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Context: Cepheids are excellent tracers of young stellar populations. Theyplay a crucial role in astrophysics as standard candles. The chemistry ofclassical Cepheids in the Milky Way is now quite well-known. Despite a muchlarger sample, the chemical composition of Magellanic Cepheids has been onlyscarcely investigated. Aims: For the first time, we study the chemicalcomposition of several Cepheids located in the same populous cluster: NGC 1866,in the Large Magellanic Cloud (LMC). To also investigate the chemicalcomposition of Cepheids at lower metallicity, four targets are located in theSmall Magellanic Cloud (SMC). Our sample allows us to increase the number ofCepheids with known metallicities in the LMC/SMC by 20%/25% and the number ofCepheids with detailed chemical composition in the LMC/SMC by 46%/50%. Methods:We use canonical spectroscopic analysis to determine the chemical compositionof Cepheids and provide abundances for a good number of $\alpha$, iron-peak andneutron-capture elements. Results: We find that six Cepheids in the LMC clusterNGC 1866 have a very homogeneous chemical composition, also consistent with redgiant branch (RGB) stars in the cluster. Period--age relations that include noor average rotation indicate that all the Cepheids in NGC 1866 have a similarage and therefore belong to the same stellar population. Our results are ingood agreement with theoretical models accounting for luminosity and radialvelocity variations. Using distances based on period-luminosity relations inthe near- or mid-infrared, we investigate for the first time the metallicitydistribution of the young population in the SMC in the depth direction.Preliminary results show no metallicity gradient along the SMC main body, butour sample is small and does not contain Cepheids in the inner few degrees ofthe SMC.

Detailed chemical composition of classical Cepheids in the LMC cluster NGC 1866 and in the field of the SMC