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Detecting gravitational waves from precessing binaries of spinning compact objects. II. Search implementation for low-mass binaries

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Buonanno,  Alessandra
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;
Laboratoire AstroParticule et Cosmologie (APC);

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Chen,  Yanbei
Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Citation

Buonanno, A., Chen, Y., Pan, Y., Tagoshi, H., & Vallisneri, M. (2005). Detecting gravitational waves from precessing binaries of spinning compact objects. II. Search implementation for low-mass binaries. Physical Review D, 72: 084027. Retrieved from http://scitation.aip.org/getabs/servlet/GetabsServlet?prog=normal&id=PRVDAQ000072000008084027000001&idtype=cvips&gifs=yes.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0013-4F6B-3
Abstract
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): (6~12Msun, 1~3Msun), and for black-hole--neutron-star binaries with component masses (m1,m2) = (10Msun, 1.4Msun); 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 (10Msun, 1.4Msun) 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).