Detecting gravitational waves from precessing binaries of spinning compact objects: Adiabatic limit
Abstract
Black-hole (BH) binaries with single-BH masses m=(5-20)M, moving on quasicircular orbits, are among the most promising sources for first-generation ground-based gravitational-wave (GW) detectors. Until now, the development of data-analysis techniques to detect GWs from these sources has been focused mostly on nonspinning BHs. The data-analysis problem for the spinning case is complicated by the necessity to model the precession-induced modulations of the GW signal, and by the large number of parameters needed to characterize the system, including the initial directions of the spins, and the position and orientation of the binary with respect to the GW detector. In this paper we consider binaries of maximally spinning BHs, and we work in the adiabatic-inspiral regime to build families of modulated detection templates that (i) are functions of very few physical and phenomenological parameters, (ii) model remarkably well the dynamical and precessional effects on the GW signal, with fitting factors on average greater than or similar to0.97, (iii) but, however, might require increasing the detection thresholds, offsetting at least partially the gains in the fitting factors. Our detection-template families are quite promising also for the case of neutron-star-black-hole binaries, with fitting factors on average approximate to0.93. For these binaries we also suggest (but do not test) a further template family, which would produce essentially exact waveforms written directly in terms of the physical spin parameters.
Additional Information
Original: © 2003 The American Physical Society. Received 27 November 2002. Published 30 May 2003. Erratum: © 2006 The American Physical Society. Received 11 July 2006. Published 31 July 2006. A small error in the computation of the gravitational wave flux in Refs. [1,2] propagates to the calculations of Ref. [3], and consequently to Eq. (1) of this paper. Special thanks go out to David Chernoff for having started the initial discussions and investigations that led to this project. We thank Jolien Creighton, Thibault Damour, Philippe Grandcle´ment, Vicky Kalogera, Yi Pan, Sterl Phinney, Bangalore Sathyaprakash, and Kip Thorne for interesting discussions. We thank Thibault Damour for useful comments on this manuscript and Cliff Will for clarifications on the material discussed in Appendix A. We acknowledge support from NSF grant PHY-0099568 and NASA grant NAG5-10707. The research of A.B. was also supported by Caltech's Richard Chace Tolman Fund. The research of Y.C. was supported by the David and Barbara Groce Fund of the San Diego Foundation; the author thanks the gravitational-wave group at the Australian National University for their hospitality. Part of the research of M.V. was performed at the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; the author thanks the INFN group at the University of Parma, Italy, for their hospitality.Errata
Erratum: Detecting gravitational waves from precessing binaries of spinning compact objects: Adiabatic limit [Phys. Rev. D 67, 104025 (2003)] Alessandra Buonanno, Yanbei Chen, and Michele Vallisneri Phys. Rev. D 74, 029904 (2006)Attached Files
Published - PhysRevD.67.pdf
Erratum - PhysRevD.74.pdf
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Additional details
- Eprint ID
- 49607
- Resolver ID
- CaltechAUTHORS:20140911-121322757
- PHY-0099568
- NSF
- NAG5-10707
- NASA
- Richard Chace Tolman Fund
- David and Barbara Groce Fund of the San Diego Foundation
- Created
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2014-09-18Created from EPrint's datestamp field
- Updated
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2023-06-01Created from EPrint's last_modified field