TY - JOUR

T1 - Sensitivity of the Advanced LIGO detectors at the beginning of gravitational wave astronomy

AU - The LIGO Scientific Collaboration

AU - Collaboration, The LIGO Scientific

AU - Martynov, D. V.

AU - Hall, E. D.

AU - Abbott, B. P.

AU - Abbott, R.

AU - Abbott, T. D.

AU - Abernathy, M. R.

AU - Ackley, K.

AU - Adams, C.

AU - Addesso, P.

AU - Adhikari, R. X.

AU - Adya, V. B.

AU - Allen, B.

AU - Danilishin, S. L.

AU - Danzmann, K.

AU - Heurs, M.

AU - Luck, H.

AU - Shaltev, M.

AU - Steinmeyer, D.

AU - Vahlbruch, H.

AU - Willke, B.

AU - Wittel, H.

N1 - Funding information: 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.

PY - 2016/6/2

Y1 - 2016/6/2

N2 - 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 0textasciicircum23sqrttextbracelefttexttextbraceleftHztextbracerighttextbraceright00 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 textdollarMtextunderscoreodot.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.

AB - 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 0textasciicircum23sqrttextbracelefttexttextbraceleftHztextbracerighttextbraceright00 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 textdollarMtextunderscoreodot.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.

UR - http://www.scopus.com/inward/record.url?scp=84974849312&partnerID=8YFLogxK

U2 - 10.1103/PhysRevD.93.112004

DO - 10.1103/PhysRevD.93.112004

M3 - Article

VL - 93

JO - Physical Review D

JF - Physical Review D

SN - 0556-2821

IS - 11

M1 - 112004

ER -