Published June 1, 2016
| Submitted + Published
Journal Article
Open
Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy
- Creators
- Martynov, D. V.
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Hall, E. D.
- Abbott, B. P.
- Abbott, R.
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Adhikari, R. X.
- Anderson, R. A.
- Anderson, S. B.
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Arai, K.
- Austin, L.
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Billingsley, G.
- Black, E.
- Bork, R.
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Brooks, A. F.
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Coyne, D. C.
- Dannenberg, R.
- Etzel, T.
- Gushwa, E.
- Gustafson, E. K.
- Heefner, J.
- Heptonstall, A. W.
- Ivanov, A.
- Jacobson, M.
- James, E.
- Kells, W.
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Korth, W. Z.
- Lewis, J. B.
- Mageswaran, M.
- Mailand, K.
- Maros, E.
- Marx, J. N.
- McIntyre, G.
- McIver, J.
- Osthelder, C.
- Quintero, E. A.
- Reitze, D. H.
- Rollins, J. G.
- Sanchez, E. J.
- Sannibale, V.
- Shao, Z.
- Smith, M. R.
- Smith-Lefebvre, N. D.
- Stochino, A.
- Taylor, R.
- Torrie, C. I.
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Vajente, G.
- Willems, P. A.
- Wipf, C. C.
- Yamamoto, H.
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Zhang, L.
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Zucker, M. E.
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Zweizig, J.
Chicago
An error occurred while generating the citation.
Abstract
The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10^(−23)/√Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M⊙ could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.
Additional Information
© 2016 American Physical Society. Received 5 April 2016; published 2 June 2016. The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Foundation for Fundamental Research on Matter supported by the Netherlands Organisation for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, Department of Science and Technology, India, Science & Engineering Research Board (SERB), India, Ministry of Human Resource Development, India, the Spanish Ministerio de EconomÃa y Competitividad, the Conselleria d'Economia i Competitivitat and Conselleria d'Educació, Cultura i Universitats of the Govern de les Illes Balears, the National Science Centre of Poland, the European Commission, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the Lyon Institute of Origins (LIO), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, and Innovation, Russian Foundation for Basic Research, the Leverhulme Trust, the Research Corporation, Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authors gratefully acknowledge the support of the NSF, STFC, MPS, INFN, CNRS and the State of Niedersachsen/Germany for provision of computational resources.Attached Files
Published - PhysRevD.93.112004.pdf
Submitted - 1604.00439v1.pdf
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Additional details
- Eprint ID
- 67776
- Resolver ID
- CaltechAUTHORS:20160608-105846398
- NSF
- Science and Technology Facilities Council (STFC)
- Max-Planck-Society
- State of Niedersachsen/Germany
- Australian Research Council
- Istituto Nazionale di Fisica Nucleare (INFN)
- Centre National de la Recherche Scientifique (CNRS)
- Stichting voor Fundamenteel Onderzoek der Materie (FOM)
- Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)
- Council of Scientific and Industrial Research (India)
- Department of Science and Technology (India)
- Science and Engineering Research Board (SERB)
- Ministry of Human Resource Development (India)
- Ministerio de EconomÃa y Competitividad (MINECO)
- Conselleria d'Economia i Competitivitat
- Conselleria d'Educació, Cultura i Universitats
- National Science Centre (Poland)
- European Commission
- Royal Society
- Scottish Funding Council
- Scottish Universities Physics Alliance
- Hungarian Scientific Research Fund (OTKA)
- Lyon Institute of Origins (LIO)
- National Research Foundation of Korea
- Industry Canada
- Ontario Ministry of Economic Development and Innovation
- Natural Science and Engineering Research Council of Canada (NSERC)
- Canadian Institute for Advanced Research (CIFAR)
- Ministério da Ciência, Tecnologia e Inovação
- Russian Foundation for Basic Research
- Leverhulme Trust
- Research Corporation
- Ministry of Science and Technology (Taipei)
- Kavli Foundation
- Created
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2016-06-08Created from EPrint's datestamp field
- Updated
-
2021-11-11Created from EPrint's last_modified field
- Caltech groups
- LIGO