SOME COLOR-MAGNITUDE DIAGRAMS AND ABUNDANCES IN THE MAGELLANIC CLOUDS Eduardo Hardy****, Jorge Melnick**, and Claude Reheault* * Dept. de Physique, Universite Laval, Quebec, Canada ** European Southern Observatory, Geneva Some C-M diagrams and photometric abundances are presented of clusters and their adjoining fields in areas of the Clouds, in an attempt to derive properties which would allow a comparison with regions in the Galaxy. THE LMC SAMPLE: Located at about 6 kpc from the Bar center, this area, which comprises NGC 2209, LW 376, LW 405 and the field, is representative of ^ 1 sq. kpc of the SE periphery of the LMC.C-M diagrams from CTIO 4 m plates calibrated using Walker's (1971) electronographic sequence are shown in Figure 1 in the above order. The V scale was artificially cut at V=18 to avoid saturated images in the digitized reduction process. We conclude that the en- tire region shows a preponder ance of intermediate-age objects of similar age O8xl0 8 yrs). From Washington System photometry (Canterna 1976) of the NGC 2209 stars D36 and F49 (Gascoigne et al. 1976) performed at Las Campanas we find [Fe/H] = -0.60 ± 0.15 in good agreement with the position of the "clump" at (B-V) ^ 0.80 in all diagrams. As shown in the first panel a good analogue in the Galaxy is the anticenter cluster NGC 2158 (Arp and Cuffey 1962, Janes 1979). James E. Hesser fed.), Star Clusters, 343-345. Copyright © 1980 by the I A U. 1 U.CMU. 1 'ii 1 / "NB 1 "*3 1 ..'..'"l Wt (&.*"'" 1 .'.. Figure 1. LMC Sample 343 available at https://www.cambridge.org/core/terms. https://doi.org/10.1017/S0074180900092123 Downloaded from https://www.cambridge.org/core. IP address: 207.241.231.81, on 28 Jul 2018 at 09:33:40, subject to the Cambridge Core terms of use,