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Technologies for the ELGAR large scale atom interferometer array

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arxiv 2007.04014 v1 pith:UBAUYW2M submitted 2020-07-08 physics.atom-ph

B. Canuel , S. Abend , P. Amaro-Seoane , F. Badaracco , Q. Beaufils , A. Bertoldi , K. Bongs , P. Bouyer
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C. Braxmaier W. Chaibi N. Christensen F. Fitzek G. Flouris N. Gaaloul S. Gaffet C. L. Garrido Alzar R. Geiger S. Guellati-Khelifa K. Hammerer J. Harms J. Hinderer M. Holynski J. Junca S. Katsanevas C. Klempt C. Kozanitis M. Krutzik A. Landragin I. Làzaro Roche B. Leykauf Y.-H. Lien S. Loriani S. Merlet M. Merzougui M. Nofrarias P. Papadakos F. Pereira dos Santos A. Peters D. Plexousakis M. Prevedelli E. M. Rasel Y. Rogister S. Rosat A. Roura D. O. Sabulsky V. Schkolnik D. Schlippert C. Schubert L. Sidorenkov J.-N. Siem{ss} C. F. Sopuerta F. Sorrentino C. Struckmann G. M. Tino G. Tsagkatakis A. Viceré W. von Klitzing L. Woerner X. Zou
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classification physics.atom-ph
keywords atomarraydetectordiscusselgargravitationlargenoise
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abstract

We proposed the European Laboratory for Gravitation and Atom-interferometric Research (ELGAR), an array of atom gradiometers aimed at studying space-time and gravitation with the primary goal of observing gravitational waves (GWs) in the infrasound band with a peak strain sensitivity of $3.3 \times 10^{-22}/\sqrt{\text{Hz}}$ at 1.7 Hz. In this paper we detail the main technological bricks of this large scale detector and emphasis the research pathways to be conducted for its realization. We discuss the site options, atom optics, and source requirements needed to reach the target sensitivity. We then discuss required seismic isolation techniques, Gravity Gradient Noise reduction strategies, and the metrology of various noise couplings to the detector.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Spatial and Pulse Efficiency Constraints in Atom Interferometric Gravitational Wave Detectors

    quant-ph 2025-06 accept novelty 6.0 of 10

    In resonant-mode atom-interferometer gravitational wave detectors, the optimal number of pulses is set mainly by per-pulse atom loss, and current large-pulse-number proposals demand fidelities roughly two orders of ma...

  2. Massive graviton dark matter searches with long-baseline atom interferometers

    hep-ph 2024-12 conditional novelty 6.0 of 10

    Long-baseline atom interferometers could detect ultra-light spin-2 dark matter through three coupling channels, reaching mass and coupling ranges that LIGO and LISA cannot cover.

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