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Our understanding of chemical evolution of stellar populations in the Milky Way has been revolutionised with the advent of improved theoretical models of stellar atmospheres, stellar evolution, and state-of-the-art chemo-dynamical models of the Galaxy. Such advances are more readily used to analyse data acquired through large observational programs, like RAVE, Gaia, and APOGEE, etc. and will be incorporated with future surveys such as SDSS V, 4MOST, and WEAVE providing exquisite information about the chemical structure of the Galactic disc, the halo, and the bulge. The conference will focus on three major topics, which constitute the backbone of observational Galaxy formation studies: spectroscopic diagnostics – such as nucleosynthesis, chemical abundance, and age determination; theoretical and observational aspects of stellar mergers and evolution of massive stars – with particular attention focused towards AT 2017gfo; and reviews on the state-of-the-art in chemo-dynamical modelling in the Milky Way. There will be a special format, where two afternoons will contain `non-conference’ break-out sessions, in which related open questions and hot topics will be discussed.