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As stellar compositions evolve over time in the Milky Way, so will theresulting planet populations. In order to place planet formation in the contextof Galactic chemical evolution, we make use of a large ($N = 5\,325$) stellarsample representing the thin and thick discs, defined chemically, and the halo,and we simulate planet formation by pebble accretion around these stars. Webuild a chemical model of their protoplanetary discs, taking into account therelevant chemical transitions between vapour and refractory minerals, in orderto track the resulting compositions of formed planets. We find that the massesof our synthetic planets increase on average with increasing stellarmetallicity [Fe/H] and that giant planets and super-Earths are most commonaround thin-disc ($\alpha$-poor) stars since these stars have an overall higherbudget of solid particles. Giant planets are found to be very rare($\lesssim$1\%) around thick-disc ($\alpha$-rich) stars and nearly non-existentaround halo stars. This indicates that the planet population is more diversefor more metal-rich stars in the thin disc. Water-rich planets are less commonaround low-metallicity stars since their low metallicity prohibits efficientgrowth beyond the water ice line. If we allow water to oxidise iron in theprotoplanetary disc, this results in decreasing core mass fractions withincreasing [Fe/H]. Excluding iron oxidation from our condensation model insteadresults in higher core mass fractions, in better agreement with the core-massfraction of Earth, that increase with increasing [Fe/H]. Our work demonstrateshow the Galactic chemical evolution and stellar parameters, such as stellarmass and chemical composition, can shape the resulting planet population.

Planet formation throughout the Milky Way: Planet populations in the context of Galactic chemical evolution