Open clusters appear as simple objects in many aspects, with a high degree of homogeneity in their (initial) chemical composition, and the typical solar-scaled abundance pattern for the majority of the chemical species. With ages ranging from few Myr to several Gyr, they represents the ideal tracers of the time evolution of the atomic elements in our Galaxy. One striking singularity is represented by young open clusters (ages less than a few hundred Myr) which exhibit extreme and atypical enhancement in their barium [Ba/Fe] ratios (~0.6-0.7 dex over solar), not followed by the other s-process elements as lanthanum or cerium. Together with this, also the unexpected sub-solar iron [Fe/H] content displayed at such young ages challenges the expections of the Galactic chemical evolution models. The definite explanation for such a peculiar trend is still wanting (and missing), as many solutions have been envisaged. In this talk, I will review the status of the spectroscopic analysis of young stars, presenting new methods and new results, important to enhance the legacy of past, present and future spectroscopic surveys.