Dark energy constraints from the thermal Sunyaev-Zeldovich power spectrum

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 marginalizing 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 Omega(m) and sigma(8)). We find that the amplitude of the tSZ power spectrum at l less than or similar to 10(3) depends primarily on F = sigma(8)(Omega(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 per cent precision, F = 0.460 +/- 0.012 (68 per cent 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 +/- 0.12, sigma(8) = 0.802 +/- 0.037, and Omega(m) = 0.265 +/- 0.022 (68 per cent 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 Lambda cold dark matter model, the mass bias of B = 1.71 +/- 0.17, i. e. 1 - b = 0.58 +/- 0.06 (68 per cent CL).