Noise from scattered light in Virgo's second science run data

被引：58

作者：

Accadia, T. ^{[1
]}

Acernese, F. ^{[2
,4
]}

Antonucci, F. ^{[5
]}

Astone, P. ^{[5
]}

Ballardin, G. ^{[7
]}

Barone, F. ^{[2
,4
]}

Barsuglia, M. ^{[8
]}

Bauer, Th S. ^{[9
]}

Beker, M. G. ^{[9
]}

Belletoile, A. ^{[1
]}

Birindelli, S. ^{[11
]}

Bitossi, M. ^{[13
]}

Bizouard, M. A. ^{[16
]}

Blom, M. ^{[9
]}

Bondu, F. ^{[12
]}

Bonelli, L. ^{[13
,14
]}

Bonnand, R. ^{[18
]}

Boschi, V. ^{[13
]}

Bosi, L. ^{[19
]}

Bouhou, B. ^{[8
]}

Braccini, S. ^{[13
]}

Bradaschia, C. ^{[13
]}

Brillet, A. ^{[11
]}

Brisson, V. ^{[16
]}

Budzynski, R. ^{[22
]}

Bulik, T. ^{[23
,24
]}

Bulten, H. J. ^{[9
,10
]}

Buskulic, D. ^{[1
]}

Buy, C. ^{[8
]}

Cagnoli, G. ^{[28
]}

Calloni, E. ^{[21
,22
]}

Campagna, E. ^{[28
,29
]}

Canuel, B. ^{[7
]}

Carbognani, F. ^{[7
]}

Cavalier, F. ^{[16
]}

Cavalieri, R. ^{[7
]}

Cella, G. ^{[13
]}

Cesarini, E. ^{[29
]}

Mottin, E. Chassande

Chincarini, A. ^{[30
]}

Cleva, F. ^{[11
]}

Coccia, E. ^{[31
]}

Colacino, C. N. ^{[13
,14
]}

Colas, J. ^{[7
]}

Colla, A. ^{[5
]}

Colombini, M. ^{[6
]}

Corsi, A. ^{[5
]}

Coulon, J-P ^{[11
]}

Cuoco, E. ^{[7
]}

D'Antonio, S. ^{[31
]}

机构：

[1] Univ Savoie, LAPP, IN2P3, CNRS, F-74941 Annecy Le Vieux, France

[2] INFN, Sez Napoli, Naples, Italy

[3] Univ Naples Federico II, Naples, Italy

[4] Univ Salerno Fisciano, I-84084 Salerno, Italy

[5] INFN, Sez Roma, I-00185 Rome, Italy

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

[7] EGO, I-56021 Cascina, PI, Italy

[8] Univ Denis Diderot Paris 7, CNRS, IN2P3, APC, Paris, France

[9] Natl Inst Subatom Phys, Nikhef, NL-1009 DB Amsterdam, Netherlands

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

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

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

[13] INFN, Sez Pisa, I-56127 Pisa, Italy

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

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

[16] Univ Paris 11, CNRS, IN2P3, LAL, F-91898 Orsay, France

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

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

[19] INFN, Sez Perugia, I-06123 Perugia, Italy

[20] Univ Perugia, I-06123 Perugia, Italy

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

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

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

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

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

[26] IPJ, PL-05400 Otwock, Poland

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

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

[29] Univ Urbino, I-61029 Urbino, Italy

[30] INFN, Sez Genova, I-16146 Genoa, Italy

[31] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy

[32] Univ Roma Tor Vergata, I-00133 Rome, Italy

[33] RMKI, H-2933 Budapest, Hungary

[34] INFN, Grp Collegato Trento, I-38050 Trento, Italy

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

[36] INFN, Sez Padova, I-35131 Padua, Italy

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

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

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

来源：

CLASSICAL AND QUANTUM GRAVITY | 2010年 / 27卷 / 19期

关键词：

WAVE INTERFEROMETRIC DETECTORS;

D O I：

10.1088/0264-9381/27/19/194011

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Virgo is one of the large, ground-based interferometers aimed at detecting gravitational waves. One of the technical problems limiting its sensitivity is caused by light in the output beams which is backscattered by seismically excited surfaces and couples back into the main beam of the interferometer. The resulting noise was thoroughly studied, measured and mitigated before Virgo's second science run (VSR2). The residual noise during VSR2, which increases in periods with a large microseism activity, is accurately predicted by the theoretical model. The scattered light has been associated with transient events in the gravitational-wave signal of the interferometer.

引用

页数：9

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