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The chemical and physical evolution of starless and pre-stellar cores are ofparamount importance to understanding the process of star formation. The TaurusMolecular Cloud cores TMC 1-C and TMC 1-CP share similar initial conditions andprovide an excellent opportunity to understand the evolution of the pre-stellarcore phase. We investigated the evolutionary stage of starless cores based onobservations towards the prototypical dark cores TMC 1-C and TMC 1-CP, mappingthem in the CS $3\rightarrow 2$, C$^{34}$S $3\rightarrow 2$, $^{13}$CS$2\rightarrow 1$, DCN $1\rightarrow 0$, DCN $2\rightarrow 1$, DNC $1\rightarrow0$, DNC $2\rightarrow 1$, DN$^{13}$C $1\rightarrow 0$, DN$^{13}$C $2\rightarrow1$, N$_2$H$^+$ $1\rightarrow 0$, and N$_2$D$^+$ $1\rightarrow 0$ transitions.We performed a multi-transitional study of CS and its isotopologs, DCN, and DNClines to characterize the physical and chemical properties of these cores. Westudied their chemistry using the state-of-the-art gas-grain chemical codeNautilus and pseudo time-dependent models to determine their evolutionarystage. Observational diagnostics seem to indicate that TMC 1-C is in a laterevolutionary stage than TMC 1-CP, with a chemical age $\sim$1 Myr. TMC 1-Cshows signs of being an evolved core at the onset of star formation, while TMC1-CP appears to be in an earlier evolutionary stage due to a more recentformation or, alternatively, a collapse slowed down by a magnetic support.

Evolutionary view through the starless cores in Taurus: deuteration in TMC 1-C and TMC 1-CP