Aasi, J. and Abbott, B. P. and Abbott, R. and Abernathy, M. R. and Adhikari, R. X. and Anderson, S. B. and Arai, K. and Araya, M. C. and Barayoga, J. C. and Barish, B. C. and Billingsley, G. and Blackburn, J. K. and Bork, R. and Brooks, A. F. and Cepeda, C. and Chakraborty, R. and Chalermsongsak, T. and Coyne, D. C. and Dergachev, V. and Driggers, J. C. and Ehrens, P. and Etzel, T. and Gushwa, K. and Gustafson, E. K. and Hall, E. D. and Heptonstall, A. W. and Hodge, K. A. and Jacobson, M. and Kanner, J. B. and Kells, W. and Kondrashov, V. and Korth, W. Z. and Kozak, D. B. and Lazzarini, A. and Lewis, J. and Li, T. G. F. and Libbrecht, K. and Mageswaran, M. and Mailand, K. and Maros, E. and Martynov, D. and Marx, J. N. and McIntyre, G. and Meshkov, S. and Nash, T. and Osthelder, C. and Pedraza, M. and Phelps, M. and Price, L. R. and Privitera, S. and Quintero, E. and Raymond, V. and Reitze, D. H. and Robertson, N. A. and Rollins, J. G. and Sachdev, S. and Sannibale, V. and Schmidt, P. and Shao, Z. and Singer, A. and Singer, L. and Smith, M. R. and Smith, R. J. E. and Smith-Lefebvre, N. D. and Taylor, R. and Thirugnanasambandam, M. P. and Thrane, E. and Torrie, C. I. and Vajente, G. and Vass, S. and Wallace, L. and Weinstein, A. J. and Whitcomb, S. E. and Williams, R. and Yamamoto, H. and Zhang, L. and Zweizig, J. and Chen, Y. and Cutler, C. and Gossan, S. and Nissanke, S. and Ott, C. D. and Thorne, K. S. and Vallisneri, M. (2015) Advanced LIGO. Classical and Quantum Gravity, 32 (7). Art. No. 074001. ISSN 0264-9381. doi:10.1088/0264-9381/32/7/074001. https://resolver.caltech.edu/CaltechAUTHORS:20150417-133457450
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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.
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| 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 Economía 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. | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | LIGO, TAPIR | ||||||||||||||||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | gravitational waves, interferometers, seismic isolation, optics | ||||||||||||||||||||||||||||||||||||||||||||||||||
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| Issue or Number: | 7 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Classification Code: | PACS: 04.80.Nn, 95.55.Ym, 07.60.Ly. MSC: 83C35 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1088/0264-9381/32/7/074001 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20150417-133457450 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20150417-133457450 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Official Citation: | Advanced LIGO The LIGO Scientific Collaboration et al 2015 Class. Quantum Grav. 32 074001 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 56746 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | Ruth Sustaita | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 17 Apr 2015 22:32 | ||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 12 Jul 2022 19:49 |
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