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Photometric Calibration and Large-Scale Clustering in the Universe

Published online by Cambridge University Press:  26 July 2016

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

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The machine measurements of UK Schmidt plates have produced two very large galaxy surveys, the APM survey and the Edinburgh-Durham Southern Galaxy Catalogue (or COSMOS survey). These surveys can constrain the power on large scales of ≳ 10h−1 Mpc better than current redshift surveys, simply because such large numbers, ≳ 2 million galaxies to bJ ≤ 20.5, provide very high signal/noise in the estimated two-point correlation function for galaxies. Furthermore, the results for the three-dimensional galaxy two point correlation function, ξ(r), obtained from the measured projected function, ω(θ), should be quite robust for reasonable model number-redshift distributions, N(z), for these magnitude limits (see, e.g., Roche et al. 1993). Another clear advantage of measuring ω(θ) is that it is unaffected by the peculiar velocities of the galaxies, whereas they have an important effect on the corresponding ξ,(s) using galaxy redshift surveys.

Type
Part Six: Calibration: Astrometric and Photometric
Information
Symposium - International Astronomical Union , Volume 161: Astronomy from Wide-Field Imaging , 1994 , pp. 295 - 300
Copyright
Copyright © Kluwer 1994 

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