Advanced LIGO
- Creators
- Aasi, J.
- Abbott, B. P.
- Abbott, R.
- Abernathy, M. R.
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Adhikari, R. X.
- Anderson, S. B.
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Arai, K.
- Araya, M. C.
- Barayoga, J. C.
- Barish, B. C.
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Billingsley, G.
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Blackburn, J. K.
- Bork, R.
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Brooks, A. F.
- Cepeda, C.
- Chakraborty, R.
- Chalermsongsak, T.
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Coyne, D. C.
- Dergachev, V.
- Driggers, J. C.
- Ehrens, P.
- Etzel, T.
- Gushwa, K.
- Gustafson, E. K.
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Hall, E. D.
- Heptonstall, A. W.
- Hodge, K. A.
- Jacobson, M.
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Kanner, J. B.
- Kells, W.
- Kondrashov, V.
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Korth, W. Z.
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Kozak, D. B.
- Lazzarini, A.
- Lewis, J.
- Li, T. G. F.
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Libbrecht, K.
- Mageswaran, M.
- Mailand, K.
- Maros, E.
- Martynov, D.
- Marx, J. N.
- McIntyre, G.
- Meshkov, S.
- Nash, T.
- Osthelder, C.
- Pedraza, M.
- Phelps, M.
- Price, L. R.
- Privitera, S.
- Quintero, E.
- Raymond, V.
- Reitze, D. H.
- Robertson, N. A.
- Rollins, J. G.
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Sachdev, S.
- Sannibale, V.
- Schmidt, P.
- Shao, Z.
- Singer, A.
- Singer, L.
- Smith, M. R.
- Smith, R. J. E.
- Smith-Lefebvre, N. D.
- Taylor, R.
- Thirugnanasambandam, M. P.
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Thrane, E.
- Torrie, C. I.
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Vajente, G.
- Vass, S.
- Wallace, L.
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Weinstein, A. J.
- Whitcomb, S. E.
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Williams, R.
- Yamamoto, H.
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Zhang, L.
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Zweizig, J.
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Chen, Y.
- Cutler, C.
- Gossan, S.
- Nissanke, S.
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Ott, C. D.
- Thorne, K. S.
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Vallisneri, M.
- LIGO Scientific Collaboration
Abstract
The Advanced LIGO gravitational wave detectors are second-generation instruments designed and built for the two LIGO observatories in Hanford, WA and Livingston, LA, USA. The two instruments are identical in design, and are specialized versions of a Michelson interferometer with 4 km long arms. As in Initial LIGO, Fabry–Perot cavities are used in the arms to increase the interaction time with a gravitational wave, and power recycling is used to increase the effective laser power. Signal recycling has been added in Advanced LIGO to improve the frequency response. In the most sensitive frequency region around 100 Hz, the design strain sensitivity is a factor of 10 better than Initial LIGO. In addition, the low frequency end of the sensitivity band is moved from 40 Hz down to 10 Hz. All interferometer components have been replaced with improved technologies to achieve this sensitivity gain. Much better seismic isolation and test mass suspensions are responsible for the gains at lower frequencies. Higher laser power, larger test masses and improved mirror coatings lead to the improved sensitivity at mid and high frequencies. Data collecting runs with these new instruments are planned to begin in mid-2015.
Additional Information
© 2015 IOP Publishing Ltd. Received 11 November 2014, revised 12 December 2014. Accepted for publication 30 December 2014. Published 3 March 2015. The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities Council of the United Kingdom, the Max-Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the International Science Linkages programme of the Commonwealth of Australia, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de EconomÃa y Competitividad, the Conselleria d'Economia, Hisenda i Innovació of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, OTKA of Hungary, the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the National Science and Engineering Research Council Canada, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, and the Alfred P. Sloan Foundation. This article has LIGO document number LIGO-P1400177.Additional details
- Eprint ID
- 56746
- Resolver ID
- CaltechAUTHORS:20150417-133457450
- NSF
- Science and Technology Facilities Council (STFC)
- Max-Planck-Society
- Australian Research Council
- International Science Linkages programme of the Commonwealth of Australia
- Council of Scientific and Industrial Research (India)
- Istituto Nazionale di Fisica Nucleare (INFN)
- Ministerio de EconomÃa y Competitividad (MINECO)
- Conselleria d'Economia Hisenda i Innovaciό of the Govern de les Illes Balears
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- NASA
- Hungarian Scientific Research Fund (OTKA)
- National Research Foundation of Korea
- Industry Canada
- Natural Sciences and Engineering Research Council of Canada (NSERC)
- Carnegie Trust
- Leverhulme Trust
- David and Lucile Packard Foundation
- Research Corporation
- Alfred P. Sloan Foundation
- State of Niedersachsen/Germany
- Ontario Ministry of Research and Innovation
- Created
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2015-04-17Created from EPrint's datestamp field
- Updated
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2022-07-12Created from EPrint's last_modified field
- Caltech groups
- LIGO, TAPIR
- Other Numbering System Name
- LIGO Document
- Other Numbering System Identifier
- LIGO-P1400177