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Context. While most (if not all) Type I Galactic globular clusters (GGCs) arecharacterised by spreads in the abundances of light chemical elements (e.g. Li,N, O, Na, Mg, Al), it is not yet well established whether similar spreads mayexist in s-process elements as well. Aims. We investigated the possibledifference in Ba abundance between the primordial (1P) and polluted (2P) starsin the Galactic globular cluster (GGC) 47 Tuc (NGC 104). For this, we obtainedhomogeneous abundances of Fe, Na, and Ba in a sample of 261 red giant branch(RGB) stars which is the largest sample used for Na and Ba abundance analysisin any GGC so far. Methods. Abundances of Na and Ba were determined usingarchival GIRAFFE/VLT spectra and 1D non-local thermodynamic equilibrium (NLTE)abundance analysis methodology. Results. Contrary to the finding of Gratton etal. (2013), we did not detect any significant Ba-Na correlation or 2P-1P Baabundance difference in the sample of 261 RGB stars in 47 Tuc. Thiscorroborates the result of D'Orazi et al. (2010) who found no statisticallysignificant Ba-Na correlation in 110 RGB stars in this GGC. The averagebarium-to-iron ratio obtained in the sample of 261 RGB stars, $\langle{\rmBa/Fe}_{\rm 1D~NLTE}\rangle = -0.01\pm0.06$, agrees well with those determinedin Galactic field stars at this metallicity and may therefore represent theabundance of primordial proto-cluster gas that has not been altered during thesubsequent chemical evolution of the cluster.

Abundance of barium in the atmospheres of red giants in the Galactic globular cluster NGC 104 (47 Tuc)