A gravitational wave observatory operating beyond the quantum shot-noise limit

Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.; Adams, C.; Adhikari, R. X.; Affeldt, C.; Allen, B.; Allen, G.; Ceron, E. Amador; Amariutei, D.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Atkinson, D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P. T.; Ballmer, S. W.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Batch, J. C.; Bauchrowitz, J.; Behnke, B.; Bell, A. S.; Belopolski, Ilya; Benacquista, M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, David; Bland, B.; Böck, O.; Bodiya, T. P.; Bogan, C.; Bondarescu, Ruxandra; Bork, R.; Born, M.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Brummitt, A.; Buonanno, A.; Burguet–Castell, J.; Burmeister, O.; Byer, Robert L.; Cadonati, L.; Camp, J. B.; Campsie, P.; Cannizzo, J. K.; Cannon, K. C.; Cao, Junwei; Capano, C. D.; Caride, S.; Caudill, S.; Cavaglià, M.; Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chelkowski, S.; Chen, Y.; Christensen, N.; Cho, H.; Chua, S.; Chung, S.; Chung, C. T.Y.; Ciani, G.; Clara, F.; Clark, D.; Clark, J. A.; Clayton, J. H.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M. W.; Couvares, P.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham, L.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.; Danzmann, K.; Daudert, B.; Daveloza, H.; Davies, G. S.; Daw, E. J.; Dayanga, T.; DeBra, D.; Degallaix, J.; Dent, T.; Dergachev, V.; DeRosa, R. T.; DeSalvo, R.; Dhurandhar, S.; DiGuglielmo, James; Palma, I. Di; Díaz, M. C.; Donovan, F.; Dooley, K. L.; Dorsher, S.; Drever, R. W. P.; Driggers, J. C.; Du, Z.; Dumas, J. C.; Dwyer, S. E.; Eberle, T.; Edgar, M.; Edwards, M. C.; Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, K.; Evans, M.; Evans, T. M.; Factourovich, M.; Fairhurst, S.; Fan, Y.; Farr, B.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Finn, L. S.; Fisher, R. P.; Flanigan, Meghan E.; Foley, S.; Forsi, E.; Fotopoulos, N.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, Daniel; Fritschel, P.; Фролов, В. В.; Fulda, P.; Fyffe, M.; Ganija, M. R.; García, Javier A.; Garofoli, J.; Geng, R.; Gergely, L.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Gill, C.; Goetz, E.; Goggin, L. M.; González, Gabriela; Gorodetsky, M. L.; Goßler, S.; Graef, C.; Grant, A.; Gras, S.; Gray, C.; Gray, Norman; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grünewald, S.; Guido, C.; Gupta, Ranjan; Gustafson, E. K.; Gustafson, R.; Ha, T.; Hage, B.; Hallam, J. M.; Hammer, D. A.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Hartman, M. T.; Haughian, K.; Hayama, K.; Heefner, J.; Heintze, M. C.; Hendry, M.; Heng, I. S.; Heptonstall, A. W.; Herrera, V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Hong, T.; Hooper, S.; Hosken, David J.; Hough, J.; Howell, E. J.; Hughey, B.; Huynh─Dinh, T.; Husa, S.; Huttner, S. H.; Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson, M.; Jang, H.; Johnson, W. W.; Jones, D. I.; Jones, Gareth; Jones, R.; Li, Ju; Kalmus, P.; Kalogera, V.; Kamaretsos, I.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Katsavounidis, E.; Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura, Seiji; Kawazoe, F.; Kells, W.; Keppel, D. G.; Keresztes, Zoltán; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, B.; Kim, C.; Kim, D.; Kim, H.; Kim, K.; Kim, N.; Kim, Yong-Mi; King, Peter; Kinsey, M.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Korth, W. Z.; Kozak, D. B.; Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Kuehn, G.; Kumar, Rahul; Kwee, P.; Lam, Ping Koy; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lawrie, Craig; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee, H. M.; Leindecker, N.; Leong, J. R.; Leonor, I.; Li, J.; Lindquist, P.