The three-dimensional power spectrum measured from the APM Galaxy Survey-2. Use of the two-dimensional power spectrum

Details The three-dimensional power spectrum measured from the APM Galaxy Survey-2. Use of the two-dimensional power spectrum The three-dimensional power spectrum measured from the APM Galaxy Survey-2. Use of the two-dimensional power spectrum

Mar 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.267..323b&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 267, no. 2, p. 323-332

Statistics

Computation

98

Dark Matter, Galactic Clusters, Power Spectra, Sky Surveys (Astronomy), Universe, Computational Astrophysics, Fourier Transformation, Integral Equations, Stellar Magnitude

Scientific paper

We present the results of a Fourier transform analysis of galaxies from the APM Survey in the magnitude range 17 less than or = bj less than or = 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 approximately 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) infinity k-1.25, for wavenumbers k greater than or = 0.2 h/Mpc. It rises above this power law in the range 0.08 h/Mpc less than or = k less than or = 0.2h/Mpc. At wavenumbers smaller than approximately 0.01 h/Mpc, systematic and random errors dominate our estimates of the power spectrum.

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