Measurements of Superattenuator seismic isolation by Virgo interferometer

Each mirror of the interferometric gravitational wave antenna Virgo is attached to a Superattenuator, a chain of mechanical filters designed to suppress seismic vibrations, starting from a few Hz. The filter chain attenuation has been measured by exciting its suspension point with sinuisodal forces and using the interferometer as sensor. The attenuation, measured at different frequencies, is compliant with the requirements of the next generation antenna Advanced Virgo. In the third generation detector Einstein Telescope, the attenuation is sufficient above 3 Hz, independently of the underground site choice. © 2010 Elsevier B.V. All rights reserved.

Measurements of Superattenuator seismic isolation by Virgo interferometer

Acernese F.;Antonucci F.;Aoudia S.;Arun K. G.;Astone P.;Ballardin G.;Barone F.;Barsuglia M.;Bauer Th. S.;Beker M. G.;Bigotta S.;Birindelli S.;Bitossi M.;Bizouard M. A.;Blom M.;Boccara C.;Bondu F.;Bonelli L.;Bosi L.;Braccini S.;Bradaschia C.;Brillet A.;Brisson V.;Budzynski R.;Bulik T.;Bulten H. J.;Buskulic D.;Cagnoli G.;Calloni E.;Campagna E.;Canuel B.;Carbognani F.;Cavalier F.;Cavalieri R.;Cella G.;Cesarini E.;Chassande-Mottin E.;Chincarini A.;Cleva F.;Coccia E.;Colacino C. N.;Colas J.;Colla A.;Colombini M.;Corda C.;Corsi A.;Coulon J. -P.;Cuoco E.;D'Antonio S.;Dari A.;Dattilo V.;Davier M.;Day R.;De Rosa R.;Del Prete M.;Di Fiore L.;Di Lieto A.;Di Paolo Emilio M.;Di Virgilio A.;Dietz A.;Drago M.;Fafone V.;Ferrante I.;Fidecaro F.;Fiori I.;Flaminio R.;Fournier J. -D.;Franc J.;Frasca S.;Frasconi F.;Freise A.;Gammaitoni L.;Garufi F.;Gemme G.;Genin E.;Gennai A.;Giazotto A.;Granata M.;Greverie C.;Guidi G.;Heitmann H.;Hello P.;Hild S.;Huet D.;Jaranowski P.;Kowalska I.;Krolak A.;La Penna P.;Leroy N.;Letendre N.;Li T. G. F.;Lorenzini M.;Loriette V.;Losurdo G.;Mackowski J. -M.;Majorana E.;Man N.;Mantovani M.;Marchesoni F.;Marion F.;Marque J.;Martelli F.;Masserot A.;Menzinger F.;Michel C.;Milano L.;Minenkov Y.;Mohan M.;Moreau J.;Morgado N.;Morgia A.;Mosca S.;Moscatelli V.;Mours B.;Neri I.;Nocera F.;Pagliaroli G.;Palomba C.;Paoletti F.;Pardi S.;Parisi M.;Pasqualetti A.;Passaquieti R.;Passuello D.;Persichetti G.;Pichot M.;Piergiovanni F.;Pietka M.;Pinard L.;Poggiani R.;Prato M.;Prodi G. A.;Punturo M.;Puppo P.;Rabaste O.;Rabeling D. S.;Rapagnani P.;Re V.;Regimbau T.;Ricci F.;Robinet F.;Rocchi A.;Rolland L.;Romano R.;Rosinska D.;Ruggi P.;Salemi F.;Sassolas B.;Sentenac D.;Sturani R.;Swinkels B.;Toncelli A.;Tonelli M.;Tournefier E.;Travasso F.;Trummer J.;Vajente G.;van den Brand J. F. J.;van der Putten S.;Vavoulidis M.;Vedovato G.;Verkindt D.;Vetrano F.;Vicere A.;Vinet J. -Y.;Vocca H.;Was M.;Yvert M.

2010

Abstract

Each mirror of the interferometric gravitational wave antenna Virgo is attached to a Superattenuator, a chain of mechanical filters designed to suppress seismic vibrations, starting from a few Hz. The filter chain attenuation has been measured by exciting its suspension point with sinuisodal forces and using the interferometer as sensor. The attenuation, measured at different frequencies, is compliant with the requirements of the next generation antenna Advanced Virgo. In the third generation detector Einstein Telescope, the attenuation is sufficient above 3 Hz, independently of the underground site choice. © 2010 Elsevier B.V. All rights reserved.

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	Anno
	
				2010
			
	Rivista su cui è pubblicata l'opera
	
				ASTROPARTICLE PHYSICS
			
	Codice DOI
	
				https://dx.doi.org/10.1016/j.astropartphys.2010.01.006
			
	Codice Scopus
	
				2-s2.0-77649340862
			
	Appare nelle tipologie:
	
				01.01 - Articolo in rivista

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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11577/3578150

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