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With one exception, previous analyses of the measurement accuracy ofgravitational wave experiments for comparable-mass binary systems haveneglected either spin-precession effects or subdominant harmonics and amplitudemodulations. Here we give the first explicit description of how these effectscombine to improve parameter estimation. We consider supermassive black holebinaries as expected to be observed with the planned space-based interferometerLISA, and study the measurement accuracy for several astrophysicallyinteresting parameters obtainable taking into account the full 2PN waveform forspinning bodies, as well as spin-precession effects. We find that for binarieswith a total mass in the range 10^5 M_Sun < M < 10^7 M_Sun at a redshift of 1,a factor ~1.5 is in general gained in accuracy, with the notable exception ofthe determination of the individual masses in equal-mass systems, for which afactor ~5 can be gained. We also find, as could be expected, that using thefull waveform helps increasing the upper mass limit for detection, which can beas high as M = 10^8 M_Sun at a redshift of 1, as well as the redshift limitwhere some information can be extracted from a system, which is roughly z = 10for M < 10^7 M_Sun, 1.5-5 times higher than with the restricted waveform. Wecomputed that the full waveform allows to use supermassive black hole binariesas standard sirens up to a redshift of z = 1.6, about 0.4 larger than whatprevious studies allowed. We found that for lower unequal-mass binary systems,the measurement accuracy is not as drastically improved as for other systems.This suggests that for these systems, adding parameters such as eccentricity oralternative gravity parameters could be achieved without much loss in theaccuracy.

physical review. d. particles, fields, gravitation, and cosmology/physical review. d, particles, fields, gravitation, and cosmology

Parameter estimation for coalescing massive binary black holes with LISA  using the full 2-post-Newtonian gravitational waveform and spin-orbit  precession