GRB 200219A

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

At 07:36:49 UT on 19 Feb 2020, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 200219A (trigger 603790614.095852 / 200219317).

The on-ground calculated location, using the Fermi GBM trigger data, is RA = 344.1, Dec = -60.0 (J2000 degrees, equivalent to J2000 22h 56m, -60d 00'), with a statistical uncertainty of 13.9 degrees.

The angle from the Fermi LAT boresight is 48.0 degrees.

The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200219317/quicklook/glg_skymap_all_bn200219317.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/bn200219317/quicklook/glg_healpix_all_bn200219317.fit

The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2020/bn200219317/quicklook/glg_lc_medres34_bn200219317.gif

A. Y. Lien (GSFC/UMBC), E. Ambrosi (INAF-IASFPA),
A. D'Ai (INAF-IASFPA), J. A. Kennea (PSU), N. J. Klingler (PSU),
K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 07:36:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 200219A (trigger=957271).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 342.644, -59.108 which is 
   RA(J2000) = 22h 50m 35s
   Dec(J2000) = -59d 06' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single
peak with a duration of about 1 sec.  The peak count rate
was ~15000 counts/sec (15-350 keV), at ~0.3 sec after the trigger. 

The XRT began observing the field at 07:37:56.6 UT, 67.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
342.6376, -59.1200 which is equivalent to:
   RA(J2000)  = 22h 50m 33.02s
   Dec(J2000) = -59d 07' 11.8"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 44 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 (1.93 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 6.1
(+3.05/-2.63) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 4.22e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 74 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 A. Y. Lien (amy.y.lien AT nasa.gov). 
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/)

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

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

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),

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

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

MASTER Global Robotic Net Catalog System  (http://observ.pereplet.ru, 
Lipunov et 
al.,  2010,Advances in Astronomy,v. 2010, 30L)
reducted  GRB 200219A (Lien et al. GCN 27125
Loading...
 
 , Lipunov et al GCN 
27124
Loading...
 
 ) XRT error box.

It found possible Host Galaxy in 1 sec from XRT center error box:

  	The Guide Star Catalog,  	WISE All-Sky Data Release (Cutri+ 
2012) 	AllWISE Data Release (Cutri+ 2013), The VISTA Hemisphere Survey 
(VHS) catalog DR4.1 (McMahon+, 2013)

RA,DEC (AllWISE) coordinates
22 50 33.023904	-59 07 10.83396

This message can be used.

E. Bissaldi (Politecnico and INFN Bari) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:


"At 07:36:49.10 UT on 19 February 2020, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 200219A (trigger 603790614/200219317),
which was also detected by the Swift/BAT (Lien et al. 2020, GCN 27125
Loading...
 
 ).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 49 degrees.

The GBM light curve consists of a single emission episode
with a duration (T90) of about 1.1 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.448 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.60 +/- 0.06 and
the cutoff energy, parameterized as Epeak, is 1.4 +/- 0.2 MeV.

The event fluence (10-1000 keV) in this time interval is
(2.8 +/- 0.1)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.192 s in the 10-1000 keV band
is 16.1 +/- 1.1 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/"

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 1921 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 200219A, 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 = 342.63837, -59.11954 which is equivalent
to:

RA (J2000): 22h 50m 33.21s
Dec (J2000): -59d 07' 10.4"

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.

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Tohuvavohu (U. Toronto), B.
Sbarufatti (PSU), D.N. Burrows (PSU), A.P. Beardmore (U. Leicester),
P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri
(INAF-OAB) and A.Y. Lien report on behalf of the Swift-XRT team:

We have analysed 6.7 ks of XRT data for GRB 200219A (Lien et al. GCN
Circ. 27125
Loading...
 
 ), from 57 s to 13.6 ks after the  BAT trigger. The data
comprise 28 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 Osborne et
al. (GCN Circ. 27138
Loading...
 
 ). We cannot determine at the present time whether
the source is fading.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00957271.

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

A. D'Ai (INAF-IASFPA), B. Sbarufatti (PSU), D.N. Burrows (PSU), J. D.
Gropp (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.
Melandri (INAF-OAB), T. Sbarrato (INAF-OAB) and A. Y. Lien (GSFC/UMBC)
report on behalf of the Swift-XRT team:

We have analysed 9.8 ks of XRT data for GRB 200219A (Lien et al. GCN
Circ. 27125
Loading...
 
