GRB 200519A
GCN Circular 27756
Subject
GRB 200519A: Swift detection of a burst with an optical afterglow
Date
2020-05-19T11:42:49Z (5 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
B. Sbarufatti (PSU), S. B. Cenko (GSFC), C. Gronwall (PSU),
J.D. Gropp (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC) and K. L. Page (U Leicester) report on
behalf of the Neil Gehrels Swift Observatory Team:
At 11:20:23 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200519A (trigger=973140). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 255.334, -30.380 which is
RA(J2000) = 17h 01m 20s
Dec(J2000) = -30d 22' 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 80 sec. The peak count rate
was ~37000 counts/sec (15-350 keV), at ~23 sec after the trigger.
The XRT began observing the field at 11:21:13.3 UT, 49.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 255.3327, -30.3782 which is equivalent to:
RA(J2000) = 17h 01m 19.85s
Dec(J2000) = -30d 22' 41.5"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 7.6 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy.
The initial flux in the 2.5 s image was 1.36e-08 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 57 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 17:01:20.00 = 255.33335
DEC(J2000) = -30:22:40.9 = -30.37803
with a 90%-confidence error radius of about 0.61 arc sec. This position is 2.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.38 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.47.
Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)
GCN Circular 27757
Subject
GRB 200519A: iTelescope optical afterglow detection
Date
2020-05-19T16:37:18Z (5 years ago)
From
Albert Kong at NTHU <akhkong@gmail.com>
A.K.H. Kong (NTHU, Taiwan) reports
We observed the field of GRB 200519A (Sbarufatti et al. GCN 27756)
with the T31 0.5m telescope of iTelescope.Net in Siding Spring,
Australia. The observation was done with a luminance filter (400-700
nm) beginning at 2020-05-19 15:07:45 UT (about 3.8 hours after the
trigger) for 300 sec. The optical afterglow (Sbarufatti et al. GCN
27756) was detected with an estimated magnitude of 19.3+/-0.8 by
calibrating with the USNO UCAC5 catalogue.
GCN Circular 27759
Subject
GRB 200519A: LCO Optical Afterglow Detection
Date
2020-05-19T17:04:42Z (5 years ago)
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 200519A (Sbarufatti et al., GCN 27756) with the LCO 1-m Sinistro instrument at the Siding Spring Observatory Australia site, on May 9, from 12:39 to 13:02 UT (corresponding to 1.05 to 1.38 hours from the GRB trigger time) with the Bessel R and I filters.
We performed a series of 5x120s exposures in R and I. We detect an optical source in stacked images at the UVOT afterglow candidate position position. Using the USNO-B.1 catalog as reference, we calculate the following magnitudes:
R = 17.07 +/- 0.02
I = 16.69 +/- 0.02
These magnitudes are not corrected for galactic extinction.
R.S. is funded by NSF AST grant #1831682
GCN Circular 27760
Subject
GRB 200519A: BOOTES-3/YA optical counterpart observations
Date
2020-05-19T21:41:56Z (5 years ago)
From
Youdong HU at IAA-CSIC <youdong@iaa.es>
Y.-D. Hu, E. Fernandez-Garcia, A. J. Castro-Tirado (IAA-CSIC), I.
Carrasco and C. Perez del Pulgar (Univ. de Malaga), M. D.
Caballero-Garcia (ASU-CAS, CZ) and R. Querel (NIWA), on behalf of a
larger collaboration, report:
The 60cm BOOTES-3/YA robotic telescope at NIWA Lauder in Otago (New
Zealand) automatically responded to the Swift trigger of GRB 200519A
(Sbarufatti et al. GCNC 27756). The first image (clear filter) were
obatined starting at 11:20:57 UT (~ 34 s after trigger). At the position
reported by Swift/UVOT (Sbarufatti et al. GCNC 27756), we found the
optical counterpart with a magnitude of 14.96+-0.12 mag in the 1s
exposure image whose median time at 52s that also reported by iTelescope
(Kong et al. GCNC 27757) and LCO (Strausbaugh et al. GCNC 27759), which
calibrated with nearby stars in USNO-B 1.0 catalog. Further analysis is
ongoing.
