Quantum correlations between light and the kilogram-mass mirrors of LIGO

Yu, Haocun; McCuller, L.; Tse, M.; Barsotti, L.; Mavalvala, N.; Betzwieser, J.; Blair, C. D.; Dwyer, S. E.; Effler, A.; Evans, M.; Fernandez-Galiana, A.; Fritschel, P.; Frolov, V. V.; Kijbunchoo, N.; Matichard, F.; McClelland, D. E.; McRae, T.; Mullavey, A.; Sigg, D.; Slagmolen, B. J. J.; Whittle, C.; Buikema, A.; Chen, Y.; Corbitt, T. R.; Schnabel, R.; Abbott, R.; Adams, C.; Adhikari, R. X.; Ananyeva, A.; Appert, S.; Arai, K.; Areeda, J. S.; Asali, Y.; Aston, S. M.; Austin, C.; Baer, A. M.; Ball, M.; Ballmer, S. W.; Banagiri, S.; Barker, D.; Bartlett, J.; Berger, B. K.; Bhattacharjee, D.; Billingsley, G.; Biscans, S.; Blair, R. M.; Bode, N.; Booker, P.; Bork, R.; Bramley, A.; Brooks, A. F.; Brown, D. D.; Cahillane, C.; Cannon, K. C.; Chen, X.; Ciobanu, A. A.; Clara, F.; Cooper, S. J.; Corley, K. R.; Countryman, S. T.; Covas, P. B.; Coyne, D. C.; Datrier, L. E. H.; Davis, D.; Fronzo, C. Di; Dooley, K L; Driggers, J. C.; Dupej, P.; Etzel, T.; Evans, T. M.; Feicht, J.; Fulda, P.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Godwin, P.; Goetz, E.; Gras, S.; Gray, C.; Gray, R.; Green, A. C.; Gupta, Anchal; Gustafson, E. K.; Gustafson, R.; Hanks, J.; Hanson, J.; Hardwick, T.; Hasskew, R. K.; Heintze, M. C.; Helmling-Cornell, A. F.; Holland, N. A.; Jones, J. D.; Kandhasamy, S.; Karki, S.; Kasprzack, M.; Kawabe, K.; King, P. J.; Kissel, J. S.; Kumar, Rahul; Landry, M.; Lane, B. B.; Lantz, B.; Laxen, M.; Lecoeuche, Y. K.; Leviton, J. N.; Liu, J.; Lormand, M.; Lundgren, A. P.; Macas, R.; MacInnis, M.; Macleod, D. M.; Mansell, G. L.; Márka, S.; Márka, Z.; Мартынов, Д. В.; Mason, K.; Massinger, T. J.; McCarthy, R.; McCormick, S.; McIver, J.; Mendell, G.; Merfeld, K.; Merilh, E. L.; Meylahn, F.; Mistry, T.; Mittleman, R.; Moreno, G.; Mow–Lowry, C. M.; Mozzon, S.; Nelson, T. J. N.; Nguyen, P.; Nuttall, L. K.; Oberling, J.; Oram, Richard J.; Osthelder, C.; Ottaway, D. J.; Overmier, H.; Palamos, J. R.; Parker, W.; Payne, E.; Pele, A.; Perez, C. J.; Pirello, M.; Radkins, H.; Ramirez, K. E.; Richardson, J. W.; Riles, K.; Robertson, N. A.; Rollins, J. G.; Romel, C. L.; Romie, J. H.; Ross, M. P.; Ryan, K.; Sadecki, T.; Sanchez, E. J.; Sanchez, L. E.; Saravanan, T. R.; Savage, R. L.; Schaetzl, D.; Schofield, R. M. S.; Schwartz, E.; Sellers, D.; Shaffer, T.; Smith, J. R.; Soni, S.; Sorazu, B.; Spencer, A. P.; Strain, K. A.; Sun, L.; Szczepańczyk, M. J.; Thomas, M.; Thomas, P.; Thorne, K. A.; Toland, K.; Torrie, C. I.; Traylor, G.; Urban, Alexander; Vajente, G.; Valdes, G.; Vander-Hyde, D. C.; Veitch, P. J.; Venkateswara, K.; Venugopalan, G.; Viets, A. D.; Vo, T.; Vorvick, C.; Wade, M.; Ward, R. L.; Warner, J.; Weaver, B.; Weiss, R.; Willke, B.; Wipf, C. C.; Xiao, L.; Yamamoto, H.; Yu, Hang; Zhang, L.; Zucker, M. E.; Zweizig, J.

