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We have observed the late-type peculiar galaxy NGC 4424 during VESTIGE, ablind narrow-band Halpha[NII] imaging survey of the Virgo cluster carried outwith MegaCam at the CFHT. The presence of a 110 kpc long HI tail in the Sdirection indicates that this galaxy is undergoing a ram pressure strippingevent. The deep narrow-band image revealed the presence of a low surfacebrightness ionised gas tail ~10 kpc long extending from the centre of thegalaxy to the NW direction, in the direction opposite to the HI tail. Chandraand XMM X-rays data do not show any compact source in the nucleus nor thepresence of an extended tail of hot gas, while MUSE spectroscopy indicates thatthe gas is photo-ionised in the inner regions and shock-ionised in the outerparts. IFU spectroscopy confirms that the ionised gas is kinematicallydecoupled from the stellar component and indicates the presence of twokinematically distinct structures in the stellar disc. The analysis of the SEDof the galaxy indicates that the activity of star formation has been totallyquenched in the outer disc ~ 250-280 Myr ago, while only reduced by ~80% in thecentral regions. All this observational evidence suggests that NGC 4424 is theremnant of an unequal-mass merger occurred <= 500 Myr ago, when the galaxy wasalready a member of the Virgo cluster, now undergoing a ram pressure strippingevent which has removed the gas and quenched the activity of star formation inthe outer disc. The tail of ionised gas probably results from the outflowproduced by a central starburst fed by the collapse of gas induced by themerging episode. This outflow is sufficiently powerful to overcome the rampressure induced by the intracluster medium on the disc of the galaxy crossingthe cluster. This analysis thus suggests that feedback can participate in thequenching process of galaxies in high-density regions.

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).IV. A tail of Ionised Gas in the Merger Remnant NGC 4424