Bilinear noise subtraction at the GEO 600 observatory

Mukund, N.; Lough, J. D.; Affeldt, C.; Bergamin, F.; Bisht, A.; Brinkmann, M.; Kringel, V.; Lück, H.; Nadji, S. L.; Weinert, M.; Danzmann, K.

doi:10.1103/physrevd.101.102006

Cited by 11 publications

(9 citation statements)

References 50 publications

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“…As seen in Figure 7, the contribution of these auxiliary channels to the DARM noise is larger than expected based on coherence alone, suggesting nonlinear, bilinear, and/or nonstationary coupling to DARM. Nonstationary coupling has already been observed due to modulation from motion of the angular degrees of freedom, and can be partially removed offline [79,80]. Additional work is required to understand this type of contribution to the interferometer noise floor.…”

Section: G Auxiliary Length Control Noisementioning

confidence: 99%

Sensitivity and performance of the Advanced LIGO detectors in the third observing run

Buikema¹,

Cahillane²,

Mansell³

et al. 2020

Phys. Rev. D

295

262

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On April 1st, 2019, the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), joined by the Advanced Virgo detector, began the third observing run, a year-long dedicated search for gravitational radiation. The LIGO detectors have achieved a higher duty cycle and greater sensitivity to gravitational waves than ever before, with LIGO Hanford achieving angle-averaged sensitivity to binary neutron star coalescences to a distance of 111 Mpc, and LIGO Livingston to 134 Mpc with duty factors of 74.6% and 77.0% respectively. The improvement in sensitivity and stability is a result of several upgrades to the detectors, including doubled intracavity power, the addition of an in-vacuum optical parametric oscillator for squeezed-light injection, replacement of core optics and end reaction masses, and installation of acoustic mode dampers. This paper explores the purposes behind these upgrades, and explains to the best of our knowledge the noise currently limiting the sensitivity of each detector.

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Section: G Auxiliary Length Control Noisementioning

confidence: 99%

Sensitivity and performance of the Advanced LIGO detectors in the third observing run

Buikema¹,

Cahillane²,

Mansell³

et al. 2020

Phys. Rev. D

295

262

View full text Add to dashboard Cite

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“…Despite the auto-alignment system, residual mirror misalignments can couple directly to the strain signal or through the interlinked cavities. One well-known mechanism is bilinear noise coupling [20], where the Michelson misalignment couples via the SR longitudinal degree. Such a coupling pathway exists since the PRC and SRC share the Michelson.…”

Section: Automatic Alignmentmentioning

confidence: 99%

First demonstration of neural sensing and control in a kilometer-scale gravitational wave observatory

Mukund¹,

Lough²,

Bisht³

et al. 2023

Preprint

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Suspended optics in gravitational wave (GW) observatories are susceptible to alignment perturbations and, in particular, to slow drifts over time due to variations in temperature and seismic levels. Such misalignments affect the coupling of the incident laser beam into the optical cavities, degrade both circulating power and optomechanical photon squeezing, and thus decrease the astrophysical sensitivity to merging binaries. Traditional alignment techniques involve differential wavefront sensing using multiple quadrant photodiodes, but are often restricted in bandwidth and are limited by the sensing noise. We present the first-ever successful implementation of neural network-based sensing and control at a gravitational wave observatory and demonstrate low-frequency control of the signal recycling mirror at the GEO 600 detector. Alignment information for three critical optics is simultaneously extracted from the interferometric dark port camera images via a CNN-LSTM network architecture and is then used for MIMO control using soft actor-critic-based deep reinforcement learning. Overall sensitivity improvement achieved using our scheme demonstrates deep learning's capabilities as a viable tool for real-time sensing and control for current and next-generation GW interferometers.

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“…Weiner filtering is particularly useful in cases where a linear coupling exists between the noise source and the gravitational-wave strain data. Additional subtraction procedures based on machine learning [127][128][129] are also being explored. These new methods have shown promise in subtracting sources of noise that exhibit non-linear couplings to the gravitational-wave strain.…”

Section: Noise Subtractionmentioning

confidence: 99%

Detector Characterization and Mitigation of Noise in Ground-Based Gravitational-Wave Interferometers

Davis

Walker

2022

Galaxies

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Since the early stages of operation of ground-based gravitational-wave interferometers, careful monitoring of these detectors has been an important component of their successful operation and observations. Characterization of gravitational-wave detectors blends computational and instrumental methods of investigating the detector performance. These efforts focus both on identifying ways to improve detector sensitivity for future observations and understand the non-idealized features in data that has already been recorded. Alongside a focus on the detectors themselves, detector characterization includes careful studies of how astrophysical analyses are affected by different data quality issues. This article presents an overview of the multifaceted aspects of the characterization of interferometric gravitational-wave detectors, including investigations of instrumental performance, characterization of interferometer data quality, and the identification and mitigation of data quality issues that impact analysis of gravitational-wave events. Looking forward, we discuss efforts to adapt current detector characterization methods to meet the changing needs of gravitational-wave astronomy.

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Bilinear noise subtraction at the GEO 600 observatory

Cited by 11 publications

References 50 publications

Sensitivity and performance of the Advanced LIGO detectors in the third observing run

Sensitivity and performance of the Advanced LIGO detectors in the third observing run

First demonstration of neural sensing and control in a kilometer-scale gravitational wave observatory

Detector Characterization and Mitigation of Noise in Ground-Based Gravitational-Wave Interferometers

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