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Active galactic nuclei (AGNs) have been proposed as plausible sites forhosting a sizable fraction of the binary black hole (BBH) mergers measuredthrough gravitational waves (GWs) by the LIGO-Virgo-Kagra (LVK) experiment.These GWs could be accompanied by radiation feedback due to the interaction ofthe BBH merger remnant with the AGN disc. We present a new predicted radiationsignature driven by the passage of a kicked BBH remnant throughout a thin AGNdisc. We analyse the situation of a merger occurring outside the thin disc,where the merger is of second or higher generation in a merging hierarchicalsequence. The coalescence produces a kicked BH remnant that eventually plungesinto the disc, accretes material, and inflates jet cocoons. We consider thecase of a jet cocoon propagating quasi-parallel to the disc plane and study theoutflow that results when the cocoon emerges from the disc. We calculate thetransient emission of the emerging cocoon using a photon diffusion modeltypically employed to describe the light curves of supernovae. Depending on theparameter configuration, the flare produced by the emerging cocoon could becomparable to or exceed the AGN background emission at optical, and extremeultraviolet wavelengths. For instance, in AGNs with central engines of $\sim5\times10^{6}$ M$_\odot$, flares driven by BH remnants with masses of $\sim$100 M$_\odot$ can appear in about $\sim$[10-100] days after the GW, lasting forfew days.

Optical Emission Model for Binary Black Hole Merger Remnants Travelling through Discs of Active Galactic Nuclei