First joint gravitational wave search by the AURIGA–EXPLORER–NAUTILUS–Virgo Collaboration

Acernese, F.; Alshourbagy, M.; Amico, P.; Antonucci, F.; Aoudia, S.; Astone, P.; Avino, S.; Babusci, D.; Baggio, Lucio; Ballardin, G.; Barone, F.; Barsotti, L.; Barsuglia, M.; Bassan, M.; Bauer, Th.; Bignotto, M.; Bigotta, S.; Birindelli, S.; Bizouard, M. A.; Boccara, Claude; Bonaldi, M.; Bondu, F.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brillet, A.; Brisson, V.; Buskulic, D.; Cagnoli, G.; Calloni, E.; Camarda, M.; Campagna, E.; Carbognani, F.; Carelli, P.; Cavalier, F.; Cavalieri, R.; Cavallari, G.; Cella, G.; Cerdonio, M.; Cesarini, E.; Chassande–Mottin, E.; Chincarini, A.; Clapson, A. C.; Cleva, F.; Coccia, E.; Conti, L.; Corda, Christian; Corsi, A.; Cottone, F.; Coulon, J.‐P.; Cuoco, E.; D’Antonio, S.; Dari, A.; Dattilo, V.; Davier, M.; Rosa, R. De; Prete, M. Del; Fiore, L. Di; Lieto, A. Di; Emilio, M. Di Paolo; Virgilio, A. Di; Drago, M.; Dubath, F.; Evans, M.; Fafone, V.; Falferi, P.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Foffa, Stefano; Fortini, P.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Garufi, F.; Gemme, G.; Genin, É.; Gennai, A.; Giazotto, A.; Giordano, G.; Giordano, L.; Granata, V.; Greverie, C.; Grosjean, Daniel; Guidi, G. M.; Hamdani, S.; Hebri, S.; Heitmann, H.; Hello, P.; Huet, D.; Kreckelbergh, S.; Penna, P. La; Laval, M.; Leroy, N.; Letendre, N.; Liguori, N.; Longo, Stefano B.; López, B.; Lorenzini, M.; Loriette, V.; Losurdo, G.; Mackowski, J.‐M.; Maggiore, Michele; Majorana, E.; Man, C. N.; Mantovani, M.; Marchesoni, F.; Marini, A.; Marion, F.; Marque, J.; Martelli, F.; Masserot, A.; Menzinger, F.; Mezzena, R.; Milano, L.; Minenkov, Y.; Mion, A.; Modena, I.; Modestino, G.; Moins, C.; Moleti, Arturo; Moreau, Julien; Morgado, N.; Mosca, S.; Mours, B.; Neri, I.; Nocera, F.; Ortolan, A.; Pagliaroli, G.; Pallottino, G. V.; Palomba, C.; Paoletti, F.; Pardi, S.; Parodi, R.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Mortari, G. Piano; Piergiovanni, F.; Pinard, L.; Pizzella, G.; Poggi, S.; Poggiani, R.; Prodi, G. A.; Punturo, M.; Puppo, P.; Quintieri, L.; Rapagnani, P.; Re, V.; Regimbau, T.; Remillieux, A.; Ricci, F.; Ricciardi, I.; Rocchi, A.; Rolland, L.; Romano, R.; Ronga, F.; Ruggi, P.; Russo, G.; Salemi, F.; Solimeno, S.; Spallicci, A.; Sturani, R.; Taffarello, L.; Tarallo, M.; Terenzi, R.; Toncelli, A.; Tonelli, M.; Torrioli, G.; Tournefier, E.; Travasso, F.; Tremola, C.; Vaccarone, R.; Vajente, G.; Vandoni, G.; Vedovato, G.; Brand, Johannes; Putten, S. van der; Verkindt, D.; Vetrano, F.; Viceré, A.; Vinante, Andrea; Vinet, J.-Y.; Visco, M.; Vitale, S.; Vocca, H.; Yvert, M.; Zendri, J.-P.

doi:10.1088/0264-9381/25/20/205007

Cited by 13 publications

(9 citation statements)

References 28 publications

(29 reference statements)

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“…43 The AURIGA-EXPLORER-NAUTILUS-Virgo Collaboration applied a methodology to the search for coincident burst excitations over a 24 h long joint data set. 44 The MiniGRAIL 45 and Schenberg 46 cryogenic spherical GW detectors are for omnidirectional GW detection.…”

Section: High Frequency Band (10 Hz -100 Khz)mentioning

confidence: 99%

Gravitational waves: Classification, methods of detection, sensitivities and sources

Kuroda

Pan

2015

Int. J. Mod. Phys. D

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After giving a brief introduction and presenting a complete classification of gravitational waves (GWs) according to their frequencies, we review and summarize the detection methods, the sensitivities, and the sources. We notice that real-time detections are possible above 300 pHz. Below 300 pHz, the detections are possible on GW imprints or indirectly. We are on the verge of detection. The progress in this field will be promising and thriving. We will see improvement of a few orders to several orders of magnitude in the GW detection sensitivities over all frequency bands in the next hundred years.

