GRB 201116A
GCN Circular 28923
Subject
GRB 201116A: CALET Gamma-Ray Burst Monitor detection
Date
2020-11-19T09:01:00Z (5 years ago)
From
Valentin Pal'shin at AGU <val@phys.aoyama.ac.jp>
N. Cannady (GSFC/UMBC),
A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U), M. L. Cherry (LSU),
S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The bright GRB 201116A (Fermi GBM Final Real-time Localization: The Fermi
GBM team, GCN Circ. 28897; BALROG localization: Kunzweiler et al.,
GCN Circ. 28898; Fermi-LAT detection: Axelsson and Ohno, GCN Circ. 28907;
Konus-Wind detection: Ridnaia et al., GCN Circ. 28920;
https://gcn.gsfc.nasa.gov/other/201116A.gcn3) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 00:49:45.039 UTC on 16 November 2020
(http://cgbm.calet.jp/cgbm_trigger/flight/1289522797/).
The burst signal was seen by all CGBM detectors.
The burst light curve shows a multi-peaked pulse which starts at T+2.6
sec, peaks at T+7.9 sec, and ends at T+12.4 sec. The T90 and T50 durations
measured by the SGM data are 6.5 +- 0.6 sec and 3.0 +- 0.4 sec (40-1000
keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1289522797/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.
GCN Circular 28920
Subject
Konus-Wind detection of GRB 201116A
Date
2020-11-18T13:18:10Z (5 years ago)
From
Anna Ridnaia at Ioffe Institute <ridnaia@mail.ioffe.ru>
A. Ridnaia, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 201116A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 28897,
Kunzweiler et al., GCN Circ. 28898;
Fermi-LAT detection: Axelsson et al., GCN Circ. 28907)
triggered Konus-Wind at T0=2988.982 s UT (00:49:48.982).
The burst light curve shows a multipeaked structure
which starts at ~T0-1.3 s and has a total duration of ~9.5 s.
The emission is seen up to ~4 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB201116_T02988/
As observed by Konus-Wind, the burst
had a fluence of 2.46(-0.34,+0.33)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.792 s,
of 9.01(-2.15,+2.14)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+7.680 s)
is best fit in the 20 keV - 4 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.53(-0.23,+0.25),
the high energy photon index beta = -2.56(-0.69,+0.23),
the peak energy Ep = 220(-28,+40) keV
(chi2 = 90/97 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 28917
Subject
GRB 201116A: NOT optical observations
Date
2020-11-17T11:25:52Z (5 years ago)
From
Daniele B Malesani at DTU Space <malesani@space.dtu.dk>
Z.P. Zhu (NAOC, HUST), D. B. Malesani (DTU Space), D. Xu (NAOC), A. de
Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), L. Izzo (DARK/NBI), P. Galindo
(NOT), report on behalf of a larger collaboration:
On 2020 Nov 17, we observed the afterglow (de Ugarte Postigo et al., GCN
28915; Tohuvavohu�� et al., GCN 28916) of GRB 201116A, detected by
Fermi/GBM and Fermi/LAT (Axelsson et al., GCN 28907), using the Nordic
Optical Telescope (NOT) equipped with the ALFOSC camera. We obtained one
and three 300-s images in the r and z bands, respectively.
An optical source is detected in both filters, respectively, being
consistent with the reported OSN position as well as with the Swift/XRT
position. Preliminary photometry results are as follows:
������ T_start������������������ T_mid���� Exptime�� Filter���� Mag���� MagErr
�������� (UT)���������������������� (day)���� (s)
2020-11-17T04:33:15�� 1.157���� 1x300������ sdss-r���� 23.18 0.20
2020-11-17T04:38:51�� 1.165���� 3x300������ sdss-z���� 22.50 0.27
calibrated against nearby PS1 stars. Our observations confirm the
presence of the source, which is a clear afterglow candidate, though the
photometric error and short time difference do not allow to establish
variability compared to the OSN measurement (de Ugarte Postigo et al.,
GCN 28915).
GCN Circular 28916
Subject
GRB 201116A: Swift-XRT afterglow detection
Date
2020-11-17T08:48:42Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), T. Sbarrato (INAF-OAB), P.
D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), D.N. Burrows (PSU) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:
Swift-XRT has performed follow-up observations of the
Fermi/LAT-detected burst GRB 201116A (Axelsson et al. GCN Circ. 28907)
in a series of observations tiled on the sky. The total exposure time
is 4.8 ks, distributed over 3 tiles; the maximum exposure at a single
sky location was 3.1 ks. The data were collected between T0+46.5 ks and
T0+62.3 ks, and are entirely in Photon Counting (PC) mode.
Four uncatalogued X-ray sources are detected, of which one ("Source 3")
is above the RASS 3-sigma upper limit at this position, and shows
signes of fading, and is therefore likely the GRB afterglow. Using 2405
s of PC mode data and 4 UVOT images, we find an enhanced XRT position
(using the XRT-UVOT alignment and matching UVOT field sources to the
USNO-B1 catalogue): RA, Dec = 149.32493, +0.27586 which is equivalent
to:
RA (J2000): 09h 57m 17.98s
Dec(J2000): +00d 16' 33.1"
with an uncertainty of 2.5 arcsec (radius, 90% confidence). This
position is 2.4 arcmin from the Fermi/LAT position. As already
reported by de Ugarte Postigo et al (GCN Circ. 28915), there is an
optical afterglow counterpart consistent with this X-ray object. The
light curve is consistent with a constant source of mean count rate
5.2e-02 ct/sec, however fading also cannot be ruled out. A power-law
fit gives an index of 1.6 (+1.4, -2.0), thus the large uncertainties
hinder a confident statement about fading.
