In the small-universe limit of Horava-Lifshitz gravity, the Wheeler-DeWitt equation separates and the anisotropy wave functions become normalizable harmonic-oscillator states, predicting small initial anisotropies set by the coupling g_B.
The Wave Function of the Universe and CMB Fluctuations
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The Hartle-Hawking and Tunneling (Vilenkin) wave functions are treated in the Hamiltonian formalism. We find that the leading (i.e. quadratic) terms in the fluctuations around a maximally symmetric background, are indeed Gaussian (rather than inverse Gaussian), for both types of wave function, when properly interpreted. However the suppression of non-Gaussianities and hence the recovery of the Bunch-Davies state is not transparent.
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Anisotropic quantum universe in Ho\v{r}ava-Lifshitz gravity
In the small-universe limit of Horava-Lifshitz gravity, the Wheeler-DeWitt equation separates and the anisotropy wave functions become normalizable harmonic-oscillator states, predicting small initial anisotropies set by the coupling g_B.