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Section: High Frequency Band (10 Hz -100 Khz)mentioning

confidence: 99%

Gravitational waves: Classification, methods of detection, sensitivities and sources

Kuroda

Pan

2015

Int. J. Mod. Phys. D

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“…The interferometer detectors LIGO [14], Virgo [15], and KAGRA [16] with km size arm lengths can search for gravitational waves with frequencies from 10 Hz to 1 kHz. In this frequency band, resonant bar experiments [17] are complementary to the interferometers [18]. Furthermore, interferometers can be used to measure gravitational waves with the frequencies between 1 kHz and 100 MHz.…”

Section: Introductionmentioning

confidence: 99%

Probing GHz gravitational waves with graviton–magnon resonance

et al. 2020

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A novel method for extending the frequency frontier in gravitational wave observations is proposed. It is shown that gravitational waves can excite a magnon. Thus, gravitational waves can be probed by a graviton-magnon detector which measures resonance fluorescence of magnons. Searching for gravitational waves with a wave length λ by using a ferromagnetic sample with a dimension l, the sensitivity of the graviton-magnon detector reaches spectral densities, around 5.4 × 10 −22 × ( l λ/2π ) −2 [Hz −1/2 ] at 14 GHz and 8.6 × 10 −21 × ( l λ/2π ) −2 [Hz −1/2 ] at 8.2 GHz, respectively.

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“…NAUTILUS put an upper limit on periodic sources ranging from 3.4 × 10 −23 to 1.3 × 10 −22 depending on frequency in their all-sky search [23]. The AURIGA-EXPLORER-NAUTILUS-Virgo Collaboration applied a methodology to the search for coincident burst excitations over a 24 h long joint data set [4]. The…”

Section: Cryogenic Resonator Experimentsmentioning

confidence: 99%

A brief history of gravitational wave research

Chen

Nester

2017

Chinese Journal of Physics

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For the benefit of the readers of this journal, the editors requested that we prepare a brief review of the history of the development of the theory, the experimental attempts to detect them, and the recent direct observations of gravitational waves (GWs). The theoretical ideas and disputes beginning with Einstein in 1916 regarding the existence and nature of GWs and the extent to which one can rely on the electromagnetic analogy, especially the controversies regarding the quadrupole formula and whether GWs carry energy, are discussed. The theoretical conclusions eventually received strong observational support from the binary pulsar. This provided compelling, although indirect, evidence for GWs carrying away energy--as predicted by the quadrupole formula. On the direct detection experimental side, Weber started more than 50 years ago. In 1966, his bar for GW detection reached a strain sensitivity of a few times 10^-16. His announcement of coincident signals (now considered spurious) stimulated many experimental efforts from room temperature resonant masses to cryogenic detectors and laser-interferometers. Now there are km-sized interferometric detectors (LIGO Hanford, LIGO Livingston, Virgo and KAGRA). Advanced LIGO first reached a strain sensitivity of the order of 10^-22. During their first 130 days of observation (O1 run), with the aid of templates generated by numerical relativity, they did make the first detections: two 5-sigma GW events and one likely event. Besides earth-based GW detectors, the drag-free sensitivity of the LISA Pathfinder has already reached to the LISA goal level, paving the road for space GW detectors. Over the whole GW spectrum (from aHz to THz) there are efforts for detection, notably the very-low-frequency band (pulsar timing array [PTA], 300 pHz-100 nHz) and the extremely-low (Hubble)-frequency (cosmic microwave background [CMB] experiment, 1 aHz-10 fHz).Comment: revised version to appear in Chinese Journal of Physic

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First joint gravitational wave search by the AURIGA–EXPLORER–NAUTILUS–Virgo Collaboration

Cited by 13 publications

References 28 publications

Gravitational waves: Classification, methods of detection, sensitivities and sources

Gravitational waves: Classification, methods of detection, sensitivities and sources

Probing GHz gravitational waves with graviton–magnon resonance

A brief history of gravitational wave research

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