We present new imaging and spectroscopic observations of the interacting system Arp 194 ( \equiv UGC 06945 \equiv VV 126 ) .
The northern component ( A194N ) is a distorted spiral or ring galaxy likely disrupted by a collision or close encounter with a southern galaxy ( A194S ) .
There is evidence that a third galaxy with similar recession velocity is projected on A194N but its role is likely secondary .
A194S is connected to A194N by a string of emission knots which motivates our interpretation that the former was the intruder .
Three of the knots are easily discernible in B , R , and H \alpha images and are assumed to trace the path of the intruder following the encounter , which we estimate occurred a few 10 ^ { 8 } yr ago .

Both A194S and N are experiencing strong bursts of star formation : the H \alpha luminosity indicates a total star formation rate \sim 10 M _ { \odot } yr ^ { -1 } .
The lack of detectable J and K emission from the blobs , along with strong H \alpha emission , indicates that an evolved stellar population is not likely to be present .
The brightest knot ( closest to A194S ) shows a star formation rate of \approx 1.2 M _ { \odot } yr ^ { -1 } which , if sustained over a time \approx 7 \times 10 ^ { 7 } yr , could explain the spectral energy distribution .
This suggests that the stripped matter was originally predominantly gaseous .
The brightest knot is detected as a FIRST radio source and this is likely the signature of supernova remnants related to enhanced star formation .
Motions in the gas between the brightest knot and A194S , traced by an emission line link of increasing radial velocity , suggests infall toward the center of the intruder .
Arp 194 is therefore one of the few galaxies where evidence of “ cross-fueling ” is observed .