt telescope equipped with the 
TAUKAM 6k x 6k CCD camera and the wide V-band filter (VB). The 
transmission curve of this filter closely follows the Gaia GBP filter.

The fading optical transient detected by MASTER Global Robotic Net 
(Lipunov et al., GCN 27555, 27556) is clearly detected on our images (for 
other optical observations see also Kumar et al., GCN 27564; Belkin et 
al., GCN 27566). Using Gaia DR2 stars in the field, we measure the 
following preliminary magnitudes (Vega system):

Mean time: April 12, 21:29:48 UT, VB = 18.43 +/- 0.01
Mean time: April 13, 02:22:38 UT, VB = 19.00 +/- 0.01


GRB_name: GRB200405B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27568
SUBJECT: GRB 200405B: Further Swift-XRT observations
DATE:    20/04/13 13:47:26 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

Swift-XRT has performed a second follow-up observation of the
INTEGRAL/SPI-ACS and Swift-BAT GUANO detected possible short burst GRB
200405B (James DeLaunay et al. GCN Circ. 27497), collecting ~1.2 ks of
Photon Counting (PC) mode data between T0+550.8 ks and T0+584.0 ks. Of the
four uncatalogued X-ray sources reported in GCN 27500 (Sbarufatti et al.),
none shows any evidence of fading. We therefore conclude that Swift did
not detect the X-ray afterglow of this GRB.

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


GRB_name: GRB200412B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27570
SUBJECT: GRB 200412B: SAO RAS observations of OT
DATE:    20/04/14 01:54:38 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. Moskvitin on behalf of the larger GRB follow-up team report.

We observed the field of the GRB 200412B (The Fermi GBM team,
GCN 27547; Longo et al. GCN 27557) with the 1-m telescope
of SAO RAS, equipped with the Multi-Mode Photometer-Polarimeter.
We obtained 6 x 300 sec. images in Rc band on 2020.04.14
00:09:20--00:41:40 UT, T_mid - T0 = 1.6367 days.

The OT (Lipunov et al., GCNs 27555, 27556; Kumar et al., GCN
27564; Belkin et al., GCN 27566) is clearly visible in individual
images and stacked frame with the brightness of R = 20.8 +/- 0.1.
The photometry is based on R2 magnitudes of nearby USNO-B1 stars.


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27571
SUBJECT: GRB 200412B:  Xinglong TNT  optical observations
DATE:    20/04/14 04:22:19 GMT
FROM:    Liping Xin at NAOC, SVOM  <xlp@nao.cas.cn>

L. P. Xin, X. F. Wang,  J. Zheng, Y. L. Qiu, J. Y. Wei,  J. Wang,  
L. H. Li ,  C. Wu,  X. H. Han and J. S. Deng, report:

We began to observe GRB 200412B (The Fermi GBM team,
GCN 27547; Longo et al. GCN 27557)  
with Xinglong TNT telescope at 18:09:54 (UT), 13th. Apr. 2020,  
about 33 hours after  the burst. 

10  x 300 sec R band images were obtained. 

The optical afterglow  (Lipunov et al., GCNs 27555, 27556; Kumar et al., GCN
27564; Belkin et al., GCN 27566, Stecklum et al., GCN 27567, 
Moskvitin GCN 27570) is clearly detected in individual
images with the brightness of R = 20.0 +/- 0.1.
The photometry is based on R2 magnitudes of nearby USNO-B1 stars.

With the reports from  (Kumar et al., GCN
27564; Belkin et al., GCN 27566, Stecklum et al., GCN 27567, 
Moskvitin GCN 27570), the brightness is fading with a slope of  -1.5 
for a single power law (t~t^a) from 10 hours to 39 hours after the burst trigger.


GRB_name: GRB200412B
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27572
SUBJECT: GRB 200412B: CALET Gamma-Ray Burst Monitor detection
DATE:    20/04/14 08:20:52 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

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

The bright GRB 200412B (BALROG localization: Burgess et al.,
GCN Circ. 27548; Fermi-LAT detection: Longo et al., GCN Circ. 27557;
Fermi GBM detection: Mailyan and Hamburg, GCN Circ. 27558;
https://gcn.gsfc.nasa.gov/other/200412B.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 09:08:43.975 UTC
on 12 April 2020. The burst signal was seen by all CGBM detectors.

The burst light curve shows a multi-peaked structure which starts
at T-0.3 sec, peaks at T+6.2 sec and ends at T+13.1 sec. The T90 and T50
durations measured by the SGM data are 6.1 +- 0.5 sec and 1.8 +- 0.1 sec
(40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1270717362/

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


GRB_name: GRB200411A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27573
SUBJECT: GRB 200411A: ATCA 5/9 GHz radio observations
DATE:    20/04/14 09:58:55 GMT
FROM:    Gemma Anderson at Curtin U  <gemma.anderson@curtin.edu.au>

G. E. Anderson (Curtin), M. E. Bell (UTS), J. Stevens (CASS), P. J. Hancock
(Curtin), J. C. A. Miller-Jones (Curtin), M. D. Aksulu (UvA), A. Bahramian
(Curtin), K. W. Bannister (CASS), A. J. van der Horst (GWU), S. D. Ryder
(Macquarie), J-P. Macquart (Curtin), R. M. Plotkin (UNR), A. Rowlinson
(UvA), R. A. M. J. Wijers (UvA)

We used the Australia Telescope Compact Array (ATCA) to perform a radio
observation of the short GRB 200411A. The rapidly scheduled observations
began on 2020 Apr 11.25 UT for 5 hours (1.5 hrs post-burst; Fermi GBM Team
GCN 27535, A. Tohuvavohu et al., GCN 27536). No radio source was detected
at the enhanced Swift-XRT position (J.P. Osborne et al., GCN 27538), with
preliminary 3 sigma upper-limits of 45 microJy and 36 microJy at 5.5 and 9 GHz,
respectively. Further observations are planned.

We thank the ATCA and CSIRO Astronomy and Space Science (CASS) staff for
scheduling these observations.


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27574
SUBJECT: GRB 200412B: contunued AbAO optical observations
DATE:    20/04/14 10:19:21 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 200412B (Fermi GBM team, GCN 27547; Mailyan
et al., GCN 27558; see also Burgess et al., GCN 27548; Longo et al., GCN
27557; Page et al., GCN 27561; Gupta et al., GCN 27563; Zheng et al., 
GCN 27565)  with AS-32 (0.7m) telescope of Abastumani Observatory 
starting on 2020-04-14 (UT) 00:16:57.  We  clearly detected  the 
afterglow of GRB 200412B  (Lipunov et al., GCNs 27555, 27556; Kumar et 
al., GCN 27564; Belkin et al., GCN 27566, Stecklum et al., GCN 27567,
Moskvitin GCN 27570; Xin  et al., GCN 27571).  Preliminary photometry of 
the afterglow is following.

