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The Galaxy is in continuous elemental evolution. Since new elements producedby dying stars are delivered to the interstellar medium, the formation of newenerations of stars and planetary systems is influenced by this metalenrichment. We aim to study the role of the metallicity on the gas phasechemistry of the interstellar medium. Using a system of coupled-ordinarydifferential equations to model the chemical reactions, we simulate theevolution of the abundance of molecules in the gas phase for different initialinterstellar elemental compositions. These varying initial elementalcompositions consider the change in the "elemental abundances" predicted by aself-consistent model of the elemental evolution of the Galaxy. As far as weare aware, this is the first attempt to combine elemental evolution of theGalaxy and chemical evolution of molecular clouds. The metallicity was found tohave a strong effect on the overall gas phase composition. With decreasingmetallicity, the number of long carbon chains was found to increase, thetime-scale on which small molecular species are increases, and the main form ofoxygen changed from O and CO to O2. These effects were found to be mainly dueto the change in electron, H3+, and atomic oxygen abundance.

Modelling the chemical evolution of molecular clouds as a function of metallicity