Chemistry of Dark Molecular Clouds

Abstract

Recent molecular line surveys, particularly toward the starless core TMC-1 CP (Taurus molecular cloud–1 cyanopolyyne peak), have greatly expanded the inventory of interstellar molecules, revealing numerous isomers and even aromatic species. Their diverse formation pathways—from ion–molecule reactions to the possible fragmentation of carbonaceous grains—remain under debate, linking chemistry to the life cycle of the interstellar medium. Simple tracers such as carbon chains and deuterated ions are used to probe the physical conditions and evolutionary state of nearby filaments and cores, as well as in massive infrared dark clouds. Ice chemistry has also entered a new era with the James Webb Space Telescope : Spatial distributions of ices indicate a connection between catastrophic freezeout, established in the prestellar core L1544, and formation of complex organic molecules. Overall, TMC-1 CP and L1544 are not outliers but representative laboratories of molecular cloud physics and chemistry. Extending these findings across diverse environments, from the Central Molecular Zone to low-metallicity galaxies, is essential for a unified picture of how interstellar chemistry regulates the path from clouds to stars and planets.