Pixelated Dark Energy
Jonathan J. Heckman, Craig Lawrie, Ling Lin, Jeremy Sakstein, Gianluca Zoccarato
TL;DR
This work presents a UV-complete cosmological model derived from F-theory on Spin(7) that replaces the inflaton with a pixelated spacetime built from wrapped five-branes, yielding a radiatively stable cosmological constant scaling as $\\Lambda \\sim 1/N$. Inflation and reheating arise from rare flux-pixel jumps that generate radiation and rapidly increase the pixel count, while late-time dark energy evolves with a time-dependent equation of state $w= -1 + rac{\\dot N}{3 H N}$, and a global relation $w_a = -\frac{3}{2}\\Omega_{m,0}(1+w_0)$; observational bounds from Planck and DES accommodate this behavior. The model predicts a large-$l$ cutoff $l_{\rm max} \\sim O(N)$ in the angular power spectrum and provides a microscopic, holographic description of de Sitter thermodynamics with $S_{\rm obs} \\sim N$ and $T_{\rm obs} \\sim 1/\\sqrt{N}$. A 1D pixel matrix model captures the dynamics of pixel/hole transitions, winding/unwinding processes, and their coupling to radiation, offering a framework to connect stringy microphysics to cosmological observables and potentially detectable gravitational signatures. Overall, the pixel cosmology links UV string theory to testable cosmological phenomenology, including a measurable time variation in dark energy and high-$l$ structure in the CMB.
Abstract
We study the phenomenology of a recent string construction with a quantum mechanically stable dark energy. A mild supersymmetry protects the vacuum energy but also allows $O(10 - 100)$ TeV scale superpartner masses. The construction is holographic in the sense that the 4D spacetime is generated from "pixels" originating from five-branes wrapped over metastable five-cycles of the compactification. The cosmological constant scales as $Λ\sim 1/N$ in the pixel number. An instability in the construction leads to cosmic expansion. This also causes more five-branes to wind up in the geometry, leading to a slowly decreasing cosmological constant which we interpret as an epoch of inflation followed by (pre-)heating when a rare event occurs in which the number of pixels increases by an order one fraction. The sudden appearance of radiation triggers an exponential increase in the number of pixels. Dark energy has a time varying equation of state with $w_a=-3Ω_{m,0}(1+w_0)/2$, which is compatible with current bounds, and could be constrained further by future data releases. The pixelated nature of the Universe also implies a large-$l$ cutoff on the angular power spectrum of cosmological observables with $l_{\rm max} \sim O(N)$. We also use this pixel description to study the thermodynamics of de Sitter space, finding rough agreement with effective field theory considerations.
