Optimal observational strategies for kilonovae and jet afterglows

Determine the optimal observational strategy—including cadence, sensitivity, filter choices, and telescope selection—for discovering and following up kilonova emission and relativistic jet afterglows associated with compact binary mergers, so as to maximize identification and characterization of these counterparts across the electromagnetic spectrum.

Background

The paper studies the detectability of prompt emission and afterglows from relativistic jets launched by binary neutron star mergers detected by current (LVK O5) and next-generation (Cosmic Explorer and Einstein Telescope) gravitational-wave detectors. Because electromagnetic counterparts can occur across X-ray, ultraviolet, optical/infrared, and radio wavelengths, devising effective observing plans is essential to maximize scientific return.

The authors simulate afterglow light curves under a range of jet structures and microphysical parameters and compare them to sensitivities of numerous facilities. Despite these efforts, they note that selecting the ideal observing strategy—covering cadence, depth, filter choices, and instrument selection—for both kilonovae and afterglows remains only partially resolved, underscoring the need to establish best practices for counterpart searches.