Neutron-capture element signatures in globular clusters: Insights from the Gaia -ESO Survey

Context. Globular clusters (GCs) are crucial to our understanding of the formation and evolution of our Galaxy. While their abundances of light and iron-peak elements have been extensively studied, research on heavier elements and their possible link to both the multiple stellar population phenomenon and the origin of GCs remains relatively limited. Aims. We aim to analyse the chemical abundances of various neutron-capture elements using GCs as tracers of the Galactic halo. Furthermore, we explore the potential connection between these elements and the multiple stellar population phenomenon in GCs to better constrain the nature of the polluters responsible for the intracluster enrichment. Additionally, we seek to determine the origins of GCs based on their neutron-capture element abundances. Methods. We analysed a sample of 14 GCs spanning a wide metallicity range, [Fe/H] from 0.40 to 2.32, observed as a part of the Gaia-ESO Survey and analysed using a homogeneous methodology. Here we present results for Y, Zr, Ba, La, Ce, Nd, Pr, and Eu obtained from FLAMES-UVES spectra. We compared our results with a stochastic Galactic chemical evolution model. Results. Except for Zr, the Galactic chemical evolution model, when available, closely describes the broad trend displayed by neutron-capture elements in GCs. Moreover, in some clusters, a strong correlation between hot H-burning (Na and Al) and s-process elements suggests a shared nucleosynthetic site, for example asymptotic giant branch stars of different masses and/or fast-rotating massive stars that produced the intracluster pollution. Additionally, we identified clear differences in the [Eu/Mg] ratio between in situ (⟨[Eu/Mg]]⟩=0.14 dex) and ex situ (⟨[Eu/Mg]]⟩=0.32 dex) GCs, which reveal their distinct chemical enrichment histories. Finally, on average, the Type II GCs NGC 362, NGC 1261, and NGC 1851 show a spread ratio in s-process elements between second- and first-generation stars that is roughly twice as large as that observed in Type I clusters.