LIGO detector characterization in the second and third observing runs

Davis, D.; Areeda, J. S.; Berger, B. K.; Bruntz, R.; Effler, A.; Essick, R. C.; Fisher, R. P.; Godwin, P.; Goetz, E.; Helmling-Cornell, A. F.; Hughey, B.; Katsavounidis, E.; Lundgren, A. P.; Macleod, D. M.; Márka, Z.; Massinger, T. J.; Matas, A.; McIver, J.; Mo, G.; Mogushi, K.; Nguyen, P.; Nuttall, L. K.; Schofield, R. M. S.; Shoemaker, D. H.; Soni, S.; Stuver, A. L.; Urban, A. L.; Valdes, G.; Walker, M.; Abbott, R.; Adams, C.; Adhikari, R. X.; Ananyeva, A.; Appert, S.; Arai, K.; Asali, Y.; Aston, S. M.; Austin, C.; Baer, A. M.; Ball, M.; Ballmer, S. W.; Banagiri, S.; Barker, D.; Barschaw, C.; Barsotti, L.; Bartlett, J.; Betzwieser, J.; Beda, R.; Bhattacharjee, D.; Bidler, J.; 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.; Callister, T. A.; Santoro, G. Caneva; Cannon, K. C.; Carlin, J.; Chandra, K.; Chen, X.; Christensen, N.; Ciobanu, A. A.; Clara, F.; Compton, C. M.; Cooper, S. J.; Corley, K. R.; Coughlin, M. W.; Countryman, S. T.; Covas, P. B.; Coyne, D. C.; Crowder, S. G.; Canton, T. Dal; Danila, B.; Datrier, L. E. H.; Davies, G. S.; Dent, T.; Didio, N. A.; Fronzo, C. Di; Dooley, K. L.; Driggers, J. C.; Dupej, P.; Dwyer, S. E.; Etzel, T.; Evans, M.; Evans, T. M.; Fairhurst, S.; Feicht, J.; Fernandez-Galiana, A.; Frey, R.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gadre, B. U.; Giaime, J. A.; Giardina, K. D.; González, G.; Gras, S.; Gray, C.; Gray, R.; Green, A. C.; Gupta, A.; Gustafson, E. K.; Gustafson, R.; Hanks, J.; Hanson, J.; Hardwick, T.; Harry, I. W.; Hasskew, R. K.; Heintze, M. C.; Heinzel, J.; Holland, N. A.; Hollows, I. J.; Hoy, C. G.; Hughey, S.; Jadhav, S. J.; Janssens, K.; Johns, G.; Jones, J. D.; Kandhasamy, S.; Karki, S.; Kasprzack, M.; Kawabe, K.; Keitel, D.; Kijbunchoo, N.; Kim, Y. M.; King, P. J.; Kissel, J. S.; Kulkarni, S.; Kumar, Rahul; Landry, M.; Lane, B. B.; Lantz, B.; Laxen, M.; Lecoeuche, Y. K.; Leviton, J.; Liu, J.; Lormand, M.; Macas, R.; Macedo, A.; MacInnis, M.; Mandic, V.; Mansell, G. L.; Márka, S.; Martinez, B.; Martinovic, K.; Martynov, D. V.; Mason, K.; Matichard, F.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McCormick, S.; McCuller, L.; McIsaac, C.; McRae, T.; Mendell, G.; Merfeld, K.; Merilh, E. L.; Meyers, P. M.; Meylahn, F.; Michaloliakos, I.; Middleton, H.; Mills, J. C.; Mistry, T.; Mittleman, R.; Moreno, G.; Mow-Lowry, C. M.; Mozzon, S.; Mueller, L.; Mukund, N.; Mullavey, A.; Muth, J.; Nelson, T. J. N.; Neunzert, A.; Nichols, S.; Nitoglia, E.; Oberling, J.; Oh, J. J.; Oh, S. H.; Oram, Richard J.; Ormiston, R. G.; Ormsby, N.; Osthelder, C.; Ottaway, D. J.; Overmier, H.; Pai, A.; Palamos, J. R.; Pannarale, F.; Parker, W.; Patane, O.; Patel, M.; Payne, E.; Pele, A.; Penhorwood, R.; Perez, C. J.; Phukon, K. S.; Pillas, M.; Pirello, M.; Radkins, H.; Ramirez, K. E.; Richardson, J. W.; Riles, K.; Rink, K.; Robertson, N. A.; Rollins, J. G.; Romel, C. L.; Romie, J. H.; Ross, M. P.; Ryan, K.; Sadecki, T.; Sakellariadou, M.; Sanchez, E. J.; Sanchez, L. E.; Sandles, L.; Saravanan, T. R.; Savage, R. L.; Schaetzl, D.; Schnabel, R.; Schwartz, E.; Sellers, D.; Shaffer, T.; Sigg, D.; Sintes, A. M.; Slagmolen, B. J. J.; Smith, J. R.; Soni, K.; Sorazu, B.; Spencer, A. P.; Strain, K. A.; Strom, D.; Sun, L.; Szczepańczyk, M. J.; Tasson, J.; Tenorio, R.; Thomas, M.; Thomas, P.; Thorne, K. A.; Toland, K.; Torrie, C. I.; Tran, A.; Traylor, G.; Trevor, M.; Tse, M.; Vajente, G.; Remortel, N. van; Vander-Hyde, D. C.; Vargas, A.; Veitch, J.; Veitch, P. J.; Venkateswara, K.; Venugopalan, G.; Viets, A. D.; Villa-Ortega, V.; Vo, T.; Vorvick, C.; Wade, M.; Wallace, G. S.; Ward, R. L.; Warner, J.; Weaver, B.; Weinstein, A. J.; Weiss, R.; Wette, K.; White, D. D.; White, L. V.; Whittle, C.; Williamson, A. R.; Willke, B.; Wipf, C. C.; Xiao, L.; Xu, R.; Yamamoto, H.; Yu, Hang; Yu, Haocun; Zhang, L.; Zheng, Y.; Zucker, M. E.; Zweizig, J.

