Searching for the causes of anomalous Advanced LIGO noise

Creators: Berger, B. K. (Contact Person); Areeda, J. S.; Barker, J. D.; Effler, A.; Goetz, E.; Helmling-Cornell, A. F.; Lantz, B.; Lundgren, A. P.; Macleod, D. M.; McIver, J.; Mittleman, R.; Nguyen, P.; Pele, A.; Pham, H.; Rangnekar, P.; Rink, K.; Schofield, R. M. S.; Smith, J. R.; Soni, S.; Warner, J.; Abbott, R.; Adhikari, R. X.; Ananyeva, A.; Appert, S.; Arai, K.; Asali, Y.; Aston, S. M.; Baer, A. M.; Ball, M.; Ballmer, S. W.; Banagiri, S.; Barker, D.; Barsotti, L.; Betzwieser, J.; Bhattacharjee, D.; Billingsley, G.; Biscans, S.; Blair, C. D.; Blair, R. M.; Bode, N.; Booker, P.; Bork, R.; Brooks, A. F.; Brown, D. D.; Cahillane, C.; Chen, X.; Ciobanu, A. A.; Clara, F.; Compton, C. M.; 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.; Driggers, J. C.; Dwyer, S. E.; Etzel, T.; Evans, M.; Evans, T. M.; Feicht, J.; Fernandez-Galiana, A.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Giaime, J. A.; Giardina, K. D.; Godwin, P.; Gras, S.; Gray, C.; Gray, R.; Green, A. C.; Gupta, A.; Gustafson, E. K.; Gustafson, R.; Hanks, J.; Hanson, J.; Hasskew, R. K.; Heintze, M. C.; Holland, N. A.; Kandhasamy, S.; Karki, S.; Kasprzack, M.; Kawabe, K.; Kijbunchoo, N.; King, P. J.; Kissel, J. S.; Kumar, Rahul; Landry, M.; Lane, B. B.; Laxen, M.; Lecoeuche, Y. K.; Leviton, J.; Liu, J.; Lormand, M.; Macas, R.; MacInnis, M.; Mansell, G. L.; Márka, S.; Márka, Z.; Martynov, D. V.; Mason, K.; Matichard, F.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McCuller, L.; McRae, T.; Mendell, G.; Merfeld, K.; Merilh, E. L.; Meylahn, F.; Mistry, T.; Moreno, G.; Mow-Lowry, C. M.; Mozzon, S.; Mullavey, A.; Nelson, T. J. N.; Nuttall, L. K.; Oberling, J.; Oram, Richard J.; Osthelder, C.; Ottaway, D. J.; Overmier, H.; Parker, W.; Payne, E.; Penhorwood, R.; Perez, C. J.; Pirello, M.; 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.; Sorazu, B.; Spencer, A. P.; Sun, L.; Szczepańczyk, M. J.; Thomas, M.; Thomas, P.; Thorne, K. A.; Toland, K.; Torrie, C. I.; Traylor, G.; Tse, M.; Vajente, G.; Valdes, G.; Vander-Hyde, D. C.; Veitch, P. J.; Venugopalan, G.; Viets, A. D.; Vorvick, C.; Wade, M.; Ward, R. L.; 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.

Abstract

Advanced LIGO and Advanced Virgo have detected gravitational waves from astronomical sources to open a new window on the Universe. To explore this new realm requires an exquisite level of detector sensitivity, meaning that the much stronger signal from instrumental and environmental noise must be rejected. Selected examples of unwanted noise in Advanced LIGO are presented. The initial focus is on how the existence of this noise (characterized by particular frequencies or time intervals) was discovered. Then, a variety of methods are used to track down the source of the noise, e.g., a fault within the instruments or coupling from an external source. The ultimate goal of this effort is to mitigate the noise by either fixing equipment or by augmenting methods to suppress the coupling to the environment.

Acknowledgement

The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom and the Max-Planck-Society (MPS) for support of the construction of Advanced LIGO. Additional support for Advanced LIGO was provided by the Australian Research Council.

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 Award No. PHY-0823459. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grant Nos. PHY-0757058 and PHY-0823459. This work carries LIGO Document No. P2000495.

This material is based upon work supported by NSF's LIGO Laboratory, which is a major facility fully funded by the National Science Foundation.

The authors are grateful for computational resources provided by the LIGO Laboratory at Caltech, LHO, and LLO and supported by the National Science Foundation Grant Nos. PHY-0757058 and PHY-0832459.

Data Availability

The data that support the findings of this study are available from the corresponding author upon reasonable request.

Conflict of Interest

The authors have no conflicts to disclose.

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