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.9 (+0.6, -0.5). The
best-fitting absorption column is 2.7 (+2.5, -1.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.8 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum is 3.2 x 10^-11 (4.4 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 2.7 (+2.5, -1.9) x 10^21 cm^-2
Galactic foreground: 2.8 x 10^20 cm^-2
Excess significance: 2.1 sigma
Photon index: 1.9 (+0.6, -0.5)
The results of the XRT-team automatic analysis of the afterglow are at:
https://www.swift.ac.uk/xrt_products/00021040.
The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00095.
This circular is an official product of the Swift-XRT team.
GCN Circular 28915
Subject
GRB 201116A: OSN Afterglow Candidate
Date
2020-11-17T04:36:25Z (5 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D. A. Kann, M. Blazek,
C. C. Thoene, J. F. Agui Fernandez (all HETH/IAA-CSIC), and A. Sota
(IAA-CSIC) report:
We observed the location of the Swift XRT source #3 found in tiled Swift
observations (Evans, GCN #28906), potentially the (X-ray) afterglow of
Fermi GBM/LAT GRB 201116A (Fermi GBM Team, GCN #28897; Kunzweiler et
al., GCN #28898; Axelsson et al., GCN #28907) with the 1.5m telescope of
the Observatorio Sierra Nevada, in Granada, Spain. We obtained 15 x 180
s images in Rc, beginning 2020-11-17 03:24:46.56 UT, 1.1076 days after
the GRB.
We detect a faint source in the Rc-band stack at (J2000)
RA = 09:57:17.94
Dec. = +00:16:34.1
with Rc = 23.18 +/ 0.18 mag (AB), as measured against multiple SDSS
comparison stars.
This source is not visible in SDSS or PanSTARRS imaging, suggesting it
is the GRB afterglow. We cannot determine evidence for fading, however.
We wish to congratulate the SpaceX Crew-1 astronauts for their
successful arrival at the ISS.
GCN Circular 28907
Subject
GRB 201116A: Fermi-LAT detection
Date
2020-11-16T14:09:02Z (5 years ago)
From
Frederic Piron at CNRS/IN2P3/LUPM <piron@in2p3.fr>
M. Axelsson (KTH & Stockholm Univ.), M. Ohno (Hiroshima Univ. & Eotvos
Univ.),
E. Bissaldi (Politecnico & INFN Bari), F. Longo (University and INFN,
Trieste) and
F. Piron (CNRS/IN2P3/LUPM) report on behalf of the Fermi-LAT Collaboration:
On November 16, 2020 Fermi-LAT detected high-energy emission from
GRB 201116A, which was also detected by Fermi-GBM (trigger 627180592,
GCN 28897).
The best LAT on-ground location is found to be
RA, Dec 149.33, 0.32 (degrees, J2000)
with an error radius of 0.24 deg (90% containment, statistical error only).
This was 14 deg from the LAT boresight at the time of the GBM trigger:
T0 = 00:49:47 UT.
The data from the Fermi-LAT show a significant increase
in the event rate after the GBM trigger that is spatially correlated
with the
GBM emission (4 degrees from the GBM location) with high significance.
The photon flux above 100 MeV in the time interval 0-1000s after the
GBM trigger is (2.25+/-0.07)e-06 ph/cm2/s.
The estimated photon index above 100 MeV is -1.9 +/- 0.3.
The highest-energy photon is a 2.4 GeV event which is observed 82
seconds after the GBM trigger.
A Swift ToO has been approved for this burst.
The Fermi-LAT point of contact for this burst is
Frederic Piron (piron@in2p3.fr).
The Fermi-LAT is a pair conversion telescope designed to cover
the energy band from 20 MeV to greater than 300 GeV.
It is the product of an international collaboration between
NASA and DOE in the U.S. and many scientific institutions
across France, Italy, Japan and Sweden.
GCN Circular 28906
Subject
GRB 201116A: Tiled Swift observations
Date
2020-11-16T13:43:44Z (5 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. A. Evans (U. Leicester) reports on behalf of the Swift team:
Swift has initiated a series of observations, tiled on the sky, of the
Fermi/LAT GRB 201116A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00095
Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.
Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).
This circular is an official product of the Swift-XRT team.
GCN Circular 28898
Subject
GRB 201116A: BALROG localization (Fermi Trigger 627180592 / GRB 201116035)
Date
2020-11-16T01:14:14Z (5 years ago)
From
Jochen Greiner at MPE,Garching <jcg@mpe.mpg.de>
F. Kunzweiler, B. Biltzinger, F. Berlato, J. Burgess & J. Greiner (all MPE Garching) report:
The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
627180592 at 00:49:47 on 16 Nov. 2020 were automatically fitted for spectrum
and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;
Berlato et al. 2019, ApJ 873, 60).
The best-fit position (1 sigma statistical errors) is:
RA(2000.0) = 148.42+/-0.33 deg
Decl.(2000.0) = 2.46+/-0.57 deg
We estimate an additional systematic error of 1 deg.
Further details are available at:
https://grb.mpe.mpg.de/grb/GRB201116035/
The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB201116035/healpix
The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB201116035/json
GCN Circular 28897
Subject
GRB 201116A: Fermi GBM Final Real-time Localization
Date
2020-11-16T01:00:12Z (5 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 00:49:47 UT on 16 Nov 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 201116A (trigger 627180592.69203 / 201116035).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 149.5, Dec = -4.2 (J2000 degrees, equivalent to J2000 09h 58m, -4d 12'), with a statistical uncertainty of 1.0 degrees.
The angle from the Fermi LAT boresight is 14.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201116035/quicklook/glg_skymap_all_bn201116035.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201116035/quicklook/glg_healpix_all_bn201116035.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn201116035/quicklook/glg_lc_medres34_bn201116035.gif