Date       UT start  t-T0    Filter Exp.  OT    Err. UL
                     (mid, days)     (s)
2020-04-14 00:16:57  1.65401 R      67*60 20.7 0.1   22.1

The photometry is based on nearby USNO-B1.0 stars
UUSNO-B1.0_id R2
1525-0302108 17.21
1524-0300914 17.20
1525-0301929 17.85

The index of power law decay of the afterglow light curve between the 
two epochs of our observations (Belkin et al., GCN 27566 at 0.41793 
days) and reported in this circular (at 1.65401 days) is -1.58+/-0.07 
which is corroborate with the index reported by Xin  et al. (GCN 27571).


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27575
SUBJECT: GRB 200412B: Tautenburg observations 
DATE:    20/04/14 10:45:57 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose, B. Stecklum, S. Melnikov, and A. Nicuesa Guelbenzu (all 
Tautenburg) report:

We continued observing the field of GRB 200412B (Fermi GBM team, GCN 
27547) with the Tautenburg 1.34m Schmidt telescope equipped with the 
TAUKAM 6k x 6k CCD camera and the wide V-band filter (VB; Stecklum et al., 
GCN 27567).

For the optical transient (Lipunov et al., GCN 27555, 27556) at a mean 
time APR 13, 21:08:59 UT (1.500 days post burst) we measure VB = 20.27 +/- 
0.03. Compared to our 1st-epoch observations (dt=0.51 days; Stecklum et 
al., GCN 27567) this provides a decay slope of alpha = 1.58 (F\nu \propto 
t**(-\alpha)), in agreement with the results reported by Xin et al. (GCN 
27571) and Belkin et al. (GCN 27574).


GRB_name: GRB200412B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27576
SUBJECT: GRB 200412B: MITSuME Akeno optical observation
DATE:    20/04/14 11:52:40 GMT
FROM:    Ogawa Futa at Tokyo Institute of Technology  <ogawa@hp.phys.titech.ac.jp>

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

We searched for the optical counterpart of GRB 200412B (The Fermi GBM
team, GCN Circular #27547) with the optical three color (g', Rc, and
Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno
Observatory, Yamanashi, Japan.
The observation started on 2020-04-13 15:27:09 UT. We detected the
point source at the position consistent with the afterglow detected
previously (E. Gorbovskoy et al. GCN #27555).
We measured the magnitudes as follows.
T0+[hour] MID-UT T-EXP[sec] measured magnitudes
------------------------------------------------------------------------------------------------
30.2 2020-04-13 17:19:02 10800 g'=20.1+/-0.2,Rc=19.6+/-0.2,Ic=19.5+/-0.2
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.
The magnitudes are expressed in the Vega system.


GRB_name: GRB200412A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27577
SUBJECT: Konus-Wind observation of GRB 200412A
DATE:    20/04/14 15:38:35 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 200412A
(BALROG localization: Kunzweiler et al., GCN Circ. 27546;
Fermi-GBM detection: Mailyan and Hamburg., GCN Circ. 27550;
IPN triangulation: Hurley et al., GCN Circ. 27560)
triggered Konus-Wind at T0=25034.8 s UT (06:57:14.800).

The burst light curve shows a multipeaked structure
which starts at ~T0-0.2 s and has a total duration of ~13.3 s.
The emission is seen up to ~4 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.27(-0.32,+0.35)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.792 s,
of 1.18(-0.15,+0.15)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+13.056 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 = -0.59(-0.11,+0.12),
the high energy photon index beta = -2.68(-0.41,+0.23),
the peak energy Ep = 229(-19,+20) keV
(chi2 = 56/68 dof).

The spectrum near the maximum count rate
(measured from T0+0.256 to T0+4.864 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.69(-0.08,+0.09)
and Ep = 275(-16,+18) keV (chi2 = 47/68 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.8
(chi2 = 46/67 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200412_T25034/

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


GRB_name: GRB200410A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27578
SUBJECT: GRB 200410A: Swift-BAT refined analysis
DATE:    20/04/15 03:19:33 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. Laha (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
K. K. Simpson (PSU), 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 200410A (trigger #965638)
(Simpson et al., GCN Circ. 27518).  The BAT ground-calculated position is
RA, Dec = 299.644, 51.745 deg which is
   RA(J2000)  =  19h 58m 34.6s
   Dec(J2000) = +51d 44' 40.9"
with an uncertainty of 2.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 53%.

The mask-weighted light curve shows several weak pulses. The two main
pulses occur at ~T-20 s and ~T+2 s, respectively, followed by some weak
emission that lasts till ~T+50 s. T90 (15-350 keV) is 108.8 +- 40.7 sec
(estimated error including systematics).

The time-averaged spectrum from T-90.88 to T+50.62 sec is best fit by a
simple
power-law model.  The power law index of the time-averaged spectrum is
1.41 +- 0.31.  The fluence in the 15-150 keV band is 1.2 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+1.43 sec in the 15-150 keV band
is 1.8 +- 0.3 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/965638/BA/


GRB_name: GRB200415A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27579
SUBJECT: GRB 200415A: Fermi GBM Final Real-time Localization
DATE:    20/04/15 08:58:27 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 08:48:05 UT on 15 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200415A (trigger 608633290.563746 / 200415367).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 6.1, Dec = -32.0 (J2000 degrees, equivalent to J2000 00h 24m, -32d 00'), with a statistical uncertainty of 2.0 degrees.

The angle from the Fermi LAT boresight is 43.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200415367/quicklook/glg_skymap_all_bn200415367.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/bn200415367/quicklook/glg_healpix_all_bn200415367.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200415367/quicklook/glg_lc_medres34_bn200415367.gif


GRB_name: GRB200415A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27580
SUBJECT: GRB 200415A: BALROG localization (Fermi Trigger 608633290 / GRB 200415367)
DATE:    20/04/15 09:11:15 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
608633290 at 08:48:05 on 15 April 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) = 10.8+/-6.4 deg
Decl.(2000.0) = -26.3+/-4.7 deg
We estimate an additional systematic error of 1 deg.

Further details are available at:
https://grb.mpe.mpg.de/grb/GRB200415367/

The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB200415367/healpix

The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB200415367/json

                        


GRB_name: GRB200412B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27581
SUBJECT: Konus-Wind observation of GRB 200412B
DATE:    20/04/15 09:16:05 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 200412B
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27547;
Mailyan and Hamburg, GCN Circ. 27558;
BALROG localization: Burgess et al., GCN Circ. 27548;
Fermi-LAT detection: Longo et al., GCN Circ. 27557;
AstoSat CZTI detection: Gupta et al., GCN Circ. 27563;
Insight-HXMT/HE detection: Zheng et al., GCN Circ. 27565;
CALET-GRBM detection: Tamura et al., GCN Circ. 27572)
triggered Konus-Wind at T0=32924.203 s UT (09:08:44.203).

