Co-evolution of Dust and Chemistry in Galaxy Simulations with a Resolved Interstellar Medium

Abstract

Nearby dwarf irregular galaxies are ideal laboratories for studying the interstellar medium (ISM) at low metallicity, which is expected to be common for galaxies at very high redshift being observed by the James Webb Space Telescope. We present the first high-resolution ($\sim 0.2$~pc) hydrodynamical simulations of an isolated low-metallicity ($0.1Z_{\odot }$) dwarf galaxy coupled with a time-dependent chemistry network and a dust evolution model where dust is locally produced and destroyed by various processes. To accurately model carbon monoxide (CO), we post-process the simulations with a detailed chemistry network including the time-dependent effect of molecular hydrogen (H${}_2$). Our model successfully reproduces the observed star formation rate and CO(1-0) luminosity ($L_{\mathrm{CO}}$). We find that dust growth in dense gas is required to reproduce the observed $L_{\mathrm{CO}}$ as otherwise CO would be completely photodissociated. In contrast, the H${}_2$ abundance is extremely small and is insensitive to dust growth, leading to a CO-to-H${}_2$ conversion factor that is only slightly higher than the Milky Way value despite the low metallicity. An observationally inferred dust-to-gas ratio is thus underestimated if adopting the metallicity-dependent CO-to-H${}_2$ conversion factor. The newly-produced dust in dense gas mixes with the ISM through supernova feedback without being completely destroyed by sputtering, which leads to galactic outflows 20% - 50% dustier than the ISM, providing a possible source for intergalactic dust.

arXiv commentApJ accepted. 19 pages, 10 figures

References in corpus (72)

