It all started with tiny quantum flickers on the primal canvas. Inflation — an avalanche-like expansion proposed by Alan Guth — stretched those brushstrokes to the scale of galaxies. For a long time, it was thought the paint had dried: interaction with the cosmological horizon (the boundary of the visible universe) erases quantum fuzziness and builds up entropy (a measure of disorder). The picture became classical and predictable.
But a fresh hypothesis allows that the brushstrokes may never have fully set — a relic quantum blurriness might have survived. To catch it, Andrei Linde and other theorists, including Stephen Hawking, turn to the Wigner function — a sensitive scanner that spots where the paint is still wet. Surprise twist: this tool, invented in 1932 for single particles, can yield negative values — nonsense for an ordinary snapshot, but a sure sign of lingering quantumness.
as written by the authors arXiv:2604.01283
The origin of cosmic structure is widely regarded as quantum, yet the Universe today appears classical. Standard lore attributes this to a "quantum-to-classical" transition on super-horizon scales during inflation. Gravity plays a central role: super-horizon dynamics squeeze quantum states, while the cosmological horizon enforces a system-environment split, leading to decoherence. But are these mechanisms always sufficient? We revisit this question, identifying assumptions and limitations in conventional arguments. We highlight recent work showing that beyond slow roll, non-linear dynamics of cosmological perturbations can generate non-classical features that may survive in observables. This raises the tantalizing possibility that quantum signatures may persist in cosmic structure. We propose a phase-space analysis based on the Wigner function as a concrete route to identifying and probing such signatures.
The Wigner function, proposed in 1932 to describe individual particles, now helps peer into the very first moments of the entire universe.