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With MUSE, Chandra, VLA, ALMA and UVIT data from the GASP programme we studythe multiphase baryonic components in a jellyfish galaxy (JW100) with a stellarmass 3.2 X 10^{11} M_sun hosting an AGN. We present its spectacular extraplanartails of ionized and molecular gas, UV stellar light, X-ray and radio continuumemission. This galaxy represents an excellent laboratory to study the interplaybetween different gas phases and star formation, and the influence of gasstripping, gas heating, and AGN. We analyze the physical origin of the emissionat different wavelengths in the tail, in particular in-situ star formation(related to Halpha, CO and UV emission), synchrotron emission from relativisticelectrons (producing the radio continuum) and heating of the strippedinterstellar medium (ISM) (responsible for the X-ray emission). We show thesimilarities and differences of the spatial distributions of ionized gas,molecular gas and UV light, and argue that the mismatch on small scales (1kpc)is due to different stages of the star formation process. We present therelation Halpha--X-ray surface brightness, which is steeper for star-formingregions than for diffuse ionised gas regions with high [OI]/Halpha ratio. Wepropose that ISM heating due to interaction with the intracluster medium(either for mixing, thermal conduction or shocks) is responsible for the X-raytail, the observed [OI]-excess and the lack of star formation in the northernpart of the tail. We also report the tentative discovery in the tail of themost distant (and among the brightest) currently known ULX, a point-likeultraluminous X-ray source commonly originating in a binary stellar systempowered either by an intermediate-mass black hole or a magnetized neutron star.

GASP XXIII: A jellyfish galaxy as an astrophysical laboratory of the baryonic cycle