GRB 200219C
GCN Circular 27298
Subject
GRB 200219C: VLA Detection
Date
2020-03-03T03:29:34Z (6 years ago)
From
Virginia Cunningham at U of MD <vcunning@astro.umd.edu>
V. Cunningham (UMD), S. B. Cenko (NASA GSFC), S. Vogel (UMD)
We observed the Fermi GBM/LAT GRB 200219C (The Fermi GBM Team,
GCN 27145; Dirirsa et al., GCN 27151; Hamburg et al., GCN 27155) at 6 GHz
with the Karl G. Jansky Very Large Array (VLA) on 2020 Feb 25 11:23:02 UTC
(5.48 days post GBM trigger). We report a preliminary flux density of ~658 uJy
at position:
RA (J2000): 17:30:02.295 +/- 0.011
Dec (J2000): +10:32:22.237 +/- 0.011
This is consistent with the position of the potential host galaxy (Xu
et al., GCN
27161), optical afterglow (Reva et al., GCN 27162; Blazek et al., GCN 27166),
and X-ray afterglow (Burrows et al., GCN 27157).
We thank the VLA staff for their assistance in completing these observations.
GCN Circular 27228
Subject
Konus-Wind observation of GRB 200219C
Date
2020-02-26T19:03:50Z (6 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Ridnaia, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 200219C
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27145;
Hamburg et al., GCN Circ. 27155;
Fermi-LAT detection: Dirirsa et al., GCN Circ. 27151;
CALET-GBM detection: Sugita et al., GCN Circ. 27163)
triggered Konus-Wind at T0=86229.162 s UT (23:57:09.162).
The burst light curve shows a bright peak which starts at ~T0-3.4 s
and has a duration of ~9.8 s, followed by a weaker emission
seen up to ~T0+23 s. Total burst duration is ~27 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/GRB200219_T86229
As observed by Konus-Wind, the burst
had a fluence of 1.87(-0.11,+0.13)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+3.488 s,
of 5.40(-1.08,+1.23)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+29.952 s)
is best fit in the 20 keV - 2 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.08(-0.12,+0.12)
and Ep = 209(-21,+27) keV (chi2 = 60/61 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 60/60 dof).
The spectrum near the maximum count rate
(measured from T0+0.256 to T0+5.376 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 = -0.83(-0.10,+0.12),
the high energy photon index beta = -3.58(-6.42,+0.82),
the peak energy Ep = 234(-22,+20) keV
(chi2 = 62/75 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 27180
Subject
GRB 200219C: Swift-XRT afterglow confirmation
Date
2020-02-24T21:22:36Z (6 years ago)
From
Valerio D'Elia at ASDC <valerio.delia@ssdc.asi.it>
V. D���Elia (SSDC) reports on behalf of the Swift-XRT team:
We provide an update on the XRT light curve evolution of the candidate X-ray afterglow of GRB 200219C (GCN Circ. 27157).
The XRT light curve now comprises data up to 260 ks from the Fermi trigger (GCN Circs. 27151 and 27155). There is a firm indication of fading with respect to the first observation, with a decay index of 0.8 (+0.4 -0.3). We thus confirm that this is indeed the afterglow of GRB 200219C.
The latest results can be viewed via: https://www.swift.ac.uk/xrt_curves/00020973/ <https://eur02.safelinks.protection.outlook.com/?url=https%3A%2F%2Fwww.swift.ac.uk%2Fxrt_curves%2F00020973%2F&data=02%7C01%7Cvalerio.delia%40ssdc.asi.it%7Ccbb05988e1604c1b0a9608d7b9502580%7Ccbfc58d4e60f468d8fe490676de085f7%7C0%7C0%7C637181626207379817&sdata=y0NsJNyq79oZqD4RZJb5be%2Fwwkz6UNNz%2B%2F3wajd%2Bs54%3D&reserved=0>
This circular is an official product of the Swift-XRT team.
GCN Circular 27166
Subject
GRB 200219C: OAJ afterglow confirmation
Date
2020-02-21T20:03:17Z (6 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
M. Blazek, D. A. Kann (both HETH/IAA-CSIC), A. de Ugarte Postigo
(HETH/IAA-CSIC, DARK/NBI), C. C. Thoene, J. F. Agui Fernandez (both
HETH/IAA-CSIC), N. Maicas, and J. L. Lamadrid (both CEFCA) report:
We observed the position of the Fermi GBM/LAT GRB 200219C (Fermi GBM
team, GCN #27145, Hamburg et al., GCN #27155, Dirirsa et al., GCN
#27151) with the Javalambre Observatory OAJ 80cm telescope in g'r'i'z',
obtaining 3 x 300 s exposures in g'r' each, and 5 x 180 s exposures in
i'z' each. Observations started on 2020-02-21, 03:17:55 UT. No
observations were obtained the night before as the LAT position came
only after twilight had started.
