Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO's First Observing Run
By The Ligo Scientific Collaboration, T. Abbott, R. Abbott, T. Abbott, M. Abernathy, F. Acernese, K. Ackley, C. Adams, T. Adams, P. Addesso and 983 more. 2016
221 citations recorded by the source corpus.
A wide variety of astrophysical and cosmological sources are expected to contribute to a stochastic gravitational-wave background. Following the observations of GW150914 and GW151226, the rate and mass of coalescing binary black holes appear to be greater than many previous expectations. As a result, the stochastic background from unresolved compact binary coalescences is expected to be particularly loud. We perform a search for the isotropic stochastic gravitational-wave background using data from Advanced LIGO's first observing run. The data display no evidence of a stochastic gravitational-wave signal. We constrain the dimensionless energy density of gravitational waves to be $\Omega_0<1.7\times 10^{-7}$ with 95% confidence, assuming a flat energy density spectrum in the most sensitive part of the LIGO band (20-86 Hz). This is a factor of ~33 times more sensitive than previous measurements. We also constrain arbitrary power-law spectra. Finally, we investigate the implications of this search for the background of binary black holes using an astrophysical model for the background.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/b15a4cc8ef73a192994f56013189d0ef4885a64b
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In Astronomy and Astrophysics
Citations in the corpus
- Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo (2019, unknown): “, [163,164]) target the stochastic GW background signal which is formed by the superposition of a wide variety of independent and unresolved sources from different stages of the evolution of the Universe.”
- A Review of Gravitational Waves from Cosmic Domain Walls (2017, methodology): “7 × 10−7 with 95% confidences for 20–86 Hz by assuming a flat GW spectrum [124], and these limits are about 33 times tighter than the previous limits set by Initial LIGO and Virgo [125].”
- Measuring the Binary Black Hole Mass Spectrum with an Astrophysically Motivated Parameterization (2018, methodology): “Using a (hyper)parameterization that does not accurately describe the true distribution leads to a biased estimate of the fraction of mergers that are individually resolvable and hence the merger rate (Abadie et al. 2010; Abbott et al. 2017a).”
- Generating PBHs and small-scale GWs in two-field models of inflation (2020, methodology): “range of values. result that GW h2 (at least for the highest values of b 1) can be detected simultaneously by the DECIGO/BBO, Magis-AION-space [95], the Einstein Telescope [96], Advanced Ligo + Virgo [97] and CE [98]. We stress again that the height of the peak in GW is only logarithmically dependen”