Poster Presentation
Application of dust evolution model with chemical evolution to distant galaxies
Presenter: Erina Kawamoto (Nagoya University)
Galaxies have abundant dust, which absorbs ultraviolet and visible light from stars and reradiates infrared. It is also cooling and contracting the gas to promote star formation. Therefore, the amount, size distribution, and type of dust affect the physical quantities such as star formation efficiency and spectral energy distribution (SED). Therefore, understanding the source and growth process of dust is important for understanding galaxy evolution.
Asano et al. (2013a, b, 2014) developed a theoretical model of dust evolution based on chemical evolution (Asano model), and Nishida et al. (2021) developed a galaxy SED model which adopts the Asano model. In these Asano model and SED model adopt Salpeter IMF (Salpeter, 1955) as the initial mass function (IMF), and reproduced the SED of nearby galaxies such as Milky Way. However, it have not been able to reproduce the SED of many distant galaxies with high dust content.
In this study, we calculate the Asano model and the SED model with a top-heavy IMF instead of the Salpeter IMF. This change increases the fraction of massive stars compared to the calculation of Salpeter IMF. In addition, since massive stars have shorter lifetimes than small-mass stars and emit a large amount of dust into interstellar space, which promotes the growth of dust and star formation. Based on the above, we have created a SED that is more similar to the SEDs of distant galaxies obtained from observations, where ultraviolet and infrared emissions are more prominent in the young galaxy phase.
asiaa.sinica.edu.tw