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We analyze new high spatial resolution (~60 pc) ALMA CO(2-1) observations ofthe isolated luminous infrared galaxy ESO 320-G030 (d=48 Mpc) in combinationwith ancillary HST optical and near-IR imaging as well as VLT/SINFONI near-IRintegral field spectroscopy. We detect a high-velocity (~450 km/s) spatiallyresolved (size~2.5 kpc; dynamical time ~3 Myr) massive (~10^7 Msun; massrate~2-8 Msun/yr) molecular outflow originated in the central ~250 pc. Weobserve a clumpy structure in the outflowing cold molecular gas with clumpsizes between 60 and 150 pc and masses between 10^5.5 and 10^6.4 Msun. The massof the clumps decreases with increasing distance, while the velocity isapproximately constant. Therefore, both the momentum and kinetic energy of theclumps decrease outwards. In the innermost (~100 pc) part of the outflow, wemeasure a hot-to-cold molecular gas ratio of 7x10^-5, which is similar to thatmeasured in other resolved molecular outflows. We do not find evidence of anionized phase in this outflow. The nuclear IR and radio properties arecompatible with strong and highly obscured star-formation (A_k ~ 4.6 mag;SFR~15 Msun/yr). We do not find any evidence for the presence of an activegalactic nucleus. We estimate that supernova explosions in the nuclearstarburst (\nu(SN) ~ 0.2 yr^-1) can power the observed molecular outflow. Thekinetic energy and radial momentum of the cold molecular phase of the outflowcorrespond to about 2% and 20%, respectively, of the supernovae output. Thecold molecular outflow velocity is lower than the escape velocity, so the gaswill likely return to the galaxy disk. The mass loading factor is ~0.1-0.5, sothe negative feedback due to this star-formation powered molecular outflow isprobably limited.

High-velocity extended molecular outflow in the star-formation dominated luminous infrared galaxy ESO 320-G030