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We present the results of a Fourier transform analysis of galaxies from the APM Survey in the magnitude range |17 b_ J 20|. The two-dimensional power spectrum of galaxy clustering is found to obey a power law with |K^-1. 33|, displaying a break at |K 30|, where K is the physical wavenumber on the plane of the sky and has units of inverse radians. We compare this with the power spectrum of the Lick Survey using a scaling relationship. We then recover the three-dimensional power spectrum from the two-dimensional power spectrum and reproduce results that we have previously obtained using the angular correlation function. The APM power spectrum in three dimensions is a power law, |P (k) k^-1. 25|, for wavenumbers |k 0. 2 h Mpc^-1|. It rises above this power law in the range |0. 08 h Mpc^-1 k 0. 2 h Mpc^-1|. At wavenumbers smaller than approximately | 0. 01 h Mpc^-1|, systematic and random errors dominate our estimates of the power spectrum.
Baugh et al. (Tue,) studied this question.