A combined measurement of cosmic growth and expansion from clusters of galaxies, the CMB and galaxy clustering

Rapetti, David, Blake, Chris, Allen, Steven W., Mantz, Adam, Parkinson, David and Beutler, Florian (2013) A combined measurement of cosmic growth and expansion from clusters of galaxies, the CMB and galaxy clustering. Monthly Notices of the Royal Astronomical Society, 432 2: 973-985. doi:10.1093/mnras/stt514

Author Rapetti, David
Blake, Chris
Allen, Steven W.
Mantz, Adam
Parkinson, David
Beutler, Florian
Title A combined measurement of cosmic growth and expansion from clusters of galaxies, the CMB and galaxy clustering
Journal name Monthly Notices of the Royal Astronomical Society   Check publisher's open access policy
ISSN 0035-8711
Publication date 2013-06-21
Sub-type Article (original research)
DOI 10.1093/mnras/stt514
Open Access Status DOI
Volume 432
Issue 2
Start page 973
End page 985
Total pages 13
Place of publication Oxford, United Kingdom
Publisher Oxford University Press
Collection year 2014
Language eng
Formatted abstract
Combining galaxy cluster data from the ROSAT All-Sky Survey and the Chandra X-ray Observatory, cosmic microwave background (CMB) data from the Wilkinson Microwave Anisotropy Probe, and galaxy clustering data from the WiggleZ Dark Energy Survey, the 6-degree Field Galaxy Survey and the Sloan Digital Sky Survey III, we test for consistency the cosmic growth of structure predicted by General Relativity (GR) and the cosmic expansion history predicted by the cosmological constant plus cold dark matter paradigm (ΛCDM). The combination of these three independent, well-studied measurements of the evolution of the mean energy density and its fluctuations is able to break strong degeneracies between model parameters. We model the key properties of cosmic growth with the normalization of the matter power spectrum, 𝜎8, and the cosmic growth index, 𝛾, and those of cosmic expansion with the mean matter density, Ωm, the Hubble constant, H0, and a kinematical parameter equivalent to that for the dark energy equation of state, 𝓌. For a spatially flat geometry, 𝓌 = −1, and allowing for systematic uncertainties, we obtain 𝜎8 = 0.785 ± 0.019 and 𝛾=0.570(+0.064/−0.063) (at the 68.3 per cent confidence level). Allowing both 𝓌 and 𝛾 to vary we find 𝓌 = −0.950(+0.069/−0.070) and 𝛾 = 0.533 ± 0.080. To further tighten the constraints on the expansion parameters, we also include supernova, Cepheid variable and baryon acoustic oscillation data. For 𝓌 = −1, we have 𝛾 = 0.616 ± 0.061. For our most general model with a free 𝓌, we measure Ωm=0.278(+0.012/−0.011), H0 = 70.0 ± 1.3 km s−1 Mpc−1 and 𝓌 =−0.987(+0.054/−0.053) for the expansion parameters, and 𝜎8 = 0.789 ± 0.019 and 𝛾 = 0.604 ± 0.078 for the growth parameters. These results are in excellent agreement with GR+ΛCDM (𝛾 ≃ 0.55; 𝓌 = −1) and represent the tightest and most robust simultaneous constraint on cosmic growth and expansion to date.
Keyword Cosmological parameters
Cosmology: observations
Dark energy
Large-scale structure of Universe
X-rays: galaxies: clusters
Dark Energy Survey
Oscillation Spectroscopic Survey
Microwave background anisotropies
Baryon acoustic-oscillations
Probe WMAP observations
Observations cosmological interpretation
Redshift-space distortions
Digital Sky Survey
Data release
Q-Index Code C1
Q-Index Status Confirmed Code
Institutional Status UQ

Document type: Journal Article
Sub-type: Article (original research)
Collections: School of Mathematics and Physics
Official 2014 Collection
Version Filter Type
Citation counts: TR Web of Science Citation Count  Cited 21 times in Thomson Reuters Web of Science Article | Citations
Scopus Citation Count Cited 20 times in Scopus Article | Citations
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