The burst light curve shows a multipeaked structure
which starts at ~T0-0.5 s and has a total duration of ~30.5 s.
The emission is seen up to ~6 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.12(-0.05,+0.05)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+5.744 s,
of 5.12(-0.43,+0.44)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+15.360 s)
is best fit in the 20 keV - 6 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.67(-0.05,+0.05),
the high energy photon index beta = -2.45(-0.12,+0.10),
the peak energy Ep = 289(-16,+16) keV
(chi2 = 66/79 dof).

The spectrum near the maximum count rate
(measured from T0+5.376 to T0+5.888 s)
is best fit in the 20 keV - 6 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.15(-0.10,+0.11),
the high energy photon index beta = -2.58(-0.17,+0.14),
the peak energy Ep = 316(-24,+24) keV
(chi2 = 56/56 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200412_T32924/

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


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27582
SUBJECT: GRB 200412B: continued Tautenburg observations 
DATE:    20/04/15 09:30:32 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

B. Stecklum, S. Klose, S. Melnikov, and A. Nicuesa Guelbenzu (all 
Tautenburg) report:

We continued observing the field of GRB 200412B (Fermi GBM team, GCN 
27547) with the Tautenburg 1.34m Schmidt telescope equipped with the 
TAUKAM 6k x 6k CCD camera and the wide V-band filter (VB; Stecklum et al., 
GCN 27567; Klose et al., GCN 27575).

For the optical transient (Lipunov et al., GCN 27555, 27556) at a mean 
time of 2.521 days post burst we measure VB = 21.38 +/- 0.06. This is 
about 0.2 mag fainter than expected for a decay slope of alpha = 1.582 +/- 
0.004 based on our previous VB-band data (see also Xin et al., GCN 27571; 
Belkin et al., GCN 27574), suggesting that the light curve decay is 
steepening. Additional data are required to confirm (or reject) this 
conclusion.

We note that in our images there is still no evidence for an underlying 
host galaxy.


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27583
SUBJECT: GRB 200412B: Mondy optical observations
DATE:    20/04/15 10:11:58 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

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

We observed the field of GRB 200412B (Fermi GBM team, GCN 27547; Mailyan
et al., GCN 27558; see also Burgess et al., GCN 27548; Longo et al., GCN
27557; Page et al., GCN 27561; Gupta et al., GCN 27563; Zheng et al., 
GCN 27565) with AZT-33IK 1.5-m telescope of Sayan observatory (Mondy) 
starting on 2020-04-14 (UT) 14:24:54.

We  clearly detected  the afterglow of GRB 200412B  (Lipunov et al., 
GCNs 27555, 27556; see also Kumar et al., GCN 27564; Belkin et al., GCN 
27566, Stecklum et al., GCN 27567, Moskvitin GCN 27570; Xin  et al., GCN 
27571).  Preliminary photometry of the afterglow is following.

Date       UT start  t-T0    Filter Exp.   OT    Err. UL
                     (mid, days)     (s)
2020-04-14 14:24:54  2.23002 R      15*120 21.22 0.08 22.8

The photometry is based on nearby USNO-B1.0 stars
UUSNO-B1.0_id R2
1525-0302108 17.21
1524-0300914 17.20
1525-0301929 17.85


GRB_name: GRB200410A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27584
SUBJECT: GRB 200410A: CALET Gamma-Ray Burst Monitor detection
DATE:    20/04/15 12:20:30 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, S. Torii (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 Swift GRB 200410A (Simpson et al., GCN Circ. 27518, Laha et al.,
GCN Circ. 27578; https://gcn.gsfc.nasa.gov/other/200410A.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 02:25:15.105 UTC
on 10 April 2020. The burst signal was seen by the SGM detector.
No real-time CGBM GCN notice was distributed about this trigger because
the real-time communication from the ISS was off (loss of signal).

The burst light curve shows a weak pulse which starts at T-3.9 sec, peaks
at T-1.0 sec and ends at T+2.4 sec. The T90 and T50 durations measured by
the SGM data are 5.5 +- 2.2 sec and 2 +- 2 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1270520355/

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


GRB_name: GRB200415A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27585
SUBJECT: IPN triangulation of GRB 200415A (possible Magnetar Giant Flare in Sculptor Galaxy?)
DATE:    20/04/15 16:51:17 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, K. Hurley, and  D. Frederiks, 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. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team, and

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

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

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

The short-duration, extremely bright GRB 200415A
(Fermi-GBM detection: The Fermi GBM Team, GCN Circ. 27579;
BALROG localization : Kunzweiler, et al., GCN Circ. 27580)
has been detected by Fermi (GBM trigger 608633290), Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and Swift (BAT),
so far, at about 31686 s UT (08:48:06).
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:
    11.960 (00h 47m 50s) -25.937 (-25d 56' 13")
  Corners:
    11.481 (00h 45m 55s) -23.109 (-23d 06' 33")
    11.740 (00h 46m 58s) -22.955 (-22d 57' 17")
    12.354 (00h 49m 25s) -28.885 (-28d 53' 07")
    12.073 (00h 48m 18s) -29.074 (-29d 04' 25")
  ---------------------------------------------
The error box area is 1.53 sq. deg, and its maximum
dimension is 6.126 deg (the minimum one is 15.4 arcmin).
The Sun distance was about 35 deg.

The IPN localization is consistent with, but reduces the area of,
the Fermi-GBM final position (GCN Circ. 27579) and
BALROG localization (GCN 27580).

The Fermi (GBM) light curve shows an extremely bright short pulse
with a duration of ~10 ms, followed, after a ~1 ms gap, by a decaying 
emission lasting for ~150 ms. The light curve shape is very similar to
the extragalactic soft gamma-repeater giant flare candidates:
GRB 051103 - Frederiks et al., AstL 33, 1, 19, 2007 (fig. 1 and 2) and
GRB 070201 - Mazets at al., ApJ 680, 1, 545, 2008 (fig. 1 and 2).
The IPN box contains a nearby Sculptor Galaxy (3.5 Mpc),
supporting the hypothesis of the magnetar Giant Flare nature
of the burst.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200415_T31685/IPN/

Further localization improvements along with the burst time history and 
spectrum will be given in forthcoming GCN Circulars.

[GCN OPS NOTE(15apr20):  Per request of the author, the journal
in the Frederiks et al reference was changed from "ApJL" to "AstL".]


