Constraining dark energy via baryon acoustic oscillations in the (an)isotropic light-cone power spectrum

Details Constraining dark energy via baryon acoustic oscillations in the (an)isotropic light-cone power spectrum Constraining dark energy via baryon acoustic oscillations in the (an)isotropic light-cone power spectrum

2007-05-02

arxiv.org/abs/0705.0354v2

Astron.Astrophys.487:63-74,2008

Astronomy and Astrophysics

Astrophysics

12 pages, 15 figures. Matches version published by A&A. Expanded significantly compared to the previous version

Scientific paper

10.1051/0004-6361:20077688

The measurement of the scale of the baryon acoustic oscillations (BAO) in the galaxy power spectrum as a function of redshift is a promising method to constrain the equation-of-state parameter of the dark energy w. To measure the scale of the BAO precisely, a substantial volume of space must be surveyed. We test whether light-cone effects are important and whether the scaling relations used to compensate for an incorrect reference cosmology are in this case sufficiently accurate. We investigate the degeneracies in the cosmological parameters and the benefits of using the two-dimensional anisotropic power spectrum. Finally, we estimate the uncertainty with which w can be measured by proposed surveys at redshifts of about z=3 and z=1, respectively. In the simulated survey we find that light-cone effects are small and that the simple scaling relations used to correct for the cosmological distortion work fairly well even for large survey volumes. The analysis of the two-dimensional anisotropic power spectra enables an independent determination to be made of the apparent scale of the BAO, perpendicular and parallel to the line of sight. This is essential for two-parameter w-models, such as the redshift-dependent dark energy model w=w_0+(1-a)w_a. Using Planck priors for the matter and baryon density and Delta(H_0)=5% for the Hubble constant, we estimate that the BAO measurements of future surveys around z=3 and z=1 will be able to constrain, independently of other cosmological probes, a constant w to ~ 12% and ~ 11% (68% c.l.), respectively.

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