Probable Values of the Cosmological Constant in a Holographic Theory

We point out that for a large class of universes, holography implies that the most probable value for the cosmological constant is zero. In four space-time dimensions, the probability distribution takes the Baum-Hawking form, $\mathrm{dP}\ensuremath{\sim}\mathrm{exp}({\mathrm{cM}}_{p}^{2}/\ensuremath{\Lambda})d\ensuremath{\Lambda}$.

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