GRB_name: GRB200415A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27586
SUBJECT: GRB 200415A: Fermi-LAT detection 
DATE:    20/04/15 19:29:32 GMT
FROM:    Nicola Omodei at Stanford U.  <nicola.omodei@slac.stanford.edu>

N. Omodei (Stanford University), M. Axelsson (KTH & Stockholm Univ.), F. Piron (CNRS/IN2P3/LUPM), F. Longo (University and INFN, Trieste), D. Kocevski (NASA/MSFC), E. Bissaldi (Politecnico & INFN Bari) and A. Berretta (University & INFN Perugia) 
report on behalf of the Fermi-LAT Collaboration:

On April 15, 2020, Fermi-LAT detected high-energy emission from GRB 200415A, which was also detected by Fermi-GBM (trigger 608633290/200415367).

The GRB is marginally detected at high energy (>100 MeV) by Fermi-LAT at a location of: 
RA, Dec = 11.0, -25.1 (degrees, J2000) with an error radius of 0.5 deg (90% containment, statistical error only).

This was 49 deg from the LAT boresight at the time of the GBM trigger,  T0 = 08:48:05.56 UT, and 8.1 deg from the GBM final ground position (The Fermi GBM team, GCN27579). The location is also consistent within errors with the location from the IPN (Svinkin et al., GCN27585).

The photon flux above 100 MeV in the time interval 0-500 seconds after the GBM trigger is 3.4e-06 +/- 2.1e-06 ph/cm^2/s. The estimated photon index above 100 MeV is -1.7 +/ - 0.3. The highest-energy photon is a 1.7 GeV event, which is observed 284 seconds after the GBM trigger. 

The Fermi-LAT point of contact for this burst is:
Alessandra Berretta (alessandra.berretta@pg.infn.it).

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


GRB_name: GRB200415A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27587
SUBJECT: GRB 200415A: Fermi GBM observation
DATE:    20/04/15 19:54:14 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico and INFN Bari), M. Briggs (UAH),
E. Burns (GSFC), O.J. Roberts (USRA) and P. Veres (UAH)
report on behalf of the Fermi GBM Team:


"At 08:48:05.56 UT on 15 April 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200415A (trigger 608633290 / 200415367),
which was also detected by Fermi-LAT (Omodei et al., GCN 27586).
The Fermi GBM Final Real-time Localization (GCN 27579)
is consistent with the LAT position.

The angle from the Fermi LAT boresight
at the GBM trigger time is 49 degrees.

The GBM light curve shows a bright single pulse
with a duration (T90) of about 0.2 s (50-300 keV).
The time-averaged spectrum from T0-0.032 s to T0+0.160 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is 0.07 +/- 0.05 and
the cutoff energy, parameterized as Epeak, is 950 +/- 40 keV.

The event fluence (10-1000 keV) in this time interval
is (5.2 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux
measured starting from T0 in the 10-1000 keV band
is 74 +/- 2 ph/s/cm^2.

While we report the source to be a possible short GRB,
we cannot conclusively rule out a giant magnetar flare
of extragalactic origin, as reported by IPN (GCN 27585).
Periodicity is not evident in the GBM data.
Assuming a distance of 3.5 Mpc and the spectral shape reported above,
the isotropic equivalent energy in the 1 keV-10 MeV range is
(1.22 +/- 0.03)E+46 erg. Further analysis is ongoing.


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: GRB200412A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27588
SUBJECT: GRB 200412A : AstroSat CZTI detection
DATE:    20/04/15 20:59:14 GMT
FROM:    Soumya Gupta at IUCAA/ASTROSAT  <soumya@iucaa>

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

Analysis of AstroSat CZTI data showed the detection of a long GRB 200412A, which was also detected by BALROG (Kunzweiler F. et al., GCN #27546) , Fermi GBM (Mailyan B. et al., GCN #27550), Global MASTER-Net (Lipunov V. et al., GCN #27559), IPN (Hurley K. et al., GCN #27560) and Konus-Wind (Ridnaia A. et al., GCN #27577).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 2020-04-12 06:57:14.500 UT. The measured peak count rate associated with the burst is 2671 +/- 57 cts/s above the background in the combined data of four quadrants, with a total of 12092 +/- 16 cts. The local mean background count rate was 487 +/- 0.8 cts/s. Using cumulative rates, we measure a T90 of 12.5 +/- 0.002 s. In preliminary analysis, we find that 959 Compton events are associated with this event.

It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.

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: GRB200411A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27589
SUBJECT: GRB 200411A: Chandra observations indicative of temporal steepening
DATE:    20/04/15 21:20:48 GMT
FROM:    Wen-fai Fong at Northwestern U  <wfong@northwestern.edu>

A. Rouco Escorial, W. Fong (Northwestern), and E. Berger (Harvard) report:

â€œWe initiated observations with the Chandra X-ray Observatory of the position of the short-duration GRB 200411A (Fermi-GBM et al., GCN 27535; Tohuvavohu et al., GCN 27536; Bissaldi et al., GCN 27543) starting on 2020 April 15 00:16:54 UT, or at a mid-time of 3.95 days after the GRB trigger. ACIS-S observations were taken under Proposal 21500089 (ObsID 22427; PI: Berger), with a total exposure time of 19.8 ksec.
 
We do not detect an X-ray source within or around the enhanced Swift-XRT position (90% confidence; Osborne et al., GCN 27538). Centered on the XRT position, we calculate a 3-sigma limit of <4.5e-4 cts/s in the 0.5-8 keV energy range following the method described by Gehrels (1986) for small numbers of events. Applying the best-fit PC mode XRT spectral parameters (Gamma=1.7, intrinsic NH=1.5e21 cm^-2) and fixing the Galactic NH=1.55e20 cm^-2 (Willingale et al. 2013), we calculate a 3-sigma unabsorbed flux limit of FX<8.4e-15 erg/s/cm^2 in the 0.3-10 keV energy range. 
 
The XRT afterglow starting from 200 sec post-burst exhibits a power-law decline with decay index alpha=-0.84 (+/- 0.2) (where FX~t^alpha), while the Chandra upper limit indicates a potential steepening to alpha<-1.3. If this steepening is interpreted as a jet break at ~0.5-2 days post-burst, using median values for the explosion properties and redshift based on properties of short GRBs gives an opening angle of ~4-7 degrees.
 
We thank the Chandra staff for the rapid planning and scheduling of these observations.â€


GRB_name: GRB200415A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27590
SUBJECT: Fermi GRB 200415A: Global MASTER-Net observations report 
DATE:    20/04/16 04:15:14 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

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

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

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

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

D. Buckley 
(South African Astronomical Observatory),

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

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

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




MASTER-SAAO robotic telescope  (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)  located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 200415A ( Fermi GBM team, GCN 27579) errorbox  59974 sec after notice time and 60005 sec after trigger time at 2020-04-16 01:28:11 UT, with upper limit up to  18.9 mag. The observations began at zenith distance = 74 deg. The sun  altitude  is -45.2 deg. 

The galactic latitude b = -57 deg., longitude l = 304 deg.


Real time updated cover map and OT discovered available here: 
https://master.sai.msu.ru/site/master2/observ.php?id=1337394

We obtain a following upper limits.  

