On the intensity interferometry and the second-order correlation function $g^{(2)}$ in astrophysics

TL;DR

This paper explores the potential of second-order correlation functions in astrophysics, suggesting that quantum optical properties of light from cosmic sources could reveal new information beyond traditional first-order coherence measurements.

Contribution

It introduces the application of second-order correlation function g^(2) to astrophysical sources, highlighting its potential to uncover non-classical light properties in cosmic phenomena.

Findings

g^(2) offers richer information than traditional intensity measurements

Microquasars are promising targets for observing non-thermal light

Potential to test quantum optical properties in astrophysical contexts

Abstract

Most observational techniques in astronomy can be understood as exploiting the various forms of the first-order correlation function g^(1). As however demonstrated by the Narrabri Stellar Intensity Interferometer back in the 1960's by Hanbury Brown & Twiss, and which is the first experiment to measure the second-order correlation function g^(2), light can carry more information than simply its intensity, spectrum and polarization. Since this experiment, theoretical and laboratory studies of non-classical properties of light have become a very active field of research, namely quantum optics. Despite the variety of results in this field, astrophysics remained focused essentially on first-order coherence. In this paper, we study the possibility that quantum properties of light could be observed in cosmic sources. We provide the basic mathematical ingredients about the first and the second order correlation functions, applied to the modern context of astronomical observations. The exploitation of g^(2) is certainly richer than what a modern intensity interferometer could bring and is particularly interesting for sources of non-thermal light. We conclude by briefly presenting why microquasars in our galaxy and their extragalactic parents can represent an excellent first target in the optical/near-infrared where to observe non-thermal light, and test the use of g^(2) in astrophysical sources.