Here we discuss the properties of star cluster winds in the supercritical, catastrophic cooling regime. We demonstrate that catastrophic cooling inhibits superwinds and that after a rapid phase of accumulation of the ejected material within the star-forming volume, a new stationary isothermal regime, supported by the ionizing radiation from the central cluster, is established. The expected appearance of this core/halo supernebula in the visible-line regime and possible late evolutionary tracks of super star cluster winds in the absence of ionizing radiation are thoroughly discussed.