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1826206988407668736
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MIT
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© 2020 authors. Published by the American Physical Society. 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.
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2024-09-23T13:42:04Z
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Article
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mit-1721.1/133376
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Massachusetts Institute of Technology
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| language |
English
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2024-09-23T13:42:04Z
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| publishDate |
2021
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| publisher |
American Physical Society (APS)
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dspace
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| spelling |
mit-1721.1/1333762022-09-28T15:38:24Z Sensitivity and performance of the Advanced LIGO detectors in the third observing run © 2020 authors. Published by the American Physical Society. 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. 2021-10-27T19:52:26Z 2021-10-27T19:52:26Z 2020 2021-07-09T15:43:37Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/133376 en 10.1103/PHYSREVD.102.062003 Physical Review D Creative Commons Attribution 4.0 International license https://creativecommons.org/licenses/by/4.0/ application/pdf American Physical Society (APS) APS
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| spellingShingle |
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
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| title |
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
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| title_full |
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
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| title_fullStr |
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
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| title_full_unstemmed |
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
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| title_short |
Sensitivity and performance of the Advanced LIGO detectors in the third observing run
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| title_sort |
sensitivity and performance of the advanced ligo detectors in the third observing run
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| url |
https://hdl.handle.net/1721.1/133376
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