We thank the staff at NIWA for its excellent support.
GCN Circular 27761
Subject
GRB 200519A: Enhanced Swift-XRT position
Date
2020-05-19T22:12:54Z (5 years ago)
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 832 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 200519A, 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 = 255.33318, -30.37824 which is equivalent
to:
RA (J2000): 17h 01m 19.96s
Dec (J2000): -30d 22' 41.7"
with an uncertainty of 1.8 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 27763
Subject
GRB 200519A: Swift-XRT refined Analysis
Date
2020-05-19T23:42:47Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
D.N. Burrows (PSU), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo (INAF-OAB), M.G.
Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , J. D. Gropp (PSU),
J.A. Kennea (PSU) and B. Sbarufatti report on behalf of the Swift-XRT
team:
We have analysed 8.2 ks of XRT data for GRB 200519A (Sbarufatti et al.
GCN Circ. 27756), from 42 s to 35.4 ks after the BAT trigger. The data
comprise 970 s in Windowed Timing (WT) mode (the first 5 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. 27761).
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.16 (+/-0.05).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.902 (+/-0.029). The
best-fitting absorption column is 4.35 (+0.17, -0.16) x 10^21 cm^-2,
in excess of the Galactic value of 3.3 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.75 (+/-0.08) and a
best-fitting absorption column of 4.7 (+/-0.5) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 4.7 x 10^-11 (6.6 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.7 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 3.3 x 10^21 cm^-2
Excess significance: 4.4 sigma
Photon index: 1.75 (+/-0.08)
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 0.11 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.1 x
10^-12 (7.1 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00973140.
This circular is an official product of the Swift-XRT team.
GCN Circular 27764
Subject
GRB 200519A: 1.3m DFOT Optical Afterglow Detection
Date
2020-05-20T01:58:43Z (5 years ago)
From
Amit Kumar at ARIES, India <amitkundu515@gmail.com>
A. Kumar (ARIES), S. B. Pandey (ARIES), K. Chand (ARIES), A. Aryan (ARIES),
R. Gupta (ARIES), A. Ghosh (ARIES), Dimple (ARIES), and K. Misra (ARIES)
report:
We observed the optical afterglow of the Swift detected GRB 200519A (GCN
27756, GCN 27761 and GCN 27763) with the 1.3m Devsthal Fast Optical
Telescope (DFOT) at
Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital
(India), from 2020-05-19T19:17:27 to 2020-05-19T22:01:38 UTC.
We observed 11 frames each of 300 seconds in Bessell R filter, whereas, a
serious of 7x300 seconds exposure in Bessell I filter.
In the stacked images, we clearly detected the optical afterglow of GRB
200519A in both Bessell R and I filters within the Swift XRT enhanced error
circle (Osborne et al. GCN 27761).
The estimated magnitudes are consistent with optical detections by Kong et
al. GCN 27757, Strausbaugh et al. GCN 27759, and Hu et al. 27760.
The observed magnitudes are as follows:
T_start-T0 (hours) Start Date (UTC) Filter
Magnitudes (mag)
---------------------------------------------------------------------------------------------------------------
7.95 2020-05-19T19:17:27 R 19.4
+- 0.1
9.98 2020-05-19T21:19:27 I
18.2 +- 0.1
Photometry is done based on the USNO-B1.0 catalog. The quoted magnitudes
are not corrected for Galactic extinction.
GCN Circular 27765
Subject
Swift GRB 200519A: Global MASTER-Net observations report
Date
2020-05-20T05:38:25Z (5 years ago)
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 200519A ( B. Sbarufatti et al., GCN 27756) errorbox 23275 sec after notice time and 23295 sec after trigger time at 2020-05-19 17:48:38 UT, with upper limit up to 17.0 mag. The observations began at zenith distance = 75 deg. The sun altitude is -25.5 deg.
MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB 200519A errorbox 46397 sec after notice time and 46416 sec after trigger time at 2020-05-20 00:14:00 UT, with upper limit up to 16.6 mag. The observations began at zenith distance = 69 deg. The sun altitude is -31.7 deg.
The galactic latitude b = 7 deg., longitude l = 354 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1360465
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
23385 | MASTER-SAAO | C | 180 | 16.9 |
23385 | MASTER-SAAO | C | 180 | 16.2 |
24012 | MASTER-SAAO | C | 180 | 17.0 |
24012 | MASTER-SAAO | C | 180 | 16.6 |
46507 | MASTER-OAFA | C | 180 | 16.6 |
47353 | MASTER-OAFA | C | 180 | 16.5 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 27766
Subject
GRB 200519A: AstroSat CZTI detection
Date
2020-05-20T09:38:42Z (5 years ago)
From
Soumya Gupta at IUCAA/ASTROSAT <soumya@iucaa>
S. Gupta, V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (IUCAA/TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data showed the detection of a long GRB 200519A, which was also detected by Swift (Sbarufatti B. et al., GCN #27756), iTelescope (Kong A.et al., GCN # 27757), LCO (Strausbaugh R. et al., GCN # 27759), BOOTES-3/YA (Hu Y. et al., GCN # 27760), 1.3m DFOT (Kumar A. et al., GCN # 27764) and Global MASTER-Net (Lipunov V. et al., GCN # 27765).
The source was clearly detected in the 40-200 keV energy range. Of the ~80-second duration reported by Swift/BAT, CZTI detected only the brightest segment peaking at 2020-05-19 11:20:46.500 UT. The measured peak count rate associated with the burst is 983 +/- 39 cts/s above the background in the combined data of four quadrants, with a total of 3616 +/- 17 cts. The local mean background count rate was 519 +/- 1 cts/s. Using cumulative rates, we measure a T90 of 8.46 +/- 0.05 s.
It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed a single peak of emission peaking at 2020-05-19 11:20:46.000 UT. The measured peak count rate is 2339 +/- 62 cts/s above the background in the combined Veto data of four quadrants, with a total of 8499 +/- 21 cts. The local mean background count rate was 1541 +/- 1 cts/s. We measure a T90 of 8.64 +/- 0.02 s from the cumulative Veto light curve.
CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN Circular 27767
Subject
GRB 200519A: GROWTH-India optical follow-up
Date
2020-05-20T16:32:17Z (5 years ago)
From
Harsh Kumar at Indian Inst of Tech,Bombay <harshkosli13@gmail.com>
H. Kumar, V. Bhalerao(IITB), G. C. Anupama, S. Barway, J. Stanzin (IIA)
report on behalf of the GROWTH-India collaboration:
We followed up GRB200519A (R. Sbarufatti et al., GCN 27756, A. Kong et al., GCN
27757, R. Strausbaugh et al., GCN 27759, Y. Hu et al., GCN 27760, A Kumar
et al., GCN 27764) with 0.7m GROWTH-India telescope. We obtained 600-sec
exposures in SDSS g, r, i filters starting at UT 20-05-19T17:11:06 (~5.85
hrs after the burst).
We obtained the following magnitudes with PSF photometry, calibrated
against PanSTARRs PS1 data release (Flewelling et al., 2018).
