L. McCuller, LIGO, Massachusetts Institute of Technology
S. E. Dwyer, LIGO Hanford
A. C. Green, University of Florida
Haocun Yu, LIGO, Massachusetts Institute of Technology
K. Kuns, LIGO, Massachusetts Institute of Technology
L. Barsotti, LIGO, Massachusetts Institute of Technology
C. D. Blair, LIGO Livingston
D. D. Brown, The University of Adelaide
A. Effler, LIGO Livingston
M. Evans, LIGO, Massachusetts Institute of Technology
A. Fernandez-Galiana, LIGO, Massachusetts Institute of Technology
P. Fritschel, LIGO, Massachusetts Institute of Technology
V. V. Frolov, LIGO Livingston
N. Kijbunchoo, The Australian National University
G. L. Mansell, LIGO, Massachusetts Institute of Technology
F. Matichard, LIGO, Massachusetts Institute of Technology
N. Mavalvala, LIGO, Massachusetts Institute of Technology
D. E. McClelland, The Australian National University
T. McRae, The Australian National University
A. Mullavey, LIGO Livingston
D. Sigg, LIGO Hanford
B. J.J. Slagmolen, The Australian National University
M. Tse, LIGO, Massachusetts Institute of Technology
T. Vo, Syracuse University
R. L. Ward, The Australian National University
C. Whittle, LIGO, Massachusetts Institute of Technology
R. Abbott, California Institute of Technology
C. Adams, LIGO Livingston
R. X. Adhikari, California Institute of Technology
A. Ananyeva, California Institute of Technology
S. Appert, California Institute of Technology
K. Arai, California Institute of Technology
J. S. Areeda, California State University, Fullerton

Document Type

Article

Publication Date

9-15-2021

Abstract

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.

Publication Source (Journal or Book title)

Physical Review D

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