Constraints on the dark energy equation of state from the imprint of baryons on the power spectrum of clusters
Acoustic oscillations in the baryon-photon fluid leave a signature in the matter power spectrum. The overall shape of the spectrum and the wavelength of the oscillations depend upon the sound horizon scale at recombination. Using the $Λ$ cold dark matter Hubble Volume simulation, we show that the im...
| Main Authors: | , , , , , |
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| Format: | Text |
| Language: | unknown |
| Published: |
arXiv
2005
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| Subjects: | |
| Online Access: | https://dx.doi.org/10.48550/arxiv.astro-ph/0504456 https://arxiv.org/abs/astro-ph/0504456 |
| Summary: | Acoustic oscillations in the baryon-photon fluid leave a signature in the matter power spectrum. The overall shape of the spectrum and the wavelength of the oscillations depend upon the sound horizon scale at recombination. Using the $Λ$ cold dark matter Hubble Volume simulation, we show that the imprint of baryons is visible in the power spectrum of cluster-mass dark matter haloes, in spite of significant differences between the halo power spectrum and the prediction of linear perturbation theory. A measurement of the sound horizon scale can constrain the dark energy equation of state. We show that a survey of clusters at intermediate redshift ($ z\sim1 $), like the Sunyaev-Zeldovich survey proposed by the South Pole Telescope or a red sequence photometric survey with VISTA, could potentially constrain the sound horizon scale to an accuracy of $\sim 2%$, in turn fixing the ratio of the pressure of the dark energy to its density ($w$) to better than $\sim 10%$. Our approach does not require knowledge of the cluster mass, unlike those that depend upon the abundance of clusters. : accepted by MNRAS; colour versions of plots included |
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