Abstract
The distribution of redshift differences for a sample of 250 close double galaxies is shown to depend strongly upon the emission properties of the component galaxies and to some extent upon interaction morphology. The distribution is not significantly dependent either upon physical or angular separation or upon the magnitude differential. The Delta-V distribution can be decomposed into a sharply peaked component with dispersion about 100 km/s characterized by emission objects, and a broad component with dispersion about 300 km/s characterized by absorption spectra. Within these two components, especially the sharply peaked one, there appears to be a dependence of emission strength, and to a lesser extent interaction morphology, upon physical separation in the range 5-20 kpc.
