LIGO’s quantum response to squeezed states
LIGO’s quantum response to squeezed states
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DOI：
10.1103/physrevd.104.062006
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发表时间：
2021-05
影响因子：
5
通讯作者：
L. McCuller;S. Dwyer;A. Green;Haocun Yu;L. Barsotti;C. Blair;D. Brown;A. Effler;M. Evans;Á. Fernández-Galiana;P. Fritschel;V. Frolov;N. Kijbunchoo;G. Mansell;F. Matichard;N. Mavalvala;D. McClelland;T. McRae;A. Mullavey;D. Sigg;B. Slagmolen;M. Tse;T. Vo;R. Ward;C. Whittle;R. Abbott;C. Adams;R. Adhikari;A. Ananyeva;S. Appert;K. Arai;J. Areeda;Y. Asali;0. S. M. Aston;C. Austin;A. Baer;M. Ball;S. Ballmer;S. Banagiri;D. Barker;J. Bartlett;B. Berger;J. Betzwieser;D. Bhattacharjee;G. Billingsley;S. Biscans;R. Blair;N. Bode;P. Booker;R. Bork;A. Bramley;A. Brooks;A. Buikema;C. Cahillane;K. Cannon;X. Chen;0. A. A. Ciobanu-0.-A.-A.-Ciobanu-2105164804;F. Clara;C. Compton;S. Cooper;K. Corley;0. S. T. Countryman;0. P. B. Covas;D. Coyne;L. Datrier;D. Davis;C. D. Fronzo;K. Dooley;J. Driggers;T. Etzel;T. Evans;J. Feicht;P. Fulda;M. Fyffe;J. Giaime;K. Giardina;P. Godwin;E. Goetz;S. Gras;C. Gray;R. Gray;E. Gustafson;R. Gustafson;J. Hanks;J. Hanson;T. Hardwick;R. Hasskew;M. Heintze;A. Helmling-Cornell;N. Holland;J. Jones;S. Kandhasamy;S. Karki;M. Kasprzack;K. Kawabe;P. King;J. Kissel;Rahul Kumar;M. Landry;B. Lane;B. Lantz;M. Laxen;Y. Lecoeuche;J. Leviton;J. Liu;M. Lormand;A. Lundgren;0. R. Macas;M. Macinnis;D. Macleod;S. Márka;0. Z. Marka;0. D. V. Martynov;K. Mason;T. Massinger;R. McCarthy;S. Mccormick;J. McIver;G. Mendell;K. Merfeld;E. Merilh;F. Meylahn;T. Mistry;R. Mittleman;G. Moreno;C. Mow-Lowry;S. Mozzon;0. T. J. N. Nelson;P. Nguyen;L. Nuttall;0. J. Oberling;R. Oram;C. Osthelder;D. Ottaway;H. Overmier;J. R. Palamos;W. Parker;E. Payne;A. Pele;R. Penhorwood;C. Perez;M. Pirello;H. Radkins;K. Ramirez;J. Richardson;K. Riles;N. Robertson;J. Rollins;C. Romel;J. Romie;M. Ross;K. Ryan;T. Sadecki;E. Sanchez;L. Sanchez;T. R. Saravanan;R. Savage;D. Schaetzl;R. Schnabel;R. Schofield;E. Schwartz;D. Sellers;T. Shaffer;J. R. Smith;S. Soni;B. Sorazu;A. Spencer;K. Strain;L. Sun;M. Szczepańczyk;M. Thomas;P. Thomas;K. Thorne;K. Toland;C. Torrie;G. Traylor;A. Urban;G. Vajente;G. Valdes;D. Vander-Hyde;P. Veitch;K. Venkateswara;Gautam Venugopalan;A. Viets;C. Vorvick;M. Wade;J. Warner;B. Weaver;R. Weiss;B. Willke;C. Wipf;L. Xiao;H. Yamamoto;Hang Yu;L. Zhang;M. Zucker;J. V. R. I. O. Technology;Ligo Hanford Observatory;U. Florida;Ligo Livingston Observatory;OzGrav;U. Adelaide;A. N. University;Ligo;C. I. O. Technology.;S. University;C. Fullerton;C. University;Louisiana State University;Christopher Newport