Locating the Baryon Acoustic Peak
arXiv:0901.3085 · doi:10.1103/PhysRevD.79.063508
Abstract
Forthcoming photometric redshift surveys should provide an accurate probe of the acoustic peak in the two-point galaxy correlation function, in the form of angular clustering of galaxies within a given shell in redshift space. We investigate the form of the anticipated signal, quantifying the distortions that arise due to projection effects, and in particular explore the validity of applying the Limber approximation. A single-integral prescription is presented, which provides an alternative to Limber's equation, and produces a significantly improved prediction in the regime of interest. The position of the acoustic peak within the angular correlation function relates to the angular diameter distance to the far side of the redshift bin. Thicker redshift bins therefore shift comoving features towards smaller angular scales. As a result, the value of the photometric redshift error acquires a greater significance, particularly at lower redshifts. In order to recover the dark energy equation of state to a level of 1%, we find the total redshift dispersion must be determined to within Δσ_z ~ 10^-3, which may prove challenging to achieve in practice.
8 pages, 7 figures, minor changes reflect published version
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Cited by in corpus (6)
- Modeling the angular correlation function and its full covariance in Photometric Galaxy Surveys
- Tracing The Sound Horizon Scale With Photometric Redshift Surveys
- The effect of redshift-space distortions on projected 2-pt clustering measurements
- Large-scale analysis of the SDSS-III DR8 photometric luminous galaxies angular correlation function
- Using galaxy pairs as cosmological tracers
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