HYACINTH: HYdrogen And Carbon chemistry in the INTerstellar medium in Hydro simulations

Abstract

Aims. We present a new sub-grid model, HYACINTH -- HYdrogen And Carbon chemistry in the INTerstellar medium in Hydro simulations -- for computing the non-equilibrium abundances of ${\mathrm{H}}_2$ and its carbon-based tracers, namely $\mathrm{CO}$, $\mathrm{C}$, and ${\mathrm{C}}^{+}$, in cosmological simulations of galaxy formation. Methods. The model accounts for the unresolved density structure in simulations using a variable probability distribution function of sub-grid densities and a temperature-density relation. Included is a simplified chemical network that has been tailored for hydrogen and carbon chemistry within molecular clouds and easily integrated into large-scale simulations with minimal computational overhead. As an example, we applied HYACINTH to a simulated galaxy at redshift $z\sim 2.5$ in post-processing and compared the resulting abundances with observations. Results. The chemical predictions from HYACINTH are in reasonable agreement with high-resolution molecular-cloud simulations at different metallicities. By post-processing a galaxy simulation with HYACINTH, we reproduced the $\mathrm{H}\mathrm{I}-{\mathrm{H}}_2$ transition as a function of the hydrogen column density $N_{\mathrm{H}}$ for both Milky-Way-like and Large-Magellanic-Cloud-like conditions. Column density maps reveal that $\mathrm{CO}$ is concentrated in the peaks of the ${\mathrm{H}}_2$ distribution, while atomic carbon more broadly traces the bulk of ${\mathrm{H}}_2$ in our post-processed galaxy. Based on both the column density maps and the surface density profiles of the different gas species in the post-processed galaxy, we find that ${\mathrm{C}}^{+}$ maintains a substantially high surface density out to $\sim 10\mathrm{kpc}$ as opposed to other components that exhibit a higher central concentration. This is similar to the extended $[\mathrm{C}\mathrm{II}]$ emission found in some recent observations at high redshifts.

arXiv comment21 pages, 11 figures. Accepted for publication in A&A, version matches accepted version

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