Detecting gravitational waves from precessing binaries of spinning compact objects: Adiabatic limit
Abstract
Blackhole (BH) binaries with singleBH masses m=(520)M_{⊙}, moving on quasicircular orbits, are among the most promising sources for firstgeneration groundbased gravitationalwave (GW) detectors. Until now, the development of dataanalysis techniques to detect GWs from these sources has been focused mostly on nonspinning BHs. The dataanalysis problem for the spinning case is complicated by the necessity to model the precessioninduced 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 adiabaticinspiral 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 ≳0.97, (iii) but, however, might require increasing the detection thresholds, offsetting at least partially the gains in the fitting factors. Our detectiontemplate families are quite promising also for the case of neutronstar blackhole binaries, with fitting factors on average ≈0.93. 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.
 Publication:

Physical Review D
 Pub Date:
 May 2003
 DOI:
 10.1103/PhysRevD.67.104025
 arXiv:
 arXiv:grqc/0211087
 Bibcode:
 2003PhRvD..67j4025B
 Keywords:

 04.30.Db;
 04.25.Nx;
 04.80.Nn;
 95.55.Ym;
 Wave generation and sources;
 PostNewtonian approximation;
 perturbation theory;
 related approximations;
 Gravitational wave detectors and experiments;
 Gravitational radiation detectors;
 mass spectrometers;
 and other instrumentation and techniques;
 General Relativity and Quantum Cosmology
 EPrint:
 38 pages, 16 figures, RevTeX4. Final PRD version. Lingering typos corrected. Small corrections to GW flux terms as per Blanchet et al., PRD 71, 129902(E)129904(E) (2005)