Probing Spacetime Foam with Extragalactic Sources of High-Energy Photons

TL;DR

This paper reviews methods to observationally constrain spacetime foam models by analyzing phase distortions in light from distant high-energy sources, exploring effects on image quality and interferometric measurements.

Contribution

It proposes new observational strategies using ultra-high energy photons and interferometry to detect spacetime foam effects on light wave-fronts from distant sources.

Findings

Ultra-high energy photons can reveal spacetime foam effects.

Wave-front distortions may cause distant objects to become undetectable.

Interferometry can detect phase fluctuations caused by spacetime foam.

Abstract

Quantum fluctuations can endow spacetime with a foamy structure. In this review article we discuss our various proposals to observationally constrain models of spacetime foam. One way is to examine if the light wave-front from a distant quasar or GRB can be noticeably distorted by spacetime-foam-induced phase incoherence. As the phase fluctuations are proportional to the distance to the source, but inversely proportional to the wavelength, ultra-high energy photons ($>1$ TeV) from distant sources are particularly useful. We elaborate on several proposals, including the possibility of detecting spacetime foam by observing "seeing disks" in the images of distant quasars and active galactic nuclei. We also discuss the appropriate distance measure for calculating the expected angular broadening. In addition, we discuss our more recent work in which we investigate whether wave-front distortions on small scales (due to spacetime foam) can cause distant objects become undetectable because the phase fluctuations have accumulated to the point at which image formation is impossible. Another possibility that has recently become accessible is to use interferometers to observe cosmologically distant sources, therefore giving a large baseline perpendicular to the local wave vector over which the wave front could become corrugated and thus distorted, reducing or eliminating its fringe visibility. We argue that all these methods ultimately depend on the availability of ways (if any) to carry out proper averaging of contributions from different light paths from the source to the telescope.