GRB 200216B
GCN Circular 27128
Subject
GRB 200216B: second epoch optical upper limit at Mondy observatory
Date
2020-02-19T12:01:00Z (6 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), E. Mazaeva (IKI),
A. Volnova (IKI) report on behalf of IKI-GRB-FuN:
We observed the field of GRB 200216B (D'Avanzo et al., GCN 27102: Fermi
GBM team, GCN 27101) with AZT-33IK telescope of Sayan observatory
(Mondy) starting on Feb. 18 (UT) 16:02:31. We did not detect any object
in the enhanced Swift-XRT position (Goad et al., GCN 27106). In
particular we do not detect possible IR-counterpart (Levan et al., GCN
27114). Upper limit is 22.8R.
We detected the object reported earlier (Pozanenko et al., GCN 27122)
with coordinates (J2000) 10:41:44.54 +19:28:19.3 which is 14.5 arcsec
apart from center of enhanced XRT error circle (Goad et al., GCN 27106).
Preliminary photometry of the object is following:
Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
(mid, days) (s)
2020-02-18 16:02:31 2.12497 R 30*120 22.7 0.3 22.8
Power law index of a light curve of the object calculated between the
two epochs is about -0.3. Therefore the object might not be related to
GRB 200216B.
GCN Circular 27122
Subject
GRB 200216B: Mondy and AbAO optical upper limits
Date
2020-02-18T16:01:19Z (6 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Pozanenko (IKI), S. Belkin (IKI), E. Klunko (ISTP), R. Ya.
Inasaridze (AbAO), E. Mazaeva (IKI), A. Volnova (IKI), I. Molotov
(KIAM) report on behalf of IKI-GRB-FuN:
We observed the field of GRB 200216B (D'Avanzo et al. GCN 27102; Fermi
GBM team, GCN 27101) with AZT-33IK telescope of Sayan observatory
(Mondy) starting on Feb. 16 (UT) 13:47:34 i.e. 15 minutes after GRB
trigger. We also observed the GRB 200216B with AS-32 (0.7m) telescope of
Abastumani Observatory starting on Feb. 16 (UT) 20:00:20. We do not
detect any object in the enhanced Swift-XRT position (Goad et al. GCN
27106). In particular we do not detect possible IR-counterpart (Levan et
al., GCN 27114). Preliminary photometry of the field is following.
Date UT start t-T0 Filter Exp. OT UL(3sigma)
(mid, days) (s)
2020-02-16 13:47:34 0.06915 R 30*60 n/d 22.0
2020-02-16 20:00:20 0.29256 R 67*60 n/d 21.8
Photometry is based on the USNO-B2.0 nearby stars.
We note the presense the optical object at coordinates (J2000)
10:41:44.54 +19:28:19.3 and brightess of R=21.75 +/- 0.25 at 0.06915
days (mid time) after triger, and do not detect the object in the secod
epoch R > 21.8 at 0.29256 days. The object is absent in both SDSS ans
Pan-SARRS catalogues. The object is apart 14.5 arcsec from center of
enhanced XRT erro circle (Goad et al. GCN 27106) and the object lies
within 90% BAT ground-calculated position (Krimm et al., GCN 27117).
GCN Circular 27120
Subject
GRB 200216B: Swift-XRT refined Analysis
Date
2020-02-18T10:07:24Z (6 years ago)
From
Paolo D'Avanzo at INAF - OAB <paolo.davanzo@inaf.it>
P. D'Avanzo (INAF-OAB) and P.A. Evans (U. Leicester) report on behalf
of the Swift-XRT team:
We have analysed 1.6 ks of XRT data for GRB 200216B (D'Avanzo et al.
GCN Circ. 27102), from 105 s to 1.7 ks after the BAT trigger. The data
comprise 90 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. 27106).
The light curve can be modelled with a power-law decay with a decay
index of alpha=1.91 (+0.07, -0.06).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.18 (+0.20, -0.19). The
best-fitting absorption column is 7.3 (+2.3, -1.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.63 (+0.27, -0.26)
and a best-fitting absorption column of 9.2 (+2.9, -2.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 5.8 x 10^-11 (8.5 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 9.2 (+2.9, -2.5) x 10^21 cm^-2
Galactic foreground: 2.0 x 10^20 cm^-2
Excess significance: 6.0 sigma
Photon index: 1.63 (+0.27, -0.26)
If the light curve continues to decay with a power-law decay index of
1.91, the count rate at T+24 hours will be 5.4 x 10^-5 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-15 (4.6 x 10^-15) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00956824.
This circular is an official product of the Swift-XRT team.
GCN Circular 27117
Subject
GRB 200216B: Swift-BAT refined analysis
Date
2020-02-17T21:26:59Z (6 years ago)
From
Hans Krimm at NSF/NASA-GSFC <hkrimm@nsf.gov>
H. A. Krimm (NSF), S. D. Barthelmy (GSFC), P. D'Avanzo (INAF-OAB),
S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+908 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 200216B (trigger #956824)
(D'Avanzo, et al., GCN Circ. 27102). The BAT ground-calculated position is
RA, Dec = 160.452, 19.468 deg which is
RA(J2000) = 10h 41m 48.4s
Dec(J2000) = +19d 28' 05.5"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 84%.
