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Published January 2021 | Submitted
Journal Article Open

Reducing scattered light in LIGO's third observing run

Soni, S. ORCID icon
Austin, C.
Effler, A.
Schofield, R. M. S.
González-Abad, G. ORCID icon
Frolov, V. V.
Driggers, J. C.
Pele, A. ORCID icon
Urban, A. L.
Valdes, G.
Abbott, R.
Adams, C.
Adhikari, R. X. ORCID icon
Ananyeva, A.
Appert, S.
Arai, K. ORCID icon
Areeda, J. S.
Asali, Y.
Aston, S. M.
Baer, A. M.
Ball, M.
Ballmer, S. W.
Banagiri, S.
Barker, D.
Barsotti, L. ORCID icon
Bartlett, J.
Berger, B. K.
Betzwieser, J.
Bhattacharjee, D.
Billingsley, G. ORCID icon
Biscans, S. ORCID icon
Blair, C. D.
Blair, R. M.
Bode, N.
Booker, P.
Bork, R.
Bramley, A.
Brooks, A. F. ORCID icon
Brown, D. D.
Buikema, A. ORCID icon
Cahillane, C. ORCID icon
Cannon, K. C. ORCID icon
Chen, X.
Ciobanu, A. A. ORCID icon
Clara, F.
Cooper, S. J.
Corley, K. R.
Countryman, S. T.
Covas, P. B.
Coyne, D. C. ORCID icon
Datrier, L. E. H.
Davis, D. ORCID icon
Di Fronzo, C.
Dooley, K. L. ORCID icon
Dupej, P.
Dwyer, S. E.
Etzel, T.
Evans, M. ORCID icon
Evans, T. M. ORCID icon
Feicht, J. ORCID icon
Fernandez-Galiana, A. ORCID icon
Fritschel, P. ORCID icon
Fulda, P.
Fyffe, M.
Giaime, J. A.
Giardina, K. D.
Godwin, P.
Goetz, E.
Gras, S.
Gray, C.
Gray, R.
Green, A. C.
Gustafson, E. K.
Gustafson, R.
Hanks, J.
Hanson, J.
Hardwick, T.
Hasskew, R. K.
Heintze, M. C.
Helmling-Cornell, A. F. ORCID icon
Holland, N. A.
Jones, J. D.
Kandhasamy, S.
Karki, S.
Kasprzack, M. ORCID icon
Kawabe, K.
Kijbunchoo, N. ORCID icon
King, P. J.
Kissel, J. S. ORCID icon
Kumar, Rahul
Landry, M.
Lane, B. B.
Lantz, B. ORCID icon
Laxen, M.
Lecoeuche, Y. K. ORCID icon
Leviton, J.
Liu, J.
Lormand, M.
Lundgren, A. P.
Macas, R.
MacInnis, M.
Macleod, D. M.
Mansell, G. L.
Márka, S.
Márka, Z.
Martynov, D. V.
Mason, K.
Massinger, T. J. ORCID icon
Matichard, F. ORCID icon
Mavalvala, N.
McCarthy, R.
McClelland, D. E. ORCID icon
McCormick, S.
McCuller, L. ORCID icon
McIver, J. ORCID icon
McRae, T.
Mendell, G.
Merfeld, K.
Merilh, E. L.
Meylahn, F.
Mistry, T.
Mittleman, R.
Moreno, G.
Mow-Lowry, C. M. ORCID icon
Mozzon, S.
Mullavey, A. ORCID icon
Nelson, T. J. N.
Nguyen, P.
Nuttall, L. K.
Oberling, J.
Oram, Richard J.
Osthelder, C.
Ottaway, D. J. ORCID icon
Overmier, H.
Palamos, J. R.
Parker, W.
Payne, E.
Penhorwood, R.
Perez, C. J.
Pirello, M.
Radkins, H.
Ramirez, K. E.
Richardson, J. W. ORCID icon
Riles, K.
Robertson, N. A.
Rollins, J. G. ORCID icon
Romel, C. L.
Romie, J. H.
Ross, M. P.
Ryan, K.
Sadecki, T.
Sanchez, E. J.
Sanchez, L. E. ORCID icon
Saravanan, T. R.
Savage, R. L.
Schaetzl, D.
Schnabel, R. ORCID icon
Schwartz, E. ORCID icon
Sellers, D.
Shaffer, T.
Sigg, D. ORCID icon
Slagmolen, B. J. J. ORCID icon
Smith, J. R.
Sorazu, B.
Spencer, A. P.
Strain, K. A.
Sun, L. ORCID icon
Szczepańczyk, M. J.
Thomas, M.
Thomas, P.
Thorne, K. A.
Toland, K.
Torrie, C. I.
Traylor, G.
Tse, M. ORCID icon
Vajente, G. ORCID icon
Vander-Hyde, D. C.
Veitch, P. J.
Venkateswara, K.
Venugopalan, G. ORCID icon
Viets, A. D. ORCID icon
Vo, T.
Vorvick, C.
Wade, M.
Ward, R. L.
Warner, J.
Weaver, B.
Weiss, R.
Whittle, C. ORCID icon
Willke, B.
Wipf, C. C.
Xiao, L. ORCID icon
Yamamoto, H. ORCID icon
Yu, Hang ORCID icon
Yu, Haocun ORCID icon
Zhang, L. ORCID icon
Zucker, M. E. ORCID icon
Zweizig, J. ORCID icon
LIGO Scientific Collaboration


Noise due to scattered light has been a frequent disturbance in the advanced LIGO gravitational wave detectors, hindering the detection of gravitational waves. The non stationary scatter noise caused by low frequency motion can be recognized as arches in the time-frequency plane of the gravitational wave channel. In this paper, we characterize the scattering noise for LIGO and Virgo's third observing run O3 from April, 2019 to March, 2020. We find at least two different populations of scattering noise and we investigate the multiple origins of one of them as well as its mitigation. We find that relative motion between two specific surfaces is strongly correlated with the presence of scattered light and we implement a technique to reduce this motion. We also present an algorithm using a witness channel to identify the times this noise can be present in the detector.

Additional Information

© 2020 IOP Publishing Ltd. Received 14 August 2020; Revised 18 October 2020; Accepted 10 November 2020; Published 14 December 2020. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under Cooperative Agreement No. PHY-1764464. Advanced LIGO was built under Grant No. PHY-0823459. We acknowledge support from the NSF grant PHY-1806656, PHY-1505779, and PHY-1912604. We also acknowledge the discussions with the members of Detector Characterization Group of the LIGO Scientific Collaboration. For this paper, we use the data from the advanced LIGO detectors and we used the LIGO computing clusters to perform the analysis and calculations.

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August 20, 2023
October 20, 2023