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GCN Circular 30780

Konus-Wind detection of GRB 210905A
2021-09-06T15:08:33Z (3 years ago)
Dmitry Frederiks at Ioffe Institute <>
D. Frederiks, S. Golenetskii, A.Lysenko, D. Svinkin,
A. Ridnaya, A. Tsvetkova,  M. Ulanov, and T. Cline, report:

The long GRB GRB 210905A (Swift-BAT detection: Sonbas et al., GCN 30765;
Fermi GBM Sub-Threshold Detection: Veres & Roberts, GCN 30779),
T0 (BAT) = 00:12:41, was detected by Konus-Wind (KW) in the waiting mode.

A Bayesian block analysis of the KW waiting mode data in reveals
two major emission episodes, separated by ~750 s.
The first episode, from ~T0-25.5s to ~t0+13 s, corresponds to the BAT and GBM detections;
and the second episode, from ~T0-750 s to ~t0+870 s, corresponds to a bright flare visible
in the XRT light curve ( ).

The KW light curve of this burst is available

Modeling the KW 3-channel spectrum of the first episode
by a power law with exponential cutoff (CPL) model
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.45 (-0.24, + 0.38) and Ep = 203 (-58,+111) keV.
The spectrum of the second episode can be described by a CPL
with alpha = -0.88 (-0.30, + 0.76) and Ep = 167 (-61,+88) keV.

In the 10 keV -10 MeV band, standard for the KW analysis,
the total burst fluence is (1.7 �� 0.7)x10^-5 erg/cm^2,
and the 2.944 s peak energy flux is (3.6 �� 0.7)x10^-7 erg/cm^2.

Assuming the redshift z=6.318 (Tanvir et al., GCN 30771)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the isotropic energy release E_iso to ~1.1x10^54 erg,
the isotropic luminosity L_iso to ~1.7x10^53 erg/s,
and the rest-frame peak energy of the time-integrated spectrum Ep,z to ~1300 keV.
With these values, GRB 210905A lies within 68% prediction bands for
for both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW GRBs
with known redshifts (Tsvetkova et al., 2021, ApJ, 908, 83),

All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.
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