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Accretion disks around supermassive black holes (SMBH) are promising sitesfor stellar mass black hole (BH) mergers due to mass segregation and mergeracceleration by disk gas torques. Here we show that a GW-kick at BH mergercauses ram-pressure stripping of gas within the BH Hill sphere. If $R_{H}\geqH$, the disk height, an off-center UV flare at $a_{\rm BH} \sim 10^{3}r_{g}$emerges within $t_{\rm UV} \sim \rm{O}(2 {\rm days})(a_{\rmBH}/10^{3}r_{g})(M_{\rm SMBH}/10^{8}M_{\odot})(v_{\rm kick}/10^{2}\rm{km/s})$post-merger and lasts O$(R_{H}/v_{\rm kick}) \sim \rm{O}(5 t_{\rm UV}$). Theflare emerges with luminosity O($10^{42}{\rm erg/s})(t_{\rm UV}/2{\rmdays})^{-1}(M_{\rm Hill}/1M_{\odot})(v_{\rm kick}/10^{2}{\rm km/s})^{2}$. AGNoptical/UV photometry alters and asymmetric broad emission line profiles candevelop after weeks. If $R_{H}<H$, detectability depends on disk optical depth.Follow-up by large optical sky surveys is optimized for small GW error volumesand for LIGO/Virgo triggers $>50M_{\odot}$.

Ram-pressure stripping of a kicked Hill sphere: Prompt electromagnetic emission from the merger of stellar mass black holes in an AGN accretion disk