Abstract
To make quantitative comparisons between the theories of galaxy formation described in Chap. 13 and the observed distribution of galaxies, we need to make assumptions about the spectrum of the fluctuations from which galaxies and larger scale structures formed. The natural way of describing the distribution of galaxies on the large scale is in terms of correlation functions and their associated power spectra. The objective is to relate these properties of the distribution of galaxies at the present day to the spectrum of initial fluctuations which must have been present in the very early Universe. Let us first review the properties of the correlation function of galaxies at the present day, extending our introduction of Sect. 2.2.
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Longair, M.S. (1998). Correlation Functions and the Spectrum of the Initial Fluctuations. In: Galaxy Formation. Astronomy and Astrophysics Library. Springer, Berlin, Heidelberg. https://doi.org/10.1007/978-3-662-03571-9_14
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