Dust SEDs in Milky Way-like galaxies in the IllustrisTNG simulations based on the evolution of grain size distribution

Abstract

To understand how the evolution of grain size distribution in galaxies affects observed dust properties, we apply a post-processing dust evolution model to galaxy merger trees from the IllustrisTNG cosmological hydrodynamical simulation. Our dust model includes stellar dust production, sputtering in hot gas, dust growth by accretion and coagulation in the dense interstellar medium (ISM), and shattering in the diffuse ISM. We decompose the grain size distribution into different dust species depending on the elemental abundances and the dense ISM fraction given by the simulation. In our previous work, we focused on Milky Way (MW) analogs and reproduced the observed MW extinction curve. In this study, we compute dust spectral energy distributions (SEDs) for the MW analogues. Our simulated SEDs broadly reproduce the observed MW SED within their dispersion and so does the observational data of nearby galaxies, although they tend to underpredict the MW SED at short wavelengths where emission is dominated by polycyclic aromatic hydrocarbons (PAHs). We find that metallicity and dense gas fraction are the most critical factors for the SED shape, through their influence on coagulation and shattering.The overall success of our models in reproducing the MW SED further justifies the dust evolution processes included in the model and predicts the dispersion in the SEDs caused by the variety in the assembly history. We also show that the most significant increase in the dust SED occurs between redshifts $z\sim 3$ and 2 in the progenitors of the simulated MW-like galaxies.

10 pages, 8 figure, accepted for publication in MNRAS

References in corpus (30)

• Infrared Emission from Interstellar Dust. IV. The Silicate-Graphite-PAH Model in the Post-Spitzer Era
• Simulating galaxy formation with black hole driven thermal and kinetic feedback
• 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
• A Unified Representation of Gas-Phase Element Depletions in the Interstellar Medium
• The evolution of amorphous hydrocarbons in the ISM: dust modelling from a new vantage point
• Metallicity Effects on Dust Properties in Starbursting Galaxies
• Stellar Evolutionary Effects on the Abundances of PAH and SN-Condensed Dust in Galaxies
• Modelling Dust Evolution in Galaxies with a Multiphase, Inhomogeneous ISM
• Galaxy Simulation with Dust Formation and Destruction
• A Nearby Galaxy Perspective on Dust Evolution. Scaling relations and constraints on the dust build-up in galaxies with the DustPedia and DGS samples
• Detailed dust modelling in the L-Galaxies semi-analytic model of galaxy formation
• Dust scaling relations in a cosmological simulation
• The Polycyclic Aromatic Hydrocarbon Mass Fraction on a 10 pc scale in the Magellanic Clouds
• Updated 34-Band Photometry for the SINGS/KINGFISH Samples of Nearby Galaxies
• Thermal and nonthermal dust sputtering in hydrodynamical simulations of the multiphase interstellar medium
• The origin of dust in galaxies across cosmic time
• The MOSDEF Survey: Metallicity Dependence of the PAH Emission at High Redshift and Implications for 24 micron-inferred IR Luminosities and Star Formation Rates at z~2
• Carriers of the mid-IR emission bands in PNe reanalysed. Evidence of a link between circumstellar and interstellar aromatic dust
• Dust evolution in zoom-in cosmological simulations of galaxy formation
• Self-consistent modelling of aromatic dust species and extinction curves in galaxy evolution
• Evolution of grain size distribution in high-redshift dusty quasars: Integrating large amounts of dust and unusual extinction curves
• Shiva: the dust destruction model
• Populating H${}_2$ and CO in galaxy simulation with dust evolution
• The Origin of the Dust Extinction Curve in Milky Way-like Galaxies
• Evolution of the grain size distribution in galactic discs
• The role of dust destruction and dust growth in the evolution of the interstellar medium
• BEDE: Bayesian Estimates of Dust Evolution For Nearby Galaxies
• Spectral energy distributions of dust and PAHs based on the evolution of grain size distribution in galaxies
• Evolution of the grain size distribution in Milky Way-like galaxies in post-processed IllustrisTNG simulations

Cited by in corpus (3)

• Evolution of grain size distribution with enhanced abundance of small carbonaceous grains in galactic environments
• Cosmic evolution of grain size distribution in galaxies using the ${\nu }^2$GC semi-analytic model
• Observational signatures of the dust size evolution in isolated galaxy simulations