Measuring the non-Gaussian stochastic gravitational-wave background: a method for realistic interferometer data

TL;DR

This paper introduces a maximum likelihood estimator to detect and characterize non-Gaussian features in the stochastic gravitational-wave background, helping distinguish between different astrophysical and cosmological sources.

Contribution

A novel maximum likelihood method for measuring non-Gaussianity in the SGWB, applicable to realistic interferometer data with colored noise, extending the stochastic radiometer approach.

Findings

Effective in identifying non-Gaussian signals in simulated data

Robust against colored, non-Gaussian noise in interferometer networks

Generalizes existing stochastic radiometer algorithms

Abstract

A stochastic gravitational-wave background (SGWB) can arise from the superposition of many independent events. If the rate of events per unit time is sufficiently high, the resulting background is Gaussian, which is to say that it is characterized only by a gravitational-wave strain power spectrum. Alternatively, if the event rate is low, we expect a non-Gaussian background, characterized by intermittent sub-threshold bursts. Many experimentally accessible models of the SGWB, such as the SGWB arising from compact binary coalescences, are expected to be of this non-Gaussian variety. Primordial backgrounds from the early universe, on the other hand, are more likely to be Gaussian. Measuring the Gaussianity of the SGWB can therefore provide additional information about its origin. In this paper we introduce a novel maximum likelihood estimator that can be used to estimate the non-Gaussian component of an SGWB signature measured in a network of interferometers. This method can be robustly applied to spatially separated interferometers with colored, non-Gaussian noise. Furthermore, it can be cast as a generalization of the widely used stochastic radiometer algorithm.