Matter Distribution for Power Spectra with Broken Scale Invariance

Details Matter Distribution for Power Spectra with Broken Scale Invariance Matter Distribution for Power Spectra with Broken Scale Invariance

1994-08-31

arxiv.org/abs/astro-ph/9408104v1

Astrophys.J.451:444,1995

Astronomy and Astrophysics

Astrophysics

13 pages, uuencoded tar-compressed file, one additional figure available on request, preprint Fermilab-Pub- 94/262-A

Scientific paper

10.1086/176233

To test the primordial power spectra predicted by a double inflationary model with a break of amplitude $\Delta=3$ at a scale of $2\pi/k\approx 10 \hm$ and CDM as dominant matter content, we perform PM simulations with 128$^3$ particles on a 256$^3$ grid. The broken scale invariance of the power spectra explains the extra power observed in the large-scale matter distribution. COBE-normalized spectra and a linear biasing with $b\approx 2$ are shown to reproduce the reconstructed power spectra from the CfA catalog. Identifying galactic halos with overdensity of approximately two times the cell variance, we can fit the angular correlation function using both the Limber equation and creating a APM-like angular projection with the observed luminosity function. Finally, the higher order moments of the galaxy distribution are shown to fit reasonably well the observed values.

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