Buonanno, Alessandra and Chen, Yanbei and Pan, Yi and Tagoshi, Hideyuki and Vallisneri, Michele (2005) Detecting gravitational waves from precessing binaries of spinning compact objects. II. Search implementation for low-mass binaries. Physical Review D, 72 (8). Art. No. 084027. ISSN 0556-2821. http://resolver.caltech.edu/CaltechAUTHORS:BUOprd05
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Detection template families (DTFs) are built to capture the essential features of true gravitational waveforms using a small set of phenomenological waveform parameters. Buonanno, Chen, and Vallisneri [Phys. Rev. D 67, 104025 (2003)] proposed the BCV2 DTF to perform computationally efficient searches for signals from precessing binaries of compact stellar objects. Here we test the signal-matching performance of the BCV2 DTF for asymmetric-mass-ratio binaries, and specifically for double-black-hole binaries with component masses (m1,m2)[is-an-element-of][6,12]M[sun]×[1,3]M[sun], and for black-hole–neutron-star binaries with component masses (m1,m2)=(10M[sun],1.4M[sun]); we take all black holes to be maximally spinning. We find a satisfactory signal-matching performance, with fitting factors averaging between 0.94 and 0.98. We also scope out the region of BCV2 parameters needed for a template-based search, we evaluate the template match metric, we discuss a template-placement strategy, and we estimate the number of templates needed for searches at the LIGO design sensitivity. In addition, after gaining more insight in the dynamics of spin-orbit precession, we propose a modification of the BCV2 DTF that is parametrized by physical (rather than phenomenological) parameters. We test this modified "BCV2P" DTF for the (10M[sun], 1.4M[sun]) black-hole–neutron-star system, finding a signal-matching performance comparable to the BCV2 DTF, and a reliable parameter-estimation capability for target-binary quantities such as the chirp mass and the opening angle (the angle between the black-hole spin and the orbital angular momentum).
|Additional Information:||©2005 The American Physical Society (Received 22 August 2005; published 26 October 2005) We thank B. S. Sathyaprakash for useful discussions, and the LSC internal referee for providing valuable comments. M.V. is grateful to the LISA group at APC-Colle`ge de France for hospitality during the completion of this work. Research that led to this paper was supported by NSF Grant No. PHY-0099568; Y. C.’s research was also supported by the David and Barbara Groce Fund at the San Diego Foundation, and by the Alexander von Humboldt Foundation Sofja Kovalevskaja Program, funded by the German Federal Ministry of Education and Research; M.V.’s research was also supported by the LISA Mission Science Office at the Jet Propulsion Laboratory, California Institute of Technology, where it was performed under contract with the National Aeronautics and Space Administration; H. T.’s research was partially supported by Grants-in-Aid for Scientific Research (No. 14047214, No. 12640269, and No. 16540251) at the Ministry of Education of Japan.|
|Subject Keywords:||gravitational waves; binary stars; stellar mass; black holes; neutron stars|
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|Deposited By:||Archive Administrator|
|Deposited On:||22 Feb 2006|
|Last Modified:||11 Sep 2014 16:41|
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