Matter distribution for power spectra with broken scale invariance

Journal Article · Sun Oct 01 04:00:00 EDT 1995 · Astrophysical Journal

DOI:https://doi.org/10.1086/176233· OSTI ID:278461

Amendola, L ^[1]; Gottloeber, S ^[2]; Muecket, J P; Mueller, V ^[3]

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1. Osservatorio Astronomico di Roma, Viale del Parco Mellini, 84, I-00136 Rome (Italy)
2. Astrophysical Institute Potsdam, An der Sternwarte 16, D-14482 Potsdam (Germany)
3. Astrophyical Institute Potsdam, An der Sternwarte 16, D-14482 Potsdam (Germany)

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}/{ital k}{approx_equal}10 {ital h}{sup {minus}1} Mpc and cold dark matter (CDM) as dominant matter content, we perform particle-mesh simulations with 128{sup 3} particles on a 256{sup 3} grid. The broken scale invariance of the power spectra explains the extra power observed in the large-scale matter distribution. {ital COBE}-normalized spectra and a linear biasing with {ital b}{approx_equal}2 are shown to reproduce the reconstructed power spectra from the CfA catalog. By identifying galactic halos with a random selection of particles in overdensity regions of approximately 2 times the cell variance, we can fit the angular correlation function using both the Limber equation and creating an 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. {copyright} {ital 1995 The American Astronomical Society.}

• OSTI ID: 278461
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 2 Vol. 451; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

66 PHYSICS
ANGULAR DISTRIBUTION
CORRELATION FUNCTIONS
GALACTIC HALOS
INFLATIONARY UNIVERSE
LUMINOSITY
LUMINOSITY FUNCTION
NUMERICAL SOLUTION
POWER SPECTRA
SPATIAL DISTRIBUTION