  We present ALMA cycle 0 observations of the molecular gas and dust in the
IR-bright mid-stage merger VV114 obtained at 160 - 800 pc resolution. The main
aim of this study is to investigate the distribution and kinematics of the
cold/warm gas and to quantify the spatial variation of the excitation
conditions across the two merging disks. The data contain 10 molecular lines,
including the first detection of extranuclear CH3OH emission in interacting
galaxies, as well as continuum emission. We map the 12CO(3-2)/12CO(1-0) and the
12CO(1-0)/13CO(1-0) line ratio at 800 pc resolution (in the units of K km/s),
and find that these ratios vary from 0.2 - 0.8 and 5 - 50, respectively.
Conversely, the 200 pc resolution HCN(4-3)/HCO+(4-3) line ratio shows low
values (< 0.5) at a filament across the disks except for the unresolved eastern
nucleus which is three times higher (1.34 +/- 0.09). We conclude from our
observations and a radiative transfer analysis that the molecular gas in the
VV114 system consists of five components with different physical and chemical
conditions; i.e., 1) dust-enshrouded nuclear starbursts and/or AGN, 2)
wide-spread star forming dense gas, 3) merger-induced shocked gas, 4) quiescent
tenuous gas arms without star formation, 5) H2 gas mass of (3.8 +/- 0.7) * 10^7
Msun (assuming a conversion factor of {\alpha}_CO = 0.8 Msun (K km s^-1
pc^2)^-1) at the tip of the southern tidal arm, as a potential site of tidal
dwarf galaxy formation.
