Oral Presentation
Exploring SED evolution considering the dust Size Evolution of a zoom-in galaxy simulation with Gadget4-Osaka
Presenter: Kosei Matsumoto (Ghent University)
Dust within the interstellar medium (ISM) holds significant importance in revealing the observed characteristics of galaxies, yet the evolution of dust itself within galaxies and its manifestation as observable properties remain elusive. To address these problems, we employ a hydro-simulation code, Gadget4-Osaka, to model the evolution of grain size distribution within the framework of galaxy evolution. Subsequently, we conduct post-processing dust radiative transfer simulations using SKIRT based on the developed model. Gadget4-Osaka encompasses AGN and star-formation feedback models, as well as dynamic dust evolution: the production of dust from Supernova and AGB stars and interstellar dust processing such as accretion, shattering, coagulation, and sputtering.
In a previous study (Matsumoto et al., 2024), we applied this framework to simulate an isolated galaxy reperesenting the Milky Way galaxy, observing the progressive production of small grains, including polycyclic aromatic hydrocarbons (PAHs), through the shattering of larger grains over time. Consequently, distinct PAH features emerged within the spectral energy distribution (SED) of the galaxy at the later galaxy evolutionary stage. However, the influences of gas accretion flows from the Intergalactic medium, galaxy mergers, and starburst on dust evolution have not been considered in the simulation. Thus, we also conduct a zoom-in simulation of a Milky Way-like galaxy throughout cosmic time and examine these effects. Furthermore, we discuss the spectral characteristics present in the SED of the galaxy across various galaxy evolutionary stages.
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