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.

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

References in corpus (39)

• Cosmic Star Formation History
• Theory of Star Formation
• The Atomic to Molecular Transition in Galaxies. II: HI and H_2 Column Densities
• On the Star Formation Efficiency of Turbulent Magnetized Clouds
• Primordial Star Formation under the Influence of Far Ultraviolet Radiation: 1540 Cosmological Halos and the Stellar Mass Distribution
• The Cosmic Baryon and Metal Cycles
• Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions
• The lifecycle of molecular clouds in nearby star-forming disc galaxies
• Ultraviolet Survey of CO and H_2 in Diffuse Molecular Clouds: The Reflection of Two Photochemistry Regimes in Abundance Relationships
• Simulating the formation of molecular clouds. II. Rapid formation from turbulent initial conditions
• On the Density Distribution in Star-forming Interstellar Clouds
• Fast and inefficient star formation due to short-lived molecular clouds and rapid feedback
• HI-to-H2 Transitions and H I Column Densities in Galaxy Star-Forming Regions
• The Atomic to Molecular Transition in Galaxies. I: An Analytic Approximation for Photodissociation Fronts in Finite Clouds
• Radiative recombination data for modelling dynamic finite-density plasmas
• CO-dark gas and molecular filaments in Milky Way type galaxies
• [CII] 158 $\mu$m Emission as a Star Formation Tracer
• Studying the YMC population of M83: how long clusters remain embedded, their interaction with the ISM and implications for GC formation theories
• The impact of chemistry on the structure of high-z galaxies
• The ISM in spiral galaxies: can cooling in spiral shocks produce molecular clouds?
• Turbulent Gas in Lensed Planck-selected Starbursts at redshifts 1-3.5
• Chemical Rates on Small Grains and PAHs: C^+ Recombination and H_2 Formation
• H$\alpha$ Morphologies of Star Clusters: A LEGUS study of HII region evolution timescales and stochasticity in low mass clusters
• Metallicity dependence of the H/H${}_2$ and C${}^{+}$/C/CO distributions in a resolved self-regulating interstellar medium
• The natural emergence of the correlation between H2 and star formation rate surface densities in galaxy simulations
• The Nature of High ${[\mathrm{OIII}]}_{88\mu \mathrm{m}}$/${[\mathrm{CII}]}_{158\mu \mathrm{m}}$ Galaxies in the Epoch of Reionization: Low Carbon Abundance and a Top-Heavy IMF?
• The chemistry of interstellar argonium and other probes of the molecular fraction in diffuse clouds
• A Far Ultraviolet Spectroscopic Explorer Survey of Interstellar Molecular Hydrogen in the Galactic Disk
• Evolving Molecular Cloud Structure and the Column Density Probability Distribution Function
• OH+ and H2O+ absorption toward PKS1830-211
• Atomic carbon as a powerful tracer of molecular gas in the high-redshift Universe: perspectives for ALMA
• Simulating the H2 content of high-redshift galaxies
• An extended [CII] halo around a massive star-forming galaxy at z = 5.3
• Co-evolution of Dust and Chemistry in Galaxy Simulations with a Resolved Interstellar Medium
• Planck's Dusty GEMS. II. Extended [CII] emission and absorption in the Garnet at z=3.4 seen with ALMA
• SUNRISE: The rich molecular inventory of high-redshift dusty galaxies revealed by broadband spectral line surveys
• HD molecules at high redshift: cosmic-ray ionization rate in the diffuse interstellar medium
• Molecular gas properties of Q1700-MD94: a massive, main-sequence galaxy at $z\approx 2$
• Escaping the maze: a statistical sub-grid model for cloud-scale density structures in the interstellar medium

Cited by in corpus (7)

• Atomic and molecular gas as traced by [C II] emission
• Hybrid-chimes: A model for radiative cooling and the abundances of ions and molecules in simulations of galaxy formation
• Simulated [CII] in high-z galaxies
• The [C II] line emission as an interstellar medium probe in the MARIGOLD galaxies
• High$-z$ [OI] emission lines: ColdSIM simulations and ALMA observations
• Constraining the [CII] luminosity function from the power spectrum of line-intensity maps at redshift 3.6
• Dust and gas modelling in radiative transfer simulations of disc-dominated galaxies with RADMC-3D