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Abstract:
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Within this dissertation results from the analysis of formation, abundance
and evolution of the dwarf galaxies from cosmological simulations will be
presented. We will present results from first cosmological simulation which was
performed and analyzed in its entirety in Serbia. From the obtained results it was
shown how the large scale structure formed, primarily the formation of clusters
of galaxies. Since the clusters of galaxies are dominant structures in the universe,
which are relatively slowly forming in relation to the existence of the universe,
using the Illustris cosmological simulation, with included hydrodynamics, it will
be shown that a significant part of the clusters of galaxies are not in the state
of dynamic equilibrium, as some authors claim, therefore their formation process
continues. The obtained results will be used to divide the clusters of galaxies into
three types: interacting clusters, clusters interacting with smaller groups (weakly
interacting clusters), and clusters of galaxies that are not interacting. As the dwarf
galaxies constitute largest number of galaxies in the universe, notably largest number
in the clusters of galaxies, this raises the question how cluster’s interactions
affect the structure and abundance of a diverse type of dwarf galaxies within them.
After a brief review of today’s known types of dwarf galaxies, we will show that
there is susceptibility of the abundance of dwarf irregular galaxies in relation to
whether the parent cluster of galaxies is in interaction or not. As it is assumed
that the dwarf irregular galaxies are predecessors for the formation of the most
numerous types of dwarf galaxies, this could point to the dominant channel of delivering
these galaxies to clusters of galaxies where they are expected to undergo
morphological transformation. In the end, the discovery of two formation channels
for compact elliptical galaxies in the clusters of galaxies will be presented. The
formation of this type of dwarf galaxies has been the subject of discussion due to
limitations in observations and their compact nature from which it could not be
concluded which process leads to their formation. It has been shown here that
they occur either by tidal stripping of large spiral galaxies after their spiraling into
the cluster of galaxies or forming directly inside clusters from the clouds of gas
which is most probably formed by the accretion of cold gas from the environment. |