Abstract
We describe three-dimensional Kerr–de Sitter space using similar methods as recently applied to the BTZ black hole. A rigorous form of the classical connection between gravity in three dimensions and two-dimensional conformal field theory is employed, where the fundamental degrees of freedom are described in terms of two dependent SL(2, C) currents. In contrast to the BTZ case, however, quantization does not give the Bekenstein–Hawking entropy connected to the cosmological horizon of Kerr–de Sitter space.
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