Left: mid-plane cross-sections of δρ/ρ (percent) for the models with M ~ 0.5. From top to bottom: increasing conduction with f = 0 (hydro), 10^-3, 10^-2, 10^-1 (the latter very similar to the f = 1 run). Middle: same cross-sections but for the module of total velocity (km s^-1). The hydro runs show sharp filamentary density structures produced by the turbulent velocity field, which are later deformed by Kelvin-Helmholtz and Rayleigh-Taylor instabilities. Strong conduction damps these perturbations, while leaving the Kolmogorov cascade of turbulent eddies unaltered. The v and δρ/ρ fields have correlated amplitude but different phases (the density field is the tracer). Right: observed relative line broadening (percent) due to turbulent motions along the y-axis view, , where σ_1D,ew is the projected X-ray emission-weighted velocity dispersion. The forthcoming Astro-H telescope should be able to detect projected turbulent velocities above ~200 km s^-1 or ΔE/E₀> 0.1 percent (FWHM = 1.66 ΔE), using the Fe XXV line.