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Publisher Search for gravitational waves from binary black hole inspiral, merger, and ringdown

Research output: Contribution to journal › Article › Research

Authors

  • The LIGO Scientific Collaboration

Research Organisations

External Research Organisations

  • Max Planck Institute for Gravitational Physics (Albert Einstein Institute)

Details

Original languageUndefined/Unknown
JournalPhysical Review D
Volume85
Issue number12
Publication statusPublished - 2011

Abstract

We present the first modeled search for gravitational waves using the complete binary black hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched approximately 2 years of LIGO data taken between November 2005 and September 2007 for systems with component masses of 1-99 solar masses and total masses of 25-100 solar masses. We did not detect any plausible gravitational-wave signals but we do place upper limits on the merger rate of binary black holes as a function of the component masses in this range. We constrain the rate of mergers for binary black hole systems with component masses between 19 and 28 solar masses and negligible spin to be no more than 2.0 per Mpc per Myr at 90textpercent confidence.

Cite this

Publisher Search for gravitational waves from binary black hole inspiral, merger, and ringdown. / The LIGO Scientific Collaboration.
In: Physical Review D, Vol. 85, No. 12, 2011.

Research output: Contribution to journal › Article › Research

The LIGO Scientific Collaboration. Publisher Search for gravitational waves from binary black hole inspiral, merger, and ringdown. Physical Review D. 2011;85(12). doi: 10.1103/PhysRevD.83.122005; 10.1103/PhysRevD.85.089904
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title = "Publisher Search for gravitational waves from binary black hole inspiral, merger, and ringdown",
abstract = "We present the first modeled search for gravitational waves using the complete binary black hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched approximately 2 years of LIGO data taken between November 2005 and September 2007 for systems with component masses of 1-99 solar masses and total masses of 25-100 solar masses. We did not detect any plausible gravitational-wave signals but we do place upper limits on the merger rate of binary black holes as a function of the component masses in this range. We constrain the rate of mergers for binary black hole systems with component masses between 19 and 28 solar masses and negligible spin to be no more than 2.0 per Mpc per Myr at 90textpercent confidence.",
author = "{The LIGO Scientific Collaboration} and J. Abadie and Abbott, {B. P.} and R. Abbott and M. Abernathy and T. Accadia and F. Acernese and C. Adams and R. Adhikari and P. Ajith and B. Allen and Allen, {G. S.} and Ceron, {E. Amador} and Amin, {R. S.} and Anderson, {S. B.} and Anderson, {W. G.} and F. Antonucci and Arain, {M. A.} and Araya, {M. C.} and M. Aronsson and Y. Aso and Aston, {S. M.} and P. Astone and D. Atkinson and P. Aufmuth and C. Aulbert and S. Babak and P. Baker and G. Ballardin and T. Ballinger and Danilishin, {S. L.} and K. Danzmann and M. Hewitson and F. Kawazoe and H. L{\"u}ck and H. Vahlbruch and Alexander Wanner and B. Willke and K. Yamamoto and Z. Zhang",
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doi = "10.1103/PhysRevD.83.122005; 10.1103/PhysRevD.85.089904",
language = "Undefined/Unknown",
volume = "85",
journal = "Physical Review D",
issn = "0556-2821",
publisher = "American Institute of Physics",
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Download

TY - JOUR

T1 - Publisher Search for gravitational waves from binary black hole inspiral, merger, and ringdown

AU - The LIGO Scientific Collaboration

AU - Abadie, J.

AU - Abbott, B. P.

AU - Abbott, R.

AU - Abernathy, M.

AU - Accadia, T.

AU - Acernese, F.

AU - Adams, C.

AU - Adhikari, R.

AU - Ajith, P.

AU - Allen, B.

AU - Allen, G. S.

AU - Ceron, E. Amador

AU - Amin, R. S.

AU - Anderson, S. B.

AU - Anderson, W. G.

AU - Antonucci, F.

AU - Arain, M. A.

AU - Araya, M. C.

AU - Aronsson, M.

AU - Aso, Y.

AU - Aston, S. M.

AU - Astone, P.

AU - Atkinson, D.

AU - Aufmuth, P.

AU - Aulbert, C.

AU - Babak, S.

AU - Baker, P.

AU - Ballardin, G.

AU - Ballinger, T.

AU - Danilishin, S. L.

AU - Danzmann, K.

AU - Hewitson, M.

AU - Kawazoe, F.

AU - Lück, H.

AU - Vahlbruch, H.

AU - Wanner, Alexander

AU - Willke, B.

AU - Yamamoto, K.

AU - Zhang, Z.

PY - 2011

Y1 - 2011

N2 - We present the first modeled search for gravitational waves using the complete binary black hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched approximately 2 years of LIGO data taken between November 2005 and September 2007 for systems with component masses of 1-99 solar masses and total masses of 25-100 solar masses. We did not detect any plausible gravitational-wave signals but we do place upper limits on the merger rate of binary black holes as a function of the component masses in this range. We constrain the rate of mergers for binary black hole systems with component masses between 19 and 28 solar masses and negligible spin to be no more than 2.0 per Mpc per Myr at 90textpercent confidence.

AB - We present the first modeled search for gravitational waves using the complete binary black hole gravitational waveform from inspiral through the merger and ringdown for binaries with negligible component spin. We searched approximately 2 years of LIGO data taken between November 2005 and September 2007 for systems with component masses of 1-99 solar masses and total masses of 25-100 solar masses. We did not detect any plausible gravitational-wave signals but we do place upper limits on the merger rate of binary black holes as a function of the component masses in this range. We constrain the rate of mergers for binary black hole systems with component masses between 19 and 28 solar masses and negligible spin to be no more than 2.0 per Mpc per Myr at 90textpercent confidence.

U2 - 10.1103/PhysRevD.83.122005; 10.1103/PhysRevD.85.089904

DO - 10.1103/PhysRevD.83.122005; 10.1103/PhysRevD.85.089904

M3 - Article

VL - 85

JO - Physical Review D

JF - Physical Review D

SN - 0556-2821

IS - 12

ER -