University;U. Oregon;U. Minnesota;S. University;Missouri University of Science;Technology;M. F. Physics;L. Hannover;Resceu;U. Tokyo;U. O. S. Australia;U. Birmingham;Universitat de les Illes Balears;Supa;U. Glasgow;Cardiff University;The University of Mississippi;T. O. S. University;U. Columbia;U. Michigan;Inter-University Centre for Astronomy;Astrophysics;U. Portsmouth;The University of Sheffield;S. University;A. College;S. O. PhysicsAstronomy;The Valley;U. Washington;U. Hamburg;Concordia University Wisconsin;Kenyon College
中科院分区：
文献类型：
--
作者：
L. McCuller;S. Dwyer;A. Green;Haocun Yu;L. Barsotti;C. Blair;D. Brown;A. Effler;M. Evans;Á. Fernández-Galiana;P. Fritschel;V. Frolov;N. Kijbunchoo;G. Mansell;F. Matichard;N. Mavalvala;D. McClelland;T. McRae;A. Mullavey;D. Sigg;B. Slagmolen;M. Tse;T. Vo;R. Ward;C. Whittle;R. Abbott;C. Adams;R. Adhikari;A. Ananyeva;S. Appert;K. Arai;J. Areeda;Y. Asali;0. S. M. Aston;C. Austin;A. Baer;M. Ball;S. Ballmer;S. Banagiri;D. Barker;J. Bartlett;B. Berger;J. Betzwieser;D. Bhattacharjee;G. Billingsley;S. Biscans;R. Blair;N. Bode;P. Booker;R. Bork;A. Bramley;A. Brooks;A. Buikema;C. Cahillane;K. Cannon;X. Chen;0. A. A. Ciobanu-0.-A.-A.-Ciobanu-2105164804;F. Clara;C. Compton;S. Cooper;K. Corley;0. S. T. Countryman;0. P. B. Covas;D. Coyne;L. Datrier;D. Davis;C. D. Fronzo;K. Dooley;J. Driggers;T. Etzel;T. Evans;J. Feicht;P. Fulda;M. Fyffe;J. Giaime;K. Giardina;P. Godwin;E. Goetz;S. Gras;C. Gray;R. Gray;E. Gustafson;R. Gustafson;J. Hanks;J. Hanson;T. Hardwick;R. Hasskew;M. Heintze;A. Helmling-Cornell;N. Holland;J. Jones;S. Kandhasamy;S. Karki;M. Kasprzack;K. Kawabe;P. King;J. Kissel;Rahul Kumar;M. Landry;B. Lane;B. Lantz;M. Laxen;Y. Lecoeuche;J. Leviton;J. Liu;M. Lormand;A. Lundgren;0. R. Macas;M. Macinnis;D. Macleod;S. Márka;0. Z. Marka;0. D. V. Martynov;K. Mason;T. Massinger;R. McCarthy;S. Mccormick;J. McIver;G. Mendell;K. Merfeld;E. Merilh;F. Meylahn;T. Mistry;R. Mittleman;G. Moreno;C. Mow-Lowry;S. Mozzon;0. T. J. N. Nelson;P. Nguyen;L. Nuttall;0. J. Oberling;R. Oram;C. Osthelder;D. Ottaway;H. Overmier;J. R. Palamos;W. Parker;E. Payne;A. Pele;R. Penhorwood;C. Perez;M. Pirello;H. Radkins;K. Ramirez;J. Richardson;K. Riles;N. Robertson;J. Rollins;C. Romel;J. Romie;M. Ross;K. Ryan;T. Sadecki;E. Sanchez;L. Sanchez;T. R. Saravanan;R. Savage;D. Schaetzl;R. Schnabel;R. Schofield;E. Schwartz;D. Sellers;T. Shaffer;J. R. Smith;S. Soni;B. Sorazu;A. Spencer;K. Strain;L. Sun;M. Szczepańczyk;M. Thomas;P. Thomas;K. Thorne;K. Toland;C. Torrie;G. Traylor;A. Urban;G. Vajente;G. Valdes;D. Vander-Hyde;P. Veitch;K. Venkateswara;Gautam Venugopalan;A. Viets;C. Vorvick;M. Wade;J. Warner;B. Weaver;R. Weiss;B. Willke;C. Wipf;L. Xiao;H. Yamamoto;Hang