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Luan, Jing; Łubiński, M.; Lück, H.; Lundgren, A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Mageswaran, M.; Mailand, K.; Mandel, Ilya; Mandic, V.; Marandi, Alireza; Márka, S.; Márka, Z.; Markosyan, A. S.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone, L.; Matzner, Richard A.; Mavalvala, N.; Mazzolo, G.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.; Meadors, G. D.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, Adrian C.; Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M.; Miao, H.; Miller, John M.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Moesta, Philipp; Mohanty, Soumya D.; Moraru, D.; Moreno, G.; Mori, Toshiyuki; Mossavi, K.; Mow–Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, Soma; Mullavey, A.; Müller‐Ebhardt, H.; Münch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.; Nash, T.; Nawrodt, R.; Necula, V.; Nelson, J.; Newton, G.; Nishizawa, A.; Nolting, D.; Nuttall, L. K.; O’Dell, J.; O’Reilly, B.; O’Shaughnessy, R.; Ochsner, E.; Oelker, E.; Oh, J. J.; Oh, S. H.; Ogin, G. H.; Oldenburg, R. G.; Osthelder, C.; Ott, Christian D.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, Amanda J.; Pan, Y.; Pankow, C.; Papa, M. A.; Ajith, P.; Patel, P.; Pedraza, M.; Peiris, P.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Phelps, M.; Pickenpack, M.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Pöld, J.; Postiglione, F.; Predoi, V.; Price, Larry R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix, R.; Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Radkins, H.; Raffai, P.; Rakhmanov, M.; Ramet, C.; Rankins, B.; Mohapatra, S. R. P.; Raymond, V.; Redwine, K.; Reed, C. M.; Reed, T.; Reid, S.; Reitze, D. H.; Riesen, Rolf; Riles, K.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, Carl L.; Rodruck, M.; Rollins, J. G.; Romano, J. D.; Romie, J. H.; Röver, Christian; Rowan, S.; Rüdiger, A.; Ryan, K.; Ryll, H.; Sainathan, P.; Sakosky, M.; Salemi, F.; Samblowski, Aiko; Sammut, L.; Jordana, L. Sancho De La; Sandberg, V.; Sankar, S.; Sannibale, V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.; Schilling, R.; Schlamminger, Stephan; Schnabel, R.; Schofield, R. M. S.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, John D.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.; Singer, L. P.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, Roger; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Soto, J.; Speirits, Fiona C.; Stein, A. J.; Steinert, E.; Steinlechner, J.; Steinlechner, S.; Steplewski, S.; Stefszky, Michael; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, Robert W.; Thomas, P.; Thorne, K. A.; Thorne, Kip S.; Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Torres, C. V.; Torrie, C. I.; Traylor, G.; Trias, M.; Tseng, K.; Ugolini, D.; Urbánek, Karel; Vahlbruch, H.; Vallisneri, Michele; Veggel, A. A. van; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A.; Vitale, Salvatore; Vorvick, C.; Vyatchanin, S. P.; Wade, A. R.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wanner, A.; Wang, X.; Wang, Z.; Ward, R. L.; Wei, Peng; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Weßels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D. J.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wittel, H.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yablon, J.; Yakushin, I.; Yamamoto, K.; Yamamoto, H.; Yang, Huan; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Zanolin, M.; Zhang, L.; Zhang, W.; Zhang, Z.; Zhao, C.; Zotov, N.; Zweizig, J.; Zucker, J. E.

