Atomic and molecular gas as traced by [C

The latest ALMA and JWST observations provide new information on the birth and evolution of galaxies in the early Universe at the epoch of reionization. Measurements at redshift z > 5 of their cold-gas budget are particularly important because this budget is known to be the main fuel for star formation. A powerful tool for probing the physics characterising galaxies at high redshift is the [C <ns0:sc>II</ns0:sc>] 158 μm emission line. Due to its low excitation potential, [C <ns0:sc>II</ns0:sc>] emission can be produced in photodissociation regions, neutral atomic gas, and molecular clouds. To properly capture the cold-gas processes taking place in these environments (molecule formation, self-shielding, dust grain catalysis, and photoelectric and cosmic-ray heating), we made use of a new set of dedicated hydrodynamic simulations (C<ns0:sc>OLD</ns0:sc>SIM) including time-dependent non-equilibrium chemistry, star formation, stellar evolution, metal spreading, and feedback mechanisms. We were able to accurately track the evolution of H <ns0:sc>I</ns0:sc>, H <ns0:sc>II</ns0:sc> and H2 in a cosmological context and predict the contribution of each gas phase to [C <ns0:sc>II</ns0:sc>] luminosity. We provide formulas that can be used to estimate the mass of molecular and atomic gas from [C <ns0:sc>II</ns0:sc>] detections. Furthermore, we analysed the evolution of conversion factors with galactic properties, such as stellar metallicity, star formation rate, and stellar mass. We demonstrate that [C <ns0:sc>II</ns0:sc>] emission is dominated by H <ns0:sc>I</ns0:sc> gas and that most of the [C <ns0:sc>II</ns0:sc>] luminosity is generated in warm, dense, star-forming regions. We conclude that although [C <ns0:sc>II</ns0:sc>] predominantly traces atomic rather than molecular gas, the [C <ns0:sc>II</ns0:sc>] luminosity remains a robust indicator of the H2 mass.