A fluctuation analysis for optical cluster galaxies - I. Theory

Details A fluctuation analysis for optical cluster galaxies - I. Theory A fluctuation analysis for optical cluster galaxies - I. Theory

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000mnras.319..591w&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 319, Issue 2, pp. 591-605.

Astronomy and Astrophysics

Astronomy

2

Techniques: Image Processing, Galaxies: Clusters: General, Galaxies: Luminosity Function, Mass Function

Scientific paper

It is evident that considerable information exists in astronomical data below the threshold for the detection of individual sources (perhaps set for a `5σ' total detection, or for isophotal detection thresholds of `2σ' above the sky background), and that such information, if descriptive of an underlying population of objects characterized by a relatively small parameter set, could in principle be used to set constraints on these parameters. We therefore derive a general theoretical framework for fluctuation analysis (after the radio astronomers' `P(D)' analysis) of optical imaging data on faint galaxy fields, in particular; on fields containing rich clusters of galaxies, in an attempt to determine the Schechter luminosity function of the dwarf galaxies that dominate the statistics at this magnitude range.

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