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The observability of afterglows from binary neutron star mergers, occurringwithin AGN disks is investigated. We perform 3D GRMHD simulations of apost-merger system, and follow the jet launched from the compact object. We usesemi-analytic techniques to study the propagation of the blast wave powered bythe jet through an AGN disk-like external environment, extending to distancesbeyond the disk scale height. The synchrotron emission produced by thejet-driven forward shock is calculated to obtain the afterglow emission. Theobservability of this emission at different frequencies is assessed bycomparing it to the quiescent AGN emission. In the scenarios where theafterglow could temporarily outshine the AGN, we find that detection will bemore feasible at higher frequencies (> 10^(14) Hz) and the electromagneticcounterpart could manifest as a fast variability in the AGN emission, ontimescales less than a day.

Afterglows from binary neutron star post-merger systems embedded in AGN disks