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Sensitivity and performance of the Advanced LIGO detectors in the third observing run

Physical review. D/Physical review. D. · 2020 · Vol. 102(6)

A. Buikema✉(LIGO Scientific Collaboration)C. Cahillane(California Institute of Technology)G. L. Mansell(Massachusetts Institute of Technology)C. D. Blair(The University of Western Australia)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)Corey Austin(Louisiana State University)A. M. Baer(Christopher Newport University)M. Ball(University of Oregon)S. W. Ballmer(Syracuse University)S. Banagiri(University of Minnesota)D. BarkerL. Barsotti(Massachusetts Institute of Technology)J. BartlettB. 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)D. G. BlairN. 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. D. Brown(ARC Centre of Excellence for Gravitational Wave Discovery)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. ClaraS. 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)Jennifer C DriggersP. Dupej(University of Glasgow)S. E. DwyerA. Effler(LIGO Scientific Collaboration)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)V. V. Frolov(LIGO Scientific Collaboration)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(Louisiana State University)S. Gras(Massachusetts Institute of Technology)C. GrayR. Gray(University of Glasgow)A. C. Green(University of Florida)E. K. Gustafson(California Institute of Technology)R. Gustafson(University of Michigan)J. HanksJ. Hanson(LIGO Scientific Collaboration)T. Hardwick(Louisiana State University)R. K. Hasskew(LIGO Scientific Collaboration)M. C. Heintze(LIGO Scientific Collaboration)A. F. Helmling-Cornell(University of Oregon)N. A. Holland(Australian National University)J. D. JonesS. Kandhasamy(Inter-University Centre for Astronomy and Astrophysics)S. Karki(University of Oregon)M. Kasprzack(California Institute of Technology)K. KawabeN. Kijbunchoo(Australian National University)P. J. KingJ. S. KisselR. KumarM. LandryB. B. Lane(Massachusetts Institute of Technology)B. Lantz(Stanford University)M. Laxen(LIGO Scientific Collaboration)Y. K. LecoeucheJ. Leviton(University of Michigan)J. Liu(Leibniz University Hannover)M. Lormand(LIGO Scientific Collaboration)A. P. Lundgren(University of Portsmouth)R. Macas(Cardiff University)M. MacInnis(Massachusetts Institute of Technology)D. M. Macleod(Cardiff University)Szabolcs Márka(Columbia University)Z. Márka(Columbia University)Д. В. Мартынов(University of Birmingham)K. Mason(Massachusetts Institute of Technology)T. J. Massinger(Massachusetts Institute of Technology)F. Matichard(California Institute of Technology)N. Mavalvala(Massachusetts Institute of Technology)R. McCarthyD. E. McClelland(Australian National University)S. McCormick(LIGO Scientific Collaboration)L. McCuller(Massachusetts Institute of Technology)J. McIver(California Institute of Technology)T. McRae(Australian National University)G. MendellK. Merfeld(University of Oregon)E. L. MerilhF. Meylahn(Leibniz University Hannover)T. Mistry(University of Sheffield)R. Mittleman(Massachusetts Institute of Technology)G. MorenoC. M. Mow‐Lowry(University of Birmingham)S. Mozzon(University of Portsmouth)A. Mullavey(LIGO Scientific Collaboration)T. J. N. Nelson(LIGO Scientific Collaboration)P. Nguyen(University of Oregon)L. K. Nuttall(University of Portsmouth)J. OberlingRichard J. Oram(LIGO Scientific Collaboration)B. O’Reilly(LIGO Scientific Collaboration)C. Osthelder(California Institute of Technology)D. J. Ottaway(ARC Centre of Excellence for Gravitational Wave Discovery)H. Overmier(LIGO Scientific Collaboration)J. R. Palamos(University of Oregon)W. Parker(Southern University and Agricultural and Mechanical College)Ethan Payne(ARC Centre of Excellence for Gravitational Wave Discovery)A. Pele(LIGO Scientific Collaboration)R. Penhorwood(University of Michigan)C. J. PerezM. PirelloH. RadkinsK. E. Ramirez(The University of Texas Rio Grande Valley)J. W. Richardson(California Institute of Technology)K. Riles(University of Michigan)N. A. Robertson(California Institute of Technology)J. G. Rollins(California Institute of Technology)C. L. RomelJ. H. Romie(LIGO Scientific Collaboration)M. P. Ross(University of Washington)K. RyanT. SadeckiE. J. Sanchez(California Institute of Technology)L. E. Sanchez(California Institute of Technology)T. R. Saravanan(Inter-University Centre for Astronomy and Astrophysics)R. L. SavageD. Schaetzl(California Institute of Technology)Roman Schnabel(Universität Hamburg)R. M. S. Schofield(University of Oregon)E. Schwartz(LIGO Scientific Collaboration)D. Sellers(LIGO Scientific Collaboration)T. ShafferD. SiggB. J. J. Slagmolen(Australian National University)J. R. Smith(California State University, Fullerton)K. Soni(Louisiana State University)B. Sorazu(University of Glasgow)A. P. Spencer(University of Glasgow)K. A. Strain(University of Glasgow)L. Sun(California Institute of Technology)M. J. Szczepańczyk(University of Florida)M. Thomas(LIGO Scientific Collaboration)P. ThomasK. Thorne(LIGO Scientific Collaboration)K. Toland(University of Glasgow)C. I. Torrie(California Institute of Technology)G. Traylor(LIGO Scientific Collaboration)M. Tse(Massachusetts Institute of Technology)A. L. Urban(Louisiana State University)G. Vajente(California Institute of Technology)G. Valdés(Louisiana State University)Daniel Vander-Hyde(Syracuse University)P. J. Veitch(ARC Centre of Excellence for Gravitational Wave Discovery)K. Venkateswara(University of Washington)G. Venugopalan(California Institute of Technology)A. D. Viets(Concordia University Wisconsin)T. Vo(Syracuse University)C. VorvickM. Wade(Kenyon College)R. L. Ward(Australian National University)J. WarnerB. WeaverR. Weiss(Massachusetts Institute of Technology)C. Whittle(Massachusetts Institute of Technology)B. Willke(Leibniz University Hannover)C. C. Wipf(California Institute of Technology)S. Xiao(California Institute of Technology)H. Yamamoto(California Institute of Technology)Hang Yu(Massachusetts Institute of Technology)Haocun Yu(Massachusetts Institute of Technology)L. Zhang(California Institute of Technology)M. E. Zucker(California Institute of Technology)J. Zweizig(California Institute of Technology)

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Abstract

On April 1st, 2019, the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), joined by the Advanced Virgo detector, began the third observing run, a year-long dedicated search for gravitational radiation. The LIGO detectors have achieved a higher duty cycle and greater sensitivity to gravitational waves than ever before, with LIGO Hanford achieving angle-averaged sensitivity to binary neutron star coalescences to a distance of 111 Mpc, and LIGO Livingston to 134 Mpc with duty factors of 74.6% and 77.0% respectively. The improvement in sensitivity and stability is a result of several upgrades to the detectors, including doubled intracavity power, the addition of an in-vacuum optical parametric oscillator for squeezed-light injection, replacement of core optics and end reaction masses, and installation of acoustic mode dampers. This paper explores the purposes behind these upgrades, and explains to the best of our knowledge the noise currently limiting the sensitivity of each detector.

Pulsars and Gravitational Waves Research Geophysics and Sensor Technology Seismic Waves and AnalysisLIGOGravitational wavePhysicsDetectorGravitational-wave observatorySensitivity (control systems)ObservatoryInterferometryOpticsDuty cycle