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

   60036 | 2020-04-16 01:28:11 |         MASTER-SAAO | (00h 26m 38.28s , -62d 06m 18.6s) |   C |    60 | 18.4 |        
   60040 | 2020-04-16 01:28:15 |         MASTER-SAAO | (00h 41m 32.15s , -62d 05m 14.4s) |   C |    60 | 18.0 |        
   62934 | 2020-04-16 02:16:29 |         MASTER-SAAO | (00h 26m 30.17s , -62d 06m 01.0s) |   C |    60 | 18.9 |        
   62938 | 2020-04-16 02:16:33 |         MASTER-SAAO | (00h 41m 27.25s , -62d 04m 57.1s) |   C |    60 | 18.7 |        
   63014 | 2020-04-16 02:17:49 |         MASTER-SAAO | (00h 24m 54.86s , -60d 05m 54.9s) |   C |    60 | 18.9 |        
   63018 | 2020-04-16 02:17:53 |         MASTER-SAAO | (00h 38m 56.88s , -60d 04m 50.7s) |   C |    60 | 18.8 |        
   63097 | 2020-04-16 02:19:12 |         MASTER-SAAO | (00h 36m 38.06s , -58d 03m 33.9s) |   C |    60 | 18.6 |        
   63173 | 2020-04-16 02:20:28 |         MASTER-SAAO | (00h 53m 41.50s , -58d 06m 07.0s) |   C |    60 | 18.6 |        
   63946 | 2020-04-16 02:33:21 |         MASTER-SAAO | (00h 24m 52.11s , -60d 06m 10.1s) |   C |    60 | 18.6 |        
   63950 | 2020-04-16 02:33:25 |         MASTER-SAAO | (00h 38m 49.79s , -60d 05m 07.9s) |   C |    60 | 18.6 |        
   64029 | 2020-04-16 02:34:45 |         MASTER-SAAO | (00h 36m 38.94s , -58d 04m 49.4s) |   C |    60 | 18.5 |        
   64105 | 2020-04-16 02:36:00 |         MASTER-SAAO | (00h 53m 43.98s , -58d 04m 24.7s) |   C |    60 | 18.3 |        
Filter C is a clear (unfiltred) band. 


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


GRB_name: GRB200416A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27591
SUBJECT: GRB 200416A: Swift detection of a burst with an optical afterglow
DATE:    20/04/16 07:19:36 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. A. Evans (U Leicester), V. D'Elia (SSDC), J.D. Gropp (PSU),
N. J. Klingler (PSU), S. Laha (GSFC/UMBC/CRESST),
A. Y. Lien (GSFC/UMBC), 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 07:05:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200416A (trigger=966554).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 335.691, -7.530 which is 
   RA(J2000) = 22h 22m 46s
   Dec(J2000) = -07d 31' 47"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 10 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 07:06:57.1 UT, 99.9 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 335.69906, -7.51816 which
is equivalent to:
   RA(J2000)  = 22h 22m 47.77s
   Dec(J2000) = -07d 31' 05.4"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 51 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 (6.54 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.2
(+3.00/-2.56) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 102 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 22:22:47.83 = 335.69929
  DEC(J2000) = -07:31:05.9  =  -7.51831
with a 90%-confidence error radius of about 0.75 arc sec. This position is 1.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.47 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.06. 

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


GRB_name: GRB200416A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27592
SUBJECT: GRB 200416A: Fermi GBM observation
DATE:    20/04/16 13:41:38 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

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


"At 07:05:17.38 UT on 16 April 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200416A (trigger 608713522 /200416295),
which was also detected by the Swift/BAT (Evans et al. 2020, GCN 27591).
The trigger was initially misclassified as a particle event by the flight software.
The GBM on-ground location is consistent with the Swift position.

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

The GBM light curve shows a double-peaked emission episode
with a duration (T90) of about 9 s (50-300 keV).
The time-averaged spectrum from T0-2 s to T0+6 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.87 +/- 0.15 and
the cutoff energy, parameterized as Epeak, is 74 +/- 6 keV.

The event fluence (10-1000 keV) in this time interval is
(1.43 +/-  0.08)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.064 s in the 10-1000 keV band
is 6.5 +/- 0.3 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 64 +/- 9 keV, alpha = -0.66 +/- 0.24
and beta = -2.5 +/- 0.3.


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: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27593
SUBJECT: GRB 200412B: continued Tautenburg observations 
DATE:    20/04/16 14:25:46 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

S. Klose, B. Stecklum, S. Melnikov, and A. Nicuesa Guelbenzu (all 
Tautenburg) report:

We continued observing the field of GRB 200412B (Fermi GBM team, GCN 
27547) with the Tautenburg 1.34m Schmidt telescope equipped with the 
TAUKAM 6k x 6k CCD camera and the wide V-band filter (VB; Stecklum et al., 
GCN 27567, 27582; Klose et al., GCN 27575).

For the optical transient (Lipunov et al., GCN 27555, 27556) at a mean 
time of 3.53 days post burst we measure VB = 22.29 +/- 0.11. This confirms 
the suspected steepening of the light curve decay (Stecklum et al., GCN 
27582). Our present VB-band data imply alpha2 = 2.52 +/- 0.02 and a break 
time of 2.04 +/- 0.02 days.


GRB_name: GRB200416A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27594
SUBJECT: GRB 200416A: Swift-XRT refined Analysis
DATE:    20/04/16 15:03:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

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

We have analysed 677 s of XRT data for GRB 200416A (Evans et al. GCN
Circ. 27591), from 84 s to 773 s after the  BAT trigger. The data
comprise 43 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The refined XRT position is RA, Dec = 335.6986, -7.5179 which is
equivalent to:

RA (J2000): 22 22 47.66
Dec(J2000): -07 31 04.3

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

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.9 (+/-0.5), followed by a break at T+167 s to an alpha
of 0.25 (+0.18, -0.25).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.86 (+0.22, -0.20). The
best-fitting absorption column is  9.6 (+6.3, -3.1) x 10^20 cm^-2,
consistent with the Galactic value of 6.5 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 3.6 x 10^-11 (4.3 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      9.6 (+6.3, -3.1) x 10^20 cm^-2
Galactic foreground: 6.5 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.86 (+0.22, -0.20)

The GRB entered Swift's Moon-proximity observing constraint shortly
after the trigger, and will not be observable until early on Monday
April 20th; observations are planned for that time. The light curve
appears to be in the plateau phase common to X-ray afterglows and is
expected to break to a steeper decay at some point within the next ~24
hours, so we do not attempt to predict the flux at T0+24 hours.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00966554.

