One of the most useful statistics employed in studying the statistics of galaxy clustering is the two-point correlation function.This statistic quantifies the clustering of galaxies, and is directly related to the powerspectrum of density fluctuations in the galaxy distribution. Determining the evolution of
the correlation function is therefore essential for an understanding of cosmological structure
formation.[1]
For a given distance, the two-point correlation function is a function of one variable (distance) which describes the probability that two galaxies are separated by this particular distance. It can be thought of as a lumpiness factor - the higher the value for some distance scale, the more lumpy the universe is at that distance scale. [2]
the correlation function is therefore essential for an understanding of cosmological structure
formation.[1]
For a given distance, the two-point correlation function is a function of one variable (distance) which describes the probability that two galaxies are separated by this particular distance. It can be thought of as a lumpiness factor - the higher the value for some distance scale, the more lumpy the universe is at that distance scale. [2]
