The seismic Superattenuators of the Virgo gravitational waves interferometer

被引：28

作者：

Accadia, T. ^{[21
]}

Acernese, F. ^{[6
,8
]}

Antonucci, F. ^{[14
]}

Astone, P. ^{[14
]}

Ballardin, G. ^{[1
]}

Barone, F. ^{[6
,8
]}

Barsuglia, M. ^{[2
]}

Bauer, Th. S. ^{[23
]}

Beker, M. G. ^{[23
]}

Belletoile, A. ^{[3
,21
]}

Birindelli, S. ^{[25
]}

Bitossi, M. ^{[11
]}

Bizouard, M. A. ^{[19
]}

Blom, M. ^{[23
]}

Boccara, C. ^{[20
]}

Bondu, F. ^{[25
,26
]}

Bonelli, L. ^{[11
,12
]}

Bonnand, R. ^{[22
]}

Boschi, V. ^{[11
]}

Bosi, L. ^{[9
]}

Bouhou, B. ^{[2
]}

Braccini, S. ^{[11
]}

Bradaschia, C. ^{[11
]}

Brillet, A. ^{[25
]}

Brisson, V. ^{[19
]}

Budzynski, R. ^{[32
]}

Bulik, T. ^{[33
,34
]}

Bulten, H. J. ^{[23
,24
]}

Buskulic, D. ^{[21
]}

Buy, C. ^{[2
]}

Cagnoli, G. ^{[3
]}

Calloni, E. ^{[6
,7
]}

Campagna, E. ^{[3
,4
]}

Canuel, B. ^{[1
]}

Carbognani, F. ^{[1
]}

Cavalier, F. ^{[19
]}

Cavalieri, R. ^{[1
]}

Cella, G. ^{[11
,12
]}

Cesarini, E. ^{[4
]}

Chassande-Mottin, E.

Chincarini, A. ^{[5
]}

Cleva, F. ^{[25
]}

Coccia, E. ^{[16
,17
]}

Colacino, C. N. ^{[11
,12
]}

Colas, J. ^{[1
]}

Colla, A. ^{[14
,15
]}

Colombini, M.

Corsi, A. ^{[14
]}

Coulon, J. -P. ^{[25
]}

Cuoco, E. ^{[1
]}

机构：

[1] European Gravitat Observ, I-56021 Cascina, Pi, Italy

[2] Univ Paris 07, CNRS, UMR7164, IN2P3,Observ Paris,CEA,DSM IRFU, F-75221 Paris 05, France

[3] INFN, Sez Firenze, I-50019 Sesto Fiorentino, Italy

[4] Univ Urbino Carlo Bo, I-61029 Urbino, Italy

[5] Ist Nazl Fis Nucl, Sez Genova, I-16146 Genoa, Italy

[6] Ist Nazl Fis Nucl, Sez Napoli, I-80126 Naples, Italy

[7] Complesso Univ Monte S Angelo, Univ Naples Federico II, I-80126 Naples, Italy

[8] Univ Salerno, I-84084 Salerno, Italy

[9] INFN, Sez Perugia, I-6123 Perugia, Italy

[10] Univ Perugia, I-6123 Perugia, Italy

[11] Ist Nazl Fis Nucl, Sez Perugia, I-56127 Pisa, Italy

[12] Univ Pisa, I-56127 Pisa, Italy

[13] Univ Siena, I-53100 Siena, Italy

[14] Ist Nazl Fis Nucl, Sez Roma, I-00185 Rome, Italy

[15] Univ Roma La Sapienza, I-00185 Rome, Italy

[16] Ist Nazl Fis Nucl, Sez Roma Tor Vergata, I-67100 Laquila, Italy

[17] Univ Roma Tor Vergata, I-67100 Laquila, Italy

[18] Univ Aquila, I-67100 Laquila, Italy

[19] Univ Paris Sud, LAL, IN2P3, CNRS, F-91898 Orsay, France

[20] ESPCI, CNRS, F-75005 Paris, France

[21] Univ Savoie, Lab Annecy Le Vieux Phys Particules, IN2P3, CNRS, F-74941 Annecy Le Vieux, France

[22] CNRS, IN2P3, LMA, F-69622 Villeurbanne, France

[23] Natl Inst Subat Phys, NL-1009 DB Amsterdam, Netherlands

[24] Vrije Univ Amsterdam, NL-1081 HV Amsterdam, Netherlands

[25] Univ Nice Sophia Antipolis, CNRS, Observ Cote Azur, F-06304 Nice, France

[26] Univ Rennes 1, CNRS, Inst Phys Rennes, F-35042 Rennes, France

[27] Ist Nazl Fis Nucl, Grp Collegato Trento, I-38050 Trento, Italy

[28] Univ Trent, I-38050 Trento, Italy

[29] Ist Nazl Fis Nucl, Sez Padova, I-35131 Padua, Italy

[30] Univ Padua, I-35131 Padua, Italy

[31] IM PAN, PL-00956 Warsaw, Poland

[32] Warsaw Univ, PL-00681 Warsaw, Poland

[33] Warsaw Univ, Astron Observ, PL-00478 Warsaw, Poland

[34] CAMK PAN, PL-00716 Warsaw, Poland

[35] Bialystok Univ, PL-15424 Bialystok, Poland

[36] IPJ, PL-05400 Otwock, Poland

[37] Inst Astron, PL-65265 Zielona Gora, Poland

[38] RMKI, H-1121 Budapest, Hungary

[39] Univ Birmingham, Birmingham B15 2TT, W Midlands, England

[40] Univ Glasgow, Glasgow G12 8QQ, Lanark, Scotland

来源：

JOURNAL OF LOW FREQUENCY NOISE VIBRATION AND ACTIVE CONTROL | 2011年 / 30卷 / 01期

基金：

英国科学技术设施理事会;

关键词：

SUPER ATTENUATOR; NOISE; BAND;

D O I：

10.1260/0263-0923.30.1.63

中图分类号：

O42 [声学];

学科分类号：

070206 ; 082403 ;

摘要：

The Virgo experiment, located near Pisa, Italy, is a large laser Michelson interferometer aiming at the first direct detection of gravitational waves. The interferometer monitors the relative distance of its mirrors placed at the ends of two 3 km-long perpendicular arms. The goal is to measure spectral differential variations of the arm lengths of 10(-18) m/Hz(1/2) in the frequency range from 10 Hz to 10 kHz. Avoiding spurious motions of the optical components is therefore essential to detect gravitational waves. Since the ground motion is 9 orders of magnitude larger than the arm length variations induced by gravitational waves, the seismic noise is the dominant low frequency noise source for terrestrial gravitational wave interferometers. The seismic isolation is obtained suspending the mirrors by an 8-meter tall chain of cascaded mechanical filters, called "Superattenuator" (SA). The Superattenuator is a passive device acting as a low pass filter in all six degrees of freedom, capable of attenuating the ground motion by more than 10 orders of magnitude, starting from a few Hz. To further reduce the seismic disturbances, the filter chain is suspended from an actively stabilized platform that compensates for low frequency and large amplitude oscillations caused by the mechanical resonances of the chain. In this article we describe the Superattenuator together with its control system, and we report about its performance.

引用

页码：63 / 79

页数：17