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- W1036796901 abstract "Galaxies are the building blocks of the universe, and we mankind live in the Milky Way which itself is a typical spiral galaxy. If one takes a look at an image photographed by a big telescope, e.g. the Hubble Space Telescope (HST) or the Sloan Digital Sky Survey (SDSS), except for a small fraction of stars in our Milky Way, most of the sources are galaxies. Therefore it is pivotal to understand how galaxies are formed and evolved either to probe the nature of our universe, or to probe the origin of mankind. In the current paradigm of galaxy formation, galaxies are thought to be formed via a two-stage process (White & Rees, 1978). First, small perturbations in the density field believed to originate from quantum fluctuations in the inflation grow and collapse to give rise to a population of virialized dark matter halos. Second, the baryonic mass associated with these halos accumulates at the halo centers via cooling and cold flows, increasing the baryonic densities to a point high enough to form stars, and transforming the baryonic gas into dense aggregates of stars, namely galaxies. Because of the hierarchical nature of structure formation in a CDM cosmogony, dark matter halos merge, giving rise to halos containing multiple galaxies (e.g. clusters), and to galaxygalaxy mergers that are believed to be the main formation channel of elliptical galaxies (Mo et al., 2010). The first stage of this process has been studied in great detail using the (extended) Press-Schechter formalism (Press & Schechter, 1974), spherical and ellipsoidal collapse models and, most importantly, numerical simulations. These studies have provided us with an accurate description of the properties of the CDM halo population, such as their mass function, spatial distribution, formation histories, and internal structure. The second stage of the galaxy formation process is however far less established, mainly because the baryonic processes involved (cooling, star-formation and feedback) are poorly understood. In order to build a coherent picture of galaxy formation, we first need to be able to link the properties of the halo population to those of the galaxy population. In other words, we need to know how dark matter halos are populated by galaxies. There are three different approaches" @default.
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- W1036796901 date "2011-01-01" @default.
- W1036796901 modified "2023-10-17" @default.
- W1036796901 title "Probing the Formation and Evolution of Galaxies via HOD/CLF Models" @default.
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