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The Sensitivity of the Advanced LIGO Detectors at the Beginning of Gravitational Wave Astronomy

The LIGO Scientific Collaboration, Martynov, D. V., Hall, E. D., Abbott, B. P., Abbott, R., Abbott, T. D., et al. (2016). The Sensitivity of the Advanced LIGO Detectors at the Beginning of Gravitational Wave Astronomy. Physical Review D, 93: 112004. doi:10.1103/PhysRevD.93.112004.

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1604.00439.pdf (Preprint), 5MB
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### Creators

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Creators:
The LIGO Scientific Collaboration, Author
Martynov, D. V., Author
Hall, E. D., Author
Abbott, B. P., Author
Abbott, R., Author
Abbott, T. D., Author
Abernathy, M. R., Author
Ackley, K., Author
Affeldt, C.1, Author
Aggarwal, N., Author
Aguiar, O. D., Author
Ain, A., Author
Ajith, P., Author
Allen, B.2, Author
Altin, P. A., Author
Anderson, R. A., Author
Affiliations:
1Laser Interferometry & Gravitational Wave Astronomy, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24010
2Observational Relativity and Cosmology, AEI-Hannover, MPI for Gravitational Physics, Max Planck Society, ou_24011
3Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290
4Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013

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Free keywords: Astrophysics, Instrumentation and Methods for Astrophysics, astro-ph.IM, Physics, Instrumentation and Detectors, physics.ins-det
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 $10^{-23}/\sqrt{\text{Hz}}$ was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the observable volume in the universe. The average distance at which coalescing binary black hole systems with individual masses of 30 $M_\odot$ could be detected was 1.3 Gpc. Similarly, the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of Universe increased respectively by a factor 69 and 43. These improvements allowed Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.

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Dates: 2016-04-012016
Publication Status: Published in print
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### Source 1

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Title: Physical Review D
Other : Phys. Rev. D.
Source Genre: Journal
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Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 93 Sequence Number: 112004 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258