Observing the positions of spinning binary systems using LISA

Details Observing the positions of spinning binary systems using LISA Observing the positions of spinning binary systems using LISA

Jan 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009phrvd..79b4022w&link_type=abstract

Physical Review D, vol. 79, Issue 2, id. 024022

Physics

Post-Newtonian Approximation, Perturbation Theory, Related Approximations

Scientific paper

We present an analysis of the expected angular and distance uncertainties of spinning binary systems as measured by the space-based gravitational-wave observatory LISA. We focus on two distinct cases: supermassive coalescing black holes at high redshift and nearby binary star systems with roughly constant orbital frequency. We calculate the uncertainties using least-squares parameter estimation of simulated waveforms that are accurate to 4/2 post-Newtonian order. Our results show that the presence of spin can decrease massive black hole distance and positional uncertainties by as much as factors of 10 and 100, respectively. In optimal circumstances, we find that LISA’s massive black hole merger resolution can be as low as 10-6 steradians. However, in low-mass binary systems the presence of spin tends to degrade LISA’s resolution by anywhere from a factor of 3 to a factor of 100.

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