Volume 449, Number 3, April III 2006
|Page(s)||925 - 928|
|Section||Cosmology (including clusters of galaxies)|
|Published online||24 March 2006|
Large-scale galaxy correlations as a test for dark energy
LATT, 14 avenue Édouard Belin, 31400 Toulouse, France e-mail: firstname.lastname@example.org
2 LATT, 14 avenue Édouard Belin, 31400 Toulouse, France e-mail: email@example.com
3 Astrophysics Group, Imperial College, Blackett Laboratory, Prince Consort Road, London SW7 2BW, UK
4 Rudolf Peierls Centre for Theoretical Physics, University of Oxford, 1 Keble Road, Oxford OX1 3NP, UK e-mail: firstname.lastname@example.org
Accepted: 30 December 2005
We have shown earlier that, contrary to popular belief, Einstein-de Sitter (E-deS) models can still fit the WMAP data on the cosmic microwave background provided one adopts a low Hubble constant and relaxes the usual assumption that the primordial density perturbation is scale-free. The recent SDSS measurement of the large-scale correlation function of luminous red galaxies at has however provided a new constraint by detecting a “baryon acoustic peak”. Our best-fit E-deS models do possess a baryonic feature at a similar physical scale as the best-fit ΛCDM concordance model, but do not fit the new observations as well as the latter. In particular the shape of the correlation function in the range ~ Mpc cannot be reproduced properly without violating the CMB angular power spectrum in the multipole range . Thus, the combination of the CMB fluctuations and the shape of the correlation function up to ~ Mpc, if confirmed, does seem to require dark energy for a homogeneous cosmological model based on (adiabatic) inflationary perturbations.
Key words: cosmic microwave background / large-scale structure of Universe / cosmological parameters
© ESO, 2006
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