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Dr Mikhail Korobko (University of Hamburg)21/05/2026, 09:00Quantum NoisePresentation
Quantum squeezed light is a key technology in gravitational-wave detection, enabling improved sensitivity in current and future detectors. Achieving its full benefit requires controlling optical decoherence beyond nominal loss and phase noise. A particularly important mechanism is hyperloss: spatial mode mismatch at interferometric interfaces coherently couples the squeezed field into...
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Byeong-Yoon Go21/05/2026, 09:18Quantum NoisePresentation
Squeezed light is a key technology for reducing quantum noise in gravitational-wave detectors. Frequency-dependent squeezing enables broadband noise suppression but is highly sensitive to mode mismatch between the squeezed field and the filter cavity. We experimentally demonstrate robust frequency-dependent squeezing under mode mismatch using a self-imaging filter cavity.
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The self-imaging... -
Yuheng Ye (The University of Tokyo)21/05/2026, 09:36Quantum NoisePresentation
While squeezing is essential for reducing high-frequency quantum noise in gravitational-wave detectors, inhomogeneous birefringence in sapphire Input Test Masses (ITMs) poses a challenge for KAGRA. ITM birefringence couples the fundamental S-polarized HG00 mode into P polarization and higher-order modes (HOMs). We show that the impact of birefringence cannot be captured as simple optical loss:...
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Jonas Rittmeyer (Institut für Quantenphysik, Universität Hamburg)21/05/2026, 09:54Quantum NoisePresentation
Squeezed light in an integral part of LIGO, Virgo and future ground-based observatories and is essential to optimize their sensitivity and range. High quantum enhancement is currently limited by interferometer, injection and detection losses. While interferometer losses are fundamental, detection losses can be mitigated by parametric amplification.
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We propose a new approach to produce... -
Ryo Iden (Science Tokyo)21/05/2026, 10:12Quantum NoisePresentation
Quantum noise limits the sensitivity of gravitational-wave detectors over a broad frequency band. A promising technique to reduce this noise is the injection of frequency-dependent squeezed states. In current detectors such as LIGO, this is achieved using a filter cavity. However, the Einstein Telescope (ET) employs a detuned interferometer configuration, for which implementing...
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Matteo Carlassara (Max Plank Institute for Gravitational Physics - AEI Hannover - 10 m Prototype)21/05/2026, 11:00Quantum NoisePresentation
Upgrades to current and third generation ground-based Gravitational Wave Detectors (GWDs) will use Balanced Homodyne Detection (BHD) as a readout scheme with the interferometers locked at the dark fringe to suppress laser noise and improve their sensitivity. This will require an ultra-low phase noise local oscillator and the design of a more advanced locking scheme.
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This presentation provides... -
Robert Ward (Australian National University)21/05/2026, 11:18Quantum NoisePresentation
Quantum technology is now a well-established method for enhancing the sensitivity of gravitational wave detectors, with the injection and input filtering of squeezed vacuum at the primary laser wavelength routinely operating in both the Advanced LIGO and Advanced Virgo gravitational wave detectors. Development continues on demonstrations of other quantum techniques. At the ANU, we have...
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Isander Ahrend21/05/2026, 11:36Quantum NoisePresentation
Gravitational-wave detectors rely on frequency-dependent quantum squeezing to minimize quantum noise across the entire detection bandwidth. While current detectors achieve this with a single filter cavity (FC), future instruments like the Einstein Telescope Low-Frequency (ETLF) will operate with a detuned signal recycling cavity, requiring a complex rotation of the squeezing ellipse for...
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Mr Kaido Suzuki (Tokyo Institute of Technology)21/05/2026, 11:54Quantum NoisePresentation
The high-frequency sensitivity of ground-based gravitational-wave detectors is fundamentally limited by quantum noise, dominated by shot noise, while increasing the circulating optical power is constrained by thermal effects and optomechanical instabilities. Extending detector sensitivity into the kilohertz band is particularly important, as it may enable observations of post-merger signals...
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Eleonora Capocasa (APC)Quantum NoisePoster
Performant quantum noise reduction is one of the key elements for achieving the target sensitivity of the Einstein Telescope, which aims at an ambitious 10 dB of broadband quantum noise reduction.
We will discuss the current design of the system for both ET-HF and ET-LF. In particular, the ET-LF configuration requires the use of two filter cavities to achieve the optimal frequency...
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Liu Tao (Université Paris Cité, CNRS, Astroparticule et Cosmologie)Quantum NoisePresentation
Precise sensing and control of spatial mode content is essential for the performance of precision optical systems, particularly interferometric gravitational-wave detectors, where misalignment and mode mismatch can lead to significant optical losses and degraded quantum noise suppression. Conventional approaches, including heterodyne wavefront sensing and phase camera techniques, are effective...
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