Testing ansatze for Quasi-nonlinear Clustering: the linear APM power spectrum

Details Testing ansatze for Quasi-nonlinear Clustering: the linear APM power spectrum Testing ansatze for Quasi-nonlinear Clustering: the linear APM power spectrum

1996-01-16

arxiv.org/abs/astro-ph/9601085v2

Astronomy and Astrophysics

Astrophysics

5 pages, 4 postscript figures, final version MNRAS Letter in press; also available as postscript file at http://star-www.dur

Scientific paper

We compare the accuracy of published formulae that transform the linear perturbation theory power spectrum into the nonlinear regime against the results of an ensemble of large N-body simulations. We find that the modified transformation given by Jain, Mo and White (1995) performs well for initial fluctuations that have a power law power spectrum, but is less succesful for scale dependent spectra. The inverse transformation to obtain the linear power spectrum is applied to the APM Galaxy Survey power spectrum measured by Baugh \& Efstathiou (1993). The resulting linear spectrum is used to generate the initial density fluctuations in an N-body simulation, which is evolved to match the measured APM amplitude on large scales. We find very good agreement between the final power spectrum of the simulation and the measured APM power spectrum. However, the higher moments for the particle distribution only match the ones recovered from the APM Survey on large scales, $R \simgt 10 \mpc$. On small scales, $R \simlt 10 \mpc$, the APM estimations give smaller amplitudes, indicating that non-gravitational effects, such as biasing, are important on those scales. Our approach can be used to constrain a model of how light from galaxies traces the underlying mass distribution.

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