doi:10.1088/1361-6382/abfd85

Published July 12, 2021 | Version Submitted

Journal Article Open

LIGO detector characterization in the second and third observing runs

1. Laser Interferometer Gravitational Wave Observatory
2. California State University, Fullerton
3. Stanford University
4. Christopher Newport University
5. University of Chicago
6. Pennsylvania State University
7. University of British Columbia
8. Missouri University of Science and Technology
9. Louisiana State University
10. University of Oregon
11. Embry–Riddle Aeronautical University
12. Massachusetts Institute of Technology
13. University of Portsmouth
14. Cardiff University
15. Columbia University
16. Max Planck Institute for Gravitational Physics
17. Villanova University
18. Syracuse University
19. University of Minnesota
20. Leibniz University Hannover
21. Stony Brook University
22. Sapienza University of Rome
23. INFN Sezione di Roma I
24. University of Tokyo
25. University of Melbourne
26. Indian Institute of Technology Bombay
27. University of Western Australia
28. Carleton College
29. University of Birmingham
30. University of the Balearic Islands
31. Bellevue College
32. Laboratoire de Physique des 2 Infinis Irène Joliot-Curie
33. University of Szeged
34. University of Glasgow
35. University of Santiago de Compostela
36. University of Mississippi
37. University of Florida
38. University of Michigan–Ann Arbor
39. Australian National University
40. University of Sheffield
41. Inter-University Centre for Astronomy and Astrophysics
42. University of Antwerp
43. Ulsan National Institute of Science and Technology
44. The University of Texas Rio Grande Valley
45. King's College London
46. National Institute for Mathematical Sciences
47. Southern University and Agricultural and Mechanical College
48. Monash University
49. National Institute for Subatomic Physics
50. University of Amsterdam
51. University of Washington
52. Universität Hamburg
53. University of Maryland, College Park
54. Concordia University Wisconsin
55. Kenyon College
56. University of Strathclyde

The characterization of the Advanced LIGO detectors in the second and third observing runs has increased the sensitivity of the instruments, allowing for a higher number of detectable gravitational-wave signals, and provided confirmation of all observed gravitational-wave events. In this work, we present the methods used to characterize the LIGO detectors and curate the publicly available datasets, including the LIGO strain data and data quality products. We describe the essential role of these datasets in LIGO–Virgo Collaboration analyses of gravitational-waves from both transient and persistent sources and include details on the provenance of these datasets in order to support analyses of LIGO data by the broader community. Finally, we explain anticipated changes in the role of detector characterization and current efforts to prepare for the high rate of gravitational-wave alerts and events in future observing runs.

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© 2021 IOP Publishing Ltd. Received 28 January 2021; Revised 31 March 2021; Accepted 30 April 2021; Published 3 June 2021. The authors would like to thank members of the Virgo and KAGRA detector characterization groups who have contributed to an environment of open collaboration that enabled this work. 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 PHY-1764464. Advanced LIGO was built under award PHY-0823459. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants PHY-0757058 and PHY-0823459. This work carries LIGO Document number P2000495. We would like to thank all of the essential workers who put their health at risk during the COVID-19 pandemic, without whom we would not have been able to complete this work. Data availability statement. The data that support the findings of this study are available upon reasonable request from the authors.

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Eprint ID: 108577
Resolver ID: CaltechAUTHORS:20210329-152811037

Describes: https://arxiv.org/abs/2101.11673 (URL)

Science and Technology Facilities Council (STFC)
Max-Planck-Society
Australian Research Council
NSF
PHY-1764464
NSF
PHY-0823459
NSF
PHY-0757058
NSF
PHY-0823459

Created: 2021-03-31

Created from EPrint's datestamp field
Updated: 2022-07-12

Created from EPrint's last_modified field

Caltech groups: LIGO , Physics Department
Other Numbering System Name: LIGO Document
Other Numbering System Identifier: P2000495

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LIGO detector characterization in the second and third observing runs

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