Titlebook: Extragalactic Astronomy and Cosmology; An Introduction Peter Schneider Textbook 20061st edition Springer-Verlag Berlin Heidelberg 2006 Cosm

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Introduction and Overview,ge representative of the class of spiral galaxies. Two other examples of spiral galaxies are shown in Fig. 1.1 and Fig. 1.2, one of which we are viewing from above (face-on), the other from the side (edge-on). These are all stellar systems in which the majority of stars are confined to a relatively

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Cosmology I: Homogeneous Isotropic World Models,instead we will turn our attention to the space and time in which these objects are embedded. These considerations will then lead to a world model, the model of our cosmos. .This chapter will deal with aspects of homogeneous cosmology. As we will see, the Universe can, to first approximation, be con

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Clusters and Groups of Galaxies,he projection of bright galaxies on the sky (see Figs. 6.1 and 6.2). The Milky Way itself is a member of a group, called the Local Group (Sect. 6.1), which implies that we are living in a locally overdense region of the Universe.

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Cosmology II: Inhomogeneities in the Universe,ption of a (spatially) homogeneous and isotropic Universe. Of course, the assumption of homogeneity is justified only on large scales because observations show us that our Universe is inhomogeneous on small scales – otherwise no galaxies or stars would exist.

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The Universe at High Redshift, This might have given the impression that, with the determination of the values for ., ., etc., cosmology is nearing its conclusion. As a matter of fact, for several decades cosmologists have considered the determination of the density parameter and the expansion rate of the Universe their prime ta