Challenges
Datasets
Workspaces
Papers
Discussions
Leaderboard
Log inSign up
Challenges
Datasets
Workspaces
Papers
Discussions
Leaderboard
Blog
Job Board
Q3AS

© 2026 Aqora Quantum S.A.S.

TermsPrivacyLegal Notice

arXiv:gr-qc/0508102 · Physical Review A

Frequency-dependent squeeze-amplitude attenuation and squeeze-angle rotation by electromagnetically induced transparency for gravitational-wave interferometers

Eugeniy E. Mikhailov, Keisuke Goda, T. R. Corbitt, N. Mavalvala

Published May 10, 2006• 25 citations
arXivHTMLPDF

Abstract

We study the effects of frequency-dependent squeeze-amplitude attenuation and squeeze-angle rotation by electromagnetically induced transparency (EIT) on gravitational-wave (GW) interferometers. We propose the use of low-pass, bandpass, and high-pass EIT filters, an S-shaped EIT filter, and an intracavity EIT filter to generate frequency-dependent squeezing for injection into the antisymmetric port of GW interferometers. We find that the EIT filters have several advantages over the previous filter designs with regard to optical losses, compactness, and the tunability of the filter linewidth.

DOI
10.1103/physreva.73.053810

Related papers

Increasing Quantum Limited Sensitivity of Interferometers Using Electromagnetically Induced Transparency

H. Rew

We explore the properties of electromagnetically induced transparency (EIT) and its applications as a frequency filter in the field of gravitational wave interferometry. Through modeling and simulation, we determine parameters for atom-light configurations of multi- state atoms which will theoretically allow for transmission frequencies and intensities of squeezed light in a range suitable for increasing sensitiviy levels in gravitational wave interferometers. This corresponds to contrasts greater than 50% and linewidths of 100 Hz or less. We produce EIT experimentally and characterize the distributions by fitting them to a generalized Lorentzian. The largest contrast observed is 3.9% with a linewidth of 657 Hz. The smallest linewidth observed is 202 Hz with a contrast of 0.84%.

•Jan 1, 2016•0 citations

Frequency-Dependent Squeezing for Advanced LIGO

Lee P. McCuller, Chris Whittle, D. Ganapathy +13 more

The first detection of gravitational waves by the Laser Interferometer Gravitational-Wave Observatory (LIGO) in 2015 launched the era of gravitational-wave astronomy. The quest for gravitational-wave signals from objects that are fainter or farther away impels technological advances to realize ever more sensitive detectors. Since 2019, one advanced technique, the injection of squeezed states of light, is being used to improve the shot-noise limit to the sensitivity of the Advanced LIGO detectors, at frequencies above ∼50 Hz. Below this frequency, quantum backaction, in the form of radiation pressure induced motion of the mirrors, degrades the sensitivity. To simultaneously reduce shot noise at high frequencies and quantum radiation pressure noise at low frequencies requires a quantum noise filter cavity with low optical losses to rotate the squeezed quadrature as a function of frequency. We report on the observation of frequency-dependent squeezed quadrature rotation with rotation frequency of 30 Hz, using a 16-m-long filter cavity. A novel control scheme is developed for this frequency-dependent squeezed vacuum source, and the results presented here demonstrate that a low-loss filter cavity can achieve the squeezed quadrature rotation necessary for the next planned upgrade to Advanced LIGO, known as "A+."

arXiv:2003.13443•Physical Review Letters•Apr 28, 2020•173 citations

Frequency-dependent squeezing for gravitational-wave detection through quantum teleportation

Yohei Nishino, S. L. Danilishin, Yutaro Enomoto +1 more

Abstract Ground-based interferometric gravitational wave detectors are highly precise sensors for weak forces, limited in sensitivity across their detection band by quantum fluctuations of light. Current and future instruments address this limitation by injecting frequency-dependent squeezed vacuum into the detection port, utilizing narrow-band, low-loss optical cavities for optimal rotation of the squeezing ellipse at each signal frequency. This study introduces a novel scheme employing the principles of quantum teleportation and entangled states of light. It allows achieving broadband suppression of quantum noise in detuned signal recycled-Fabry-Perot--Michelson interferometers, which is the baseline design of the low-frequency detector within the Einstein Telescope xylophone detector, without requiring additional filter cavities or modifications to the core optics of the main interferometer.

arXiv:2401.04295•Physical Review A•Aug 1, 2024•13 citations

All-atomic generation and noise-quadrature filtering of squeezed vacuum in hot Rb vapor

