GCN Circular 31544

A. Tsvetkova, D. Frederiks, A.Lysenko, D. Svinkin,
A. Ridnaia, M. Ulanov (all Ioffe), and A.Y. Lien (U Tampa), report:

The long GRB 211227A (Swift-BAT detection:
Beardmore et al., GCN 31316
Not found
 
 
; Lien et al., GCN 31326
Not found
 
 
;
MAXI/GSC detection: Tominaga et al., GCN 31319
Not found
 
 
;
CALET-GRBM detection: Cherry et al., GCN 31333
Not found
 
 
),
T0 (BAT) = 23:32:06.867, was detected by Konus-Wind (KW)
in the waiting mode.

A Bayesian block analysis of the KW waiting mode data in 25-400 keV range
reveals two episodes with count rate excess >10 sigma over background.
The first one, lasting from ~T0-50 s to ~T0-10 s, is due to the solar
activity and is not associated with the GRB.
The second episode, from ~T0-1.5 s to ~T0+81 s, is consistent in time
with the BAT detection. It has a double-peaked structure,
with the first, narrow pulse peaking at ~T0, and the second,
more broad pulse - at ~T0 + 11 s.

To derive broad-band spectral parameters of this burst,
we performed a joint spectral analysis of the Swift/BAT data (15-150 keV)
and the KW 3-channel spectral data (25-1700 keV).

A fit to the time-averaged spectrum, measured from T0-1.540 s�� to 
T0+83.836 s,
by the Band GRB function gives alpha = -1.34 (-0.08,+0.10),
beta = -2.26 (-1.11,+0.24), and Ep = 192 (-42,+45) keV; chi^2 = 48.5/ 57 
dof.

A fit to the spectrum near the peak KW count rate, measured from 
T0+10.236 s to T0+19.068 s,
by the Band function gives alpha = -1.09 (-0.07,+0.08), beta = -2.29 
(-0.11,+0.28),
and Ep = 374 (-70,+66) keV; chi^2 = 47.1/58 dof.

The spectrum of the short initial pulse, measured from T0-1.540 s to 
T0+4.348 s,
is well fit by a power law with an exponential cutoff (CPL), with
alpha = -1.56 (-0.06,+0.15) and Ep = 366 (-179,+1201) keV; chi^2 = 
49.3/59 dof.
Although the Band model fit to this spectrum is not constrained,
fixing beta to the value -2.26, obtained for the time-integrated spectrum,
gives alpha = -1.49 (-0.18, +0.24) and Ep = 240 (-116, +759) keV; chi^2 
= 49.0/59 dof.

In the 15-1500 keV band, the total burst fluence is 
2.60(-0.21,+0.21)x10^-5 erg/cm^2,
and the 64 ms peak energy flux is 2.0(-0.4,+0.4)x10^-6 erg/cm^2/s.

Assuming the redshift z=0.228 (Malesani et al., GCN 31324
Not found
 
 
)
of the host galaxy candidate (Fu et al., GCN 31320
Not found
 
 
),
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 4.9(-0.4,+0,4)x10^51 erg,
the isotropic luminosity L_iso to 4.7(-1.0,+1,0)x10^50 erg/s,
and the rest-frame peak energies of the time-integrated and peak spectra
to 235(-51,+56) keV and 460 (-86, +81) keV, correspondingly.
With these values, GRB 211227A is consistent with the 90% prediction 
bands for the 'Amati'
relation and is an outlier in the 'Yonetoku' relation for the sample of�� 
 >300 long KW GRBs
with known redshifts (Tsvetkova et al., 2021, ApJ, 908, 83).
However, if we assume a higher burst redshift (z>0.5), GRB 211227A is 
consistent
with both 'Amati' and 'Yonetoku' relations,
see http://www.ioffe.ru/LEA/GRBs/GRB211227A/GRB211227A_rest_frame.pdf

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

The KW light curve of this burst is available at 
http://www.ioffe.ru/LEA/GRBs/GRB211227A/