Yu;L. Zhang;M. Zucker;J. V. R. I. O. Technology;Ligo Hanford Observatory;U. Florida;Ligo Livingston Observatory;OzGrav;U. Adelaide;A. N. University;Ligo;C. I. O. Technology.;S. University;C. Fullerton;C. University;Louisiana State University;Christopher Newport University;U. Oregon;U. Minnesota;S. University;Missouri University of Science;Technology;M. F. Physics;L. Hannover;Resceu;U. Tokyo;U. O. S. Australia;U. Birmingham;Universitat de les Illes Balears;Supa;U. Glasgow;Cardiff University;The University of Mississippi;T. O. S. University;U. Columbia;U. Michigan;Inter-University Centre for Astronomy;Astrophysics;U. Portsmouth;The University of Sheffield;S. University;A. College;S. O. PhysicsAstronomy;The Valley;U. Washington;U. Hamburg;Concordia University Wisconsin;Kenyon College
引力波干涉仪通过将迈克尔逊干涉仪与光学腔、悬浮质量以及现在的光的压缩量子态相结合来实现其深刻的灵敏度。这些状态修改了LIGO，VIRGO和GEO 600干涉仪的测量过程，以减少掩盖天体物理信号的量子噪声;因此，对压缩的改进对于进一步扩展我们的宇宙引力观至关重要。进一步降低量子噪声将需要降低损耗引起的退相干，以及更复杂的操作来抵消辐射压力引起的量子反作用。这两项任务都需要充分理解压缩光与公里级干涉仪的许多组件之间的物理相互作用。为此，来自两个LIGO天文台在观测运行三的数据表示使用频率相关的度量来分析每个探测器的量子响应压缩状态。响应度量的推导和用于简明地描述背后的压缩的同时与横模选择性光学腔和悬挂镜的量子辐射压力噪声的相互作用的物理机制。这些指标和相关分析广泛适用于腔增强光学力学实验，这些实验包括外部压缩，并且首次给出了迄今为止在LIGO探测器量子噪声中观察到的每个特征的物理描述。
Gravitational Wave interferometers achieve their profound sensitivity by combining a Michelson interferometer with optical cavities, suspended masses, and now, squeezed quantum states of light. These states modify the measurement process of the LIGO, VIRGO and GEO600 interferometers to reduce the quantum noise that masks astrophysical signals; thus, improvements to squeezing are essential to further expand our gravitational view of the universe. Further reducing quantum noise will require both lowering decoherence from losses as well more sophisticated manipulations to counter the quantum back-action from radiation pressure. Both tasks require fully understanding the physical interactions between squeezed light and the many components of km-scale interferometers. To this end, data from both LIGO observatories in observing run three are expressed using frequency-dependent metrics to analyze each detector's quantum response to squeezed states. The response metrics are derived and used to concisely describe physical mechanisms behind squeezing's simultaneous interaction with transverse-mode selective optical cavities and the quantum radiation pressure noise of suspended mirrors. These metrics and related analysis are broadly applicable for cavity-enhanced optomechanics experiments that incorporate external squeezing, and -- for the first time -- give physical descriptions of every feature so far observed in the quantum noise of the LIGO detectors.