Travis Horrom, Gleb Romanov, Irina Novikova +1 more

With our all-atomic squeezing and filtering setup, we demonstrate control over the noise amplitudes and manipulation of the frequency-dependent squeezing angle of a squeezed vacuum quantum state by passing it through an atomic medium with electromagnetically induced transparency (EIT). We generate low sideband frequency squeezed vacuum using the polarization self-rotation effect in a hot Rb vapor cell, and direct it through a second atomic vapor subject to EIT conditions. We use the frequency-dependent absorption of the EIT window to demonstrate an example of squeeze amplitude attenuation and squeeze angle rotation of the quantum noise quadratures of the squeezed probe. These studies have implications for quantum memory and storage as well as gravitational wave interferometric detectors.

arXiv:1204.3967•Journal of Modern Optics•Oct 16, 2012•9 citations

Frequency-dependent squeezing generation with EPR entanglement

B. Garaventa, M. Bawaj, M. De Laurentis +8 more

Abstract The sensitivity of gravitational wave interferometric detectors is ultimately limited by the quantum noise, which arises from the quantum nature of light and it is driven by vacuum fluctuations of the optical field entering from the dark port of the interferometer. One way to improve the sensitivity of gravitational wave interferometers is to inject squeezed vacuum into the dark port. This has been already demonstrated for the main gravitational wave detectors (GEO, Advanced LIGO and Advanced VIRGO). We are studying tricks to produce a “frequency- dependent squeezing”: a standard method is to filter the squeezed optical field with one or more optical cavities (300 m long cavities). An alternative method using a pair of squeezed EPR (Einstein-Podolsky-Rosen) entangled beams to produce frequency-dependent squeezing by a non-degenerate OPO (Optical Parametric Oscillator) will be discussed in this paper. This method promises to achieve a frequency-dependent optimization of the injected squeezed light fields without the need for an external filter cavity.

Journal of Physics Conference Series•May 1, 2020•0 citations

Conversion of conventional gravitational-wave interferometers into quantum nondemolition interferometers by modifying their input and/or output optics

Harry J. Kimble, Yuri Levin, Andrey B. Matsko +2 more

The LIGO-II gravitational-wave interferometers (ca. 2006--2008) are designed to have sensitivities near the standard quantum limit (SQL) in the vicinity of 100 Hz. This paper describes and analyzes possible designs for subsequent LIGO-III interferometers that can beat the SQL. These designs are identical to a conventional broad band interferometer (without signal recycling), except for new input and/or output optics. Three designs are analyzed: (i) a squeezed-input interferometer (conceived by Unruh based on earlier work of Caves) in which squeezed vacuum with frequency-dependent (FD) squeeze angle is injected into the interferometer's dark port; (ii) a variational-output interferometer (conceived in a different form by Vyatchanin, Matsko and Zubova), in which homodyne detection with FD homodyne phase is performed on the output light; and (iii) a squeezed-variational interferometer with squeezed input and FD-homodyne output. It is shown that the FD squeezed-input light can be produced by sending ordinary squeezed light through two successive Fabry-P\'erot filter cavities before injection into the interferometer, and FD-homodyne detection can be achieved by sending the output light through two filter cavities before ordinary homodyne detection. With anticipated technology (power squeeze factor ${e}^{\ensuremath{-}2R}=0.1$ for input squeezed vacuum and net fractional loss of signal power in arm cavities and output optical train ${\ensuremath{\epsilon}}_{*}=0.01)$ and using an input laser power ${I}_{o}$ in units of that required to reach the SQL (the planned LIGO-II power, ${I}_{\mathrm{SQL}}),$ the three types of interferometer could beat the amplitude SQL at 100 Hz by the following amounts $\ensuremath{\mu}\ensuremath{\equiv}\sqrt{{S}_{h}}/\sqrt{{S}_{h}^{\mathrm{SQL}}}$ and with the following corresponding increase $\mathcal{V}=1/{\ensuremath{\mu}}^{3}$ in the volume of the universe that can be searched for a given noncosmological source: $\mathrm{Squeezed}\mathrm{input}---\ensuremath{\mu}\ensuremath{\simeq}\sqrt{{e}^{\ensuremath{-}2R}}\ensuremath{\simeq}0.3$ and $\mathcal{V}\ensuremath{\simeq}{1/0.3}^{3}\ensuremath{\simeq}30$ using ${I}_{o}{/I}_{\mathrm{SQL}}=1.$ $Variational\ensuremath{-}output---\ensuremath{\mu}\ensuremath{\simeq}{\ensuremath{\epsilon}}_{*}^{1/4}\ensuremath{\simeq}0.3$ and $\mathcal{V}\ensuremath{\simeq}30$ but only if the optics can handle a ten times larger power: ${I}_{o}{/I}_{\mathrm{SQL}}\ensuremath{\simeq}1/\sqrt{{\ensuremath{\epsilon}}_{*}}=10.$ $\mathrm{Squeezed}\mathrm{varational}---\ensuremath{\mu}{=1.3(e}^{\ensuremath{-}2R}{\ensuremath{\epsilon}}_{*}{)}^{1/4}\ensuremath{\simeq}0.24$ and $\mathcal{V}\ensuremath{\simeq}80$ using ${I}_{o}{/I}_{\mathrm{SQL}}=1;$ and $\ensuremath{\mu}\ensuremath{\simeq}{(e}^{\ensuremath{-}2R}{\ensuremath{\epsilon}}_{*}{)}^{1/4}\ensuremath{\simeq}0.18$ and $\mathcal{V}\ensuremath{\simeq}180$ using ${I}_{o}{/I}_{\mathrm{SQL}}=\sqrt{{e}^{\ensuremath{-}2R}/{\ensuremath{\epsilon}}_{*}}\ensuremath{\simeq}3.2.$

