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From the first part of Table 2 we can derive two preliminary conclusions: (1) There is no close correspondence between cluster richness and form-type (for the nearest clusters) on the present system; clusters of Type I range in richness from 0 to 2; clusters of Type III also range between the same limits. (2) The phenomenon of two centrally located galaxies in a common envelope is encountered in a number of clusters of Types II and III.

From the nine richest clusters (second part of Table 2) we note that all classes from I to III are represented; from this independent material we again conclude that there is no close relationship between classified type and richness. There is also another interesting characteristic of the richest clusters: the majority are irregular in shape, and two (A545 and A665) are highly irregular, with density minima within their main bodies.

The two radio galaxies in the final section of Table 2 are of special interest: both have double nuclei; and one (Cyg A) has an emission spectrum that resembles typical Seyfert galaxies (see spectrum reproduced in Schmidt 1965). Some similarity in the spectrum of Cyg A to Seyfert galaxies had been noted earlier by Baade and Minkowski (1954).