The motivation for studying distant open clusters primarily arose out of a desire to gain some understanding of star formation processes in the general context of galactic structure. Of specific interest are faint open clusters (c.f. Alter, Balázs and Ruprecht 1970) near the galactic anticenter which are part of a larger survey of objects which may be located in the “periphery” of the Galaxy. Table I contains a sample of results from broad-band photometric studies for clusters near ZII=180°, bII=0°. The characteristics of these clusters are consistent with other investigations, which suggest that the disk of the galaxy extends to large galactocentric distances; for example, deep surveys of blue stars (Chromey 1979; McCarthy and Miller 1974) and investigations of the rotation curve of the galaxy (Blitz 1979; Knapp, Tremaine and Gunn 1978), to mention a few. There is also a considerable amount of evidence that the distributions of distant objects basically reflect the locations of local absorbing clouds and low absorption “windows” (Westpfah1 and Christian 1979), rather than distant galactic structure. Therefore, in this study, emphasis is being placed on the determination of ages, abundances and luminosity functions of clusters, rather than considering them as “spiral tracers”.