arXiv:gr-qc/0008026•Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields•Dec 26, 2001•669 citations
We study the effects of frequency-dependent squeeze-amplitude attenuation and squeeze-angle rotation by electromagnetically induced transparency (EIT) on gravitational-wave (GW) interferometers. We propose the use of low-pass, bandpass, and high-pass EIT filters, an S-shaped EIT filter, and an intracavity EIT filter to generate frequency-dependent squeezing for injection into the antisymmetric port of GW interferometers. We find that the EIT filters have several advantages over the previous filter designs with regard to optical losses, compactness, and the tunability of the filter linewidth.
We explore the properties of electromagnetically induced transparency (EIT) and its applications as a frequency filter in the field of gravitational wave interferometry. Through modeling and simulation, we determine parameters for atom-light configurations of multi- state atoms which will theoretically allow for transmission frequencies and intensities of squeezed light in a range suitable for increasing sensitiviy levels in gravitational wave interferometers. This corresponds to contrasts greater than 50% and linewidths of 100 Hz or less. We produce EIT experimentally and characterize the distributions by fitting them to a generalized Lorentzian. The largest contrast observed is 3.9% with a linewidth of 657 Hz. The smallest linewidth observed is 202 Hz with a contrast of 0.84%.
The first detection of gravitational waves by the Laser Interferometer Gravitational-Wave Observatory (LIGO) in 2015 launched the era of gravitational-wave astronomy. The quest for gravitational-wave signals from objects that are fainter or farther away impels technological advances to realize ever more sensitive detectors. Since 2019, one advanced technique, the injection of squeezed states of light, is being used to improve the shot-noise limit to the sensitivity of the Advanced LIGO detectors, at frequencies above ∼50 Hz. Below this frequency, quantum backaction, in the form of radiation pressure induced motion of the mirrors, degrades the sensitivity. To simultaneously reduce shot noise at high frequencies and quantum radiation pressure noise at low frequencies requires a quantum noise filter cavity with low optical losses to rotate the squeezed quadrature as a function of frequency. We report on the observation of frequency-dependent squeezed quadrature rotation with rotation frequency of 30 Hz, using a 16-m-long filter cavity. A novel control scheme is developed for this frequency-dependent squeezed vacuum source, and the results presented here demonstrate that a low-loss filter cavity can achieve the squeezed quadrature rotation necessary for the next planned upgrade to Advanced LIGO, known as "A+."
Abstract Ground-based interferometric gravitational wave detectors are highly precise sensors for weak forces, limited in sensitivity across their detection band by quantum fluctuations of light. Current and future instruments address this limitation by injecting frequency-dependent squeezed vacuum into the detection port, utilizing narrow-band, low-loss optical cavities for optimal rotation of the squeezing ellipse at each signal frequency. This study introduces a novel scheme employing the principles of quantum teleportation and entangled states of light. It allows achieving broadband suppression of quantum noise in detuned signal recycled-Fabry-Perot--Michelson interferometers, which is the baseline design of the low-frequency detector within the Einstein Telescope xylophone detector, without requiring additional filter cavities or modifications to the core optics of the main interferometer.
With our all-atomic squeezing and filtering setup, we demonstrate control over the noise amplitudes and manipulation of the frequency-dependent squeezing angle of a squeezed vacuum quantum state by passing it through an atomic medium with electromagnetically induced transparency (EIT). We generate low sideband frequency squeezed vacuum using the polarization self-rotation effect in a hot Rb vapor cell, and direct it through a second atomic vapor subject to EIT conditions. We use the frequency-dependent absorption of the EIT window to demonstrate an example of squeeze amplitude attenuation and squeeze angle rotation of the quantum noise quadratures of the squeezed probe. These studies have implications for quantum memory and storage as well as gravitational wave interferometric detectors.
