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SN 2005kd is among the most luminous supernovae (SNe) to be discovered atX-ray wavelengths. We have re-analysed all good angular resolution (better than$20"$ FWHM PSF) archival X-ray data for SN 2005kd. The data reveal an X-raylight curve that decreases as t$^{-1.62 \pm 0.06}$. Our modelling of the datasuggests that the early evolution is dominated by emission from the forwardshock in a high-density medium. Emission from the radiative reverse shock isabsorbed by the cold dense shell formed behind the reverse shock. Our resultssuggest a progenitor with a mass-loss rate towards the end of its evolution of$\ge$ 4.3 $\times$ 10$^{-4} M_{\odot} \,{\rm yr}^{-1}$, for a wind velocity of10 km s$^{-1}$, at 4.0 $\times$ 10$^{16}$ cm. This mass-loss rate is too highfor most known stars, except perhaps hypergiant stars. A higher wind velocitywould lead to a correspondingly higher mass-loss rate. A Luminous Blue Variablestar undergoing a giant eruption could potentially fulfill this requirement,but would need a high mass-loss rate lasting for several hundred years, andneed to explain the plateau observed in the optical light curve. The lattercould perhaps be due to the ejecta expanding in the dense circumstellarmaterial at relatively small radii. These observations are consistent with thefact that Type IIn SNe appear to expand into high density and high mass-lossrate environments, and also suggest rapid variability in the wind mass-lossparameters within at least the last 5000 years of stellar evolution prior tocore-collapse.

X-Ray and Radio Emission from the Luminous Supernova 2005kd