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The Virgo interferometer
B Caron1, A Dominjon1, C Drezen1, R Flaminio1, X Grave1, F Marion1, L Massonnet1, C Mehmel1, R Morand1, B Mours1, V Sannibale1, M Yvert1, D Babusci2, S Bellucci2, S Candusso2, G Giordano2, G Matone2, J-M Mackowski3, L Pinard3, F Barone4, E Calloni4, L Di Fiore4, M Flagiello4, F Garufi4, A Grado4, M Longo4, M Lops4, S Marano4, L Milano4, S Solimeno4, V Brisson5, F Cavalier5, M Davier5, P Hello5, P Heusse5, P Mann5, Y Acker6, M Barsuglia6, B Bhawal6, F Bondu6, A Brillet6, H Heitmann6, J-M Innocent6, L Latrach6, C N Man6, M Pham-Tu6, E Tournier6, M Taubmann6, J-Y Vinet6, C Boccara7, Ph Gleyzes7, V Loriette7, J-P Roger7, G Cagnoli8, L Gammaitoni8, J Kovalik8, F Marchesoni8, M Punturo8, M Beccaria9, M Bernardini9, E Bougleux9, S Braccini9, C Bradaschia9, G Cella9, A Ciampa9, E Cuoco9, G Curci9, R Del Fabbro9, R De Salvo9, A Di Virgilio9, D Enard9, I Ferrante9, F Fidecaro9, A Giassi9, A Giazotto9, L Holloway9, P La Penna9, G Losurdo9, S Mancini9, M Mazzoni9, F Palla9, H-B Pan9, D Passuello9, P Pelfer9, R Poggiani9, R Stanga9, A Viceré9, Z Zhang9, V Ferrari10, E Majorana10, P Puppo10, P Rapagnani10 and F Ricci10
The Virgo gravitational wave detector is an interferometer with 3 km long arms in construction near Pisa to be commissioned in the year 2000. Virgo has been designed to achieve a strain sensitivity of a few times at 200 Hz. A large effort has gone into the conception of the mirror suspension system, which is expected to reduce noise to the level of at 10 Hz. The expected signals and main sources of noise are briefly discussed; the choices made are illustrated together with the present status of the experiment.
of a few times 
at 200 Hz. A large effort has gone into the conception of the mirror suspension system, which is expected to reduce noise to the level of 
at 10 Hz. The expected signals and main sources of noise are briefly discussed; the choices made are illustrated together with the present status of the experiment.