Abstract
The probability of finding a void in a random volume in a distribution of galaxies is related to the generating function of the sequence of correlation amplitudes. This Letter describes methods for measuring this function from volume-limited or apparent-magnitude-limited data and shows how to deconvolve the observed function to infer an underlying positive definite continuum density distribution ..integral..(p), and hence a consistent sequence of correlation amplitudes, which are proportional to the irreducible moments of the continuum distribution. The method is good for the purpose of determining the distribution ..integral..(p) in underdense regions, p< or approx. =p-bar, but it is inferior (at least for apparent-magnitude-limited data) to traditional methods for measuring correlation amplitudes, which depend mainly on the behavior of f(p) at large p. Conversely, correlation amplitudes provide a poor characterization of ..integral..(p) at small p. The continuum density distribution distribution ..integral..(p) inferred from the CfA redshift catalog of galaxies resembles a lognormal for p
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