In the stacked r' image (midtime 1.14375 days after the GRB), we clearly
detect a source within the enhanced XRT error circle (Burrows et al.,
GCN #27157) for which we measure r'(AB) = 22.11 �� 0.13 mag against
PanSTARRS field stars.
We note this implies a decay compared with the afterglow discovery by
Reva et al. (GCN #27162) who find R ~ 21.72 �� 0.15 mag (AB) about six
hours earlier. It is still brighter than the PanSTARRS host galaxy
magnitude given by Xu et al. (GCN #27161) at r' = 22.70 �� 0.15 mag.
The relatively bright host galaxy may be indicative of a low-redshift
event. As the source is improving in visibility and will be observable
for several months to come, a search for associated supernova emission
may be worthwhile. Spectroscopy is encouraged.
GCN Circular 27163
Subject
GRB 200219C: CALET Gamma-Ray Burst Monitor detection
Date
2020-02-21T15:33:14Z (6 years ago)
From
Valentin Pal'shin at AGU <val@phys.aoyama.ac.jp>
S. Sugita, A. Yoshida, T. Sakamoto, V. Pal'shin (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), P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The long GRB 200219C (Fermi GBM detection: Fermi GBM Team,
GCN Circ. 27145, Hamburg et al., GCN Circ. 27155;
Fermi-LAT detection: Dirirsa et al., GCN Circ. 27151;
https://gcn.gsfc.nasa.gov/other/200219C.gcn3)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:57:10.630 UTC
on 19 February 2020. The burst signal was seen by only the SGM detector.
The burst light curve shows a multi-peaked pulse which starts at T+0.1 sec,
peaks at T+1.6 sec and ends at T+4.6 sec. The T90 and T50 durations
measured by the SGM data are 4.0 +- 0.7 sec and 2.1 +- 0.9 sec (40-1000
keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1266191565/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.
GCN Circular 27162
Subject
GRB 200219C: Mondy and TSHAO optical observations
Date
2020-02-21T10:54:35Z (6 years ago)
Edited On
2026-04-15T14:19:31Z (2 months ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Edited By
Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov>
I. Reva (FAPHI), A. Pozanenko (IKI), M. Krugov (FAPHI), with Zeiss-1000
1-m telescope of Tien Shan Astronomical Observatory
A. Pozanenko (IKI), S. Belkin (IKI), E. Klunko (ISTP), I. Reva (FAPHI),
M. Krugov (FAPHI), E. Mazaeva (IKI), A. Volnova (IKI) report on behalf
of IKI-GRB-FuN:
We observed the field of GRB 200219C (The Fermi GBM team, GCN 27145;
Dirirsa et al., GCN 27151; Hamburg et al., GCN 27155) with AZT-33IK
1.5-m telescope of Sayan observatory (Mondy) starting on Feb. 20 (UT)
21:21:45 and with Zeiss-1000 1-m telescope of Tien Shan Astronomical
Observatory starting on Feb. 20 (UT) 23:17:45. Within enhanced XRT
position of XRT afterglow (Burrows et al., GCN 27157) we detected an
optical object in coordinates of (J2000) 17:30:02.275 +10:32:22.47 with
uncertainities of 0.3 arcsec in both coordinates. Coordinates are
consistent with possible host galaxy (Xu et al., GCN 27161) which is
presented in Pan-STARRS catalaog. Preliminary photometry of the object
is following.
Date UT start t-T0 Filter Exp. OT Err UL(3sigma) telesope
(mid, days) (s)
2020-02-20 21:21:45 0.90596 R 40*60 21.55 0.15 22.2 AZT-33IK
2020-02-20 23:17:45 0.99207 R 56*60 n/d n/d 21.3 Z-1000
Photometry is based on the USNO-B2.0 nearby stars.
USNO-B1.0 R2
1005-0285285 17.74
1005-0285301 19.23
1005-0285213 19.99
The object is somewhat brighter than that presented in Pan-STARRS DR1,
and we suggest this object is a candidate for the afterglow of GRB 200115A.
