Template banks to search for compact binaries with spinning components in gravitational wave data

Chris Van Den Broeck, Duncan A. Brown, Thomas Cokelaer, Ian Harry, Gareth Jones, B. S. Sathyaprakash, Hideyuki Tagoshi, and Hirotaka Takahashi
Phys. Rev. D 80, 024009 – Published 10 July 2009

Abstract

Gravitational waves from coalescing compact binaries are one of the most promising sources for detectors such as LIGO, Virgo, and GEO600. If the components of the binary possess significant angular momentum (spin), as is likely to be the case if one component is a black hole, spin-induced precession of a binary’s orbital plane causes modulation of the gravitational-wave amplitude and phase. If the templates used in a matched-filter search do not accurately model these effects then the sensitivity, and hence the detection rate, will be reduced. We investigate the ability of several search pipelines to detect gravitational waves from compact binaries with spin. We use the post-Newtonian approximation to model the inspiral phase of the signal and construct two new template banks using the phenomenological waveforms of Buonanno, Chen, and Vallisneri [A. Buonanno, Y. Chen, and M. Vallisneri, Phys. Rev. D 67, 104025 (2003)]. We compare the performance of these template banks to that of banks constructed using the stationary phase approximation to the nonspinning post-Newtonian inspiral waveform currently used by LIGO and Virgo in the search for compact binary coalescence. We find that, at the same false alarm rate, a search pipeline using phenomenological templates is no more effective than a pipeline which uses nonspinning templates. We recommend the continued use of the nonspinning stationary phase template bank until the false alarm rate associated with templates which include spin effects can be substantially reduced.

  • Figure
  • Received 10 April 2009

DOI:https://doi.org/10.1103/PhysRevD.80.024009

©2009 American Physical Society

Authors & Affiliations

Chris Van Den Broeck1,*, Duncan A. Brown2,†, Thomas Cokelaer1,‡, Ian Harry1,§, Gareth Jones1,∥, B. S. Sathyaprakash1,¶, Hideyuki Tagoshi3,**, and Hirotaka Takahashi4,††

  • 1School of Physics and Astronomy, Cardiff University, 5 The Parade, Cardiff, CF24 3YB, United Kingdom
  • 2Department of Physics, Syracuse University, Syracuse, New York 13244, USA
  • 3Department of Earth and Space Science, Graduate School of Science, Osaka University, Toyonaka 560-0043, Japan
  • 4Department of Management and Information Systems Science, Nagaoka University of Technology, Nagaoka, Niigata 940-2188, Japan

  • *Chris.van-den-Broeck@astro.cf.ac.uk
  • dabrown@phys.syr.edu
  • Thomas.Cokelaer@astro.cf.ac.uk, Thomas.Cokelaer@inria.fr
  • §Ian.Harry@astro.cf.ac.uk
  • Gareth.Jones@astro.cf.ac.uk
  • B.Sathyaprakash@astro.cf.ac.uk
  • **tagoshi@vega.ess.sci.osaka-u.ac.jp
  • ††hirotaka@oberon.nagaokaut.ac.jp

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Vol. 80, Iss. 2 — 15 July 2009

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