 ), from 57 s to 24.9 ks after the  BAT trigger. The data
comprise 165 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 Osborne et
al. (GCN Circ. 27138
Loading...
 
 ).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.10 (+/-0.16). At T+136 s  the decay
steepens to an alpha of 4.7 (+3.3, -0.4) before breaking again at T+444
s to a final decay with index alpha=1.2 (+0.4, -0.6).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 1.36 (+/-0.06). The
best-fitting absorption column is  1.26 (+0.26, -0.24) x 10^21 cm^-2,
in excess of 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 4.9 x 10^-11 (5.4 x 10^-11) erg
cm^-2 count^-1. 

A summary of the WT-mode spectrum is thus:
Total column:	     1.26 (+0.26, -0.24) x 10^21 cm^-2
Galactic foreground: 1.9 x 10^20 cm^-2
Excess significance: 7.2 sigma
Photon index:	     1.36 (+/-0.06)

If the light curve continues to decay with a power-law decay index of
1.2, the count rate at T+24 hours will be 2.1 x 10^-4 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-14 (1.1 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/00957271.

Due to data delivery problems, the GCN Circ. 27139
Loading...
 
  (D'Elia et al.) was
sent while the analysis was still running, which is why it was
incomplete.

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

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),
J. P. Norris (BSU), 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+962 sec from the recent telemetry
downlink,
we report further analysis of BAT GRB 200219A (trigger #957271)
(Lien et al., GCN Circ. 27125
Loading...
 
 ).  The BAT ground-calculated position is
RA, Dec = 342.595, -59.101 deg which is
   RA(J2000)  =  22h 50m 22.7s
   Dec(J2000) = -59d 06' 04.5"
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.

The mask-weighted light curve shows a short pulse that starts and peaks at
~T0,
and ends at ~T+0.5 s. It is followed by an extended emission that lasting
until ~T+90 s. In addition, there may be some even weaker emission until
~T+300 s.
T90 (15-350 keV) is 288.0 +- 50.6 sec (estimated error including
systematics).

The time-averaged spectrum from T-0.2 to T+86.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.47 +- 0.25.  The fluence in the 15-150 keV band is 7.4 +- 1.1 x 10^-7
erg/cm2.
The 1-sec peak photon flux measured from T-0.268 sec in the 15-150 keV band
is 2.4 +- 0.2 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level.

Because the burst seems to be similar to short GRBs with extended emission,
we perform further spectral analysis for the short pulse and the extended
emission. The short pulse from T-0.224 s to T+0.496 s (determined by the
Bayesian block analysis) is best fit by a simple power-law model.
The power law index of the time-averaged spectrum is 0.69 +- 0.14. The
fluence in the 15-150 keV band is 2.5 +- 0.2 x 10^-7 erg/cm2.
The extended emission from T+0.496 s to T+86.704 s is best fit by a
simple power-law model. The power law index of the time-averaged
spectrum is 1.78 +- 0.33.  The fluence in the 15-150 keV band is
4.9 +- 1.0 x 10^-7 erg/cm2.

The spectral lag of the short pulse is 14 (+5, -5) ms for the 100-350 keV
to 25-50 keV bands, and 20 (+15, -10) ms for the 50-100 keV to 15-25 keV
bands. These values are more consistent with those of long GRBs.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/957271/BA/

Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ),
Martin Masek, Petr Janecek, Sergey Karpov, Jakub
Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and
Michael Prouza (Institute of Physics, Prague, CZ)

report:

The 30cm robotic telescope FRAM-Auger in Malargue
(Argentina) reacted robotically to the Swift/BAT alert
of GRB200219A (Lien et al., GCNC 27125, D'Elia et al.,
GCNC 27139, and Bissaldi et al., GCNC 27137), starting
with a series of 20s unfiltered images at 07:43:16 UT,
i.e. 6.45 min post trigger.

We do not detect any new or strongly variable source at
or around the reported gamma-ray errorbox at single
frames or a combined 20 x 20s image taken between 6.45
min and 15.39 min after the initial trigger. The
combined exposure has a limiting magnitude r'(AB) =
18.9, as calibrated against the APASS Catalogue.

M. H. Siegel (PSU) and A. Y. Lien (GSFC/UMBC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 200219A
75 s after the BAT trigger (Lien et al., GCN Circ. 27125
Loading...
 
