paper

Redshift-space distortions from the cross-correlation of photometric populations

arXiv:1305.0934 · doi:10.1093/mnras/stu1955

Abstract

Several papers have recently highlighted the possibility of measuring redshift space distortions from angular auto-correlations of galaxies in photometric redshift bins. In this work we extend this idea to include as observables the cross-correlations between redshift bins, as an additional way of measuring radial information. We show that this extra information allows to reduce the recovered error in the growth rate index γby a factor of ~2. Although the final error in γdepends on the bias and the mean photometric accuracy of the galaxy sample, the improvement from adding cross-correlations is robust in different settings. Another factor of 2-3 improvement in the determination of γcan be achieved by considering two galaxy populations over the same photometric sky area but with different biases. This additional gain is shown to be much larger than the one from the same populations when observed over different areas of the sky (with twice the combined area). The total improvement of ~5 implies that a photometric survey such as the Dark Energy Survey should be able to recover γat the 5-10% from the angular clustering in linear scales of two different tracers. It can also constrain the evolution of f(z)xσ_8(z) in few bins beyond z~0.8-0.9 at the 10-15% level per-bin, compatible with recent constrains from lower-z spectroscopic surveys. We also show how further improvement can be achieved by reducing the photometric redshift error.

13 pages, 11 figures. Matches the published version in MNRAS. Minor typos corrected, (Fig. 9) and impact of photo-z uncertainties added. Fig 11 updated. Results un-changed

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