  Accurate estimation of galaxy cluster masses is a central problem in
cosmology. Turbulence is believed to introduce significant deviations from the
hydrostatic mass estimates. Estimation of turbulence properties is complicated
by projection of the 3D cluster onto the 2D plane of the sky, and is commonly
done in the form of indirect probes from fluctuations in the X-ray surface
brightness and Sunyaev-Zeldovich effect maps. In this paper, we address this
problem using simulations. We examine different methods for estimating the
power spectrum on 2D projected fluctuation data, emulating data projected onto
a 2D plane of the sky, and comparing them to the original, expected 3D power
spectrum. Noise can contaminate the power spectrum of ICM observations, so we
also briefly compare a few methods of reducing noise in the images for better
spectral estimation.
