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Stars and star formation in the Milky Way system
Dwarf galaxies in the Milky Way (MW) system provide us with important information of the star formation in the early Universe. In particular, extremely metal-poor stars in them are likely to form in the environment that is directly influenced by the first stars. In this thesis, I utilise the semi-analytic code a-sloth to study the properties of these dwarf galaxies. A new star formation model that allows tracking of individual stars is implemented. The star formation efficiency is important in determining the stellar mass of ultra-faint galaxies at z = 0. To better quantify the goodness-of-fit of the physical models, I develop a new analysis method, which utilises the unsupervised clustering. With this method, the results suggest that the fiducial model cannot reproduce the mean metallicity of the dwarf galaxies. A temporary improvement of the model is implemented and the goodness-of-fit improves by a factor of 2, compared to the fiducial model. I further analyse the location of EMP stars of MW/M31-like systems in the hydrodynamical simulation TNG50. The analysis is based on the spatial and kinematic information of stars. I find that EMP stars reside mostly in the Stellar halo in the galaxy, regardless of the definition of EMP stars. The model and analysis methods introduced in this thesis provide a new framework for future works to understand dwarf galaxy formation and stars that reside in them.
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520 Astronomie
520 Astronomy and allied sciences