doi:10.1038/nphys2083

Cited by 783 publications

(377 citation statements)

References 31 publications

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“…GEO 600 implements a number of advanced interferometric techniques such as signal recycling and squeezed light to improve sensitivity at frequencies above a few hundred Hz [63,64]. The LIGO [65] and Virgo [66] observatories are power-recycled interferometers of similar design, with Fabry-Perot cavities in the arms to increase the effective arm length and improve the sensitivity to GWs.…”

Section: Gw Observatoriesmentioning

confidence: 99%

Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors

Aasi¹,

Abbott²,

Abbott³

et al. 2014

Phys. Rev. D

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In this paper we report on a search for short-duration gravitational wave bursts in the frequency range 64 Hz-1792 Hz associated with gamma-ray bursts (GRBs), using data from GEO 600 and one of the LIGO or Virgo detectors. We introduce the method of a linear search grid to analyze GRB events with large sky localization uncertainties, for example the localizations provided by the Fermi Gamma-ray Burst Monitor (GBM). Coherent searches for gravitational waves (GWs) can be computationally intensive when the GRB sky position is not well localized, due to the corrections required for the difference in arrival time between detectors. Using a linear search grid we are able to reduce the computational cost of the analysis by a factor of Oð10Þ for GBM events. Furthermore, we demonstrate that our analysis pipeline can improve upon the sky localization of GRBs detected by the GBM, if a high-frequency GW signal is observed in coincidence. We use the method of the linear grid in a search for GWs associated with 129 GRBs observed satellitebased gamma-ray experiments between 2006 and 2011. The GRBs in our sample had not been previously analyzed for GW counterparts. A fraction of our GRB events are analyzed using data from GEO 600 while the detector was using squeezed-light states to improve its sensitivity; this is the first search for GWs using data from a squeezed-light interferometric observatory. We find no evidence for GW signals, either with any individual GRB in this sample or with the population as a whole. For each GRB we place lower bounds on the distance to the progenitor, under an assumption of a fixed GW emission energy of 10 −2 M⊙c 2 , with a median exclusion distance of 0.8 Mpc for emission at 500 Hz and 0.3 Mpc at 1 kHz. The reduced computational cost associated with a linear search grid will enable rapid searches for GWs associated with Fermi GBM events once the advanced LIGO and Virgo detectors begin operation.

show abstract

Section: Gw Observatoriesmentioning

confidence: 99%

Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors

Aasi¹,

Abbott²,

Abbott³

et al. 2014

Phys. Rev. D

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“…It has also been employed in frequency and phase estimation to beat their standard quantum limits on measurement precision [4][5][6][7][8][9][10]. Furthermore, entanglement has applications across diverse research areas, including dynamic biological measurement [11], delicate material probing [12], gravitational wave detection [13], and quantum lithography [14]. Entanglement, however, is fragile; it is easily destroyed by quantum decoherence arising from environmental loss and noise.…”

mentioning

confidence: 99%

Optimum Mixed-State Discrimination for Noisy Entanglement-Enhanced Sensing

2017

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Quantum metrology utilizes nonclassical resources, such as entanglement or squeezed light, to realize sensors whose performance exceeds that afforded by classical-state systems. Environmental loss and noise, however, easily destroy nonclassical resources and, thus, nullify the performance advantages of most quantum-enhanced sensors. Quantum illumination (QI) is different. It is a robust entanglement-enhanced sensing scheme whose 6 dB performance advantage over a coherent-state sensor of the same average transmitted photon number survives the initial entanglement's eradication by loss and noise. Unfortunately, an implementation of the optimum quantum receiver that would reap QI's full performance advantage has remained elusive, owing to its having to deal with a huge number of very noisy optical modes. We show how sum-frequency generation (SFG) can be fruitfully applied to optimum multimode Gaussian-mixedstate discrimination. Applied to QI, our analysis and numerical evaluations demonstrate that our SFG receiver saturates QI's quantum Chernoff bound. Moreover, augmenting our SFG receiver with a feedforward (FF) mechanism pushes its performance to the Helstrom bound in the limit of low signal brightness. The FF-SFG receiver, thus, opens the door to optimum quantum-enhanced imaging, radar detection, state and channel tomography, and communication in practical Gaussian-state situations. DOI: 10.1103/PhysRevLett.118.040801 Introduction.-Entanglement is essential for deviceindependent quantum cryptography [1], quantum computing [2], and quantum-enhanced metrology [3]. It has also been employed in frequency and phase estimation to beat their standard quantum limits on measurement precision [4][5][6][7][8][9][10]. Furthermore, entanglement has applications across diverse research areas, including dynamic biological measurement [11], delicate material probing [12], gravitational wave detection [13], and quantum lithography [14]. Entanglement, however, is fragile; it is easily destroyed by quantum decoherence arising from environmental loss and noise. Consequently, the entanglement-enabled performance advantages of most quantum-enhanced sensing schemes quickly dissipate with increasing quantum decoherence, challenging their merits for practical situations.Quantum illumination (QI) is an entanglement-enhanced paradigm for target detection that thrives on entanglementbreaking loss and noise [15][16][17][18][19][20][21][22]. Its optimum quantum receiver enjoys a 6 dB advantage in error-probability exponent over optimum classical sensing using the same transmitted photon number. Remarkably, QI's advantage occurs despite the initial entanglement being completely destroyed.To date, the only in-principle realization of QI's optimum quantum receiver requires a Schur transform on a quantum computer [23], so that its physical implementation is unlikely to occur in the near future. At present, the best known suboptimum QI receivers [20,21]-one of which, the optical parametric amplifier (OPA) receiver, has been