The mask-weighted light curve shows a single bright pulse followed by some
extended emission. The main pulse has a FRED shape, starting at T-2 sec, peaking
around T+2 sec and decaying by T+18 sec. Lower-level extended emission with
some weak pulses lasts until around T+100 sec. T90 (15-350 keV) is 81.3 +- 13.0 sec
(estimated error including systematics).
The time-averaged spectrum from -0.72 to +100.33 sec is best fit by a power law
with an exponential cutoff. This fit gives a photon index 0.81 +- 0.52,
and Epeak of 47.6 +- 6.6 keV (chi squared 48.83 for 56 d.o.f.). For this
model the total fluence in the 15-150 keV band is 1.6 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+2.80 sec in the 15-150 keV band is
1.5 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index
of 1.90 +- 0.10 (chi squared 65.47 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/956824/BA/
GCN Circular 27114
Subject
GRB 200216B - possible IR counterpart from VLT
Date
2020-02-17T11:37:45Z (6 years ago)
From
Andrew Levan at U.of Leicester <a.levan@astro.ru.nl>
A. J. Levan (Radboud Univ), A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. Xu (NAOC), D. A. Kann (HETH-IAA/CSIC), J. P. U. Fynbo (DAWN/NBI/DTU), K. E. Heinz (Univ. Iceland), N. R. Tanvir (Univ. Leicester), G. Pugliese (API, Univ. Amsterdam), D. H. Hartmann (Clemson University) report on behalf of the Stargate Consortium:
"We observed the localisation of GRB 200216B (D���Avanzo et al. GCN 27102) with the Very Large Telescope and the HAWK-I instrument in the JHK bands beginning on 17 Feb 2020 at 02:44 UT, approximately 13.2 hours after the burst.
In our K-band images we identify a candidate IR counterpart within the refined XRT localisation (Goad et al. GCN 27106). The location of the source is
RA(J2000) 10:41:44.28
DEC(J2000) 19:28:31.3
With an uncertainty of ~0.3���.
The source has a magnitude of K(AB)~22. The source is not well detected in either the J or H-band observations, but the depths are such that these observations offer limited constraints on the colour of the source. Given the inferred high X-ray column a high redshift origin is unlikely. We cannot make any statements regarding variability at this stage.
We thank the staff at the VLT, in particular Bin Yang and Trystyn Berg for their work in acquiring these data."
GCN Circular 27110
Subject
GRB 200216B: z-band limit from NOT
Date
2020-02-17T01:20:29Z (6 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Martikainen (NOT and
U. Helsinki), D. Perley (LJMU), K.E. Heintz (U. Iceland), D. Xu (NAOC),
A. Levan (Radboud U.) report on behalf of a larger collaboration:
We observed the field of GRB 200216B (Fermi GBM team GCN
27101; D���Avanzo et al. GCN 27102) with the 2.5 m Nordic Optical
Telescope equipped with AlFOSC. Observations consisted of 5x200s
imaging in z-band, with mean epoch 17 Feb 2020 00:11:22 UT
(10.647 hr after the burst). We do not detect any source within the
refined XRT error box (Goad et al. GCN 27106) down to a 3-sigma
limit of z > 23.3 mag.
GCN Circular 27109
Subject
GRB 200216B: Fermi GBM observation
Date
2020-02-16T23:24:33Z (6 years ago)
From
Christian Malacaria at NASA-MSFC/USRA <cmalacaria@usra.edu>
C. Malacaria (NASA-MSFC/USRA), B. Mailyan (UAH) and C. Meegan (UAH),
report on behalf of the Fermi GBM Team:
"At 13:32:34.75 UT on 16 February 2020, the Fermi
Gamma-ray Burst Monitor (GBM)
triggered and located GRB 200216B (trigger 603552759 / 200216564),
which also triggered the Swift/BAT (D'Avanzo et al. 2020, GCN 27102).
The Fermi GBM Final Real-time Localization (GCN 27101)
is consistent with the Swift position.
The angle from the Fermi LAT boresight is 78 degrees.
The GBM light curve consists of a single bright pulse followed by
some extended emission with a duration (T90)
of about 12.0 s (10-1000 keV). The time-averaged spectrum
from T0-1.0 to T0+15.4 s is best fit by by a power law function
with an exponential high-energy cutoff.
The power law index is 0.07 +/- 0.30, and
the cutoff energy, parameterized as Epeak, is 69.5 +/- 4.9 keV.
The fluence (10-1000 keV) in this time interval
is (1.141 +/- 0.074)E-06 erg/cm^2.
