Iron and carbon abundances are determined for F dwarfs in several open clusters and the field in order to investigate the homogeneity of chemical mixing in the Galactic disk. Abundances are based on measurements of eight Fe I lines and six high-excitation C I lines in the spectral region 7065-7155 A analyzed with model atmospheres. Cluster mean values of Fe/H and C/H show cluster-to-cluster variations well in excess of observational errors, indicating both that the overall metal content of the gas from which these clusters formed preserved small but significant differences over periods of several billion years, and that the production of carbon closely followed that of iron so that these regions of star formation had the same ratio of C/Fe.
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Friel et al. (1992) studied this question.