doi:10.1038/s41586-020-2420-8

Cited by 168 publications

(107 citation statements)

References 22 publications

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“…The first was performed during the preparation phase prior to the third joint Advanced LIGO-Virgo scientific run O3, the second set was carried out during a dedicated break within the science run period. In the same time frame, QRPN has also been observed in the Advanced LIGO detector [16].…”

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confidence: 79%

“…J. Tanasijczuk, 41 E. N. Tapia San Martin, 17 M. Tonelli, 7,6 A. Torres-Forné, 94 I. Tosta e Melo, 46,47 A. Trapananti, 80,26 F. Travasso, 26,80 M. C. Tringali, 42 A. Trovato, 11 K. W. Tsang, 17,95,69 M. Turconi, 34 M. Valentini, 58,59 N. van Bakel, 17 M. van Beuzekom, 17 J. F. J. van den Brand, 72,43,17 C. Van Den Broeck, 69,17 L. van der Schaaf, 17 M. Vardaro, 76,17 M. Vasúth, 25 G. Vedovato, 29 D. Verkindt, 16 F. Vetrano, 32 A. Viceré, 32,33 J.-Y. Vinet, 34 H. Vocca, 27,26 R. C. Walet, 17 M. Was, 16 A. Zadrożny, 74 T. Zelenova, 13 and J.-P. Zendri 29 (The Virgo Collaboration) 1 Dipartimento di Farmacia, Università di Salerno, I-84084 Fisciano, Salerno, Italy The quantum radiation pressure and the quantum shot noise in laser-interferometric gravitational wave detectors constitute a macroscopic manifestation of the Heisenberg inequality. If quantum shot noise can be easily observed, the observation of quantum radiation pressure noise has been elusive, so far, due to the technical noise competing with quantum effects.…”

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confidence: 99%

See 1 more Smart Citation

Quantum Backaction on Kg-Scale Mirrors: Observation of Radiation Pressure Noise in the Advanced Virgo Detector

Acernese¹,

Agathos²,

Aiello³

et al. 2020

Phys. Rev. Lett.

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mentioning

confidence: 79%

mentioning

confidence: 99%

Quantum Backaction on Kg-Scale Mirrors: Observation of Radiation Pressure Noise in the Advanced Virgo Detector

Acernese¹,

Agathos²,

Aiello³

et al. 2020

Phys. Rev. Lett.

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“…These improvements come with a corresponding increase in QRPN, which is acceptable because QRPN does not dominate the low frequency gravitational-wave spectrum. However, QRPN is close to limiting the current gravitational-wave noise floor [50].…”

Section: A Quantum Noisementioning

confidence: 95%

“…This increases range by reducing low-frequency radiation pressure noise at the expense of a 0.5 dB increase in shot noise at high frequencies. This effect is more fully explored in [50].…”

Section: B Squeezermentioning

confidence: 98%

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

Buikema¹,

Cahillane²,

Mansell³

et al. 2020

Phys. Rev. D

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312

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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“…Researchers achieved this sensitivity by reducing "technical" noise-for example, from seismic disturbances and electronics-enough that detector performance is close to the fundamental limits imposed by quantum shot noise (QSN). Now, the Virgo and LIGO collaborations have independently observed a second, fainter source of noise that comes from the lasers' radiation pressure on the interferometer mirrors [1,2]. As technical noise is reduced even further, managing this quantum radiation-pressure noise (QRPN) will become increasingly important.…”

mentioning

confidence: 99%