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Future cluster surveys will observe galaxy clusters numbering in the hundredthousands. We consider this work how these surveys can be used to constraindark energy parameters: in particular, the equation of state parameter w andthe non-adiabatic sound speed c_s^2. We demonstrate that, in combination withCosmic Microwave Background (CMB) observations from Planck, cluster surveyssuch as that in the ESA Euclid project will be able to determine atime-independent w with subpercent precision. Likewise, if the dark energysound horizon falls within the length scales probed by the cluster survey, thenc_s^2 can be pinned down to within an order of magnitude. In the course of thiswork, we also investigate the process of dark energy virialisation in thepresence of an arbitrary sound speed. We find that dark energy clustering andvirialisation can lead to dark energy contributing to the total cluster mass atapproximately the 0.1% level at maximum.

Confronting the sound speed of dark energy with future cluster surveys