GRB 160219A

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa,
and A. Goldstein, on behalf of the Fermi GBM team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and

S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, report:

A short-duration GRB 160219A has been detected by Konus-Wind, Fremi 
(GBM; trigger 477557782), Swift (BAT), and INTEGRAL (SPI-ACS), so far, 
at about 24978 s UT (06:56:18). The burst was outside the coded field of 
view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box whose 
coordinates are:
--------------------------------
  RA(2000), deg    Dec(2000), deg
--------------------------------
Center:
    1.3524          -21.9573
Corners:
    352.3480        -23.1597
    350.3712        -23.9066
    9.4050          -15.0431
    7.6407          -16.0195
---------------------------------
The error box area is 18.39 sq. deg, and its maximum
dimension is 20.0 deg (the minimum one is 58 arcmin).
The Sun distance was about 20 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB160219_T24973/IPN/

The time history and spectrum will be given in forthcoming GCN Circulars.

H.-F. Yu (MPE) and O. J. Roberts (UCD), 
report on behalf of the Fermi GBM Team:

"At 06:56:18.14 UT on the 19th of February 2015, the Fermi 
Gamma-Ray Burst Monitor (GBM) triggered and located GRB 160219A 
(trigger 477557782 / 160219289). The on-ground calculated location, 
using the Fermi GBM trigger data, is RA = 350.6, Dec = -29.7 deg.
(J2000 degrees, equivalent to 23h 22m 24s, -29d 42'), with a 
statistical uncertainty of 6.34 degrees (radius, 1-sigma containment, 
statistical only; there is additionally a systematic error which we 
have characterized as a core-plus-tail model, with 90% of GRBs having 
a 3.7 deg error and a small tail suffering a larger than 10 deg 
systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ). 

The angle from the Fermi LAT boresight for the IPN position 
is 51 degrees (Svinkin et al. 2016, GCN 19035
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 ).

The GBM light curve consists of two short pulses with a duration
(T90) of about 3.5 s (50-300 keV). The time-averaged spectrum from
T0-0.064 s to T0+3.456 s is best fit by a power law function with
an exponential high-energy cutoff. The power law index is
-0.97 +/- 0.15 and the cutoff energy, parameterized as Epeak, is
689 +/- 308 keV.

The event fluence (10-1000 keV) in this time interval is
(1.25 +/- 0.12)E-06 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.00 s in the 10-1000 keV band is
19.2 +/- 1.1 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko,
and T. Cline, on behalf of the Konus-Wind team, report:

The short-duration, hard-spectrum GRB 160219A
(IPN triangulation: Svinkin et al., GCN 19035
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 ;
Fermi-GBM detection: Yu & Roberts, GCN 19041
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 )
triggered Konus-Wind at T0=24973.245 s UT (06:56:13.245).

The burst light curve starts with a short (~0.09 s) pulse,
followed by a weaker pulse at ~T0+3.1 s (with a duration of~0.96 s).

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB160219_T24973/

As observed by Konus-Wind, the burst had a fluence of
1.57(-0.21,+0.25)x10^-6 erg/cm2 and a 16-ms peak flux,
measured from ~T0-0.028 s, of 1.22(-0.27,+0.27)x10^-5 erg/cm2/s
(both in the 20 - 1200 keV energy range).

Since the bulk of the burst emission was detected before
the trigger, the spectral analysis was performed using
the KW 3-channel light curve data.

Modelling the K-W 3-channel spectrum of the first pulse
(measured from T0-0.066 s to T0+0.022 s)
by the cutoff power law yields the following model parameters:
the photon index alpha = -0.29(-0.37,+0.55),
and the peak energy Ep = 753(-187,+395) keV.

Modelling the K-W 3-channel spectrum of the second pulse
(measured from T0+3.072 s to T0+4.032 s)
by the cutoff power law yields the following model parameters:
the photon index alpha = -0.98(-0.22,+0.73),
and a lower limit on the Ep: Ep > 760 keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.