The morphological and velocity structures in the gaseous ( Hi and CO ) and stellar components of two interacting systems are examined .
Both Arp 140 and Arp 104 reveal extended tidal tails in the Hi .
The H \alpha and FIR fluxes of Arp 140 yield similar SFR of \sim 0.8 \mathrm { M } _ { \odot } \mathrm { yr } ^ { -1 } .
In contrast the H \alpha flux of Arp 104 yields a SFR of \sim 0.05 \mathrm { M } _ { \odot } \mathrm { yr } ^ { -1 } , \sim 20 times smaller than that obtained from the FIR flux .
Spectra were used to examine the changing velocity of atomic and molecular gas in NGC 5218 ( Arp 104 ) .
The atomic and molecular gas were found to be dynamically similar with comparable velocities and velocity widths across the galaxy ; consistent with the two phases responding similarly to the interaction , or enhanced Hi to CO conversion in the centre of the galaxy .