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


GRB_name: GRB200415A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27595
SUBJECT: Improved IPN error box for GRB 200415A (consistent with the Sculptor Galaxy)
DATE:    20/04/16 16:16:25 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. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team, and

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

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

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

Using the Konus-Wind data we have
triangulated this GRB to an improved, but still preliminary,
3 sigma error box whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    11.874 (00h 47m 30s) -25.194 (-25d 11' 37")
  Corners:
    11.760 (00h 47m 02s) -25.393 (-25d 23' 34")
    12.022 (00h 48m 05s) -25.302 (-25d 18' 09")
    11.987 (00h 47m 57s) -24.994 (-24d 59' 38")
    11.726 (00h 46m 54s) -25.085 (-25d 05' 05")
  ---------------------------------------------
The error box area is about 274 sq. arcmin, and its maximum
dimension is 27 arcmin (the minimum one is 14.7 arcmin).
The Sun distance was about 37 deg.

This error box reduces the initial error box (Svinkin et al.,
GCN Circ. 27585). The Sculptor Galaxy (NGC 253) is mostly inside
the box, strengthen the association the burst with the galaxy
proposed in GCN 27585.

We encourage an extensive search, both retrospective and
follow-up, for an accompanying radio emission.

This box may be further improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB200415_T31685/IPN/

The Swift (BAT) event data used for the IPN localization
came from the GUANO system (https://www.swift.psu.edu/guano/).

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


GRB_name: GRB200415A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27596
SUBJECT: Konus-Wind observation of GRB 200415A (a magnetar Giant Flare in Sculptor Galaxy?)
DATE:    20/04/16 16:48:53 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 extremely-bright, short-duration GRB 200415A
(IPN localization: Svinkin et al., GCN Circ. 27585, 27595;
Fermi-GBM observation: Bissaldi et al., GCN Circ. 27587)
triggered Konus-Wind at T0=31681.401 s UT (08:48:01.401).

The burst light curve starts at ~T0-2 ms with the sharp
rise of extremely-bright pulse, with a duration of ~5 ms.
This pulse is followed by a weaker, steadily decaying
emission which is visible up to ~T0+200 ms.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst had a fluence of
8.1(-0.8, +0.9)x10^-6 erg/cm2,
and a 2-ms peak flux, measured from T0-0.002 s,
of 1.0(-0.08,+0.08)x10^-3 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+0.192 s)
is best fit in the 20 keV - 15 MeV range
by a power law with exponential cutoff (CPL) model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = +0.10(-0.23,+0.27)
and Ep = 818(-112,+136) keV (chi2 = 34/49 dof).
Fitting by a GRB (Band) model yields similar alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.5
(chi2 =33/49 dof).

The spectrum measured near the peak count rate (from T0 to T0+0.064 s)
is best fit in the 20 keV - 15 MeV range by the CPL model
with alpha = +0.12(-0.24,+0.20) and Ep = 1060(-160,+190) keV
(chi2 = 25/36 dof). Fitting by a GRB (Band) model yields similar
alpha and Ep, and an upper limit on the high energy photon index:
beta < -2.6 (chi2 =24/35 dof).

Assuming the likely GRB 200415A association with the nearby Sculptor
galaxy at ~3.5 Mpc (Svinkin et al., GCN 27585, GCN 27595),
we estimate the burst isotropic energy to ~1.3x10^46 erg and
the 2-ms peak luminosity to ~1.6x10^48 erg/s.
These values closely resemble the energetics of the initial pulse of
the SGR 1806-20 giant magnetar flare (GF) measured by KW and HELICON
(Frederiks et al., 2007 AstL 33 1).

GRB 200415A also shows a striking similarity, in light curve, spectrum,
and energy, with GRB 051103 (Frederiks et al., 2007 AstL 33 19),
the extragalactic GF candidate in the M81/M82 group of galaxies
located at nearly the same distance, ~3.6 Mpc.

Even the giant magnetar flare origin of GRB 200415A and GRB 051103
cannot be established unequivocally (the key evidence, pulsating tail,
could hardly be detected by KW or Fermi-GBM from ~3.5 Mpc),
the common nature of the two ultra-bright flares is highly probable.

The Konus-Wind light curve of GRB 200415A is available at
http://www.ioffe.ru/LEA/GRBs/GRB200415_T31681/

A comparison of Konus-Wind light curves of GRB 200415A and GRB 051103
can be found at http://www.ioffe.ru/LEA/GRBs/GRB200415_T31681/051103_200415.pdf


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


GRB_name: GRB200415A
Detection_method: Fermi LAT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27597
SUBJECT: GRB 200415A: Fermi-LAT localization update
DATE:    20/04/16 20:48:00 GMT
FROM:    Nicola Omodei at Stanford U.  <nicola.omodei@slac.stanford.edu>

N. Omodei (Stanford University),  F. Piron (CNRS/IN2P3/LUPM), M. Axelsson (KTH & Stockholm Univ.), F. Longo (University and INFN, Trieste), D. Kocevski (NASA/MSFC), E. Bissaldi (Politecnico & INFN Bari)  and A. Berretta (University & INFN Perugia) 
report on behalf of the Fermi-LAT Collaboration:

We performed additional analysis to estimate the localization contour of GRB 200415A detected at high energy by Fermi-LAT (GCN 27586).
The best localization is at: R.A., Dec. = 11.07, -25.02 (degrees, J2000) with a circular error of 0.38 and 0.59 degrees (statistical only), respectively at 68% and 90% confidence levels.

The shape of the contour shows an elongation toward the location of the IPN error box (GCN 27595) placing the Sculptor Galaxy (NGC 253) between the 68% and the 90% c.l. contours. 
A localization map is posted at:
https://www-glast.stanford.edu/pub_data/1775/GRB200415A_TSMAP_LAT.gif

The Fermi-LAT point of contact for this burst is Alessandra Berretta (alessandra.berretta@pg.infn.it).

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


GRB_name: GRB200412B
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27598
SUBJECT: GRB200412B: GROWTH India detection of afterglow
DATE:    20/04/17 06:59:26 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

H. Kumar, M. Khandagale, K. Deshmukh, V. Bhalerao(IITB), G. C. Anupama, B. Kumar, A. Singh, A. Dutta, S. Barway(IIA), P. Dorji (IAO), U. Stanzin (IAO), report on behalf of the GROWTH collaboration:

We observed GRB200412B reported by Fermi GBM Team (GCN 27547) and Burgess J. et al, (GCN 27548) with 0.7m robotic GROWTH-India telescope. We switched from tiled observations to targeted follow-up based on the afterglow identification by Lipunov V. et al, (GCN 27555) at RA(J2000) = 18:33:15.33  Dec(J2000) = +62:31:57.0 . The field was observed multiple times in g and r filters with 550 sec exposure time, starting about 7.4 hours after the trigger. We clearly detect the afterglow emission. The decay is well-described by a power law with alpha = 1.05 +/- 0.14 for g band data and 0.85 +/- 0.17 for r band data.

