Abundance and Clustering of QSOs in Cosmic Structure Formation Models

Details Abundance and Clustering of QSOs in Cosmic Structure Formation Models Abundance and Clustering of QSOs in Cosmic Structure Formation Models

1997-04-04

arxiv.org/abs/astro-ph/9704044v1

Astronomy and Astrophysics

Astrophysics

7 pages, 6 figures, to appeare in A&A

Scientific paper

Combining the observations of spatial abundance and two-point correlation function of QSOs, we can effectively set constraints on models of cosmic structure formation. Both the abundance of gravitationally confined halos and their two-point correlation functions can be calculated in the conventional Press-Schechter formalism. We apply this method to examine the properties of possible host halos of QSOs in three popular models: the standard cold dark matter (SCDM) model, the low density flat cold dark matter (LCDM) model and the cold-plus-hot dark matter (CHDM) model. The LCDM and CHDM models are normalized to the COBE-DMR observations, and the SCDM is normalized to $\sigma = 0.58$. We find that the SCDM and LCDM models can pass the abundance-plus-correlation test for QSOs. However, the CHDM are difficult to produce host halos to fit with the number density of high redshift QSOs and their clustering on large scales (10 h^{-1} Mpc) simultaneously. We studied various mechanisms, originated both gravitationally and non-gravitationally, which may lead to a biasing of the halo clustering. We conclude that these effects are too weak in order to release the trouble of the CHDM models.

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