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We present an analysis of the gas kinematics in NGC 2992, based on VLT/MUSE,ALMA and VLA data, aimed at characterising the disk, the wind and theirinterplay in the cold molecular and warm ionised phases. CO(2-1) and H$\rm\alpha~$ arise from a multiphase disk with inclination 80 deg and radii 1.5 and1.8 kpc, respectively. We find that the velocity dispersion of the coldmolecular phase is consistent with that of star forming galaxies at the sameredshift, except in the inner 600 pc region, and in the region between the conewalls and the disk. This suggests that a disk-wind interaction locally booststhe gas turbulence. We detect a clumpy ionised wind distributed in two wideopening angle ionisation cones reaching scales of 7 kpc. The [O III] windexpands with velocity exceeding -1000 km/s in the inner 600 pc, a factor of 5larger than the previously reported wind velocity. Based on spatially resolvedelectron density and ionisation parameter maps, we infer an ionised outflowmass of $M_{\rm of,ion} = (3.2 \pm 0.3) \times \, 10^7 \, M_{\odot}$, and atotal ionised outflow rate of $\dot M_{\rm of,ion}=13.5\pm1$ \sfr. We detectedclumps of cold molecular gas located above and below the disk reaching maximumprojected distances and velocities of 1.7 kpc and 200 km/s, respectively. Onthese scales, the wind is multiphase, with a fast ionised component and aslower molecular one, and a total mass of $M_{\rm of, ion+mol}= 5.8 \times 10^7\, M_{\odot}$, of which the molecular component carries the bulk of the mass.The dusty molecular outflowing clumps and the turbulent ionised gas are locatedat the edges of the radio bubbles, suggesting that the bubbles interact withthe surrounding medium through shocks. We detect a dust reservoir co-spatialwith the molecular disk, with a cold dust mass $M_{\rm dust} = (4.04 \pm 0.03)\times \, 10^{6} \, M_{\odot}$.

NGC 2992: The interplay between the multiphase disk, wind and radio bubbles