Volume 460, Number 1, December II 2006
|Page(s)||37 - 44|
|Section||Cosmology (including clusters of galaxies)|
|Published online||12 September 2006|
Large-scale structure and the Cardassian fluid
School of Mathematical Science, Queen Mary, University of London, Mile End road, London E1 4NS, UK e-mail: firstname.lastname@example.org
2 Laboratoire Univers et Théories (LUTH), UMR 8102, Observatoire de Paris, 92195 Meudon Cedex, France
3 Institute of Theoretical Astrophysics, University of Oslo, PO Box 1029 Blindern, 0315 Oslo, Norway e-mail: email@example.com
Accepted: 24 August 2006
In this paper, we confront the predictions of the power law Cardassian model for the baryon power spectrum with the observations of the SDSS galaxy survey. We show that they fit only for very unusual values of the cold dark matter or baryon density parameters, the Hubble parameter or the spectral index of the initial power spectrum. Moreover, the best-fit Cardassian models turn out to be phantom models. If one wants to recover the usual values for these constants, as quoted by the WMAP team, the power law Cardassian model turns out to be indistinguishable from a ΛCDM model.
Key words: cosmology: theory / cosmological parameters / large-scale structure of Universe
© ESO, 2006
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