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We present interferometric observations of the CN(1-0) line emission inMrk231 and combine them with previous observations of CO and other H$_2$ gastracers to study the physical properties of the massive molecular outflow. Wefind a strong boost of the CN/CO(1-0) line luminosity ratio in the outflow,which is unprecedented compared to any other known Galactic or extragalacticsource. For the dense gas phase in the outflow traced by the HCN and CNemissions, we infer $\rm X_{\rm CN}\equiv [CN]/[H_2] > X_{\rm HCN}$ by at leasta factor of three, with H$_2$ gas densities of $n_{\rm H_2}\sim10^{5-6}$cm$^{-3}$. In addition, for the first time, we resolve narrow spectral featuresin the HCN(1-0) and HCO$^+$(1-0) high-velocity line wings tracing the densephase of the outflow. The velocity dispersions of these spectral features,$\sigma_v\sim7-20$ km s$^{-1}$, are consistent with those of massiveextragalactic giant molecular clouds detected in nearby starburst nuclei. TheH$_2$ gas masses inferred from the HCN data are quite high,$M_{mol}\sim0.3-5\times10^8$ $M_{\odot}$. Our results suggest that massive,denser molecular gas complexes survive embedded into the more diffuse H$_2$phase of the outflow, and that the chemistry of such outflowing dense clouds isaffected by enhanced UV radiation.

Enhanced UV radiation and dense clumps in Mrk231's molecular outflow