Correlated noise in networks of gravitational-wave detectors: Subtraction and mitigation

Thrane, E.; Christensen, N.; Schofield, R. M. S.; Effler, A.

doi:10.1103/physrevd.90.023013

Cited by 80 publications

(134 citation statements)

References 43 publications

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“…In the Supplementary Matrial [51], which includes Refs. [52][53][54][55], we discuss in more detail the removed times and frequencies, the recovery of hardware and software injections, and an analysis of correlated noise due to geophysical Schumann resonances.…”

mentioning

confidence: 99%

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

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255

268

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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 Ω0 < 1.7 × 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. The recent detections of binary black hole (BBH) coalescences by Advanced LIGO [32,33] suggest that the Universe may be rich with coalescing BBHs. While events like GW150914 and GW151226 are loud enough to be clearly detected, we expect there to be many more events that are too far away to be individually resolved and that contribute to the background. Since this BBH population originates from sources that are too distant to be individually detected, the stochastic search probes a distinct population of binaries compared to nearby sources [34]. The background from these binaries provides complementary information to individually resolved binary coalescences [35].In this Letter, we report on the search for an isotropic background using data from Advanced LIGO's first observing run O1. We search for the background by crosscorrelating data streams from the two separate LIGO detectors and looking for a coherent signal. We find no evidence for the background and place the best upper limits to date on the energy density of the background in the LIGO frequency band. We also update the impli-

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mentioning

confidence: 99%

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Abbott¹,

Abbott²,

Abbott³

et al. 2017

Phys. Rev. Lett.

Self Cite

255

268

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“…It is now clear that common magnetic field noise from the Schumann resonances [23,37] may very well inhibit the attempt by Advanced LIGO and Advanced Virgo to measure or set limits on the strength of a stochastic gravitational-wave background [13,14] due to an undesired sensitivity of the instruments to magnetic fields. However, through the observations of the December 12, 2009 positive gigantic jet [20] it became apparent that LIGO and Virgo needed to worry about large magnetic transient events that could possibly create coincident short duration noise events at the different gravitational-wave detectors.…”

Section: Ligo/virgo Datamentioning

confidence: 99%

“…In a search for a SGWB the data from two detectors are correlated over a timescale of many months to year [16]; hence the long-term presence of correlated magnetic field noise from the Schumann resonances would create a systematic error in the SGWB signal search. It has been demonstrated that a search for a SGWB by Advanced LIGO and Advanced Virgo could be corrupted by correlated magnetic field noise [13,14].…”

Section: Introductionmentioning

confidence: 99%

Globally coherent short duration magnetic field transients and their effect on ground based gravitational-wave detectors

Kowalska-Leszczynska

Bizouard

Bulik

et al. 2017

Class. Quantum Grav.

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Abstract. It has been recognized that the magnetic fields from the Schumann resonances could affect the search for a stochastic gravitational-wave background by LIGO and Virgo. Presented here are the observations of short duration magnetic field transients that are coincident in the magnetometers at the LIGO and Virgo sites. Data from low-noise magnetometers in Poland and Colorado, USA, are also used and show short duration magnetic transients of global extent. We measure at least 2.3 coincident (between Poland and Colorado) magnetic transient events per day where one of the pulses exceeds 200 pT. Given the recently measured values of the magnetic coupling to differential arm motion for Advanced LIGO, there would be a few events per day that would appear simultaneously at the gravitational-wave detector sites and could move the test masses of order 10 −18 m. We confirm that in the advanced detector era short duration transient gravitational-wave searches must account for correlated magnetic field noise in the global detector network.

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“…For the widely-separated detectors in Livingston, LA and Hanford, WA, the physical separation (∼ 3000 km) eliminates the coupling of local instrumental and environmental noise between the two detectors, while global disturbances such as electromagnetic resonances are at a sufficiently low level that they are not observable in coherence measurements between the (first-generation) detectors at their design sensitivity [5,[26][27][28][29][30].…”

Section: Introductionmentioning

confidence: 99%

“…This is the first stochastic analysis using LIGO science data that addresses the complications introduced by correlated environmental noise. As discussed in the references [29,30], the coupling of global magnetic fields to non-colocated advanced LIGO detectors could produce significant correlations between them thereby reducing their sensitivity to SGWB by an order of magnitude. We expect the current H1-H2 analysis to provide a useful precedent for SGWB searches with advanced detectors in such (expected) correlated noise environment.…”

Section: Introductionmentioning

confidence: 99%

Searching for stochastic gravitational waves using data from the two colocated LIGO Hanford detectors

Aasi¹,

Abadie²,

Abbott³

et al. 2015

Phys. Rev. D

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Searches for a stochastic gravitational-wave background (SGWB) using terrestrial detectors typically involve cross-correlating data from pairs of detectors. The sensitivity of such cross-correlation analyses depends, among other things, on the separation between the two detectors: the smaller the separation, the better the sensitivity. Hence, a co-located detector pair is more sensitive to a gravitational-wave background than a nonco-located detector pair. However, co-located detectors are also expected to suffer from correlated noise from instrumental and environmental effects that could contaminate the measurement of the background. Hence, methods to identify and mitigate the effects of correlated noise are necessary to achieve the potential increase in sensitivity of co-located detectors. Here we report on the first SGWB analysis using the two LIGO Hanford detectors and address the complications arising from correlated environmental noise. We apply correlated noise identification and mitigation techniques to data taken by the two LIGO Hanford detectors, H1 and H2, during LIGO's fifth science run. At low frequencies, 40 − 460 Hz, we are unable to sufficiently mitigate the correlated noise to a level where we may confidently measure or bound the stochastic gravitational-wave signal. However, at high frequencies, 460 − 1000 Hz, these techniques are sufficient to set a 95% confidence level (C.L.) upper limit on the gravitational-wave energy density of Ω(f ) < 7.7 × 10 −4 (f /900 Hz) 3 , which improves on the previous upper limit by a factor of ∼ 180. In doing so, we demonstrate techniques that will be useful for future searches using advanced detectors, where correlated noise (e.g., from global magnetic fields) may affect even widely separated detectors.

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Correlated noise in networks of gravitational-wave detectors: Subtraction and mitigation

Cited by 80 publications

References 43 publications

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Upper Limits on the Stochastic Gravitational-Wave Background from Advanced LIGO’s First Observing Run

Globally coherent short duration magnetic field transients and their effect on ground based gravitational-wave detectors

Searching for stochastic gravitational waves using data from the two colocated LIGO Hanford detectors

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