We obtained the following results:
------------------------------------------------------------------
 JD(Start)| Exposure(sec) | Filter | Mag | lim_Mag |
------------------------------------------------------------------
2458952.1903 | 550 |  g  |  18.301+/-0.034 |  20.92  
2458952.3277 | 550 |  g  |  18.590+/-0.039 |  20.54   
2458952.3601 | 550 |  g  |  18.761+/-0.040 |  20.52
2458952.3768 | 550 |  g  |  18.826+/-0.039 |  20.56
2458952.4216 | 550 |  g  |  18.984+/-0.041 |  20.65
2458952.1982 | 550 |  r  |  17.854+/-0.027 |  20.83     
2458952.3356 | 550 |  r  |  17.998+/-0.036 |  20.32   
2458952.3681 | 550 |  r  |  18.231+/-0.031 |  20.58
2458952.3847 | 550 |  r  |  18.314+/-0.039 |  20.65
2458952.4295 | 550 |  r  |  18.379+/-0.033 |  20.77
------------------------------------------------------------------

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: GRB200415A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27599
SUBJECT: GRB 200415A: MASTER imspection and possible localisation 
DATE:    20/04/17 07:49:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, N.Tyurina,
E. Gorbovskoy, V.Kornilov, P.Balanutsa,A.Kuznetsov,F.Balakin,
V.Vladimirov, D. Vlasenko, I.Gorbunov, D.Zimnukhov, V.Senik, T.Pogrosheva,
D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico Felix
Aguilar OAFA),
H. Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio 
ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova (Irkutsk State University, API),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational State
University)


MASTER OTJ 004724.94-252125.6s  (AT2020hok)

MASTER-SAAO auto-detection system ( Lipunov et al., "MASTER Global Robotic
Net", Advances in Astronomy, 2010, 30L )
  proposed interesting  source at (RA, Dec) = 00h 47m 24.94s -25d 21m 25.6s
on  2020-04-17.15061 UT during GRB 200415 error box inspection 
(GCN  27579; 27580; 27586; 27595; 27597;).

Inside galaxy NGC 0253 (Svinkin, 27595; Frederiks 27597;) there 
is  an  interesting extended object with an XMM X-ray source  at 00 47 
25.0800 -25 21 23.760 .
This is may be globular cluster: B-V ~ 1
The  unfiltered magnitude is 15.8m (mlim 17.9).
The source  is seen in 24 images. No optical variability detected.

We have reference image on 2018-08-10.99113 UT with  unfiltered 
mlim=20.3m.

Follow up observations are required.

The cover map is available at
https://master.sai.msu.ru/site/master2/event.php?id=1337630

The inspection  and reference images are available at:

http://master.sai.msu.ru/static/OT/183315.33623157.0.png


GRB_name: GRB200412B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27600
SUBJECT: GRB 200412B: Swift XRT confirmation of afterglow and UVOT upper limits
DATE:    20/04/17 17:02:07 GMT
FROM:    Boris Sbarufatti at PSU  <bxs60@psu.edu>

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

Swift XRT performed follow up observations on the afterglow candidate reported by Page et al. (GCN #27561).

XRT data now comprise 6.1 ks of Photon Counting data covering times from T+20 ks to T+370 ks.

The light curve is best fit by a power-law with decay index 1.6 +/- 0.3. We thus confirm that this is indeed the afterglow of GRB 200412B.
The latest results can be viewed via: https://www.swift.ac.uk/xrt_curves/00020981/

In the initial Swift observation about 20ks after the trigger, the source was not in the UVOT field of view, which is smaller than that of the XRT.  In the follow up observations around 360ks after the trigger we obtained the following 3-sigma upper limits to the source (Vega magnitudes, uncorrected for reddening):
filter exposure   UL (mag)
 v       374       >19.76
 b       374       >20.74
 u       374       >20.41
uvw1     749       >20.31
uvm2    1201      >20.48
uvw2    1499      >20.83 

This circular is an official product of the Swift team.


GRB_name: GRB200416A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27601
SUBJECT: GRB 200416A: Swift-BAT refined analysis
DATE:    20/04/17 18:07:53 GMT
FROM:    Sibasish Laha at GSFC  <sibasish.laha@nasa.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), P. A. Evans (U Leicester)
H. A. Krimm (NSF), S. Laha (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-61 to T+242 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 200416A (trigger #966554)
(P. A. Evans et al., GCN Circ. 27591).  The BAT ground-calculated position is
RA, Dec = 335.691, -7.525 deg which is
   RA(J2000)  =  22h 22m 45.8s
   Dec(J2000) = -07d 31' 29.5"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 33%.

The mask weighted light curve shows multi-peaked structure. The
overall structure starts at ~T-2 s and lasts till ~T+6 s.
T90 (15-350 keV) is 5.04 +- 0.73 sec (estimated error including systematics).

The time-averaged spectrum from T-1.31 to T+4.69 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.76 +- 0.15.  The fluence in the 15-150 keV band is 8.7 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.05 sec in the 15-150 keV band
is 3.8 +- 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/966554/BA/


GRB_name: GRB200416A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27602
SUBJECT: GRB 200416A: Swift/UVOT Detection
DATE:    20/04/18 06:40:43 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 200416A: Swift/UVOT Detection

K. K. Simpson (PSU) and P. A. Evans (U. Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200416A
102 s after the BAT trigger (Evans et al., GCN Circ. 27591).
A source consistent with the XRT position
(Evans GCN Circ. 27594)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  22:22:47.84 = 335.69934 (deg.)
    Dec (J2000) = -07:31:06.0  =  -7.51833 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).

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

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

white              102          252          147         16.57 +/- 0.03
v                  644          664           19         17.05 +/- 0.32
b                  570          590           20         17.48 +/- 0.20
u                  314          564          246         16.44 +/- 0.04
w1                 694          714           20         16.59 +/- 0.23
m2                 668          688           19        >16.3
w2                 620          640           19        >17.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.06 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB200410A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27603
SUBJECT: GRB 200410A: Optical upper limit
DATE:    20/04/18 07:14:21 GMT
FROM:    Amit Kumar at ARIES, India  <amitkundu515@gmail.com>

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

We observed the field of Swift GRB 200410A (Simpson et al., GCN Circ.
27518, Gropp et al., GCN 27523, Kuin et al., GCN 27532, Pizzuto et al., GCN
27552, Laha et al., GCN Circ. 27578, Valentin et al., GCN 27584) with the
1.3m Devsthal Fast Optical Telescope (DFOT) at Aryabhatta Research
Institute of Observational Sciences (ARIES), Nainital
(India), from 2020-04-10 UT 21:34:29 to 2020-04-10 UT 23:31:07
(corresponding to
19.15 to 21.09 hours from the GRB trigger time). We observed 12 frames
each of 300 seconds in Bessel R filter and a series of 11x300 seconds
exposures in
Bessel I filter. As mentioned by Jelinek et al., 27520, at the position of
the optical afterglow of GRB 200410A there are two nearby stars, so to do
the photometry we observed 300 seconds frame in Bessel R and I filter on
2020-04-15 UT 21:26:22 (5.79 days since burst) to do the template
subtraction. Template subtraction was done using the IRAF (
http://iraf.noao.edu/).

