The importance of chemical characterization for studying the history of the Milky Way (MW) and its accretion events is well established. However, challenges remain, especially at lower metallicities. N-capture elements carry insightful information concerning chemical evolution, but their distribution especially in very MW metal-poor stars shows a large dispersion in chemical space that chemical evolution models are still not able to explain. One of the possibilities may be the diversity of accreted satellites that contributed to the actual MW stellar composition. In this scenario, I am investigate the role of the interaction between the Sagittarius dwarf spheroidal galaxy (dSph) and the MW in its structure and chemical evolution. For this purpose I observed a sample of around 100 Sagittarius stars (-2 < [Fe/H] < -0.5) with FLAMES to derive precise chemical abundances, specifically the pure r-process element Eu and the neutron-capture first and second peak s-process elements (Y, Zr, Ba, La). These analysis can shed light on the star formation history of Sagittarius and on its contribution to the MW build-up. Moreover, the determination of the [α/Fe]-knee position, still not well characterized in the literature can help us to gain information about the early evolution and the initial mass function of this system. These studies can be keys results for tracing the evolution of our Galaxy and of other system, e.g dwarf satellites galaxies, with which it interacts.
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