Reducing scattered light in LIGO's third observing run
- Creators
- Soni, S.
- Austin, C.
- Effler, A.
- Schofield, R. M. S.
- González-Abad, G.
- Frolov, V. V.
- Driggers, J. C.
- Pele, A.
- Urban, A. L.
- Valdes, G.
- Abbott, R.
- Adams, C.
- Adhikari, R. X.
- Ananyeva, A.
- Appert, S.
- Arai, K.
- Areeda, J. S.
- Asali, Y.
- Aston, S. M.
- Baer, A. M.
- Ball, M.
- Ballmer, S. W.
- Banagiri, S.
- Barker, D.
- Barsotti, L.
- Bartlett, J.
- Berger, B. K.
- Betzwieser, J.
- Bhattacharjee, D.
- Billingsley, G.
- Biscans, S.
- Blair, C. D.
- Blair, R. M.
- Bode, N.
- Booker, P.
- Bork, R.
- Bramley, A.
- Brooks, A. F.
- Brown, D. D.
- Buikema, A.
- Cahillane, C.
- Cannon, K. C.
- Chen, X.
- Ciobanu, A. A.
- Clara, F.
- Cooper, S. J.
- Corley, K. R.
- Countryman, S. T.
- Covas, P. B.
- Coyne, D. C.
- Datrier, L. E. H.
- Davis, D.
- Di Fronzo, C.
- Dooley, K. L.
- Dupej, P.
- Dwyer, S. E.
- Etzel, T.
- Evans, M.
- Evans, T. M.
- Feicht, J.
- Fernandez-Galiana, A.
- Fritschel, P.
- 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.
- Holland, N. A.
- Jones, J. D.
- Kandhasamy, S.
- Karki, S.
- Kasprzack, M.
- Kawabe, K.
- Kijbunchoo, N.
- King, P. J.
- Kissel, J. S.
- Kumar, Rahul
- Landry, M.
- Lane, B. B.
- Lantz, B.
- Laxen, M.
- Lecoeuche, Y. K.
- 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.
- Matichard, F.
- Mavalvala, N.
- McCarthy, R.
- McClelland, D. E.
- McCormick, S.
- McCuller, L.
- McIver, J.
- McRae, T.
- Mendell, G.
- Merfeld, K.
- Merilh, E. L.
- Meylahn, F.
- Mistry, T.
- Mittleman, R.
- Moreno, G.
- Mow-Lowry, C. M.
- Mozzon, S.
- Mullavey, A.
- Nelson, T. J. N.
- Nguyen, P.
- Nuttall, L. K.
- Oberling, J.
- Oram, Richard J.
- Osthelder, C.
- Ottaway, D. J.
- Overmier, H.
- Palamos, J. R.
- Parker, W.
- Payne, E.
- Penhorwood, R.
- Perez, C. J.
- Pirello, M.
- Radkins, H.
- Ramirez, K. E.
- Richardson, J. W.
- Riles, K.
- Robertson, N. A.
- Rollins, J. G.
- Romel, C. L.
- Romie, J. H.
- Ross, M. P.
- Ryan, K.
- Sadecki, T.
- Sanchez, E. J.
- Sanchez, L. E.
- Saravanan, T. R.
- Savage, R. L.
- Schaetzl, D.
- Schnabel, R.
- Schwartz, E.
- Sellers, D.
- Shaffer, T.
- Sigg, D.
- Slagmolen, B. J. J.
- Smith, J. R.
- Sorazu, B.
- Spencer, A. P.
- Strain, K. A.
- Sun, L.
- Szczepańczyk, M. J.
- Thomas, M.
- Thomas, P.
- Thorne, K. A.
- Toland, K.
- Torrie, C. I.
- Traylor, G.
- Tse, M.
- Vajente, G.
- Vander-Hyde, D. C.
- Veitch, P. J.
- Venkateswara, K.
- Venugopalan, G.
- Viets, A. D.
- Vo, T.
- Vorvick, C.
- Wade, M.
- Ward, R. L.
- Warner, J.
- Weaver, B.
- Weiss, R.
- Whittle, C.
- Willke, B.
- Wipf, C. C.
- Xiao, L.
- Yamamoto, H.
- Yu, Hang
- Yu, Haocun
- Zhang, L.
- Zucker, M. E.
- Zweizig, J.
- LIGO Scientific Collaboration
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 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.
Attached Files
Submitted - 2007.14876.pdf
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Additional details
- Eprint ID
- 105189
- DOI
- 10.1088/1361-6382/abc906
- Resolver ID
- CaltechAUTHORS:20200901-071323982
- arXiv
- arXiv:2007.14876
- PHY-1764464
- NSF
- PHY-0823459
- NSF
- PHY-1806656
- NSF
- PHY-1505779
- NSF
- PHY-1912604
- NSF
- Created
-
2020-09-08Created from EPrint's datestamp field
- Updated
-
2022-10-28Created from EPrint's last_modified field
- Caltech groups
- LIGO