Martynov, D. V. and Hall, E. D. and Abbott, B. P. and Abbott, R. and Adhikari, R. X. and Anderson, R. A. and Anderson, S. B. and Arai, K. and Austin, L. and Billingsley, G. and Black, E. and Bork, R. and Brooks, A. F. and Coyne, D. C. and Dannenberg, R. and Etzel, T. and Gushwa, E. and Gustafson, E. K. and Heefner, J. and Heptonstall, A. W. and Ivanov, A. and Jacobson, M. and James, E. and Kells, W. and Korth, W. Z. and Lewis, J. B. and Mageswaran, M. and Mailand, K. and Maros, E. and Marx, J. N. and McIntyre, G. and McIver, J. and Osthelder, C. and Quintero, E. A. and Reitze, D. H. and Rollins, J. G. and Sanchez, E. J. and Sannibale, V. and Shao, Z. and Smith, M. R. and Smith-Lefebvre, N. D. and Stochino, A. and Taylor, R. and Torrie, C. I. and Vajente, G. and Willems, P. A. and Wipf, C. C. and Yamamoto, H. and Zhang, L. and Zucker, M. E. and Zweizig, J. (2016) Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy. Physical Review D, 93 (11). Art. No. 112004. ISSN 2470-0010. doi:10.1103/PhysRevD.93.112004. https://resolver.caltech.edu/CaltechAUTHORS:20160608-105846398
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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.
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| 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 Economía 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. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Group: | LIGO | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Issue or Number: | 11 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1103/PhysRevD.93.112004 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20160608-105846398 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20160608-105846398 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Official Citation: | Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy D. V. Martynov et al. Phys. Rev. D 93, 112004 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 67776 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | Tony Diaz | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 08 Jun 2016 18:45 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 11 Nov 2021 03:54 |
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