Abstract
Galaxy cluster peculiar velocities can be inferred from high—sensitivity, high—resolution multiple-frequency observations in the 30 to 400 GHz range. While galaxy cluster counts and power spectra are sensitive to the growth factor, peculiar velocities are sensitive to the time—derivative of the growth factor and are hence complementary. Using linear perturbation theory, we forecast constraints on ω m , H 0 and the dark—energy equation of state parameter, w, given 820 densely sampled cluster locations (at z ≅ 1) from a ΛCDM N-body simulation and 820 sparsely sampled cluster locations in a broader redshift range.
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