The importance of galaxy mergers in the context of galaxy formation and evolution have been clearly demonstrated in various numerical simulations. The violent merger event not only results in large scale morphological transformation and mass accumulation, but it also triggers gas compression, turbulence, and gas inflow to the galactic center region. We present high resolution 12CO(1-0), (CO)-C-13(1-0), HCN(4-3), HCO+(4-3), CN(1(3/2)-0(1/2)), CN(1(1/2)-0(1/2)), CS (2-1), CH3OH(2-1), and CS(7-6) maps of an IR-bright late stage merger VV114 obtained during cycle 0 of ALMA. An unresolved strong HCN(4-3) source is detected at the nucleus of VV114E and has a high velocity dispersion (similar or equal to 300 km s(-1)), and these features are also shown in HCO+ (4-3). These evidences suggest that this source has an obscured AGN. We also find a clumpy filament with resolved dense gas across the galaxy disks. This filament has clumpy star-forming regions at each regions. Each region of this filament clearly shows the physical and chemical differences in our molecular line results.