A Flat Space Analogue for the Quantum Origin of Structure

Abstract

The analytic structure of non-Gaussian correlators in inflationary cosmologies has recently been proposed as a test of the quantum origin of structure in the universe. To further understand this proposal, we explore the analogous equal-time in-in correlators in flat space and show they exhibit the same features as their cosmological counterparts. The quantum vacuum is uniquely identified by in-in correlators with a total energy pole and no additional poles at physical momenta. We tie this behavior directly to the S-matrix and show that poles at physical momenta always arise from scattering of particles present in the initial state. We relate these flat-space in-in correlators to the probability amplitude for exciting multiple Unruh-de Witt detectors. Localizing the detectors in spacetime, through the uncertainty principle, provides the energy and momentum needed to excite the vacuum and explains the connection to cosmological particle production. In addition, the entanglement of these detectors provides a probe of the entangled state of the underlying field and connects the properties of the correlators to the range of entanglement of the detectors.

Non-Gaussianities in collider energy flux

“…for a flattened triangle configuration. This should be viewed in analogy with the case of an excited initial state in cosmology [162,163].…”

“…for the tensor case [50]. For example, ghost inflation [153], DBI [154,155], and general higher-derivative operators have non-gaussianities peaked in the equilateral region [32,33,156]; solid inflation is peaked in the squeezed limit [157]; and excited initial states lead to enhanced non-gaussianities in the flattened limit [33,[158][159][160][161][162][163]. This last example has been studied in detail recently, trying to use the absence of enhancement of non-gaussianity in the flattened limit to prove the quantum nature of cosmological fluctuations [162,163].…”

Non-Gaussianities in Collider Energy Flux

“…[32,33] or more recently for the tensor case [50]. For example, ghost inflation [153], DBI [154,155], and general higher-derivative operators have nongaussianities peaked in the equilateral region [32,33,156]; solid inflation is peaked in the squeezed limit [157]; and excited initial states lead to enhanced non-gaussianities in the flattened limit [33,[158][159][160][161][162][163]. This last example has been studied in detail recently, trying to use the absence of enhancement of non-gaussianity in the flattened limit to prove the quantum nature of cosmological fluctuations [162,163].…”

“…Here, we see that the result is maximized for a flattened triangle configuration. This should be viewed in analogy with the case of an excited initial state in cosmology [162,163].…”