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“…They generally fall into two categories: (i) a sensitivity-oriented category-using external squeezing [9,10] or internal squeezing [11,12] to reduce the shot noise while keeping broad bandwidth (external squeezing has been implemented in large-scale GW detectors [13,14] and is also planned for future upgrades [15][16][17]), and (ii) a bandwidth-oriented category-the so-called white-light-cavity idea [18][19][20][21][22][23][24][25]that uses an atomic medium with negative dispersion to cancel the positive dispersion of optical cavities.…”

mentioning

confidence: 99%

Enhancing the Bandwidth of Gravitational-Wave Detectors with Unstable Optomechanical Filters

et al. 2015

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Advanced interferometric gravitational-wave detectors use optical cavities to resonantly enhance their shotnoise-limited sensitivity. Because of positive dispersion of these cavities-signals at different frequencies pick up different phases, there is a tradeoff between the detector bandwidth and peak sensitivity, which is a universal feature for quantum measurement devices having resonant cavities. We consider embedding an active unstable filter inside the interferometer to compensate the phase, and using feedback control to stabilize the entire system. We show that this scheme in principle can enhance the bandwidth without sacrificing the peak sensitivity. However, the unstable filter under our current consideration is a cavity-assisted optomechanical device operating in the instability regime, and the thermal fluctuation of the mechanical oscillator puts a very stringent requirement on the environmental temperature and the mechanical quality factor. , are kilometer-scale laser interferometers that measure GW-induced differential arm length change. These detectors are macroscopic in size, and yet one of the major noises that limit their sensitivity is the quantum noise-quantum radiation pressure noise at low frequencies and quantum shot noise at high frequencies (above ∼100 Hz). To reduce the shot noise, they incorporate optical cavities in two arms that resonantly enhance both the optical power and signal, as shown schematically in Fig. 1(a). In addition, they include a power-recycling mirror (PRM) at the bright (common) port and a signal-recycling mirror (SRM) at the dark (differential) port-PRM further increases the power circulating inside arm cavities, e.g., up to ∼1 MW for Advanced LIGO, while SRM coherently reflects the signal back to the interferometer and modifies the detector response to GW signals at different frequencies. For instance, Advanced LIGO, in its nominal operation mode, uses a SRM to broaden the detector bandwidth, which equalizes the response to both low-frequency and high-frequency signals. However, this is at a price of decreasing the peak sensitivity when considering the shot noise, as illustrated in Fig. 1(b). Such a tradeoff between the bandwidth and the peak sensitivity (with their product being approximately constant) can be attributable to the positive dispersion of optical cavities-signals at different frequencies are not simultaneously resonant due to the frequency-dependent propagation phase. This feature was first pointed out by Mizuno [4] in the GW community. It turns out to be universal for all quantum measurement devices with resonant cavities, e.g., optomechanically based force or position sensors [5], and laser ring gyros [6]. The bandwidth-sensitivity product is ultimately bounded by the amount of energy stored inside the devices, which is a consequence of the quantum Cramér-Rao bound [7,8].

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A gravitational wave observatory operating beyond the quantum shot-noise limit

Cited by 783 publications

References 31 publications

Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors

Methods and results of a search for gravitational waves associated with gamma-ray bursts using the GEO 600, LIGO, and Virgo detectors

Optimum Mixed-State Discrimination for Noisy Entanglement-Enhanced Sensing

Enhancing the Bandwidth of Gravitational-Wave Detectors with Unstable Optomechanical Filters

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