Classification methods for noise transients in advanced gravitational-wave detectors

Powell, J.; Trifirò, D.; Cuoco, E.; Heng, I. S.; Cavaglià, M.

doi:10.1088/0264-9381/32/21/215012

Cited by 93 publications

(114 citation statements)

References 37 publications

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“…The coupling to the differential arm length displacement is given by (8) where N grav is the fluctuation of the local gravity field projected on the arm cavity axis, the factor of 2 accounts for the incoherent sum of noises from the four test masses, G is the gravitational constant, ρ 1800 kg m −3 is the ground density near the mirror, β 10 is a geometric factor, and N sei is the seismic motion near the test mass. Since the ground near the test masses moves by 10 −9 m/ √ Hz at 10 Hz, local gravity fluctuations at this frequency are N grav ≈ 10 −15 m s −2 / √ Hz and the total noise coupled into the gravitational wave channel at 10 Hz is L ≈ 5 × 10 −19 m/ √ Hz.…”

Section: A Seismic and Thermal Noisesmentioning

confidence: 99%

“…These instruments target gravitational waves produced by compact binary coalescences, supernovae, non-axisymmetric pulsars and cosmological background in the audio frequency band, from 10 Hz to 10 kHz [7]. The network of widely separated instruments is required to distinguish gravitational wave signals from intrinsic noise transients [8] and to localize astrophysical sources in the sky [9].…”

Section: Introductionmentioning

confidence: 99%

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Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Мартынов¹,

Hall²,

Abbott³

et al. 2016

Phys. Rev. D

369

268

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The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10 −23 / √ Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophsyical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.

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Section: A Seismic and Thermal Noisesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Мартынов¹,

Hall²,

Abbott³

et al. 2016

Phys. Rev. D

369

268

View full text Add to dashboard Cite

show abstract

“…(3) Glitch-detection strategies based on Bayesian inference (e.g., [103,104]) or machine learning (e.g., [104,105]) (4) Using external triggers from EM or neutrino observations to inform the temporal "on-source window" in which we expect to find GW signals and consequently reduce the time period searched.…”

Section: B the Duty Cycle Of The Detectors Is Not 100%mentioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on the potential sensitivity of prospective detection scenarios for GWs from CCSNe within 5 Mpc, using realistic noise at the predicted sensitivity of the Advanced LIGO and Advanced Virgo detectors for 2015, 2017, and 2019. We quantify the detectability of GWs from CCSNe within the Milky Way and Large Magellanic Cloud, for which there will be an observed neutrino burst. We also consider extreme GW emission scenarios for more distant CCSNe with an associated EM signature. We find that a three-detector network at design sensitivity will be able to detect neutrino-driven CCSN explosions out to ∼5.5 kpc, while rapidly rotating core collapse will be detectable out to the Large Magellanic Cloud at 50 kpc. Of the phenomenological models for extreme GW emission scenarios considered in this study, such as long-lived bar-mode instabilities and disk fragmentation instabilities, all models considered will be detectable out to M31 at 0.77 Mpc, while the most extreme models will be detectable out to M82 at 3.52 Mpc and beyond.

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“…PCA via Singular Value Decomposition (SVD) is applied to the catalog waveforms to create signal models that represent each explosion mechanism. Similar techniques have been used to extract physical parameters of GW signals from binary systems [71][72][73] and in characterizing noise sources in GW detectors [74,75].…”

Section: Smeementioning

confidence: 99%

“…To account for this, we aim to quantify the impact of the number of PCs for each model. This is typically achieved by studying the variance encompassed by each PC, and using the number of PCs that cumulatively contain above some fraction of the total variance [74,81]. However, as this method only uses the waveforms it does not account for the limitations of the analysis method implemented in SMEE.…”

Section: Number Of Pcsmentioning

confidence: 99%

Inferring the core-collapse supernova explosion mechanism with gravitational waves

et al. 2016

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A detection of a core-collapse supernova (CCSN) gravitational-wave (GW) signal with an Advanced LIGO and Virgo detector network may allow us to measure astrophysical parameters of the dying massive star. GWs are emitted from deep inside the core and, as such, they are direct probes of the CCSN explosion mechanism. In this study we show how we can determine the CCSN explosion mechanism from a GW supernova detection using a combination of principal component analysis and Bayesian model selection. We use simulations of GW signals from CCSN exploding via neutrino-driven convection and rapidly-rotating core collapse. Previous studies have shown that the explosion mechanism can be determined using one LIGO detector and simulated Gaussian noise. As real GW detector noise is both non-stationary and non-Gaussian we use real detector noise from a network of detectors with a sensitivity altered to match the advanced detectors design sensitivity. For the first time we carry out a careful selection of the number of principal components to enhance our model selection capabilities. We show that with an advanced detector network we can determine if the CCSN explosion mechanism is neutrino-driven convection for sources in our Galaxy and rapidly-rotating core collapse for sources out to the Large Magellanic Cloud.

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Classification methods for noise transients in advanced gravitational-wave detectors

Cited by 93 publications

References 37 publications

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

Observing gravitational waves from core-collapse supernovae in the advanced detector era

Inferring the core-collapse supernova explosion mechanism with gravitational waves

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