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GDR Ondes Gravitationnelles: workshop "développement des détecteurs"

10 juin 2025
IJCLab
Fuseau horaire Europe/Paris

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  1. 1. Mot d'accueil
    Valerie CHAMBERT (IJCLAB-in2p3-Universite-Paris-Saclay)
    10/06/2025 10:25
  2. 3. Nombres et Lumière : introduction à la propagation numérique de la lumière
    Jean-Yves Vinet
    10/06/2025 10:30
  3. 5. Zemax simulations for GW detectors : design, optimization, tolerancing and knowledge of instruments
    Christelle Buy (L2I Toulouse, CNRS/IN2P3, Université de Toulouse)
    10/06/2025 11:20
  4. 4. Simulation optique avec OSCAR : un code FFT sur Matlab
    Jerome DEGALLAIX (Laboratoire des Matéraux Avancés)
    10/06/2025 12:10

    Cette présentation abordera le principe des simulations optiques basés sur la propagation dite par FFT puis, après une présentation de l'outil, sera abordé une introduction à l'utilisation de OSCAR permettant de réaliser ce type de simulation avec différentes sortes d'imperfections.
    En particulier, après avoir vu les bonnes pratiques pour...

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  5. 8. Finesse 3 simulation for GW detector: using multi-modal simulation to design and prepare the O5 upgrade on Virgo
    Augustin DEMAGNY (LAPP)
    10/06/2025 14:00

    Backscattered light is a source of noise in the Virgo interferometer. A fraction of light scattered by elements in optical benches recouples with the main beam, either in the Fabry-Perot cavity for end-arm benches or in the Signal Recycling Cavity for detection benches. During O4, the mirror of the signal recycling cavity (SR) was misaligned to increase the sensitivity.
    If it’s possible to...

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  6. 6. Optical simulation methods to study the losses in the stable recycling cavities of Advanced Virgo+
    Ward AMAR
    10/06/2025 14:20

    In this talk, we present the methods used to study losses in the stable recycling cavities of the Advanced Virgo+ detector. The analysis is based on FFT simulation tools developed within the LIGO-Virgo collaboration, specifically the OSCAR and SIS codes.

    We explore three simulation methods. First, we study beam reflection on curved mirrors at non-negligible angles of incidence. This...

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  7. 9. Optical Simulation using python : analysis of tilt-to-length coupling for LISA
    Maxime VINCENT (AstroParticule et Cosmologie)
    10/06/2025 14:40

    Space based gravitational wave detectors are plagued with a parasitic coupling between the jitter of the laser beams relative to one another and the optical path length read out of the interferometer. This noise source was not limiting on ground based GW detectors since the state of the art stabilisation technologies developed for LVK observatories allow to have extremely stable test masses,...

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  8. 11. Reduction of flexing-filtering noise in TDI
    Shivani Harer
    10/06/2025 15:00

    In early 2024, ESA formally adopted the Laser Interferometer Space Antenna (LISA) space mission -- with the aim of measuring gravitational waves emitted in the millihertz range. The constellation employs three spacecrafts that exchange laser beams to make interferometric measurements over a distance of 2.5 million kms. The measurements will then telemetered down to Earth at a lower sampling...

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  9. 12. Recent progress on a noise budget for a lunar GW detector
    Léon Vidal (APC/IPGP)
    10/06/2025 15:40

    The Moon offers a unique environment for gravitational wave (GW) detection thanks to its low seismic noise and lack of atmosphere. During the Apollo missions, the Lunar Surface Gravimeter (LSG) was deployed in an early attempt to detect GWs via ground motion, though it ultimately fell short of its objectives. Today, in the context of renewed lunar exploration, new mission concepts such as LGWA...

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  10. 7. Filter Cavities for Squeezing in the Einstein Telescope: Design and Challenges
    M. Yuhang Zhao (APC, Université Paris Cité)
    10/06/2025 16:00

    The Einstein Telescope (ET) is a next-generation observatory for gravitational waves. It will push sensitivity beyond current detectors. One major challenge is quantum noise. This limits the detector at both low and high frequencies. The baseline design uses frequency-dependent squeezing to reduce this noise. It includes two filter cavities (FCs) for the low-frequency interferometers and one...

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  11. 10. Quantum performances of resonant cavities schemes for frequency-dependent squeezing in future generation gravitational-wave detectors
    Isander-Louis AHREND
    10/06/2025 16:20

    Gravitational-wave detectors use frequency-dependent quantum squeezing
    to reduce the impact of quantum noise on the detector bandwidth. While a
    single filter cavity (FC) is enough to achieve the frequency dependence for cur-
    rent detectors, future generations such as Einstein Telescope Low-Frequency
    (ETLF) will be operated with a detuned signal recycling cavity. This will re-
    quire a...

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  12. 2. Linear three-mirror cavity for quantum noise reduction: resonant behavior, stability and meter-scale prototype
    M. Paul STEVENS (CNRS / IJCLab)
    10/06/2025 16:40

    Fabry-Perot cavities are used in present GW interferometers for the frequency-dependent squeezing technique, which reduces quantum noise across the entire observation frequency range. However, they may not offer sufficient control over the squeezing properties required for next-generation detectors, in particular the Einstein Telescope. To this end, different filtering system configurations...

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