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We compare two different methods of constraining the characteristic velocityand spatial scales of gas motions in the X-ray bright, nearby Centauruscluster, using new deep (760ks) Chandra observations. The power spectrum ofexcess surface brightness fluctuations in the 0.5-6.0 keV band in a sector tothe west is measured and compared to theoretical expectations for Kolmogorovindex fluctuations. The observed power spectrum is flatter than theseexpectations, and the surface brightness fluctuations are around the 8 percentlevel on length scales of 2 kpc. We convert the 2D power spectrum offluctuations into a 3D power spectrum using the method of Churazov et al., andthen convert this into constraints on the one-component velocity of the gasmotions as a function of their length scale. We find one-component velocitiesin the range 100-150 km/s on spatial scales of 4-10 kpc. An independentconstraint on the characteristic velocity and length scales of the gas motionsis then found by considering the diffusion coefficient needed to explain thedistribution of metals in the Centaurus cluster, combined with the need tobalance the rate of gas cooling with the rate of heat dissipated by the gasmotions. We find that these two methods of constraining the velocity and lengthscales of the gas motions are in good agreement.

Constraining gas motions in the Centaurus cluster using X-ray surface brightness fluctuations and metal diffusion