  The observability of afterglows from binary neutron star mergers, occurring
within AGN disks is investigated. We perform 3D GRMHD simulations of a
post-merger system, and follow the jet launched from the compact object. We use
semi-analytic techniques to study the propagation of the blast wave powered by
the jet through an AGN disk-like external environment, extending to distances
beyond the disk scale height. The synchrotron emission produced by the
jet-driven forward shock is calculated to obtain the afterglow emission. The
observability of this emission at different frequencies is assessed by
comparing it to the quiescent AGN emission. In the scenarios where the
afterglow could temporarily outshine the AGN, we find that detection will be
more feasible at higher frequencies (> 10^(14) Hz) and the electromagnetic
counterpart could manifest as a fast variability in the AGN emission, on
timescales less than a day.
