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We perform a comparative analysis of the spatial distribution of young (<50Myr) open star clusters and field Cepheids with different metallicities. Asignificant fraction of young clusters are shown to have low metallicitiesatypical of field Cepheids. Both types of objects exhibit approximately equal(in magnitude) negative radial metallicity gradients, while their azimuthalmetallicity gradients differ outside the error limits and have opposite signs.Among the stellar complexes identified by young clusters, the most metal-poorclusters are grouped in the Perseus complex. It is the clusters of this complexthat are responsible for the radial and azimuthal metallicity gradients amongyoung clusters. The described properties are indicative of a weak mixing ofinterstellar matter before the onset of star formation there. Significantdifferences between the spatial distributions of open clusters and field starswith different metallicities suggest different conditions required for theformation of these types of objects.

Young Open Star Clusters: The Spatial Distribution of Metallicity in the Solar Neighborhood