 ).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 27138
Loading...
 
 )
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            75          225          147         >20.2
u_FC               287          537          246         >19.3
white               75        19365         1139         >21.2
v                  617        30839         1770         >19.7
b                  543        36572         2257         >20.9
u                  287        25105         2431         >20.7
w1                 666        40797         1248         >20.4
m2                 641        40734         2104         >20.4
w2                 592        28878          914         >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).

T. Sakamoto (AGU), E. Troja (NASA/GSFC/ORAU), J. Norris (BSU),
S. D. Barthelmy (GSFC), J. L. Racusin (GSFC), N. Kawai (Tokyo Tech),
A. Fruchter (STScI), M. Im (SNU)

A Chandra ToO observation of GRB 200219A (Lien et al., GCN Circ. 27125
Loading...
 
 ;
Bissaldi et al., GCN Circ. 27137
Loading...
 
 ) started on February 23 16:32 UT (~4.4 days
after the GRB trigger) for a total of 19.2 ksec.

We do not detect an X-ray afterglow at the location of the enhanced XRT position
(Osborne et al., GCN Circ. 27138
Loading...
 
 ).  The calculated 3-sigma upper limit is 3.3e-4 c/s
in the 0.35-8 keV band using aprates of the CIAO software package.
Using the best fit spectral parameters of the XRT PC mode data, we estimated
an 3-sigma unabsorbed flux upper limit of 5.0e-15 erg/cm2/s in the 0.35-8 keV band.

We would like to thank the Chandra operation team for rapidly approving and
making this observation.

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 200219A
(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 27123
Loading...
 
 ;
Bissaldi and Meegan, GCN Circ. 27137
Loading...
 
 ;
Swift-BAT detection: Lien et al., GCN Circ. 27125
Loading...
 
 ;
Laha et al., GCN Circ. 27148
Loading...
 
 )
triggered Konus-Wind at T0=27405.513 s UT (07:36:45.513).

The burst light curve shows a single multi-peaked pulse
which starts at ~T0-0.2 s and has a total duration of ~0.4 s.
The emission is seen up to ~8 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB200219_T27405/

As observed by Konus-Wind, the burst
had a fluence of 4.12(-0.61,+0.67)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.182 s,
of 2.34(-0.73,+0.76)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+0.256 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 = -0.06(-0.28,+0.35)
and Ep = 952(-173,+218) keV (chi2 = 29/27 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 = 29/26 dof).

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

D. d���Antonio (UTS), M. E. Bell (UTS), G. E. Anderson (Curtin), 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 200219A. The scheduled observations began on
2020 Feb 22.8 UT for 7.5 hours (3.5 days post-burst; Fermi GBM Team GCN
27123
Loading...
 
 , A. Y. Lien et al., GCN 27125
Loading...
 
 ). No radio source was detected at the XRT
position (J.P. Osborne et al., GCN 27138
Loading...
 
 ), with preliminary 3 sigma upper-limits
of 53 microJy and 57 microJy at 5.5 and 9 GHz, respectively.

We thank the ATCA and CSIRO Astronomy and Space Science (CASS) staff for
scheduling these observations.

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 the short GRB 200219A, which was also detected by Fermi GBM Final Real-time (GCN #27123
Loading...
 
 ), Swift (Lien A. et al., GCN #27125
Loading...
 
 ), MASTER (Tiurina N. et al., GCN #27126
Loading...
 
 ), Swift-BAT (Laha S. et al., GCN #27148
Loading...
 
 ), FRAM-Auger (Jelinek M. et al., GCN #27164
Loading...
 
 ), UVOT (Siegel M. et al., GCN #27165
Loading...
 
 ), Konus-Wind (Svinkin D. et al., GCN #27226
Loading...
 
 ) and ATCA 5/9 GHz (Antonio D. et al., GCN #27245
Loading...
 
 ).
The source was clearly detected in the 40-200 keV energy range. The light curve showed a single peak of emission peaking at 2020-02-19 07:36:49 UT. The measured peak count rate associated with the burst is 426 +/- 30.7 cts/s above the background in the combined data of four quadrants, with a total of 413 +/- 4.4 cts. The local mean background count rate was 489 +/- 2.2 cts/s. Using cumulative rates, we measure a T90 of 1.1 +/- 0.45 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.