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We aim to analyze the chemical evolution of the Small Magellanic Cloud adding12 additional clusters to our existing sample having accurate and homogeneouslyderived metallicities. We are particularly interested in seeing if there is anycorrelation between age and metallicity for the different structural componentsto which the clusters belong. Spectroscopic metallicities of red giant starsare derived from the measurement of the equivalent width of the near-IR calciumtriplet lines. Cluster membership analysis was carried out using criteria thatinclude radial velocities, metallicities, proper motions and distance from thecluster center. The mean cluster radial velocity and metallicity weredetermined with a typical error of 2.1 km/s and 0.03 dex, respectively. Weadded this information to that available in the literature for other clustersstudied with the same method, compiling a final sample of 48 clusters withmetallicities homogeneously determined. Clusters of the final sample aredistributed in an area of ~ 70 deg^2 and cover an age range from 0.4 Gyr to10.5 Gyr. The metallicity distribution of our new cluster sample shows a lowerprobability of being bimodal than suggested in previous studies. The separatechemical analysis of clusters in the six components (Main Body, Counter-Bridge,West Halo, Wing/Bridge, Northern Bridge and Southern Bridge) shows that onlyclusters belonging to the Northern Bridge appear to trace a V-Shape, showing aclear inversion of the metallicity gradient in the outer regions. There is asuggestion of a metallicity gradient in the West Halo, similar to thatpreviously found for field stars. It presents, however, a very largeuncertainty. Also, clusters belonging to the West Halo, Wing/Bridge andSouthern Bridge exhibit a well-defined age-metallicity relation with relativelylittle scatter in abundance at fixed age compared to other regions.

Ca II Triplet Spectroscopy of Small Magellanic Cloud Red Giants. V. Abundances and Velocities for 12 Massive Clusters