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arXiv · 2606.27037

Gamma-ray Bursts and Kilonovae from Gravitational Wave Events

Alberto Colombo·Marcello Giroletti·Susanna D. Vergani·Lauren Rhodes
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Abstract

The detection of gravitational waves (GWs) from binary black holes in 2015 and the joint GW-electromagnetic (EM) observation of the binary neutron star merger GW170817 set a milestone in the multimessenger era in astrophysics. After four observing runs by the LIGO, Virgo, and KAGRA interferometers, a new cycle is planned for 2028, paving the way for next-generation detectors in the 2030s -- such as the Einstein Telescope, Cosmic Explorer, and LISA. The prospects for joint GW-EM studies, including kilonova searches in wide optical surveys, are vast but demanding. In the radio domain, connected interferometers and VLBI arrays have already proven essential in constraining the ejecta properties of GW170817. Radio emission from gamma-ray burst (GRB) afterglows, whether on- or off-axis, remains detectable for very long time, making radio observations the most effective method for identifying and tracking GW merger counterparts. These observations enable precise characterization of system evolution, detailed probing of GRB jet structures, and possible detection of misaligned jets once their velocity becomes non-relativistic. Even in its initial configuration (AA*), the SKAO will provide the sensitivity and field of view needed to complement GW counterpart searches during O5 and beyond, offering unmatched capabilities for long-term monitoring. Furthermore, independent of the GW detections, SKAO will enable population studies of the properties of both long (produced by the collapse of massive stars) and short (produced by the merger of neutron stars) GRBs, of their jets and of their environment. We present an overview of this evolving observational landscape and of the key scientific questions SKAO will address.

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Alberto Colombo, Marcello Giroletti, Susanna D. Vergani, Lauren Rhodes. 2026-06-25. Gamma-ray Bursts and Kilonovae from Gravitational Wave Events. https://arxiv.org/abs/2606.27037

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