• A Universal Density Profile from Hierarchical Clustering
• On the variation of the Initial Mass Function
• The cosmological simulation code GADGET-2
• Grids of stellar models with rotation - I. Models from 0.8 to 120 Msun at solar metallicity (Z = 0.014)
• Physical Models of Galaxy Formation in a Cosmological Framework
• GIZMO: A New Class of Accurate, Mesh-Free Hydrodynamic Simulation Methods
• The UMIST database for astrochemistry 2012
• A standard stellar library for evolutionary synthesis: I. Calibration of theoretical spectra
• Structure of Stationary Photodissociation Fronts
• Theoretical Challenges in Galaxy Formation
• Gas-to-Dust mass ratios in local galaxies over a 2 dex metallicity range
• A standard stellar library for evolutionary synthesis: II. The M dwarf extension
• The Evolution of the Star-forming Interstellar Medium across Cosmic Time
• Dust Formation and Survival in Supernova Ejecta
• Evolution of interstellar dust and stardust in the solar neighbourhood
• Simulating the formation of molecular clouds. I. Slow formation by gravitational collapse from static initial conditions
• Herschel Survey of Galactic OH+, H2O+, and H3O+: Probing the Molecular Hydrogen Fraction and Cosmic-Ray Ionization Rate
• Low CO Luminosities in Dwarf Galaxies
• On the Relationship Between Molecular Hydrogen and Carbon Monoxide Abundances in Molecular Clouds
• Photodissociation of H2 in Protogalaxies: Modeling Self-Shielding in 3D Simulations
• A systematic metallicity study of DustPedia galaxies reveals evolution in the dust-to-metal ratios
• Intergalactic Dust and Observations of Type Ia Supernovae
• Dust Production and Particle Acceleration in Supernova 1987A Revealed with ALMA
• Measuring the galaxy-mass and galaxy-dust correlations through magnification and reddening
• The Molecular ISM of Dwarf Galaxies on Kiloparsec Scales: A New Survey for CO in Northern, IRAS-detected Dwarf Galaxies
• The Dust-to-Gas and Dust-to-Metals Ratio in Galaxies from z=0-6
• Tracing the total molecular gas in galaxies: [CII] and the CO-dark gas
• TreeCol: a novel approach to estimating column densities in astrophysical simulations
• Dust Destruction in the High-Velocity Shocks Driven by Supernovae in the Early Universe
• Star formation and molecular hydrogen in dwarf galaxies: a non-equilibrium view
• Simulating the dust content of galaxies: successes and failures
• GALEX Ultraviolet Imaging of Dwarf Galaxies and Star Formation
• Modelling Dust Evolution in Galaxies with a Multiphase, Inhomogeneous ISM
• SILCC-Zoom: The dynamical and chemical evolution of molecular clouds
• Galaxy Simulation with Dust Formation and Destruction
• Star formation in metal-poor gas clouds
• Variable interstellar radiation fields in simulated dwarf galaxies: supernovae versus photoelectric heating
• Simulating an Isolated Dwarf Galaxy with Multi-Channel Feedback and Chemical Yields from Individual Stars
• Simulating galactic dust grain evolution on a moving mesh
• Supernova-driven winds in simulated dwarf galaxies
• The GRIFFIN project -- Formation of star clusters with individual massive stars in a simulated dwarf galaxy starburst
• Cosmological simulation with dust formation and destruction
• Astrophysical Weighted Particle Magnetohydrodynamics
• Dense cloud cores revealed by CO in the low metallicity dwarf galaxy WLM
• Dust Destruction by the Reverse Shock in the Cassiopeia A Supernova Remnant
• Approximations for modelling CO chemistry in GMCs: a comparison of approaches
• Dust in the Circumgalactic Medium of Low-Redshift Galaxies
• Dust survival rates in clumps passing through the Cas A reverse shock I: results for a range of clump densities
• IGM metal enrichment through dust sputtering
• Iron and silicate dust growth in the Galactic interstellar medium: clues from element depletions
• The X_CO conversion factor from galactic multiphase ISM simulations
• Modeling the gas-phase chemistry of the transitional disk around HD 141569A
• Interstellar Depletion onto Very Small Dust Grains
• Metallicity dependence of the H/H${}_2$ and C${}^{+}$/C/CO distributions in a resolved self-regulating interstellar medium
• Thermal and nonthermal dust sputtering in hydrodynamical simulations of the multiphase interstellar medium
• Formation of silicon oxide grains at low temperature
• METAL: The Metal Evolution, Transport, and Abundance in the Large Magellanic Cloud Hubble program. III. Interstellar Depletions, Dust-to-Metal, and Dust-to-Gas Ratios Versus Metallicity
• Dependence of $X_{\mathrm{CO}}$ on metallicity, intensity, and spatial scale in a self-regulated interstellar medium
• The challenge of simulating the star cluster population of dwarf galaxies with resolved interstellar medium
• Dust Abundance Variations in the Magellanic Clouds: Probing the Lifecycle of Metals with All-Sky Surveys
• Code Comparison in Galaxy Scale Simulations with Resolved Supernova Feedback: Lagrangian vs. Eulerian Methods
• Dust entrainment in galactic winds
• Formation of star clusters and enrichment by massive stars in simulations of low-metallicity galaxies with a fully sampled initial stellar mass function
• The co-evolution of molecular hydrogen and the grain size distribution in an isolated galaxy
• Dust evolution with MUPPI in cosmological volumes
• DUSTiER (DUST in the Epoch of Reionization): dusty galaxies in cosmological radiation-hydrodynamical simulations of the Epoch of Reionization with RAMSES-CUDATON
• Separate silicate and carbonaceous solids formed from mixed atomic and molecular species diffusing in neon ice
• Magnetic fields do not suppress global star formation in low metallicity dwarf galaxies
• Properties of shocked dust grains in supernova remnants
• Is the molecular KS relationship universal down to low metallicities?
• The efficiency of grain growth in the diffuse interstellar medium
• Cosmic Sands: The Origin of Dusty, Star-forming Galaxies in the Epoch of Reionization

Cited by in corpus (6)

• Atomic and molecular gas as traced by [C II] emission
• HYACINTH: HYdrogen And Carbon chemistry in the INTerstellar medium in Hydro simulations
• The First Star-by-star $N$-body/Hydrodynamics Simulation of Our Galaxy Coupling with a Surrogate Model
• Quokka-based understanding of outflows (QED) -- II. X-ray metallicity gradients as a signature of galactic wind metal loading
• Constraining the halo-ISM connection through multi-transition carbon monoxide line-intensity mapping
• The role of young and evolved stars in the heating of dust in local galaxies