Dark Energy from the Thermal Sunyaev Zeldovich Power Spectrum

Boris Bolliet; Barbara Comis; Eiichiro Komatsu; Juan Francisco Macías-Pérez

doi:10.1093/mnras/sty823

paper

Dark Energy from the Thermal Sunyaev Zeldovich Power Spectrum

arXiv:1712.00788 · doi:10.1093/mnras/sty823

Abstract

We constrain the dark energy equation of state parameter, $w$ , using the power spectrum of the thermal Sunyaev-Zeldovich (tSZ) effect. We improve upon previous analyses by taking into account the trispectrum in the covariance matrix and marginalising over the foreground parameters, the correlated noise, the mass bias $B$ in the Planck universal pressure profile, and all the relevant cosmological parameters (i.e., not just $Ω_{m}$ and $σ_{8}$ ). We find that the amplitude of the tSZ power spectrum at $ℓ ≲ 1 0^{3}$ depends primarily on $F \equiv σ_{8} (Ω_{m} / B)^{0.40} h^{- 0.21}$ , where $B$ is related to more commonly used variable $b$ by $B = (1 - b)^{- 1}$ . We measure this parameter with 2.6\% precision, $F = 0.460 \pm 0.012$ (68% CL). By fixing the bias to $B = 1.25$ and adding the local determination of the Hubble constant $H_{0}$ and the amplitude of the primordial power spectrum constrained by the Planck Cosmic Microwave Background (CMB) data, we find $w = - 1.10 \pm 0.12$ , $σ_{8} = 0.802 \pm 0.037$ , and $Ω_{m} = 0.265 \pm 0.022$ (68% CL). Our limit on $w$ is consistent with and is as tight as that from the distance-alone constraint from the CMB and $H_{0}$ . Finally, by combining the tSZ power spectrum and the CMB data we find, in the $Λ$ Cold Dark Matter (CDM) model, the mass bias of $B = 1.71 \pm 0.17$ , i.e., $1 - b = 0.58 \pm 0.06$ (68% CL).

Accepted version (MNRAS)

Dark Energy from the Thermal Sunyaev Zeldovich Power Spectrum

Abstract

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