------------------------------------------------------------------
JD(Start) | T-T0(hrs) | Filter | Mag |
------------------------------------------------------------------
2458989.216 | 5.85 | g | 19.926 +/- 0.09
2458989.321 | 8.36 | g | 20.514 +/- 0.09
2458989.354 | 9.16 | g | 20.779 +/- 0.13
2458989.281 | 7.41 | r | 19.359 +/- 0.07
2458989.305 | 7.98 | r | 19.505 +/- 0.06
2458989.329 | 8.56 | r | 19.788 +/- 0.06
2458989.361 | 9.33 | r | 19.891 +/- 0.08
2458989.265 | 7.02 | i | 19.529 +/- 0.12
2458989.313 | 8.17 | i | 19.984 +/- 0.14
2458989.369 | 9.52 | i | 20.206 +/- 0.18
2458989.392 | 10.07| i | 20.583 +/- 0.26
------------------------------------------------------------------
We found that the source is fading with a power-law of 1.65 +/- 0.28 in g
band, 2.36 +/- 0.4 using in r band and 2.37 +/- 0.33 in i band observations.
The magnitudes are not corrected for galactic extinction.
The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7 degree
field of view, set up by the Indian Institute of Astrophysics and the
Indian Institute of Technology Bombay with support from the Indo-US Science
and Technology Forum (IUSSTF) and the Science and Engineering Research
Board (SERB) of the Department of Science and Technology (DST), Government
of India (https://sites.google.com/view/growthindia/). It is located at the
Indian Astronomical Observatory (Hanle), operated by the Indian Institute
of Astrophysics (IIA).
GCN Circular 27769
Subject
GRB 200519A: Swift/UVOT Detection
Date
2020-05-20T19:09:27Z (5 years ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
M. H. Siegel (PSU) and B. Sbarufatti (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 200519A
58 s after the BAT trigger (Sbarufatti et al., GCN Circ. 27756).
A source consistent with the XRT position
(Sbarufatti et al. GCN Circ. 27756)
is detected in the initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 17:01:20.01 = 255.33337 (deg.)
Dec (J2000) = -30:22:41.1 = -30.37808 (deg.)
with an estimated uncertainty of 0.42 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 58 208 147 15.43 +/- 0.02
v 599 619 20 16.30 +/- 0.16
b 525 545 19 17.13 +/- 0.13
u 270 519 246 16.27 +/- 0.04
w1 648 840 39 17.46 +/- 0.25
w2 747 766 19 >17.5
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.47 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 27770
Subject
GRB 200519A: Insight-HXMT/HE detection
Date
2020-05-21T02:10:25Z (5 years ago)
From
Shuo Xiao at IHEP <xiaoshuo@ihep.ac.cn>
GRB 200519A: Insight-HXMT/HE detection
S. Xiao, Y. G. Zheng, C. Cai, Y. F. Du, W. C. Xue,
Q. Luo, Q. B. Yi, Y. Huang, C. K. Li, G. Li,
X. B. Li, J. Y. Liao, S. L. Xiong,C. Z. Liu,
X. F. Li, Z. W. Li, Z. Chang, A. M. Zhang, Y. F. Zhang,
X. F. Lu, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU),
T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
At 2020-05-19T11:20:23.73 (T0), Insight-HXMT/HE detected
GRB 200519A (trigger ID: HEB200519472) in a routine search of the data,
which also triggered Swift/BAT (GCN #27756).
The Insight-HXMT/HE light curve mainly consists of multiple
pulses with a duration (T90) of 8.97 s measured from T0+19.85 s.
The 1-ms peak rate, measured from T0+23.18 s, is 1206 cnts/sec.
The total counts from this burst is 4010 counts.
URL_LC: http://twiki.ihep.ac.cn/twiki/viewfile/HXMT/GRBList?filename=HEB200519472_lc.jpg;rev=2
All measurements above are made with the CsI detectors operating in the
normal mode with the energy range of about 80-800 keV (deposited energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the telescope.
Insight-HXMT is the first Chinese space X-ray telescope, which was
funded jointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information about it could be found at:
http://www.hxmt.org.
