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This is the second paper in the series that confronts predictions of a model of the landscape with cosmological observations. We show here how the modifications of the Friedmann equation due to the decohering effects of long wavelength modes on the wavefunction of the Universe defined on the landscape leave unique signatures on the CMB spectra and large scale structure (LSS). We show that the effect of the string corrections is to suppress σ 8 and the CMB T T spectrum at large angles, thereby bringing WMAP and SDSS data for σ 8 into agreement.We find interesting features imprinted on the matter power spectrum P(k): power is suppressed at large scales indicating the possibility of primordial voids competing with the ISW effect. Furthermore, power is enhanced at structure and substructure scales, k ≃ 10 −2−0 h Mpc −1 . Our smoking gun for discriminating this proposal from others with similar CMB and LSS predictions come from correlations between cosmic shear and temperature anisotropies, which here indicate a noninflationary channel of contribution to LSS, with unique ringing features of nonlocal entanglement displayed at structure and substructure scales.

We investigate the effects of quantum entanglement between our horizon patch and others due to the tracing out of long wavelength modes in the wavefunction of the Universe as defined on a particular model of the landscape. In this, the first of two papers devoted to this topic, we find that the SUSY breaking scale is bounded both above and below: 10 −10 M P ≤ M SUSY ≤ 10 −8 M P for GUT scale inflation. The lower bound is at least five orders of magnitude larger than the expected value of this parameter and can be tested by LHC physics.

We investigate the Selection of Original Universe Proposal (SOUP) of Tye et al and show that as it stands, this proposal is flawed. The corrections to the Euclidean gravity action that were to select a Universe with a sufficiently large value of the cosmological constant to allow for an inflationary phase only serve to renormalize the cosmological constant so that ! eff . SOUP then predicts a wave function that is highly peaked around eff ! 0, thereby reintroducing the issue of how to select initial conditions allowing for inflation in the early Universe.