Constraints on the dark energy equation of state from the imprint of baryons on the power spectrum of clusters

Abstract

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 $\Lambda$ 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 ($z\sim 1$), 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.

arXiv commentaccepted by MNRAS; colour versions of plots included

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