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Template banks for binary black hole searches with numerical relativity waveforms

Prayush Kumar1,*, Ilana MacDonald2,3, Duncan A. Brown1,4, Harald P. Pfeiffer2,5, Kipp Cannon2, Michael Boyle6, Lawrence E. Kidder6, Abdul H. Mroué2, Mark A. Scheel7 et al.

Béla Szilágyi7 and Anıl Zenginoğlu7

  • 1Department of Physics, Syracuse University, Syracuse, New York 13244, USA
  • 2Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, Ontario M5S 3H8, Canada
  • 3Department of Astronomy and Astrophysics, University of Toronto, Toronto, Ontario M5S 3H4, Canada
  • 4LIGO Laboratory, California Institute of Technology, Pasadena, California 91125, USA
  • 5Canadian Institute for Advanced Research, 180 Dundas St. West, Toronto, Ontario M5G 1Z8, Canada
  • 6Center for Radiophysics and Space Research, Cornell University, Ithaca, New York 14853, USA
  • 7Theoretical Astrophysics 350-17, California Institute of Technology, Pasadena, California 91125, USA

  • *prayush.kumar@ligo.org
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Phys. Rev. D 89, 042002 – Published 18 February, 2014

DOI: https://doi.org/10.1103/PhysRevD.89.042002

Abstract

Gravitational waves from coalescing stellar-mass black hole binaries (BBHs) are expected to be detected by the Advanced Laser Interferometer gravitational-wave observatory and Advanced Virgo. Detection searches operate by matched filtering the detector data using a bank of waveform templates. Traditionally, template banks for BBHs are constructed from intermediary analytical waveform models which are calibrated against numerical relativity simulations and which can be evaluated for any choice of BBH parameters. This paper explores an alternative to the traditional approach, namely, the construction of template banks directly from numerical BBH simulations. Using nonspinning BBH systems as an example, we demonstrate which regions of the mass-parameter plane can be covered with existing numerical BBH waveforms. We estimate the required number and required length of BBH simulations to cover the entire nonspinning BBH parameter plane up to mass ratio 10, thus illustrating that our approach can be used to guide parameter placement of future numerical simulations. We derive error bounds which are independent of analytical waveform models; therefore, our formalism can be used to independently test the accuracy of such waveform models. The resulting template banks are suitable for advanced LIGO searches.

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Phys. Rev. D 89, 042002– Published 18 February, 2014
  • Received 13 November 2013

© 2014 American Physical Society

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