TITLE:   GCN CIRCULAR
NUMBER:  31648
SUBJECT: GRB 220101A: The first example of a Petanova
DATE:    22/02/25 11:38:50 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, Y. Aimuratov, L. Becerra, C.L. Bianco, Y-C. Chen, C. Cherubini,
Y.F. Cai, S. Eslamzadeh, S. Filippi, M. Karlica, Liang Li, G.J. Mathews, R.
Moradi, M. Muccino, G.B, Pisani, F. Rastegar Nia, J.A. Rueda, N. Sahakyan,
Y. Wang,  S.S. Xue,  Y.F. Yuan, Y.L. Zheng, on behalf of ICRA, ICRANet and
USTC team, report:

We confirm the results of our previous GCN (Ruffini et al. 2022, GCN
31465). Following the release of the X-ray afterglow (Tohuvavohu et al.
2022, GCN 31347) and the GeV data (Arimoto et al. 2022, GCN 31350) of this
source, we can estimate the total (keV+MeV+GeV) isotropic energy (see e.g.
Ruffini et al. 2021, MNRAS 504, 5301) to be ~6E54 erg, making this GRB the
most powerful GRB in 26 years (a "Petanova"). The period of the new neutron
star (see e.g. Ruffini et al. 2021, MNRAS 504, 5301) generating the X-ray
afterglow is ~1 ms, the initial mass of the BH (see e.g. Ruffini et al.
2019 ApJ 886, 82) is 6.15 solar mass, the spin parameter is 0.95, and the
irreducible mass is 4.98 solar masses (see Fig. 1). The peak of the
bolometric flux of supernova is of the order of 1E-17 erg/s/cm^2 and will
appear in 73+/-15 days after the GRB trigger, with emissions lasting ~ one
month peaking in different infrared bands. The observational follow up
of this source is encouraged.

Fig. 1: http://www.icranet.org/docs/GRB220101A.pdf