Point absorbers in Advanced LIGO

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Authors

  • The LIGO Scientific Collaboration

Research Organisations

External Research Organisations

  • Max Planck Institute for Gravitational Physics (Albert Einstein Institute)
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Details

Original languageEnglish
Pages (from-to)4047-4063
Number of pages17
JournalApplied optics
Volume60
Issue number13
Early online date30 Apr 2021
Publication statusPublished - 1 May 2021

Abstract

Small, highly absorbing points are randomly present on the surfaces of the main interferometer optics in Advanced LIGO. The resulting nanometer scale thermo-elastic deformations and substrate lenses from these micronscale absorbers significantly reduce the sensitivity of the interferometer directly though a reduction in the power-recycling gain and indirect interactions with the feedback control system. We review the expected surface deformation from point absorbers and provide a pedagogical description of the impact on power buildup in second generation gravitational wave detectors (dual-recycled Fabry-Perot Michelson interferometers). This analysis predicts that the power-dependent reduction in interferometer performance will significantly degrade maximum stored power by up to 50 hence, limit GW sensitivity, but it suggests system wide corrections that can be implemented in current and future GW detectors. This is particularly pressing given that future GW detectors call for an order of magnitude more stored power than currently used in Advanced LIGO in Observing Run 3. We briefly review strategies to mitigate the effects of point absorbers in current and future GW wave detectors to maximize the success of these enterprises. (C) 2021 Optical Society of America

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Cite this

Point absorbers in Advanced LIGO. / The LIGO Scientific Collaboration.
In: Applied optics, Vol. 60, No. 13, 01.05.2021, p. 4047-4063.

Research output: Contribution to journal › Article › Research › peer review

The LIGO Scientific Collaboration 2021, 'Point absorbers in Advanced LIGO', Applied optics, vol. 60, no. 13, pp. 4047-4063. https://doi.org/10.48550/arXiv.2101.05828, https://doi.org/10.1364/AO.419689
The LIGO Scientific Collaboration. Point absorbers in Advanced LIGO. Applied optics. 2021 May 1;60(13):4047-4063. Epub 2021 Apr 30. doi: 10.48550/arXiv.2101.05828, 10.1364/AO.419689
The LIGO Scientific Collaboration. / Point absorbers in Advanced LIGO. In: Applied optics. 2021 ; Vol. 60, No. 13. pp. 4047-4063.
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@article{31dfe8fa9e63421fa6752436a3ccc3af,
title = "Point absorbers in Advanced LIGO",
abstract = "Small, highly absorbing points are randomly present on the surfaces of the main interferometer optics in Advanced LIGO. The resulting nanometer scale thermo-elastic deformations and substrate lenses from these micronscale absorbers significantly reduce the sensitivity of the interferometer directly though a reduction in the power-recycling gain and indirect interactions with the feedback control system. We review the expected surface deformation from point absorbers and provide a pedagogical description of the impact on power buildup in second generation gravitational wave detectors (dual-recycled Fabry-Perot Michelson interferometers). This analysis predicts that the power-dependent reduction in interferometer performance will significantly degrade maximum stored power by up to 50 hence, limit GW sensitivity, but it suggests system wide corrections that can be implemented in current and future GW detectors. This is particularly pressing given that future GW detectors call for an order of magnitude more stored power than currently used in Advanced LIGO in Observing Run 3. We briefly review strategies to mitigate the effects of point absorbers in current and future GW wave detectors to maximize the success of these enterprises. (C) 2021 Optical Society of America",
author = "{The LIGO Scientific Collaboration} and Brooks, {Aidan F.} and Gabriele Vajente and Hiro Yamamoto and Rich Abbott and Carl Adams and Adhikari, {Rana X.} and Alena Ananyeva and Stephen Appert and Koji Arai and Areeda, {Joseph S.} and Yasmeen Asali and Aston, {Stuart M.} and Corey Austin and Baer, {Anne M.} and Matthew Ball and Ballmer, {Stefan W.} and Sharan Banagiri and David Barker and Lisa Barsotti and Jeffrey Bartlett and Berger, {Beverly K.} and Joseph Betzwieser and Dripta Bhattacharjee and Garilynn Billingsley and Sebastien Biscans and Blair, {Carl D.} and Blair, {Ryan M.} and Nina Bode and Phillip Booker and Rolf Bork and Alyssa Bramley and Brown, {Daniel D.} and Aaron Buikema and Craig Cahillane and Cannon, {Kipp C.} and Cao, {Huy Tuong} and Xu Chen and Ciobanu, {Alexei A.} and Filiberto Clara and Camilla Compton and Cooper, {Sam J.} and Corley, {Kenneth R.} and Countryman, {Stefan T.} and Covas, {Pep B.} and Coyne, {Dennis C.} and Datrier, {Laurence E.} and Derek Davis and Difronzo, {Chiara D.} and Benno Willke",
note = "Funding Information: Acknowledgment. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and aLIGO 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 aLIGO. Additional support for aLIGO was provided by the Australian Research Council. The authors acknowledge the LIGO Scientific Collaboration Fellows program for additional support. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the NSF, and operates under cooperative agreement PHY-1764464. aLIGO was built under award PHY-0823459. This paper carries LIGO Document Number LIGO-P1900287.",
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Download

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T1 - Point absorbers in Advanced LIGO

AU - The LIGO Scientific Collaboration

AU - Brooks, Aidan F.

