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Wolf-Rayet stars are known to eject winds. Thus, when a Wolf-Rayet starexplodes as a supernova, a fast, $>30,000$ km/s, shock is expected to be driventhrough a wind. We study the signal expected from a fast supernova shockpropagating through an optically thick wind, and find that the electrons behindthe shock driven into the wind are cooled efficiently, by inverse Compton oversoft photons that were deposited by the radiation mediated shock that crossedthe star. Therefore, the bolometric luminosity is comparable to the kineticenergy flux through the shock, and the spectrum is found to be a power-law,which slope and frequency range depend on the number flux of soft photonsavailable for cooling. Wolf-Rayet supernovae that explode through a thick windhave a high flux of soft photons, producing a flat spectrum, $\nuF_{\nu}=Const$, in the X-ray range $0.1\lesssim T\lesssim 50$ keV. As the shockexpands into an optically thin wind, the soft photons are no longer able tocool the shock that plows through the wind, and the bulk of the emission takesthe form of a standard core-collapse supernova (without a wind). However, asmall fraction of the soft photons is upscattered by the shocked wind andproduces a transient unique X-ray signature.

Spectrum and light curve of a supernova shock breakout through a thick Wolf-Rayet wind