I brightest galaxies, a preliminary set of 700 is presented here. For an overview, survey parameters as well as data calibration and imaging techniques see Staveley-Smith et al. Barnes et al. This is the first time that galaxy clustering can be studied uninhibited by foreground stars and dust from our own Galaxy. The most prominent structures in Fig.
Detailed studies are under way.
The H I mass function, catalog completeness, as well as H I and optical galaxy parameters will be discussed. I wish to particularly thank Virginia Kilborn, Lister Staveley-Smith and Stuart Ryder for their continuous contributions.