AU - Vajente, Gabriele

AU - Yamamoto, Hiro

AU - Abbott, Rich

AU - Adams, Carl

AU - Adhikari, Rana X.

AU - Ananyeva, Alena

AU - Appert, Stephen

AU - Arai, Koji

AU - Areeda, Joseph S.

AU - Asali, Yasmeen

AU - Aston, Stuart M.

AU - Austin, Corey

AU - Baer, Anne M.

AU - Ball, Matthew

AU - Ballmer, Stefan W.

AU - Banagiri, Sharan

AU - Barker, David

AU - Barsotti, Lisa

AU - Bartlett, Jeffrey

AU - Berger, Beverly K.

AU - Betzwieser, Joseph

AU - Bhattacharjee, Dripta

AU - Billingsley, Garilynn

AU - Biscans, Sebastien

AU - Blair, Carl D.

AU - Blair, Ryan M.

AU - Bode, Nina

AU - Booker, Phillip

AU - Bork, Rolf

AU - Bramley, Alyssa

AU - Brown, Daniel D.

AU - Buikema, Aaron

AU - Cahillane, Craig

AU - Cannon, Kipp C.

AU - Cao, Huy Tuong

AU - Chen, Xu

AU - Ciobanu, Alexei A.

AU - Clara, Filiberto

AU - Compton, Camilla

AU - Cooper, Sam J.

AU - Corley, Kenneth R.

AU - Countryman, Stefan T.

AU - Covas, Pep B.

AU - Coyne, Dennis C.

AU - Datrier, Laurence E.

AU - Davis, Derek

AU - Difronzo, Chiara D.

AU - Willke, Benno

N1 - Funding Information: Acknowledgment. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and aLIGO 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 aLIGO. Additional support for aLIGO was provided by the Australian Research Council. The authors acknowledge the LIGO Scientific Collaboration Fellows program for additional support. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the NSF, and operates under cooperative agreement PHY-1764464. aLIGO was built under award PHY-0823459. This paper carries LIGO Document Number LIGO-P1900287.

PY - 2021/5/1

Y1 - 2021/5/1

N2 - Small, highly absorbing points are randomly present on the surfaces of the main interferometer optics in Advanced LIGO. The resulting nanometer scale thermo-elastic deformations and substrate lenses from these micronscale absorbers significantly reduce the sensitivity of the interferometer directly though a reduction in the power-recycling gain and indirect interactions with the feedback control system. We review the expected surface deformation from point absorbers and provide a pedagogical description of the impact on power buildup in second generation gravitational wave detectors (dual-recycled Fabry-Perot Michelson interferometers). This analysis predicts that the power-dependent reduction in interferometer performance will significantly degrade maximum stored power by up to 50 hence, limit GW sensitivity, but it suggests system wide corrections that can be implemented in current and future GW detectors. This is particularly pressing given that future GW detectors call for an order of magnitude more stored power than currently used in Advanced LIGO in Observing Run 3. We briefly review strategies to mitigate the effects of point absorbers in current and future GW wave detectors to maximize the success of these enterprises. (C) 2021 Optical Society of America

AB - Small, highly absorbing points are randomly present on the surfaces of the main interferometer optics in Advanced LIGO. The resulting nanometer scale thermo-elastic deformations and substrate lenses from these micronscale absorbers significantly reduce the sensitivity of the interferometer directly though a reduction in the power-recycling gain and indirect interactions with the feedback control system. We review the expected surface deformation from point absorbers and provide a pedagogical description of the impact on power buildup in second generation gravitational wave detectors (dual-recycled Fabry-Perot Michelson interferometers). This analysis predicts that the power-dependent reduction in interferometer performance will significantly degrade maximum stored power by up to 50 hence, limit GW sensitivity, but it suggests system wide corrections that can be implemented in current and future GW detectors. This is particularly pressing given that future GW detectors call for an order of magnitude more stored power than currently used in Advanced LIGO in Observing Run 3. We briefly review strategies to mitigate the effects of point absorbers in current and future GW wave detectors to maximize the success of these enterprises. (C) 2021 Optical Society of America

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U2 - 10.48550/arXiv.2101.05828

DO - 10.48550/arXiv.2101.05828

M3 - Article

VL - 60

SP - 4047

EP - 4063

JO - Applied optics

JF - Applied optics

SN - 1559-128X

IS - 13

ER -