Constraining alternative theories of gravity by gravitational waves from precessing eccentric compact binaries with LISA

We calculate how strongly one can put constraints on alternative theories of gravity such as Brans-Dicke and massive graviton theories with LISA. We consider inspiral gravitational waves from a compact binary composed of a neutron star and an intermediate mass black hole in Brans-Dicke (BD) theory and that composed of a super massive black hole in massive graviton theories. We use the restricted second post-Newtonian waveforms including the effects of spins. We also take both precession and eccentricity of the orbit into account. For simplicity, we set the fiducial value for the spin of one of the binary constituents to zero so that we can apply the approximation called simple precession. We perform the Monte Carlo simulations of 104 binaries, estimating the determination accuracy of binary parameters including the BD parameter omega(BD) and the Compton wavelength of graviton lambda(g) for each binary using the Fisher matrix method. We find that including both the spin-spin coupling sigma and the eccentricity e into the binary parameters reduces the determination accuracy by an order of magnitude for the Brans-Dicke case, while it has less influence on massive graviton theories. On the other hand, including precession enhances the constraint on omega(BD) only 20% but it increases the constraint on lambda(g) by several factors. Using a (1: 4 + 1000)M-circle dot neutron star/black hole binary of SNR = root 200, one can put a constraint omega(BD) > 6944, while using a (10(7) + 10(6))M-circle dot black hole/black hole binary at 3 Gpc, one can put lambda(g) > 3.10 x 10(21) cm, on average. The latter is 4 orders of magnitude stronger than the one obtained from the solar system experiment. These results are consistent with previous results within uncontrolled errors and indicate that the effects of precession and eccentricity must be taken carefully in the parameter estimation analysis.