After the template subtraction, we do not find any new optical source
within the Swift XRT enhanced error circle in any individual as well as the
stacked frame.


The 3-sigma upper limits are as follows:

T_start-T0 (days)    Start Date (UTC)             End Date (UTC)
 Filter        3-sigma upper limit (mag)
---------------------------------------------------------------------------------------------------------------
19.15                2020-04-10 21:34:29          2020-04-10 22:30:06
 R               >22.2
20.18                2020-04-10 22:35:46          2020-04-10 23:31:07
 I               >22.4



Photometry is done based on the USNO-B1.0 catalog. The quoted magnitudes
are not corrected for Galactic extinction.

[GCN OPS NOTE(18apr20): The author-constructed header was removed.  The header
is supplied by the GCN processing system.]


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27604
SUBJECT: GRB 200412B: continued AbAO, Mondy, TSHAO, Terskol optical observations
DATE:    20/04/18 16:55:29 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), A.V. Shein (INASAN), I.A. Izvekova 
(ICAMER NASU),  E. Klunko (ISTP),  M. Eselevich (ISTP), R. Ya. 
Inasaridze (AbAO), V.R. Ayvazian (AbAO),  G. V.  Kapanadze (AbAO), I. 
Reva (FAPHI),  E. Mazaeva (IKI), A. Volnova  (IKI),  I. Molotov (KIAM) 
report on behalf of  GRB IKI FuN:

We observed the field of GRB 200412B (Fermi GBM team, GCN 27547; Mailyan
et al., GCN 27558; see also Burgess et al., GCN 27548; Longo et al., GCN
27557; Page et al., GCN 27561; Gupta et al., GCN 27563; Zheng et al., 
GCN 27565)  with Zeiss-2000 of Mt.Terskol observatory, Zeiss-1000 1-m 
telescope of Tien Shan Astronomical Observatory,  AZT-33IK 1.5-m 
telescope of Sayan observatory (Mondy) and AS-32 (0.7m) telescope of 
Abastumani Observatory.  We  still detected  the afterglow of GRB 
200412B  (Lipunov et al., GCNs 27555, 27556; see also e.g. Kumar et al., 
GCN 27564; Belkin et al., GCN 27566, Stecklum et al., GCN 27567,
Moskvitin GCN 27570; Xin  et al., GCN 27571).  Preliminary photometry of 
the afterglow is following.

Date       UT start  t-T0       Filter  OT Err. UL   Observatory
                     (mid, days)
2020-04-13 23:10:27 1.59707 18*120 R 20.57 0.03 22.8 Terskol Z-2000
2020-04-15 14:55:11 3.25105 15*120 V 21.95 0.14 22.8 Mondy AZT-33IK
2020-04-16 17:04:23 4.33800 11*120 R n/d   n/d  20.5 Mondy AZT-33IK
2020-04-16 22:30:40 4.57812 61*60  R n/d   n/d  22.2 AbAO AS-32
2020-04-17 14:51:32 5.25754 28*120 R 23.22 0.28 23.4 Mondy AZT-33IK
2020-04-17 19:53:06 5.47912 91*60  R n/d   n/d  22.3 TSHAO Z-1000
2020-04-17 20:12:07 5.48573 36*120 R 23.29 0.29 23.4 Terskol Z-2000

The photometry is based on nearby USNO-B1.0 stars.
The light curve based on on above photometry  and photometry published 
earlier (Belkin  et al., GCN 27574;  Belkin  et al., GCN 27566;  Belkin 
et al., GCN 27583) can be found at 
http://grb.rssi.ru/GRB200412B/GRB200412B_LC.png
(For reference, we also posted the photometric results of the Tautenburg 
Observatory (Klose et al., GCN 27593; Stecklum et al., GCN 27582; Klose 
et al., GCN 27575; Stecklum et al., GCN 27567).

The index of power law decay taken from our R-filter observations up to 
2.3 days is -1.58+/-0.07 (see also  Xin  et al. GCN 27571; Klose et al., 
GCN 27575). Later we may assume  a jet break previously suggested by 
Klose et al. (GCN 27575) and Stecklum et al. (GCN 27567).


GRB_name: GRB200412B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27605
SUBJECT: GRB 200412B: continued Terskol optical observations
DATE:    20/04/19 13:50:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Pozanenko (IKI), A.V. Shein (INASAN), I.A. Izvekova 
(ICAMER NASU), E. Mazaeva (IKI), A. Volnova  (IKI) report on behalf of 
GRB IKI FuN:

We observed the field of GRB 200412B (Fermi GBM team, GCN 27547; Mailyan
et al., GCN 27558; see also Burgess et al., GCN 27548; Longo et al., GCN
27557; Page et al., GCN 27561; Gupta et al., GCN 27563; Zheng et al., 
GCN 27565)  with Zeiss-2000 of Mt.Terskol observatory.  We  marginally 
detected  the afterglow of GRB 200412B  (Lipunov et al., GCNs 27555, 
27556; see also e.g. Kumar et al., GCN 27564; Belkin et al., GCN 27566, 
Stecklum et al., GCN 27567, Moskvitin GCN 27570; Xin  et al., GCN 
27571).  Preliminary photometry of the afterglow is following.

Date       UT start  t-T0       Filter  OT Err. UL   Observatory
                     (mid, days)
2020-04-18 19:52:22 6.47687 43*120 R 23.6 0.3 23.6 Terskol Z-2000

The photometry is based on nearby USNO-B1.0 stars.
The update light curve can be found at 
http://grb.rssi.ru/GRB200412B/GRB200412B_LC.png


GRB_name: GRB200420A
Detection_method: Fermi GBM final loc
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  27607
SUBJECT: GRB 200420A: Fermi GBM Final Real-time Localization
DATE:    20/04/20 02:43:21 GMT
FROM:    Fermi GBM Team at MSFC/Fermi-GBM  <do_not_reply@GIOC.nsstc.nasa.gov>

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

At 02:32:58 UT on 20 Apr 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200420A (trigger 609042783.59756 / 200420106).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 310.3, Dec = -27.5 (J2000 degrees, equivalent to J2000 20h 41m, -27d 30'), with a statistical uncertainty of 85.4 degrees.

The angle from the Fermi LAT boresight is 19.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200420106/quicklook/glg_skymap_all_bn200420106.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/bn200420106/quicklook/glg_healpix_all_bn200420106.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200420106/quicklook/glg_lc_medres34_bn200420106.gif


