Reducing scattered light in LIGO’s third observing run
S. Soni(Louisiana State University), Corey Austin(Louisiana State University), A. Effler(LIGO Scientific Collaboration), R. M. S. Schofield(University of Oregon), G. González(Louisiana State University), V. V. Frolov(LIGO Scientific Collaboration), J. C. Driggers, A. Pele(LIGO Scientific Collaboration), A. L. Urban(Louisiana State University), G. Valdés(Louisiana State University), R. Abbott(California Institute of Technology), C. Adams(LIGO Scientific Collaboration), R. X. Adhikari(California Institute of Technology), A. Ananyeva(California Institute of Technology), S. Appert(California Institute of Technology), K. Arai(California Institute of Technology), J. S. Areeda(California State University, Fullerton), Y. Asali(Columbia University), S. M. Aston(LIGO Scientific Collaboration), A. M. Baer(Christopher Newport University), M. Ball(University of Oregon), S. Ballmer(Syracuse University), S. Banagiri(University of Minnesota), D. Barker, L. Barsotti(Massachusetts Institute of Technology), J. Bartlett, B. K. Berger(Stanford University), J. Betzwieser(LIGO Scientific Collaboration), D. Bhattacharjee(Missouri University of Science and Technology), G. Billingsley(California Institute of Technology), Sébastien Biscans(California Institute of Technology), C. D. Blair(LIGO Scientific Collaboration), R. M. Blair, N. Bode(Leibniz University Hannover), P. Booker(Leibniz University Hannover), R. Bork(California Institute of Technology), A. Bramley(LIGO Scientific Collaboration), A. F. Brooks(California Institute of Technology), D. Brown(ARC Centre of Excellence for Gravitational Wave Discovery), A. Buikema(Massachusetts Institute of Technology), C. Cahillane(California Institute of Technology), K. C. Cannon(The University of Tokyo), X. Chen(The University of Western Australia), A. A. Ciobanu(ARC Centre of Excellence for Gravitational Wave Discovery), F. Clara, S. J. Cooper(University of Birmingham), K. R. Corley(Columbia University), S. T. Countryman(Columbia University), P. B. Covas(Universitat de les Illes Balears), D. C. Coyne(California Institute of Technology), L. E. H. Datrier(University of Glasgow), D. Davis(Syracuse University), C. Di Fronzo(University of Birmingham), K. L. Dooley(University of Mississippi), P. Dupej(University of Glasgow), S. E. Dwyer, T. Etzel(California Institute of Technology), M. Evans(Massachusetts Institute of Technology), T. M. Evans(LIGO Scientific Collaboration), J. Feicht(California Institute of Technology), A. Fernandez-Galiana(Massachusetts Institute of Technology), P. Fritschel(Massachusetts Institute of Technology), P. Fulda(University of Florida), M. Fyffe(LIGO Scientific Collaboration), J. A. Giaime(Louisiana State University), K. D. Giardina(LIGO Scientific Collaboration), P. Godwin(Pennsylvania State University), E. Goetz(Missouri University of Science and Technology), S. Gras(Massachusetts Institute of Technology), C. Gray, R. Gray(University of Glasgow), A. C. Green(University of Florida), E. K. Gustafson, R. Gustafson(University of Michigan), J. Hanks, J. Hanson, T. Hardwick, R. K. Hasskew, M. C. Heintze, A. F. Helmling-Cornell(University of Oregon), N. A. Holland(Australian National University), J. D. Jones, S. Kandhasamy(Inter-University Centre for Astronomy and Astrophysics), S. Karki, M. Kasprzack, K. Kawabe, N. Kijbunchoo, Peter King, J. S. Kissel, Rahul Kumar, M. Landry, B. B. Lane, B. Lantz(Stanford University), M. Laxen, Y. K. Lecoeuche, J. Leviton, J. Liu(Leibniz University Hannover), M. Lormand, A. P. Lundgren(University of Portsmouth), R. Macas(Cardiff University), M. MacInnis, D. M. Macleod, G. L. Mansell, Szabolcs Márka, Z. Márka, Д. В. Мартынов(University of Birmingham), K. Mason, T. J. Massinger, F. Matichard, N. Mavalvala, R. McCarthy, D. E. McClelland, S. McCormick, L. McCuller, J. McIver, T. McRae, G. Mendell, K. Merfeld, E. L. Merilh, F. Meylahn, T. Mistry(University of Sheffield), R. Mittleman, G. Moreno, C. M. Mow–Lowry, S. Mozzon, A. Mullavey, T. J. N. Nelson, P. Nguyen, L. K. Nuttall, J. Oberling, Richard J. Oram, C. Osthelder, D. J. Ottaway(ARC Centre of Excellence for Gravitational Wave Discovery), H. Overmier, J. R. Palamos, W. Parker(Southern University and Agricultural and Mechanical College), Ethan Payne(ARC Centre of Excellence for Gravitational Wave Discovery), R. Penhorwood, C. J. Perez, M. Pirello, H. Radkins, K. E. Ramirez(The University of Texas Rio Grande Valley), J. W. Richardson, K. Riles, N. A. Robertson, J. G. Rollins, C. L. Romel, J H Romie, M. P. Ross(University of Washington), K. Ryan, T. Sadecki, E. J. Sanchez, L. E. Sanchez, T. R. Saravanan, R. L. Savage, D. Schaetzl, Roman Schnabel(Universität Hamburg), E. Schwartz, D. Sellers, T. Shaffer, D. Sigg, B. J. J. Slagmolen, J. R. Smith, B. Sorazu, A. P. Spencer, K. A. Strain, L. Sun, M. J. Szczepańczyk, M. Thomas, P. Thomas, K. Thorne, K. Toland, C I Torrie, G. Traylor, M. Tse, G. Vajente, D. C. Vander‐Hyde, P. J. Veitch, K. Venkateswara, G. Venugopalan, A. D. Viets(Concordia University Wisconsin), T. Vo, C. Vorvick, M. Wade(Kenyon College), R. L. Ward, J. Warner, B. Weaver, R. Weiss, C. Whittle, B. Willke, C. C. Wipf, S. Xiao, H. Yamamoto, Hang Yu, Haocun Yu, L. Zhang, M. E. Zucker, J. Zweizig
Cited by 106Open Access
Abstract
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'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.
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