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Galaxy Clustering to B = 27M

Published online by Cambridge University Press:  26 July 2016

N. Roche ,
T. Shanks ,
N. Metcalfe  and
R. Fong
N. Roche
Affiliation:
Department of Physics, University of Durham, South Road, Durham DH1 3LE, U.K.
T. Shanks
Affiliation:
Department of Physics, University of Durham, South Road, Durham DH1 3LE, U.K.
N. Metcalfe
Affiliation:
Department of Physics, University of Durham, South Road, Durham DH1 3LE, U.K.
R. Fong
Affiliation:
Department of Physics, University of Durham, South Road, Durham DH1 3LE, U.K.

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The angular two-point correlation function, ω(θ), for galaxies can be used as a probe of their redshift distribution N(z) and, therefore, of galaxy luminosity evolution. Without redshift data, we can still observe the projection onto the two-dimensional sky of the three-dimensional clustering of galaxies. The autocorrelation of this projected distribution is described by ω(θ). Observations have indicated that ω(θ) follows a θ−0.8 power-law (Peebles 1980) and that the index of the power-law remains approximately constant to the faintest limits of photographic surveys (Jones, Shanks & Fong 1987).

Type
Part Thirteen: Properties and Clustering of Galaxies and Clusters
Information
Symposium - International Astronomical Union , Volume 161: Astronomy from Wide-Field Imaging , 1994 , pp. 635 - 643
Copyright
Copyright © Kluwer 1994 

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