The 1-sec peak photon flux measured starting from T0+2.3 s
in the 10-1000 keV band is 1.95 +/- 0.2 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official
Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN Circular 27108
Subject
GRB 200216B: Swift/UVOT Upper Limits
Date
2020-02-16T22:15:58Z (6 years ago)
From
Paul Kuin at MSSL <npkuin@gmail.com>
N. P. M. Kuin (UCL-MSSL) and P. D'Avanzo (INAF-OAB) report on
behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 200216B
124 s after the BAT trigger (D'Avanzo et al., GCN Circ. 27102). No optical
afterglow consistent with the XRT position (Goad et al. GCN Circ. 27106)
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 124 274 147 >21.0
white 124 1535 334 >21.5
w1 1095 1635 39 >20.2
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).
GCN Circular 27106
Subject
GRB 200216B: Enhanced Swift-XRT position
Date
2020-02-16T19:50:33Z (6 years ago)
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 1480 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 200216B, 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 = 160.43469, +19.47516 which is equivalent
to:
RA (J2000): 10h 41m 44.32s
Dec (J2000): +19d 28' 30.6"
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.
GCN Circular 27104
Subject
GRB 200216B: Nanshan/NEXT early optical upper limit and possible host galaxy
Date
2020-02-16T15:09:41Z (6 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
D. Xu, Z.P. Zhu, X. Liu, B.Y. Yu, Y. Ma (NAOC), X. Gao (Urumqi No.1
Senior High School) report:
We observed the field of GRB 200216B (D'Avanzo et al., GCN 27102) using
the NEXT 0.6m optical telescope located at Nanshan, Xinjiang, China.
Observations automatically started at 13:33:46 UT on 2002-02-16, i.e.,
73 s after the BAT trigger. We obtained 3x40 s, 4x60 s, 3x90 s and
onging 200 s frames in the Sloan r-filter. The altitude for the GRB and
the weather has been improving.
No optical afterglow is detected in our images at the XRT position
(D'Avanzo et al., GCN 27102) down to a limiting magnitude of r~20.0.
Meanwhile, we note that there exists a very marginally detected blob
(thus noise fluctuation not ruled out yet), extended and being
positionally consistent with the XRT position both in PanSTAR r-band
field, centred at coordinates: R.A. (J2000) = 10:41:44.23, Dec. (J2000)
= +19:28:33.18. The source would be of r~23 in depth, and might be the
host galaxy of the GRB. Deep imaging would identify the nature of the blob.
GCN Circular 27103
Subject
GRB 200216B: GMG upper limit
Date
2020-02-16T14:36:13Z (6 years ago)
From
Jirong Mao at Yunnan Obs <jirongmao_obs@ynao.ac.cn>
J. Mao, D.-Q. Wang, and J.-M. Bai (YNAO) report:
We observed the field of GRB 200216B (D'Avanzo et al. GCN circ. 27102) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 13:46:56, 16th, Feb, 2020, about 14 min after the trigger. We did not detect any optical source in the Swift-XRT error circle. A preliminary measurement provided an upper limit of R~21.8.
GCN Circular 27102
Subject
GRB 200216B: Swift detection of a burst
Date
2020-02-16T13:57:44Z (6 years ago)
From
Paolo D'Avanzo at INAF - OAB <paolo.davanzo@inaf.it>
P. D'Avanzo (INAF-OAB), M. G. Bernardini (INAF-OAB), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
T. Sbarrato (INAF-OAB) and A. Tohuvavohu (U Toronto) report on behalf
of the Neil Gehrels Swift Observatory Team:
At 13:32:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200216B (trigger=956824). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 160.461, +19.454 which is
RA(J2000) = 10h 41m 51s
Dec(J2000) = +19d 27' 15"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed one long peak
with a duration of about 30 sec, there is possible evidence for weaker
emission out to T0+60 seconds. The peak count rate was ~2000 counts/sec
(15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 13:34:29.0 UT, 115.1 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
160.4343, 19.4757 which is equivalent to:
RA(J2000) = 10h 41m 44.23s
Dec(J2000) = +19d 28' 32.4"
with an uncertainty of 2.0 arcseconds (radius, 90% containment). This
location is 119 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 (2.03 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 9.9
(+3.22/-2.80) x 10^21 cm^-2 (90% confidence).
The initial flux in the 2.5 s image was 1.33e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 124 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.02.
Burst Advocate for this burst is P. D'Avanzo (paolo.davanzo AT inaf.it).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)
GCN Circular 27101
Subject
GRB 200216B: Fermi GBM Final Real-time Localization
Date
2020-02-16T13:42:51Z (6 years ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
The Fermi GBM team reports the detection of a likely LONG GRB
At 13:32:34 UT on 16 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200216B (trigger 603552759.75478 / 200216564).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 159.2, Dec = 21.0 (J2000 degrees, equivalent to J2000 10h 36m, 21d 00'), with a statistical uncertainty of 6.5 degrees.
The angle from the Fermi LAT boresight is 78.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200216564/quicklook/glg_skymap_all_bn200216564.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/bn200216564/quicklook/glg_healpix_all_bn200216564.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200216564/quicklook/glg_lc_medres34_bn200216564.gif