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

  title={Measuring the non-Gaussian stochastic gravitational-wave background: A method for realistic interferometer data},
  author={Eric Thrane},
  journal={Physical Review D},
  • E. Thrane
  • Published 2 January 2013
  • Physics
  • Physical Review D
A stochastic gravitational-wave background (SGWB) can arise from the superposition of many independent events. If the fraction of time that events emit in some frequency band is sufficiently high, the resulting background is Gaussian in that band, which is to say that it is characterized only by a gravitational-wave strain power spectrum. Alternatively, if this fraction is low, we expect a non-Gaussian background, characterized by intermittent subthreshold signals. Many experimentally… 

Figures from this paper

Stochastic gravitational wave background : detection methods in non-Gaussian regimes

The new generation of interferometers should allow us to detect stochastic gravitational wave backgrounds that are expected to arise from a large number of random, independent, unresolved events of

Probability distribution of astrophysical gravitational-wave background fluctuations

The coalescence of compact binary stars is expected to produce a stochastic background of gravitational waves (GWs) observable with future GW detectors. Such backgrounds are usually characterized by

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

The collection of individually resolvable gravitational wave (GW) events makes up a tiny fraction of all GW signals that reach our detectors, while most lie below the confusion limit and are

Detection methods for stochastic gravitational-wave backgrounds: a unified treatment

The article considers both Bayesian and frequentist searches using ground-based and space-based laser interferometers, spacecraft Doppler tracking, and pulsar timing arrays; and it allows for anisotropy, non-Gaussianity, and non-standard polarization states.

Polarization-Based Tests of Gravity with the Stochastic Gravitational-Wave Background

The direct observation of gravitational waves with Advanced LIGO and Advanced Virgo offers novel opportunities to test general relativity in strong-field, highly dynamical regimes. One such

On the (In)Efficiency of the Cross-Correlation Statistic for Gravitational Wave Stochastic Background Signals with Non-Gaussian Noise and Heterogeneous Detector Sensitivities

The results suggest that introducing an alternative detection statistic can lead to noticeable sensitivity gains when noise distributions are possibly non-Gaussian and/or when detector sensitivities exhibit substantial differences, a situation that is expected to hold in joint detections from Advanced LIGO and Advanced Virgo, in particular in the early phases of development of the detectors.

Search for the isotropic stochastic background using data from Advanced LIGO’s second observing run

The stochastic gravitational-wave background is a superposition of sources that are either too weak or too numerous to detect individually. In this study we present the results from a

GW150914: Implications for the Stochastic Gravitational-Wave Background from Binary Black Holes.

It is concluded that the stochastic gravitational-wave background from binary black holes, created from the incoherent superposition of all the merging binaries in the Universe, is potentially measurable by the Advanced LIGO and Advanced Virgo detectors operating at their projected final sensitivity.

Optimal Search for an Astrophysical Gravitational-Wave Background

The statistically optimal search strategy is derived (producing minimum credible intervals) for a background of unresolved binaries and this framework independently constrains the merger rate and black hole mass distribution, breaking a degeneracy present in the cross-correlation approach.

Gravitational waves at interferometer scales and primordial black holes in axion inflation

We study the prospects of detection at terrestrial and space interferometers, as well as at pulsar timing array experiments, of a stochastic gravitational wave background which can be produced in



The LIGO Scientific Collaboration

A listing of members of the LIGO Scientific Collaboration is given in the PDF file.

The LCGT Collaboration

A listing of members of the LCGT Collaboration is given in the PDF file.


  • Rev. D 59, 102001
  • 1999


  • Rev. D 67, 082003
  • 2003


  • Rev. D 84, 084004
  • 2011

Harry (for the LIGO Scientific Collaboration), Class

  • Quantum Grav. 27,
  • 2010


  • Rev. D 86, 104007
  • 2012


  • Rev. Lett. 85, 3761
  • 2000

Super-Kamiokande Collaboration), Astrophys

  • J. 697,
  • 2009


  • Rev. D 73, 104024
  • 2006