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NGC 3201 is a globular cluster suspected to have an intrinsic spread in theiron content. We re-analysed a sample of 21 cluster stars observed withUVES-FLAMES at the Very Large Telescope and for which Simmerer et al. found a0.4 dex wide [Fe/H] distribution with a metal-poor tail. We confirmed that whenspectroscopic gravities are adopted, the derived [Fe/H] distribution spans ~0.4dex. On the other hand, when photometric gravities are used, the metallicitydistribution from Fe I lines remains large, while that derived from Fe II linesis narrow and compatible with no iron spread. We demonstrate that themetal-poor component claimed by Simmerer et al. is composed by asymptotic giantbranch stars that could be affected by non local thermodynamical equilibriumeffects driven by iron overionization. This leads to a decrease of the Fe Iabundance, while leaving the Fe II abundance unaltered. A similar finding hasbeen already found in asymptotic giant branch stars of the globular clusters M5and 47 Tucanae. We conclude that NGC 3201 is a normal cluster, with no evidenceof intrinsic iron spread.

The origin of the spurious iron spread in the globular cluster NGC 3201