Upper limits on a stochastic gravitational-wave background using LIGO and Virgo interferometers at 600-1000 Hz

J. Abadie; N. A. Lockerbie; K. V. Tokmakov; LIGO Scientific Collaboration; Virgo Collaboration

doi:10.1103/PhysRevD.85.122001

Upper limits on a stochastic gravitational-wave background using LIGO and Virgo interferometers at 600-1000 Hz

J. Abadie, N. A. Lockerbie, K. V. Tokmakov, LIGO Scientific Collaboration, Virgo Collaboration

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Abstract

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 Omega(GW)(f) = Omega(3)(f/900 Hz)(3), of Omega(3) <0.32, assuming a value of the Hubble parameter of h(100) = 0.71. These new limits are a factor of seven better than the previous best in this frequency band.

Original language	English
Article number	122001
Number of pages	14
Journal	Physical Review D
Volume	85
Issue number	12
DOIs	https://doi.org/10.1103/PhysRevD.85.122001
Publication status	Published - 4 Jun 2012

Keywords

gravitational waves
LIGO scientific collaboration
Hubble telescope
frequency bands

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Abadie-etal-PRD2012-Upper-limits-stochastic-gravitational-wave-background-using-LIGO-VirgoFinal published version, 638 KB

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title = "Upper limits on a stochastic gravitational-wave background using LIGO and Virgo interferometers at 600-1000 Hz",

abstract = "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 Omega(GW)(f) = Omega(3)(f/900 Hz)(3), of Omega(3) <0.32, assuming a value of the Hubble parameter of h(100) = 0.71. These new limits are a factor of seven better than the previous best in this frequency band.",

keywords = "gravitational waves, LIGO scientific collaboration, Hubble telescope, frequency bands",

author = "J. Abadie and Lockerbie, {N. A.} and Tokmakov, {K. V.} and {LIGO Scientific Collaboration} and {Virgo Collaboration}",

note = "J. Abadie et al. (LIGO Scientific Collaboration, Virgo Collaboration) Phys. Rev. D 85, 122001. {\textcopyright}2012 American Physical Society",

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doi = "10.1103/PhysRevD.85.122001",

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AU - Abadie, J.

AU - Lockerbie, N. A.

AU - Tokmakov, K. V.

AU - LIGO Scientific Collaboration

AU - Virgo Collaboration

PY - 2012/6/4

Y1 - 2012/6/4

N2 - 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 Omega(GW)(f) = Omega(3)(f/900 Hz)(3), of Omega(3) <0.32, assuming a value of the Hubble parameter of h(100) = 0.71. These new limits are a factor of seven better than the previous best in this frequency band.

AB - 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 Omega(GW)(f) = Omega(3)(f/900 Hz)(3), of Omega(3) <0.32, assuming a value of the Hubble parameter of h(100) = 0.71. These new limits are a factor of seven better than the previous best in this frequency band.

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KW - LIGO scientific collaboration

KW - Hubble telescope

KW - frequency bands

U2 - 10.1103/PhysRevD.85.122001

DO - 10.1103/PhysRevD.85.122001

M3 - Article

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VL - 85

JO - Physical Review D

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IS - 12

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ER -

Upper limits on a stochastic gravitational-wave background using LIGO and Virgo interferometers at 600-1000 Hz

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