Upper limits on a stochastic gravitational-wave background using LIGO<? format?> and Virgo interferometers at 600–1000 Hz
J Abadie, BP Abbott, R Abbott, TD Abbott… - Physical Review D …, 2012 - APS
J Abadie, BP Abbott, R Abbott, TD Abbott, M Abernathy, T Accadia, F Acernese, C Adams…
Physical Review D—Particles, Fields, Gravitation, and Cosmology, 2012•APSA stochastic background of gravitational waves is expected to arise from a superposition of
many incoherent sources of gravitational waves, of either cosmological or astrophysical
origin. This background is a target for the current generation of ground-based detectors. In
this article we present the first joint search for a stochastic background using data from the
LIGO and Virgo interferometers. In a frequency band of 600–1000 Hz, we obtained a 95%
upper limit on the amplitude of Ω GW (f)= Ω 3 (f/900 Hz) 3, of Ω 3< 0.32, assuming a value of …
many incoherent sources of gravitational waves, of either cosmological or astrophysical
origin. This background is a target for the current generation of ground-based detectors. In
this article we present the first joint search for a stochastic background using data from the
LIGO and Virgo interferometers. In a frequency band of 600–1000 Hz, we obtained a 95%
upper limit on the amplitude of Ω GW (f)= Ω 3 (f/900 Hz) 3, of Ω 3< 0.32, assuming a value of …
A stochastic background of gravitational waves is expected to arise from a superposition of many incoherent sources of gravitational waves, of either cosmological or astrophysical origin. This background is a target for the current generation of ground-based detectors. In this article we present the first joint search for a stochastic background using data from the LIGO and Virgo interferometers. In a frequency band of 600–1000 Hz, we obtained a 95% upper limit on the amplitude of , of , assuming a value of the Hubble parameter of . These new limits are a factor of seven better than the previous best in this frequency band.
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