Observational signatures of the dust size evolution in isolated galaxy simulations

Abstract

We aim to provide observational signatures of the dust size evolution in the ISM. In particular, we explore indicators of the polycyclic aromatic hydrocarbon (PAH) mass fraction ($q_{PAH}$), defined as the mass fraction of PAHs relative to total dust grains. In addition, we validate our dust evolution model by comparing the observational signatures from our simulations to observations. We used the hydrodynamic simulation code, GADGET4-OSAKA to model the dust properties of Milky Way-like and NGC 628-like galaxies representing star-forming galaxies. This code incorporates the evolution of grain size distributions driven by dust production and interstellar processing. Furthermore, we performed post-processing dust radiative transfer with SKIRT based on the simulations to predict the observational properties. We find that the intensity ratio between 8 um and 24 um is correlated with $q_{PAH}$ and can be used as an indicator of PAH mass fraction. However, this ratio is influenced by the radiation field. We suggest the 8 um-to-total infrared intensity ratio ($\nu I_{\nu }(8\mu m)/I$(TIR)) as another indicator, since it is tightly correlated with $q_{PAH}$. Furthermore, we explored the spatially resolved $q_{PAH}$ in the simulated Milky Way-like galaxy using $\nu I_{\nu }(8\mu m)/I$(TIR). We find that the spatially resolved $q_{PAH}$ increases with metallicity at metallicity at Z<0.2 Zsun due to the interplay between accretion and shattering while it decreases at Z>0.2 Zsun because of coagulation. Finally, we compared the above indicators in the NGC 628-like simulation with those observed in NGC 628 by recent observations. Consequently, we find that our simulation underestimates the PAH mass fraction throughout the entire galaxy by a factor of $\sim 8$ on average. This could be due to the efficient loss of PAHs by coagulation in our model.

16 pages, 12 figures, accepted by A&A

References in corpus (44)

• Infrared Emission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era
• A simple model to interpret the ultraviolet, optical and infrared emission from galaxies
• Dust Masses, PAH Abundances, and Starlight Intensities in the SINGS Galaxy Sample
• Grackle: a Chemistry and Cooling Library for Astrophysics
• SKIRT: an Advanced Dust Radiative Transfer Code with a User-Friendly Architecture
• Variations of the Mid-IR Aromatic Features Inside and Among Galaxies
• Environmental Dependence of the Kennicutt-Schmidt Relation in Galaxies
• Stellar Evolutionary Effects on the Abundances of PAH and SN-Condensed Dust in Galaxies
• Dust temperature and mid-to-total infrared color distributions for star-forming galaxies at 0<z<4
• CHAOS I: Direct Chemical Abundances for HII Regions in NGC 628
• Photodissociation and X-Ray Dominated Regions
• The unusual hydrocarbon emission from the early carbon star HD 100764: The connection between aromatics and aliphatics
• The Astrodust+PAH Model: A Unified Description of the Extinction, Emission, and Polarization from Dust in the Diffuse Interstellar Medium
• DustPedia - A Definitive Study of Cosmic Dust in the Local Universe
• Galaxy Simulation with Dust Formation and Destruction
• The PHANGS-JWST Treasury Survey: Star Formation, Feedback, and Dust Physics at High Angular resolution in Nearby GalaxieS
• Old and young stellar populations in DustPedia galaxies and their role in dust heating
• The Magellanic zoo: Mid-infrared Spitzer spectroscopy of evolved stars and circumstellar dust in the Magellanic Clouds
• Carbon-rich dust past the asymptotic giant branch: aliphatics, aromatics, and fullerenes in the Magellanic Clouds
• Modeling Dust and Starlight in Galaxies Observed by Spitzer and Herschel: The KINGFISH Sample
• Dust scaling relations in a cosmological simulation
• The Polycyclic Aromatic Hydrocarbon Mass Fraction on a 10 pc scale in the Magellanic Clouds
• Chemical evolution library for galaxy formation simulation
• PHANGS-JWST First Results: Destruction of the PAH molecules in HII regions probed by JWST and MUSE
• PHANGS-JWST First Results: Variations in PAH Fraction as a Function of ISM Phase and Metallicity
• Osaka Feedback Model: Isolated Disk Galaxy Simulations
• The Galactic Dust-Up: Modeling Dust Evolution in FIRE
• Self-consistent modelling of aromatic dust species and extinction curves in galaxy evolution
• X-ray radiative transfer in full 3D with SKIRT
• High-resolution synthetic UV-submm images for simulated Milky Way-type galaxies from the Auriga project
• UV to submillimetre luminosity functions of TNG50 galaxies
• High-resolution synthetic UV-submm images for Milky Way-mass simulated galaxies from the ARTEMIS project
• The atomic-to-molecular hydrogen transition in the TNG50 simulation: Using realistic UV fields to create spatially resolved HI maps
• The co-evolution of molecular hydrogen and the grain size distribution in an isolated galaxy
• A Framework for Modeling Polycyclic Aromatic Hydrocarbon Emission in Galaxy Evolution Simulations
• Self-consistent dust and non-LTE line radiative transfer with SKIRT
• Effects of Spatial Discretization in Lyman-alpha Line Radiation Transfer Simulations
• Dust diffusion in SPH simulations of an isolated galaxy
• Coagulation-Fragmentation Equilibrium for Charged Dust: Abundance of Submicron Grains Increases Dramatically in Protoplanetary Disks
• Dust grain size evolution in local galaxies: a comparison between observations and simulations
• Evolution of grain size distribution with enhanced abundance of small carbonaceous grains in galactic environments
• A new galaxy spectral energy distribution model consistent with the evolution of dust
• Metallicity-PAH Relation of MIR-selected Star-forming Galaxies in AKARI North Ecliptic Pole-wide Survey
• Dust SEDs in Milky Way-like galaxies in the IllustrisTNG simulations based on the evolution of grain size distribution

Cited by in corpus (2)

• The multi-wavelength Tully-Fisher relation in the TNG50 cosmological simulation
• CO-to-H${}_2$ conversion factor and grain size distribution through the analysis of ${\alpha }_{\mathrm{CO}}$-$q_{\mathrm{PAH}}$ relation