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We report ~2" resolution Atacama Large Millimeter/submillimeter Arrayobservations of the HCN(1-0), HCO+(1-0), CO(1-0), CO(2-1), and CO(3-2) linestowards the nearby merging double-nucleus galaxy NGC 3256. We find that thehigh density gas outflow traced in HCN(1-0) and HCO+(1-0) emission isco-located with the diffuse molecular outflow emanating from the southernnucleus, where a low-luminosity active galactic nucleus (AGN) is believed to bethe dominant source of the far-infrared luminosity. On the other hand, the samelines were undetected in the outflow region associated with the northernnucleus, whose primary heating source is likely related to starburst activitywithout obvious signs of AGN. Both HCO+(1-0)/CO(1-0) line ratio (i.e. dense gasfraction) and the CO(3-2)/CO(1-0) line ratio are larger in the southern outflow(0.20$\pm$0.04 and 1.3$\pm$0.2, respectively) than in the southern nucleus(0.08$\pm$0.01, 0.7$\pm$0.1, respectively). By investigating these line ratiosfor each velocity component in the southern outflow, we find that the dense gasfraction increases and the CO(3-2)/CO(1-0) line ratio decreases towards thelargest velocity offset. This suggests the existence of a two-phase (diffuseand clumpy) outflow. One possible scenario to produce such a two-phase outflowis an interaction between the jet and the interstellar medium, which possiblytriggers shocks and/or star formation associated with the outflow.

ALMA observations of HCN and HCO+ outflows in the merging galaxy NGC 3256