Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy
Name
PhysRevD.93.112004.pdf
Size
2.97 MB
Format
Adobe PDF
Checksum (MD5)
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Author(s)
Martynov, D. V.
Hall, E. D.
Abbott, B. P.
Abbott, R.
Abbott, T. D.
Adams, C.
Adhikari, R. X.
Anderson, R. A.
Anderson, S. B.
Arai, K.
Date Issued
June 2016
Journal
Physical Review D
Publisher
American Physical Society
Citation
Martynov, D. V.; Hall, E. D.; Abbott, B. P. et al. "Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy." Physical Review D 93, 11 (June 2016): 112004 © 2016 American Physical Society
Version
Final published version
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[subscript ⊙] 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.
MIT Department
Massachusetts Institute of Technology. Department of Physics
LIGO (Observatory : Massachusetts Institute of Technology)
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1103/PhysRevD.93.112004
