Characterising stellar haloes of low-mass galaxies
Elisa Tau
Detecting and characterising stellar haloes and substructures in dwarf galaxies provide essential evidence that hierarchical structure formation occurs at all scales. Observationally, this topic is challenging because low-mass galaxies are inherently dim, with their outer regions even fainter. Therefore, theoretical approaches come in handy when studying these structures.
Low-mass galaxies had not been studied in great detail with simulations so far because the resolution needed to carry it out is very high and, until a few years ago, we did not have access to them. The Auriga project recently introduced cosmological hydrodynamical simulations of dwarf galaxies with remarkably high resolution. In this study, we use these simulations to characterise and analyse the stellar haloes of dwarf galaxies, focusing on their material distribution and properties. Additionally, we investigate the evolution of their accreted and in-situ components to comprehend their evolution history and also the stellar populations within their haloes. We propose a possible mechanism for the formation of the in-situ component that we find the stellar halo.
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