in the interval \[$m_{1}$,$m_{1}+3$\]. Furthermore, many of our groups have $m_{1} + 3 > m_{\rm lim}$, where $m_{\rm lim,Zw}=15.5$ is the limiting magnitude of the survey. Thus we do not necessarily include all of the galaxies which might be in the interval \[$m_{1}$,$m_{1}+3$\]. We later examine POSS images of the groups and find few fainter galaxies inside the group radii.

Second, we do not implement Hickson’s isolation criteria in our initial group selection. Third, we do not reject groups on the basis of surface brightness. However, all but four very nearby groups in our catalog automatically satisfy the surface brightness criterion because we require galaxy projected separations comparable with the size of a galaxy. Finally, we note that unlike the HCG’s, our sample is a complete listing of compact groups of three or more galaxies. Hickson includes a triplet only when one member of his initial group has a discordant redshift.

In general, our limits on the physical extent of compact groups are more restrictive than Hickson’s. 23 HCG’s are within the redshift survey boundaries and contain at least three galaxies brighter than the magnitude limit. We detect parts or all of 15 of these HCG’s. We fail to detect 