Title: Neutron-Capture Element Signatures in Globular Clusters: Insights from the Gaia-ESO Survey Show Chinese title

Title: 球状星团中的中子俘获元素特征：来自盖亚-欧几里得巡天的见解

Abstract: Globular clusters (GCs) are key to understanding the formation and evolution of our Galaxy. While the abundances of light and Fe-peak elements in GCs have been widely studied, investigations into heavier, neutron-capture elements -- and their connection to multiple stellar populations and GC origins -- remain limited. In this work, we analysed the chemical abundances of neutron-capture elements in GCs to trace the Galactic halo and to explore possible links to the MP phenomenon. Our goal is to better constrain the nature of the polluters responsible for intracluster enrichment and to distinguish the origin of GCs through the chemical signature of neutron-capture elements. We examined 14 GCs from the Gaia-ESO Survey, spanning a wide metallicity range, [Fe/H] from -0.40 to -2.32, using a homogeneous methodology. We focused on the abundances of Y, Zr, Ba, La, Ce, Nd, Pr, and Eu, derived from FLAMES-UVES spectra. These were compared with predictions from a stochastic Galactic chemical evolution model. With the exception of Zr, the model broadly reproduces the observed trends in neutron-capture elements. In some GCs, we found strong correlations between hot H-burning products (Na, Al) and s-process elements, pointing to a shared nucleosynthesis site, e.g., asymptotic giant branch stars of different masses and/or fast-rotating massive stars. We also detect a distinct difference in [Eu/Mg] ratio between in-situ ($\langle$[Eu/Mg]$\rangle$ = 0.14 dex) and ex-situ ($\langle$[Eu/Mg]$\langle$ = 0.32 dex) GCs, highlighting their different enrichment histories. Finally, on average, Type II GCs (NGC 362, NGC 1261, and NGC 1851) showed a s-process element spread ratio between second- and first-generations about twice as large as those seen in Type I clusters. Show Chinese abstract

Abstract: 球状星团（GCs）对于理解我们银河系的形成和演化至关重要。尽管轻元素和铁峰元素在球状星团中的丰度已被广泛研究，但对更重的中子俘获元素的研究以及它们与多重恒星星族和球状星团起源之间的联系仍然有限。在这项工作中，我们分析了球状星团中中子俘获元素的化学丰度，以追踪银河晕并探索可能与多重恒星现象（MP现象）的联系。我们的目标是更好地约束负责星团内富集的污染物的本质，并通过中子俘获元素的化学特征来区分球状星团的起源。我们使用均匀的方法学检查了来自盖亚-欧洲南方天文台巡天的14个球状星团，这些星团的金属丰度范围从[Fe/H] -0.40到-2.32。我们专注于从FLAMES-UVES光谱中得出的Y、Zr、Ba、La、Ce、Nd、Pr和Eu的丰度。这些数据与随机银河化学演化模型的预测进行了比较。除了Zr之外，该模型大致再现了观测到的中子俘获元素的趋势。在一些球状星团中，我们发现热氢燃烧产物（Na、Al）和s过程元素之间存在强烈的相关性，这指向了共享的核合成场所，例如不同质量的渐近巨星分支星和/或快速旋转的大质量恒星。我们还检测到了在场（$\langle$[Eu/Mg]$\rangle$= 0.14 dex）和外来（$\langle$[Eu/Mg]$\langle$= 0.32 dex）球状星团之间[Eu/Mg]比值的显著差异，突显了它们不同的富集历史。最后，平均而言，II型球状星团（NGC 362、NGC 1261和NGC 1851）显示第二代和第一代之间的s过程元素分布比率大约是I型星团的两倍。