GCN Circular 27161
Subject
GRB 200219C: Nanshan/NEXT optical upper limit and possible host galaxy from PanSTARRS
Date
2020-02-21T05:15:46Z (6 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
D. Xu, X. Liu, Z.P. Zhu, B.Y. Yu, Y. Ma (NAOC), X. Gao (Urumqi No.1
Senior High School) report:
We observed the field of the possible X-ray afterglow by Swift/XRT
(Burrows et al., GCN 27157) of GRB 200219C detected by Fermi/GBM and
Fermi/LAT (GCN 27145; Dirirsa et al., GCN 27151), using the 0.6m NEXT
telescope located at Nanshan, Xinjiang, China. Observations started at
22:45:55 UT on 2020-02-20 (i.e., 22.8 h after the Fermi trigger) and
10x300 s Sloan r-band frames were obtained.
No optical counterpart is detected in our stacked image at the Swift XRT
position, down to a limiting magnitude of r~21.0.
Inspection of PanSTARRS reveals a faint, extended source within the XRT
error circle. It's localized at coordinates: R.A. (J2000) = 17:30:02.21,
Dec.(J2000) = +10:32:22.69, and has r = 22.70 +/- 0.15 mag. Thus is may
be the host galaxy of the GRB, if the Swift XRT detection is the
afterglow of the GRB.
GCN Circular 27157
Subject
GRB 200219C: Swift-XRT afterglow detection
Date
2020-02-20T20:10:40Z (6 years ago)
From
Valerio D'Elia at ASDC <valerio.delia@ssdc.asi.it>
D.N. Burrows (PSU), J. D. Gropp (PSU), J.A. Kennea (PSU), J.P. Osborne
(U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), A. Melandri (INAF-OAB), T. Sbarrato (INAF-OAB), P. D'Avanzo
(INAF-OAB) and 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 200219C (Dirirsa et al. GCN Circ. 27151)
in a series of observations tiled on the sky. The total exposure time
is 2.4 ks, distributed over 4 tiles; the maximum exposure at a single
sky location was 2.4 ks. The data were collected between T0+43.0 ks and
T0+56.0 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 2417 s of PC mode data and 5 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 = 262.50899, +10.53933 which is
equivalent to:
RA (J2000): 17h 30m 02.16s
Dec(J2000): +10d 32' 21.6"
with an uncertainty of 2.1 arcsec (radius, 90% confidence). This
position is 12.9 arcmin from the Fermi/LAT position. The light curve
is consistent with a constant source of mean count rate 1.1e-01 ct/sec.
A power-law fit gives an index of 0.9 (+1.4, -1.5).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.1 (+/-0.4). The
best-fitting absorption column is 3.2 (+1.6, -1.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.2 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 3.1 x 10^-11 (4.9 x 10^-11) erg
cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 3.2 (+1.6, -1.4) x 10^21 cm^-2
Galactic foreground: 1.2 x 10^21 cm^-2
Excess significance: 2.4 sigma
Photon index: 2.1 (+/-0.4)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020973.
The results of the full analysis of the tiled XRT observations are
available at https://www.swift.ac.uk/xrt_products/TILED_GRB00088.
This circular is an official product of the Swift-XRT team.
GCN Circular 27156
Subject
GRB 200219C: DDOTI Observations
Date
2020-02-20T18:58:16Z (6 years ago)
From
Alan M Watson at UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Eleonora Troja (GSFC/UMD), Nat Butler (ASU),
William H. Lee (UNAM), Simone Dichiara (GSFC/UMD), Alexander Kutyrev
(GSFC/UMD), Margarita Pereyra (UNAM), Rosa L. Becerra (UNAM), Diego
Gonzalez (UNAM), and Tanner Wolfram (ASU) report:
We observed the field of 200219C, detected by both Fermi/GBM (Fermi GBM
Team, GCN Circ. 27145) and Fermi/LAT (Dirirsa et al., GCN Circ. 27151),
with the DDOTI/OAN wide-field imager at the Observatorio Astronomico
Nacional on Sierra San Pedro Martir (http://ddoti.astroscu.unam.mx) on
the night of 2020-02-20 UTC.
We observed from 2020-02-20 11:37 UTC to 2020-02-13 13:08 UTC (from 11.7
to 13.2 hours after the event) obtaining 72 minutes of exposure in the w
filter. We calibrate our images against the APASS catalog. Our 5-sigma
limiting magnitude is w = 20.4.
