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Fig. 5

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Comparison of the Cepheid (black dots) metallicity gradient with iron abundances of early B-type stars located either in the solar neighborhood or in the Orion star forming region (Nieva & Simón-Díaz 2011; Nieva & Przybilla 2012). The green square marks the iron abundance of the two red supergiants in the Galactic center measured by Davies et al. (2009a), the magenta diamonds the 26 red supergiants in the Scutum Clusters measured by Davies et al. (2009b), the gray diamond the three red supergiants in the cluster RSGC2 measured by Origlia et al. (2013), the red cross the two luminous blue variables (LBVs) in the Quintuplet cluster (Najarro et al. 2009), and the light-blue triangle three Wolf–Rayet and two O-type stars in the Arches cluster (Martins et al. 2008). The red vertical bar in the bottom right corner shows the mean uncertainty on iron abundances.

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