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We present high-resolution observations (0".2-1".5) of multiple dense gastracers, HCN and HCO$^+$ ($J$ = 1-0, 3-2, and 4-3), HNC ($J$ = 1-0), and CS($J$ = 7-6) lines, toward the nearby luminous infrared galaxy VV 114 with theAtacama Large Millimeter/submillimeter Array. All lines are robustly detectedat the central gaseous filamentary structure including the eastern nucleus andthe Overlap region, the collision interface of the progenitors. We found thatthere is no correlation between star formation efficiency and dense gasfraction, indicating that the amount of dense gas does not simply control starformation in VV 114. We predict the presence of more turbulent and diffusemolecular gas clouds around the Overlap region compared to those at the nuclearregion assuming a turbulence-regulated star formation model. The intracloudturbulence at the Overlap region might be excited by galaxy-merger-inducedshocks, which also explains the enhancement of gas-phase CH$_3$OH abundancepreviously found there. We also present spatially resolved spectral line energydistributions of HCN and HCO$^+$ for the first time, and derive excitationparameters by assuming optically-thin and local thermodynamic equilibrium (LTE)conditions. The LTE model revealed that warmer, HCO$^+$-poorer molecular gasmedium is dominated around the eastern nucleus, harboring an AGN. The HCNabundance is remarkably flat ($\sim$3.5 $\times$ 10$^{-9}$) independently ofthe various environments within the filament of VV 114 (i.e., AGN, starformation, and shock).

Spatially-resolved Dense Molecular Gas Excitation in the Nearby LIRG VV 114