Lunar Gravitational-wave Antenna

Harms, J.; Ambrosino, Filippo; Angelini, L.; Braito, V.; Branchesi, M.; Brocato, E.; Cappellaro, E.; Coccia, E.; Coughlin, M. W.; Ceca, R. Della; Valle, M. Della; Dionisio, C.; Federico, C.; Formisano, M.; Frigeri, Alessandro; Grado, A.; Izzo, L.; Marcelli, A.; Maselli, Andrea; Olivieri, Marco; Pernechele, Claudio; Possenti, A.; Ronchini, S.; Serafinelli, Roberto; Severgnini, P.; Agostini, Maila; Badaracco, F.; Bertolini, A.; Betti, L.; Civitani, M.; Collette, Christophe; Covino, S.; Dall’Osso, S.; D’Avanzo, P.; DeSalvo, R.; Giovanni, M. Di; Focardi, M.; Giunchi, C.; Heijningen, J. V. van; Khetan, N.; Melini, Daniele; Mitri, G.; Mow–Lowry, C. M.; Naponiello, Luca; Noce, Vladimiro; Oganesyan, G.; Pace, E.; Paik, Ho Jung; Pajewski, Alessandro; Palazzi, E.; Pallavicini, M.; Pareschi, G.; Pozzobon, Riccardo; Sharma, A.; Spada, Giorgio; Stanga, R.; Tagliaferri, G.; Votta, Raffaele

doi:10.3847/1538-4357/abe5a7

Cited by 62 publications

(49 citation statements)

References 226 publications

(264 reference statements)

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“…The corresponding PI curve has a minimum of Ω( f ) ≈ 1.3 × 10 −2 at f ≈ 1.6 mHz. Recently, a trio of similar experiments have been proposed in which gravimeters installed on the Lunar surface could be used to monitor the Moon's normal modes, providing a cleaner probe of GWs in the megahertz frequency band [308,309].…”

Section: Other Stochastic Background Searchesmentioning

confidence: 99%

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Renzini¹,

Goncharov²,

Jenkins³

et al. 2022

Preprint

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The collection of individually resolvable gravitational wave (GW) events makes up a tiny fraction of all GW signals that reach our detectors, while most lie below the confusion limit and are undetected. Similarly to voices in a crowded room, the collection of unresolved signals gives rise to a background that is well-described via stochastic variables and, hence, referred to as the stochastic GW background (SGWB). In this review, we provide an overview of stochastic GW signals and characterise them based on features of interest such as generation processes and observational properties. We then review the current detection strategies for stochastic backgrounds, offering a ready-to-use manual for stochastic GW searches in real data. In the process, we distinguish between interferometric measurements of GWs, either by ground-based or space-based laser interferometers, and timing-residuals analyses with pulsar timing arrays (PTAs). These detection methods have been applied to real data both by large GW collaborations and smaller research groups, and the most recent and instructive results are reported here. We close this review with an outlook on future observations with third generation detectors, space-based interferometers, and potential noninterferometric detection methods proposed in the literature.

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Section: Other Stochastic Background Searchesmentioning

confidence: 99%

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Renzini¹,

Goncharov²,

Jenkins³

et al. 2022

Preprint

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“…Lunar Gravitational-Wave Antenna 5,23 One of the first concepts proposed for the detection of gravitational waves by Joseph Weber is to monitor the quadrupolar vibrations of elastic bodies excited by GWs. At laboratory scale, these experiments became known as resonant-bar detectors, which form an important part of the history of GW detection.…”

Section: 1mentioning

confidence: 99%

“…A design error made it impossible to carry out the intended search for GWs, but the idea remains intriguing. Harms et al 5,23 have proposed a new concept, the Lunar Gravitational-Wave Antenna (LGWA), based on Weber's idea. LGWA would have a rich GW and multi-messenger science case with galactic binaries and more massive black-hole binaries.…”

Section: 1mentioning

confidence: 99%

Mid-Frequency Gravitational Waves (0.1-10 Hz): Sources and Detection Methods Summary of the parallel session GW2 of MG16 Meeting

Gao¹,

Ni²,

Wang³

et al. 2021

Preprint

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This article summarizes the talks in the session GW2 of the Sixteenth Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Gravitation, and Relativistic Field Theories, 5-10 July, 2021, on Mid-frequency (0.1-10 Hz) gravitational waves: Sources and detection methods with a review on strain power spectral density amplitude of various mid-frequency gravitational wave projects/concepts and with extended summaries on the progress of ZAIGA project and on the conceptual study of AMIGO.

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“…With RasDif on the Moon, seismic waves can be measured, specially at low frequency. A passing GW may change the Moon's humm, which can be measured [7,8]. The detection of weak, but continues GW signals from pulsars may be possible.…”

Section: Aant Benamingmentioning

confidence: 99%

The ultimate performance of the Rasnik 3-point alignment system

Graaf¹,

Bertolini²,

Heijningen³

et al. 2021

Preprint

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The Rasnik system is a 3-point optical displacement monitor with sub-nanometer precision. The CCD-Rasnik alignment system was developed in 1993 for the monitoring of the alignment of the muon chambers of the ATLAS Muon Spectrometer at CERN. Since then, the development has continued as new CMOS imaging pixel chips became available. The system's processes and parameters that limit the precision have been studied in detail. We conclude that only the quantum fluctuations to which the light level content of sensor pixels are subject to, is limiting the spatial resolution. The results of two Rasnik systems are compared to results from simulations, which are in good agreement: the best spatial resolution of 7 pm/ √Hz is reported. Finally, some applications of high-precision Rasnik systems are set out.

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Lunar Gravitational-wave Antenna

Cited by 62 publications

References 226 publications

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Stochastic Gravitational-Wave Backgrounds: Current Detection Efforts and Future Prospects

Mid-Frequency Gravitational Waves (0.1-10 Hz): Sources and Detection Methods Summary of the parallel session GW2 of MG16 Meeting

The ultimate performance of the Rasnik 3-point alignment system

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