Comparing our observations to the USNO-B1 and PanSTARRS PS1 DR2
catalogs, we detect no uncatalogued sources in the Fermi/LAT error
region (Dirirsa et al., GCN Circ. 27151) to our 5-sigma limit.
The Fermi/LAT error includes the probably XRT afterglow candidate (Evans
et al., GCN Circ. 27152) at 17:30:02.34 +10:32:22.9 J2000 (source #2
at https://www.swift.ac.uk/xrt_products/TILED_GRB00088/). We see no
evidence for an optical counterpart at this position to our 5-sigma
limit.
We thank the staff of the Observatorio Astronomico Nacional in San Pedro
Martir.
GCN Circular 27155
Subject
GRB 200219C: Fermi GBM detection
Date
2020-02-20T17:06:32Z (6 years ago)
From
Rachel Hamburg at UAH <rkh0007@uah.edu>
R. Hamburg (UAH), C. Meegan (UAH) and E. Bissaldi (Politecnico and INFN
Bari)
report on behalf of the Fermi GBM Team:
"At 23:57:10.33 UT on 19 February 2020, the Fermi Gamma-Ray Burst Monitor
(GBM)
triggered and located GRB 200219C (trigger 603849435 / 200219998), which was
also detected by Fermi-LAT (Dirirsa et al. 2020, GCN 27151). The Fermi GBM
Final Real-time Localization (GCN 27145) is consistent with the LAT
position.
The GBM light curve shows a bright main peak followed by a weaker emission
episode and has a duration (T90) of about 22 s (50-300 keV).
The time-averaged spectrum from T0-0.00 s to T0+25.9 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.09 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 199 +/- 9 keV.
A Band function fits the spectrum equally well with
Epeak = 181 +/- 12 keV, alpha = -1.05 +/- 0.03 and beta = -2.50 +/- 0.24.
The event fluence (10-1000 keV) in this time interval is
(1.87 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+3.7 s in the 10-1000 keV band
is 24.8 +/- 0.4 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/"
GCN Circular 27152
Subject
GRB 200219C: Tiled Swift observations
Date
2020-02-20T12:01:20Z (6 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 200219C. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00088
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 27151
Subject
GRB 200219C: Fermi-LAT detection
Date
2020-02-20T07:49:00Z (6 years ago)
From
Makoto Arimoto at Tokyo Inst of Tech <arimoto@hp.phys.titech.ac.jp>
F. Dirirsa (Univ. of Johannesburg), M. Arimoto (Kanazawa Univ.), M.
Axelsson (KTH & Stockholm Univ.), F. Longo (University & INFN
Trieste), and N. Omodei (Stanford U.)
report on behalf of the Fermi-LAT Collaboration:
On February 19, 2020, Fermi-LAT detected high-energy emission from
GRB 200219C, which was also detected by Fermi-GBM (trigger
603849435/200219998, GCN 27145).
The best LAT on-ground location is found to be
RA, Dec = 262.7, 10.5 (degrees, J2000)
with an error radius of 0.24 deg (90% containment, statistical error only).
This was 43 deg from the LAT boresight at the time of the GBM trigger:
T0 = 23:57:10.3 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 (2.7 degrees from the GBM position) with high significance.
The photon flux above 100 MeV in the time interval 0-1500 s after the
GBM trigger is 2.2 +/- 0.8 e-6 ph/cm2/s.
The estimated photon index above 100 MeV is -2.1 +/- 0.3.
The highest-energy photon is a 1.17 GeV event which is observed 344.6 seconds
after the GBM trigger.
A Swift ToO has been requested for this burst.
The Fermi-LAT point of contact for this burst is
Feraol Fana Dirirsa (fdirirsa@uj.ac.za).
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 27145
Subject
GRB 200219C: Fermi GBM Final Real-time Localization
Date
2020-02-20T00:07:23Z (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 23:57:10 UT on 19 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200219C (trigger 603849435.33311 / 200219998).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 264.5, Dec = 8.4 (J2000 degrees, equivalent to J2000 17h 37m, 8d 24'), with a statistical uncertainty of 1.0 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/bn200219998/quicklook/glg_skymap_all_bn200219998.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/bn200219998/quicklook/glg_healpix_all_bn200219998.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200219998/quicklook/glg_lc_medres34_bn200219998.gif