A detailed analysis of the Hα emission‐line profile shapes across the whole field of view shows them to be composed of a bright narrow feature [intrinsic full width at half‐maximum (FWHM) ∼50 km s⁻¹] superimposed on a fainter broad component (FWHM ≤300 km s⁻¹). By mapping the properties of each individual component, we investigate the small‐scale structure and properties of the ionized interstellar medium, including reddening, excitation and electron densities, and for the first time find spatial correlations between the line component properties. We discuss in detail the possible mechanisms that could give rise to the two components and these correlations, and conclude that the most likely explanation for the broad emission is that it is produced in a turbulent mixing layer on the surface of the cool gas clumps embedded within the hot, fast‐flowing cluster winds. We discuss implications for the mass‐loading of the flow under these circumstances. The average radial velocity difference between the narrow and broad components is small compared to the linewidths, implying that within the IFU field of view, turbulent motions dominate over large‐scale bulk motions. We are therefore sampling well within the outer bounding shocks of the expanding superbubbles and within the outflow ‘energy injection zone’.