A peculiarly short-duration gamma-ray burst from massive star core collapse
Gamma-ray bursts (GRBs) have been phenomenologically classified into long and short populations based on the observed bimodal distribution of duration1. Multi-wavelength and multi-messenger observations in recent years have revealed that in general long GRBs originate from massive star core collapse events2, whereas short GRBs originate from binary neutron star mergers3. It has been known that the duration criterion is sometimes unreliable, and multi-wavelength criteria are needed to identify the physical origin of a particular GRB4. Some apparently long GRBs have been suggested to have a neutron star merger origin5, whereas some apparently short GRBs have been attributed to genuinely long GRBs6 whose short, bright emission is slightly above the detector's sensitivity threshold. Here, we report the comprehensive analysis of the multi-wavelength data of the short, bright GRB 200826A. Characterized by a sharp pulse, this burst shows a duration of 1 second and no evidence of an underlying longer-duration event. Its other observational properties such as its spectral behaviours, total energy and host galaxy offset are, however, inconsistent with those of other short GRBs believed to originate from binary neutron star mergers. Rather, these properties resemble those of long GRBs. This burst confirms the existence of short-duration GRBs with stellar core-collapse origin4, and presents some challenges to the existing models. © 2021, The Author(s), under exclusive licence to Springer Nature Limited. ; B.-B.Z. acknowledges support by the National Key Research and Development Programs of China (2018YFA0404204), the National Natural Science Foundation of China (grant nos. 11833003 and U2038105) and the Innovative and Entrepreneurial Talent Program in Jiangsu. Y.-Z.M. is supported by the National Postdoctoral Program for Innovative Talents (grant no. BX20200164). This work was supported in part by the Natural Science Foundation of China (grant nos. U1831135 (X.-H.Z.), 11922301 (H.-J.L.), 12041306 (Y.L.) and U1938201 (X.-G.W.)), the Guangxi Science Foundation (2017GXNSFFA198008 (H.-J.L.), 2017AD22006 (X.-G.W.) and 2016GXNSFFA380006 (X.-G.W.)) and the Bagui Young Scholars Program (H.-J.L.). Part of this work is based on observations made with the GTC installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias, on the island of La Palma. We also acknowledge the use of public data from the Fermi Science Support Center. ; With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709. ; Peer reviewed