Abstract The sensitivity of gravitational wave interferometric detectors is ultimately limited by the quantum noise, which arises from the quantum nature of light and it is driven by vacuum fluctuations of the optical field entering from the dark port of the interferometer. One way to improve the sensitivity of gravitational wave interferometers is to inject squeezed vacuum into the dark port. This has been already demonstrated for the main gravitational wave detectors (GEO, Advanced LIGO and Advanced VIRGO). We are studying tricks to produce a “frequency- dependent squeezing”: a standard method is to filter the squeezed optical field with one or more optical cavities (300 m long cavities). An alternative method using a pair of squeezed EPR (Einstein-Podolsky-Rosen) entangled beams to produce frequency-dependent squeezing by a non-degenerate OPO (Optical Parametric Oscillator) will be discussed in this paper. This method promises to achieve a frequency-dependent optimization of the injected squeezed light fields without the need for an external filter cavity.
The LIGO-II gravitational-wave interferometers (ca. 2006--2008) are designed to have sensitivities near the standard quantum limit (SQL) in the vicinity of 100 Hz. This paper describes and analyzes possible designs for subsequent LIGO-III interferometers that can beat the SQL. These designs are identical to a conventional broad band interferometer (without signal recycling), except for new input and/or output optics. Three designs are analyzed: (i) a squeezed-input interferometer (conceived by Unruh based on earlier work of Caves) in which squeezed vacuum with frequency-dependent (FD) squeeze angle is injected into the interferometer's dark port; (ii) a variational-output interferometer (conceived in a different form by Vyatchanin, Matsko and Zubova), in which homodyne detection with FD homodyne phase is performed on the output light; and (iii) a squeezed-variational interferometer with squeezed input and FD-homodyne output. It is shown that the FD squeezed-input light can be produced by sending ordinary squeezed light through two successive Fabry-P\'erot filter cavities before injection into the interferometer, and FD-homodyne detection can be achieved by sending the output light through two filter cavities before ordinary homodyne detection. With anticipated technology (power squeeze factor ${e}^{\ensuremath{-}2R}=0.1$ for input squeezed vacuum and net fractional loss of signal power in arm cavities and output optical train ${\ensuremath{\epsilon}}_{*}=0.01)$ and using an input laser power Io{I}_{o}Io​ in units of that required to reach the SQL (the planned LIGO-II power, ISQL),{I}_{\mathrm{SQL}}),ISQL​), the three types of interferometer could beat the amplitude SQL at 100 Hz by the following amounts $\ensuremath{\mu}\ensuremath{\equiv}\sqrt{{S}_{h}}/\sqrt{{S}_{h}^{\mathrm{SQL}}}$ and with the following corresponding increase $\mathcal{V}=1/{\ensuremath{\mu}}^{3}$ in the volume of the universe that can be searched for a given noncosmological source: $\mathrm{Squeezed}\mathrm{input}---\ensuremath{\mu}\ensuremath{\simeq}\sqrt{{e}^{\ensuremath{-}2R}}\ensuremath{\simeq}0.3$ and $\mathcal{V}\ensuremath{\simeq}{1/0.3}^{3}\ensuremath{\simeq}30$ using Io/ISQL=1.{I}_{o}{/I}_{\mathrm{SQL}}=1.Io​/ISQL​=1. $Variational\ensuremath{-}output---\ensuremath{\mu}\ensuremath{\simeq}{\ensuremath{\epsilon}}_{*}^{1/4}\ensuremath{\simeq}0.3$ and $\mathcal{V}\ensuremath{\simeq}30$ but only if the optics can handle a ten times larger power: ${I}_{o}{/I}_{\mathrm{SQL}}\ensuremath{\simeq}1/\sqrt{{\ensuremath{\epsilon}}_{*}}=10.$ $\mathrm{Squeezed}\mathrm{varational}---\ensuremath{\mu}{=1.3(e}^{\ensuremath{-}2R}{\ensuremath{\epsilon}}_{*}{)}^{1/4}\ensuremath{\simeq}0.24$ and $\mathcal{V}\ensuremath{\simeq}80$ using Io/ISQL=1;{I}_{o}{/I}_{\mathrm{SQL}}=1;Io​/ISQL​=1; and $\ensuremath{\mu}\ensuremath{\simeq}{(e}^{\ensuremath{-}2R}{\ensuremath{\epsilon}}_{*}{)}^{1/4}\ensuremath{\simeq}0.18$ and $\mathcal{V}\ensuremath{\simeq}180$ using ${I}_{o}{/I}_{\mathrm{SQL}}=\sqrt{{e}^{\ensuremath{-}2R}/{\ensuremath{\epsilon}}_{*}}\ensuremath{\simeq}3.2.$