Calibration of the Advanced LIGO detectors for the discovery of the binary black-hole merger GW150914

Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Ackley, K.; Adams, C.; Addesso, P.; Adhikari, R. X.; Adya, V. B.; Affeldt, C.; Aggarwal, N.; Aguiar, O. D.; Ain, A.; Ajith, P.; Allen, B.; Altin, P. A.; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya, M. C.; Arceneaux, C. C.; Areeda, J. S.; Arun, K. G.; Ashton, G.; Ast, M.; Aston, S. M.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P. T.; Ballmer, S. W.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker, D.; Barr, B.; Barsotti, L.; Bartlett, J.; Bartos, I.; Bassiri, R.; Batch, J. C.; Baune, C.; Behnke, B.; Bell, A. S.; Bell, C.; Berger, B. K.; Bergman, J.; Bergmann, G.; Berry, C. P. L.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Birney, R.; Biscans, S.; Bisht, A.; Biwer, C.; Blackburn, J. K.; Blair, C. D.; Blair, D. G.; Blair, R. M.; Böck, O.; Bodiya, T. P.; Bogan, C.; Bohé, A.; Bojtos, P.; Bond, C.; Bork, R.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. 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L.; Wu, G.; Yablon, J.; Yam, W.; Yamamoto, H.; Yancey, C. C.; Yap, M. J.; Yu, Hang; Zanolin, M.; Zevin, M.; Zhang, F.; Zhang, L.; Zhang, M.; Zhang, Y.; Zhao, C.; Zhou, M.; Zhou, Z.; Zhu, X. J.; Zucker, M. E.; Zuraw, S. E.; Zweizig, J.

doi:10.1103/physrevd.95.062003

Cited by 98 publications

(125 citation statements)

References 33 publications

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“…Errors introduced by mismatches between template waveforms and signals [51] are expected to introduce a similar effect in all detectors, and therefore the effect on the time difference, and localization, is likely to be negligible. On the other hand, errors in the calibration of GW detectors [137] will be uncorrelated, and these errors can significantly impact localization. For instance, roughly one third of the localization error budget for GW150914 was due to strain calibration uncertainty [9,137].…”

Section: Discussionmentioning

confidence: 99%

“…On the other hand, errors in the calibration of GW detectors [137] will be uncorrelated, and these errors can significantly impact localization. For instance, roughly one third of the localization error budget for GW150914 was due to strain calibration uncertainty [9,137]. At high SNR, calibration errors are expected to dominate the overall error budget for localization [51].…”

Section: Discussionmentioning

confidence: 99%

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Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

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The observation of gravitational wave signals from binary black hole and binary neutron star mergers has established the field of gravitational wave astronomy. It is expected that future networks of gravitational wave detectors will possess great potential in probing various aspects of astronomy. An important consideration for successive improvement of current detectors or establishment on new sites is knowledge of the minimum number of detectors required to perform precision astronomy. We attempt to answer this question by assessing the ability of future detector networks to detect and localize binary neutron stars mergers on the sky. Good localization ability is crucial for many of the scientific goals of gravitational wave astronomy, such as electromagnetic follow-up, measuring the properties of compact binaries throughout cosmic history, and cosmology. We find that although two detectors at improved sensitivity are sufficient to get a substantial increase in the number of observed signals, at least three detectors of comparable sensitivity are required to localize majority of the signals, typically to within around 10 deg 2 -adequate for follow-up with most wide field of view optical telescopes.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Mills¹,

Tiwari²,

Fairhurst³

2018

Phys. Rev. D

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“…Accurately reconstructing the gravitational wave signals requires precise and accurate calibration of the responses of the detectors to variations in the relative lengths of the 4-km-long interferometer arms. 4 Extracting the parameters of the events that generated the waves also imposes stringent requirements on detector calibration. 5 The estimated required calibration accuracy for LIGO's initial detection phase was on the order of 5 %, while the requirements for making precision measurements of source parameters are on the order of 0.5 %.…”

Section: Introductionmentioning

confidence: 99%

“…The results of measurement like these are used to model the response of the interferometer to gravitational waves. 4 …”

mentioning

confidence: 99%

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The Advanced LIGO photon calibrators

Karki

Tuyenbayev

Kandhasamy

et al. 2016

Review of Scientific Instruments

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111

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The two interferometers of the Laser Interferometry Gravitaional-wave Observatory (LIGO) recently detected gravitational waves from the mergers of binary black hole systems. Accurate calibration of the output of these detectors was crucial for the observation of these events, and the extraction of parameters of the sources. The principal tools used to calibrate the responses of the second-generation (Advanced) LIGO detectors to gravitational waves are systems based on radiation pressure and referred to as Photon Calibrators. These systems, which were completely redesigned for Advanced LIGO, include several significant upgrades that enable them to meet the calibration requirements of second-generation gravitational wave detectors in the new era of gravitational-wave astronomy. We report on the design, implementation, and operation of these Advanced LIGO Photon Calibrators that are currently providing fiducial displacements on the order of 10 −18 m/ √ Hz with accuracy and precision of better than 1 %.

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Reframing SU(1,1) Interferometry

Caves

2020

Adv Quantum Tech

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interferometry, proposed in a classic 1986 paper by Yurke, McCall, and Klauder [Phys. Rev. A 33, 4033 (1986)], involves squeezing, displacing, and then unsqueezing two bosonic modes. It has, over the past decade, been implemented in a variety of experiments. Here I take SU(1,1) interferometry apart, to see how and why it ticks. SU(1,1) interferometry arises naturally as the two-mode version of active-squeezing-enhanced, back-action-evading measurements aimed at detecting the phase-space displacement of a harmonic oscillator subjected to a classical force. Truncating an SU(1,1) interferometer, by omitting the second two-mode squeezer, leaves a prototype that uses the entanglement of two-mode squeezing to detect and characterize a disturbance on one of the two modes from measurement statistics gathered from both modes. 1 2 (v G /c) 2 2 × 10 −7 , corresponding to a coherence time τ = 1/∆ν 5 × 10 6 τ a , where τ a = 1/ν a is the axion period and thus the period of the cavity mode. One * Electronic address: ccaves@unm.edu arXiv:1912.12530v1 [quant-ph] 28 Dec 2019 II. SU(1,1) INTERFEROMETRY , McCall, and Klauder [32] introduced the notion of SU(1,1) interferometry by replacing the beamsplitters of a standard SU(2) interferometer with active elements now called two-mode squeezers. YurkeA standard interferometer uses beamsplitters acting on a pair of modes, a and b, to send waves down two different paths and to bring those waves into interference after they have received phase shifts that one wants to detect. A standard interferometer is

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Calibration of the Advanced LIGO detectors for the discovery of the binary black-hole merger GW150914

Cited by 98 publications

References 33 publications

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

Localization of binary neutron star mergers with second and third generation gravitational-wave detectors

The Advanced LIGO photon calibrators

Reframing SU(1,1) Interferometry

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