GCN Circular 27771
Subject
GRB 200519A: Swift-BAT refined analysis
Date
2020-05-21T03:38:57Z (5 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
M. Stamatikos (OSU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), B. Sbarufatti (PSU),
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 200519A (trigger #973140)
(Sbarufatti et al., GCN Circ. 27756). The BAT ground-calculated position is
RA, Dec = 255.319, -30.393 deg which is
RA(J2000) = 17h 01m 16.6s
Dec(J2000) = -30d 23' 35.6"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.
The mask-weighted light curve shows a multi-peaked structure that starts
at ~T0 and ends at ~T+100 s. The three main peaks occur at ~T+1 s, ~T+24 s,
and ~T+75 s, respectively. T90 (15-350 keV) is 71.88 +- 1.28 sec (estimated
error including systematics).
The time-averaged spectrum from T-0.45 to T+103.00 sec is best fit
by a simple power-law model. The power law index of the time-averaged
spectrum is 1.42 +- 0.03. The fluence in the 15-150 keV band
is 1.2 +- 0.02 x 10^-05 erg/cm2. The 1-sec peak photon flux measured
from T+23.53 sec in the 15-150 keV band is 20.6 +- 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/973140/BA/
GCN Circular 27772
Subject
GRB 200519A: R-band follow-up from HCT
Date
2020-05-21T10:52:29Z (5 years ago)
From
Brajesh Kumar at Indian Inst. of Astrophysics <brajesh.kumar@iiap.res.in>
Brajesh Kumar, Anirban Dutta, Avinash Singh, G. C. Anupama, D. K. Sahu
and Pramod Kumar (IIA, Bengaluru)
We observed the optical afterglow of GRB 200519A (Sbarufatti et al., GCN
27756) with the 2-m Himalayan Chandra Telescope (HCT) located at the
Indian Astronomical Observatory, Hanle, India. The observations started
on 2020-05-19 (20:10:35 UT) under good sky conditions and three
consecutive frames (120, 240, and 240 sec) in Bessell R-band were
obtained. The OT candidate (Kong et al., GCN 27757, Strausbaugh et al.,
GCN 27759, Hu et al., GCN 27760, Kumar et al., GCN 27764, Kumar et al.
GCN 27767, Siegel & Sbarufatti, GCN 27769) is clearly detected in each
frame. The preliminary photometry is performed relative to the USNO-B1.0
catalogue. The initial magnitude of the OT is 19.70 +- 0.10 (uncorrected
for the galactic extinction).
We thank the observing staff at IAO and CREST for helping with the
observations.
GCN Circular 27773
Subject
GRB 200519A: CALET Gamma-Ray Burst Monitor detection
Date
2020-05-21T14:03:23Z (5 years ago)
From
Valentin Pal'shin at AGU <val@phys.aoyama.ac.jp>
P. S. Marrocchesi (U of Siena),
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),
N. Cannady (GSFC/UMBC), M. L. Cherry (LSU),
S. Ricciarini (U of Florence),
and the CALET collaboration:
The Swift GRB 200519A (Swift detection: Sbarufatti et al.,
GCN Circ. 27756, Stamatikos et al., GCN Circ. 27771;
AstroSat CZTI detection: Gupta et al., GCN Circ. 27766;
Insight-HXMT/HE detection: GCN Circ. 27770;
https://gcn.gsfc.nasa.gov/other/200519A.gcn3) triggered the CALET
Gamma-ray Burst Monitor (CGBM) at 11:20:43.755 UTC on 19 May 2020 (trigger
#1273922014: http://cgbm.calet.jp/cgbm_trigger/flight/1273922014/).
The burst signal was seen mainly by the SGM detector. The source location
was outside the FOV of the HXM detectors.
The burst light curve shows a double-peaked pulse which starts at T-2.0 sec,
peaks at T+4.4 sec and ends at T+5.9 sec. The T90 and T50 durations
measured by the SGM data are 6.9 +- 1.5 sec and 3.3 +- 1.9 sec (40-1000
keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1273922014/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.